[
{
"id": "authors:ffy4c-7y118",
"collection": "authors",
"collection_id": "ffy4c-7y118",
"cite_using_url": "https://authors.library.caltech.edu/records/ffy4c-7y118",
"type": "article",
"title": "SPHEREx Pre-perihelion Mapping of H\u2082O, CO\u2082, and CO in Interstellar Object 3I/ATLAS",
"author": [
{
"family_name": "Lisse",
"given_name": "Carey M.",
"orcid": "0000-0002-9548-1526"
},
{
"family_name": "Bach",
"given_name": "Yoonsoo P.",
"orcid": "0000-0002-2618-1124"
},
{
"family_name": "Crill",
"given_name": "Brendan P.",
"orcid": "0000-0002-4650-8518",
"clpid": "Crill-Brendan-P"
},
{
"family_name": "Korngut",
"given_name": "Phil M.",
"orcid": "0009-0003-8869-3365",
"clpid": "Korngut-Philip-M"
},
{
"family_name": "Cukierman",
"given_name": "Ari J.",
"orcid": "0000-0002-7471-719X",
"clpid": "Cukierman-Ari-J"
},
{
"family_name": "Bryan",
"given_name": "Sean A.",
"orcid": "0000-0003-4607-9562"
},
{
"family_name": "Cooray",
"given_name": "Asantha",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dowell",
"given_name": "C. Darren",
"orcid": "0009-0002-0098-6183",
"clpid": "Dowell-C-Darren"
},
{
"family_name": "Werner",
"given_name": "Michael W.",
"orcid": "0000-0003-4990-189X",
"clpid": "Werner-Michael-W"
},
{
"family_name": "Hora",
"given_name": "Joseph L.",
"orcid": "0000-0002-5599-4650"
},
{
"family_name": "Rustamkulov",
"given_name": "Zafar",
"orcid": "0000-0003-4408-0463",
"clpid": "Rustamkulov-Zafar"
},
{
"family_name": "Lee",
"given_name": "Jeong-Eun",
"orcid": "0000-0003-3119-2087"
},
{
"family_name": "Lim",
"given_name": "Bumhoo",
"orcid": "0000-0002-8244-4603"
},
{
"family_name": "Fernandez",
"given_name": "Y. R.",
"orcid": "0000-0003-1156-9721"
},
{
"family_name": "Tolls",
"given_name": "Volker",
"orcid": "0000-0003-1841-2241"
},
{
"family_name": "Reach",
"given_name": "W. T.",
"orcid": "0000-0001-8362-4094"
},
{
"family_name": "Dor\u00e9",
"given_name": "O.",
"orcid": "0000-0001-7432-2932",
"clpid": "Dor\u00e9-O"
},
{
"family_name": "Zemcov",
"given_name": "Michael",
"orcid": "0000-0001-8253-1451"
},
{
"family_name": "Bock",
"given_name": "James J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cheng",
"given_name": "Yun-Ting",
"orcid": "0000-0002-5437-0504",
"clpid": "Cheng-Yun-Ting"
},
{
"family_name": "Champagne",
"given_name": "C.",
"orcid": "0009-0001-1093-3715"
},
{
"family_name": "Choi",
"given_name": "Seungwon",
"orcid": "0009-0006-1028-1653"
},
{
"family_name": "Connelley",
"given_name": "M.",
"orcid": "0000-0002-8293-1428"
},
{
"family_name": "Emery",
"given_name": "J. P.",
"orcid": "0000-0001-9265-9475"
},
{
"family_name": "Everett",
"given_name": "Spencer",
"orcid": "0000-0002-3745-2882",
"clpid": "Everett-Spencer-W"
},
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Geem",
"given_name": "Jooyeon",
"orcid": "0000-0002-3291-4056"
},
{
"family_name": "Hui",
"given_name": "Howard",
"orcid": "0000-0001-5812-1903",
"clpid": "Hui-Howard"
},
{
"family_name": "Ishiguro",
"given_name": "Masateru",
"orcid": "0000-0002-7332-2479"
},
{
"family_name": "Jin",
"given_name": "Sunho",
"orcid": "0000-0002-0460-7550"
},
{
"family_name": "Jo",
"given_name": "Hangbin",
"orcid": "0009-0004-9591-8646"
},
{
"family_name": "Mahlke",
"given_name": "Max",
"orcid": "0000-0003-2831-0513"
},
{
"family_name": "Masters",
"given_name": "Daniel C.",
"orcid": "0000-0001-5382-6138",
"clpid": "Masters-Dan"
},
{
"family_name": "Melnick",
"given_name": "Gary J.",
"orcid": "0000-0002-6025-0680"
},
{
"family_name": "Nguyen",
"given_name": "Chi H.",
"orcid": "0000-0001-9368-3186",
"clpid": "Nguyen-Chi-H"
},
{
"family_name": "Paladini",
"given_name": "Roberta",
"orcid": "0000-0002-5158-243X",
"clpid": "Paladini-Roberta"
},
{
"family_name": "Sitko",
"given_name": "M. L.",
"orcid": "0000-0003-1799-1755"
},
{
"family_name": "Yang",
"given_name": "Yujin",
"orcid": "0000-0003-3078-2763"
}
],
"abstract": "\n
From 2025 August 1 to August 15 UT, the SPHEREx spacecraft observed interstellar object 3I/ATLAS. Using R = 40–130 spectrophotometry at λ = 0.7–5 μm, lightcurves, spectra, and imaging of 3I were obtained. From these, robust detections of water gas emission at 2.7–2.8 μm and CO2 gas at 4.23–4.27 μm plus tentative detections of 13CO2 and CO gas were found. A slightly extended H2O coma was detected, and a huge CO2 atmosphere extending out to at least 4.2 × 105 km was discovered. Gas production rates and 1σ errors for H2O, 12CO2, 13CO2, and CO were Qgas = 3.2 × 1026 ± 20%, 1.6 × 1027 ± 10%, 1.3 × 1025 ± 25%, and 1.0 × 1026 ± 25%, respectively. Coaddition of all λ = 1.0–1.5 μm scattered light continuum images from 3I produced an image with high signal-to-noise ratio consistent with an unresolved source. The lightcurve of scattered light showed \u227215% variability over the observation period. The absolute brightness of 3I at 1.0–1.5 μm is consistent with a nucleus of <2.5 km radius surrounded by a 100 times brighter coma. The 1.5–4.0 μm continuum structure shows a strong spectral feature commensurate with water ice absorption seen in Kuiper Belt objects and distant comets. The observed cometary behavior of 3I, including its preponderance of CO2 emission, lack of CO output, small size, and predominance of large icy chunks of material in a flux-dominant coma, is similar to the behavior of short-period comet 103P/Hartley 2, the ”hyperactive, strongly thermally processed comet” flyby target of the NASA Deep Impact Extended mission in 2010. This correspondence suggests that interstellar objects can be significantly thermally processed before ejection into the interstellar medium, and by comparison to 1I and 2I, this processing can be widely variable in its physical outcome.
\n
\n
Gaseous halos around galaxies play an important role in galaxy evolution. The exchange of metals from the interstellar medium (ISM) to the circumgalactic medium (CGM) is caused by the formation, feedback, and/or merging history of galaxies. We study the variation in chemical composition between the ISM (\u22723 kpc) and CGM (∼5–10 kpc) for a sample of M\u22c6 > 109.5 M\u2299 main-sequence galaxies at 4 < z < 6 with both JWST and Atacama Large Millimeter/submillimeter Array observations. Using JWST/NIRSpec integral field spectroscopy, we derive the optical line ratios from the ISM and the CGM for our sample, focusing on the typical optical lines used for metallicity studies. Our comparison shows that the ISM and the CGM have similar chemical abundances. This indicates that the CGM of these typical 4 < z < 6 galaxies is enriched to the level of their ISM in the early Universe. Using statistical tests, we find that some of the line ratios show marginal differences between the ISM and CGM. Combined with Cloudy modeling, our results suggest that a difference in ionization level (higher for the ISM) is the dominant reason for the observed ratio difference of oxygen line ratios. There is also indication of a deficit in the nitrogen abundance with respect to oxygen in the CGM, which suggests a delay in redistribution of secondary nitrogen. Finally, an enhanced F[C II]158μm/FHα ratio is observed in the CGM, suggesting that feedback and/or mergers play a key role in metal mixing.
\n
\n
We model the impact of source confusion on photometry and the resulting spectrophotometric redshifts for SPHEREx, a NASA Medium-Class Explorer that is carrying out an all-sky near-infrared spectral survey. Spectral confusion from untargeted background galaxies degrades sensitivity and introduces a spectral bias. Using interpolated spectral energy distributions (SEDs) from the COSMOS2020 catalog, we construct a Monte Carlo library of confusion spectra that captures the cumulative impact from faint galaxies. By injecting confusion realizations into galaxy SEDs and performing forced photometry at known source positions, we quantify photometric and redshift error and bias. For our current expected selection of sources for the cosmology analysis, we find typical 1σ confusion levels range from 0.8–3.8 μJy across 0.75–5.0 μm. While negligible at full-sky survey depth, spectral confusion becomes significant in the SPHEREx deep fields, reducing the number of intermediate-precision redshifts and inducing a small systematic overestimation in redshift. In parallel, we also model targeted source blending from beam overlaps, which contributes additional photometric noise without systematic redshift bias, provided that positions are known exactly. Together, confusion and blending vary with the depth of the selected reference sample, revealing a trade-off, where deeper selections reduce confusion but increase blending-induced noise. Our methodology informs optimization of the SPHEREx source selection strategy and future treatments of stellar source blending and confusion.
\n
Spectro-Photometer for the History of the Universe, Epoch of Reionization, and Ices Explorer (SPHEREx), a NASA Explorer satellite launched on 2025 March 11, is carrying out the first all-sky near-infrared spectral survey. The satellite observes in 102 spectral bands from 0.75 to 5.0 μm with a resolving power ranging from λ/Δλ = 35–130 in 6.\"2 pixels. The observatory obtains a 5σ depth of 19.5–19.9 AB mag for 0.75 < λ < 3.8 μm with λ/Δλ ∼ 40 and 17.8–18.8 AB mag for 3.8 < λ < 5.0 μm with λ/Δλ ∼ 120 after mapping the full sky four times over two years. Scientifically, SPHEREx will produce a large galaxy redshift survey over the full sky to constrain the amplitude of inflationary non-Gaussianity. The observations will produce two deep spectral maps near the ecliptic poles that use intensity mapping to probe the evolution of galaxies over cosmic history. By mapping the depth of infrared absorption features over the Galactic plane, SPHEREx will comprehensively survey the abundance and composition of water and other biogenic ice species in the interstellar medium. The project will release initial data rapidly in the form of spectral images, and specialized data products over the life of the mission as the surveys proceed. The science team will also produce spectral catalogs of planet-bearing and low-mass stars, solar system objects, and galaxy clusters three years after launch. We describe the design of the instrument and spacecraft, which flow from the core science requirements. Finally, we present an initial evaluation of the satellite’s in-flight performance and key characteristics.
",
"doi": "10.3847/1538-4357/ae2be2",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2026-03-01",
"series_number": "1",
"volume": "999",
"issue": "1",
"pages": "139"
},
{
"id": "authors:zb6hv-xbm62",
"collection": "authors",
"collection_id": "zb6hv-xbm62",
"cite_using_url": "https://authors.library.caltech.edu/records/zb6hv-xbm62",
"type": "article",
"title": "The Extended Mapping Obscuration to Reionization with ALMA (Ex-MORA) Survey: 5\u03c3 Source Catalog and Redshift Distribution",
"author": [
{
"family_name": "Long",
"given_name": "Arianna S.",
"orcid": "0000-0002-7530-8857"
},
{
"family_name": "Casey",
"given_name": "Caitlin M.",
"orcid": "0000-0002-0930-6466"
},
{
"family_name": "McKinney",
"given_name": "Jed",
"orcid": "0000-0002-6149-8178"
},
{
"family_name": "Zavala",
"given_name": "Jorge A.",
"orcid": "0000-0002-7051-1100"
},
{
"family_name": "Akins",
"given_name": "Hollis B."
},
{
"family_name": "Cooper",
"given_name": "Olivia R.",
"orcid": "0000-0003-3881-1397"
},
{
"family_name": "Lambrides",
"given_name": "Erini L.",
"orcid": "0000-0003-3216-7190"
},
{
"family_name": "Franco",
"given_name": "Maximilien",
"orcid": "0000-0002-3560-8599"
},
{
"family_name": "Aravena",
"given_name": "Manuel",
"orcid": "0000-0002-6290-3198"
},
{
"family_name": "Bethermin",
"given_name": "Matthieu",
"orcid": "0000-0002-3915-2015"
},
{
"family_name": "Caputi",
"given_name": "Karina",
"orcid": "0000-0001-8183-1460"
},
{
"family_name": "Champagne",
"given_name": "Jaclyn B.",
"orcid": "0000-0002-6184-9097"
},
{
"family_name": "Clements",
"given_name": "D. L.",
"orcid": "0000-0002-9548-5033"
},
{
"family_name": "da Cunha",
"given_name": "Elisabete",
"orcid": "0000-0001-9759-4797"
},
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Gentile",
"given_name": "Fabrizio",
"orcid": "0000-0002-8008-9871"
},
{
"family_name": "Hodge",
"given_name": "Jacqueline",
"orcid": "0000-0001-6586-8845"
},
{
"family_name": "Man",
"given_name": "Allison W. S.",
"orcid": "0000-0003-2475-124X"
},
{
"family_name": "Manning",
"given_name": "Sinclaire M.",
"orcid": "0000-0003-0415-0121"
},
{
"family_name": "Sanders",
"given_name": "David B.",
"orcid": "0000-0002-1233-9998"
},
{
"family_name": "Talia",
"given_name": "Margherita",
"orcid": "0000-0003-4352-2063"
},
{
"family_name": "Treister",
"given_name": "Ezequiel",
"orcid": "0000-0001-7568-6412"
},
{
"family_name": "Brammer",
"given_name": "Gabriel",
"orcid": "0000-0003-2680-005X"
},
{
"family_name": "Brusa",
"given_name": "Marcella",
"orcid": "0000-0002-5059-6848"
},
{
"family_name": "Finkelstein",
"given_name": "Steven L.",
"orcid": "0000-0001-8519-1130"
},
{
"family_name": "Fujimoto",
"given_name": "Seiji",
"orcid": "0000-0001-7201-5066"
},
{
"family_name": "Hayward",
"given_name": "Christopher C.",
"orcid": "0000-0003-4073-3236"
},
{
"family_name": "Ilbert",
"given_name": "Olivier",
"orcid": "0000-0002-7303-4397"
},
{
"family_name": "Jolly",
"given_name": "Jean-Baptiste",
"orcid": "0000-0002-3405-5646"
},
{
"family_name": "Kartaltepe",
"given_name": "Jeyhan S.",
"orcid": "0000-0001-9187-3605"
},
{
"family_name": "Knudsen",
"given_name": "Kirsten",
"orcid": "0000-0002-7821-8873"
},
{
"family_name": "Koekemoer",
"given_name": "Anton M.",
"orcid": "0000-0002-6610-2048"
},
{
"family_name": "Liu",
"given_name": "Daizhong",
"orcid": "0000-0001-9773-7479"
},
{
"family_name": "Magdis",
"given_name": "Georgios",
"orcid": "0000-0002-4872-2294"
},
{
"family_name": "McCracken",
"given_name": "Henry Joy",
"orcid": "0000-0002-9489-7765"
},
{
"family_name": "Rhodes",
"given_name": "Jason",
"orcid": "0000-0002-4485-8549",
"clpid": "Rhodes-Jason"
},
{
"family_name": "Robertson",
"given_name": "Brant E.",
"orcid": "0000-0002-4271-0364"
},
{
"family_name": "Scoville",
"given_name": "Nick",
"orcid": "0000-0002-0438-3323",
"clpid": "Scoville-N-Z"
},
{
"family_name": "Sheth",
"given_name": "Kartik",
"orcid": "0000-0002-5496-4118"
},
{
"family_name": "Smolcic",
"given_name": "Vernesa",
"orcid": "0000-0002-3893-8614"
},
{
"family_name": "Spilker",
"given_name": "Justin",
"orcid": "0000-0003-3256-5615"
},
{
"family_name": "Taniguchi",
"given_name": "Yoshiaki",
"orcid": "0000-0003-2247-3741"
},
{
"family_name": "Toft",
"given_name": "Sune",
"orcid": "0000-0003-3631-7176"
},
{
"family_name": "Urry",
"given_name": "C. Megan",
"orcid": "0000-0002-0745-9792"
},
{
"family_name": "Yun",
"given_name": "Min",
"orcid": "0000-0001-7095-7543"
}
],
"abstract": "One of the greatest challenges in galaxy evolution over the last decade has been constraining the prevalence of heavily dust-obscured galaxies in the early Universe. At z > 3, these galaxies are increasingly rare, and difficult to identify, as they are interspersed among the more numerous dust-obscured galaxy population at z = 1–3, making efforts to secure confident spectroscopic redshifts expensive, and sometimes unsuccessful. In this work, we present the Extended Mapping Obscuration to Reionization with the Atacama Large Millimeter/submillimeter Array (ALMA; Ex-MORA) Survey—a 2 mm blank-field survey in the COSMOS-Web field, and the largest ever ALMA blank-field survey to date, covering 577 arcmin². Ex-MORA is an expansion of the MORA survey designed to identify primarily z > 3 dusty, star-forming galaxies while simultaneously filtering out the more numerous z < 3 population by leveraging the very negative K -correction at observed-frame 2 mm. We identify 37 significant (>5 σ ) sources, 33 of which are robust thermal dust emitters. We measure a median redshift of\u3008 z \u3009= 3.8_(−1.52)^(+1.7), with two-thirds of the sample at z > 3, and just under half at z > 4, demonstrating the overall success of the 2 mm selection technique. The total integrated z > 3 volume density of Ex-MORA sources is ∼1–3 × 10\u207b\u2075 Mpc\u207b³, consistent with other surveys of infrared luminous galaxies at similar epochs. We also find that techniques using rest-frame optical emission (or lack thereof) to identify z > 3 heavily dust-obscured galaxies miss at least half of Ex-MORA galaxies. This supports the idea that the dusty galaxy population is heterogeneous, and that synergies across observatories spanning multiple energy regimes are critical to understanding their formation and evolution at z > 3.
