[
{
"id": "authors:fj0qq-ckq70",
"collection": "authors",
"collection_id": "fj0qq-ckq70",
"cite_using_url": "https://authors.library.caltech.edu/records/fj0qq-ckq70",
"type": "article",
"title": "AT2019cmw: A highly luminous, cooling featureless TDE candidate from the disruption of a high mass star in an early-type galaxy",
"author": [
{
"family_name": "Wise",
"given_name": "Jacob L"
},
{
"family_name": "Perley",
"given_name": "Daniel A",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Sarin",
"given_name": "Nikhil"
},
{
"family_name": "Matsumoto",
"given_name": "Tatsuya"
},
{
"family_name": "Hinds",
"given_name": "K-Ryan"
},
{
"family_name": "Yao",
"given_name": "Yuhan"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Schulze",
"given_name": "Steve"
},
{
"family_name": "Bochenek",
"given_name": "Aleksandra"
},
{
"family_name": "Coughlin",
"given_name": "Michael W"
},
{
"family_name": "De",
"given_name": "Kishalay"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"clpid": "Dekany-Richard"
},
{
"family_name": "Frederick",
"given_name": "Sara"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Gezari",
"given_name": "Suvi"
},
{
"family_name": "Graham",
"given_name": "Matthew J",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Ho",
"given_name": "Anna Y Q"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Omand",
"given_name": "Conor",
"orcid": "0000-0002-9646-8710"
},
{
"family_name": "Johnson",
"given_name": "Natalya"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "Ward",
"given_name": "Charlotte"
},
{
"family_name": "Wold",
"given_name": "Avery",
"orcid": "0000-0002-9998-6732",
"clpid": "Wold-Avery"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "We present optical/UV photometric and spectroscopic observations, as well as X-ray and radio follow-up, of the extraordinary event AT2019cmw. With a peak bolometric luminosity of ~10^(45.6) erg s\u207b¹, it is one of the most luminous thermal transients ever discovered. Extensive spectroscopic follow-up post-peak showed only a featureless continuum throughout its evolution. This, combined with its nuclear location, blue colour at peak and lack of prior evidence of an AGN in its host lead us to interpret this event as a \"featureless\" tidal disruption event (TDE). It displays photometric evolution atypical of most TDEs, cooling from ~30 kK to ~10 kK in the first ~300 days post-peak, with potential implications for future photometric selection of candidate TDEs. No X-ray or radio emission is detected, placing constraints on the presence of on-axis jetted emission or a visible inner-accretion disk. Modelling the optical light curve with existing theoretical prescriptions, we find that AT2019cmw may be the result of the disruption of a star in the tens of solar masses by a supermassive black hole (SMBH). Combined with a lack of detectable star formation in its host galaxy, it could imply the existence of a localised region of star formation around the SMBH. This could provide a new window to probe nuclear star formation and the shape of the initial mass function (IMF) in close proximity to SMBHs out to relatively high redshifts.
",
"doi": "10.1093/mnras/stag130",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2026-03",
"series_number": "3",
"volume": "546",
"issue": "3",
"pages": "stag130"
},
{
"id": "authors:024hn-k0f54",
"collection": "authors",
"collection_id": "024hn-k0f54",
"cite_using_url": "https://authors.library.caltech.edu/records/024hn-k0f54",
"type": "article",
"title": "A thermonuclear supernova interacting with hydrogen- and helium-deficient circumstellar material. SN 2020aeuh as a SN Ia-CSM-C/O?",
"author": [
{
"family_name": "Tsalapatas",
"given_name": "K.",
"orcid": "0009-0004-1062-8886"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Chiba",
"given_name": "R.",
"orcid": "0009-0003-4594-3715"
},
{
"family_name": "Kool",
"given_name": "E.",
"orcid": "0000-0002-7252-3877"
},
{
"family_name": "Johansson",
"given_name": "J.",
"orcid": "0000-0001-5975-290X"
},
{
"family_name": "Rosswog",
"given_name": "S."
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Moriya",
"given_name": "T. J.",
"orcid": "0000-0003-1169-1954"
},
{
"family_name": "Andreoni",
"given_name": "I.",
"orcid": "0000-0002-8977-1498"
},
{
"family_name": "Brink",
"given_name": "T. G.",
"orcid": "0000-0001-5955-2502"
},
{
"family_name": "Chen",
"given_name": "T. X.",
"orcid": "0000-0001-9152-6224",
"clpid": "Chen-Tracy-X"
},
{
"family_name": "Covarrubias",
"given_name": "S.",
"clpid": "Covarrubias-S"
},
{
"family_name": "De",
"given_name": "K.",
"orcid": "0000-0002-8989-0542"
},
{
"family_name": "Dimitriadis",
"given_name": "G.",
"orcid": "0000-0001-9494-179X"
},
{
"family_name": "Filippenko",
"given_name": "A. V.",
"orcid": "0000-0003-3460-0103"
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Gangopadhyay",
"given_name": "A.",
"orcid": "0000-0002-3884-5637"
},
{
"family_name": "Maguire",
"given_name": "K.",
"orcid": "0000-0002-9770-3508"
},
{
"family_name": "Mo",
"given_name": "G.",
"orcid": "0000-0001-6331-112X"
},
{
"family_name": "Sharma",
"given_name": "Y.",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Sravan",
"given_name": "N."
},
{
"family_name": "Terwel",
"given_name": "J. H.",
"orcid": "0000-0001-9834-3439"
},
{
"family_name": "Yang",
"given_name": "Y."
}
],
"abstract": "Identifying the progenitors of thermonuclear supernovae (Type Ia supernovae; SNe Ia) remains a key objective in contemporary astronomy. The rare sub-class of SNe Ia-CSM that interacts with circumstellar material (CSM) allows for studies of the progenitor’s environment before explosion, and generally favours single-degenerate progenitor channels. The case of SN Ia-CSM PTF11kx clearly connected thermonuclear explosions with hydrogen-rich CSM-interacting events, and the more recent SN 2020eyj connected SNe Ia with helium-rich companion progenitors. Both of these objects displayed delayed CSM interaction which established their thermonuclear nature. Here we present a study of SN 2020aeuh, a Type Ia-CSM with delayed interaction. We analyse photometric and spectroscopic data that monitor the evolution of SN 2020aeuh and compare its properties with those of peculiar SNe Ia and core-collapse SNe. At early times, the evolution of SN 2020aeuh resembles a slightly overluminous SN Ia. Later, the interaction-dominated spectra develop the same pseudocontinuum seen in Type Ia-CSM PTF11kx and SN 2020eyj. However, the later-time spectra of SN 2020aeuh lack hydrogen and helium narrow lines. Instead, a few narrow lines could be attributed to carbon and oxygen. We fit the pseudobolometric light curve with a CSM-interaction model, yielding a CSM mass of 1\u2005−\u20052 M\u2299. We propose that SN 2020aeuh was a Type Ia supernova that eventually interacted with a dense medium that was deficient in both hydrogen and helium. Whereas previous SNe Ia-CSM constitute our best evidence of non-degenerate companion progenitors, the CSM around SN 2020aeuh is more difficult to understand. We include a hydrodynamical simulation for a double-degenerate dynamical collision to showcase that such a progenitor scenario could produce significant amounts of hydrogen-poor CSM, although likely not as much as the inferred CSM mass around SN 2020aeuh. It is clear that SN 2020aeuh challenges current models of stellar evolution leading up to a SN Ia explosion.
",
"doi": "10.1051/0004-6361/202556369",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy & Astrophysics",
"publication_date": "2025-12",
"volume": "704",
"pages": "A135"
},
{
"id": "authors:mj6ey-k6315",
"collection": "authors",
"collection_id": "mj6ey-k6315",
"cite_using_url": "https://authors.library.caltech.edu/records/mj6ey-k6315",
"type": "article",
"title": "The ambiguous AT2022rze: changing-look AGN mimicking a supernova in a merging galaxy system",
"author": [
{
"family_name": "Pessi",
"given_name": "P J",
"orcid": "0000-0002-8041-8559"
},
{
"family_name": "Lunnan",
"given_name": "R"
},
{
"family_name": "Sollerman",
"given_name": "J",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Yan",
"given_name": "L",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Le\u00a0Reste",
"given_name": "A",
"orcid": "0000-0003-1767-6421"
},
{
"family_name": "Yao",
"given_name": "Y"
},
{
"family_name": "Nordblom",
"given_name": "S"
},
{
"family_name": "Sharma",
"given_name": "Y",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Gilfanov",
"given_name": "M",
"orcid": "0000-0003-4029-6769"
},
{
"family_name": "Sunyaev",
"given_name": "R",
"orcid": "0000-0002-2764-7192"
},
{
"family_name": "Schulze",
"given_name": "S"
},
{
"family_name": "Johansson",
"given_name": "J"
},
{
"family_name": "Gangopadhyay",
"given_name": "A"
},
{
"family_name": "Fremling",
"given_name": "C",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Tristram",
"given_name": "K",
"orcid": "0000-0001-8281-5059"
},
{
"family_name": "Hayes",
"given_name": "M J",
"orcid": "0000-0001-8587-218X"
},
{
"family_name": "Fransson",
"given_name": "C"
},
{
"family_name": "Hu",
"given_name": "Y",
"orcid": "0000-0002-9744-3910"
},
{
"family_name": "Brennan",
"given_name": "S J"
},
{
"family_name": "Rose",
"given_name": "S",
"clpid": "Rose-S"
},
{
"family_name": "De",
"given_name": "K",
"orcid": "0000-0002-8989-0542"
},
{
"family_name": "Hinds",
"given_name": "K-R",
"orcid": "0000-0002-0129-806X"
},
{
"family_name": "Liu",
"given_name": "C",
"orcid": "0000-0002-7866-4531"
},
{
"family_name": "Miller",
"given_name": "A A",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Qin",
"given_name": "Y-J",
"orcid": "0000-0003-3658-6026",
"clpid": "Qin-Yu-Jing"
},
{
"family_name": "Charalampopoulos",
"given_name": "P",
"orcid": "0000-0002-0326-6715"
},
{
"family_name": "Gkini",
"given_name": "A",
"orcid": "0009-0000-9383-2305"
},
{
"family_name": "Graham",
"given_name": "M J",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Guti\u00e9rrez",
"given_name": "C P",
"orcid": "0000-0003-2375-2064"
},
{
"family_name": "Mattila",
"given_name": "S",
"orcid": "0000-0001-7497-2994"
},
{
"family_name": "Nagao",
"given_name": "T",
"orcid": "0000-0002-3933-7861"
},
{
"family_name": "P\u00e9rez-Fournon",
"given_name": "I",
"orcid": "0000-0002-2807-6459"
},
{
"family_name": "Poidevin",
"given_name": "F",
"orcid": "0000-0002-5391-5568"
},
{
"family_name": "Bloom",
"given_name": "J S",
"orcid": "0000-0002-7777-216X"
},
{
"family_name": "Brugger",
"given_name": "J",
"clpid": "Brugger-James"
},
{
"family_name": "Chen",
"given_name": "T X",
"orcid": "0000-0001-9152-6224",
"clpid": "Chen-Tracy-X"
},
{
"family_name": "Kasliwal",
"given_name": "M M",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Masci",
"given_name": "F J",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Purdum",
"given_name": "J N",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah-N"
}
],
"abstract": "AT2022rze is a luminous, ambiguous transient located south-east of the geometric centre of its host galaxy at redshift $z = 0.08$. The host appears to be formed by a merging galaxy system. The observed characteristics of AT2022rze are reminiscent of active galactic nuclei (AGNs), tidal disruption events, and superluminous supernovae. The transient reached a peak absolute magnitude of $-$20.2 $\\pm$ 0.2 mag, showing a sharp rise (t$_{\\mathrm{rise,1/e}} = 27.5 \\pm 0.6$ d) followed by a slow decline (t$_{\\mathrm{dec,1/e}} = 382.9 \\pm 0.6$). Its bumpy light curve and narrow Balmer lines indicate the presence of gas (and dust). Its light curve shows rather red colours, indicating that the transient could be affected by significant host extinction. The spectra reveal coronal lines, indicative of high-energy (X-ray/UV) emission. Archival data reveal no prior activity at this location, disfavouring a steady-state AGN, although an optical spectrum obtained prior to the transient is consistent with an AGN classification of the host. Based on this, we conclude that the transient most likely represents a changing-look AGN at the centre of the smallest component of the merging system.
",
"doi": "10.1093/mnras/staf1433",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2025-10",
"series_number": "4",
"volume": "542",
"issue": "4",
"pages": "3354-3372"
},
{
"id": "authors:hmgbm-wde39",
"collection": "authors",
"collection_id": "hmgbm-wde39",
"cite_using_url": "https://authors.library.caltech.edu/records/hmgbm-wde39",
"type": "article",
"title": "Twin Peaks: SN 2021uvy and SN 2022hgk in the Landscape of Double-peaked Stripped Envelope Supernovae",
"author": [
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Meynardie",
"given_name": "William",
"orcid": "0009-0001-6903-0131"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Das",
"given_name": "Kaustav K.",
"orcid": "0000-0001-8372-997X",
"clpid": "Das-Kaustav-K"
},
{
"family_name": "Yun",
"given_name": "Gene",
"orcid": "0009-0001-3390-5151"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Wise",
"given_name": "Jacob",
"orcid": "0000-0003-0733-2916"
},
{
"family_name": "Brennan",
"given_name": "Se\u00e1n J.",
"orcid": "0000-0003-1325-6235"
},
{
"family_name": "Brink",
"given_name": "Thomas G.",
"orcid": "0000-0001-5955-2502"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Hinds",
"given_name": "K. R.",
"orcid": "0000-0002-0129-806X"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Li",
"given_name": "Maggie L.",
"orcid": "0009-0001-6911-9144",
"clpid": "Li-Maggie-L"
},
{
"family_name": "Nolan",
"given_name": "Kira",
"orcid": "0009-0002-4724-7118",
"clpid": "Nolan-Kira"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Purdum",
"given_name": "Josiah N.",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah-N"
},
{
"family_name": "Rose",
"given_name": "Sam",
"orcid": "0000-0003-4725-4481",
"clpid": "Rose-Sam"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Sit",
"given_name": "Tawny",
"orcid": "0000-0001-8208-9755"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331"
},
{
"family_name": "Wold",
"given_name": "Avery",
"orcid": "0000-0002-9998-6732",
"clpid": "Wold-Avery"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509"
}
],
"abstract": "\n
In recent years, a class of stripped-envelope supernovae (SESNe) has emerged that show two distinct peaks in their light curves, where the first peak cannot be attributed to shock cooling emission. Such peculiar supernovae are often studied individually, explained by invoking some combination of powering mechanisms. However, they have seldom been discussed in the broader context of double-peaked SESNe. In this paper, we attempt to form a picture of the landscape of double-peaked SESNe and their powering mechanisms by adding two more objects—SN 2021uvy and SN 2022hgk. SN 2021uvy is a broad and luminous SN Ib with an unusually long rise of the first peak and constant color evolution with rising photospheric temperature during the second peak. Although its first peak is similar to that of SN 2019stc, their second peaks differ in properties, making it unique among double-peaked objects. SN 2022hgk shows striking photometric similarity to SN 2019cad and spectroscopic similarity to SN 2005bf, both of which have been suggested to be powered by a double-nickel distribution in their ejecta. We analyze their light curves and colors, compare them with a sample of other double-peaked published supernovae for which we have additional data, and analyze the light curve parameters of the sample. We observe a correlation (p-value ∼ 0.025) between the peak absolute magnitudes of the first and second peaks. The sample shows variety in the photometric and spectroscopic properties, and thus no single definitive powering mechanism applies to the whole sample. However, sub-groups of similarity exist that can be explained by mechanisms like the double-nickel distribution, magnetar central engine, interaction, and fallback accretion. We also map out the duration between the peaks (Δt21) versus the difference between peak absolute magnitudes (ΔM21) as a phase-space that could potentially delineate the most promising powering mechanisms for the double-peaked SESNe.
\n
Stars are initially powered by the fusion of hydrogen to helium. These ashes serve as fuel in a series of stages, transforming massive stars into a structure of shells. These are composed of natal hydrogen on the outside and consecutively heavier compositions inside, predicted to be dominated by He, C/O, O/Ne/Mg and O/Si/S (refs. 4,5). Silicon and sulfur are fused into iron, leading to the collapse of the core and either a supernova explosion or the formation of a black hole. Stripped stars, in which the outer hydrogen layer has been removed and the internal He-rich or even the C/O layer below it is exposed, provide evidence for this shell structure and the cosmic element production mechanism it reflects. The supernova types that arise from stripped stars embedded in shells of circumstellar material (CSM) confirm this scenario. However, direct evidence for the most interior shells, which are responsible for producing elements heavier than oxygen, is lacking. Here we report the discovery of the supernova (SN) 2021yfj resulting from a star stripped to its O/Si/S-rich layer. We directly observe a thick, massive Si/S-rich shell, expelled by the progenitor shortly before the supernova explosion. Exposing such an inner stellar layer is theoretically challenging and probably requires a rarely observed mass-loss mechanism. This rare supernova event reveals advanced stages of stellar evolution, forming heavier elements, including silicon, sulfur and argon, than those detected on the surface of any known class of massive stars.
",
"doi": "10.1038/s41586-025-09375-3",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "2025-08-21",
"series_number": "8077",
"volume": "644",
"issue": "8077",
"pages": "634-639"
},
{
"id": "authors:zc70w-ew217",
"collection": "authors",
"collection_id": "zc70w-ew217",
"cite_using_url": "https://authors.library.caltech.edu/records/zc70w-ew217",
"type": "article",
"title": "The First Systematically Identified Repeating Partial Tidal Disruption Event",
"author": [
{
"family_name": "Somalwar",
"given_name": "Jean J.",
"orcid": "0000-0001-8426-5732",
"clpid": "Somalwar-Jean-J"
},
{
"family_name": "Ravi",
"given_name": "Vikram",
"orcid": "0000-0002-7252-5485",
"clpid": "Ravi-Vikram"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509"
},
{
"family_name": "Guolo",
"given_name": "Muryel",
"orcid": "0000-0002-5063-0751"
},
{
"family_name": "Graham",
"given_name": "Matthew",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Hammerstein",
"given_name": "Erica",
"orcid": "0000-0002-5698-8703"
},
{
"family_name": "Lu",
"given_name": "Wenbin",
"orcid": "0000-0002-1568-7461"
},
{
"family_name": "Nicholl",
"given_name": "Matt",
"orcid": "0000-0002-2555-3192"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Stein",
"given_name": "Robert",
"orcid": "0000-0003-2434-0387",
"clpid": "Stein-Robert"
},
{
"family_name": "van Velzen",
"given_name": "Sjoert",
"orcid": "0000-0002-3859-8074"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed"
}
],
"abstract": "\n
Tidal disruption events (TDEs) occur when a star enters the tidal radius of a supermassive black hole. If the star only grazes the tidal radius, a fraction of the stellar mass will be accreted in a partial TDE (pTDE). The remainder can continue orbiting and may be redisrupted at pericenter, causing a repeating pTDE. pTDEs may be as or more common than full TDEs, yet few are known. In this work, we present the discovery of the first repeating pTDE from a systematically selected sample, AT 2020vdq. AT 2020vdq was originally identified as an optically and radio-flaring TDE. Around 947 days after its discovery, it rebrightened dramatically in the optical. The optical flare was remarkably fast and luminous given its black hole mass compared to previous TDEs. It was accompanied by extremely broad (∼0.1c) optical/UV spectral features and faint X-ray emission (LX ∼ 3 × 1041 erg s−1), but no new radio-emitting component. Based on the transient optical/UV spectral features and the broadband lightcurve, we show that AT 2020vdq is a repeating pTDE. We then use it to constrain TDE models; in particular, we favor a star originally in a very tight binary system that is tidally broken apart by the Hills mechanism. We also constrain the repeating pTDE rate to be 10−6–10−5 yr−1 galaxy−1, with uncertainties dominated by the unknown distribution of pTDE repeat timescales. In the Hills framework, this means the binary fraction in the galactic nucleus is of the order of a few percent.
\n
We present the luminosity function and volumetric rate of a sample of Type IIP supernovae (SNe) from the Zwicky Transient Facility Census of the Local Universe survey (CLU). This is the largest sample of Type IIP SNe from a systematic volume-limited survey to-date. The final sample includes 330 Type IIP SNe and 36 low-luminosity Type II (LLIIP) SNe with Mr,peak > −16 mag, which triples the literature sample of LLIIP SNe. The fraction of LLIIP SNe is 19\u207a³\u208b\u2084% of the total CLU Type IIP SNe population (8\u207a¹\u208b\u2082% of all core-collapse SNe). This implies that while LLIIP SNe likely represent the fate of core-collapse SNe of 8–12 M\u2299 progenitors, they alone cannot account for the fate of all massive stars in this mass range. To derive an absolute rate, we estimate the ZTF pipeline efficiency as a function of the apparent magnitude and the local surface brightness. We derive a volumetric rate of (3.9^(+0.4)_(−0.4)) × 10\u2074 Gpc\u207b³ yr\u207b¹ for Type IIP SNe and (7.3^(+0.6)_(-0.6) x 10³ Gpc\u207b³ yr\u207b¹ for LLIIP SNe. Now that the rate of LLIIP SNe is robustly derived, the unresolved discrepancy between core-collapse SN rates and star formation rates cannot be explained by LLIIP SNe alone.
",
"doi": "10.1088/1538-3873/adcaeb",
"issn": "0004-6280",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2025-04",
"series_number": "4",
"volume": "137",
"issue": "4",
"pages": "044203"
},
{
"id": "authors:msjpj-n0609",
"collection": "authors",
"collection_id": "msjpj-n0609",
"cite_using_url": "https://authors.library.caltech.edu/records/msjpj-n0609",
"type": "article",
"title": "Sample of hydrogen-rich superluminous supernovae from the Zwicky Transient Facility",
"author": [
{
"family_name": "Pessi",
"given_name": "P. J.",
"orcid": "0000-0002-8041-8559"
},
{
"family_name": "Lunnan",
"given_name": "R.",
"orcid": "0000-0001-9454-4639"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Gkini",
"given_name": "A.",
"orcid": "0009-0000-9383-2305"
},
{
"family_name": "Gangopadhyay",
"given_name": "A.",
"orcid": "0000-0002-3884-5637"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Gal-Yam",
"given_name": "A.",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Perley",
"given_name": "D. A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Chen",
"given_name": "T.-W.",
"orcid": "0000-0002-1066-6098"
},
{
"family_name": "Hinds",
"given_name": "K. R.",
"orcid": "0000-0002-0129-806X"
},
{
"family_name": "Brennan",
"given_name": "S. J.",
"orcid": "0000-0003-1325-6235"
},
{
"family_name": "Hu",
"given_name": "Y.",
"orcid": "0000-0002-9744-3910"
},
{
"family_name": "Singh",
"given_name": "A.",
"orcid": "0000-0003-2091-622X"
},
{
"family_name": "Andreoni",
"given_name": "I.",
"orcid": "0000-0002-8977-1498"
},
{
"family_name": "Cook",
"given_name": "D. O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Ho",
"given_name": "A. Y. Q.",
"orcid": "0000-0002-9017-3567"
},
{
"family_name": "Sharma",
"given_name": "Y.",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "van Velzen",
"given_name": "S."
},
{
"family_name": "Kangas",
"given_name": "T."