",
"doi": "10.3847/1538-4357/ae2fda",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2026-03-01",
"series_number": "1",
"volume": "999",
"issue": "1",
"pages": "47"
},
{
"id": "authors:ff2vr-67m69",
"collection": "authors",
"collection_id": "ff2vr-67m69",
"cite_using_url": "https://authors.library.caltech.edu/records/ff2vr-67m69",
"type": "article",
"title": "The redshifts from 122 bands: Comparative redshift forecast for low-resolution spectra from SPHEREx and the 7-Dimensional Sky Survey (7DS)",
"author": [
{
"family_name": "Bae",
"given_name": "Jangho",
"orcid": "0000-0002-4477-1208"
},
{
"family_name": "Lee",
"given_name": "Bomee",
"orcid": "0000-0003-1954-5046"
},
{
"family_name": "Im",
"given_name": "Myungshin",
"orcid": "0000-0002-8537-6714"
},
{
"family_name": "Bahk",
"given_name": "Hyeonguk",
"orcid": "0009-0002-9878-1126"
},
{
"family_name": "Dachan",
"given_name": "Kim",
"orcid": "0009-0001-3899-7198"
},
{
"family_name": "Hwang",
"given_name": "Ho Seong",
"orcid": "0000-0003-3428-7612"
},
{
"family_name": "Hong",
"given_name": "Sungryong",
"orcid": "0000-0001-9991-8222"
},
{
"family_name": "Kim",
"given_name": "Suk",
"orcid": "0000-0003-3474-9047"
},
{
"family_name": "Kim",
"given_name": "Minjin",
"orcid": "0000-0002-3560-0781"
},
{
"family_name": "Kim",
"given_name": "Taewan",
"orcid": "0009-0001-3758-9440"
},
{
"family_name": "Lee",
"given_name": "Jeyeon"
},
{
"family_name": "Sohn",
"given_name": "Jubee",
"orcid": "0000-0002-9254-144X"
},
{
"family_name": "Song",
"given_name": "Hyunmi",
"orcid": "0000-0002-4362-4070"
},
{
"family_name": "Chang",
"given_name": "Seo-Won",
"orcid": "0000-0002-3118-8275"
},
{
"family_name": "Cheng",
"given_name": "Yun-Ting",
"orcid": "0000-0002-5437-0504",
"clpid": "Cheng-Yun-Ting"
},
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Huai",
"given_name": "Zhaoyu",
"orcid": "0009-0009-1219-5128",
"clpid": "Huai-Zhaoyu"
},
{
"family_name": "Jeong",
"given_name": "Woong-Seob",
"orcid": "0000-0002-2770-808X"
},
{
"family_name": "Kim",
"given_name": "Ji Hoon",
"orcid": "0000-0002-1418-3309"
},
{
"family_name": "Kim",
"given_name": "Dohyeong",
"orcid": "0000-0002-6925-4821"
},
{
"family_name": "Kim",
"given_name": "Yongjung",
"orcid": "0000-0003-1647-3286"
},
{
"family_name": "Lee",
"given_name": "Seong-Kook",
"orcid": "0000-0001-5342-8906"
},
{
"family_name": "Masters",
"given_name": "Daniel C.",
"orcid": "0000-0001-5382-6138",
"clpid": "Masters-Dan"
},
{
"family_name": "Ko",
"given_name": "Eunhee",
"orcid": "0000-0002-8130-8044"
}
],
"abstract": "The recently initiated SPHEREx and 7DS surveys will deliver low-resolution spectra (R\u2004∼\u200420\u2005−\u2005130) for hundreds of millions of galaxies over the optical to near-infrared range (0.4\u2005−\u20055.0\u2006μm), covering a wide sky area without sample selection. These unique datasets will improve redshift estimation and provide a rich redshift catalog for the community. In this study, we forecast the performance of photometric redshift estimations using simulated SPHEREx and 7DS data. Four widely used template-fitting approaches and two machine-learning (ML) methods are used to derive photometric redshifts from low-resolution spectrophotometric data. We measured redshifts using mock catalogs based on the GAMA and COSMOS galaxy samples and achieved high precision for bright (13\u2004<\u2004i\u2004<\u200418) galaxies, with σNMAD\u2004\u2272\u20040.005, bias \u22720.005, and a catastrophic failure rate \u22720.005 for all methods employed. We find that the combined SPHEREx + 7DS dataset significantly improves redshift estimation compared to using either the SPHEREx or 7DS datasets alone, highlighting the synergy between the two surveys. Moreover, we compare the redshift estimation performance across magnitude ranges for the different methods and examine the probability distribution functions (PDFs) produced by the template-fitting approaches. As a result, we identify some factors that can affect the redshift measurements, for example, treatments on dust extinction or inclusion of flux uncertainty in the ML model. We also show that the PDFs are relatively well calibrated, although the confidence intervals are generally underestimated, particularly for bright galaxies in the template-fitting methods. This study demonstrates the strong potential of SPHEREx and 7DS to deliver improved redshift measurements from low-resolution spectrophotometric data, underscoring the scientific value of jointly utilizing both datasets.
",
"doi": "10.1051/0004-6361/202556999",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy & Astrophysics",
"publication_date": "2026-02",
"volume": "706",
"pages": "A347"
},
{
"id": "authors:cwtxw-2jm54",
"collection": "authors",
"collection_id": "cwtxw-2jm54",
"cite_using_url": "https://authors.library.caltech.edu/records/cwtxw-2jm54",
"type": "article",
"title": "COSMOS Spectroscopic Redshift Compilation (First Data Release): 488,000 Redshifts Encompassing Two Decades of Spectroscopy",
"author": [
{
"family_name": "Khostovan",
"given_name": "Ali Ahmad",
"orcid": "0000-0002-0101-336X"
},
{
"family_name": "Kartaltepe",
"given_name": "Jeyhan S.",
"orcid": "0000-0001-9187-3605"
},
{
"family_name": "Salvato",
"given_name": "Mara",
"orcid": "0000-0001-7116-9303"
},
{
"family_name": "Ilbert",
"given_name": "Olivier",
"orcid": "0000-0002-7303-4397"
},
{
"family_name": "Casey",
"given_name": "Caitlin M.",
"orcid": "0000-0002-0930-6466"
},
{
"family_name": "Algera",
"given_name": "Hiddo",
"orcid": "0000-0002-4205-9567"
},
{
"family_name": "Antwi-Danso",
"given_name": "Jacqueline",
"orcid": "0000-0002-0243-6575"
},
{
"family_name": "Battisti",
"given_name": "Andrew",
"orcid": "0000-0003-4569-2285"
},
{
"family_name": "Brinch",
"given_name": "Malte",
"orcid": "0000-0002-0245-6365"
},
{
"family_name": "Brusa",
"given_name": "Marcella",
"orcid": "0000-0002-5059-6848"
},
{
"family_name": "Calabr\u00f2",
"given_name": "Antonello",
"orcid": "0000-0003-2536-1614"
},
{
"family_name": "Capak",
"given_name": "Peter L.",
"orcid": "0000-0003-3578-6843",
"clpid": "Capak-P"
},
{
"family_name": "Chartab",
"given_name": "Nima",
"orcid": "0000-0003-3691-937X",
"clpid": "Chartab-Nima"
},
{
"family_name": "Cooper",
"given_name": "Olivia R.",
"orcid": "0000-0003-3881-1397"
},
{
"family_name": "Cox",
"given_name": "Isa G.",
"orcid": "0000-0002-1803-794X"
},
{
"family_name": "Darvish",
"given_name": "Behnam",
"orcid": "0000-0003-4919-9017"
},
{
"family_name": "Drakos",
"given_name": "Nicole E.",
"orcid": "0000-0003-4761-2197"
},
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "George",
"given_name": "Matthew R."
},
{
"family_name": "Gozaliasl",
"given_name": "Ghassem",
"orcid": "0000-0002-0236-919X"
},
{
"family_name": "Harish",
"given_name": "Santosh",
"orcid": "0000-0003-0129-2079"
},
{
"family_name": "Hasinger",
"given_name": "G\u00fcnther",
"orcid": "0000-0002-0797-0646"
},
{
"family_name": "Hatamnia",
"given_name": "Hossein",
"orcid": "0009-0007-3673-4523"
},
{
"family_name": "Iovino",
"given_name": "Angela",
"orcid": "0000-0001-6958-0304"
},
{
"family_name": "Jin",
"given_name": "Shuowen",
"orcid": "0000-0002-8412-7951"
},
{
"family_name": "Kashino",
"given_name": "Daichi",
"orcid": "0000-0001-9044-1747"
},
{
"family_name": "Koekemoer",
"given_name": "Anton M.",
"orcid": "0000-0002-6610-2048"
},
{
"family_name": "Laishram",
"given_name": "Ronaldo",
"orcid": "0000-0002-0322-6131"
},
{
"family_name": "Lee",
"given_name": "Khee-Gan",
"orcid": "0000-0001-9299-5719"
},
{
"family_name": "Lertprasertpong",
"given_name": "Jitrapon",
"orcid": "0000-0002-3535-4066"
},
{
"family_name": "Lilly",
"given_name": "Simon J.",
"orcid": "0000-0002-6423-3597"
},
{
"family_name": "Liu",
"given_name": "Daizhong",
"orcid": "0000-0001-9773-7479"
},
{
"family_name": "Masters",
"given_name": "Daniel C.",
"orcid": "0000-0001-5382-6138",
"clpid": "Masters-Daniel-C"
},
{
"family_name": "Mobasher",
"given_name": "Bahram",
"orcid": "0000-0001-5846-4404"
},
{
"family_name": "Nagao",
"given_name": "Tohru",
"orcid": "0000-0002-7402-5441"
},
{
"family_name": "Onodera",
"given_name": "Masato",
"orcid": "0000-0003-3228-7264"
},
{
"family_name": "Peng",
"given_name": "Yingjie",
"orcid": "0000-0003-0939-9671"
},
{
"family_name": "Sanders",
"given_name": "David B.",
"orcid": "0000-0002-1233-9998"
},
{
"family_name": "Sanders",
"given_name": "Ryan L.",
"orcid": "0000-0003-4792-9119"
},
{
"family_name": "Sattari",
"given_name": "Zahra",
"orcid": "0000-0002-0364-1159",
"clpid": "Sattari-Zahra"
},
{
"family_name": "Scoville",
"given_name": "Nick",
"orcid": "0000-0002-0438-3323",
"clpid": "Scoville-N-Z"
},
{
"family_name": "Shah",
"given_name": "Ekta A.",
"orcid": "0000-0001-7811-9042"
},
{
"family_name": "Silverman",
"given_name": "John D.",
"orcid": "0000-0002-0000-6977"
},
{
"family_name": "Suzuki",
"given_name": "Nao",
"orcid": "0000-0001-7266-930X"
},
{
"family_name": "Taamoli",
"given_name": "Sina",
"orcid": "0000-0003-0749-4667"
},
{
"family_name": "Tanaka",
"given_name": "Masayuki",
"orcid": "0000-0002-5011-5178"
},
{
"family_name": "Tasca",
"given_name": "Lidia A. M."
},
{
"family_name": "Toft",
"given_name": "Sune",
"orcid": "0000-0003-3631-7176"
},
{
"family_name": "Toni",
"given_name": "Greta",
"orcid": "0009-0005-3133-1157"
},
{
"family_name": "Trakhtenbrot",
"given_name": "Benny",
"orcid": "0000-0002-3683-7297"
},
{
"family_name": "Trump",
"given_name": "Jonathan R.",
"orcid": "0000-0002-1410-0470"
},
{
"family_name": "Vaccari",
"given_name": "Mattia",
"orcid": "0000-0002-6748-0577"
},
{
"family_name": "Valentino",
"given_name": "Francesco",
"orcid": "0000-0001-6477-4011"
},
{
"family_name": "Vanderhoof",
"given_name": "Brittany N.",
"orcid": "0000-0002-8163-0172"
},
{
"family_name": "Weaver",
"given_name": "John R.",
"orcid": "0000-0003-1614-196X"
},
{
"family_name": "Yun",
"given_name": "Min S.",
"orcid": "0000-0001-7095-7543"
},
{
"family_name": "Zavala",
"given_name": "Jorge A.",
"orcid": "0000-0002-7051-1100"
}
],
"abstract": "\n
We present the COSMOS Spectroscopic Redshift Compilation encompassing ∼20 yr of spectroscopic redshifts within a 10 deg2 area centered on the 2 deg2 COSMOS legacy field. This compilation contains 487,666 redshifts of 266,284 unique objects from 138 individual programs up to z ∼ 8 with median stellar mass ∼108.4–1010 M\u2299 (redshift dependent). Rest-frame NUVrJ colors and star formation rate–stellar mass correlations show that the compilation primarily contains low-to-intermediate-mass star-forming and massive, quiescent galaxies at z < 1.25 and mostly low-mass bursty star-forming galaxies at z > 2. Sources in the compilation cover a diverse range of environments, including protoclusters such as “Hyperion.” The full compilation is 50% spectroscopically complete by i ∼ 23.4 mag and Ks ∼ 21.6 mag; however, this is redshift dependent. Spatially, the compilation is >50% (>30%) complete within the central (outer) region limited to i < 24 mag and Ks < 22.5 mag, separately. We demonstrate how the compilation can be used to validate photometric redshifts and investigate calibration metrics. By training self-organizing maps on COSMOS2020/Classic and projecting the compilation onto it, we find key subpopulations currently lacking spectroscopic coverage, including z < 1 intermediate-mass quiescent and low-/intermediate-mass bursty star-forming galaxies, z ∼ 2 massive quiescent galaxies, and z > 3 massive star-forming galaxies. This highlights how combining self-organizing maps with our compilation can provide guidance for future spectroscopic observations to get a complete spectroscopic view of galaxy populations. Lastly, the compilation will undergo periodic data releases incorporating new spectroscopic redshifts and providing a lasting legacy resource for the community.
\n
We describe the SPHEREx Sky Simulator (henceforth the Simulator), a software tool designed to model science data for NASA’s SPHEREx mission that will carry out a series of all-sky spectrophotometric surveys at ∼6″ spatial resolution in 102 spectral channels spanning 0.75–5 μm. The Simulator software implements models for astrophysical emission, instrument characteristics, and survey strategy to generate realistic infrared sky scenes as they will be observed by SPHEREx. The simulated data include a variety of realistic noise and systematic effects that are estimated using up-to-date astrophysical measurements and information from prelaunch instrument characterization campaigns. Through the preflight mission phases, the Simulator has been critical in predicting the impact of various effects on SPHEREx science performance and has played an important role in guiding the development of the SPHEREx data analysis pipeline. In this paper, we describe the Simulator architecture, preflight instrument, and sky models, and summarize high-level predictions from the Simulator, including a prelaunch prediction for the 5σ point source sensitivity of SPHEREx, which we estimate to be mAB 18.5–19 from 0.75 to 3.8 μm and mAB 16.6–18 from 3.8 to 5 μm, with the sensitivity limited by the zodiacal light background at all wavelengths. In the future, on-orbit data will be used to improve the Simulator, which will form the basis of a variety of forward-modeling tools that will be used to model myriad instrumental and astrophysical processes to characterize their systematic effects on our final data products and analyses.
",
"doi": "10.3847/1538-4365/ae04cc",
"issn": "0067-0049",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2025-11",
"series_number": "1",
"volume": "281",
"issue": "1",
"pages": "10"
},
{
"id": "authors:pytp2-2ab91",
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"collection_id": "pytp2-2ab91",
"cite_using_url": "https://authors.library.caltech.edu/records/pytp2-2ab91",
"type": "article",
"title": "The ALPINE\u2013CRISTAL\u2013JWST survey: revealing less massive black holes in high-redshift galaxies",
"author": [
{
"family_name": "Ren",
"given_name": "Wenke",
"orcid": "0000-0002-3742-6609"
},
{
"family_name": "Silverman",
"given_name": "John D",
"orcid": "0000-0002-0000-6977"
},
{
"family_name": "Faisst",
"given_name": "Andreas L",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Fujimoto",
"given_name": "Seiji",
"orcid": "0000-0001-7201-5066"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Liu",
"given_name": "Zhaoxuan",
"orcid": "0000-0002-9252-114X"
},
{
"family_name": "Tsujita",
"given_name": "Akiyoshi",
"orcid": "0000-0002-0498-5041"
},
{
"family_name": "Aravena",
"given_name": "Manuel",
"orcid": "0000-0002-6290-3198"
},
{
"family_name": "Davies",
"given_name": "Rebecca L",
"orcid": "0000-0002-3324-4824"
},
{
"family_name": "De\u00a0Looze",
"given_name": "Ilse",
"orcid": "0000-0001-9419-6355"
},
{
"family_name": "Dessauges-Zavadsky",
"given_name": "Miroslava",
"orcid": "0000-0003-0348-2917"
},
{
"family_name": "Herrera-Camus",
"given_name": "Rodrigo",
"orcid": "0000-0002-2775-0595"
},
{
"family_name": "Ibar",
"given_name": "Edo",
"orcid": "0009-0008-9801-2224"
},
{
"family_name": "Jones",
"given_name": "Gareth C",
"orcid": "0000-0002-0267-9024"
},
{
"family_name": "Kartaltepe",
"given_name": "Jeyhan S",
"orcid": "0000-0001-9187-3605"
},
{
"family_name": "Koekemoer",
"given_name": "Anton M",
"orcid": "0000-0002-6610-2048"
},
{
"family_name": "Lin",
"given_name": "Yu-Heng",
"orcid": "0000-0001-8792-3091",
"clpid": "Lin-Yu-Heng"
},
{
"family_name": "Mitsuhashi",
"given_name": "Ikki",
"orcid": "0000-0001-7300-9450"
},
{
"family_name": "Molina",
"given_name": "Juan",
"orcid": "0000-0002-8136-8127"
},
{
"family_name": "Nanni",
"given_name": "Ambra",
"orcid": "0000-0001-6652-1069"
},
{
"family_name": "Relano",
"given_name": "Monica",
"orcid": "0000-0003-1682-1148"
},
{
"family_name": "Romano",
"given_name": "Michael",
"orcid": "0000-0002-9948-3916"
},
{
"family_name": "Sanders",
"given_name": "David B",
"orcid": "0000-0002-1233-9998"
},
{
"family_name": "Solimano",
"given_name": "Manuel",
"orcid": "0000-0001-6629-0379"
},
{
"family_name": "Veraldi",
"given_name": "Enrico",
"orcid": "0009-0007-1304-7771"
},
{
"family_name": "Villanueva",
"given_name": "Vicente",
"orcid": "0000-0002-5877-379X"
},
{
"family_name": "Wang",
"given_name": "Wuji",
"orcid": "0000-0002-7964-6749",
"clpid": "Wang-Wuji"
},
{
"family_name": "Zamorani",
"given_name": "Giovanni",
"orcid": "0000-0002-2318-301X"
}
],
"abstract": "We present a systematic search for broad-line active galactic nuclei (AGNs) in the ALPINE–CRISTAL–JWST sample of 18 star-forming galaxies (\u2060\u2060M\u22c6 > 10^(9.5) M\u2299) at redshifts \u2060z = 4.4 - 5.7. Using James Webb Space Telescope (JWST)/NIRSpec IFU, we identify seven AGN candidates through the detection of broad H emission lines from 33 aperture spectra centred on photometric peaks. These candidates include one highly robust AGN detection with full width at half-maximum (FWHM) 2800 km s \u207b¹and six showing broad components with FWHM ~600 - 1600 km s\u207b¹\u2060, with two in a merger system. We highlight that only broad-line detection is effective since these candidates uniformly lie within narrow emission-line ratio diagnostic diagrams where star-forming galaxies and AGNs overlap. The broad-line AGN fraction ranges from 5.9 per cent to 33 per cent, depending on the robustness of the candidates. Assuming that the majority are AGNs, the relatively high AGN fraction is likely due to targeting high-mass galaxies, where simulations demonstrate that broad-line detection is more feasible. Their black hole masses range from 10\u2076 to 10^(7.5)M\u2299 with \u20600.1 \u227e L_(bol)/L_(edd) \u227e 1. Counter to previous JWST studies at high redshift that found overmassive black holes relative to their host galaxies, our candidates lie close to or below the local M_(BH) - M\u22c6 scaling relations, thus demonstrating the effect of selection biases. This study provides new insights into AGN–host galaxy co-evolution at high redshift by identifying faint broad-line AGNs in galaxy samples, highlighting the importance of considering mass-dependent selection biases and the likelihood of a large population of AGNs being undermassive and just now being tapped by JWST.
",
"doi": "10.1093/mnras/staf1709",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2025-11",
"series_number": "1",
"volume": "544",
"issue": "1",
"pages": "211-233"
},
{
"id": "authors:t3npn-1y712",
"collection": "authors",
"collection_id": "t3npn-1y712",
"cite_using_url": "https://authors.library.caltech.edu/records/t3npn-1y712",
"type": "article",
"title": "The Potential of the SPHEREx Mission for Characterizing Polycyclic Aromatic Hydrocarbon 3.3 \u03bcm Emission in Nearby Galaxies",
"author": [
{
"family_name": "Zhang",
"given_name": "Edward",
"orcid": "0009-0003-1284-3507",
"clpid": "Zhang-Edward"
},
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Crill",
"given_name": "Brendan P.",
"orcid": "0000-0002-4650-8518",
"clpid": "Crill-Brendan-P"
},
{
"family_name": "Inami",
"given_name": "Hanae",
"orcid": "0000-0003-4268-0393"
},
{
"family_name": "Lai",
"given_name": "Thomas",
"orcid": "0000-0001-8490-6632",
"clpid": "Lai-Thomas"
},
{
"family_name": "Ohyama",
"given_name": "Youichi",
"orcid": "0000-0001-9490-3582"
},
{
"family_name": "Pyo",
"given_name": "Jeonghyun",
"orcid": "0000-0001-9937-8270"
},
{
"family_name": "Akeson",
"given_name": "Rachel",
"orcid": "0000-0001-9674-1564",
"clpid": "Akeson-Rachel"
},
{
"family_name": "Ashby",
"given_name": "Matthew L. N.",
"orcid": "0000-0002-3993-0745"
},
{
"family_name": "Bock",
"given_name": "James J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cheng",
"given_name": "Yun-Ting",
"orcid": "0000-0002-5437-0504",
"clpid": "Cheng-Yun-Ting"
},
{
"family_name": "Chiang",
"given_name": "Yi-Kuan",
"orcid": "0000-0001-6320-261X"
},
{
"family_name": "Cooray",
"given_name": "Asantha",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dor\u00e9",
"given_name": "Olivier",
"orcid": "0000-0001-7432-2932",
"clpid": "Dor\u00e9-O"
},
{
"family_name": "Feder",
"given_name": "Richard M.",
"orcid": "0000-0002-9330-8738"
},
{
"family_name": "Kim",
"given_name": "Yongjung",
"orcid": "0000-0003-1647-3286"
},
{
"family_name": "Lee",
"given_name": "Bomee",
"orcid": "0000-0003-1954-5046"
},
{
"family_name": "Masters",
"given_name": "Daniel",
"orcid": "0000-0001-5382-6138",
"clpid": "Masters-Daniel"
},
{
"family_name": "Melnick",
"given_name": "Gary",
"orcid": "0000-0002-6025-0680"
},
{
"family_name": "Paladini",
"given_name": "Roberta",
"orcid": "0000-0002-5158-243X",
"clpid": "Paladini-Roberta"
},
{
"family_name": "Werner",
"given_name": "Michael W.",
"orcid": "0000-0003-4990-189X",
"clpid": "Werner-Michael-W"
}
],
"abstract": "Together with gas, stars, and supermassive black holes, dust is crucial in stellar and galaxy evolution. Hence, understanding galaxies’ dust properties across cosmic time is critical to studying their evolution. In addition to photometric constraints on the absorption of blue light and its reemission at infrared wavelengths, dust grain properties can be explored spectroscopically via polycyclic aromatic hydrocarbon (PAH) emission bands in the mid-IR. The new SPHEREx space telescope conducts an all-sky spectrophotometric survey of stars and galaxies at wavelengths of 0.75–5 μm, making it ideal for studying the widespread presence of the 3.3 μm PAH emission across galaxy populations out to z ∼ 0.4. In this paper, we simulated galaxy spectra to investigate SPHEREx's capability to study PAH emission in such galaxies. We find that for the all-sky survey the PAH 3.3 μm emission band flux can be measured to 30% accuracy at log (M/M\u2299) > 9.5 and star formation rate (SFR) > 1 M\u2299 yr\u207b¹ at z = 0.1, log (M/M\u2299) > 10.5 and SFR > 10 M\u2299 yr\u207b¹ at z = 0.2–0.3, and log (M/M\u2299) > 11 and SFR > 100 M\u2299 yr\u207b¹ at z = 0.4. For deep SPHEREx fields, a factor of ∼10 deeper sensitivity limits can be reached. Overall, SPHEREx will enable the measurement of the 3.3 μm PAH band emission in several hundred thousand galaxies across the sky, providing a population study of the smallest dust grains (“nano grains”) and radiation properties in massive galaxies in the nearby Universe.
",
"doi": "10.3847/1538-4357/adfd5a",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2025-10-10",
"series_number": "1",
"volume": "992",
"issue": "1",
"pages": "3"
},
{
"id": "authors:m7w1n-7vb15",
"collection": "authors",
"collection_id": "m7w1n-7vb15",
"cite_using_url": "https://authors.library.caltech.edu/records/m7w1n-7vb15",
"type": "article",
"title": "COSMOS-Web: The Role of Galaxy Interactions and Disk Instabilities in Producing Starbursts at z\u00a0<\u00a04",
"author": [
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Yang",
"given_name": "Lilan",
"orcid": "0000-0002-8434-880X"
},
{
"family_name": "Brinch",
"given_name": "M.",
"orcid": "0000-0002-0245-6365"
},
{
"family_name": "Casey",
"given_name": "C. M.",
"orcid": "0000-0002-0930-6466"
},
{
"family_name": "Chartab",
"given_name": "N.",
"orcid": "0000-0003-3691-937X"
},
{
"family_name": "Dessauges-Zavadsky",
"given_name": "M.",
"orcid": "0000-0003-0348-2917"
},
{
"family_name": "Drakos",
"given_name": "N. E.",
"orcid": "0000-0003-4761-2197"
},
{
"family_name": "Gillman",
"given_name": "S.",
"orcid": "0000-0001-9885-4589"
},
{
"family_name": "Gozaliasl",
"given_name": "G.",
"orcid": "0000-0002-0236-919X"
},
{
"family_name": "Hayward",
"given_name": "C. C.",
"orcid": "0000-0003-4073-3236"
},
{
"family_name": "Ilbert",
"given_name": "O.",
"orcid": "0000-0002-7303-4397"
},
{
"family_name": "Jablonka",
"given_name": "P.",
"orcid": "0000-0002-9655-1063"
},
{
"family_name": "Kaminsky",
"given_name": "A.",
"orcid": "0009-0000-3672-0198"
},
{
"family_name": "Kartaltepe",
"given_name": "J. S.",
"orcid": "0000-0001-9187-3605"
},
{
"family_name": "Koekemoer",
"given_name": "A. M.",
"orcid": "0000-0002-6610-2048"
},
{
"family_name": "Kokorev",
"given_name": "V.",
"orcid": "0000-0002-5588-9156"
},
{
"family_name": "Lambrides",
"given_name": "E.",
"orcid": "0000-0003-3216-7190"
},
{
"family_name": "Liu",
"given_name": "D.",
"orcid": "0000-0001-9773-7479"
},
{
"family_name": "Maraston",
"given_name": "C.",
"orcid": "0000-0001-7711-3677"
},
{
"family_name": "Martin",
"given_name": "C. L.",
"orcid": "0000-0001-9189-7818"
},
{
"family_name": "Renzini",
"given_name": "A.",
"orcid": "0000-0002-7093-7355"
},
{
"family_name": "Robertson",
"given_name": "B. E.",
"orcid": "0000-0002-4271-0364"
},
{
"family_name": "Sanders",
"given_name": "D. B.",
"orcid": "0000-0002-1233-9998"
},
{
"family_name": "Sattari",
"given_name": "Z.",
"orcid": "0000-0002-0364-1159"
},
{
"family_name": "Scoville",
"given_name": "N.",
"orcid": "0000-0002-0438-3323",
"clpid": "Scoville-N-Z"
},
{
"family_name": "Urry",
"given_name": "C. M.",
"orcid": "0000-0002-0745-9792"
},
{
"family_name": "Vijayan",
"given_name": "A. P.",
"orcid": "0000-0002-1905-4194"
},
{
"family_name": "Weaver",
"given_name": "J. R.",
"orcid": "0000-0003-1614-196X"
},
{
"family_name": "Akins",
"given_name": "H. B.",
"orcid": "0000-0003-3596-8794"
},
{
"family_name": "Allen",
"given_name": "N.",
"orcid": "0000-0001-9610-7950"
},
{
"family_name": "Arango-Toro",
"given_name": "R. C.",
"orcid": "0000-0002-0569-5222"
},
{
"family_name": "Cooper",
"given_name": "O. R.",
"orcid": "0000-0003-3881-1397"
},
{
"family_name": "Franco",
"given_name": "M.",
"orcid": "0000-0002-3560-8599"
},
{
"family_name": "Gentile",
"given_name": "F.",
"orcid": "0000-0002-8008-9871"
},
{
"family_name": "Harish",
"given_name": "S.",
"orcid": "0000-0003-0129-2079"
},
{
"family_name": "Hirschmann",
"given_name": "M.",
"orcid": "0000-0002-3301-3321"
},
{
"family_name": "Khostovan",
"given_name": "A. A.",
"orcid": "0000-0002-0101-336X"
},
{
"family_name": "Laigle",
"given_name": "C.",
"orcid": "0009-0008-5926-818X"
},
{
"family_name": "Larson",
"given_name": "R. L.",
"orcid": "0000-0003-2366-8858"
},
{
"family_name": "Lee",
"given_name": "M.",
"orcid": "0000-0002-2419-3068"
},
{
"family_name": "Liu",
"given_name": "Z.",
"orcid": "0000-0002-9252-114X"
},
{
"family_name": "Long",
"given_name": "A. S.",
"orcid": "0000-0002-7530-8857"
},
{
"family_name": "Magdis",
"given_name": "G.",
"orcid": "0000-0002-4872-2294"
},
{
"family_name": "Massey",
"given_name": "R.",
"orcid": "0000-0002-6085-3780"
},
{
"family_name": "McCracken",
"given_name": "H. J.",
"orcid": "0000-0002-9489-7765"
},
{
"family_name": "McKinney",
"given_name": "J.",
"orcid": "0000-0002-6149-8178"
},
{
"family_name": "Paquereau",
"given_name": "L.",
"orcid": "0000-0003-2397-0360"
},
{
"family_name": "Rhodes",
"given_name": "J.",
"orcid": "0000-0002-4485-8549",
"clpid": "Rhodes-Jason"
},
{
"family_name": "Rich",
"given_name": "R. M.",
"orcid": "0000-0003-0427-8387"
},
{
"family_name": "Shuntov",
"given_name": "M.",
"orcid": "0000-0002-7087-0701"
},
{
"family_name": "Silverman",
"given_name": "J. D.",
"orcid": "0000-0002-0000-6977"
},
{
"family_name": "Talia",
"given_name": "M.",
"orcid": "0000-0003-4352-2063"
},
{
"family_name": "Toft",
"given_name": "S.",
"orcid": "0000-0003-3631-7176"
},
{
"family_name": "Zavala",
"given_name": "J. A.",
"orcid": "0000-0002-7051-1100"
}
],
"abstract": "\n
We study of the role of galaxy–galaxy interactions and disk instabilities in producing starburst activity in galaxies out to z = 4. For this, we use a sample of 387 galaxies with robust total star formation rate measurements from Herschel, gas masses from the Atacama Large Millimeter/submillimeter Array, stellar masses and redshifts from multiband photometry, and JWST/NIRCam rest-frame optical imaging. Using mass-controlled samples, we find an increased fraction of interacting galaxies in the starburst regime at all redshifts out to z = 4. This increase correlates with star formation efficiency (SFE) but not with gas fraction. However, the correlation is weak (and only significant out to z = 2), which could be explained by the short duration of SFE increase during interaction. In addition, we find that isolated disk galaxies make up a significant fraction of the starburst population. The fraction of such galaxies with star-forming clumps (\"clumpy disks\") is significantly increased compared to the main-sequence disk population. Furthermore, this fraction directly correlates with SFE. This is direct observational evidence for a long-term increase of SFE maintained due to disk instabilities, contributing to the majority of starburst galaxies in our sample and hence to substantial mass growth in these systems. This result could also be of importance for explaining the growth of the most massive galaxies at z > 6.
\n
Galaxy protoclusters are sites of rapid growth, with a high density of massive galaxies driving elevated rates of star formation and accretion onto supermassive black holes. Here, we present new JWST/NIRSpec IFU observations of the J1000+0234 group at z\u2004=\u20044.54, a dense region of a protocluster hosting a massive, dusty star forming galaxy (DSFG). The new data reveal two extended, high-equivalent-width (EW0 > 1000 Å) [O\u202fIII] nebulae that appear at both sides of the DSFG along its minor axis (namely O3-N and O3-S). On one hand, the spectrum of O3-N shows a broad and blueshifted component with a full width at half maximum (FWHM) of ∼1300\u2006km\u2006s−1, suggesting an outflow origin. On the other hand, O3-S stretches over 8.6 kpc, and has a velocity gradient that spans 800 km\u2006s−1, but shows no evidence of a broad component. However, both sources seem to be powered at least partially by an active galactic nucleus (AGN), so we classified them as extended emission-line regions (EELRs). The strongest evidence comes from the detection of the high-ionization [Ne\u202fV] λ 3427 line toward O3-N, which paired with the lack of hard X-rays implies an obscuring column density above the Compton-thick regime. The [Ne\u202fV] line is not detected in O3-S, but we measure a He\u202fIIλ 4687 /Hβ = 0.25, which is well above the expectation for star formation. Despite the remarkable alignment of O3-N and O3-S with two radio sources, we do not find evidence of shocks from a radio jet that could be powering the EELRs. We interpret this as O3-S being externally irradiated by the AGN, akin to the famous Hanny’s Voorwerp object in the local Universe. In addition, more classical line ratio diagnostics (e.g., [O\u202fIII]/Hβ vs [N\u202fII]/Hα) put the DSFG itself in the AGN region of the diagrams, and therefore suggest it to be the most probable AGN host. These results showcase the ability of JWST to unveil obscured AGN at high redshifts.
\n
",
"doi": "10.1051/0004-6361/202451551",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2025-01",
"volume": "693",
"pages": "A70"
},
{
"id": "authors:1t5gh-pjs28",
"collection": "authors",
"collection_id": "1t5gh-pjs28",
"cite_using_url": "https://authors.library.caltech.edu/records/1t5gh-pjs28",
"type": "article",
"title": "Predicting the Spectroscopic Features of Galaxies by Applying Manifold Learning on Their Broadband Colors: Proof of Concept and Potential Applications for Euclid, Roman, and Rubin LSST",
"author": [
{
"family_name": "Jafariyazani",
"given_name": "Marziye",
"orcid": "0000-0001-8019-6661",
"clpid": "Jafariyazani-Marziye"
},
{
"family_name": "Masters",
"given_name": "Daniel",
"orcid": "0000-0001-5382-6138",
"clpid": "Masters-Daniel"
},
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Teplitz",
"given_name": "Harry I.",
"orcid": "0000-0002-7064-5424",
"clpid": "Teplitz-Harry-I"
},
{
"family_name": "Ilbert",
"given_name": "Olivier",
"orcid": "0000-0002-7303-4397",
"clpid": "Ilbert-Olivier"
}
],
"abstract": "\n
Entering the era of large-scale galaxy surveys, which will deliver unprecedented amounts of photometric and spectroscopic data, there is a growing need for more efficient, data-driven, and less model-dependent techniques to analyze the spectral energy distribution of galaxies. In this work, we demonstrate that by taking advantage of manifold learning approaches, we can estimate spectroscopic features of large samples of galaxies from their broadband photometry when spectroscopy is available only for a fraction of the sample. This will be done by applying the self-organizing map algorithm on broadband colors of galaxies and mapping partially available spectroscopic information into the trained maps. In this pilot study, we focus on estimating the 4000 Å break in a magnitude-limited sample of galaxies in the Cosmic Evolution Survey (COSMOS) field. We also examine this method to predict the HδA index given our available spectroscopic measurements. We use observed galaxy colors (u,g,r,i,z,Y,J,H), as well as spectroscopic measurements for a fraction of the sample from the LEGA-C and zCOSMOS spectroscopic surveys to estimate this feature for our parent photometric sample. We recover the D4000 feature for galaxies that only have broadband colors with uncertainties about twice the uncertainty of the employed spectroscopic surveys. Using these measurements, we observe a positive correlation between D4000 and the stellar mass of the galaxies in our sample with weaker D4000 features for higher-redshift galaxies at fixed stellar masses. These can be explained by the downsizing scenario for the formation of galaxies and the decrease in their specific star formation rate as well as the aging of their stellar populations over this time period.