},
{
"family_name": "Wold",
"given_name": "A.",
"orcid": "0000-0002-9998-6732",
"clpid": "Wold-Avery"
},
{
"family_name": "Bellm",
"given_name": "E. C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Bloom",
"given_name": "J. S.",
"orcid": "0000-0002-7777-216X"
},
{
"family_name": "Graham",
"given_name": "M. J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Riddle",
"given_name": "R.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
}
],
"abstract": "Context. Hydrogen-rich superluminous supernovae (SLSNe II) are rare. The exact mechanism producing their extreme light curve peaks is not understood. Analysis of single events and small samples suggest that circumstellar material (CSM) interaction is the main mechanism responsible for the observed features. However, other mechanisms cannot be discarded. Large sample analysis can provide clarification. Aims. We aim to characterize the light curves of a sample of 107 SLSNe II to provide valuable information that can be used to validate theoretical models. Methods. We analyzed the gri light curves of SLSNe II obtained through ZTF. We studied the peak absolute magnitudes and characteristic timescales. When possible, we computed the g\u2005−\u2005r colors and pseudo-bolometric light curves, and estimated lower limits for their total radiated energy. We also studied the luminosity distribution of our sample and estimated the fraction that would be observable by the LSST. Finally, we compared our sample to other H-rich SNe and to H-poor SLSNe I. Results. SLSNe II are heterogeneous. Their median peak absolute magnitude is ∼\u2005−\u200520.3 mag in optical bands. Their rise can take from ∼two weeks to over three months, and their decline times range from ∼twenty days to over a year. We found no significant correlations between peak magnitude and timescales. SLSNe II tend to show fainter peaks, longer declines, and redder colors than SLSNe I. Conclusions. We present the largest sample of SLSN II light curves to date, comprising 107 events. Their diversity could be explained by different CSM morphologies, although theoretical analysis is needed to explore alternative scenarios. Other luminous transients, such as active galactic nuclei, tidal disruption events or SNe Ia-CSM, can easily become contaminants. Thus, good multiwavelength light curve coverage becomes paramount. LSST could miss ∼30% of the ZTF events in its gri band footprint.
",
"doi": "10.1051/0004-6361/202452014",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2025-03",
"volume": "695",
"pages": "A142"
},
{
"id": "authors:pmxpj-pkn60",
"collection": "authors",
"collection_id": "pmxpj-pkn60",
"cite_using_url": "https://authors.library.caltech.edu/records/pmxpj-pkn60",
"type": "article",
"title": "ZTF SN Ia DR2: Environmental dependencies of stretch and luminosity for a volume-limited sample of 1000 type Ia supernovae",
"author": [
{
"family_name": "Ginolin",
"given_name": "M.",
"orcid": "0009-0004-5311-9301"
},
{
"family_name": "Rigault",
"given_name": "M.",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Smith",
"given_name": "M.",
"orcid": "0000-0002-3321-1432"
},
{
"family_name": "Copin",
"given_name": "Y.",
"orcid": "0000-0002-5317-7518"
},
{
"family_name": "Ruppin",
"given_name": "F.",
"orcid": "0000-0002-0955-8954"
},
{
"family_name": "Dimitriadis",
"given_name": "G.",
"orcid": "0000-0001-9494-179X"
},
{
"family_name": "Goobar",
"given_name": "A.",
"orcid": "0000-0002-4163-4996"
},
{
"family_name": "Johansson",
"given_name": "J.",
"orcid": "0000-0001-5975-290X"
},
{
"family_name": "Maguire",
"given_name": "K.",
"orcid": "0000-0002-9770-3508"
},
{
"family_name": "Nordin",
"given_name": "J.",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Amenouche",
"given_name": "M.",
"orcid": "0009-0006-7454-3579"
},
{
"family_name": "Aubert",
"given_name": "M.",
"orcid": "0009-0002-7667-8814"
},
{
"family_name": "Barjou-Delayre",
"given_name": "C."
},
{
"family_name": "Betoule",
"given_name": "M.",
"orcid": "0000-0003-0804-836X"
},
{
"family_name": "Burgaz",
"given_name": "U.",
"orcid": "0000-0003-0126-3999"
},
{
"family_name": "Carreres",
"given_name": "B.",
"orcid": "0000-0002-7234-844X"
},
{
"family_name": "Deckers",
"given_name": "M.",
"orcid": "0000-0001-8857-9843"
},
{
"family_name": "Dhawan",
"given_name": "S.",
"orcid": "0000-0002-2376-6979"
},
{
"family_name": "Feinstein",
"given_name": "F.",
"orcid": "0000-0001-5548-3466"
},
{
"family_name": "Fouchez",
"given_name": "D.",
"orcid": "0000-0002-7496-3796"
},
{
"family_name": "Galbany",
"given_name": "L.",
"orcid": "0000-0002-1296-6887"
},
{
"family_name": "Ganot",
"given_name": "C.",
"orcid": "0009-0000-6300-9174"
},
{
"family_name": "Harvey",
"given_name": "L.",
"orcid": "0000-0003-3393-9383"
},
{
"family_name": "de Jaeger",
"given_name": "T.",
"orcid": "0000-0001-6069-1139"
},
{
"family_name": "Kenworthy",
"given_name": "W. D.",
"orcid": "0000-0002-5153-5983"
},
{
"family_name": "Kim",
"given_name": "Y.-L.",
"orcid": "0000-0002-1031-0796"
},
{
"family_name": "Kowalski",
"given_name": "M.",
"orcid": "0000-0001-8594-8666"
},
{
"family_name": "Kuhn",
"given_name": "D.",
"orcid": "0009-0005-8110-397X"
},
{
"family_name": "Lacroix",
"given_name": "L."
},
{
"family_name": "M\u00fcller-Bravo",
"given_name": "T. E.",
"orcid": "0000-0003-3939-7167"
},
{
"family_name": "Nugent",
"given_name": "P.",
"orcid": "0000-0002-3389-0586"
},
{
"family_name": "Popovic",
"given_name": "B.",
"orcid": "0000-0002-8012-6978"
},
{
"family_name": "Racine",
"given_name": "B.",
"orcid": "0000-0001-8861-3052"
},
{
"family_name": "Rosnet",
"given_name": "P.",
"orcid": "0000-0002-6099-7565"
},
{
"family_name": "Rosselli",
"given_name": "D.",
"orcid": "0000-0001-6839-1421"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Terwel",
"given_name": "J. H.",
"orcid": "0000-0001-9834-3439"
},
{
"family_name": "Townsend",
"given_name": "A.",
"orcid": "0000-0001-6343-3362"
},
{
"family_name": "Brugger",
"given_name": "J.",
"clpid": "Brugger-J"
},
{
"family_name": "Bellm",
"given_name": "E. C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kulkarni",
"given_name": "S.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Laher",
"given_name": "R. R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "Masci",
"given_name": "F. J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Riddle",
"given_name": "R. L.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Sharma",
"given_name": "Y.",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
}
],
"abstract": "Context. Type Ia supernova (SN Ia) cosmology studies will soon be dominated by systematic, uncertainties, rather than statistical ones. Thus, it is crucial to understand the unknown phenomena potentially affecting their luminosity that may remain, such as astrophysical biases. For their accurate application in such studies, SN Ia magnitudes need to be standardised; namely, they must be corrected for their correlation with the light-curve width and colour.
\nAims. Here, we investigate how the standardisation procedure used to reduce the scatter of SN Ia luminosities is affected by their environment. Our aim is to reduce scatter and improve the standardisation process.
\nMethods. We first studied the SN Ia stretch distribution, as well as its dependence on environment, as characterised by local and global (g\u2005−\u2005z) colour and stellar mass. We then looked at the standardisation parameter, α, which accounts for the correlation between residuals and stretch, along with its environment dependency and linearity. Finally, we computed the magnitude offsets between SNe in different astrophysical environments after the colour and stretch standardisations (i.e. steps). This analysis has been made possible thanks to the unprecedented statistics of the volume-limited Zwicky Transient Facility (ZTF) SN Ia DR2 sample.
\nResults. The stretch distribution exhibits a bimodal behaviour, as previously found in the literature. However, we find the distribution to be dependent on environment. Specifically, the mean stretch modes decrease with host stellar mass, at a 9.2σ significance. We demonstrate, at the 13.4σ level, that the stretch-magnitude relation is non-linear, challenging the usual linear stretch-residuals relation currently used in cosmological analyses. In fitting for a broken-α model, we did indeed find two different slopes between stretch regimes (x1\u2004\u2276\u2004x10 with x10\u2004=\u2004−0.48\u2005±\u20050.08): αlow\u2004=\u20040.271\u2005±\u20050.011 and αhigh\u2004=\u20040.083\u2005±\u20050.009, comprising a difference of Δα\u2004=\u2004−0.188\u2005±\u20050.014. As the relative proportion of SNe Ia in the high-stretch and low-stretch modes evolves with redshift and environment, this implies that a single-fitted α also evolves with the redshift and environment. Concerning the environmental magnitude offset γ, we find it to be greater than 0.12 mag, regardless of the considered environmental tracer used (local or global colour and stellar mass), all measured at the ≥5σ level. When accounting for the non-linearity of the stretch, these steps increase to ∼0.17 mag, measured with a precision of 0.01 mag. Such strong results highlight the importance of using a large volume-limited dataset to probe the underlying SN Ia-host correlations.
",
"doi": "10.1051/0004-6361/202450378",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2025-03",
"volume": "695",
"pages": "A140"
},
{
"id": "authors:ebr8w-24m21",
"collection": "authors",
"collection_id": "ebr8w-24m21",
"cite_using_url": "https://authors.library.caltech.edu/records/ebr8w-24m21",
"type": "article",
"title": "A Diverse, Overlooked Population of Type Ia Supernovae Exhibiting Mid-infrared Signatures of Delayed Circumstellar Interaction",
"author": [
{
"family_name": "Mo",
"given_name": "Geoffrey",
"orcid": "0000-0001-6331-112X"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542"
},
{
"family_name": "Wiston",
"given_name": "Eli",
"orcid": "0009-0002-4843-2913"
},
{
"family_name": "A. J.",
"given_name": "Nayana",
"orcid": "0000-0002-8070-5400"
},
{
"family_name": "Margutti",
"given_name": "Raffaella",
"orcid": "0000-0003-4768-7586"
},
{
"family_name": "Frostig",
"given_name": "Danielle",
"orcid": "0000-0002-7197-9004"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Moriya",
"given_name": "Takashi J.",
"orcid": "0000-0003-1169-1954"
},
{
"family_name": "Burdge",
"given_name": "Kevin B.",
"orcid": "0000-0002-7226-836X"
},
{
"family_name": "Jencson",
"given_name": "Jacob",
"orcid": "0000-0001-5754-4007",
"clpid": "Jencson-Jacob"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj R.",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj-R"
},
{
"family_name": "Lourie",
"given_name": "Nathan P.",
"orcid": "0000-0002-4585-9981"
}
],
"abstract": "\n
Type Ia supernovae (SNe Ia) arise from the thermonuclear explosions of white dwarfs in multiple-star systems. A rare subclass of SNe Ia exhibit signatures of interaction with circumstellar material (CSM), allowing for direct constraints on companion material. While most known events show evidence for dense nearby CSM identified via peak-light spectroscopy (as SNe Ia-CSM), targeted late-time searches have revealed a handful of cases exhibiting delayed CSM interaction with detached shells. Here we present the first all-sky search for late CSM interaction in SNe Ia using a new image subtraction pipeline for mid-infrared data from the NEOWISE space telescope. Analyzing a sample of ≈8500 SNe Ia, we report evidence for late-time mid-infrared brightening in five previously overlooked events spanning subtypes SNe Iax, SNe Ia-91T, and super-Chandra SNe Ia. Our systematic search doubles the known sample and suggests that \u22730.05% of SNe Ia exhibit mid-infrared signatures of delayed CSM interaction. The mid-infrared light curves ubiquitously indicate the presence of multiple (or extended) detached CSM shells located at \u22731016–1017 cm, containing 10−6 to 10−4 M\u2299 of dust, with some sources showing evidence for new dust formation, possibly within the cold, dense shell of the ejecta. We do not detect interaction signatures in spectroscopic and radio follow-up; however, the limits are largely consistent with previously confirmed events given the sensitivity and observation phase. Our results highlight that CSM interaction is more prevalent than previously estimated from optical and ultraviolet searches and that mid-infrared synoptic surveys provide a unique window into this phenomenon.
\n
More than 3000 spectroscopically confirmed Type Ia supernovae (SNe Ia) are presented in the second data release (DR2) of the Zwicky Transient Facility survey. In this paper we detail the spectral properties of 482 SNe Ia near maximum light, up to a redshift limit of z\u2004≤\u20040.06. We measured the velocities and pseudo-equivalent widths (pEW) of key spectral features (Si\u202fIIλ5972 and Si\u202fIIλ6355) and investigated the relation between the properties of the spectral features and the photometric properties from the SALT2 light-curve parameters as a function of spectroscopic sub-class. We discuss the non-negligible impact of host galaxy contamination on SN Ia spectral classifications, and we investigate the accuracy of spectral template matching of the DR2 sample. We define a new subclass of underluminous SNe Ia (04gs-like) that lie spectroscopically between normal SNe Ia and transitional 86G-like SNe Ia (stronger Si\u202fIIλ5972 than normal SNe Ia, but significantly weaker Ti\u202fII features than 86G-like SNe). We model these 04gs-like SN Ia spectra using the radiative-transfer spectral synthesis code TARDIS and show that cooler temperatures alone are unable to explain their spectra; some changes in elemental abundances are also required. However, the broad continuity in spectral properties seen from bright (91T-like) to faint normal SN Ia, including the transitional and 91bg-like SNe Ia, suggests that variations within a single explosion model may be able to explain their behaviour.
",
"doi": "10.1051/0004-6361/202450386",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2025-02",
"volume": "694",
"pages": "A9"
},
{
"id": "authors:5gj69-yyr83",
"collection": "authors",
"collection_id": "5gj69-yyr83",
"cite_using_url": "https://authors.library.caltech.edu/records/5gj69-yyr83",
"type": "article",
"title": "A Link Between White Dwarf Pulsars and Polars: Multiwavelength Observations of the 9.36-minute Period Variable Gaia22ayj",
"author": [
{
"family_name": "Rodriguez",
"given_name": "Antonio C.",
"orcid": "0000-0003-4189-9668",
"clpid": "Rodriguez-Antonio-C"
},
{
"family_name": "El-Badry",
"given_name": "Kareem",
"orcid": "0000-0002-6871-1752",
"clpid": "El-Badry-Kareem"
},
{
"family_name": "Hakala",
"given_name": "Pasi",
"orcid": "0009-0003-6437-0369"
},
{
"family_name": "Rodr\u00edguez-Gil",
"given_name": "Pablo",
"orcid": "0000-0002-4717-5102"
},
{
"family_name": "Bao",
"given_name": "Tong",
"orcid": "0000-0002-5082-5049"
},
{
"family_name": "Galiullin",
"given_name": "Ilkham",
"orcid": "0000-0001-5778-2355"
},
{
"family_name": "Kurlander",
"given_name": "Jacob A.",
"orcid": "0009-0005-5452-0671"
},
{
"family_name": "Law",
"given_name": "Casey J.",
"orcid": "0000-0002-4119-9963",
"clpid": "Law-Casey-J"
},
{
"family_name": "Pelisoli",
"given_name": "Ingrid",
"orcid": "0000-0003-4615-6556"
},
{
"family_name": "Schreiber",
"given_name": "Matthias R.",
"orcid": "0000-0003-3903-8009"
},
{
"family_name": "Burdge",
"given_name": "Kevin",
"orcid": "0000-0002-7226-836X"
},
{
"family_name": "Caiazzo",
"given_name": "Ilaria",
"orcid": "0000-0002-4770-5388"
},
{
"family_name": "Roestel",
"given_name": "Jan van",
"orcid": "0000-0002-2626-2872"
},
{
"family_name": "Szkody",
"given_name": "Paula",
"orcid": "0000-0003-4373-7777"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Buckley",
"given_name": "David A. H.",
"orcid": "0000-0002-7004-9956"
},
{
"family_name": "Potter",
"given_name": "Stephen B.",
"orcid": "0000-0002-5956-2249"
},
{
"family_name": "Gaensicke",
"given_name": "Boris",
"orcid": "0000-0002-2761-3005"
},
{
"family_name": "Mori",
"given_name": "Kaya",
"orcid": "0000-0002-9709-5389"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Graham",
"given_name": "Matthew",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Rose",
"given_name": "Sam",
"orcid": "0000-0003-4725-4481",
"clpid": "Rose-Sam"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Ahumada",
"given_name": "Tom\u00e1s",
"orcid": "0000-0002-2184-6430",
"clpid": "Ahumada-Tom\u00e1s"
},
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya"
},
{
"family_name": "Viitanen",
"given_name": "Akke",
"orcid": "0000-0001-9383-786X"
},
{
"family_name": "Wold",
"given_name": "Avery",
"orcid": "0000-0002-9998-6732",
"clpid": "Wold-Avery"
},
{
"family_name": "Chen",
"given_name": "Tracy X.",
"orcid": "0000-0001-9152-6224",
"clpid": "Chen-Tracy-X"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed"
},
{
"family_name": "Smith",
"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
}
],
"abstract": "White dwarfs (WDs) are the most abundant compact objects, and recent surveys have suggested that over a third of WDs in accreting binaries host a strong (B \u2273 1 MG) magnetic field. However, the origin and evolution of WD magnetism remain under debate. Two WD pulsars, AR Sco and J191213.72–441045.1 (J1912), have been found, which are non-accreting binaries hosting rapidly spinning (1.97 minutes and 5.30 minutes, respectively) magnetic WDs. The WD in AR Sco is slowing down on a P/P\u02d9≈5.6×10\u2076 yr timescale. It is believed they will eventually become polars, accreting systems in which a magnetic WD (B ≈ 10−240 MG) accretes from a Roche lobe-filling donor spinning in sync with the orbit (\u227378 minutes). Here, we present multiwavelength data and analysis of Gaia22ayj, which outbursted in 2022 March. We find that Gaia22ayj is a magnetic accreting WD that is rapidly spinning down (P/P\u02d9=6.1_(−0.2)^(+0.3)×10\u2076 yr) like WD pulsars, but shows clear evidence of accretion, like polars. Strong linear polarization (40%) is detected in Gaia22ayj; such high levels have only been seen in the WD pulsar AR Sco and demonstrate the WD is magnetic. High speed photometry reveals a 9.36 minutes period accompanying a high amplitude (∼2 mag) modulation. We associate this with a WD spin or spin–orbit beat period, not an orbital period as was previously suggested. Fast (60 s) optical spectroscopy reveals a broad \"hump,\" reminiscent of cyclotron emission in polars, between 4000 and 8000 Å. We find an X-ray luminosity of L_X=2.7_(−0.8)^(+6.2)×10³²ergs\u207b¹ in the 0.3–8 keV energy range, while two very large array radio campaigns resulted in a non-detection with a Fr < 15.8 μJy 3σ upper limit. The shared properties of both WD pulsars and polars suggest that Gaia22ayj is a missing link between the two classes of magnetic WD binaries.
",
"doi": "10.1088/1538-3873/adb0f1",
"issn": "0004-6280",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2025-02",
"series_number": "2",
"volume": "137",
"issue": "2",
"pages": "024202"
},
{
"id": "authors:xagym-va411",
"collection": "authors",
"collection_id": "xagym-va411",
"cite_using_url": "https://authors.library.caltech.edu/records/xagym-va411",
"type": "article",
"title": "Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri",
"author": [
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509"
},
{
"family_name": "Guolo",
"given_name": "Muryel",
"orcid": "0000-0002-5063-0751"
},
{
"family_name": "Tombesi",
"given_name": "Francesco",
"orcid": "0000-0002-6562-8654"
},
{
"family_name": "Li",
"given_name": "Ruancun",
"orcid": "0000-0001-8496-4162"
},
{
"family_name": "Gezari",
"given_name": "Suvi",
"orcid": "0000-0003-3703-5154"
},
{
"family_name": "Garc\u00eda",
"given_name": "Javier A.",
"orcid": "0000-0003-3828-2448",
"clpid": "Garc\u00eda-Javier-A"
},
{
"family_name": "Dai",
"given_name": "Lixin",
"orcid": "0000-0002-9589-5235"
},
{
"family_name": "Chornock",
"given_name": "Ryan",
"orcid": "0000-0002-7706-5668"
},
{
"family_name": "Lu",
"given_name": "Wenbin",
"orcid": "0000-0002-1568-7461"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Gendreau",
"given_name": "Keith C.",
"orcid": "0000-0001-7115-2819"
},
{
"family_name": "Pasham",
"given_name": "Dheeraj R.",
"orcid": "0000-0003-1386-7861"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "Kara",
"given_name": "Erin",
"orcid": "0000-0003-0172-0854"
},
{
"family_name": "Margutti",
"given_name": "Raffaella",
"orcid": "0000-0003-4768-7586"
},
{
"family_name": "Ajay",
"given_name": "Yukta",
"orcid": "0009-0007-8764-9062"
},
{
"family_name": "Wevers",
"given_name": "Thomas",
"orcid": "0000-0002-4043-9400"
},
{
"family_name": "Kwan",
"given_name": "Tom M.",
"orcid": "0000-0003-0509-2541"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498"
},
{
"family_name": "Bloom",
"given_name": "Joshua S.",
"orcid": "0000-0002-7777-216X"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"orcid": "0000-0003-0228-6594",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Hammerstein",
"given_name": "Erica",
"orcid": "0000-0002-5698-8703"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-R-R"
},
{
"family_name": "LeBaron",
"given_name": "Natalie",
"orcid": "0000-0002-2249-0595"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "O'Connor",
"given_name": "Brendan",
"orcid": "0000-0002-9700-0036"
},
{
"family_name": "Purdum",
"given_name": "Josiah",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah"
},
{
"family_name": "Ravi",
"given_name": "Vikram",
"orcid": "0000-0002-7252-5485",
"clpid": "Ravi-Vikram"
},
{
"family_name": "Sears",
"given_name": "Huei",
"orcid": "0000-0001-8023-4912"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Smith",
"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Somalwar",
"given_name": "Jean J.",
"orcid": "0000-0001-8426-5732",
"clpid": "Somalwar-Jean-J"
},
{
"family_name": "Wold",
"given_name": "Avery",
"orcid": "0000-0002-9998-6732",
"clpid": "Wold-Avery"
}
],
"abstract": "\n
We present the tidal disruption event (TDE) AT2022lri, hosted in a nearby (≈144 Mpc) quiescent galaxy with a low-mass massive black hole (104M\u2299 < MBH < 106M\u2299). AT2022lri belongs to the TDE-H+He subtype. More than 1 Ms of X-ray data were collected with NICER, Swift, and XMM-Newton from 187 to 672 days after peak. The X-ray luminosity gradually declined from 1.5 × 1044 erg s−1 to 1.5 × 1043 erg s−1 and remains much above the UV and optical luminosity, consistent with a super-Eddington accretion flow viewed face-on. Sporadic strong X-ray dips atop a long-term decline are observed, with a variability timescale of ≈0.5 hr–1 days and amplitude of ≈2–8. When fitted with simple continuum models, the X-ray spectrum is dominated by a thermal disk component with inner temperature going from ∼146 to ∼86 eV. However, there are residual features that peak around 1 keV, which, in some cases, cannot be reproduced by a single broad emission line. We analyzed a subset of time-resolved spectra with two physically motivated models describing a scenario either where ionized absorbers contribute extra absorption and emission lines or where disk reflection plays an important role. Both models provide good and statistically comparable fits, show that the X-ray dips are correlated with drops in the inner disk temperature, and require the existence of subrelativistic (0.1–0.3c) ionized outflows. We propose that the disk temperature fluctuation stems from episodic drops of the mass accretion rate triggered by magnetic instabilities or/and wobbling of the inner accretion disk along the black hole's spin axis.
\n
\n
Eruptive mass loss of massive stars prior to supernova (SN) explosion is key to understanding their evolution and end fate. An observational signature of pre-SN mass loss is the detection of an early, short-lived peak prior to the radioactive-powered peak in the lightcurve of the SN. This is usually attributed to the SN shock passing through an extended envelope or circumstellar medium. Such an early peak is common for double-peaked Type IIb SNe with an extended hydrogen envelope but uncommon for normal Type Ibc SNe with very compact progenitors. In this paper, we systematically study a sample of 14 double-peaked Type Ibc SNe out of 475 Type Ibc SNe detected by the Zwicky Transient Facility. The rate of these events is ∼3%–9% of Type Ibc SNe. A strong correlation is seen between the peak brightness of the first and the second peak. We perform a holistic analysis of this sample’s photometric and spectroscopic properties. We find that six SNe have ejecta mass less than 1.5 M\u2299. Based on the nebular spectra and lightcurve properties, we estimate that the progenitor masses for these are less than ∼12 M\u2299. The rest have an ejecta mass >2.4 M\u2299 and a higher progenitor mass. This sample suggests that the SNe with low progenitor masses undergo late-time binary mass transfer. Meanwhile, the SNe with higher progenitor masses are consistent with wave-driven mass loss or pulsation-pair instability-driven mass-loss simulations.
\n
\n
Multipeaked supernovae with precursors, dramatic light-curve rebrightenings, and spectral transformation are rare, but are being discovered in increasing numbers by modern night-sky transient surveys like the Zwicky Transient Facility. Here, we present the observations and analysis of SN 2023aew, which showed a dramatic increase in brightness following an initial luminous (−17.4 mag) and long (∼100 days) unusual first peak (possibly precursor). SN 2023aew was classified as a Type IIb supernova during the first peak but changed its type to resemble a stripped-envelope supernova (SESN) after the marked rebrightening. We present comparisons of SN 2023aew's spectral evolution with SESN subtypes and argue that it is similar to SNe Ibc during its main peak. P-Cygni Balmer lines are present during the first peak, but vanish during the second peak's photospheric phase, before Hα resurfaces again during the nebular phase. The nebular lines ([O i], [Ca ii], Mg i], Hα) exhibit a double-peaked structure that hints toward a clumpy or nonspherical ejecta. We analyze the second peak in the light curve of SN 2023aew and find it to be broader than that of normal SESNe as well as requiring a very high 56Ni mass to power the peak luminosity. We discuss the possible origins of SN 2023aew including an eruption scenario where a part of the envelope is ejected during the first peak and also powers the second peak of the light curve through interaction of the SN with the circumstellar medium.
\n
The origin of cosmic high-energy neutrinos remains largely unexplained. For high-energy neutrino alerts from IceCube, a coincidence with time-variable emission has been seen for three different types of accreting black holes: (1) a gamma-ray flare from a blazar (TXS 0506+056), (2) an optical transient following a stellar tidal disruption event (TDE; AT2019dsg), and (3) an optical outburst from an active galactic nucleus (AGN; AT2019fdr). For the latter two sources, infrared follow-up observations revealed a powerful reverberation signal due to dust heated by the flare. This discovery motivates a systematic study of neutrino emission from all supermassive black hole with similar dust echoes. Because dust reprocessing is agnostic to the origin of the outburst, our work unifies TDEs and high-amplitude flares from AGN into a population that we dub accretion flares. Besides the two known events, we uncover a third flare that is coincident with a PeV-scale neutrino (AT2019aalc). Based solely on the optical and infrared properties, we estimate a significance of 3.6σ for this association of high-energy neutrinos with three accretion flares. Our results imply that at least ∼10 per cent of the IceCube high-energy neutrino alerts could be due to accretion flares. This is surprising because the sum of the fluence of these flares is at least three orders of magnitude lower compared to the total fluence of normal AGN. It thus appears that the efficiency of high-energy neutrino production in accretion flares is increased compared to non-flaring AGN. We speculate that this can be explained by the high Eddington ratio of the flares.
",
"doi": "10.1093/mnras/stae610",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2024-04",
"series_number": "3",
"volume": "529",
"issue": "3",
"pages": "2559-2576"
},
{
"id": "authors:n23nm-f6g05",
"collection": "authors",
"collection_id": "n23nm-f6g05",
"cite_using_url": "https://authors.library.caltech.edu/records/n23nm-f6g05",
"type": "article",
"title": "Photometric prioritization of neutron star merger candidates",
"author": [
{
"family_name": "Ofek",
"given_name": "Eran O",
"orcid": "0000-0002-6786-8774"
},
{
"family_name": "Strotjohann",
"given_name": "Nora L",
"orcid": "0000-0002-4667-6730"
},
{
"family_name": "Arcavi",
"given_name": "Iair",
"orcid": "0000-0001-7090-4898"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Kushnir",
"given_name": "Doron"
},
{
"family_name": "Waxman",
"given_name": "Eli",
"orcid": "0000-0002-9038-5877"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Drake",
"given_name": "Andrew",
"orcid": "0000-0003-0228-6594",
"clpid": "Drake-Andrew"
},
{
"family_name": "Graham",
"given_name": "Matthew",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Purdum",
"given_name": "Josiah",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah-N"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Smith",
"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
},
{
"family_name": "Wold",
"given_name": "Avery",
"orcid": "0000-0002-9998-6732",
"clpid": "Wold-Avery"
},
{
"family_name": "Healy",
"given_name": "Brian F",
"orcid": "0000-0002-7718-7884"
}
],
"abstract": "Rapid identification of the optical counterparts of neutron star (NS) merger events discovered by gravitational wave detectors may require observing a large error region and sifting through a large number of transients to identify the object of interest. Given the expense of spectroscopic observations, a question arises: How can we utilize photometric observations for candidate prioritization, and what kinds of photometric observations are needed to achieve this goal? NS merger kilonova exhibits low ejecta mass (∼5 × 10\u207b² M\u2299) and a rapidly evolving photospheric radius (with a velocity ∼0.2c). As a consequence, these sources display rapid optical-flux evolution. Indeed, selection based on fast flux variations is commonly used for young supernovae and NS mergers. In this study, we leverage the best currently available flux-limited transient survey – the Zwicky Transient Facility Bright Transient Survey – to extend and quantify this approach. We focus on selecting transients detected in a 3-day cadence survey and observed at a one-day cadence. We explore their distribution in the phase space defined by g–r, $\\dot{g}$, and $\\dot{r}$. Our analysis demonstrates that for a significant portion of the time during the first week, the kilonova AT 2017gfo stands out in this phase space. It is important to note that this investigation is subject to various biases and challenges; nevertheless, it suggests that certain photometric observations can be leveraged to identify transients with the highest probability of being fast-evolving events. We also find that a large fraction (≈75 per cent) of the transient candidates with $\\vert\\dot{g}\\vert>0.7$ mag d−1, are cataclysmic variables or active galactic nuclei with radio counterparts.
",
"doi": "10.1093/mnras/stad3380",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2024-01",
"series_number": "2",
"volume": "527",
"issue": "2",
"pages": "3741-3748"
},
{
"id": "authors:5myt5-cns50",
"collection": "authors",
"collection_id": "5myt5-cns50",
"cite_using_url": "https://authors.library.caltech.edu/records/5myt5-cns50",
"type": "article",
"title": "Long-rising Type II Supernovae in the Zwicky Transient Facility Census of the Local Universe",
"author": [
{
"family_name": "Sit",
"given_name": "Tawny",
"orcid": "0000-0001-8208-9755",
"clpid": "Sit-Tawny"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Adams",
"given_name": "Scott",
"orcid": "0000-0001-5855-5939",
"clpid": "Adams-Scott"
},
{
"family_name": "Aloisi",
"given_name": "Robert",
"orcid": "0000-0003-2822-616X"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498"
},
{
"family_name": "Chu",
"given_name": "Matthew",
"orcid": "0000-0001-5884-911X",
"clpid": "Chu-Matthew"
},
{
"family_name": "Cook",
"given_name": "David",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David"
},
{
"family_name": "Das",
"given_name": "Kaustav Kashyap",
"orcid": "0000-0001-8372-997X",
"clpid": "Das-Kaustav-Kashyap"
},
{
"family_name": "Dugas",
"given_name": "Alison"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-James-D"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Medford",
"given_name": "Michael S.",
"orcid": "0000-0002-7226-0659"
},
{
"family_name": "Purdum",
"given_name": "Josiah",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Smith",
"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
},
{
"family_name": "Stein",
"given_name": "Robert",
"orcid": "0000-0003-2434-0387",
"clpid": "Stein-Robert"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Zhang",
"given_name": "Chaoran",
"orcid": "0000-0002-0331-6727"
}
],
"abstract": "\n
SN 1987A was an unusual hydrogen-rich core-collapse supernova originating from a blue supergiant star. Similar blue supergiant explosions remain a small family of events, and are broadly characterized by their long rises to peak. The Zwicky Transient Facility Census of the Local Universe (CLU) experiment aims to construct a spectroscopically complete sample of transients occurring in galaxies from the CLU galaxy catalog. We identify 13 long-rising (>40 days) Type II supernovae from the volume-limited CLU experiment during a 3.5 yr period from 2018 June to 2021 December, approximately doubling the previously known number of these events. We present photometric and spectroscopic data of these 13 events, finding peak r-band absolute magnitudes ranging from −15.6 to −17.5 mag and the tentative detection of Ba ii lines in nine events. Using our CLU sample of events, we derive a long-rising Type II supernova rate of 1.37_(−0.30)^(+0.26) × 10\u207b\u2076 Mpc−3 yr−1, ≈1.4% of the total core-collapse supernova rate. This is the first volumetric rate of these events estimated from a large, systematic, volume-limited experiment.
\n
The fate of stars in the zero-age main-sequence (ZAMS) range \u22488\u201312 M_\u2299 is unclear. They could evolve to form white dwarfs or explode as electron-capture supernovae (SNe) or iron core-collapse SNe (CCSNe). Even though the initial mass function indicates that this mass range should account for over 40% of all CCSN progenitors, few have been observationally confirmed, likely due to the faintness and rapid evolution of some of these transients. In this paper, we present a sample of nine Ca-rich/O-poor Type IIb SNe detected by the Zwicky Transient Facility with progenitors likely in this mass range. These sources have a [Ca ii] \u03bb \u03bb7291, 7324/[O i] \u03bb \u03bb6300, 6364 flux ratio of \u22732 in their nebular spectra. Comparing the measured [O i] luminosity (\u227210\u00b3\u2079 erg s\u207b\u00b9) and derived oxygen mass (\u22480.01 M_\u2299) with theoretical models, we infer that the progenitor ZAMS mass for these explosions is less than 12 M _\u2299. The ejecta properties (M_(ej) \u2272 1 M_\u2299 and E_(kin) \u223c 10\u2075\u2070 erg) are also consistent. The low ejecta mass of these sources indicates a class of strongly-stripped SNe that is a transition between the regular stripped-envelope SNe and ultra-stripped SNe. The progenitor could be stripped by a main-sequence companion and result in the formation of a neutron star\u2212main sequence binary. Such binaries have been suggested to be progenitors of neutron star\u2212white dwarf systems that could merge within a Hubble time and be detectable with LISA.
",
"doi": "10.3847/1538-4357/acfeeb",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2023-12-10",
"series_number": "1",
"volume": "959",
"issue": "1",
"pages": "12"
},
{
"id": "authors:c7fsp-s7g30",
"collection": "authors",
"collection_id": "c7fsp-s7g30",
"cite_using_url": "https://authors.library.caltech.edu/records/c7fsp-s7g30",
"type": "article",
"title": "Minutes-duration optical flares with supernova luminosities",
"author": [
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Chen",
"given_name": "Ping",
"orcid": "0000-0003-0853-6427"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Dhillon",
"given_name": "Vik",
"orcid": "0000-0003-4236-9642"
},
{
"family_name": "Kumar",
"given_name": "Harsh",
"orcid": "0000-0003-0871-4641"
},
{
"family_name": "Suresh",
"given_name": "Aswin",
"orcid": "0009-0005-8230-030X"
},
{
"family_name": "Swain",
"given_name": "Vishwajeet",
"orcid": "0000-0002-7942-8477"
},
{
"family_name": "Bremer",
"given_name": "Michael",
"orcid": "0000-0001-7511-3745"
},
{
"family_name": "Smartt",
"given_name": "Stephen J.",
"orcid": "0000-0002-8229-1731"
},
{
"family_name": "Anderson",
"given_name": "Joseph P.",
"orcid": "0000-0003-0227-3451"
},
{
"family_name": "Anupama",
"given_name": "G. C.",
"orcid": "0000-0003-3533-7183"
},
{
"family_name": "Awiphan",
"given_name": "Supachai",
"orcid": "0000-0003-3251-3583"
},
{
"family_name": "Barway",
"given_name": "Sudhanshu",
"orcid": "0000-0002-3927-5402"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Ben-Ami",
"given_name": "Sagi",
"orcid": "0000-0001-6760-3074"
},
{
"family_name": "Bhalerao",
"given_name": "Varun",
"orcid": "0000-0002-6112-7609"
},
{
"family_name": "de Boer",
"given_name": "Thomas",
"orcid": "0000-0001-5486-2747"
},
{
"family_name": "Brink",
"given_name": "Thomas G.",
"orcid": "0000-0001-5955-2502"
},
{
"family_name": "Burruss",
"given_name": "Rick",
"clpid": "Burruss-Rick-S"
},
{
"family_name": "Chandra",
"given_name": "Poonam",
"orcid": "0000-0002-0844-6563"
},
{
"family_name": "Chen",
"given_name": "Ting-Wan",
"orcid": "0000-0002-1066-6098"
},
{
"family_name": "Chen",
"given_name": "Wen-Ping",
"orcid": "0000-0003-0262-272X"
},
{
"family_name": "Cooke",
"given_name": "Jeff",
"orcid": "0000-0001-5703-2108"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924"
},
{
"family_name": "Das",
"given_name": "Kaustav K.",
"clpid": "Das-Kaustav-K"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"orcid": "0000-0003-0228-6594",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Filippenko",
"given_name": "Alexei V.",
"orcid": "0000-0003-3460-0103"
},
{
"family_name": "Freeburn",
"given_name": "James",
"orcid": "0009-0006-7990-0547"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Fulton",
"given_name": "Michael D.",
"orcid": "0000-0003-1916-0664"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Galbany",
"given_name": "Llu\u00eds",
"orcid": "0000-0002-1296-6887"
},
{
"family_name": "Gao",
"given_name": "Hua",
"orcid": "0000-0003-1015-5367"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Gromadzki",
"given_name": "Mariusz",
"orcid": "0000-0002-1650-1518"
},
{
"family_name": "Guti\u00e9rrez",
"given_name": "Claudia P.",
"orcid": "0000-0003-2375-2064"
},
{
"family_name": "Hinds",
"given_name": "K.-Ryan",
"orcid": "0000-0002-0129-806X"
},
{
"family_name": "Inserra",
"given_name": "Cosimo",
"orcid": "0000-0002-3968-4409"
},
{
"family_name": "AJ",
"given_name": "Nayana",
"orcid": "0000-0002-8070-5400"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kulkarni",
"given_name": "Shri",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "M\u00fcller-Bravo",
"given_name": "Tom\u00e1s E.",
"orcid": "0000-0003-3939-7167"
},
{
"family_name": "Magnier",
"given_name": "Eugene A.",
"orcid": "0000-0002-7965-2815"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Moore",
"given_name": "Thomas",
"orcid": "0000-0001-8385-3727"
},
{
"family_name": "Ngeow",
"given_name": "Chow-Choong",
"orcid": "0000-0001-8771-7554"
},
{
"family_name": "Nicholl",
"given_name": "Matt",
"orcid": "0000-0002-2555-3192"
},
{
"family_name": "Ofek",
"given_name": "Eran O.",
"orcid": "0000-0002-6786-8774"
},
{
"family_name": "Omand",
"given_name": "Conor M. B.",
"orcid": "0000-0002-9646-8710"
},
{
"family_name": "Onori",
"given_name": "Francesca",
"orcid": "0000-0001-6286-1744"
},
{
"family_name": "Pan",
"given_name": "Yen-Chen",
"orcid": "0000-0001-8415-6720"
},
{
"family_name": "Pessi",
"given_name": "Priscila J.",
"orcid": "0000-0002-8041-8559"
},
{
"family_name": "Petitpas",
"given_name": "Glen"
},
{
"family_name": "Polishook",
"given_name": "David",
"orcid": "0000-0002-6977-3146"
},
{
"family_name": "Poshyachinda",
"given_name": "Saran"
},
{
"family_name": "Pursiainen",
"given_name": "Miika",
"orcid": "0000-0003-4663-4300"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed"
},
{
"family_name": "Rodriguez",
"given_name": "Antonio C.",
"orcid": "0000-0003-4189-9668",
"clpid": "Rodriguez-Antonio-C"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin-A"
},
{
"family_name": "Segre",
"given_name": "Enrico",
"orcid": "0000-0002-0913-3083"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Smith",
"given_name": "Ken W.",
"orcid": "0000-0001-9535-3199"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Srivastav",
"given_name": "Shubham",
"orcid": "0000-0003-4524-6883"
},
{
"family_name": "Strotjohann",
"given_name": "Nora Linn",
"orcid": "0000-0002-4667-6730"
},
{
"family_name": "Suhr",
"given_name": "Mark"
},
{
"family_name": "Svinkin",
"given_name": "Dmitry",
"orcid": "0000-0002-2208-2196"
},
{
"family_name": "Wang",
"given_name": "Yanan",
"orcid": "0000-0003-3207-5237"
},
{
"family_name": "Wiseman",
"given_name": "Philip",
"orcid": "0000-0002-3073-1512"
},
{
"family_name": "Wold",
"given_name": "Avery",
"orcid": "0000-0002-9998-6732",
"clpid": "Wold-Avery"
},
{
"family_name": "Yang",
"given_name": "Sheng",
"orcid": "0000-0002-2898-6532"
},
{
"family_name": "Yang",
"given_name": "Yi",
"orcid": "0000-0002-6535-8500"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Young",
"given_name": "David R.",
"orcid": "0000-0002-1229-2499"
},
{
"family_name": "Zheng",
"given_name": "WeiKang",
"orcid": "0000-0002-2636-6508"
}
],
"abstract": "In recent years, certain luminous extragalactic optical transients have been observed to last only a few days1. Their short observed duration implies a different powering mechanism from the most common luminous extragalactic transients (supernovae), whose timescale is weeks2. Some short-duration transients, most notably AT2018cow (ref.\u20093), show blue optical colours and bright radio and X-ray emission4. Several AT2018cow-like transients have shown hints of a long-lived embedded energy source5, such as X-ray variability6,7, prolonged ultraviolet emission8, a tentative X-ray quasiperiodic oscillation9,10 and large energies coupled to fast (but subrelativistic) radio-emitting ejecta11,12. Here we report observations of minutes-duration optical flares in the aftermath of an AT2018cow-like transient, AT2022tsd (the 'Tasmanian Devil'). The flares occur over a period of months, are highly energetic and are probably nonthermal, implying that they arise from a near-relativistic outflow or jet. Our observations confirm that, in some AT2018cow-like transients, the embedded energy source is a compact object, either a magnetar or an accreting black hole.
",
"doi": "10.1038/s41586-023-06673-6",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "2023-11-30",
"series_number": "7879",
"volume": "623",
"issue": "7879",
"pages": "927-931"
},
{
"id": "authors:5991k-6w460",
"collection": "authors",
"collection_id": "5991k-6w460",
"cite_using_url": "https://authors.library.caltech.edu/records/5991k-6w460",
"type": "article",
"title": "The broad-lined Type-Ic supernova SN 2022xxf and its extraordinary two-humped light curves. I. Signatures of H/He-free interaction in the first four months",
"author": [
{
"family_name": "Kuncarayakti",
"given_name": "H.",
"orcid": "0000-0002-1132-1366",
"clpid": "Kuncarayakti-Hanindyo"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Izzo",
"given_name": "L.",
"orcid": "0000-0001-9695-8472"
},
{
"family_name": "Maeda",
"given_name": "K.",
"orcid": "0000-0003-2611-7269"
},
{
"family_name": "Yang",
"given_name": "S."
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Angus",
"given_name": "C. R.",
"orcid": "0000-0002-4269-7999"
},
{
"family_name": "Aubert",
"given_name": "M."
},
{
"family_name": "Auchettl",
"given_name": "K.",
"orcid": "0000-0002-4449-9152"
},
{
"family_name": "Della Valle",
"given_name": "M.",
"orcid": "0000-0003-3142-5020"
},
{
"family_name": "Dessart",
"given_name": "L.",
"orcid": "0000-0003-0599-8407"
},
{
"family_name": "Hinds",
"given_name": "K.",
"orcid": "0000-0002-0129-806X"
},
{
"family_name": "Kankare",
"given_name": "E.",
"orcid": "0000-0001-8257-3512"
},
{
"family_name": "Kawabata",
"given_name": "M."
},
{
"family_name": "Lundqvist",
"given_name": "P."
},
{
"family_name": "Nakaoka",
"given_name": "T."
},
{
"family_name": "Perley",
"given_name": "D.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Raimundo",
"given_name": "S. I.",
"orcid": "0000-0002-6248-398X"
},
{
"family_name": "Strotjohann",
"given_name": "N. L.",
"orcid": "0000-0002-4667-6730"
},
{
"family_name": "Taguchi",
"given_name": "K."
},
{
"family_name": "Cai",
"given_name": "Y.-Z."
},
{
"family_name": "Charalampopoulos",
"given_name": "P."
},
{
"family_name": "Fang",
"given_name": "Q."
},
{
"family_name": "Fraser",
"given_name": "M."
},
{
"family_name": "Guti\u00e9rrez",
"given_name": "C. P."
},
{
"family_name": "Imazawa",
"given_name": "R."
},
{
"family_name": "Kangas",
"given_name": "T."
},
{
"family_name": "Kawabata",
"given_name": "K. S."
},
{
"family_name": "Kotak",
"given_name": "R."
},
{
"family_name": "Kravtsov",
"given_name": "T."
},
{
"family_name": "Matilainen",
"given_name": "K."
},
{
"family_name": "Mattila",
"given_name": "S."
},
{
"family_name": "Moran",
"given_name": "S."
},
{
"family_name": "Murata",
"given_name": "I."
},
{
"family_name": "Salmaso",
"given_name": "I."
},
{
"family_name": "Anderson",
"given_name": "J. P."
},
{
"family_name": "Ashall",
"given_name": "C."
},
{
"family_name": "Bellm",
"given_name": "E. C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Benetti",
"given_name": "S."
},
{
"family_name": "Chambers",
"given_name": "K. C."
},
{
"family_name": "Chen",
"given_name": "T.-W."
},
{
"family_name": "Coughlin",
"given_name": "M."
},
{
"family_name": "De Colle",
"given_name": "F."
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Galbany",
"given_name": "L."
},
{
"family_name": "Gal-Yam",
"given_name": "A.",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Gromadzki",
"given_name": "M."
},
{
"family_name": "Groom",
"given_name": "S. L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Hajela",
"given_name": "A."
},
{
"family_name": "Inserra",
"given_name": "C."
},
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Mahabal",
"given_name": "A. A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Martin-Carrillo",
"given_name": "A."
},
{
"family_name": "Moore",
"given_name": "T."
},
{
"family_name": "M\u00fcller-Bravo",
"given_name": "T. E."
},
{
"family_name": "Nicholl",
"given_name": "M."
},
{
"family_name": "Ragosta",
"given_name": "F."
},
{
"family_name": "Riddle",
"given_name": "R. L.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Sharma",
"given_name": "Y.",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Srivastav",
"given_name": "S."
},
{
"family_name": "Stritzinger",
"given_name": "M. D."
},
{
"family_name": "Wold",
"given_name": "A.",
"orcid": "0000-0002-9998-6732",
"clpid": "Wold-Avery-A"
},
{
"family_name": "Young",
"given_name": "D. R."