\n
\n
We report the discovery of 15 exceptionally luminous 10 \u2272 z \u2272 14 candidate galaxies discovered in the first 0.28 deg2 of JWST/NIRCam imaging from the COSMOS-Web survey. These sources span rest-frame UV magnitudes of −20.5 > MUV > −22, and thus constitute the most intrinsically luminous z \u2273 10 candidates identified by JWST to date. Selected via NIRCam imaging, deep ground-based observations corroborate their detection and help significantly constrain their photometric redshifts. We analyze their spectral energy distributions using multiple open-source codes and evaluate the probability of low-redshift solutions; we conclude that 12/15 (80%) are likely genuine z \u2273 10 sources and 3/15 (20%) likely low-redshift contaminants. Three of our z ∼ 12 candidates push the limits of early stellar mass assembly: they have estimated stellar masses ∼ 5 × 109M\u2299, implying an effective stellar baryon fraction of ε\u22c6 ∼ 0.2−0.5, where ε\u22c6 ≡ M\u22c6/(fbMhalo). The assembly of such stellar reservoirs is made possible due to rapid, burst-driven star formation on timescales < 100 Myr where the star formation rate may far outpace the growth of the underlying dark matter halos. This is supported by the similar volume densities inferred for M\u22c6 ∼ 1010M\u2299 galaxies relative to M\u22c6 ∼ 109M\u2299—both about 10−6 Mpc−3—implying they live in halos of comparable mass. At such high redshifts, the duty cycle for starbursts would be of order unity, which could cause the observed change in the shape of the UV luminosity function from a double power law to a Schechter function at z ≈ 8. Spectroscopic redshift confirmation and ensuing constraints of their masses will be critical to understand how, and if, such early massive galaxies push the limits of galaxy formation in the Lambda cold dark matter paradigm.
\n
\n
The ability to determine galaxy properties such as masses, ages, and star formation rates robustly is critically limited by the ability to measure dust attenuation accurately. Dust reddening is often characterized by comparing observations to models of either nebular recombination lines or the UV continuum. Here, we use a new technique to measure dust reddening by exploiting the He iiλ1640 and λ4686 emission lines originating from the stellar winds of Wolf–Rayet stars. The intrinsic line ratio is determined by atomic physics, enabling an estimate of the stellar reddening similar to how the Balmer lines probe gas-emission reddening. The He ii line ratio is measured from UV and optical spectroscopy using the Space Telescope Imaging Spectrograph on board the Hubble Space Telescope for eight nearby galaxies hosting young massive star clusters. We compare our results to dust reddening values estimated from UV spectral slopes and from Balmer line ratios and find tentative evidence for systematic differences. The reddening derived from the He ii lines tends to be higher, whereas that from the UV continuum tends to be lower. A larger sample size is needed to confirm this trend. If confirmed, this may indicate an age sequence probing different stages of dust clearing. Broad He ii lines have also been detected in galaxies more distant than in our sample, providing the opportunity to estimate the dust reddening of the youngest stellar populations out to distances of ∼100 Mpc.
\n
In this Letter, we report the discovery of the highest redshift, heavily obscured, radio-loud (RL) active galactic nucleus (AGN) candidate selected using JWST NIRCam/MIRI, mid-IR, submillimeter, and radio imaging in the COSMOS-Web field. Using multifrequency radio observations and mid-IR photometry, we identify a powerful, RL, growing supermassive black hole with significant spectral steepening of the radio spectral energy distribution (f1.28 GHz ∼ 2 mJy, q24 μm = −1.1, α1.28−3 GHz = − 1.2, Δα = − 0.4). In conjunction with ALMA, deep ground-based observations, ancillary space-based data, and the unprecedented resolution and sensitivity of JWST, we find no evidence of AGN contribution to the UV/optical/near-infrared (NIR) data and thus infer heavy amounts of obscuration (NH > 1023 cm−2). Using the wealth of deep UV to submillimeter photometric data, we report a singular solution photo-z of zphot = 7.7_(−0.3)^(+0.4) and estimate an extremely massive host galaxy (log M\u22c6 = 11.92 ± 0.5 M\u2299) hosting a powerful, growing supermassive black hole (LBol = 4−12x × 1046 erg s−1). This source represents the farthest known obscured RL AGN candidate, and its level of obscuration aligns with the most representative but observationally scarce population of AGN at these epochs.
",
"doi": "10.3847/2041-8213/ad11ee",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2024-01-20",
"series_number": "1",
"volume": "961",
"issue": "1",
"pages": "L25"
},
{
"id": "authors:ngbav-6n667",
"collection": "authors",
"collection_id": "ngbav-6n667",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230727-911770600.12",
"type": "article",
"title": "Resolving Galactic-scale Obscuration of X-Ray AGNs at z \u2273 1 with COSMOS-Web",
"author": [
{
"family_name": "Silverman",
"given_name": "John D.",
"orcid": "0000-0002-0000-6977",
"clpid": "Silverman-John-D"
},
{
"family_name": "Mainieri",
"given_name": "Vincenzo",
"orcid": "0000-0002-1047-9583",
"clpid": "Mainieri-Vincenzo"
},
{
"family_name": "Ding",
"given_name": "Xuheng",
"orcid": "0000-0001-8917-2148",
"clpid": "Ding-Xuheng"
},
{
"family_name": "Liu",
"given_name": "Daizhong",
"orcid": "0000-0001-9773-7479",
"clpid": "Liu-Daizhong"
},
{
"family_name": "Jahnke",
"given_name": "Knud",
"orcid": "0000-0003-3804-2137",
"clpid": "Jahnke-Knud"
},
{
"family_name": "Hirschmann",
"given_name": "Michaela",
"orcid": "0000-0002-3301-3321",
"clpid": "Hirschmann-Michaela"
},
{
"family_name": "Kartaltepe",
"given_name": "Jeyhan S.",
"orcid": "0000-0001-9187-3605",
"clpid": "Kartaltepe-Jeyhan-S"
},
{
"family_name": "Lambrides",
"given_name": "Erini",
"orcid": "0000-0003-3216-7190",
"clpid": "Lambrides-Erini"
},
{
"family_name": "Onoue",
"given_name": "Masafusa",
"orcid": "0000-0003-2984-6803",
"clpid": "Onoue-Masafusa"
},
{
"family_name": "Trakhtenbrot",
"given_name": "Benny",
"orcid": "0000-0002-3683-7297",
"clpid": "Trakhtenbrot-Benny"
},
{
"family_name": "Vardoulaki",
"given_name": "Eleni",
"orcid": "0000-0002-4437-1773",
"clpid": "Vardoulaki-Eleni"
},
{
"family_name": "Bongiorno",
"given_name": "Angela",
"orcid": "0000-0002-0101-6624",
"clpid": "Bongiorno-Angela"
},
{
"family_name": "Casey",
"given_name": "Caitlin M.",
"orcid": "0000-0002-0930-6466",
"clpid": "Casey-Caitlin-M"
},
{
"family_name": "Civano",
"given_name": "Francesca",
"orcid": "0000-0002-2115-1137",
"clpid": "Civano-Francesca"
},
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Franco",
"given_name": "Maximilien",
"orcid": "0000-0002-3560-8599",
"clpid": "Franco-Maximilien"
},
{
"family_name": "Gillman",
"given_name": "Steven",
"orcid": "0000-0001-9885-4589",
"clpid": "Gillman-Steven"
},
{
"family_name": "Gozaliasl",
"given_name": "Ghassem",
"orcid": "0000-0002-0236-919X",
"clpid": "Gozaliasl-Ghassem"
},
{
"family_name": "Hayward",
"given_name": "Christopher C.",
"orcid": "0000-0003-4073-3236",
"clpid": "Hayward-Christopher-C"
},
{
"family_name": "Koekemoer",
"given_name": "Anton M.",
"orcid": "0000-0002-6610-2048",
"clpid": "Koekemoer-Anton-M"
},
{
"family_name": "Kokorev",
"given_name": "Vasily",
"orcid": "0000-0002-5588-9156",
"clpid": "Kokorev-Vasily"
},
{
"family_name": "Magdis",
"given_name": "Georgios E.",
"orcid": "0000-0002-4872-2294",
"clpid": "Magdis-Georgios-E"
},
{
"family_name": "Marchesi",
"given_name": "Stefano",
"orcid": "0000-0001-5544-0749",
"clpid": "Marchesi-Stefano"
},
{
"family_name": "Rich",
"given_name": "Robert Michael",
"orcid": "0000-0003-0427-8387",
"clpid": "Rich-Robert-Michael"
},
{
"family_name": "Sparre",
"given_name": "Martin",
"orcid": "0000-0002-9735-3851",
"clpid": "Sparre-Martin"
},
{
"family_name": "Suh",
"given_name": "Hyewon",
"orcid": "0000-0002-2536-1633",
"clpid": "Suh-Hyewon"
},
{
"family_name": "Tanaka",
"given_name": "Takumi",
"clpid": "Tanaka-Takumi"
},
{
"family_name": "Valentino",
"given_name": "Francesco",
"orcid": "0000-0001-6477-4011",
"clpid": "Valentino-Francesco-M"
}
],
"abstract": "A large fraction of the accreting supermassive black hole population is shrouded by copious amounts of gas and dust, particularly in the distant (z \u2273 1) universe. While much of the obscuration is attributed to a parsec-scale torus, there is a known contribution from the larger-scale host galaxy. Using JWST/NIRCam imaging from the COSMOS-Web survey, we probe the galaxy-wide dust distribution in X-ray selected active galactic nuclei (AGNs) up to z \u223c 2. Here, we focus on a sample of three AGNs with their host galaxies exhibiting prominent dust lanes, potentially due to their edge-on alignment. These represent 27% (3 out of 11 with early NIRCam data) of the heavily obscured (N_H > 10\u00b2\u00b3 cm\u207b\u00b2) AGN population. With limited signs of a central AGN in the optical and near-infrared, the NIRCam images are used to produce reddening maps E(B \u2212 V) of the host galaxies. We compare the mean central value of E(B \u2212 V) to the X-ray obscuring column density along the line of sight to the AGN (N_H \u223c 10^(23\u221223.5) cm\u207b\u00b2). We find that the extinction due to the host galaxy is present (0.6 \u2272 E(B \u2212 V) \u2272 0.9; 1.9 \u2272 A_V \u2272 2.8) and significantly contributes to the X-ray obscuration at a level of N_H \u223c 10^(22.5) cm\u207b\u00b2 assuming an SMC gas-to-dust ratio that amounts to \u227230% of the total obscuring column density. These early results, including three additional cases from CEERS, demonstrate the ability to resolve such dust structures with JWST and separate the different circumnuclear and galaxy-scale obscuring structures.",
"doi": "10.3847/2041-8213/acdef4",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2023-07-10",
"series_number": "2",
"volume": "951",
"issue": "2",
"pages": "Art. No. L41"
},
{
"id": "authors:fnxna-kwb35",
"collection": "authors",
"collection_id": "fnxna-kwb35",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230530-441768000.58",
"type": "article",
"title": "An Atlas of Color-selected Quiescent Galaxies at z > 3 in Public JWST Fields",
"author": [
{
"family_name": "Valentino",
"given_name": "Francesco",
"orcid": "0000-0001-6477-4011",
"clpid": "Valentino-Francesco-M"
},
{
"family_name": "Brammer",
"given_name": "Gabriel",
"orcid": "0000-0003-2680-005X"
},
{
"family_name": "Gould",
"given_name": "Katriona M. L.",
"orcid": "0000-0003-4196-5960"
},
{
"family_name": "Kokorev",
"given_name": "Vasily",
"orcid": "0000-0002-5588-9156"
},
{
"family_name": "Fujimoto",
"given_name": "Seiji",
"orcid": "0000-0001-7201-5066"
},
{
"family_name": "Jespersen",
"given_name": "Christian Kragh",
"orcid": "0000-0002-8896-6496"
},
{
"family_name": "Vijayan",
"given_name": "Aswin P.",
"orcid": "0000-0002-1905-4194"
},
{
"family_name": "Weaver",
"given_name": "John R.",
"orcid": "0000-0003-1614-196X"
},
{
"family_name": "Ito",
"given_name": "Kei",
"orcid": "0000-0002-9453-0381"
},
{
"family_name": "Tanaka",
"given_name": "Masayuki",
"orcid": "0000-0002-5011-5178"
},
{
"family_name": "Ilbert",
"given_name": "Olivier",
"orcid": "0000-0002-7303-4397"
},
{
"family_name": "Magdis",
"given_name": "Georgios E.",
"orcid": "0000-0002-4872-2294"
},
{
"family_name": "Whitaker",
"given_name": "Katherine E.",
"orcid": "0000-0001-7160-3632"
},
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Gallazzi",
"given_name": "Anna",
"orcid": "0000-0002-9656-1800"
},
{
"family_name": "Gillman",
"given_name": "Steven",
"orcid": "0000-0001-9885-4589"
},
{
"family_name": "Gim\u00e9nez-Arteaga",
"given_name": "Clara",
"orcid": "0000-0001-9419-9505"
},
{
"family_name": "G\u00f3mez-Guijarro",
"given_name": "Carlos",
"orcid": "0000-0002-4085-9165"
},
{
"family_name": "Kubo",
"given_name": "Mariko",
"orcid": "0000-0002-7598-5292"
},
{
"family_name": "Heintz",
"given_name": "Kasper E.",
"orcid": "0000-0002-9389-7413"
},
{
"family_name": "Hirschmann",
"given_name": "Michaela",
"orcid": "0000-0002-3301-3321"
},
{
"family_name": "Oesch",
"given_name": "Pascal",
"orcid": "0000-0001-5851-6649"
},
{
"family_name": "Onodera",
"given_name": "Masato",
"orcid": "0000-0003-3228-7264"
},
{
"family_name": "Rizzo",
"given_name": "Francesca",
"orcid": "0000-0001-9705-2461"
},
{
"family_name": "Lee",
"given_name": "Minju",
"orcid": "0000-0002-2419-3068"
},
{
"family_name": "Strait",
"given_name": "Victoria",
"orcid": "0000-0002-6338-7295"
},
{
"family_name": "Toft",
"given_name": "Sune",
"orcid": "0000-0003-3631-7176"
}
],
"abstract": "We present the results of a systematic search for candidate quiescent galaxies in the distant Universe in eleven JWST ields with publicly available observations collected during the first three months of operations and covering an effective sky area of ~ 145 arcmin\u00b2. We homogeneously reduce the new JWST data and combine them with existing observations from the Hubble Space Telescope. We select a robust sample of ~ 80 candidate quiescent and quenching galaxies at 3 < z < 5 using two methods: (1) based on their rest-frame UVJ colors, and (2) a novel quantitative approach based on Gaussian Mixture Modeling of the NUV - U,U - V, and V - J rest-frame color space, which is more sensitive to recently quenched objects. We measure comoving number densities of massive (M_* \u2265 10\u00b9\u2070\u00b7\u2076 M_\u2299) quiescent galaxies consistent with previous estimates relying on ground-based observations, after homogenizing the results in the literature with our mass and redshift intervals. However, we find significant field-to-field variations of the number densities up to a factor of 2 - 3, highlighting the effect of cosmic variance and suggesting the presence of overdensities of red quiescent galaxies at z > 3, as it could be expected for highly clustered massive systems. Importantly, JWST enables the robust identification of quenching/quiescent galaxy candidates at lower masses and higher redshifts than before, challenging standard formation scenarios. All data products, including the literature compilation, are made publicly available.",
"doi": "10.3847/1538-4357/acbefa",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2023-04-10",
"series_number": "1",
"volume": "947",
"issue": "1",
"pages": "Art. No. 20"
},
{
"id": "authors:snknx-4jc62",
"collection": "authors",
"collection_id": "snknx-4jc62",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230321-821389800.43",
"type": "article",
"title": "A Broad-line Quasar with Unexplained Extreme Velocity Offsets: Post-shock Outflow?",
"author": [
{
"family_name": "Rusakov",
"given_name": "Vadim",
"orcid": "0000-0001-7633-3985",
"clpid": "Rusakov-Vadim"
},
{
"family_name": "Steinhardt",
"given_name": "Charles L.",
"orcid": "0000-0003-3780-6801",
"clpid": "Steinhardt-Charles-L"
},
{
"family_name": "Schramm",
"given_name": "Malte",
"orcid": "0000-0001-7825-0075",
"clpid": "Schramm-Malte"
},
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Masters",
"given_name": "Daniel",
"orcid": "0000-0001-5382-6138",
"clpid": "Masters-Daniel-C"
},
{
"family_name": "Mobasher",
"given_name": "Bahram",
"orcid": "0000-0001-5846-4404",
"clpid": "Mobasher-Bahram"
},
{
"family_name": "Pattarakijwanich",
"given_name": "Petchara",
"orcid": "0000-0001-8451-5316",
"clpid": "Pattarakijwanich-Petchara"
}
],
"abstract": "The quasar SDSS 0956 + 5128 exhibits three distinct velocity components with large offsets in emission: the systemic velocity of [O ii], [O iii], and [Ne iii] narrow lines have redshift z = 0.7142; the broad Mg ii line is shifted by \u22121200 km s\u207b\u00b9 with respect to the narrow lines; the broad H\u03b1 and H\u03b2 lines are at \u22124100 km s\u207b\u00b9. We present new Hubble Space Telescope spectra of Ly\u03b1 and C iv emission lines and high-resolution images of the quasar. The offsets of these lines are consistent with the velocity component of the Balmer emission, and the photometry in optical and near-infrared wavelengths does not show any signs of recent mergers in the host galaxy or irregularities in the location of the quasar. The data do not confirm predictions of the previous most likely hypotheses involving a special orientation and morphology of the quasar disk, such as in the recoiling black hole scenario, neither it is consistent with accretion disk winds. Instead, based on the cumulative evidence, we propose a new scenario, in which the broad-line region is in the state of outflow caused by a strong shock wave, with a supernova as a possible event for producing the shock ejecta.",