}
],
"abstract": "We report on our study of the supernova (SN) 2022xxf based on observations obtained during the first four months of its evolution. The light curves (LCs) display two humps of similar maximum brightness separated by 75 days, unprecedented for a broad-lined (BL) Type Ic supernova (SN IcBL). SN 2022xxf is the most nearby SN IcBL to date (in NGC 3705, z = 0.0037, at a distance of about 20 Mpc). Optical and near-infrared photometry and spectroscopy were used to identify the energy source powering the LC. Nearly 50 epochs of high signal-to-noise ratio spectroscopy were obtained within 130 days, comprising an unparalleled dataset for a SN IcBL, and one of the best-sampled SN datasets to date. The global spectral appearance and evolution of SN 2022xxf points to typical SN Ic/IcBL, with broad features (up to ~14 000 km s−1) and a gradual transition from the photospheric to the nebular phase. However, narrow emission lines (corresponding to ~ 1000–2500 km s−1) are present in the spectra from the time of the second rise, suggesting slower-moving circumstellar material (CSM). These lines are subtle, in comparison to the typical strong narrow lines of CSM-interacting SNe, for example, Type IIn, Ibn, and Icn, but some are readily noticeable at late times, such as in Mg I λ5170 and [O I] λ5577. Unusually, the near-infrared spectra show narrow line peaks in a number of features formed by ions of O and Mg. We infer the presence of CSM that is free of H and He. We propose that the radiative energy from the ejecta-CSM interaction is a plausible explanation for the second LC hump. This interaction scenario is supported by the color evolution, which progresses to blue as the light curve evolves along the second hump, and by the slow second rise and subsequent rapid LC drop. SN 2022xxf may be related to an emerging number of CSM-interacting SNe Ic, which show slow, peculiar LCs, blue colors, and subtle CSM interaction lines. The progenitor stars of these SNe likely experienced an episode of mass loss consisting of H/He-free material shortly prior to explosion.
",
"doi": "10.1051/0004-6361/202346526",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy & Astrophysics",
"publication_date": "2023-10",
"volume": "678",
"pages": "A209"
},
{
"id": "authors:p4rnh-xvp61",
"collection": "authors",
"collection_id": "p4rnh-xvp61",
"cite_using_url": "https://authors.library.caltech.edu/records/p4rnh-xvp61",
"type": "article",
"title": "SN 2020udy: an SN Iax with strict limits on interaction consistent with a helium-star companion",
"author": [
{
"family_name": "Maguire",
"given_name": "Kate",
"orcid": "0000-0002-9770-3508"
},
{
"family_name": "Magee",
"given_name": "Mark R",
"orcid": "0000-0002-0629-8931"
},
{
"family_name": "Leloudas",
"given_name": "Giorgos",
"orcid": "0000-0002-8597-0756"
},
{
"family_name": "Miller",
"given_name": "Adam A",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Dimitriadis",
"given_name": "Georgios",
"orcid": "0000-0001-9494-179X"
},
{
"family_name": "Pursiainen",
"given_name": "Miika",
"orcid": "0000-0003-4663-4300"
},
{
"family_name": "Bulla",
"given_name": "Mattia",
"orcid": "0000-0002-8255-5127"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Perley",
"given_name": "Daniel A",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj R",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj-R"
},
{
"family_name": "Nordin",
"given_name": "Jakob"
},
{
"family_name": "Reusch",
"given_name": "Simeon",
"orcid": "0000-0002-7788-628X"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Terreran",
"given_name": "Giacomo",
"orcid": "0000-0003-0794-5982"
},
{
"family_name": "Yang(\u6768\u8f76)",
"given_name": "Yi",
"orcid": "0000-0002-6535-8500"
},
{
"family_name": "Bellm",
"given_name": "Eric C",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Groom",
"given_name": "Steven L",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Lacroix",
"given_name": "Leander",
"orcid": "0000-0003-0629-5746"
},
{
"family_name": "Masci",
"given_name": "Frank J",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Purdum",
"given_name": "Josiah N",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah-N"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Smith",
"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
}
],
"abstract": "Early observations of transient explosions can provide vital clues to their progenitor origins. In this paper, we present the nearby Type Iax (02cx-like) supernova (SN), SN 2020udy, that was discovered within hours (∼7 h) of estimated first light. An extensive data set of ultra-violet, optical, and near-infrared observations was obtained, covering out to ∼150 d after explosion. SN 2020udy peaked at −17.86 ± 0.43 mag in the r band and evolved similarly to other ‘luminous’ SNe Iax, such as SNe 2005hk and 2012Z. Its well-sampled early light curve allows strict limits on companion interaction to be placed. Main-sequence companion stars with masses of 2 and 6 M\u2299 are ruled out at all viewing angles, while a helium-star companion is allowed from a narrow range of angles (140–180° away from the companion). The spectra and light curves of SN 2020udy are in good agreement with those of the ‘N5def’ deflagration model of a near Chandrasekhar-mass carbon–oxygen white dwarf. However, as has been seen in previous studies of similar luminosity events, SN 2020udy evolves slower than the model. Broad-band linear polarization measurements taken at and after peak are consistent with no polarization, in agreement with the predictions of the companion-star configuration from the early light-curve measurements. The host galaxy environment is low metallicity and is consistent with a young stellar population. Overall, we find the most plausible explosion scenario to be the incomplete disruption of a CO white dwarf near the Chandrasekhar-mass limit, with a helium-star companion.
",
"doi": "10.1093/mnras/stad2316",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2023-10",
"series_number": "1",
"volume": "525",
"issue": "1",
"pages": "1210-1228"
},
{
"id": "authors:hbgpj-4f191",
"collection": "authors",
"collection_id": "hbgpj-4f191",
"cite_using_url": "https://authors.library.caltech.edu/records/hbgpj-4f191",
"type": "article",
"title": "Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function",
"author": [
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Ravi",
"given_name": "Vikram",
"orcid": "0000-0002-7252-5485",
"clpid": "Ravi-Vikram"
},
{
"family_name": "Gezari",
"given_name": "Suvi",
"orcid": "0000-0003-3703-5154"
},
{
"family_name": "van Velzen",
"given_name": "Sjoert",
"orcid": "0000-0002-3859-8074"
},
{
"family_name": "Lu",
"given_name": "Wenbin",
"orcid": "0000-0002-1568-7461"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Somalwar",
"given_name": "Jean J.",
"orcid": "0000-0001-8426-5732",
"clpid": "Somalwar-Jean-J"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Hammerstein",
"given_name": "Erica",
"orcid": "0000-0002-5698-8703"
},
{
"family_name": "Nicholl",
"given_name": "Matt",
"orcid": "0000-0002-2555-3192"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "Stein",
"given_name": "Robert",
"orcid": "0000-0003-2434-0387",
"clpid": "Stein-Robert"
},
{
"family_name": "Ricarte",
"given_name": "Angelo",
"orcid": "0000-0001-5287-0452"
},
{
"family_name": "Chadayammuri",
"given_name": "Urmila"
},
{
"family_name": "Quataert",
"given_name": "Eliot",
"orcid": "0000-0001-9185-5044"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Bloom",
"given_name": "Joshua S.",
"orcid": "0000-0002-7777-216X"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"orcid": "0000-0003-0228-6594",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Ben"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "We conduct a systematic tidal disruption event (TDE) demographics analysis using the largest sample of optically selected TDEs. A flux-limited, spectroscopically complete sample of 33 TDEs is constructed using the Zwicky Transient Facility over 3 yr (from 2018 October to 2021 September). We infer the black hole (BH) mass (MBH) with host galaxy scaling relations, showing that the sample MBH ranges from 105.1M\u2299 to 108.2M\u2299. We developed a survey efficiency corrected maximum volume method to infer the rates. The rest-frame g-band luminosity function can be well described by a broken power law of \u03d5(Lg)∝[(Lg/Lbk)0.3+(Lg/Lbk)2.6]−1, with Lbk = 1043.1 erg s−1. In the BH mass regime of 105.3 \u2272 (MBH/M\u2299) \u2272 107.3, the TDE mass function follows \u03d5(MBH)∝MBH−0.25, which favors a flat local BH mass function (dnBH/dlogMBH≈constant). We confirm the significant rate suppression at the high-mass end (MBH \u2273 107.5M\u2299), which is consistent with theoretical predictions considering direct capture of hydrogen-burning stars by the event horizon. At a host galaxy mass of Mgal ∼ 1010M\u2299, the average optical TDE rate is ≈3.2 × 10−5 galaxy−1 yr−1. We constrain the optical TDE rate to be [3.7, 7.4, and 1.6] × 10−5 galaxy−1 yr−1 in galaxies with red, green, and blue colors.
",
"doi": "10.3847/2041-8213/acf216",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2023-09-20",
"series_number": "1",
"volume": "955",
"issue": "1",
"pages": "L6"
},
{
"id": "authors:czwg6-6wd41",
"collection": "authors",
"collection_id": "czwg6-6wd41",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230628-295386000.4",
"type": "article",
"title": "Uncovering a population of gravitational lens galaxies with magnified standard candle SN Zwicky",
"author": [
{
"family_name": "Goobar",
"given_name": "Ariel",
"orcid": "0000-0002-4163-4996",
"clpid": "Goobar-Ariel"
},
{
"family_name": "Johansson",
"given_name": "Joel",
"orcid": "0000-0001-5975-290X"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Arendse",
"given_name": "Nikki",
"orcid": "0000-0001-5409-6480"
},
{
"family_name": "Sagu\u00e9s Carracedo",
"given_name": "Ana",
"orcid": "0000-0002-3498-2167"
},
{
"family_name": "Dhawan",
"given_name": "Suhail",
"orcid": "0000-0002-2376-6979"
},
{
"family_name": "M\u00f6rtsell",
"given_name": "Edvard",
"orcid": "0000-0002-8380-6143"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Perley",
"given_name": "Daniel",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Joseph",
"given_name": "R\u00e9my",
"orcid": "0000-0002-2704-5028"
},
{
"family_name": "Hinds",
"given_name": "K-Ryan",
"orcid": "0000-0002-0129-806X"
},
{
"family_name": "Meynardie",
"given_name": "William",
"clpid": "Meynardie-William"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498"
},
{
"family_name": "Bellm",
"given_name": "Eric",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Bloom",
"given_name": "Josh",
"orcid": "0000-0002-7777-216X"
},
{
"family_name": "Collett",
"given_name": "Thomas E.",
"orcid": "0000-0001-5564-3140"
},
{
"family_name": "Drake",
"given_name": "Andrew",
"orcid": "0000-0003-0228-6594",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Graham",
"given_name": "Matthew",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kulkarni",
"given_name": "Shri R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Lemon",
"given_name": "Cameron",
"orcid": "0000-0003-2456-9317"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-James-D"
},
{
"family_name": "Nordin",
"given_name": "Jakob",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Pierel",
"given_name": "Justin",
"orcid": "0000-0002-2361-7201"
},
{
"family_name": "Richard",
"given_name": "Johan",
"orcid": "0000-0001-5492-1049",
"clpid": "Richard-Johan"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Rigault",
"given_name": "Mickael",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Stein",
"given_name": "Robert",
"orcid": "0000-0003-2434-0387",
"clpid": "Stein-Robert-D"
},
{
"family_name": "Stewart",
"given_name": "Gabrielle"
},
{
"family_name": "Townsend",
"given_name": "Alice",
"orcid": "0000-0001-6343-3362"
},
{
"family_name": "Vinko",
"given_name": "Jozsef",
"orcid": "0000-0001-8764-7832"
},
{
"family_name": "Wheeler",
"given_name": "J. Craig",
"orcid": "0000-0003-1349-6538"
},
{
"family_name": "Wold",
"given_name": "Avery",
"orcid": "0000-0002-9998-6732",
"clpid": "Wold-Avery"
}
],
"abstract": "Detecting gravitationally lensed supernovae is among the biggest challenges in astronomy. It involves a combination of two very rare phenomena: catching the transient signal of a stellar explosion in a distant galaxy and observing it through a nearly perfectly aligned foreground galaxy that deflects light towards the observer. Here we describe how high-cadence optical observations with the Zwicky Transient Facility, with its unparalleled large field of view, led to the detection of a multiply imaged type Ia supernova, SN Zwicky, also known as SN 2022qmx. Magnified nearly 25-fold, the system was found thanks to the standard candle nature of type Ia supernovae. High-spatial-resolution imaging with the Keck telescope resolved four images of the supernova with very small angular separation, corresponding to an Einstein radius of only \u03b8_E\u2009=\u20090.167\u2033 and almost identical arrival times. The small \u03b8_E and faintness of the lensing galaxy are very unusual, highlighting the importance of supernovae to fully characterize the properties of galaxy-scale gravitational lenses, including the impact of galaxy substructures.",
"doi": "10.1038/s41550-023-01981-3",
"pmcid": "PMC10509034",
"issn": "2397-3366",
"publisher": "Nature Publishing Group",
"publication": "Nature Astronomy",
"publication_date": "2023-09",
"series_number": "9",
"volume": "7",
"issue": "9",
"pages": "1098-1107"
},
{
"id": "authors:9nwtt-vpf67",
"collection": "authors",
"collection_id": "9nwtt-vpf67",
"cite_using_url": "https://authors.library.caltech.edu/records/9nwtt-vpf67",
"type": "article",
"title": "The Prevalence and Influence of Circumstellar Material around Hydrogen-rich Supernova Progenitors",
"author": [
{
"family_name": "Bruch",
"given_name": "Rachel J.",
"orcid": "0000-0001-8208-2473",
"clpid": "Bruch-Rachel-J"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Yaron",
"given_name": "Ofer",
"orcid": "0000-0002-0301-8017"
},
{
"family_name": "Chen",
"given_name": "Ping"
},
{
"family_name": "Strotjohann",
"given_name": "Nora L.",
"orcid": "0000-0002-4667-6730"
},
{
"family_name": "Irani",
"given_name": "Ido"
},
{
"family_name": "Zimmerman",
"given_name": "Erez",
"orcid": "0000-0001-8985-2493"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Yang",
"given_name": "Yi"
},
{
"family_name": "Kim",
"given_name": "Young-Lo",
"orcid": "0000-0002-1031-0796"
},
{
"family_name": "Bulla",
"given_name": "Mattia",
"orcid": "0000-0002-8255-5127"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Rigault",
"given_name": "Mickael",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Ofek",
"given_name": "Eran",
"orcid": "0000-0002-6786-8774"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane",
"orcid": "0000-0001-6753-1488"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Perley",
"given_name": "Daniel",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Nordin",
"given_name": "Jakob",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567"
},
{
"family_name": "Adams",
"given_name": "S.",
"clpid": "Adams-S"
},
{
"family_name": "Adreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Blagorodnova",
"given_name": "Nadia",
"orcid": "0000-0003-0901-1606"
},
{
"family_name": "Burdge",
"given_name": "Kevin",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-Kevin"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Dekany",
"given_name": "Richard G.",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Dhawan",
"given_name": "Suhail",
"orcid": "0000-0002-2376-6979"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"orcid": "0000-0003-0228-6594",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Graham",
"given_name": "Matthew",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Graham",
"given_name": "Melissa L.",
"orcid": "0000-0002-9154-3136"
},
{
"family_name": "Jencson",
"given_name": "Jacob",
"orcid": "0000-0001-5754-4007",
"clpid": "Jencson-Jacob"
},
{
"family_name": "Karamehmetoglu",
"given_name": "Emir",
"orcid": "0000-0001-6209-838X"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Miller",
"given_name": "A. A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-James-D"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Rusholme",
"given_name": "Benjamin",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin-J"
},
{
"family_name": "Sharma",
"given_name": "Y.",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Smith",
"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
},
{
"family_name": "Sravan",
"given_name": "Niharika"
},
{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "\n
Narrow transient emission lines (flash-ionization features) in early supernova (SN) spectra trace the presence of circumstellar material (CSM) around the massive progenitor stars of core-collapse SNe. The lines disappear within days after the SN explosion, suggesting that this material is spatially confined, and originates from enhanced mass loss shortly (months to a few years) prior to the explosion. We performed a systematic survey of H-rich (Type II) SNe discovered within less than 2 days from the explosion during the first phase of the Zwicky Transient Facility survey (2018–2020), finding 30 events for which a first spectrum was obtained within <2 days from the explosion. The measured fraction of events showing flash-ionization features (>36% at the 95% confidence level) confirms that elevated mass loss in massive stars prior to SN explosion is common. We find that SNe II showing flash-ionization features are not significantly brighter, nor bluer, nor more slowly rising than those without. This implies that CSM interaction does not contribute significantly to their early continuum emission, and that the CSM is likely optically thin. We measured the persistence duration of flash-ionization emission and find that most SNe show flash features for ≈5 days. Rarer events, with persistence timescales >10 days, are brighter and rise longer, suggesting these may be intermediate between regular SNe II and strongly interacting SNe IIn.
\n
\n
We present a search for extragalactic fast blue optical transients (FBOTs) during Phase I of the Zwicky Transient Facility (ZTF). We identify 38 candidates with durations above half-maximum light 1 day < t1/2 < 12 days, of which 28 have blue (g − r \u2272 −0.2 mag) colors at peak light. Of the 38 transients (28 FBOTs), 19 (13) can be spectroscopically classified as core-collapse supernovae (SNe): 11 (8) H- or He-rich (Type II/IIb/Ib) SNe, 6 (4) interacting (Type IIn/Ibn) SNe, and 2 (1) H&He-poor (Type Ic/Ic-BL) SNe. Two FBOTs (published previously) had predominantly featureless spectra and luminous radio emission: AT2018lug (The Koala) and AT2020xnd (The Camel). Seven (five) did not have a definitive classification: AT 2020bdh showed tentative broad Hα in emission, and AT 2020bot showed unidentified broad features and was 10 kpc offset from the center of an early-type galaxy. Ten (eight) have no spectroscopic observations or redshift measurements. We present multiwavelength (radio, millimeter, and/or X-ray) observations for five FBOTs (three Type Ibn, one Type IIn/Ibn, one Type IIb). Additionally, we search radio-survey (VLA and ASKAP) data to set limits on the presence of radio emission for 24 of the transients. All X-ray and radio observations resulted in nondetections; we rule out AT2018cow-like X-ray and radio behavior for five FBOTs and more luminous emission (such as that seen in the Camel) for four additional FBOTs. We conclude that exotic transients similar to AT2018cow, the Koala, and the Camel represent a rare subset of FBOTs and use ZTF’s SN classification experiments to measure the rate to be at most 0.1% of the local core-collapse SN rate.
\n
\n
The detonation of a thin (\u22720.03 M\u2299) helium shell (He-shell) atop a ∼1 M\u2299 white dwarf (WD) is a promising mechanism to explain normal Type Ia supernovae (SNe Ia), while thicker He-shells and less massive WDs may explain some recently observed peculiar SNe Ia. We present observations of SN 2020jgb, a peculiar SN Ia discovered by the Zwicky Transient Facility (ZTF). Near maximum brightness, SN 2020jgb is slightly subluminous (ZTF g-band absolute magnitude −18.7 mag \u2272 Mg \u2272 −18.2 mag depending on the amount of host-galaxy extinction) and shows an unusually red color (0.2 mag \u2272 gZTF − rZTF \u2272 0.4 mag) due to strong line-blanketing blueward of ∼5000 Å. These properties resemble those of SN 2018byg, a peculiar SN Ia consistent with an He-shell double detonation (DDet) SN. Using detailed radiative transfer models, we show that the optical spectroscopic and photometric evolution of SN 2020jgb is broadly consistent with a ∼0.95–1.00 M\u2299 (C/O core + He-shell) progenitor ignited by a \u22730.1 M\u2299 He-shell. However, one-dimensional radiative transfer models without non-local-thermodynamic-equilibrium treatment cannot accurately characterize the line-blanketing features, making the actual shell mass uncertain. We detect a prominent absorption feature at ∼1 μm in the near-infrared (NIR) spectrum of SN 2020jgb, which might originate from unburnt helium in the outermost ejecta. While the sample size is limited, we find similar 1 μm features in all the peculiar He-shell DDet candidates with NIR spectra obtained to date. SN 2020jgb is also the first peculiar He-shell DDet SN discovered in a star-forming dwarf galaxy, indisputably showing that He-shell DDet SNe occur in both star-forming and passive galaxies, consistent with the normal SN Ia population.
\n
During the Zwicky Transient Facility (ZTF) Phase I operations, 78 hydrogen-poor superluminous supernovae (SLSNe-I) were discovered in less than 3 yr, constituting the largest sample from a single survey. This paper (Paper I) presents the data, including the optical/UV light curves and classification spectra, while Paper II in this series will focus on the detailed analysis of the light curves and modeling. Our photometry is primarily taken by ZTF in the g, r, and i bands, and with additional data from other ground-based facilities and Swift. The events of our sample cover a redshift range of z = 0.06 − 0.67, with a median and 1σ error (16% and 84% percentiles) of z_(med) = 0.265^(+0.143)_(-0.135). The peak luminosity covers −22.8 mag ≤ Mg,peak ≤ −19.8 mag, with a median value of -21.48^(+1.13)_(-0.61) mag. The light curves evolve slowly with a mean rest-frame rise time of trise = 41.9 ± 17.8 days. The luminosity and timescale distributions suggest that low-luminosity SLSNe-I with a peak luminosity ∼−20 mag or extremely fast-rising events (<10 days) exist, but are rare. We confirm previous findings that slowly rising SLSNe-I also tend to fade slowly. The rest-frame color and temperature evolution show large scatters, suggesting that the SLSN-I population may have diverse spectral energy distributions. The peak rest-frame color shows a moderate correlation with the peak absolute magnitude, i.e., brighter SLSNe-I tend to have bluer colors. With optical and UV photometry, we construct the bolometric luminosity and derive a bolometric correction relation that is generally applicable for converting g, r-band photometry to the bolometric luminosity for SLSNe-I.
",
"doi": "10.3847/1538-4357/aca161",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2023-01-20",
"series_number": "1",
"volume": "943",
"issue": "1",
"pages": "41"
},
{
"id": "authors:r4cjc-p8341",
"collection": "authors",
"collection_id": "r4cjc-p8341",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230117-372591200.30",
"type": "article",
"title": "The Final Season Reimagined: 30 Tidal Disruption Events from the ZTF-I Survey",
"author": [
{
"family_name": "Hammerstein",
"given_name": "Erica",
"orcid": "0000-0002-5698-8703",
"clpid": "Hammerstein-Erica"
},
{
"family_name": "van Velzen",
"given_name": "Sjoert",
"orcid": "0000-0002-3859-8074"
},
{
"family_name": "Gezari",
"given_name": "Suvi",
"orcid": "0000-0003-3703-5154"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Ward",
"given_name": "Charlotte",
"orcid": "0000-0002-4557-6682"
},
{
"family_name": "Frederick",
"given_name": "Sara",
"orcid": "0000-0001-9676-730X"
},
{
"family_name": "Villanueva",
"given_name": "Natalia",
"orcid": "0000-0001-6917-4656"
},
{
"family_name": "Somalwar",
"given_name": "Jean J.",
"orcid": "0000-0001-8426-5732",
"clpid": "Somalwar-Jean-J"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Stern",
"given_name": "Daniel",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-Daniel"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Dhawan",
"given_name": "Suhail",
"orcid": "0000-0002-2376-6979"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"orcid": "0000-0003-0228-6594",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Gatkine",
"given_name": "Pradip",
"orcid": "0000-0002-1955-2230",
"clpid": "Gatkine-Pradip-R"
},
{
"family_name": "Groom",
"given_name": "Steven L.",
"orcid": "0000-0001-5668-3507",
"clpid": "Groom-Steven-L"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj-R"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Medford",
"given_name": "Michael S.",
"orcid": "0000-0002-7226-0659"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Purdum",
"given_name": "Josiah N.",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah-N"
},
{
"family_name": "van Roestel",
"given_name": "Jan",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-Joannes"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "Tidal disruption events (TDEs) offer a unique way to study dormant black holes. While the number of observed TDEs has grown thanks to the emergence of wide-field surveys in the past few decades, questions regarding the nature of the observed optical, UV, and X-ray emission remain. We present a uniformly selected sample of 30 spectroscopically classified TDEs from the Zwicky Transient Facility Phase I survey operations with follow-up Swift UV and X-ray observations. Through our investigation into correlations between light-curve properties, we recover a shallow positive correlation between the peak bolometric luminosity and decay timescales. We introduce a new spectroscopic class of TDE, TDE-featureless, which are characterized by featureless optical spectra. The new TDE-featureless class shows larger peak bolometric luminosities, peak blackbody temperatures, and peak blackbody radii. We examine the differences between the X-ray bright and X-ray faint populations of TDEs in this sample, finding that X-ray bright TDEs show higher peak blackbody luminosities than the X-ray faint subsample. This sample of optically selected TDEs is the largest sample of TDEs from a single survey yet, and the systematic discovery, classification, and follow-up of this sample allows for robust characterization of TDE properties, an important stepping stone looking forward toward the Rubin era.",
"doi": "10.3847/1538-4357/aca283",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2023-01-01",
"series_number": "1",
"volume": "942",
"issue": "1",
"pages": "9"
},
{
"id": "authors:vmjez-9w176",
"collection": "authors",
"collection_id": "vmjez-9w176",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230308-467584400.7",
"type": "article",
"title": "A very luminous jet from the disruption of a star by a massive black hole",
"author": [
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Lu",
"given_name": "Wenbin",
"orcid": "0000-0002-1568-7461"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "Kumar",
"given_name": "Harsh",
"orcid": "0000-0003-0871-4641"
},
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "de Ugarte Postigo",
"given_name": "Antonio",
"orcid": "0000-0001-7717-5085"
},
{
"family_name": "Sagu\u00e9s-Carracedo",
"given_name": "Ana",
"orcid": "0000-0002-3498-2167"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Kann",
"given_name": "D. Alexander",
"orcid": "0000-0003-2902-3583"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Tanvir",
"given_name": "Nial",
"orcid": "0000-0003-3274-6336"
},
{
"family_name": "Rest",
"given_name": "Armin",
"orcid": "0000-0002-4410-5387"
},
{
"family_name": "Izzo",
"given_name": "Luca",
"orcid": "0000-0001-9695-8472"
},
{
"family_name": "Somalwar",
"given_name": "Jean J.",
"orcid": "0000-0001-8426-5732",
"clpid": "Somalwar-Jean-J"
},
{
"family_name": "Kaplan",
"given_name": "David L.",
"orcid": "0000-0001-6295-2881"
},
{
"family_name": "Ahumada",
"given_name": "Tom\u00e1s",
"orcid": "0000-0002-2184-6430"
},
{
"family_name": "Anupama",
"given_name": "G. C.",
"orcid": "0000-0003-3533-7183"
},
{
"family_name": "Auchettl",
"given_name": "Katie",
"orcid": "0000-0002-4449-9152"
},
{
"family_name": "Barway",
"given_name": "Sudhanshu",
"orcid": "0000-0002-3927-5402"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Bhalerao",
"given_name": "Varun",
"orcid": "0000-0002-6112-7609"
},
{
"family_name": "Bloom",
"given_name": "Joshua S.",
"orcid": "0000-0002-7777-216X"
},
{
"family_name": "Bremer",
"given_name": "Michael",
"orcid": "0000-0001-7511-3745"
},
{
"family_name": "Bulla",
"given_name": "Mattia",
"orcid": "0000-0002-8255-5127"
},
{
"family_name": "Burns",
"given_name": "Eric",
"orcid": "0000-0002-2942-3379"
},
{
"family_name": "Campana",
"given_name": "Sergio",
"orcid": "0000-0001-6278-1576"
},
{
"family_name": "Chandra",
"given_name": "Poonam",
"orcid": "0000-0002-0844-6563"
},
{
"family_name": "Charalampopoulos",
"given_name": "Panos",
"orcid": "0000-0002-0326-6715"
},
{
"family_name": "Cooke",
"given_name": "Jeff",
"orcid": "0000-0001-5703-2108"
},
{
"family_name": "D'Elia",
"given_name": "Valerio"
},
{
"family_name": "Das",
"given_name": "Kaustav Kashyap",
"orcid": "0000-0001-8372-997X",
"clpid": "Das-Kaustav-Kashyap"
},
{
"family_name": "Dobie",
"given_name": "Dougal"
},
{
"family_name": "Ag\u00fc\u00ed Fern\u00e1ndez",
"given_name": "Jos\u00e9 Feliciano",
"orcid": "0000-0001-6991-7616"
},
{
"family_name": "Freeburn",
"given_name": "James"
},
{
"family_name": "Fremling",
"given_name": "Cristoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Cristoffer"
},
{
"family_name": "Gezari",
"given_name": "Suvi",
"orcid": "0000-0003-3703-5154"
},
{
"family_name": "Goode",
"given_name": "Simon",
"orcid": "0000-0002-9575-5152"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Hammerstein",
"given_name": "Erica",
"orcid": "0000-0002-5698-8703"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj R.",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj-R"
},
{
"family_name": "Kilpatrick",
"given_name": "Charles D.",
"orcid": "0000-0002-5740-7747"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877"
},
{
"family_name": "Krips",
"given_name": "Melanie"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Leloudas",
"given_name": "Giorgos",
"orcid": "0000-0002-8597-0756"
},
{
"family_name": "Levan",
"given_name": "Andrew",
"orcid": "0000-0001-7821-9369"
},
{
"family_name": "Lundquist",
"given_name": "Michael J.",
"orcid": "0000-0001-9589-3793"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-Ashish-A"
},
{
"family_name": "Medford",
"given_name": "Michael S.",
"orcid": "0000-0002-7226-0659"
},
{
"family_name": "Miller",
"given_name": "M. Coleman",
"orcid": "0000-0002-2666-728X"
},
{
"family_name": "M\u00f6ller",
"given_name": "Anais",
"orcid": "0000-0001-8211-8608"
},
{
"family_name": "Mooley",
"given_name": "Kunal P.",
"orcid": "0000-0002-2557-5180",
"clpid": "Mooley-Kunal-Prakash"
},
{
"family_name": "Nayana",
"given_name": "A. J."
},
{
"family_name": "Nir",
"given_name": "Guy",
"orcid": "0000-0002-7501-5579"
},
{
"family_name": "Pang",
"given_name": "Peter T. H.",
"orcid": "0000-0001-7041-3239"
},
{
"family_name": "Paraskeva",
"given_name": "Emmy",
"orcid": "0000-0003-2814-4383"
},
{
"family_name": "Perley",
"given_name": "Richard A.",
"orcid": "0000-0001-7097-8360"
},
{
"family_name": "Petitpas",
"given_name": "Glen"
},
{
"family_name": "Pursiainen",
"given_name": "Miika",
"orcid": "0000-0003-4663-4300"
},
{
"family_name": "Ravi",
"given_name": "Vikram",
"orcid": "0000-0002-7252-5485",
"clpid": "Ravi-Vikram"
},
{
"family_name": "Ridden-Harper",
"given_name": "Ryan",
"orcid": "0000-0003-1724-2885"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Rigault",
"given_name": "Mickael",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Rodriguez",
"given_name": "Antonio C.",
"orcid": "0000-0003-4189-9668",
"clpid": "Rodriguez-Antonio-C"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Smith",
"given_name": "I. A.",
"orcid": "0000-0001-8605-5608"
},
{
"family_name": "Stein",
"given_name": "Robert D.",
"orcid": "0000-0003-2434-0387",
"clpid": "Stein-Robert-D"
},
{
"family_name": "Th\u00f6ne",
"given_name": "Christina",
"orcid": "0000-0002-7978-7648"
},
{
"family_name": "Tohuvavohu",
"given_name": "Aaron",
"orcid": "0000-0002-2810-8764"
},
{
"family_name": "Valdes",
"given_name": "Frank",
"orcid": "0000-0001-5567-1301"
},
{
"family_name": "van Roestel",
"given_name": "Jan",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-Jan"
},
{
"family_name": "Vergani",
"given_name": "Susanna D.",
"orcid": "0000-0001-9398-4907"
},
{
"family_name": "Wang",
"given_name": "Qinan",
"orcid": "0000-0001-5233-6989"
},
{
"family_name": "Zhang",
"given_name": "Jielai",
"orcid": "0000-0001-5310-4186"
}
],
"abstract": "Tidal disruption events (TDEs) are bursts of electromagnetic energy that are released when supermassive black holes at the centres of galaxies violently disrupt a star that passes too close1. TDEs provide a window through which to study accretion onto supermassive black holes; in some rare cases, this accretion leads to launching of a relativistic jet, but the necessary conditions are not fully understood. The best-studied jetted TDE so far is Swift J1644+57, which was discovered in \u03b3-rays, but was too obscured by dust to be seen at optical wavelengths. Here we report the optical detection of AT2022cmc, a rapidly fading source at cosmological distance (redshift z\u2009=\u20091.19325) the unique light curve of which transitioned into a luminous plateau within days. Observations of a bright counterpart at other wavelengths, including X-ray, submillimetre and radio, supports the interpretation of AT2022cmc as a jetted TDE containing a synchrotron 'afterglow', probably launched by a supermassive black hole with spin greater than approximately 0.3. Using four years of Zwicky Transient Facility survey data, we calculate a rate of 0.02\u207a\u2070\u22c5\u2070\u2074\u208b\u2080.\u2080\u2081 Gpc\u207b\u00b3 yr\u207b\u00b9 for on-axis jetted TDEs on the basis of the luminous, fast-fading red component, thus providing a measurement complementary to the rates derived from X-ray and radio observations. Correcting for the beaming angle effects, this rate confirms that approximately 1\u2009per\u2009cent of TDEs have relativistic jets. Optical surveys can use AT2022cmc as a prototype to unveil a population of jetted TDEs.",
"doi": "10.1038/s41586-022-05465-8",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "2022-12-15",
"series_number": "7940",
"volume": "612",
"issue": "7940",
"pages": "430-434"
},
{
"id": "authors:sk1fw-ga715",
"collection": "authors",
"collection_id": "sk1fw-ga715",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20221003-756400000.28",
"type": "article",
"title": "GROWTH on S190426c II: GROWTH-India Telescope search for an optical counterpart with a custom image reduction and candidate vetting pipeline",
"author": [
{
"family_name": "Kumar",
"given_name": "Harsh",
"orcid": "0000-0003-0871-4641",
"clpid": "Kumar-Harsh"
},
{
"family_name": "Bhalerao",
"given_name": "Varun",
"orcid": "0000-0002-6112-7609",
"clpid": "Bhalerao-Varun"
},
{
"family_name": "Anupama",
"given_name": "G. C.",
"orcid": "0000-0003-3533-7183",
"clpid": "Anupama-Gadiyara-Chakrapani"
},
{
"family_name": "Barway",
"given_name": "Sudhanshu",
"orcid": "0000-0002-3927-5402",
"clpid": "Barway-Sudhanshu"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924",
"clpid": "Coughlin-M-W"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Deshmukh",
"given_name": "Kunal",
"orcid": "0000-0001-5253-3480",
"clpid": "Deshmukh-Kunal"
},
{
"family_name": "Dutta",
"given_name": "Anirban",
"orcid": "0000-0002-7708-3831",
"clpid": "Dutta-Anirban"
},
{
"family_name": "Goldstein",
"given_name": "Daniel A.",
"orcid": "0000-0003-3461-8661",
"clpid": "Goldstein-D-A"
},
{
"family_name": "Jassani",
"given_name": "Adeem",
"orcid": "0000-0003-2191-4541",
"clpid": "Jassani-Adeem"
},
{
"family_name": "Joharle",
"given_name": "Simran",
"orcid": "0000-0002-8875-6413",
"clpid": "Joharle-Simran"
},
{
"family_name": "Karambelker",
"given_name": "Viraj",
"clpid": "Karambelker-Viraj"
},
{
"family_name": "Khandagale",
"given_name": "Maitreya",
"clpid": "Khandagale-Maitreya"
},
{
"family_name": "Kumar",
"given_name": "Brajesh",
"orcid": "0000-0001-7225-2475",
"clpid": "Kumar-Brajesh"
},
{
"family_name": "Saraogi",
"given_name": "Divita",
"clpid": "Saraogi-Divita"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Shenoy",
"given_name": "Vedant",
"clpid": "Shenoy-Vedant"
},
{
"family_name": "Singer",
"given_name": "Leo",
"orcid": "0000-0001-9898-5597",
"clpid": "Singer-L-P"
},
{
"family_name": "Singh",
"given_name": "Avinash",
"orcid": "0000-0003-2091-622X",
"clpid": "Singh-Avinash"
},
{
"family_name": "Waratkar",
"given_name": "Gaurav",
"orcid": "0000-0003-3630-9440",
"clpid": "Waratkar-Gaurav"
}
],
"abstract": "S190426c/GW190426_152155 was the first probable neutron star\u2013black hole merger candidate detected by the LIGO-Virgo Collaboration. We undertook a tiled search for optical counterparts of this event using the 0.7-m GROWTH-India Telescope. Over a period of two weeks, we obtained multiple observations over a 22.1\u2009deg\u00b2 area, with a 17.5\u2009per\u2009cent probability of containing the source location. Initial efforts included obtaining photometry of sources reported by various groups, and a visual search for sources in all galaxies contained in the region. Subsequently, we have developed an image subtraction and candidate vetting pipeline with \u223c94 per cent efficiency for transient detection. Processing the data with this pipeline, we find several transients, but none that are compatible with kilonova models. We present the details of our observations, the working of our pipeline, results from the search, and our interpretations of the non-detections that will work as a pathfinder during the O4 run of LVK.",
"doi": "10.1093/mnras/stac2516",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2022-11",
"series_number": "3",
"volume": "516",
"issue": "3",
"pages": "4517-4528"
},
{
"id": "authors:kwtgw-mtj42",
"collection": "authors",
"collection_id": "kwtgw-mtj42",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220923-941669700.13",
"type": "article",
"title": "The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk-Corona System",
"author": [
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Lu",
"given_name": "Wenbin",
"orcid": "0000-0002-1568-7461"
},
{
"family_name": "Guolo",
"given_name": "Muryel",
"orcid": "0000-0002-5063-0751"
},
{
"family_name": "Pasham",
"given_name": "Dheeraj R.",
"orcid": "0000-0003-1386-7861"
},
{
"family_name": "Gezari",
"given_name": "Suvi",
"orcid": "0000-0003-3703-5154"
},
{
"family_name": "Gilfanov",
"given_name": "Marat"
},
{
"family_name": "Gendreau",
"given_name": "Keith C.",
"orcid": "0000-0001-7115-2819"
},
{
"family_name": "Harrison",
"given_name": "Fiona A.",
"orcid": "0000-0002-4226-8959",
"clpid": "Harrison-F-A"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Miller",
"given_name": "Jon M.",
"orcid": "0000-0003-2869-7682"
},
{
"family_name": "Walton",
"given_name": "Dominic J.",
"orcid": "0000-0001-5819-3552"
},
{
"family_name": "Garc\u00eda",
"given_name": "Javier A.",
"orcid": "0000-0003-3828-2448",
"clpid": "Garc\u00eda-Javier-A"
},
{
"family_name": "Velzen",
"given_name": "Sjoert van",
"orcid": "0000-0002-3859-8074"
},
{
"family_name": "Alexander",
"given_name": "Kate D.",
"orcid": "0000-0002-8297-2473"
},
{
"family_name": "Miller-Jones",
"given_name": "James C. A.",
"orcid": "0000-0003-3124-2814"
},
{
"family_name": "Nicholl",
"given_name": "Matt",
"orcid": "0000-0002-2555-3192"
},
{
"family_name": "Hammerstein",
"given_name": "Erica",
"orcid": "0000-0002-5698-8703"
},
{
"family_name": "Medvedev",
"given_name": "Pavel",
"orcid": "0000-0002-9380-8708"
},
{
"family_name": "Stern",
"given_name": "Daniel",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-D"
},
{
"family_name": "Ravi",
"given_name": "Vikram",
"orcid": "0000-0002-7252-5485",
"clpid": "Ravi-Vikram"
},
{
"family_name": "Sunyaev",
"given_name": "R."
},
{
"family_name": "Bloom",
"given_name": "Joshua S.",
"orcid": "0000-0002-7777-216X"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-Ashish-A"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Purdum",
"given_name": "Josiah N.",
"orcid": "0000-0003-1227-3738",
"clpid": "Purdum-Josiah-N"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Smith",
"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
}
],
"abstract": "We present X-ray, UV, optical, and radio observations of the nearby (\u224878 Mpc) tidal disruption event AT2021ehb/ZTF21aanxhjv during its first 430 days of evolution. AT2021ehb occurs in the nucleus of a galaxy hosting a \u2248 107 M_\u2299 black hole (M_(BH) inferred from host galaxy scaling relations). High-cadence Swift and Neutron Star Interior Composition Explorer (NICER) monitoring reveals a delayed X-ray brightening. The spectrum first undergoes a gradual soft \u2192 hard transition and then suddenly turns soft again within 3 days at \u03b4t \u2248 272 days during which the X-ray flux drops by a factor of 10. In the joint NICER+NuSTAR observation (\u03b4t = 264 days, harder state), we observe a prominent nonthermal component up to 30 keV and an extremely broad emission line in the iron K band. The bolometric luminosity of AT2021ehb reaches a maximum of 6.0^(+10.4)_(3.8)%L_(Edd) when the X-ray spectrum is the hardest. During the dramatic X-ray evolution, no radio emission is detected, the UV/optical luminosity stays relatively constant, and the optical spectra are featureless. We propose the following interpretations: (i) the soft \u2192 hard transition may be caused by the gradual formation of a magnetically dominated corona; (ii) hard X-ray photons escape from the system along solid angles with low scattering optical depth (\u223c a few) whereas the UV/optical emission is likely generated by reprocessing materials with much larger column density\u2014the system is highly aspherical; and (iii) the abrupt X-ray flux drop may be triggered by the thermal\u2013viscous instability in the inner accretion flow, leading to a much thinner disk.",
"doi": "10.3847/1538-4357/ac898a",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2022-09-01",
"series_number": "1",
"volume": "937",
"issue": "1",
"pages": "8"
},
{
"id": "authors:k0htw-ebh48",
"collection": "authors",
"collection_id": "k0htw-ebh48",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220810-402579000",
"type": "article",
"title": "India's First Robotic Eye for Time-domain Astrophysics: The GROWTH-India Telescope",
"author": [
{
"family_name": "Kumar",
"given_name": "Harsh",
"orcid": "0000-0003-0871-4641",
"clpid": "Kumar-Harsh"
},
{
"family_name": "Bhalerao",
"given_name": "Varun",
"orcid": "0000-0002-6112-7609"
},
{
"family_name": "Anupama",
"given_name": "G. C.",
"orcid": "0000-0003-3533-7183"
},
{
"family_name": "Barway",
"given_name": "Sudhanshu",
"orcid": "0000-0002-3927-5402"
},
{
"family_name": "Basu",
"given_name": "Judhajeet",
"orcid": "0000-0001-7570-545X"
},
{
"family_name": "Deshmukh",
"given_name": "Kunal",
"orcid": "0000-0001-5253-3480"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Dutta",
"given_name": "Anirban",
"orcid": "0000-0002-7708-3831"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Iyer",
"given_name": "Hrishikesh",
"orcid": "0000-0002-2395-8727"
},
{
"family_name": "Jassani",
"given_name": "Adeem",
"orcid": "0000-0003-2191-4541"
},
{
"family_name": "Joharle",
"given_name": "Simran",
"orcid": "0000-0002-8875-6413"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj-R"
},
{
"family_name": "Khandagale",
"given_name": "Maitreya"
},
{
"family_name": "Krishna",
"given_name": "K. Adithya"
},
{
"family_name": "Kulkarni",
"given_name": "Sumeet",
"orcid": "0000-0001-8057-0203"
},
{
"family_name": "Mate",
"given_name": "Sujay",
"orcid": "0000-0001-5536-4635"
},
{
"family_name": "Patil",
"given_name": "Atharva"
},
{
"family_name": "Phanindra",
"given_name": "DVS",
"orcid": "0000-0002-1762-0834"
},
{
"family_name": "Samantaray",
"given_name": "Subham",
"orcid": "0000-0003-2167-9764"
},
{
"family_name": "Sharma",
"given_name": "Kritti",
"orcid": "0000-0002-4477-3625"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Shenoy",
"given_name": "Vedant"
},
{
"family_name": "Singh",
"given_name": "Avinash",
"orcid": "0000-0003-2091-622X"
},
{
"family_name": "Srivastava",
"given_name": "Shubham",
"orcid": "0000-0003-4524-6883"
},
{
"family_name": "Swain",
"given_name": "Vishwajeet",
"orcid": "0000-0002-7942-8477"
},
{
"family_name": "Waratkar",
"given_name": "Gaurav",
"orcid": "0000-0003-3630-9440"
},
{
"family_name": "Angchuk",
"given_name": "Dorje"
},
{
"family_name": "Dorjay",
"given_name": "Padma",
"orcid": "0000-0001-5690-2212"
},
{
"family_name": "Dorjai",
"given_name": "Tsewang"
},
{
"family_name": "Gyalson",
"given_name": "Tsewang"
},
{
"family_name": "Jorphail",
"given_name": "Sonam"
},
{
"family_name": "Mahay",
"given_name": "Tashi Thsering"
},
{
"family_name": "Norbu",
"given_name": "Rigzin"
},
{
"family_name": "Sharma",
"given_name": "Tarun Kumar",
"orcid": "0000-0002-2966-2951"
},
{
"family_name": "Stanzin",
"given_name": "Jigmet"
},
{
"family_name": "Stanzin",
"given_name": "Tsewang",
"orcid": "0000-0002-1469-3958"
},
{
"family_name": "Stanzin",
"given_name": "Urgain"
}
],
"abstract": "We present the design and performance of the GROWTH-India telescope, a 0.7 m robotic telescope dedicated to time-domain astronomy. The telescope is equipped with a 4k back-illuminated camera that gives a 0.\u00b082 field of view and a sensitivity of m_(g\u2032) \u223c 20.5 in 5 minute exposures. Custom software handles observatory operations: attaining high on-sky observing efficiencies (\u227380%) and allowing rapid response to targets of opportunity. The data processing pipelines are capable of performing point-spread function photometry as well as image subtraction for transient searches. We also present an overview of the GROWTH-India telescope's contributions to the studies of gamma-ray bursts, the electromagnetic counterparts to gravitational wave sources, supernovae, novae, and solar system objects.",
"doi": "10.3847/1538-3881/ac7bea",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2022-09",
"series_number": "3",
"volume": "164",
"issue": "3",
"pages": "Art. No. 90"
},
{
"id": "authors:q0bbr-ze020",
"collection": "authors",
"collection_id": "q0bbr-ze020",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211213-225024102",
"type": "article",
"title": "PGIR 20eid (SN 2020qmp): A Type IIP Supernova at 15.6 Mpc discovered by the Palomar Gattini-IR survey",
"author": [
{
"family_name": "Srinivasaragavan",
"given_name": "G. P.",
"clpid": "Srinivasaragavan-G-P"
},
{
"family_name": "Sfaradi",
"given_name": "I.",
"clpid": "Sfaradi-Itai"
},
{
"family_name": "Jencson",
"given_name": "J.",
"orcid": "0000-0001-5754-4007",
"clpid": "Jencson-Jacob-E"
},
{
"family_name": "De",
"given_name": "K.",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Horesh",
"given_name": "A.",
"orcid": "0000-0002-5936-1156",
"clpid": "Horesh-Assaf"
},
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Tinyanont",
"given_name": "S.",
"orcid": "0000-0002-1481-4676",
"clpid": "Tinyanont-Samaporn"
},
{
"family_name": "Hankins",
"given_name": "M.",
"orcid": "0000-0001-9315-8437",
"clpid": "Hankins-Matthew-J"
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889",
"clpid": "Schulze-Steve"
},
{
"family_name": "Ashley",
"given_name": "M. C. B.",
"orcid": "0000-0003-1412-2028",
"clpid": "Ashley-Michael-C-B"
},
{
"family_name": "Graham",
"given_name": "M. J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Karambelkar",
"given_name": "V.",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj-R"
},
{
"family_name": "Lau",
"given_name": "R.",
"clpid": "Lau-Ryan-M"
},
{
"family_name": "Mahabal",
"given_name": "A. A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-Ashish-A"
},
{
"family_name": "Moore",
"given_name": "A. M.",
"orcid": "0000-0002-2894-6936",
"clpid": "Moore-Anna-Marie"
},
{
"family_name": "Ofek",
"given_name": "E. O.",
"orcid": "0000-0002-6786-8774",
"clpid": "Ofek-Eran-O"
},
{
"family_name": "Sharma",
"given_name": "Y.",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-Jesper"
},
{
"family_name": "Soon",
"given_name": "J.",
"clpid": "Soon-Jamie"
},
{
"family_name": "Soria",
"given_name": "R.",
"orcid": "0000-0002-4622-796X",
"clpid": "Soria-Roberto"
},
{
"family_name": "Travouillon",
"given_name": "T.",
"orcid": "0000-0001-9304-6718",
"clpid": "Travouillon-Tony-D"
},
{
"family_name": "Walters",
"given_name": "R.",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard-S"
}
],