"doi": "10.3847/1538-4357/acadd8",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2023-02-20",
"series_number": "2",
"volume": "944",
"issue": "2",
"pages": "Art. No. 217"
},
{
"id": "authors:75g1e-85b23",
"collection": "authors",
"collection_id": "75g1e-85b23",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230302-365334800.4",
"type": "article",
"title": "Cosmic Evolution of Gas and Star Formation",
"author": [
{
"family_name": "Scoville",
"given_name": "Nick",
"orcid": "0000-0002-0438-3323",
"clpid": "Scoville-N-Z"
},
{
"family_name": "Faisst",
"given_name": "Andreas",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Weaver",
"given_name": "John",
"orcid": "0000-0003-1614-196X"
},
{
"family_name": "Toft",
"given_name": "Sune",
"orcid": "0000-0003-3631-7176"
},
{
"family_name": "McCracken",
"given_name": "Henry J.",
"orcid": "0000-0002-9489-7765"
},
{
"family_name": "Ilbert",
"given_name": "Olivier",
"orcid": "0000-0002-7303-4397"
},
{
"family_name": "Diaz-Santos",
"given_name": "Tanio",
"orcid": "0000-0003-0699-6083"
},
{
"family_name": "Staguhn",
"given_name": "Johannes",
"orcid": "0000-0002-8437-0433"
},
{
"family_name": "Koda",
"given_name": "Jin",
"orcid": "0000-0002-8762-7863"
},
{
"family_name": "Casey",
"given_name": "Caitlin",
"orcid": "0000-0002-0930-6466"
},
{
"family_name": "Sanders",
"given_name": "David",
"orcid": "0000-0002-1233-9998"
},
{
"family_name": "Mobasher",
"given_name": "Bahram",
"orcid": "0000-0001-5846-4404"
},
{
"family_name": "Chartab",
"given_name": "Nima",
"orcid": "0000-0003-3691-937X"
},
{
"family_name": "Sattari",
"given_name": "Zahra",
"orcid": "0000-0002-0364-1159"
},
{
"family_name": "Capak",
"given_name": "Peter",
"orcid": "0000-0003-3578-6843",
"clpid": "Capak-Peter"
},
{
"family_name": "Vanden Bout",
"given_name": "Paul A.",
"orcid": "0000-0003-3304-3974"
},
{
"family_name": "Bongiorno",
"given_name": "Angela",
"orcid": "0000-0002-0101-6624"
},
{
"family_name": "Vlahakis",
"given_name": "Catherine",
"orcid": "0000-0003-3745-4228"
},
{
"family_name": "Sheth",
"given_name": "Kartik",
"orcid": "0000-0002-5496-4118"
},
{
"family_name": "Yun",
"given_name": "Min",
"orcid": "0000-0001-7095-7543"
},
{
"family_name": "Aussel",
"given_name": "Herve",
"orcid": "0000-0002-1371-5705"
},
{
"family_name": "Laigle",
"given_name": "Clotilde"
},
{
"family_name": "Masters",
"given_name": "Dan",
"orcid": "0000-0001-5382-6138",
"clpid": "Masters-Daniel-C"
}
],
"abstract": "Atacama Large Millimeter/submillimeter Array (ALMA) observations of the long-wavelength dust continuum are used to estimate the gas masses in a sample of 708 star-forming galaxies at z = 0.3\u22124.5. We determine the dependence of gas masses and star formation efficiencies (SFEs; SFR per unit gas mass) on redshift (z), M\n *, and star formation rate (SFR) relative to the main sequence (MS). We find that 70% of the increase in SFRs of the MS is due to the increased gas masses at earlier epochs, while 30% is due to increased efficiency of star formation (SF). For galaxies above the MS this is reversed\u2014with 70% of the increased SFR relative to the MS being due to elevated SFEs. Thus, the major evolution of star formation activity at early epochs is driven by increased gas masses, while the starburst activity taking galaxies above the MS is due to enhanced triggering of star formation (likely due to galactic merging). The interstellar gas peaks at z = 2 and dominates the stellar mass down to z = 1.2. Accretion rates needed to maintain continuity of the MS evolution reach >100 M_\u2299 yr\u207b\u00b9 at z > 2. The galactic gas contents are likely the driving determinant for both the rise in SF and AGN activity from z = 5 to their peak at z = 2 and subsequent fall at lower z. We suggest that for self-gravitating clouds with supersonic turbulence, cloud collisions and the filamentary structure of the clouds regulate the star formation activity.",
"doi": "10.3847/1538-4357/aca1bc",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2023-02-01",
"series_number": "2",
"volume": "943",
"issue": "2",
"pages": "Art. No. 82"
},
{
"id": "authors:qpbp6-zd163",
"collection": "authors",
"collection_id": "qpbp6-zd163",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230103-817548100.8",
"type": "article",
"title": "What Are Those Tiny Things? A First Study of Compact Star Clusters in the SMACS0723 Field with JWST",
"author": [
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Chary",
"given_name": "Ranga Ram",
"orcid": "0000-0001-7583-0621",
"clpid": "Chary-Ranga-Ram"
},
{
"family_name": "Brammer",
"given_name": "Gabriel B.",
"orcid": "0000-0003-2680-005X",
"clpid": "Brammer-Gabriel-B"
},
{
"family_name": "Toft",
"given_name": "Sune",
"orcid": "0000-0003-3631-7176",
"clpid": "Toft-Sune"
}
],
"abstract": "We use the unprecedented resolution and depth of the JWST NIRCam Early Release Observations at 1\u20135 \u03bcm to study the stellar mass, age, and metallicity of compact star clusters in the neighborhood of the host galaxies in the SMACS J0723.3\u20137327 galaxy cluster field at z = 0.39. The measured colors of these star clusters show a similar distribution as quiescent galaxies at the same redshift, but are >3 mag fainter than the current depths of wide-field galaxy survey. The star clusters are unresolved in the NIRCam/F150W data suggesting sizes smaller than 50 pc. This is significantly smaller than star-forming clumps or dwarf galaxies in local galaxies. From fitting their photometry with simple stellar population (SSP) models, we find stellar metallicities consistent with 0.2\u20130.3 Z_\u2299 and ages of 1.5_(-0.5)^(+0.5) Gyr. We rule out metallicities <0.2 Z_\u2299 and solar/supersolar at 4\u03c3 significance. Assuming mass-to-light ratios obtained from the best-fit SSP, we estimate stellar masses of 2.4_(-1.5)^(+3.0) x 10\u2076 M_\u2299. These are between average masses of local globular clusters and dwarf galaxies. Our analysis suggests middle-aged globular cluster with relatively recent formation times at z = 0.5\u20130.7, which could have been subsequently stripped away from their host galaxies due to interactions in the cluster environment or formed in cold flows onto the cluster core. However, we cannot rule out these objects being compact cores of stripped dwarf galaxies.",
"doi": "10.3847/2041-8213/aca1bf",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2022-12-10",
"series_number": "1",
"volume": "941",
"issue": "1",
"pages": "Art. No. L11"
},
{
"id": "authors:3swrg-tk337",
"collection": "authors",
"collection_id": "3swrg-tk337",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20221206-898533400.1",
"type": "article",
"title": "A new look at the infrared properties of z \u223c 5 galaxies",
"author": [
{
"family_name": "Sommovigo",
"given_name": "L.",
"orcid": "0000-0002-2906-2200",
"clpid": "Sommovigo-Laura"
},
{
"family_name": "Ferrara",
"given_name": "A.",
"orcid": "0000-0002-9400-7312",
"clpid": "Ferrara-Andrea"
},
{
"family_name": "Carniani",
"given_name": "S.",
"orcid": "0000-0002-6719-380X",
"clpid": "Carniani-Stefano"
},
{
"family_name": "Pallottini",
"given_name": "A.",
"orcid": "0000-0002-7129-5761",
"clpid": "Pallottini-Andrea"
},
{
"family_name": "Dayal",
"given_name": "P.",
"clpid": "Dayal-P"
},
{
"family_name": "Pizzati",
"given_name": "E.",
"orcid": "0000-0002-9712-0038",
"clpid": "Pizzati-Elia"
},
{
"family_name": "Ginolfi",
"given_name": "M.",
"orcid": "0000-0002-9122-1700",
"clpid": "Ginolfi-Michelle"
},
{
"family_name": "Markov",
"given_name": "V.",
"orcid": "0000-0002-5694-6124",
"clpid": "Markov-Vladan"
},
{
"family_name": "Faisst",
"given_name": "A.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
}
],
"abstract": "Recent Atacama Large Millimeter Array large surveys unveiled the presence of significant dust continuum emission in star-forming galaxies at z > 4. Unfortunately, such large programs \u2013 i.e. ALPINE (z \u223c 5) and REBELS (z \u223c 7) \u2013 only provide us with a single far-infrared (FIR) continuum data point for their individual targets. Therefore, high-z galaxies FIR spectral energy densities (SEDs) remain mostly unconstrained, hinging on an assumption for their dust temperature (T_d) in the SED fitting procedure. This introduces uncertainties in the inferred dust masses (M_d), infrared luminosities (L_(IR)), and obscured star formation rate (SFR) fraction at z > 4. In this work, we use a method that allows us to constrain T_d with a single-band measurement by combining the 158\u2009\u00b5m continuum information with the overlying [C\u2009\u026a\u026a emission line. We analyse the 21 [C\u2009\u026a\u026a and FIR continuum-detected z \u223c 5 galaxies in ALPINE, finding a range of T_d = 25\u201360\u2009K and M_d = 0.6\u201325.1\u2009\u00d7 10\u2077\u2009M_\u2299. Given the measured stellar masses of ALPINE galaxies, the inferred dust yields are around M_d/M_\u22c6 = (0.2\u20138) \u00d7 10\u207b\u00b3, consistent with theoretical dust-production constraints. We find that eight out of the 21 ALPINE galaxies have L_(IR) \u2265 10\u00b9\u00b2\u2009L_\u2299, comparable to ultraluminous IR galaxies (ULIRGs). Relying on ultraviolet-to-optical SED fitting, the SFR was underestimated by up to two orders of magnitude in four of these eight ULIRGs-like galaxies. We conclude that these four peculiar sources should be characterized by a two-phase interstellar medium structure with 'spatially segregated' FIR and ultraviolet emitting regions.",
"doi": "10.1093/mnras/stac2997",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2022-12",
"series_number": "4",
"volume": "517",
"issue": "4",
"pages": "5930-5941"
},
{
"id": "authors:an2af-12f47",
"collection": "authors",
"collection_id": "an2af-12f47",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220803-224717000",
"type": "article",
"title": "The ALMA REBELS Survey: Average [C ii] 158 \u03bcm Sizes of Star-forming Galaxies from z \u223c 7 to z \u223c 4",
"author": [
{
"family_name": "Fudamoto",
"given_name": "Y.",
"orcid": "0000-0001-7440-8832",
"clpid": "Fudamoto-Yoshinobu"
},
{
"family_name": "Smit",
"given_name": "R.",
"orcid": "0000-0001-8034-7802"
},
{
"family_name": "Bowler",
"given_name": "R. A. A.",
"orcid": "0000-0003-3917-1678"
},
{
"family_name": "Oesch",
"given_name": "P. A.",
"orcid": "0000-0001-5851-6649"
},
{
"family_name": "Bouwens",
"given_name": "R.",
"orcid": "0000-0002-4989-2471"
},
{
"family_name": "Stefanon",
"given_name": "M.",
"orcid": "0000-0001-7768-5309"
},
{
"family_name": "Inami",
"given_name": "H.",
"orcid": "0000-0003-4268-0393"
},
{
"family_name": "Endsley",
"given_name": "R.",
"orcid": "0000-0003-4564-2771"
},
{
"family_name": "Gonzalez",
"given_name": "V.",
"orcid": "0000-0002-3120-0510"
},
{
"family_name": "Schouws",
"given_name": "S.",
"orcid": "0000-0001-9746-0924"
},
{
"family_name": "Stark",
"given_name": "D.",
"orcid": "0000-0001-6106-5172"
},
{
"family_name": "Algera",
"given_name": "H. S. B.",
"orcid": "0000-0002-4205-9567"
},
{
"family_name": "Aravena",
"given_name": "M.",
"orcid": "0000-0002-6290-3198"
},
{
"family_name": "Barrufet",
"given_name": "L.",
"orcid": "0000-0003-1641-6185"
},
{
"family_name": "da Cunha",
"given_name": "E.",
"orcid": "0000-0001-9759-4797"
},
{
"family_name": "Dayal",
"given_name": "P.",
"orcid": "0000-0001-8460-1564"
},
{
"family_name": "Ferrara",
"given_name": "A.",
"orcid": "0000-0002-9400-7312"
},
{
"family_name": "Graziani",
"given_name": "L.",
"orcid": "0000-0002-9231-1505"
},
{
"family_name": "Hodge",
"given_name": "J. A.",
"orcid": "0000-0001-6586-8845"
},
{
"family_name": "Hygate",
"given_name": "A. P. S.",
"orcid": "0000-0002-6488-471X"
},
{
"family_name": "Inoue",
"given_name": "A. K.",
"orcid": "0000-0002-7779-8677"
},
{
"family_name": "Nanayakkara",
"given_name": "T.",
"orcid": "0000-0003-2804-0648"
},
{
"family_name": "Pallottini",
"given_name": "A."
},
{
"family_name": "Pizzati",
"given_name": "E.",
"orcid": "0000-0002-9712-0038"
},
{
"family_name": "Schneider",
"given_name": "R.",
"orcid": "0000-0001-9317-2888"
},
{
"family_name": "Sommovigo",
"given_name": "L."
},
{
"family_name": "Sugahara",
"given_name": "Y.",
"orcid": "0000-0001-6958-7856"
},
{
"family_name": "Topping",
"given_name": "M.",
"orcid": "0000-0001-8426-1141"
},
{
"family_name": "van der Werf",
"given_name": "P.",
"orcid": "0000-0001-5434-5942"
},
{
"family_name": "Bethermin",
"given_name": "M.",
"orcid": "0000-0002-3915-2015"
},
{
"family_name": "Cassata",
"given_name": "P.",
"orcid": "0000-0002-6716-4400"
},
{
"family_name": "Dessauges-Zavadsky",
"given_name": "M.",
"orcid": "0000-0003-0348-2917"
},
{
"family_name": "Ibar",
"given_name": "E."
},
{
"family_name": "Faisst",
"given_name": "A. L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Fujimoto",
"given_name": "S.",
"orcid": "0000-0001-7201-5066"
},
{
"family_name": "Ginolfi",
"given_name": "M.",
"orcid": "0000-0002-9122-1700"
},
{
"family_name": "Hathi",
"given_name": "N.",
"orcid": "0000-0001-6145-5090"
},
{
"family_name": "Jones",
"given_name": "G. C.",
"orcid": "0000-0002-0267-9024"
},
{
"family_name": "Pozzi",
"given_name": "F.",
"orcid": "0000-0002-7412-647X"
},
{
"family_name": "Schaerer",
"given_name": "D.",
"orcid": "0000-0001-7144-7182"
}
],
"abstract": "We present the average [C ii] 158 \u03bcm emission line sizes of UV-bright star-forming galaxies at z \u223c 7. Our results are derived from a stacking analysis of [C ii] 158 \u03bcm emission lines and dust continua observed by the Atacama Large Millimeter/submillimeter Array (ALMA), taking advantage of the large program Reionization Era Bright Emission Line Survey. We find that the average [C ii] emission at z \u223c 7 has an effective radius r\u2091 of 2.2 \u00b1 0.2 kpc. It is \u2273 2\u00d7 larger than the dust continuum and the rest-frame UV emission, in agreement with recently reported measurements for z \u2272 6 galaxies. Additionally, we compared the average [C ii] size with 4 z ii] at Early times (ALPINE). By analyzing [C ii] sizes of 4 z ii] size of r\u2091 = 2.2 \u00b1 0.2 kpc and r\u2091 = 2.5 \u00b1 0.2 kpc for z \u223c 5.5 and z \u223c 4.5 galaxies, respectively. These measurements show that star-forming galaxies, on average, show no evolution in the size of the [C ii] 158 \u03bcm emitting regions at redshift between z \u223c 7 and z \u223c 4. This finding suggests that the star-forming galaxies could be morphologically dominated by gas over a wide redshift range.",
"doi": "10.3847/1538-4357/ac7a47",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2022-08-01",
"series_number": "2",
"volume": "934",
"issue": "2",
"pages": "Art. No. 144"
},
{
"id": "authors:e8pz7-13j89",
"collection": "authors",
"collection_id": "e8pz7-13j89",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220830-526643700.782",
"type": "article",
"title": "The ALPINE\u2013ALMA [C II] Survey: The Infrared\u2013Radio Correlation and Active Galactic Nucleus Fraction of Star-forming Galaxies at z \u223c 4.4\u20135.9",
"author": [
{
"family_name": "Shen",
"given_name": "Lu",
"orcid": "0000-0001-9495-7759",
"clpid": "Shen-Lu"
},
{
"family_name": "Lemaux",
"given_name": "Brian C.",
"orcid": "0000-0002-1428-7036",
"clpid": "Lemaux-B-C"
},
{
"family_name": "Lubin",
"given_name": "Lori M.",
"orcid": "0000-0003-2119-8151"
},
{
"family_name": "Liu",
"given_name": "Guilin",
"orcid": "0000-0003-2390-7927",
"clpid": "Liu-Guilin"
},
{
"family_name": "B\u00e9thermin",
"given_name": "Matthieu",
"orcid": "0000-0002-3915-2015",
"clpid": "B\u00e9thermin-Matthieu"
},
{
"family_name": "Boquien",
"given_name": "M\u00e9d\u00e9ric",
"orcid": "0000-0003-0946-6176",
"clpid": "Boquien-M\u00e9d\u00e9ric"
},
{
"family_name": "Cucciati",
"given_name": "Olga",
"orcid": "0000-0002-9336-7551",
"clpid": "Cucciati-O"
},
{
"family_name": "Le F\u00e8vre",
"given_name": "Olivier",
"orcid": "0000-0001-5891-2596",
"clpid": "Le-F\u00e8vre-O"
},
{
"family_name": "Talia",
"given_name": "Margherita",
"orcid": "0000-0003-4352-2063",
"clpid": "Talia-Margherita"
},
{
"family_name": "Vergani",
"given_name": "Daniela",
"orcid": "0000-0003-0898-2216",
"clpid": "Vergani-Daniela"
},
{
"family_name": "Zamorani",
"given_name": "Gianni",
"orcid": "0000-0002-2318-301X"
},
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Ginolfi",
"given_name": "Michele",
"orcid": "0000-0002-9122-1700"
},
{
"family_name": "Gruppioni",
"given_name": "Carlotta",
"orcid": "0000-0002-5836-4056"
},
{
"family_name": "Jones",
"given_name": "Gareth C."