"abstract": "Aims. We present a detailed analysis of SN 2020qmp, a nearby Type IIP core-collapse supernova (CCSN) that was discovered by the Palomar Gattini-IR survey in the galaxy UGC07125 (distance of \u224815.6 \u00b1 4 Mpc). We illustrate how the multiwavelength study of this event helps our general understanding of stellar progenitors and circumstellar medium (CSM) interactions in CCSNe. We highlight the importance of near-infrared (NIR) surveys for detections of supernovae in dusty environments.\nMethods. We analyze data from observations in various bands: radio, NIR, optical, and X-rays. We use optical and NIR data for a spectroscopic and spectro-polarimetric study of the supernova and to model its light curve (LC). We obtain an estimate of the zero-age main-sequence (ZAMS) progenitor mass from the luminosity of the [O\u202fI] doublet lines (\u03bb\u03bb6300,\u20066364) normalized to the decay power of \u2075\u2076Co. We also independently estimate the explosion energy and ZAMS progenitor mass through hydrodynamical LC modeling. From radio and X-ray observations, we derive the mass-loss rate and microphysical parameters of the progenitor star, and we investigate possible deviations from energy equipartition of magnetic fields and electrons in a standard CSM interaction model. Finally, we simulate a sample of CCSNe with plausible distributions of brightness and extinction, within 40 Mpc, and test what fraction of the sample is detectable at peak light by NIR surveys versus optical surveys.\nResults. SN 2020qmp displays characteristic hydrogen lines in its optical spectra as well as a plateau in its optical LC, hallmarks of a Type IIP supernova. We do not detect linear polarization during the plateau phase, with a 3\u03c3 upper limit of 0.78%. Through hydrodynamical LC modeling and an analysis of its nebular spectra, we estimate a ZAMS progenitor mass of around 11.0 M\u2299 and an explosion energy of around 0.8 \u00d7 10\u2075\u00b9 erg. We find that the spectral energy distribution cannot be explained by a simple CSM interaction model, assuming a constant shock velocity and a steady mass-loss rate. In particular, the excess X-ray luminosity compared with the synchrotron radio luminosity suggests deviations from equipartition. Finally, we demonstrate the advantages of NIR surveys over optical surveys for the detection of dust-obscured CCSNe in the local Universe. Specifically, our simulations show that the Wide-Field Infrared Transient Explorer will detect up to 14 more CCSNe (out of the 75 expected in its footprint) within 40 Mpc over five years than would an optical survey equivalent to the Zwicky Transient Facility.\nConclusions. We have determined or constrained the main properties of SN 2020qmp and its progenitor, highlighting the value of multiwavelength follow-up observations of nearby CCSNe. We have shown that forthcoming NIR surveys will enable us to improve constraints on the local CCSN rate by detecting obscured supernovae that would be missed by optical searches.",
"doi": "10.1051/0004-6361/202142158",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2022-04",
"volume": "660",
"pages": "Art. No. A138"
},
{
"id": "authors:f2w47-e5m98",
"collection": "authors",
"collection_id": "f2w47-e5m98",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220125-215144189",
"type": "article",
"title": "A Matched Survey for the Enigmatic Low Radio Frequency Transient ILT J225347+862146",
"author": [
{
"family_name": "Huang",
"given_name": "Yuping",
"orcid": "0000-0003-4267-6108",
"clpid": "Huang-Yuping"
},
{
"family_name": "Anderson",
"given_name": "Marin M.",
"orcid": "0000-0003-2238-2698",
"clpid": "Anderson-Marin-M"
},
{
"family_name": "Hallinan",
"given_name": "Gregg",
"orcid": "0000-0002-7083-4049",
"clpid": "Hallinan-G"
},
{
"family_name": "Lazio",
"given_name": "T. Joseph W.",
"clpid": "Lazio-T-Joseph-W"
},
{
"family_name": "Price",
"given_name": "Danny C.",
"orcid": "0000-0003-2783-1608",
"clpid": "Price-Danny-C"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
}
],
"abstract": "Discovered in 2011 with LOFAR, the 15 Jy low-frequency radio transient ILT J225347+862146 heralds a potentially prolific population of radio transients at <100 MHz. However, subsequent transient searches in similar parameter space yielded no detections. We test the hypothesis that these surveys at comparable sensitivity have missed the population due to mismatched survey parameters. In particular, the LOFAR survey used only 195 kHz of bandwidth at 60 MHz, while other surveys were at higher frequencies or had wider bandwidth. Using 137 hr of all-sky images from the Owens Valley Radio Observatory Long Wavelength Array, we conduct a narrowband transient search at \u223c10 Jy sensitivity with timescales from 10 minutes to 1 day and a bandwidth of 722 kHz at 60 MHz. To model the remaining survey selection effects, we introduce a flexible Bayesian approach for inferring transient rates. We do not detect any transient and find compelling evidence that our nondetection is inconsistent with the detection of ILT J225347+862146. Under the assumption that the transient is astrophysical, we propose two hypotheses that may explain our nondetection. First, the transient population associated with ILT J225347+862146 may have a low all-sky density and display strong temporal clustering. Second, ILT J225347+862146 may be an extreme instance of the fluence distribution, of which we revise the surface density estimate at 15 Jy to 1.1 \u00d7 10\u207b\u2077 deg\u207b\u00b2 with a 95% credible interval of (3.5 \u00d7 10\u207b\u00b9\u00b2, 3.4 \u00d7 10\u207b\u2077) deg\u207b\u00b2. Finally, we find a previously identified object coincident with ILT J225347+862146 to be an M dwarf at 420 pc.",
"doi": "10.3847/1538-4357/ac4048",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2022-02-01",
"series_number": "2",
"volume": "925",
"issue": "2",
"pages": "Art. No. 171"
},
{
"id": "authors:j9tpd-hcc07",
"collection": "authors",
"collection_id": "j9tpd-hcc07",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220322-742311000",
"type": "article",
"title": "New Modules for the SEDMachine to Remove Contaminations from Cosmic Rays and Non-target Light: byecr and contsep",
"author": [
{
"family_name": "Kim",
"given_name": "Y.-L.",
"orcid": "0000-0002-1031-0796",
"clpid": "Kim-Young-Lo"
},
{
"family_name": "Rigault",
"given_name": "M.",
"orcid": "0000-0002-8121-2560",
"clpid": "Rigault-Mickael"
},
{
"family_name": "Neill",
"given_name": "J. D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-James-D"
},
{
"family_name": "Briday",
"given_name": "M.",
"orcid": "0000-0002-3156-5077",
"clpid": "Briday-Martin"
},
{
"family_name": "Copin",
"given_name": "Y.",
"orcid": "0000-0002-5317-7518",
"clpid": "Copin-Yannick"
},
{
"family_name": "Lezmy",
"given_name": "J.",
"clpid": "Lezmy-J"
},
{
"family_name": "Nicolas",
"given_name": "N.",
"orcid": "0000-0002-2681-6580",
"clpid": "Nicolas-Nora"
},
{
"family_name": "Riddle",
"given_name": "R.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Sharma",
"given_name": "Y.",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Smith",
"given_name": "M.",
"orcid": "0000-0002-3321-1432",
"clpid": "Smith-Mathew"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-Jesper"
},
{
"family_name": "Walters",
"given_name": "R.",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard-S"
}
],
"abstract": "Currently time-domain astronomy can scan the entire sky on a daily basis, discovering thousands of interesting transients every night. Classifying the ever-increasing number of new transients is one of the main challenges for the astronomical community. One solution that addresses this issue is the robotically controlled Spectral Energy Distribution Machine (SEDM) which supports the Zwicky Transient Facility (ZTF). SEDM with its pipeline pysedm demonstrates that real-time robotic spectroscopic classification is feasible. In an effort to improve the quality of the current SEDM data, we present here two new modules, byecr and contsep. The first removes contamination from cosmic rays, and the second removes contamination from non-target light. These new modules are part of the automated pysedm pipeline and fully integrated with the whole process. Employing byecr and contsep modules together automatically extracts more spectra than the current pysedm pipeline. Using SNID classification results, the new modules show an improvement in the classification rate and accuracy of 2.8% and 1.7%, respectively, while the strength of the cross-correlation remains the same. Improvements to the SEDM astrometry would further boost the improvement of the contsep module. This kind of robotic follow-up with a fully automated pipeline has the potential to provide the spectroscopic classifications for the transients discovered by ZTF and also by the Rubin Observatory's Legacy Survey of Space and Time.",
"doi": "10.1088/1538-3873/ac50a0",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2022-02",
"series_number": "1032",
"volume": "134",
"issue": "1032",
"pages": "Art. No. 024505"
},
{
"id": "authors:tw5q0-dex83",
"collection": "authors",
"collection_id": "tw5q0-dex83",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210927-205831656",
"type": "article",
"title": "A WC/WO star exploding within an expanding carbon\u2013oxygen\u2013neon nebula",
"author": [
{
"family_name": "Gal-Yam",
"given_name": "A.",
"orcid": "0000-0002-3653-5598",
"clpid": "Gal-Yam-Avishay"
},
{
"family_name": "Bruch",
"given_name": "R.",
"orcid": "0000-0001-8208-2473"
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Yang",
"given_name": "Y."
},
{
"family_name": "Perley",
"given_name": "D. A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Irani",
"given_name": "I.",
"orcid": "0000-0002-7996-8780"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Kool",
"given_name": "E. C.",
"orcid": "0000-0002-7252-3877"
},
{
"family_name": "Soumagnac",
"given_name": "M. T.",
"orcid": "0000-0001-6753-1488"
},
{
"family_name": "Yaron",
"given_name": "O.",
"orcid": "0000-0002-0301-8017"
},
{
"family_name": "Strotjohann",
"given_name": "N. L.",
"orcid": "0000-0002-4667-6730"
},
{
"family_name": "Zimmerman",
"given_name": "E.",
"orcid": "0000-0001-8985-2493"
},
{
"family_name": "Barbarino",
"given_name": "C.",
"orcid": "0000-0002-3821-6144"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "De",
"given_name": "K.",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Yao",
"given_name": "Y.",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Ofek",
"given_name": "E. O.",
"orcid": "0000-0002-6786-8774"
},
{
"family_name": "Fransson",
"given_name": "C.",
"orcid": "0000-0001-8532-3594"
},
{
"family_name": "Filippenko",
"given_name": "A. V.",
"orcid": "0000-0003-3460-0103"
},
{
"family_name": "Zheng",
"given_name": "W."
},
{
"family_name": "Brink",
"given_name": "T. G.",
"orcid": "0000-0001-5955-2502"
},
{
"family_name": "Copperwheat",
"given_name": "C. M.",
"orcid": "0000-0001-7983-8698"
},
{
"family_name": "Foley",
"given_name": "R. J."
},
{
"family_name": "Brown",
"given_name": "J.",
"orcid": "0000-0002-1885-6419"
},
{
"family_name": "Siebert",
"given_name": "M.",
"orcid": "0000-0003-2445-3891"
},
{
"family_name": "Leloudas",
"given_name": "G.",
"orcid": "0000-0002-8597-0756"
},
{
"family_name": "Cabrera Lavers",
"given_name": "A. L.",
"orcid": "0000-0002-9153-8724"
},
{
"family_name": "Garcia Alvarez",
"given_name": "D."
},
{
"family_name": "Marante-Barreto",
"given_name": "A."
},
{
"family_name": "Frederick",
"given_name": "S.",
"orcid": "0000-0001-9676-730X"
},
{
"family_name": "Hung",
"given_name": "T.",
"orcid": "0000-0002-9878-7889"
},
{
"family_name": "Wheeler",
"given_name": "J. C.",
"orcid": "0000-0003-1349-6538"
},
{
"family_name": "Vink\u00f3",
"given_name": "J.",
"orcid": "0000-0001-8764-7832"
},
{
"family_name": "Thomas",
"given_name": "B. P."
},
{
"family_name": "Graham",
"given_name": "M. J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Duev",
"given_name": "D. A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Drake",
"given_name": "A. J.",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Dekany",
"given_name": "R.",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Bellm",
"given_name": "E. C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Shupe",
"given_name": "D. L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Andreoni",
"given_name": "I.",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Sharma",
"given_name": "Y.",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Riddle",
"given_name": "R.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "van Roestel",
"given_name": "J.",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-Joannes-C"
},
{
"family_name": "Knezevic",
"given_name": "N."
}
],
"abstract": "The final fate of massive stars, and the nature of the compact remnants they leave behind (black holes and neutron stars), are open questions in astrophysics. Many massive stars are stripped of their outer hydrogen envelopes as they evolve. Such Wolf\u2013Rayet stars emit strong and rapidly expanding winds with speeds greater than 1,000\u2009kilometres\u2009per second. A fraction of this population is also helium-depleted, with spectra dominated by highly ionized emission lines of carbon and oxygen (types\u2009WC/WO). Evidence indicates that the most commonly observed supernova explosions that lack hydrogen and helium (types\u2009Ib/Ic) cannot result from massive WC/WO stars , leading some to suggest that most such stars collapse directly into black holes without a visible supernova explosion4. Here we report observations of SN\u20092019hgp, beginning about a day after the explosion. Its short rise time and rapid decline place it among an emerging population of rapidly evolving transients. Spectroscopy reveals a rich set of emission lines indicating that the explosion occurred within a nebula composed of carbon, oxygen and neon. Narrow absorption features show that this material is expanding at high velocities (greater than 1,500\u2009kilometres\u2009per second), requiring a compact progenitor. Our observations are consistent with an explosion of a massive WC/WO star, and suggest that massive Wolf\u2013Rayet stars may be the progenitors of some rapidly evolving transients.",
"doi": "10.1038/s41586-021-04155-1",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "2022-01-13",
"series_number": "7892",
"volume": "601",
"issue": "7892",
"pages": "201-204"
},
{
"id": "authors:fg24c-jmf51",
"collection": "authors",
"collection_id": "fg24c-jmf51",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210520-145957441",
"type": "article",
"title": "Real-time discovery of AT2020xnd: a fast, luminous ultraviolet transient with minimal radioactive ejecta",
"author": [
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996",
"clpid": "Perley-Daniel-A"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Anderson",
"given_name": "Joseph P.",
"orcid": "0000-0003-0227-3451"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Kumar",
"given_name": "Harsh",
"orcid": "0000-0003-0871-4641"
},
{
"family_name": "Anupama",
"given_name": "G. C.",
"orcid": "0000-0003-3533-7183"
},
{
"family_name": "Barway",
"given_name": "Sudhanshu",
"orcid": "0000-0002-3927-5402"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Bhalerao",
"given_name": "Varun",
"orcid": "0000-0002-6112-7609"
},
{
"family_name": "Chen",
"given_name": "Ting-Wan",
"orcid": "0000-0002-1066-6098"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Galbany",
"given_name": "Llu\u00eds",
"orcid": "0000-0002-1296-6887"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Gromadzki",
"given_name": "Mariusz",
"orcid": "0000-0002-1650-1518"
},
{
"family_name": "Guti\u00e9rrez",
"given_name": "Claudia P.",
"orcid": "0000-0003-2375-2064"
},
{
"family_name": "Ihanec",
"given_name": "Nada"
},
{
"family_name": "Inserram",
"given_name": "Cosimo"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-James-D"
},
{
"family_name": "Nicholl",
"given_name": "Matt",
"orcid": "0000-0002-2555-3192"
},
{
"family_name": "Pursiainen",
"given_name": "Miika",
"orcid": "0000-0003-4663-4300"
},
{
"family_name": "van Roestel",
"given_name": "Joannes C.",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-Joannes"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard-S"
},
{
"family_name": "Wiseman",
"given_name": "Philip",
"orcid": "0000-0002-3073-1512"
}
],
"abstract": "The many unusual properties of the enigmatic AT2018cow suggested that at least some subset of the empirical class of fast blue optical transients (FBOTs) represents a genuinely new astrophysical phenomenon. Unfortunately, the intrinsic rarity and fleeting nature of these events have made it difficult to identify additional examples early enough to acquire the observations necessary to constrain theoretical models. We present here the Zwicky Transient Facility discovery of AT2020xnd (ZTF20acigmel, the 'Camel') at z = 0.243, the first unambiguous AT2018cow analogue to be found and confirmed in real time. AT2018cow and AT2020xnd share all key observational properties: a fast optical rise, sustained high photospheric temperature, absence of a second peak attributable to ejection of a radioactively heated stellar envelope, extremely luminous radio, millimetre, and X-ray emission, and a dwarf-galaxy host. This supports the argument that AT2018cow-like events represent a distinct phenomenon from slower-evolving radio-quiet supernovae, likely requiring a different progenitor or a different central engine. The sample properties of the four known members of this class to date disfavour tidal disruption models but are consistent with the alternative model of an accretion powered jet following the direct collapse of a massive star to a black hole. Contextual filtering of alert streams combined with rapid photometric verification using multiband imaging provides an efficient way to identify future members of this class, even at high redshift.",
"doi": "10.1093/mnras/stab2785",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2021-12",
"series_number": "4",
"volume": "508",
"issue": "4",
"pages": "5138-5147"
},
{
"id": "authors:j9b7y-est10",
"collection": "authors",
"collection_id": "j9b7y-est10",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211109-202833624",
"type": "article",
"title": "Faintest of Them All: ZTF 21aaoryiz/SN 2021fcg\u2014Discovery of an Extremely Low Luminosity Type Iax Supernova",
"author": [
{
"family_name": "Karambelkar",
"given_name": "Viraj R.",
"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj-R"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Maguire",
"given_name": "Kate",
"orcid": "0000-0002-9770-3508",
"clpid": "Maguire-Kate"
},
{
"family_name": "Anand",
"given_name": "Shreya G.",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya-G"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Drake",
"given_name": "Andrew",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877",
"clpid": "Kool-Erik-C"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Magee",
"given_name": "Mark R.",
"orcid": "0000-0002-0629-8931",
"clpid": "Magee-Mark-R"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-Ashish-A"
},
{
"family_name": "Medford",
"given_name": "Michael S.",
"orcid": "0000-0002-7226-0659",
"clpid": "Medford-Michael-S"
},
{
"family_name": "Perley",
"given_name": "Daniel",
"orcid": "0000-0001-8472-1996",
"clpid": "Perley-Daniel-A"
},
{
"family_name": "Rigault",
"given_name": "Mickael",
"orcid": "0000-0002-8121-2560",
"clpid": "Rigault-Mickael"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889",
"clpid": "Schulze-Steve"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-Jesper"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331",
"clpid": "Tzanidakis-Anastasios"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard-S"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
}
],
"abstract": "We present the discovery of ZTF 21aaoryiz/SN 2021fcg\u2014an extremely low luminosity Type Iax supernova. SN 2021fcg was discovered by the Zwicky Transient Facility in the star-forming galaxy IC0512 at a distance of \u224827 Mpc. It reached a peak absolute magnitude of M_r = \u221212.66 \u00b1 0.20 mag, making it the least luminous thermonuclear supernova discovered to date. The E(B \u2212 V) contribution from the underlying host galaxy is unconstrained. However, even if it were as large as 0.5 mag, the peak absolute magnitude would be M_r = \u221213.78 \u00b1 0.20 mag\u2014still consistent with being the lowest-luminosity SN. Optical spectra of SN 2021fcg taken at 37 and 65 days post-maximum show strong [Ca II], Ca II, and Na I D emission and several weak [Fe II] emission lines. The [Ca II] emission in the two spectra has extremely low velocities of \u22481300 and 1000 km s\u207b\u00b9, respectively. The spectra very closely resemble those of the very low luminosity Type Iax supernovae SN 2008 ha, SN 2010ae, and SN 2019gsc taken at similar phases. The peak bolometric luminosity of SN 2021fcg is \u2248 2.5^(+1.5)_(-0.3) x 10\u2074\u2070 erg s\u207b\u00b9, which is a factor of 3 lower than that for SN 2008 ha. The bolometric lightcurve of SN 2021fcg is consistent with a very low ejected nickel mass (M_(Ni) \u2248 0.8^(+0.4)_(-0.5) x 10\u207b\u00b3 M\u2299). The low luminosity and nickel mass of SN 2021fcg pose a challenge to the picture that low-luminosity SNe Iax originate from deflagrations of near-M_(ch) hybrid carbon\u2013oxygen\u2013neon white dwarfs. Instead, the merger of a carbon\u2013oxygen and oxygen\u2013neon white dwarf is a promising model to explain SN 2021fcg.",
"doi": "10.3847/2041-8213/ac2e90",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2021-11-01",
"series_number": "1",
"volume": "921",
"issue": "1",
"pages": "Art. No. L6"
},
{
"id": "authors:n5m70-jjt30",
"collection": "authors",
"collection_id": "n5m70-jjt30",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201209-113403455",
"type": "article",
"title": "The search for fast transients with CZTI",
"author": [
{
"family_name": "Sharma",
"given_name": "Y.",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Marathe",
"given_name": "A.",
"orcid": "0000-0002-8869-8137",
"clpid": "Marathe-Aditi"
},
{
"family_name": "Bhalerao",
"given_name": "V.",
"orcid": "0000-0002-6112-7609",
"clpid": "Bhalerao-Varun-B"
},
{
"family_name": "Shenoy",
"given_name": "V.",
"orcid": "0000-0002-6429-8139",
"clpid": "Shenoy-Vedant"
},
{
"family_name": "Waratkar",
"given_name": "G.",
"orcid": "0000-0003-3630-9440",
"clpid": "Waratkar-Gaurav"
},
{
"family_name": "Nadella",
"given_name": "D.",
"orcid": "0000-0003-4942-6873",
"clpid": "Nadella-Drishika"
},
{
"family_name": "Page",
"given_name": "P.",
"orcid": "0000-0002-8239-9670",
"clpid": "Page-Pranav"
},
{
"family_name": "Hebbar",
"given_name": "P.",
"orcid": "0000-0002-4961-4690",
"clpid": "Hebbar-Pavan-R"
},
{
"family_name": "Vibhute",
"given_name": "A.",
"orcid": "0000-0003-1501-6972",
"clpid": "Vibhute-Ajay"
},
{
"family_name": "Bhattacharya",
"given_name": "D.",
"orcid": "0000-0003-3352-3142",
"clpid": "Bhattacharya-Dipankar"
},
{
"family_name": "Rao",
"given_name": "A. R.",
"orcid": "0000-0003-0833-0533",
"clpid": "Rao-A-R"
},
{
"family_name": "Vadawale",
"given_name": "S.",
"orcid": "0000-0002-2050-0913",
"clpid": "Vadawale-Santosh-V"
}
],
"abstract": "The Cadmium\u2013Zinc\u2013Telluride Imager on AstroSat has proven to be a very effective All-Sky monitor in the hard X-ray regime, detecting over three hundred GRBs and putting highly competitive upper limits on X-ray emissions from gravitational wave sources and fast radio bursts. We present the algorithms used for searching for such transient sources in CZTI data, and for calculating upper limits in case of non-detections. We introduce CIFT: the CZTI Interface for Fast Transients, a framework used to streamline these processes. We present details of 87 new GRBs detected by this framework that were previously not detected in CZTI.",
"doi": "10.1007/s12036-021-09714-6",
"issn": "0250-6335",
"publisher": "Springer",
"publication": "Journal of Astrophysics and Astronomy",
"publication_date": "2021-10",
"series_number": "2",
"volume": "42",
"issue": "2",
"pages": "Art. No. 73"
},
{
"id": "authors:amhq5-48y04",
"collection": "authors",
"collection_id": "amhq5-48y04",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210520-150008009",
"type": "article",
"title": "SNIascore: Deep-learning Classification of Low-resolution Supernova Spectra",
"author": [
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Hall",
"given_name": "Xander J.",
"orcid": "0000-0002-9364-5419",
"clpid": "Hall-Xander-J"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924",
"clpid": "Coughlin-Michael-W"
},
{
"family_name": "Dahiwale",
"given_name": "Aishwarya S.",
"clpid": "Dahiwale-Aishwarya-S"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877",
"clpid": "Kool-Erik-C"
},
{
"family_name": "Mahabal",
"given_name": "Ashish A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X",
"clpid": "Miller-Adam-A"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-James-D"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996",
"clpid": "Perley-Daniel-A"
},
{
"family_name": "Rigault",
"given_name": "Mickael",
"orcid": "0000-0002-8121-2560",
"clpid": "Rigault-Mickael"
},
{
"family_name": "Rosnet",
"given_name": "Philippe",
"orcid": "0000-0002-6099-7565",
"clpid": "Rosnet-Philippe"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Shin",
"given_name": "Kyung Min",
"orcid": "0000-0002-1486-3582",
"clpid": "Shin-Kyung-Min"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-Jesper"
},
{
"family_name": "Walters",
"given_name": "Richard S.",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard-S"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
}
],
"abstract": "We present SNIascore, a deep-learning-based method for spectroscopic classification of thermonuclear supernovae (SNe Ia) based on very low-resolution (R ~ 100) data. The goal of SNIascore is the fully automated classification of SNe Ia with a very low false-positive rate (FPR) so that human intervention can be greatly reduced in large-scale SN classification efforts, such as that undertaken by the public Zwicky Transient Facility (ZTF) Bright Transient Survey (BTS). We utilize a recurrent neural network architecture with a combination of bidirectional long short-term memory and gated recurrent unit layers. SNIascore achieves a <0.6% FPR while classifying up to 90% of the low-resolution SN Ia spectra obtained by the BTS. SNIascore simultaneously performs binary classification and predicts the redshifts of secure SNe Ia via regression (with a typical uncertainty of <0.005 in the range from z = 0.01 to z = 0.12). For the magnitude-limited ZTF BTS survey (\u224870% SNe Ia), deploying SNIascore reduces the amount of spectra in need of human classification or confirmation by \u224860%. Furthermore, SNIascore allows SN Ia classifications to be automatically announced in real time to the public immediately following a finished observation during the night.",
"doi": "10.3847/2041-8213/ac116f",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2021-08-10",
"series_number": "1",
"volume": "917",
"issue": "1",
"pages": "Art. No. L2"
},
{
"id": "authors:wtn5h-r0e31",
"collection": "authors",
"collection_id": "wtn5h-r0e31",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200916-112927301",
"type": "article",
"title": "SN 2020bqj: A Type Ibn supernova with a long-lasting peak plateau",
"author": [
{
"family_name": "Kool",
"given_name": "E. C.",
"orcid": "0000-0002-7252-3877",
"clpid": "Kool-Erik-C"
},
{
"family_name": "Karamehmetoglu",
"given_name": "E.",
"orcid": "0000-0001-6209-838X"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Lunnan",
"given_name": "R.",
"orcid": "0000-0001-9454-4639"
},
{
"family_name": "Reynolds",
"given_name": "T. M."
},
{
"family_name": "Barbarino",
"given_name": "C.",
"orcid": "0000-0002-3821-6144"
},
{
"family_name": "Bellm",
"given_name": "E. C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "De",
"given_name": "K.",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Duev",
"given_name": "D. A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Fremling",
"given_name": "C.",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Golkhou",
"given_name": "V. Z.",
"orcid": "0000-0001-8205-2506"
},
{
"family_name": "Graham",
"given_name": "M. L.",
"orcid": "0000-0002-9154-3136"
},
{
"family_name": "Green",
"given_name": "D. A."
},
{
"family_name": "Horesh",
"given_name": "A.",
"orcid": "0000-0002-5936-1156"
},
{
"family_name": "Kaye",
"given_name": "S.",
"clpid": "Kaye-Stephen-M"
},
{
"family_name": "Kim",
"given_name": "Y.-L."
},
{
"family_name": "Laher",
"given_name": "R. R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Masci",
"given_name": "F. J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Nordin",
"given_name": "J."
},
{
"family_name": "Perley",
"given_name": "D. A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Phinney",
"given_name": "E. S.",
"orcid": "0000-0002-9656-4032",
"clpid": "Phinney-E-S"
},
{
"family_name": "Porter",
"given_name": "M.",
"orcid": "0000-0003-3168-5586",
"clpid": "Porter-Michael-D"
},
{
"family_name": "Reiley",
"given_name": "D.",
"clpid": "Reiley-Daniel-J"
},
{
"family_name": "Rodriguez",
"given_name": "H.",
"clpid": "Rodriguez-Hector"
},
{
"family_name": "van Roestel",
"given_name": "J.",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-Joannes-C"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Sharma",
"given_name": "Y.",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Sfaradi",
"given_name": "I."
},
{
"family_name": "Soumagnac",
"given_name": "M. T.",
"orcid": "0000-0001-6753-1488"
},
{
"family_name": "Taggart",
"given_name": "K.",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "Tartaglia",
"given_name": "L.",
"orcid": "0000-0003-3433-1492"
},
{
"family_name": "Williams",
"given_name": "D. R. A.",
"orcid": "0000-0001-7361-0246"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "Context. Type Ibn supernovae (SNe Ibn) are a rare class of stripped envelope supernovae interacting with a helium-rich circumstellar medium (CSM). The majority of the SNe Ibn reported in the literature display a surprising homogeneity in their fast-evolving lightcurves and are typically found in actively starforming spiral galaxies.\n\nAims. We present the discovery and the study of SN 2020bqj (ZTF20aalrqbu), a SN Ibn with a long-duration peak plateau lasting 40 days and hosted by a faint low-mass galaxy. We aim to explain its peculiar properties using an extensive photometric and spectroscopic data set.\n\nMethods. We compare the photometric and spectral evolution of SN 2020bqj with regular SNe Ibn from the literature, as well as with other outliers in the SN Ibn subclass. We fit the bolometric and multi-band lightcurves with powering mechanism models such as radioactive decay and CSM interaction. We also model the host galaxy of SN 2020bqj.\n\nResults. The risetime, peak magnitude and spectral features of SN 2020bqj are consistent with those of most SNe Ibn, but the SN is a clear outlier in the subclass based on its bright, long-lasting peak plateau and the low mass of its faint host galaxy. We show through modeling that the lightcurve of SN 2020bqj can be powered predominantly by shock heating from the interaction of the SN ejecta and a dense CSM, combined with radioactive decay. The peculiar Type Ibn SN 2011hw is a close analog to SN 2020bqj in terms of lightcurve and spectral evolution, suggesting a similar progenitor and CSM scenario. In this scenario a very massive progenitor star in the transitional phase between a luminous blue variable and a compact Wolf-Rayet star undergoes core-collapse, embedded in a dense helium-rich CSM with an elevated opacity compared to normal SNe Ibn, due to the presence of residual hydrogen. This scenario is consistent with the observed properties of SN 2020bqj and the modeling results.\n\nConclusions. SN 2020bqj is a compelling example of a transitional SN Ibn/IIn based on not only its spectral features, but also its lightcurve, host galaxy properties and the inferred progenitor properties. The strong similarity with SN 2011hw suggests this subclass may be the result of a progenitor in a stellar evolution phase that is distinct from those of progenitors of regular SNe Ibn.",
"doi": "10.1051/0004-6361/202039137",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2021-08",
"volume": "652",
"pages": "Art. No. A136"
},
{
"id": "authors:2jy02-s3v71",
"collection": "authors",
"collection_id": "2jy02-s3v71",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200916-112934888",
"type": "article",
"title": "A Large Fraction of Hydrogen-rich Supernova Progenitors Experience Elevated Mass Loss Shortly Prior to Explosion",
"author": [
{
"family_name": "Bruch",
"given_name": "Rachel J.",
"orcid": "0000-0001-8208-2473",
"clpid": "Bruch-Rachel-J"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Yaron",
"given_name": "Ofer",
"orcid": "0000-0002-0301-8017"
},
{
"family_name": "Yang",
"given_name": "Yi",
"orcid": "0000-0002-9024-4150"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane",
"orcid": "0000-0001-6753-1488"
},
{
"family_name": "Rigault",
"given_name": "Mickael",
"orcid": "0000-0002-8121-2560"
},
{
"family_name": "Strotjohann",
"given_name": "Nora L.",
"orcid": "0000-0002-4667-6730"
},
{
"family_name": "Ofek",
"given_name": "Eran O.",
"orcid": "0000-0002-6786-8774"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Barbarino",
"given_name": "Cristina",
"orcid": "0000-0002-3821-6144"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Perley",
"given_name": "Daniel",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Nordin",
"given_name": "Jakob",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "Adams",
"given_name": "S.",
"orcid": "0000-0001-5855-5939",
"clpid": "Adams-Scott-M"
},
{
"family_name": "Adreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Blagorodnova",
"given_name": "Nadia",
"orcid": "0000-0003-0901-1606"
},
{
"family_name": "Bulla",
"given_name": "Mattia",
"orcid": "0000-0002-8255-5127"
},
{
"family_name": "Burdge",
"given_name": "Kevin",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-Kevin-B"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Dhawan",
"given_name": "Suhail",
"orcid": "0000-0002-2376-6979"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Dugas",
"given_name": "Alison",
"orcid": "0000-0001-7344-0208",
"clpid": "Dugas-Alison-M"
},
{
"family_name": "Graham",
"given_name": "Matthew",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Graham",
"given_name": "Melissa L.",
"orcid": "0000-0002-9154-3136"
},
{
"family_name": "Irani",
"given_name": "Ido",
"orcid": "0000-0002-7996-8780",
"clpid": "Irani-Ido"
},
{
"family_name": "Jencson",
"given_name": "Jacob",
"orcid": "0000-0001-5754-4007",
"clpid": "Jencson-Jacob-E"
},
{
"family_name": "Karamehmetoglu",
"given_name": "Emir",
"orcid": "0000-0001-6209-838X"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kim",
"given_name": "Young-Lo",
"orcid": "0000-0002-1031-0796"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484"
},
{
"family_name": "Liang",
"given_name": "Jingyi",
"clpid": "Liang-Jingyi"
},
{
"family_name": "Mahabal",
"given_name": "Ashish",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-Ashish-A"
},
{
"family_name": "Miller",
"given_name": "A. A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Sharma",
"given_name": "Y.",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Smith",
"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
},
{
"family_name": "Taddia",
"given_name": "Francesco",
"orcid": "0000-0002-2387-6801",
"clpid": "Taddia-Francesco"
},
{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard-S"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "Spectroscopic detection of narrow emission lines traces the presence of circumstellar mass distributions around massive stars exploding as core-collapse supernovae. Transient emission lines disappearing shortly after the supernova explosion suggest that the material spatial extent is compact and implies an increased mass loss shortly prior to explosion. Here, we present a systematic survey for such transient emission lines (Flash Spectroscopy) among Type II supernovae detected in the first year of the Zwicky Transient Facility survey. We find that at least six out of ten events for which a spectrum was obtained within two days of the estimated explosion time show evidence for such transient flash lines. Our measured flash event fraction (>30% at 95% confidence level) indicates that elevated mass loss is a common process occurring in massive stars that are about to explode as supernovae.",
"doi": "10.3847/1538-4357/abef05",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2021-05-01",
"series_number": "1",
"volume": "912",
"issue": "1",
"pages": "Art. No. 46"
},
{
"id": "authors:55882-yhy85",
"collection": "authors",
"collection_id": "55882-yhy85",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200414-075012273",
"type": "article",
"title": "Seventeen Tidal Disruption Events from the First Half of ZTF Survey Observations: Entering a New Era of Population Studies",
"author": [
{
"family_name": "van Velzen",
"given_name": "Sjoert",
"orcid": "0000-0002-3859-8074",
"clpid": "van-Velzen-Sjoert"
},
{
"family_name": "Gezari",
"given_name": "Suvi",
"orcid": "0000-0003-3703-5154"
},
{
"family_name": "Hammerstein",
"given_name": "Erica",
"orcid": "0000-0002-5698-8703"
},
{
"family_name": "Roth",
"given_name": "Nathaniel",
"orcid": "0000-0002-6485-2259"
},
{
"family_name": "Frederick",
"given_name": "Sara",
"orcid": "0000-0001-9676-730X"
},
{
"family_name": "Ward",
"given_name": "Charlotte",
"orcid": "0000-0002-4557-6682"
},
{
"family_name": "Hung",
"given_name": "Tiara",
"orcid": "0000-0002-9878-7889"
},
{
"family_name": "Cenko",
"given_name": "S. Bradley",
"orcid": "0000-0003-1673-970X"
},
{
"family_name": "Stein",
"given_name": "Robert",
"orcid": "0000-0003-2434-0387"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "Foley",
"given_name": "Ryan J."
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Blagorodnova",
"given_name": "Nadejda",
"orcid": "0000-0003-0901-1606"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Brinnel",
"given_name": "Valery"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard-G"
},
{
"family_name": "Feeney",
"given_name": "Michael",
"clpid": "Feeney-Michael-E"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Giomi",
"given_name": "Matteo"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kilpatrick",
"given_name": "Charles D.",
"orcid": "0000-0002-5740-7747"
},
{
"family_name": "Kulkarni",
"given_name": "Shrinivas R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Mahabal",
"given_name": "Ashish",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-Ashish-A"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Nordin",
"given_name": "Jakob",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "van Santen",
"given_name": "Jakob"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488"
}
],
"abstract": "While tidal disruption events (TDEs) have long been heralded as laboratories for the study of quiescent black holes, the small number of known TDEs and uncertainties in their emission mechanism have hindered progress toward this promise. Here we present 17 new TDEs that have been detected recently by the Zwicky Transient Facility along with Swift UV and X-ray follow-up observations. Our homogeneous analysis of the optical/UV light curves, including 22 previously known TDEs from the literature, reveals a clean separation of light-curve properties with spectroscopic class. The TDEs with Bowen fluorescence features in their optical spectra have smaller blackbody radii, lower optical luminosities, and higher disruption rates compared to the rest of the sample. The small subset of TDEs that show only helium emission lines in their spectra have the longest rise times, the highest luminosities, and the lowest rates. A high detection rate of Bowen lines in TDEs with small photometric radii could be explained by the high density that is required for this fluorescence mechanism. The stellar debris can provide a source for this dense material. Diffusion of photons through this debris may explain why the rise and fade timescale of the TDEs in our sample are not correlated. We also report, for the first time, the detection of soft X-ray flares from a TDE on ~day timescales. Based on the fact that the X-ray flares peak at a luminosity similar to the optical/UV blackbody luminosity, we attribute them to brief glimpses through a reprocessing layer that otherwise obscures the inner accretion flow.",
"doi": "10.3847/1538-4357/abc258",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2021-02-10",
"series_number": "1",
"volume": "908",
"issue": "1",
"pages": "Art. No. 4"
},
{
"id": "authors:6d951-rq497",
"collection": "authors",
"collection_id": "6d951-rq497",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210204-105727688",
"type": "article",
"title": "Bright, Months-long Stellar Outbursts Announce the Explosion of Interaction-powered Supernovae",
"author": [
{
"family_name": "Strotjohann",
"given_name": "Nora L.",
"orcid": "0000-0002-4667-6730",
"clpid": "Strotjohann-Nora-L"
},
{
"family_name": "Ofek",
"given_name": "Eran O.",
"orcid": "0000-0002-6786-8774"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Bruch",
"given_name": "Rachel J.",
"orcid": "0000-0001-8208-2473"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Shaviv",
"given_name": "Nir",
"orcid": "0000-0003-3894-8422"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Filippenko",
"given_name": "Alexei V.",
"orcid": "0000-0003-3460-0103"
},
{
"family_name": "Yaron",
"given_name": "Ofer",
"orcid": "0000-0002-0301-8017"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Nordin",
"given_name": "Jakob",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877"
},
{
"family_name": "Perley",
"given_name": "Dan A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Yang",
"given_name": "Yi"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488"
},
{
"family_name": "Graham",
"given_name": "Melissa L.",
"orcid": "0000-0002-9154-3136"
},
{
"family_name": "Barbarino",
"given_name": "Cristina",
"orcid": "0000-0002-3821-6144"
},
{
"family_name": "Tartaglia",
"given_name": "Leonardo",
"orcid": "0000-0003-3433-1492"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Goldstein",
"given_name": "Daniel A.",
"orcid": "0000-0003-3461-8661",
"clpid": "Goldstein-Daniel-A"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Brink",
"given_name": "Thomas G.",
"orcid": "0000-0001-5955-2502"
},
{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558"
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{
"family_name": "Yan",
"given_name": "Lin",
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"clpid": "Yan-Lin"
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{
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{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
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{
"family_name": "Kulkarni",
"given_name": "Shri R.",
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{
"family_name": "Nugent",
"given_name": "Peter E.",
"orcid": "0000-0002-3389-0586"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Rosnet",
"given_name": "Philippe",
"orcid": "0000-0002-6099-7565"
},
{
"family_name": "Adams",
"given_name": "Scott M.",
"orcid": "0000-0001-5855-5939",
"clpid": "Adams-Scott-M"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Bagdasaryan",
"given_name": "Ashot",
"clpid": "Bagdasaryan-Ashot"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Burdge",
"given_name": "Kevin",
"orcid": "0000-0002-7226-836X",
"clpid": "Burdge-Kevin-B"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Dugas",
"given_name": "Alison",
"orcid": "0000-0001-7344-0208",
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{
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"given_name": "Sara",
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{
"family_name": "Goldwasser",
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{
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"orcid": "0000-0002-6540-1484"
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{
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"given_name": "James D.",
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{
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"given_name": "Michael",
"orcid": "0000-0003-3168-5586",
"clpid": "Porter-Michael-D"
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{
"family_name": "Riddle",
"given_name": "Reed L.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
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{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
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},
{
"family_name": "Short",
"given_name": "Phil",
"orcid": "0000-0002-5096-9464"
},
{
"family_name": "Taddia",
"given_name": "Francesco",
"orcid": "0000-0002-2387-6801"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331",
"clpid": "Tzanidakis-Anastasios"
},
{
"family_name": "van Roestel",
"given_name": "Jan",
"orcid": "0000-0002-2626-2872",
"clpid": "van-Roestel-Jan"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard-S"
},
{
"family_name": "Zhuang",
"given_name": "Zhuyun",
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],
"abstract": "Interaction-powered supernovae (SNe) explode within an optically thick circumstellar medium (CSM) that could be ejected during eruptive events. To identify and characterize such pre-explosion outbursts, we produce forced-photometry light curves for 196 interacting SNe, mostly of Type IIn, detected by the Zwicky Transient Facility between early 2018 and 2020 June. Extensive tests demonstrate that we only expect a few false detections among the 70,000 analyzed pre-explosion images after applying quality cuts and bias corrections. We detect precursor eruptions prior to 18 Type IIn SNe and prior to the Type Ibn SN 2019uo. Precursors become brighter and more frequent in the last months before the SN and month-long outbursts brighter than magnitude \u221213 occur prior to 25% (5\u201369%, 95% confidence range) of all Type IIn SNe within the final three months before the explosion. With radiative energies of up to 10\u2074\u2079 erg, precursors could eject ~1 M\u2299 of material. Nevertheless, SNe with detected precursors are not significantly more luminous than other SNe IIn, and the characteristic narrow hydrogen lines in their spectra typically originate from earlier, undetected mass-loss events. The long precursor durations require ongoing energy injection, and they could, for example, be powered by interaction or by a continuum-driven wind. Instabilities during the neon- and oxygen-burning phases are predicted to launch precursors in the final years to months before the explosion; however, the brightest precursor is 100 times more energetic than anticipated.",
"doi": "10.3847/1538-4357/abd032",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2021-02-01",
"series_number": "2",
"volume": "907",
"issue": "2",
"pages": "Art. No. 99"
},
{
"id": "authors:7kye6-p1375",
"collection": "authors",
"collection_id": "7kye6-p1375",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210202-121536995",
"type": "article",
"title": "Is supernova SN 2020faa an iPTF14hls look-alike?",
"author": [
{
"family_name": "Yang",
"given_name": "S.",
"clpid": "Yang-Sheng"
},
{
"family_name": "Sollerman",
"given_name": "J.",
"orcid": "0000-0003-1546-6615",
"clpid": "Sollerman-Jesper"
},
{
"family_name": "Chen",
"given_name": "T.-W.",
"orcid": "0000-0002-1066-6098",
"clpid": "Chen-Ting-Wan"
},
{
"family_name": "Kool",
"given_name": "E. C.",
"orcid": "0000-0002-7252-3877",
"clpid": "Kool-Erik-C"
},
{
"family_name": "Lunnan",
"given_name": "R.",
"orcid": "0000-0001-9454-4639",
"clpid": "Lunnan-Ragnhild"
},
{
"family_name": "Schulze",
"given_name": "S.",
"orcid": "0000-0001-6797-1889",
"clpid": "Schulze-Steve"
},
{
"family_name": "Strotjohann",
"given_name": "N.",
"orcid": "0000-0002-4667-6730",
"clpid": "Strotjohann-Nora-Linn"
},
{
"family_name": "Horesh",
"given_name": "A.",
"orcid": "0000-0002-5936-1156",
"clpid": "Horesh-Assaf"
},
{
"family_name": "Kasliwal",
"given_name": "M. M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kupfer",
"given_name": "T.",
"orcid": "0000-0002-6540-1484",
"clpid": "Kupfer-Thomas"
},
{
"family_name": "Mahabal",
"given_name": "A. A.",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-Ashish-A"
},
{
"family_name": "Masci",
"given_name": "F. J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Nugent",
"given_name": "P.",
"orcid": "0000-0002-3389-0586",
"clpid": "Nugent-Peter-E"
},
{
"family_name": "Perley",
"given_name": "D. A.",
"orcid": "0000-0001-8472-1996",
"clpid": "Perley-Daniel-A"
},
{
"family_name": "Riddle",
"given_name": "R.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Sharma",
"given_name": "Y.",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
}
],
"abstract": "Context. We present observations of ZTF20aatqesi (SN 2020faa). This Type II supernova (SN) displays a luminous light curve (LC) that started to rebrighten from an initial decline. We investigate this in relation to the famous SN iPTF14hls, which received a great deal of attention and multiple interpretations in the literature, but whose nature and source of energy still remain unknown. \n\nAims. We demonstrate the great similarity between SN 2020faa and iPTF14hls during the first 6 months, and use this comparison to forecast the evolution of SN 2020faa and to reflect on the less well observed early evolution of iPTF14hls. \n\nMethods. We present and analyse our observational data, consisting mainly of optical LCs from the Zwicky Transient Facility in the gri bands and of a sequence of optical spectra. We construct colour curves and a bolometric lc, and we compare ejecta-velocity and black-body radius evolutions for the two supernovae (SNe) and for more typical Type II SNe. \n\nResults. The LCs show a great similarity with those of iPTF14hls over the first 6 months in luminosity, timescale, and colour. In addition, the spectral evolution of SN 2020faa is that of a Type II SN, although it probes earlier epochs than those available for iPTF14hls. \n\nConclusions. The similar LC behaviour is suggestive of SN 2020faa being a new iPTF14hls. We present these observations now to advocate follow-up observations, since most of the more striking evolution of SN iPTF14hls came later, with LC undulations and a spectacular longevity. On the other hand, for SN 2020faa we have better constraints on the explosion epoch than we had for iPTF14hls, and we have been able to spectroscopically monitor it from earlier phases than was done for the more famous sibling.",
"doi": "10.1051/0004-6361/202039440",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2021-02",
"volume": "646",
"pages": "Art. No. 22"
},
{
"id": "authors:5h3j9-apc36",
"collection": "authors",
"collection_id": "5h3j9-apc36",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200824-085517593",
"type": "article",
"title": "Kilonova Luminosity Function Constraints Based on Zwicky Transient Facility Searches for 13 Neutron Star Merger Triggers during O3",
"author": [
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
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{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
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},
{
"family_name": "Ahumada",
"given_name": "Tom\u00e1s",
"orcid": "0000-0002-2184-6430"
},
{
"family_name": "Stein",
"given_name": "Robert",
"orcid": "0000-0003-2434-0387"
},
{
"family_name": "Sagu\u00e9s Carracedo",
"given_name": "Ana"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
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{
"family_name": "Singer",
"given_name": "Leo P.",
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{
"family_name": "Kool",
"given_name": "Erik C.",
"orcid": "0000-0002-7252-3877"
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{
"family_name": "De",
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"orcid": "0000-0002-8989-0542",
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{
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{
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{
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{
"family_name": "Perley",
"given_name": "Daniel A.",
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"given_name": "David L.",
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{
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"given_name": "Joshua S.",
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"given_name": "Maria D.",
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{
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{
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{
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"given_name": "Kunal P.",
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"family_name": "Duev",
"given_name": "Dmitry A.",
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{
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{
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{
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{
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{
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"orcid": "0000-0003-2758-159X",
"clpid": "Karambelkar-Viraj-R"
},
{
"family_name": "Kong",
"given_name": "Albert K. H.",
"orcid": "0000-0002-5105-344X"
},
{
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"given_name": "Marek"
},
{
"family_name": "Khandagale",
"given_name": "Maitreya"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kumar",
"given_name": "Brajesh"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Li",
"given_name": "K. L.",
"orcid": "0000-0001-8229-2024"
},
{
"family_name": "Mahabal",
"given_name": "Ashish",
"orcid": "0000-0003-2242-0244",
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},
{
"family_name": "Masci",
"given_name": "Frank J.",
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"clpid": "Masci-Frank-J"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Mogotsi",
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},
{
"family_name": "Mohite",
"given_name": "Siddharth"
},
{
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"given_name": "Kunal",
"orcid": "0000-0002-2557-5180",
"clpid": "Mooley-Kunal-Prakash"
},
{
"family_name": "Mr\u00f3z",
"given_name": "Przemek",
"orcid": "0000-0001-7016-1692",
"clpid": "Mr\u00f3z-Przemek"
},
{
"family_name": "Newman",
"given_name": "Jeffrey A.",
"orcid": "0000-0001-8684-2222"
},
{
"family_name": "Ngeow",
"given_name": "Chow-Choong",
"orcid": "0000-0001-8771-7554"
},
{
"family_name": "Oates",
"given_name": "Samantha R.",
"orcid": "0000-0001-9309-7873"
},
{
"family_name": "Patil",
"given_name": "Atharva Sunil"
},
{
"family_name": "Pandey",
"given_name": "Shashi B."