},
{
"family_name": "Bardelli",
"given_name": "Sandro",
"orcid": "0000-0002-8900-0298"
},
{
"family_name": "Hathi",
"given_name": "Nimish",
"orcid": "0000-0001-6145-5090"
},
{
"family_name": "Koekemoer",
"given_name": "Anton M.",
"orcid": "0000-0002-6610-2048"
},
{
"family_name": "Romano",
"given_name": "Michael",
"orcid": "0000-0002-9948-3916"
},
{
"family_name": "Schaerer",
"given_name": "Daniel",
"orcid": "0000-0001-7144-7182"
},
{
"family_name": "Zucca",
"given_name": "Elena",
"orcid": "0000-0002-5845-8132"
},
{
"family_name": "Fang",
"given_name": "Wenjuan",
"orcid": "0000-0003-4987-7340"
},
{
"family_name": "Forrest",
"given_name": "Ben",
"orcid": "0000-0001-6003-0541"
},
{
"family_name": "Gal",
"given_name": "Roy",
"orcid": "0000-0001-8255-6560"
},
{
"family_name": "Hung",
"given_name": "Denise",
"orcid": "0000-0001-7523-140X"
},
{
"family_name": "Shah",
"given_name": "Ekta A.",
"orcid": "0000-0001-7811-9042"
},
{
"family_name": "Staab",
"given_name": "Priti",
"orcid": "0000-0002-8877-4320"
},
{
"family_name": "Vanderhoof",
"given_name": "Brittany",
"orcid": "0000-0002-8163-0172"
},
{
"family_name": "Ibar",
"given_name": "Eduardo"
}
],
"abstract": "We present the radio properties of 66 spectroscopically confirmed normal star-forming galaxies (SFGs) at 4.4 < z < 5.9 in the COSMOS field that were [C II]-detected in the Atacama Large Millimeter/submillimeter Array Large Program to INvestigate [C II] at Early times (ALPINE). We separate these galaxies (\"C II-detected-all\") into lower-redshift (\"C II-detected-lz\"; \u3008z\u3009 = 4.5) and higher-redshift (\"C II-detected-hz\"; \u3008z\u3009 = 5.6) subsamples, and stack multiwavelength imaging for each subsample from X-ray to radio bands. A radio signal is detected in the stacked 3 GHz images of the C II-detected-all and lz samples at \u22733\u03c3. We find that the infrared\u2013radio correlation of our sample, quantified by q_TIR, is lower than the local relation for normal SFGs at a \u223c3\u03c3 significance level, and is instead broadly consistent with that of bright submillimeter galaxies at 2 < z < 5. Neither of these samples show evidence of dominant active galactic nucleus activity in their stacked spectral energy distributions (SEDs), UV spectra, or stacked X-ray images. Although we cannot rule out the possible effects of the assumed spectral index and applied infrared SED templates in causing these differences, at least partially, the lower obscured fraction of star formation than at lower redshift can alleviate the tension between our stacked q_(TIR)s and those of local normal SFGs. It is possible that the dust buildup, which primarily governs the infrared emission, in addition to older stellar populations, has not had enough time to occur fully in these galaxies, whereas the radio emission can respond on a more rapid timescale. Therefore, we might expect a lower q_TIR to be a general property of high-redshift SFGs.",
"doi": "10.3847/1538-4357/ac81c5",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2022-08-01",
"series_number": "2",
"volume": "935",
"issue": "2",
"pages": "177"
},
{
"id": "authors:hjp7j-70e37",
"collection": "authors",
"collection_id": "hjp7j-70e37",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220805-204876000",
"type": "article",
"title": "The ALMA-ALPINE [CII] survey - The star formation history and the dust emission of star-forming galaxies at 4.5 < z < 6.2\u00b0",
"author": [
{
"family_name": "Burgarella",
"given_name": "D.",
"orcid": "0000-0002-4193-2539",
"clpid": "Burgarella-Denis"
},
{
"family_name": "Bogdanoska",
"given_name": "J."
},
{
"family_name": "Nanni",
"given_name": "A."
},
{
"family_name": "Bardelli",
"given_name": "S.",
"orcid": "0000-0002-8900-0298"
},
{
"family_name": "B\u00e9thermin",
"given_name": "M.",
"orcid": "0000-0002-3915-2015"
},
{
"family_name": "Boquien",
"given_name": "M.",
"orcid": "0000-0003-0946-6176"
},
{
"family_name": "Buat",
"given_name": "V.",
"orcid": "0000-0003-3441-903X"
},
{
"family_name": "Faisst",
"given_name": "A. L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Dessauges-Zavadsky",
"given_name": "M.",
"orcid": "0000-0003-0348-2917"
},
{
"family_name": "Fudamoto",
"given_name": "Y.",
"orcid": "0000-0001-7440-8832"
},
{
"family_name": "Fujimoto",
"given_name": "S.",
"orcid": "0000-0001-7201-5066"
},
{
"family_name": "Giavalisco",
"given_name": "M.",
"orcid": "0000-0002-7831-8751"
},
{
"family_name": "Ginolfi",
"given_name": "M.",
"orcid": "0000-0002-8231-821X"
},
{
"family_name": "Gruppioni",
"given_name": "C.",
"orcid": "0000-0002-5836-4056"
},
{
"family_name": "Hathi",
"given_name": "N. P.",
"orcid": "0000-0001-6145-5090"
},
{
"family_name": "Ibar",
"given_name": "E."
},
{
"family_name": "Jones",
"given_name": "G. C.",
"orcid": "0000-0002-0267-9024"
},
{
"family_name": "Koekemoer",
"given_name": "A. M.",
"orcid": "0000-0002-6610-2048"
},
{
"family_name": "Kohno",
"given_name": "K.",
"orcid": "0000-0002-4052-2394"
},
{
"family_name": "Lemaux",
"given_name": "B. C.",
"orcid": "0000-0002-1428-7036"
},
{
"family_name": "Narayanan",
"given_name": "D.",
"orcid": "0000-0002-7064-4309"
},
{
"family_name": "Oesch",
"given_name": "P.",
"orcid": "0000-0001-5851-6649"
},
{
"family_name": "Ouchi",
"given_name": "M.",
"orcid": "0000-0002-1049-6658"
},
{
"family_name": "Riechers",
"given_name": "D. A.",
"orcid": "0000-0001-9585-1462"
},
{
"family_name": "Pozzi",
"given_name": "F.",
"orcid": "0000-0002-7412-647X"
},
{
"family_name": "Romano",
"given_name": "M.",
"orcid": "0000-0002-9948-3916"
},
{
"family_name": "Schaerer",
"given_name": "D.",
"orcid": "0000-0001-7144-7182"
},
{
"family_name": "Talia",
"given_name": "M.",
"orcid": "0000-0003-4352-2063"
},
{
"family_name": "Theul\u00e9",
"given_name": "P."
},
{
"family_name": "Vergani",
"given_name": "D.",
"orcid": "0000-0003-0898-2216"
},
{
"family_name": "Zamorani",
"given_name": "G.",
"clpid": "Zamorani-G"
},
{
"family_name": "Zucca",
"given_name": "E.",
"orcid": "0000-0002-5845-8132"
},
{
"family_name": "Cassata",
"given_name": "P.",
"orcid": "0000-0002-6716-4400"
},
{
"literal": "ALPINE Team"
}
],
"abstract": "Star-forming galaxies are composed of various types of galaxies. However, the luminosity functions at z\u2004\u2273\u20044\u20135 suggest that most galaxies have a relatively low stellar mass (log M_(star)\u2004\u223c\u200410) and a low dust attenuation (A_(FUV)\u2004\u223c\u20041.0). The physical properties of these objects are quite homogeneous. We used an approach where we combined their rest-frame far-infrared and submillimeter emissions and utilized the universe and the redshift as a spectrograph to increase the amount of information in a collective way. From a subsample of 27 ALMA-detected galaxies at z\u2004>\u20044.5, we built an infrared spectral energy distribution composite template. It was used to fit, with CIGALE, the 105 galaxies (detections and upper limits) in the sample from the far-ultraviolet to the far-infrared. The derived physical parameters provide information to decipher the nature of the dust cycle and of the stellar populations in these galaxies. The derived IR composite template is consistent with the galaxies in the studied sample. A delayed star formation history with \u03c4_(main)\u2004=\u2004500 Myr is slightly favored by the statistical analysis as compared to a delayed with a final burst or a continuous star formation history. The position of the sample in the star formation rate (SFR) versus M_(star) diagram is consistent with previous papers. The redshift evolution of the log M_(star) versus A_(FUV) relation is in agreement with an evolution in redshift of this relation. This evolution is necessary to explain the cosmic evolution of the average dust attenuation of galaxies. Evolution is also observed in the L_(dust)/L_(FUV) (IRX) versus UV slope \u03b2_(FUV) diagram: younger galaxies have bluer \u03b2_(FUV). We modeled the shift of galaxies in the IRX versus the \u03b2_(FUV) diagram with the mass-weighted age as a free parameter, and we provide an equation to make predictions. The large sample studied in this paper is generally consistent with models that assume rapid dust formation from supernovae and removal of dust by outflows and supernovae blasts. However, we find that high mass dusty star-forming galaxies cannot be explained by the models.",
"doi": "10.1051/0004-6361/202142554",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2022-08",
"volume": "664",
"pages": "Art. No. A73"
},
{
"id": "authors:cp9c4-atn11",
"collection": "authors",
"collection_id": "cp9c4-atn11",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220805-205096000",
"type": "article",
"title": "COSMOS2020: Cosmic evolution of the stellar-to-halo mass relation for central and satellite galaxies up to z\u2004\u223c\u20065",
"author": [
{
"family_name": "Shuntov",
"given_name": "M.",
"orcid": "0000-0002-7087-0701",
"clpid": "Shuntov-Marko"
},
{
"family_name": "McCracken",
"given_name": "H. J.",
"orcid": "0000-0002-9489-7765",
"clpid": "McCracken-Henry-J"
},
{
"family_name": "Gavazzi",
"given_name": "R.",
"orcid": "0000-0002-5540-6935",
"clpid": "Gavazzi-Rapha\u00ebl"
},
{
"family_name": "Laigle",
"given_name": "C.",
"clpid": "Laigle-Clotilde"
},
{
"family_name": "Weaver",
"given_name": "J. R.",
"orcid": "0000-0003-1614-196X",
"clpid": "Weaver-John-R"
},
{
"family_name": "Davidzon",
"given_name": "I.",
"orcid": "0000-0002-2951-7519",
"clpid": "Davidzon-Iary"
},
{
"family_name": "Ilbert",
"given_name": "O.",
"orcid": "0000-0002-7303-4397",
"clpid": "Ilbert-Olivier"
},
{
"family_name": "Kauffmann",
"given_name": "O. B.",
"orcid": "0000-0001-5283-4662",
"clpid": "Kauffmann-Olivier-B"
},
{
"family_name": "Faisst",
"given_name": "A.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Dubois",
"given_name": "Y.",
"orcid": "0000-0003-0225-6387",
"clpid": "Dubois-Yohan"
},
{
"family_name": "Koekemoer",
"given_name": "A. M.",
"orcid": "0000-0002-6610-2048",
"clpid": "Koekemoer-Anton-M"
},
{
"family_name": "Moneti",
"given_name": "A.",
"clpid": "Moneti-A"
},
{
"family_name": "Milvang-Jensen",
"given_name": "B.",
"orcid": "0000-0002-2281-2785",
"clpid": "Milvang-Jensen-Bo"
},
{
"family_name": "Mobasher",
"given_name": "B.",
"clpid": "Mobasher-Bahram"
},
{
"family_name": "Sanders",
"given_name": "D. B.",
"orcid": "0000-0002-1233-9998",
"clpid": "Sanders-David-B"
},
{
"family_name": "Toft",
"given_name": "S.",
"orcid": "0000-0003-3631-7176",
"clpid": "Toft-Sune"
}
],
"abstract": "We used the COSMOS2020 catalog to measure the stellar-to-halo mass relation (SHMR) divided by central and satellite galaxies from z\u2004=\u20040.2 to z\u2004=\u20045.5. Starting from accurate photometric redshifts, we measured the near-infrared selected two-point angular correlation and stellar mass functions in ten redshift bins. We used a phenomenological model that parametrizes the stellar-to-halo mass relation for central galaxies and the number of galaxies inside each halo to describe our observations. This model qualitatively reproduces our measurements and their dependence on the stellar mass threshold. Surprisingly, the mean halo occupation distribution only shows a mild evolution with redshift suggesting that galaxies occupy halos similarly throughout cosmic time. At each redshift, we measured the ratio of stellar mass to halo mass, M_*/M\u2095, which shows the characteristic strong dependence of halo mass with a peak at M\u2095\u1d56\u1d49\u1d43\u1d4f\u2005\u223c\u20052\u2005\u00d7\u200510\u00b9\u00b2\u2005M_\u2299. For the first time, using a joint modeling of clustering and abundances, we measured the evolution of M\u2095\u1d56\u1d49\u1d43\u1d4f from z\u2004=\u20040.2 to z\u2004=\u20045.5. M\u2095\u1d56\u1d49\u1d43\u1d4f increases gradually with redshift from log\u2005M\u2095\u1d56\u1d49\u1d43\u1d4f/M_\u2299\u2005\u223c\u200512.1 at z\u2004\u223c\u20040.3 to log\u2005M\u2095\u1d56\u1d49\u1d43\u1d4f/M_\u2005\u223c\u200512.3 at z\u2004\u223c\u20042, and up to log\u2005M\u2095\u1d56\u1d49\u1d43\u1d4f/M_\u2299\u2005\u223c\u200512.9 at z\u2004\u223c\u20045. Similarly, the stellar mass peak M\u2217peak increases with redshift from log\u2005M\u2217\u1d56\u1d49\u1d43\u1d4f/M_\u2299\u2005\u223c\u200510.5 at z\u2004\u223c\u20040.3 to log\u2005M\u2217\u1d56\u1d49\u1d43\u1d4f/M_\u2299\u2005\u223c\u200510.9 at z\u2004\u223c\u20043. The SHMR ratio at the peak halo mass remains almost constant with redshift. These results are in accordance with the scenario in which the peak of star-formation efficiency moves toward more massive halos at higher redshifts. We also measured the fraction of satellites as a function of stellar mass and redshift. For all stellar mass thresholds, the satellite fraction decreases at higher redshifts. At a given redshift, there is a higher fraction of low-mass satellites and this fraction reaches a plateau at \u223c25% at z\u2004\u223c\u20041. The satellite contribution to the total stellar mass budget in halos becomes more important than that of the central at halo masses of about M\u2095\u2004> \u200410\u00b9\u00b3\u2006M_\u2299 and always stays below the peak, indicating that quenching mechanisms are present in massive halos that keep the star-formation efficiency low. Finally, we compared our results with three hydrodynamical simulations: HORIZON-AGN, TNG100 of the ILLUSTRISTNG project, and EAGLE. We find that the most significant discrepancy is at the high-mass end, where the simulations generally show that satellites have a higher contribution to the total stellar mass budget than the observations. This, together with the finding that the fraction of satellites is higher in the simulations, indicates that the feedback mechanisms acting in both group- and cluster-scale halos appear to be less efficient in quenching the mass assembly of satellites \u2013 and that quenching occurs much later in the simulations.",
"doi": "10.1051/0004-6361/202243136",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2022-08",
"volume": "664",
"pages": "Art. No. A61"
},
{
"id": "authors:agf5q-r6z88",
"collection": "authors",
"collection_id": "agf5q-r6z88",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220711-652666000",
"type": "article",
"title": "The ALPINE-ALMA [C\u202fII] survey. Dust attenuation curves at z = 4.4\u20135.5",
"author": [
{
"family_name": "Boquien",
"given_name": "M\u00e9d\u00e9ric",
"orcid": "0000-0003-0946-6176",
"clpid": "Boquien-M\u00e9d\u00e9ric"
},
{
"family_name": "Buat",
"given_name": "V\u00e9ronique",
"orcid": "0000-0003-3441-903X",
"clpid": "Buat-V\u00e9ronique"
},
{
"family_name": "Burgarella",
"given_name": "Denis",
"clpid": "Burgarella-Denis"
},
{
"family_name": "Bardelli",
"given_name": "Sandro",
"orcid": "0000-0002-8900-0298",
"clpid": "Bardelli-Sandro"
},
{
"family_name": "B\u00e9thermin",
"given_name": "Matthieu",
"orcid": "0000-0002-3915-2015",
"clpid": "B\u00e9thermin-Matthieu"
},
{
"family_name": "Faisst",
"given_name": "Andreas",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Ginolfi",
"given_name": "Michele",
"orcid": "0000-0002-9122-1700",
"clpid": "Ginolfi-Michele"
},
{
"family_name": "Hathi",
"given_name": "Nimish",
"orcid": "0000-0001-6145-5090",
"clpid": "Hathi-Nimish-P"
},
{
"family_name": "Jones",
"given_name": "Gareth",
"orcid": "0000-0002-0267-9024",
"clpid": "Jones-Gareth-C"
},
{
"family_name": "Koekemoer",
"given_name": "Anton",
"orcid": "0000-0002-6610-2048",
"clpid": "Koekemoer-Anton-M"
},
{
"family_name": "Lemaux",
"given_name": "Brian",
"orcid": "0000-0002-1428-7036",
"clpid": "Lemaux-Brian-C"
},
{
"family_name": "Narayanan",
"given_name": "Desika",
"orcid": "0000-0002-7064-4309",
"clpid": "Narayanan-Desika"
},
{
"family_name": "Romano",
"given_name": "Michael",
"orcid": "0000-0002-9948-3916",
"clpid": "Romano-Michael"
},
{
"family_name": "Schaerer",
"given_name": "Daniel",
"orcid": "0000-0001-7144-7182",
"clpid": "Schaerer-Daniel"
},
{
"family_name": "Vergani",
"given_name": "Daniela",
"orcid": "0000-0003-0898-2216",
"clpid": "Vergani-Daniela"
},
{
"family_name": "Zamorani",
"given_name": "Giovanni",
"orcid": "0000-0002-2318-301X",
"clpid": "Zamorani-Giovanni"
},
{
"family_name": "Zucca",
"given_name": "Elena",
"orcid": "0000-0002-5845-8132",
"clpid": "Zucca-Elena"
}
],