},
{
"family_name": "Pavana",
"given_name": "M."
},
{
"family_name": "Pian",
"given_name": "Elena",
"orcid": "0000-0001-8646-4858"
},
{
"family_name": "Riddle",
"given_name": "Reed",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Sanchez-Ram\u0131rez",
"given_name": "Ruben",
"orcid": "0000-0002-7158-5099"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Singh",
"given_name": "Avinash"
},
{
"family_name": "Smith",
"given_name": "Roger",
"orcid": "0000-0001-7062-9726",
"clpid": "Smith-R-M"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488"
},
{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558"
},
{
"family_name": "Tan",
"given_name": "Hanjie"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331",
"clpid": "Tzanidakis-Anastasios"
},
{
"family_name": "Troja",
"given_name": "Eleonora",
"orcid": "0000-0002-1869-7817"
},
{
"family_name": "Valeev",
"given_name": "Azamat F.",
"orcid": "0000-0003-3513-3527"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard"
},
{
"family_name": "Waratkar",
"given_name": "Gaurav",
"orcid": "0000-0003-3630-9440"
},
{
"family_name": "Webb",
"given_name": "Sara",
"orcid": "0000-0003-2601-1472"
},
{
"family_name": "Yu",
"given_name": "Po-Chieh",
"orcid": "0000-0001-8894-0854"
},
{
"family_name": "Zhang",
"given_name": "Bin-Bin"
},
{
"family_name": "Zhou",
"given_name": "Rongpu",
"orcid": "0000-0001-5381-4372"
},
{
"family_name": "Zolkower",
"given_name": "Jeffry",
"clpid": "Zolkower-Jeffry"
}
],
"abstract": "We present a systematic search for optical counterparts to 13 gravitational wave (GW) triggers involving at least one neutron star during LIGO/Virgo's third observing run (O3). We searched binary neutron star (BNS) and neutron star black hole (NSBH) merger localizations with the Zwicky Transient Facility (ZTF) and undertook follow-up with the Global Relay of Observatories Watching Transients Happen (GROWTH) collaboration. The GW triggers had a median localization area of 4480 deg\u00b2, a median distance of 267 Mpc, and false-alarm rates ranging from 1.5 to 10\u207b\u00b2\u2075 yr\u207b\u00b9. The ZTF coverage in the g and r bands had a median enclosed probability of 39%, median depth of 20.8 mag, and median time lag between merger and the start of observations of 1.5 hr. The O3 follow-up by the GROWTH team comprised 340 UltraViolet/Optical/InfraRed (UVOIR) photometric points, 64 OIR spectra, and three radio images using 17 different telescopes. We find no promising kilonovae (radioactivity-powered counterparts), and we show how to convert the upper limits to constrain the underlying kilonova luminosity function. Initially, we assume that all GW triggers are bona fide astrophysical events regardless of false-alarm rate and that kilonovae accompanying BNS and NSBH mergers are drawn from a common population; later, we relax these assumptions. Assuming that all kilonovae are at least as luminous as the discovery magnitude of GW170817 (\u221216.1 mag), we calculate that our joint probability of detecting zero kilonovae is only 4.2%. If we assume that all kilonovae are brighter than \u221216.6 mag (the extrapolated peak magnitude of GW170817) and fade at a rate of 1 mag day\u207b\u00b9 (similar to GW170817), the joint probability of zero detections is 7%. If we separate the NSBH and BNS populations based on the online classifications, the joint probability of zero detections, assuming all kilonovae are brighter than \u221216.6 mag, is 9.7% for NSBH and 7.9% for BNS mergers. Moreover, no more than <57% (<89%) of putative kilonovae could be brighter than \u221216.6 mag assuming flat evolution (fading by 1 mag day\u207b\u00b9) at the 90% confidence level. If we further take into account the online terrestrial probability for each GW trigger, we find that no more than <68% of putative kilonovae could be brighter than \u221216.6 mag. Comparing to model grids, we find that some kilonovae must have M_(ej) < 0.03 M_\u2299, X_(lan) > 10\u207b\u2074, or \u03c6 > 30\u00b0 to be consistent with our limits. We look forward to searches in the fourth GW observing run; even 17 neutron star mergers with only 50% coverage to a depth of \u221216 mag would constrain the maximum fraction of bright kilonovae to <25%.",
"doi": "10.3847/1538-4357/abc335",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-12-20",
"series_number": "2",
"volume": "905",
"issue": "2",
"pages": "Art. No. 145"
},
{
"id": "authors:0z0sc-hap43",
"collection": "authors",
"collection_id": "0z0sc-hap43",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200604-151423784",
"type": "article",
"title": "The Zwicky Transient Facility Census of the Local Universe. I. Systematic Search for Calcium-rich Gap Transients Reveals Three Related Spectroscopic Subclasses",
"author": [
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331",
"clpid": "Tzanidakis-Anastasios"
},
{
"family_name": "Fremling",
"given_name": "U. Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-Christoffer"
},
{
"family_name": "Adams",
"given_name": "Scott",
"orcid": "0000-0001-5855-5939",
"clpid": "Adams-Scott-M"
},
{
"family_name": "Aloisi",
"given_name": "Robert",
"orcid": "0000-0003-2822-616X"
},
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-Igor"
},
{
"family_name": "Bagdasaryan",
"given_name": "Ashot",
"clpid": "Bagdasaryan-Ashot"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Bildsten",
"given_name": "Lars"
},
{
"family_name": "Cannella",
"given_name": "Christopher",
"orcid": "0000-0003-2667-7290",
"clpid": "Cannella-Christopher-B"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-David-O"
},
{
"family_name": "Delacroix",
"given_name": "Alexandre",
"clpid": "Delacroix-Alexandre"
},
{
"family_name": "Drake",
"given_name": "Andrew",
"clpid": "Drake-Andrew-J"
},
{
"family_name": "Duev",
"given_name": "Dmitry",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-Dmitry-A"
},
{
"family_name": "Dugas",
"given_name": "Alison",
"clpid": "Dugas-Alison-M"
},
{
"family_name": "Frederick",
"given_name": "Sara",
"orcid": "0000-0001-9676-730X"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Goldstein",
"given_name": "Daniel",
"orcid": "0000-0003-3461-8661",
"clpid": "Goldstein-Daniel-A"
},
{
"family_name": "Golkhou",
"given_name": "V. Zach",
"orcid": "0000-0001-8205-2506"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Hale",
"given_name": "David",
"clpid": "Hale-David-D-S"
},
{
"family_name": "Hankins",
"given_name": "Matthew",
"orcid": "0000-0001-9315-8437",
"clpid": "Hankins-Matthew-J"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Irani",
"given_name": "Ido",
"orcid": "0000-0002-7996-8780"
},
{
"family_name": "Jencson",
"given_name": "Jacob E.",
"orcid": "0000-0001-5754-4007"
},
{
"family_name": "Kaplan",
"given_name": "David L.",
"orcid": "0000-0001-6295-2881"
},
{
"family_name": "Kaye",
"given_name": "Stephen",
"clpid": "Kaye-Stephen"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Kupfer",
"given_name": "Thomas",
"orcid": "0000-0002-6540-1484"
},
{
"family_name": "Laher",
"given_name": "Russ R.",
"orcid": "0000-0003-2451-5482",
"clpid": "Laher-Russ-R"
},
{
"family_name": "Leadbeater",
"given_name": "Robin"
},
{
"family_name": "Lunnan",
"given_name": "Ragnhild",
"orcid": "0000-0001-9454-4639",
"clpid": "Lunnan-Ragnhild"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-Frank-J"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-James-D"
},
{
"family_name": "Ofek",
"given_name": "Eran O.",
"orcid": "0000-0002-6786-8774"
},
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996"
},
{
"family_name": "Polin",
"given_name": "Abigail",
"orcid": "0000-0002-1633-6495"
},
{
"family_name": "Prince",
"given_name": "Thomas A.",
"orcid": "0000-0002-8850-3627",
"clpid": "Prince-T-A"
},
{
"family_name": "Quataert",
"given_name": "Eliot",
"orcid": "0000-0001-9185-5044"
},
{
"family_name": "Reiley",
"given_name": "Dan",
"clpid": "Reiley-Daniel-J"
},
{
"family_name": "Riddle",
"given_name": "Reed L.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-Reed-L"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Shupe",
"given_name": "David L.",
"orcid": "0000-0003-4401-0430",
"clpid": "Shupe-David-L"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Tartaglia",
"given_name": "Leonardo",
"orcid": "0000-0003-3433-1492"
},
{
"family_name": "Walters",
"given_name": "Richard",
"orcid": "0000-0002-1835-6078",
"clpid": "Walters-Richard"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Yao",
"given_name": "Yuhan",
"orcid": "0000-0001-6747-8509",
"clpid": "Yao-Yuhan"
}
],
"abstract": "Using the Zwicky Transient Facility alert stream, we are conducting a large spectroscopic campaign to construct a complete, volume-limited sample of transients brighter than 20 mag, and coincident within 100\" of galaxies in the Census of the Local Universe catalog. We describe the experiment design and spectroscopic completeness from the first 16 months of operations, which have classified 754 supernovae. We present results from a systematic search for calcium-rich gap transients in the sample of 22 low-luminosity (peak absolute magnitude M > \u221217), hydrogen-poor events found in the experiment. We report the detection of eight new events, and constrain their volumetric rate to \u2273 15% \u00b1 5% of the SN Ia rate. Combining this sample with 10 previously known events, we find a likely continuum of spectroscopic properties ranging from events with SN Ia\u2013like features (Ca-Ia objects) to those with SN Ib/c\u2013like features (Ca-Ib/c objects) at peak light. Within the Ca-Ib/c events, we find two populations distinguished by their red (g \u2212 r \u2248 1.5 mag) or green (g - r \u2248 0.5 mag) colors at the r-band peak, wherein redder events show strong line blanketing features and slower light curves (similar to Ca-Ia objects), weaker He lines, and lower [Ca ii]/[O i] in the nebular phase. We find that all together the spectroscopic continuum, volumetric rates, and striking old environments are consistent with the explosive burning of He shells on low-mass white dwarfs. We suggest that Ca-Ia and red Ca-Ib/c objects arise from the double detonation of He shells, while green Ca-Ib/c objects are consistent with low-efficiency burning scenarios like detonations in low-density shells or deflagrations.",
"doi": "10.3847/1538-4357/abb45c",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-12-10",
"series_number": "1",
"volume": "905",
"issue": "1",
"pages": "Art. No. 58"
},
{
"id": "authors:sbjdg-gc417",
"collection": "authors",
"collection_id": "sbjdg-gc417",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200916-112938445",
"type": "article",
"title": "The Zwicky Transient Facility Bright Transient Survey. II. A Public Statistical Sample for Exploring Supernova Demographics",
"author": [
{
"family_name": "Perley",
"given_name": "Daniel A.",
"orcid": "0000-0001-8472-1996",
"clpid": "Perley-D-A"
},
{
"family_name": "Fremling",
"given_name": "Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Sollerman",
"given_name": "Jesper",
"orcid": "0000-0003-1546-6615"
},
{
"family_name": "Miller",
"given_name": "Adam A.",
"orcid": "0000-0001-9515-478X"
},
{
"family_name": "Dahiwale",
"given_name": "Aishwarya S.",
"clpid": "Dahiwale-Aishwarya-S"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Bellm",
"given_name": "Eric C.",
"orcid": "0000-0001-8018-5348"
},
{
"family_name": "Biswas",
"given_name": "Rahul",
"orcid": "0000-0002-5741-7195"
},
{
"family_name": "Brink",
"given_name": "Thomas G.",
"orcid": "0000-0001-5955-2502"
},
{
"family_name": "Bruch",
"given_name": "Rachel J.",
"orcid": "0000-0001-8208-2473"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Dekany",
"given_name": "Richard",
"orcid": "0000-0002-5884-7867",
"clpid": "Dekany-Richard"
},
{
"family_name": "Drake",
"given_name": "Andrew J.",
"clpid": "Drake-A-J"
},
{
"family_name": "Duev",
"given_name": "Dmitry A.",
"orcid": "0000-0001-5060-8733",
"clpid": "Duev-D-A"
},
{
"family_name": "Filippenko",
"given_name": "Alexei V.",
"orcid": "0000-0003-3460-0103"
},
{
"family_name": "Gal-Yam",
"given_name": "Avishay",
"orcid": "0000-0002-3653-5598"
},
{
"family_name": "Goobar",
"given_name": "Ariel",
"orcid": "0000-0002-4163-4996"
},
{
"family_name": "Graham",
"given_name": "Matthew J.",
"orcid": "0000-0002-3168-0139",
"clpid": "Graham-M-J"
},
{
"family_name": "Graham",
"given_name": "Melissa L.",
"orcid": "0000-0002-9154-3136"
},
{
"family_name": "Ho",
"given_name": "Anna Y. Q.",
"orcid": "0000-0002-9017-3567",
"clpid": "Ho-Anna-Y-Q"
},
{
"family_name": "Irani",
"given_name": "Ido",
"orcid": "0000-0002-7996-8780"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "Kim",
"given_name": "Young-Lo",
"orcid": "0000-0002-1031-0796"
},
{
"family_name": "Kulkarni",
"given_name": "S. R.",
"orcid": "0000-0001-5390-8563",
"clpid": "Kulkarni-S-R"
},
{
"family_name": "Mahabal",
"given_name": "Ashish",
"orcid": "0000-0003-2242-0244",
"clpid": "Mahabal-A-A"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Modak",
"given_name": "Shaunak",
"orcid": "0000-0002-8532-827X"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-J-D"
},
{
"family_name": "Nordin",
"given_name": "Jakob",
"orcid": "0000-0001-8342-6274"
},
{
"family_name": "Riddle",
"given_name": "Reed L.",
"orcid": "0000-0002-0387-370X",
"clpid": "Riddle-R-L"
},
{
"family_name": "Soumagnac",
"given_name": "Maayane T.",
"orcid": "0000-0001-6753-1488"
},
{
"family_name": "Strotjohann",
"given_name": "Nora L.",
"orcid": "0000-0002-4667-6730"
},
{
"family_name": "Schulze",
"given_name": "Steve",
"orcid": "0000-0001-6797-1889"
},
{
"family_name": "Taggart",
"given_name": "Kirsty",
"orcid": "0000-0002-5748-4558",
"clpid": "Taggart-Kirsty"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331",
"clpid": "Tzanidakis-A"
},
{
"family_name": "Walters",
"given_name": "Richard",
"clpid": "Walters-Richard-S"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "We present a public catalog of transients from the Zwicky Transient Facility (ZTF) Bright Transient Survey, a magnitude-limited (m < 19 mag in either the g or r filter) survey for extragalactic transients in the ZTF public stream. We introduce cuts on survey coverage, sky visibility around peak light, and other properties unconnected to the nature of the transient, and show that the resulting statistical sample is spectroscopically 97% complete at <18 mag, 93% complete at <18.5 mag, and 75% complete at <19 mag. We summarize the fundamental properties of this population, identifying distinct duration\u2013luminosity correlations in a variety of supernova (SN) classes and associating the majority of fast optical transients with well-established spectroscopic SN types (primarily SN Ibn and II/IIb). We measure the Type Ia SN and core-collapse (CC) SN rates and luminosity functions, which show good consistency with recent work. About 7% of CC SNe explode in very low-luminosity galaxies (M_i > \u221216 mag), 10% in red-sequence galaxies, and 1% in massive ellipticals. We find no significant difference in the luminosity or color distributions between the host galaxies of SNe Type II and SNe Type Ib/c, suggesting that line-driven wind stripping does not play a major role in the loss of the hydrogen envelope from their progenitors. Future large-scale classification efforts with ZTF and other wide-area surveys will provide high-quality measurements of the rates, properties, and environments of all known types of optical transients and limits on the existence of theoretically predicted but as yet unobserved explosions.",
"doi": "10.3847/1538-4357/abbd98",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-11-20",
"series_number": "1",
"volume": "904",
"issue": "1",
"pages": "Art. No. 35"
},
{
"id": "authors:t228f-t9m83",
"collection": "authors",
"collection_id": "t228f-t9m83",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191120-134817021",
"type": "article",
"title": "GROWTH on S190814bv: Deep Synoptic Limits on the Optical/Near-Infrared Counterpart to a Neutron Star-Black Hole Merger",
"author": [
{
"family_name": "Andreoni",
"given_name": "Igor",
"orcid": "0000-0002-8977-1498",
"clpid": "Andreoni-I"
},
{
"family_name": "Goldstein",
"given_name": "Daniel A.",
"orcid": "0000-0003-3461-8661",
"clpid": "Goldstein-D-A"
},
{
"family_name": "Kasliwal",
"given_name": "Mansi M.",
"orcid": "0000-0002-5619-4938",
"clpid": "Kasliwal-M-M"
},
{
"family_name": "De",
"given_name": "Kishalay",
"orcid": "0000-0002-8989-0542",
"clpid": "De-Kishalay"
},
{
"family_name": "Jencson",
"given_name": "Jacob E.",
"orcid": "0000-0001-5754-4007",
"clpid": "Jencson-J-E"
},
{
"family_name": "Anand",
"given_name": "Shreya",
"orcid": "0000-0003-3768-7515",
"clpid": "Anand-Shreya"
},
{
"family_name": "Coughlin",
"given_name": "Michael W.",
"orcid": "0000-0002-8262-2924",
"clpid": "Coughlin-M-W"
},
{
"family_name": "Karambelkar",
"given_name": "Viraj R.",
"clpid": "Karambelkar-V-R"
},
{
"family_name": "Sharma",
"given_name": "Yashvi",
"orcid": "0000-0003-4531-1745",
"clpid": "Sharma-Yashvi"
},
{
"family_name": "Fremling",
"given_name": "U. Christoffer",
"orcid": "0000-0002-4223-103X",
"clpid": "Fremling-C"
},
{
"family_name": "Bagdasaryan",
"given_name": "Ashot",
"clpid": "Bagdasaryan-A"
},
{
"family_name": "Dahiwale",
"given_name": "Aishwarya",
"clpid": "Dahiwale-A-S"
},
{
"family_name": "Hankins",
"given_name": "Matthew",
"orcid": "0000-0001-9315-8437",
"clpid": "Hankins-M-J"
},
{
"family_name": "Tzanidakis",
"given_name": "Anastasios",
"orcid": "0000-0003-0484-3331",
"clpid": "Tzanidakis-A"
},
{
"family_name": "Cook",
"given_name": "David O.",
"orcid": "0000-0002-6877-7655",
"clpid": "Cook-D-O"
}
],
"abstract": "On 2019 August 14, the Advanced LIGO and Virgo interferometers detected the high-significance gravitational wave (GW) signal S190814bv. The GW data indicated that the event resulted from a neutron star\u2013black hole (NSBH) merger, or potentially a low-mass binary BH merger. Due to the low false-alarm rate and the precise localization (23 deg2 at 90%), S190814bv presented the community with the best opportunity yet to directly observe an optical/near-infrared counterpart to an NSBH merger. To search for potential counterparts, the GROWTH Collaboration performed real-time image subtraction on six nights of public Dark Energy Camera images acquired in the 3 weeks following the merger, covering >98% of the localization probability. Using a worldwide network of follow-up facilities, we systematically undertook spectroscopy and imaging of optical counterpart candidates. Combining these data with a photometric redshift catalog, we ruled out each candidate as the counterpart to S190814bv and placed deep, uniform limits on the optical emission associated with S190814bv. For the nearest consistent GW distance, radiative transfer simulations of NSBH mergers constrain the ejecta mass of S190814bv to be M_(ej) < 0.04 M\u2299 at polar viewing angles, or M_(ej) < 0.03 M\u2299 if the opacity is \u03ba < 2 cm\u00b2g\u207b\u00b9. Assuming a tidal deformability for the NS at the high end of the range compatible with GW170817 results, our limits would constrain the BH spin component aligned with the orbital momentum to be \u03c7 < 0.7 for mass ratios Q < 6, with weaker constraints for more compact NSs.",
"doi": "10.3847/1538-4357/ab6a1b",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2020-02-20",
"series_number": "2",
"volume": "890",
"issue": "2",
"pages": "Art. No. 131"
}
]