"abstract": "Context. There is ample evidence that dust is already present in abundance at high redshift. However, given the faintness of distant galaxies in the optical and the near-infrared, the data are limited and the understanding of how the dust affects the emerging radiation of galaxies at very high redshift is still limited. \n\nAims. Using the ALMA Large Program to INvestigate [C\u202fII] at Early times (ALPINE), our objective is to quantify the dust attenuation properties in galaxies at z\u2004=\u20044.4\u20135.5, particularly with regard to the shape of their attenuation curve. \n\nMethods. Using the CIGALE spectral energy distribution (SED) code, we modeled the stellar populations and their interactions with the dust to measure some of the physical properties of the ALPINE sample. We selected a subsample of 23 main-sequence galaxies requiring a detection in at least six bands in the rest-frame UV and optical, as well as in the dust continuum around 158 \u03bcm or the [C\u202fII] fine-structure line. The inclusion of this line is important for improving the constraints on the physical properties, while achieving a reasonably low uncertainty on the slope of the attenuation curves. \n\nResults. We find that the attenuation curves span a broad range of properties \u2013 from curves that are much steeper than the SMC extinction curve to those that are shallower than the starburst attenuation curve. The shape of the attenuation curves strongly depends on the V-band attenuation. Galaxies with the lowest attenuation also present the steepest curves. The steepness of such curves probably results from the combination of the intrinsic physical properties of the dust, the relative distribution of stars and dust in the interstellar medium, and the differential reddening, with an important fraction of the dust concentrated in star-forming regions. The broad range of attenuation curves found at z\u2004\u223c\u20045 shows that no single attenuation curve is appropriate for main-sequence galaxies. When SED modeling is not feasible, assuming a fixed curve can lead to large errors, for instance, in the interpretation and application of the IRX-\u03b2 diagram. \n\nConclusions. Considerable caution should be exercised when correcting high redshift galaxies for the presence of dust using the UV slope \u03b2 as it can affect the estimation of both star formation rates and stellar mass even at low V-band attenuation due to the steepness of the attenuation curve. However, when SED modeling can be used, the impact of the choice of the attenuation curve on the star formation rate and the stellar mass is limited.",
"doi": "10.1051/0004-6361/202142537",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2022-07",
"volume": "663",
"pages": "Art. No. A50"
},
{
"id": "authors:436q1-st532",
"collection": "authors",
"collection_id": "436q1-st532",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220802-743346000",
"type": "article",
"title": "Pilot-WINGS: An extended MUSE view of the structure of Abell 370",
"author": [
{
"family_name": "Lagattuta",
"given_name": "David J.",
"orcid": "0000-0002-7633-2883",
"clpid": "Lagattuta-David-J"
},
{
"family_name": "Richard",
"given_name": "Johan",
"orcid": "0000-0001-5492-1049",
"clpid": "Richard-Johan"
},
{
"family_name": "Bauer",
"given_name": "Franz Erik",
"orcid": "0000-0002-8686-8737",
"clpid": "Bauer-Franz-E"
},
{
"family_name": "Cerny",
"given_name": "Catherine",
"orcid": "0000-0002-8261-9098",
"clpid": "Cerny-Catherine"
},
{
"family_name": "Claeyssens",
"given_name": "Ad\u00e9la\u00efde",
"clpid": "Claeyssens-Ad\u00e9la\u00efde"
},
{
"family_name": "Guaita",
"given_name": "Lucia",
"clpid": "Guaita-Lucia"
},
{
"family_name": "Jauzac",
"given_name": "Mathilde",
"orcid": "0000-0003-1974-8732",
"clpid": "Jauzac-Mathilde"
},
{
"family_name": "Jeanneau",
"given_name": "Alexandre",
"clpid": "Jeanneau-Alexandre"
},
{
"family_name": "Koekemoer",
"given_name": "Anton M.",
"orcid": "0000-0002-6610-2048",
"clpid": "Koekemoer-Anton-M"
},
{
"family_name": "Mahler",
"given_name": "Guillaume",
"orcid": "0000-0003-3266-2001",
"clpid": "Mahler-Guillaume"
},
{
"family_name": "Prieto\u00a0Lyon",
"given_name": "Gonzalo",
"clpid": "Prieto-Lyon-Gonzalo"
},
{
"family_name": "Acebron",
"given_name": "Ana",
"orcid": "0000-0003-3108-9039",
"clpid": "Acebron-Ana"
},
{
"family_name": "Meneghetti",
"given_name": "Massimo",
"orcid": "0000-0003-1225-7084",
"clpid": "Meneghetti-Massimo"
},
{
"family_name": "Niemiec",
"given_name": "Anna",
"orcid": "0000-0003-3791-2647",
"clpid": "Niemiec-Anna"
},
{
"family_name": "Zitrin",
"given_name": "Adi",
"orcid": "0000-0002-0350-4488",
"clpid": "Zitrin-Adi"
},
{
"family_name": "Bianconi",
"given_name": "Matteo",
"orcid": "0000-0002-0427-5373",
"clpid": "Bianconi-Matteo"
},
{
"family_name": "Connor",
"given_name": "Thomas",
"orcid": "0000-0002-7898-7664",
"clpid": "Connor-Thomas-P"
},
{
"family_name": "Cen",
"given_name": "Renyue",
"orcid": "0000-0001-8531-9536",
"clpid": "Cen-Renyue"
},
{
"family_name": "Edge",
"given_name": "Alastair",
"clpid": "Edge-Alastair-C"
},
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Limousin",
"given_name": "Marceau",
"clpid": "Limousin-Marceau"
},
{
"family_name": "Massey",
"given_name": "Richard",
"orcid": "0000-0002-6085-3780",
"clpid": "Massey-Richard-J"
},
{
"family_name": "Sereno",
"given_name": "Mauro",
"orcid": "0000-0003-0302-0325",
"clpid": "Sereno-Mauro"
},
{
"family_name": "Sharon",
"given_name": "Keren",
"orcid": "0000-0002-7559-0864",
"clpid": "Sharon-Keren"
},
{
"family_name": "Weaver",
"given_name": "John R.",
"orcid": "0000-0003-1614-196X",
"clpid": "Weaver-John-R"
}
],
"abstract": "We investigate the strong-lensing cluster Abell 370 (A370) using a wide Integral Field Unit (IFU) spectroscopic mosaic from the Multi-Unit Spectroscopic Explorer (MUSE). IFU spectroscopy provides significant insight into the structure and mass content of galaxy clusters, yet IFU-based cluster studies focus almost exclusively on the central Einstein-radius region. Covering over 14 arcmin2, the new MUSE mosaic extends significantly beyond the A370 Einstein radius, providing, for the first time, a detailed look at the cluster outskirts. Combining these data with wide-field, multi-band Hubble Space Telescope (HST) imaging from the BUFFALO project, we analyse the distribution of objects within the cluster and along the line of sight. Identifying 416 cluster galaxies, we use kinematics to trace the radial mass profile of the halo, providing a mass estimate independent from the lens model. We also measure radially averaged properties of the cluster members, tracking their evolution as a function of infall. Thanks to the high spatial resolution of our data, we identify six cluster members acting as galaxy\u2013galaxy lenses, which constrain localized mass distributions beyond the Einstein radius. Finally, taking advantage of MUSE's 3D capabilities, we detect and analyse multiple spatially extended overdensities outside of the cluster that influence lensing-derived halo mass estimates. We stress that much of this work is only possible thanks to the robust, extended IFU coverage, highlighting its importance even in less optically dense cluster regions. Overall, this work showcases the power of combining HST\u00a0+\u00a0MUSE, and serves as the initial step towards a larger and wider program targeting several clusters.",
"doi": "10.1093/mnras/stac418",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2022-07",
"series_number": "1",
"volume": "514",
"issue": "1",
"pages": "497-517"
},
{
"id": "authors:v5q73-r1467",
"collection": "authors",
"collection_id": "v5q73-r1467",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220608-849014000",
"type": "article",
"title": "ALPINE: A Large Survey to Understand Teenage Galaxies",
"author": [
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "B\u00e9thermin",
"given_name": "Matthieu",
"orcid": "0000-0002-3915-2015",
"clpid": "B\u00e9thermin-Matthieu"
},
{
"family_name": "Cassata",
"given_name": "Paolo",
"orcid": "0000-0002-6716-4400",
"clpid": "Cassata-Paolo"
},
{
"family_name": "Dessauges-Zavadsky",
"given_name": "Miroslava",
"orcid": "0000-0003-0348-2917",
"clpid": "Dessauges-Zavadsky-Miroslava"
},
{
"family_name": "Fudamoto",
"given_name": "Yoshinobu",
"orcid": "0000-0001-7440-8832",
"clpid": "Fudamoto-Yoshinobu"
},
{
"family_name": "Ginolfi",
"given_name": "Michele",
"orcid": "0000-0002-9122-1700",
"clpid": "Ginolfi-Michele"
},
{
"family_name": "Gruppioni",
"given_name": "Carlotta",
"orcid": "0000-0002-5836-4056",
"clpid": "Gruppioni-Carlotta"
},
{
"family_name": "Jones",
"given_name": "Gareth",
"orcid": "0000-0002-0267-9024",
"clpid": "Jones-Gareth"
},
{
"family_name": "Khusanova",
"given_name": "Yana",
"orcid": "0000-0002-7220-397X",
"clpid": "Khusanova-Yana"
},
{
"family_name": "LeF\u00e8vre",
"given_name": "Olivier",
"orcid": "0000-0001-5891-2596",
"clpid": "LeF\u00e8vre-Olivier"
},
{
"family_name": "Pozzi",
"given_name": "Francesca",
"orcid": "0000-0002-7412-647X",
"clpid": "Pozzi-Francesca"
},
{
"family_name": "Romano",
"given_name": "Michael",
"orcid": "0000-0002-9948-3916",
"clpid": "Romano-Michael"
},
{
"family_name": "Silverman",
"given_name": "John",
"orcid": "0000-0002-0000-6977",
"clpid": "Silverman-John-D"
},
{
"family_name": "Vanderhoof",
"given_name": "Brittany",
"orcid": "0000-0002-8163-0172",
"clpid": "Vanderhoof-Brittany-N"
}
],
"abstract": "A multiwavelength study of galaxies is important to understand their formation and evolution. Only in the recent past, thanks to the Atacama Large (Sub) Millimeter Array (ALMA), were we able to study the far-infrared (IR) properties of galaxies at high redshifts. In this article, we summarize recent research highlights and their significance to our understanding of early galaxy evolution from the ALPINE survey, a large program with ALMA to observe the dust continuum and 158\u03bcm C\u207a emission of normal star-forming galaxies at z= 4\u20136. Combined with ancillary data at UV through near-IR wavelengths, ALPINE provides the currently largest multiwavelength sample of post-reionization galaxies and has advanced our understanding of (i) the demographics of C\u207a emission; (ii) the relation of star formation and C\u207a emission; (iii) the gas content; (iv) outflows and enrichment of the intergalactic medium; and (v) the kinematics, emergence of disks, and merger rates in galaxies at z>4. ALPINE builds the basis for more detailed measurements with the next generation of telescopes, and places itself as an important post-reionization baseline sample to allow a continuous study of galaxies over 13 billion years of cosmic time.",
"doi": "10.3390/universe8060314",
"issn": "2218-1997",
"publisher": "MDPI",
"publication": "Universe",
"publication_date": "2022-06",
"series_number": "6",
"volume": "8",
"issue": "6",
"pages": "Art. No. 314"
},
{
"id": "authors:8qtqw-50k24",
"collection": "authors",
"collection_id": "8qtqw-50k24",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220512-561157000",
"type": "article",
"title": "Joint Survey Processing. II. Stellar Proper Motions in the COSMOS Field from Hubble Space Telescope ACS and Subaru Telescope HSC Observations",
"author": [
{
"family_name": "Fajardo-Acosta",
"given_name": "Sergio B.",
"orcid": "0000-0001-9309-0102",
"clpid": "Fajardo-Acosta-Sergio-B"
},
{
"family_name": "Faisst",
"given_name": "Andreas",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Grillmair",
"given_name": "Carl J.",
"orcid": "0000-0003-4072-169X",
"clpid": "Grillmair-Carl-J"
},
{
"family_name": "Chary",
"given_name": "Ranga-Ram",
"orcid": "0000-0001-7583-0621",
"clpid": "Chary-Ranga-Ram"
},
{
"family_name": "Paladini",
"given_name": "Roberta",
"orcid": "0000-0002-5158-243X",
"clpid": "Paladini-Roberta"
},
{
"family_name": "Rusholme",
"given_name": "Ben",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Stickley",
"given_name": "Nathaniel",
"orcid": "0000-0003-0987-5738",
"clpid": "Stickley-Nathaniel-R"
}
],
"abstract": "We analyze stellar proper motions in the COSMOS field to assess the presence of bulk motions. At bright magnitudes (G-band 18.5\u201320.76 AB), we use the proper motions of 1010 stars in the Gaia DR2 catalog. At the faint end, we compute proper motions of 11,519 pointlike objects at i-band magnitudes 19\u201325 AB using Hubble ACS and Subaru HSC data, which span two epochs about 11 yr apart. In order to measure these proper motions with unprecedented accuracy at faint magnitudes, we developed a foundational set of astrometric tools that will be required for joint survey processing of data from the next generation of optical/infrared surveys. The astrometric grids of Hubble ACS and Subaru HSC mosaics were corrected at the catalog level using proper motion\u2013propagated and parallax-corrected Gaia DR2 sources. These astrometric corrections were verified using compact extragalactic sources. Upon comparison of our measured proper motions with Gaia DR2, we estimate the uncertainties in our measurements to be \u223c2\u20133 mas yr\u207b\u00b9 axis\u207b\u00b9, down to 25.5 AB mag. We correct proper motions for the mean motion of the Sun, and we find that late-type main-sequence stars predominantly in the thin disk in the COSMOS field have space velocities mainly toward the Galactic center. We detect candidate high-velocity (\u2265220 km s\u207b\u00b9) stars, six of them at \u223c0.4\u20136 kpc, from the Gaia sample, and five of them at \u223c20 kpc, from the faint star HSC and ACS sample. The sources from the faint star sample may be candidate halo members of the Sangarius stream.",
"doi": "10.3847/1538-4357/ac5a4f",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2022-05-01",
"series_number": "1",
"volume": "930",
"issue": "1",
"pages": "Art. No. 71"
},
{
"id": "authors:zpgdx-8gs83",
"collection": "authors",
"collection_id": "zpgdx-8gs83",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210323-151326953",
"type": "article",
"title": "Joint Survey Processing. I. Compact Oddballs in the COSMOS Field\u2014Low-luminosity Quasars at z > 6?",
"author": [
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Chary",
"given_name": "Ranga Ram",
"orcid": "0000-0001-7583-0621",
"clpid": "Chary-R-R"
},
{
"family_name": "Fajardo-Acosta",
"given_name": "Sergio",
"orcid": "0000-0001-9309-0102",
"clpid": "Fajardo-Acosta-Sergio-B"
},
{
"family_name": "Paladini",
"given_name": "Roberta",
"orcid": "0000-0002-5158-243X",
"clpid": "Paladini-Roberta"
},
{
"family_name": "Rusholme",
"given_name": "Benjamin",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-Benjamin"
},
{
"family_name": "Stickley",
"given_name": "Nathaniel",
"clpid": "Stickley-Nathaniel-R"
},
{
"family_name": "Helou",
"given_name": "George",
"orcid": "0000-0003-3367-3415",
"clpid": "Helou-G"
},
{
"family_name": "Weaver",
"given_name": "John R.",
"orcid": "0000-0003-1614-196X",
"clpid": "Weaver-John-R"
},
{
"family_name": "Brammer",
"given_name": "Gabriel",
"orcid": "0000-0003-2680-005X",
"clpid": "Brammer-Gabriel-B"
},
{
"family_name": "Koekemoer",
"given_name": "Anton M.",
"orcid": "0000-0002-6610-2048",
"clpid": "Koekemoer-Anton-M"
},
{
"family_name": "Miyatake",
"given_name": "Hironao",
"orcid": "0000-0001-7964-9766",
"clpid": "Miyatake-Hironao"
}
],
"abstract": "The faint-end slope of the quasar luminosity function at z \u223c 6 and its implication on the role of quasars in reionizing the intergalactic medium at early times has been an outstanding problem for some time. The identification of faint high-redshift quasars with luminosities of <10^(44.5) erg s\u207b\u00b9 is challenging. They are rare (few per square degree), and the separation of these unresolved quasars from late-type stars and compact star-forming galaxies is difficult from ground-based observations alone. In addition, source confusion becomes significant at >25 mag, with \u223c30% of sources having their flux contaminated by foreground objects when the seeing resolution is \u223c0''.7. We mitigate these issues by performing a pixel-level joint processing of ground and space-based data from Subaru/Hyper-SuprimeCam (HSC) and Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS). We create a deconfused catalog over the 1.64 deg\u00b2 of the COSMOS field, after accounting for spatial varying point-spread functions and astrometric differences between the two data sets. We identify twelve low-luminosity (M_(UV) \u223c \u221221 mag) z > 6 quasar candidates through (i) their red color measured between ACS/F814W and HSC/i band and (ii) their compactness in the space-based data. Nondetections of our candidates in Hubble DASH data argues against contamination from late-type stars. Our constraints on the faint end of the quasar luminosity function at z \u223c 6.4 suggest a negligibly small contribution to reionization compared to the star-forming galaxy population. The confirmation of our candidates and the evolution of number density with redshift could provide better insights into how supermassive galaxies grew in the first billion years of cosmic time.",
"doi": "10.3847/1538-4357/ac59b3",
"issn": "0004-637X",
"publisher": "American Physical Society",
"publication": "Astrophysical Journal",
"publication_date": "2022-04-10",
"series_number": "1",
"volume": "929",
"issue": "1",
"pages": "Art. No. 66"
},
{
"id": "authors:0gb66-trv56",
"collection": "authors",
"collection_id": "0gb66-trv56",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220406-728382450",
"type": "article",
"title": "The ALPINE-ALMA [CII] survey: The population of [CII]-undetected galaxies and their role in the L_[CII]-SFR relation",
"author": [
{
"family_name": "Romano",
"given_name": "M.",
"orcid": "0000-0002-9948-3916",
"clpid": "Romano-Michael"
},
{
"family_name": "Morselli",
"given_name": "L.",
"orcid": "0000-0003-0753-2571",
"clpid": "Morselli-Laura"
},
{
"family_name": "Cassata",
"given_name": "P.",
"orcid": "0000-0002-6716-4400",
"clpid": "Cassata-Paolo"
},
{
"family_name": "Ginolfi",
"given_name": "M.",
"orcid": "0000-0002-8231-821X",
"clpid": "Ginolfi-Michele"
},
{
"family_name": "Schaerer",
"given_name": "D.",
"orcid": "0000-0001-7144-7182",
"clpid": "Schaerer-Daniel"
},
{
"family_name": "B\u00e9thermin",
"given_name": "M.",
"orcid": "0000-0002-3915-2015",
"clpid": "B\u00e9thermin-Matthieu"
},
{
"family_name": "Capak",
"given_name": "P.",
"orcid": "0000-0003-3578-6843",
"clpid": "Capak-Peter"
},
{
"family_name": "Faisst",
"given_name": "A.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Le F\u00e8vre",
"given_name": "O.",
"orcid": "0000-0001-5891-2596",
"clpid": "Le-F\u00e8vre-Olivier"
},
{
"family_name": "Silverman",
"given_name": "J. D.",
"orcid": "0000-0002-0000-6977",
"clpid": "Silverman-John-D"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Bardelli",
"given_name": "S.",
"orcid": "0000-0002-8900-0298",
"clpid": "Bardelli-Sandro"
},
{
"family_name": "Boquien",
"given_name": "M.",
"orcid": "0000-0003-0946-6176",
"clpid": "Boquien-M\u00e9d\u00e9ric"
},
{
"family_name": "Dessauges-Zavadsky",
"given_name": "M.",
"orcid": "0000-0003-0348-2917",
"clpid": "Dessauges-Zavadsky-Miroslava"
},
{
"family_name": "Fujimoto",
"given_name": "S.",
"orcid": "0000-0001-7201-5066",
"clpid": "Fujimoto-Seiji"
},
{
"family_name": "Hathi",
"given_name": "N. P.",
"orcid": "0000-0001-6145-5090",
"clpid": "Hathi-Nimish-P"
},
{
"family_name": "Jones",
"given_name": "G. C.",
"orcid": "0000-0002-0267-9024",
"clpid": "Jones-Gareth-C"
},
{
"family_name": "Koekemoer",
"given_name": "A. M.",
"orcid": "0000-0002-6610-2048",
"clpid": "Koekemoer-Anton-M"
},
{
"family_name": "Lemaux",
"given_name": "B. C.",
"orcid": "0000-0002-1428-7036",
"clpid": "Lemaux-Brian-C"
},
{
"family_name": "M\u00e9ndez-Hern\u00e1ndez",
"given_name": "H.",
"orcid": "0000-0003-3057-9677",
"clpid": "M\u00e9ndez-Hern\u00e1ndez-Hugo"
},
{
"family_name": "Narayanan",
"given_name": "D.",
"orcid": "0000-0002-7064-4309",
"clpid": "Narayanan-Desika"
},
{
"family_name": "Talia",
"given_name": "M.",
"orcid": "0000-0003-4352-2063",
"clpid": "Talia-Margherita"
},
{
"family_name": "Vergani",
"given_name": "D.",
"orcid": "0000-0003-0898-2216",
"clpid": "Vergani-Daniela"
},
{
"family_name": "Zamorani",
"given_name": "G.",
"orcid": "0000-0002-2318-301X",
"clpid": "Zamorani-Giovanni"
},
{
"family_name": "Zucca",
"given_name": "E.",
"orcid": "0000-0002-5845-8132",
"clpid": "Zucca-Elena"
}
],
"abstract": "The [CII] 158 \u03bcm emission line represents one of the most profitable tools for the investigation of the high-redshift galaxies in the early Universe so far. Being one of the brightest cooling lines in the rest-frame far-infrared regime of star-forming galaxies, it has been successfully exploited as a tracer of the star-formation rate (SFR) in local sources. The picture is more complex at higher redshifts, where its usability in this context is still under investigation. Recent results from the ALMA Large Program to INvestigate [CII] at Early times (ALPINE) survey suggest that there is no (or weak) evolution of the L[CII]-SFR relation up to z\u2004\u223c\u20046, but their reliability is hampered by the presence of a large population of [CII] nondetected galaxies. In this work, we characterize the population of [CII] nondetections in ALPINE. By stacking their ALMA spectra, we obtained a signal detected at \u223c5.1\u03c3, resulting in a [CII] luminosity of log(L_[CII]/L_\u2299)\u223c7.8. When combining this value with those from the [CII] detections, we found a L_[CII]-SFR relation with a slope b\u2004=\u20041.14\u2005\u00b1\u20050.11, which is in agreement within the uncertainties both with the linear relation found in the local Universe and with the previous findings from ALPINE at z\u2004\u223c\u20045. This suggests that the [CII] line can be considered a good tracer of star formation up to the distant Universe. Finally, we show that the galaxies of our sample that deviate from the observed L_[CII]-SFR relation most could suffer from a less precise redshift estimation, perhaps artificially reducing their [CII] luminosity. In this respect, we claim that there is no evidence in favor of a deficit of [CII] content in high-z galaxies, in contrast with earlier studies.",
"doi": "10.1051/0004-6361/202142265",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2022-04",
"volume": "660",
"pages": "Art. No. A14"
},
{
"id": "authors:szmy9-qef80",
"collection": "authors",
"collection_id": "szmy9-qef80",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220525-92272000",
"type": "article",
"title": "The ALPINE-ALMA [C\u2009II] survey: Investigation of 10 galaxies at z \u223c 4.5 with [O\u2009II] and [C\u2009II] line emission \u2212 ISM properties and [O\u2009II]\u2212SFR relation",
"author": [
{
"family_name": "Vanderhoof",
"given_name": "Brittany N.",
"orcid": "0000-0002-8163-0172",
"clpid": "Vanderhoof-Brittany-N"
},
{
"family_name": "Faisst",
"given_name": "A. L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Shen",
"given_name": "L.",
"orcid": "0000-0001-9495-7759"
},
{
"family_name": "Lemaux",
"given_name": "B. C.",
"orcid": "0000-0002-1428-7036"
},
{
"family_name": "B\u00e9thermin",
"given_name": "M.",
"orcid": "0000-0002-3915-2015"
},
{
"family_name": "Capak",
"given_name": "P. L.",
"orcid": "0000-0003-3578-6843"
},
{
"family_name": "Cassata",
"given_name": "P.",
"orcid": "0000-0002-6716-4400"
},
{
"family_name": "Le F\u00e8vre",
"given_name": "O.",
"orcid": "0000-0001-5891-2596"
},
{
"family_name": "Schaerer",
"given_name": "D.",
"orcid": "0000-0001-7144-7182"
},
{
"family_name": "Silverman",
"given_name": "J.",
"orcid": "0000-0002-0000-6977"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Boquien",
"given_name": "M.",
"orcid": "0000-0003-0946-6176"
},
{
"family_name": "Gal",
"given_name": "R.",
"orcid": "0000-0001-8255-6560"
},
{
"family_name": "Kartaltepe",
"given_name": "J.",
"orcid": "0000-0001-9187-3605"
},
{
"family_name": "Lubin",
"given_name": "L. M.",
"orcid": "0000-0003-4249-5315"
},
{
"family_name": "Dessauges-Zavadsky",
"given_name": "M.",
"orcid": "0000-0003-0348-2917"
},
{
"family_name": "Fudamoto",
"given_name": "Y.",
"orcid": "0000-0001-7440-8832"
},
{
"family_name": "Ginolfi",
"given_name": "M.",
"orcid": "0000-0002-9122-1700"
},
{
"family_name": "Hathi",
"given_name": "N. P.",
"orcid": "0000-0001-6145-5090"
},
{
"family_name": "Jones",
"given_name": "G. C.",
"orcid": "0000-0002-0267-9024"
},
{
"family_name": "Koekemoer",
"given_name": "A. M.",
"orcid": "0000-0002-6610-2048"
},
{
"family_name": "Narayanan",
"given_name": "D.",
"orcid": "0000-0002-7064-4309"
},
{
"family_name": "Romano",
"given_name": "M.",
"orcid": "0000-0002-9948-3916"
},
{
"family_name": "Talia",
"given_name": "M.",
"orcid": "0000-0003-4352-2063"
},
{
"family_name": "Vergani",
"given_name": "D.",
"orcid": "0000-0003-0898-2216"
},
{
"family_name": "Zamorani",
"given_name": "G.",
"orcid": "0000-0002-2318-301X"
}
],
"abstract": "We present 10 main-sequence ALPINE galaxies (log\u2009(M/M_\u2299) = 9.2\u221211.1 and SFR = 23\u2212190 M_\u2299 yr\u207b\u00b9) at z \u223c 4.5 with optical [O\u2009II] measurements from Keck/MOSFIRE spectroscopy and Subaru/MOIRCS narrow-band imaging. This is the largest such multiwavelength sample at these redshifts, combining various measurements in the ultraviolet, optical, and far-infrared including [C\u2009II]_(158 \u03bcm) line emission and dust continuum from ALMA and H\u2009\u03b1 emission from Spitzer photometry. For the first time, this unique sample allows us to analyse the relation between [O\u2009II] and total star-formation rate (SFR) and the interstellar medium (ISM) properties via [O\u2009II]/[C\u2009II] and [O\u2009II]/H\u2009\u03b1 luminosity ratios at z \u223c 4.5. The [O\u2009II]\u2212SFR relation at z \u223c 4.5 cannot be described using standard local descriptions, but is consistent with a metal-dependent relation assuming metallicities around 50 per cent solar. To explain the measured dust-corrected luminosity ratios of log(L_[OII]/L_[CII]) \u223c 0.98^(+0.21)_(\u22120.22) and log(L_[OII]/L_(H\u03b1)) \u223c \u22120.22^(+0.13)_(\u22120.15) for our sample, ionization parameters log\u2009(U) < \u22122 and electron densities log(n\u2091/[cm\u207b\u00b3]) \u223c 2.5\u22123 are required. The former is consistent with galaxies at z \u223c 2\u22123, however lower than at z > 6. The latter may be slightly higher than expected given the galaxies' specific SFR. The analysis of this pilot sample suggests that typical log\u2009(M/M_\u2299) > 9 galaxies at z \u223c 4.5 to have broadly similar ISM properties as their descendants at z \u223c 2 and suggest a strong evolution of ISM properties since the epoch of reionization at z > 6.",
"doi": "10.1093/mnras/stac071",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2022-03",
"series_number": "1",
"volume": "511",
"issue": "1",
"pages": "1303-1316"
},
{
"id": "authors:ggs3f-2mr57",
"collection": "authors",
"collection_id": "ggs3f-2mr57",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220203-316033000",
"type": "article",
"title": "Molecular Gas Excitation of the Massive Dusty Starburst CRLE and the Main-sequence Galaxy HZ10 at z = 5.7 in the COSMOS Field",
"author": [
{
"family_name": "Vieira",
"given_name": "Daniel",
"orcid": "0000-0001-8019-0390",
"clpid": "Vieira-Daniel"
},
{
"family_name": "Riechers",
"given_name": "Dominik A.",
"orcid": "0000-0001-9585-1462",
"clpid": "Riechers-Domink-A"
},
{
"family_name": "Pavesi",
"given_name": "Riccardo",
"orcid": "0000-0002-2263-646X",
"clpid": "Pavesi-Riccardo"
},
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Schinnerer",
"given_name": "Eva",
"orcid": "0000-0002-3933-7677",
"clpid": "Schinnerer-Eva"
},
{
"family_name": "Scoville",
"given_name": "Nicholas Z.",
"orcid": "0000-0002-0438-3323",
"clpid": "Scoville-N-Z"
},
{
"family_name": "Stacey",
"given_name": "Gordon J.",
"clpid": "Stacey-Gordon-J"
}
],
"abstract": "We report CO(5 \u2192 4) and CO(6 \u2192 5) line observations in the dusty starbursting galaxy CRLE (z = 5.667) and the main-sequence (MS) galaxy HZ10 (z = 5.654) with the Northern Extended Millimeter Array. CRLE is the most luminous z > 5 starburst in the COSMOS field and HZ10 is the most gas-rich \"normal\" galaxy currently known at z > 5. We find line luminosities for CO(5 \u2192 4) and CO(6 \u2192 5) of (4.9 \u00b1 0.5) and (3.8 \u00b1 0.4) \u00d7 10\u00b9\u2070 K km s\u207b\u00b9 pc\u00b2 for CRLE and upper limits of 10 K km s\u207b\u00b9 pc\u00b2 for HZ10, respectively. The CO excitation of CRLE appears comparable to other z > 5 dusty star-forming galaxies. For HZ10, these line luminosity limits provide the first significant constraints of this kind for an MS galaxy at z > 5. We find the upper limit of L\u2032_(5\u21924)/L\u2032_(2\u21921) in HZ10 could be similar to the average value for MS galaxies around z \u2248 1.5, suggesting that MS galaxies with comparable gas excitation may already have existed one billion years after the Big Bang. For CRLE we determine the most likely values for the H2 density, kinetic temperature, and dust temperature based on excitation modeling of the CO line ladder. We also derive a total gas mass of (7.1 \u00b1 1.3) \u00d7 10\u00b9\u2070 M_\u2299. Our findings provide some of the currently most detailed constraints on the gas excitation that sets the conditions for star formation in a galaxy protocluster environment at z > 5.",
"doi": "10.3847/1538-4357/ac403a",
"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. 174"
},
{
"id": "authors:kmr10-tv118",
"collection": "authors",
"collection_id": "kmr10-tv118",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220310-752642000",
"type": "article",
"title": "Euclid preparation. XVII. Cosmic Dawn Survey: Spitzer Space Telescope observations of the Euclid deep fields and calibration fields",
"author": [
{
"family_name": "Moneti",
"given_name": "A.",
"clpid": "Moneti-A"
},
{
"family_name": "McCracken",
"given_name": "H. J.",
"orcid": "0000-0002-9489-7765"
},
{
"family_name": "Shuntov",
"given_name": "M.",
"orcid": "0000-0002-7087-0701"
},
{
"family_name": "Kauffmann",
"given_name": "O. B.",
"orcid": "0000-0001-5283-4662"
},
{
"family_name": "Capak",
"given_name": "P.",
"orcid": "0000-0003-3578-6843"
},
{
"family_name": "Davidzon",
"given_name": "I.",
"orcid": "0000-0002-2951-7519"
},
{
"family_name": "Ilbert",
"given_name": "O.",
"orcid": "0000-0002-7303-4397"
},
{
"family_name": "Scarlata",
"given_name": "C.",
"orcid": "0000-0002-9136-8876"
},
{
"family_name": "Toft",
"given_name": "S.",
"orcid": "0000-0003-3631-7176"
},
{
"family_name": "Weaver",
"given_name": "J.",
"orcid": "0000-0003-1614-196X"
},
{
"family_name": "Chary",
"given_name": "R.",
"orcid": "0000-0001-7583-0621",
"clpid": "Chary-Ranga-Ram"
},
{
"family_name": "Cuby",
"given_name": "J.",
"orcid": "0000-0002-8767-1442"
},
{
"family_name": "Faisst",
"given_name": "A. L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Masters",
"given_name": "D. C.",
"orcid": "0000-0001-5382-6138",
"clpid": "Masters-Daniel-C"
},
{
"family_name": "McPartland",
"given_name": "C.",
"orcid": "0000-0003-0639-025X"
},
{
"family_name": "Mobasher",
"given_name": "B."
},
{
"family_name": "Sanders",
"given_name": "D. B.",
"orcid": "0000-0002-1233-9998"
},
{
"family_name": "Scaramella",
"given_name": "R.",
"orcid": "0000-0003-2229-193X"
},
{
"family_name": "Stern",
"given_name": "D.",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-Daniel"
},
{
"family_name": "Szapudi",
"given_name": "I."
},
{
"family_name": "Teplitz",
"given_name": "H.",
"orcid": "0000-0002-7064-5424",
"clpid": "Teplitz-Harry-I"
},
{
"family_name": "Zalesky",
"given_name": "L."
},
{
"family_name": "Amara",
"given_name": "A."
},
{
"family_name": "Auricchio",
"given_name": "N.",
"orcid": "0000-0003-4444-8651"
},
{
"family_name": "Bodendorf",
"given_name": "C."
},
{
"family_name": "Bonino",
"given_name": "D.",
"orcid": "0000-0002-3336-9977"
},
{
"family_name": "Branchini",
"given_name": "E.",
"orcid": "0000-0002-0808-6908"
},
{
"family_name": "Brau-Nogue",
"given_name": "S."
},
{
"family_name": "Brescia",
"given_name": "M.",
"orcid": "0000-0001-9506-5680"
},
{
"family_name": "Brinchmann",
"given_name": "J.",
"orcid": "0000-0003-4359-8797"
},
{
"family_name": "Capobianco",
"given_name": "V.",
"orcid": "0000-0002-3309-7692"
},
{
"family_name": "Carbone",
"given_name": "C."
},
{
"family_name": "Carretero",
"given_name": "J.",
"orcid": "0000-0002-3130-0204"
},
{
"family_name": "Castander",
"given_name": "F. J.",
"orcid": "0000-0001-7316-4573"
},
{
"family_name": "Castellano",
"given_name": "M.",
"orcid": "0000-0001-9875-8263"
},
{
"family_name": "Cavuoti",
"given_name": "S.",
"orcid": "0000-0002-3787-4196"
},
{
"family_name": "Cimatti",
"given_name": "A.",
"orcid": "0000-0002-4409-5633"
},
{
"family_name": "Cledassou",
"given_name": "R.",
"orcid": "0000-0002-8313-2230"
},
{
"family_name": "Congedo",
"given_name": "G.",
"orcid": "0000-0003-2508-0046"
},
{
"family_name": "Conselice",
"given_name": "C. J.",
"orcid": "0000-0003-1949-7638"
},
{
"family_name": "Conversi",
"given_name": "L.",
"orcid": "0000-0002-6710-8476"
},
{
"family_name": "Copin",
"given_name": "Y.",
"orcid": "0000-0002-5317-7518"
},
{
"family_name": "Corcione",
"given_name": "L.",
"orcid": "0000-0002-6497-5881"
},
{
"family_name": "Costille",
"given_name": "A."
},
{
"family_name": "Cropper",
"given_name": "M.",
"orcid": "0000-0003-4571-9468"
},
{
"family_name": "Da Silva",
"given_name": "A."
},
{
"family_name": "Degaudenzi",
"given_name": "H."
},
{
"family_name": "Douspis",
"given_name": "M."
},
{
"family_name": "Dubath",
"given_name": "F."
},
{
"family_name": "Duncan",
"given_name": "C. A. J."
},
{
"family_name": "Dupac",
"given_name": "X."
},
{
"family_name": "Dusini",
"given_name": "S.",
"orcid": "0000-0002-1128-0664"
},
{
"family_name": "Farrens",
"given_name": "S.",
"orcid": "0000-0002-9594-9387"
},
{
"family_name": "Ferriol",
"given_name": "S."
},
{
"family_name": "Fosalba",
"given_name": "P.",
"orcid": "0000-0002-1510-5214"
},
{
"family_name": "Frailis",
"given_name": "M.",
"orcid": "0000-0002-7400-2135"
},
{
"family_name": "Franceschi",
"given_name": "E.",
"orcid": "0000-0002-0585-6591"
},
{
"family_name": "Fumana",
"given_name": "M."
},
{
"family_name": "Garilli",
"given_name": "B.",
"orcid": "0000-0001-7455-8750"
},
{
"family_name": "Gillis",
"given_name": "B.",
"orcid": "0000-0002-4478-1270"
},
{
"family_name": "Giocoli",
"given_name": "C.",
"orcid": "0000-0002-9590-7961"
},
{
"family_name": "Granett",
"given_name": "B. R."
},
{
"family_name": "Grazian",
"given_name": "A."
},
{
"family_name": "Grupp",
"given_name": "F."
},
{
"family_name": "Haugan",
"given_name": "S. V. H."
},
{
"family_name": "Hoekstra",
"given_name": "H.",
"orcid": "0000-0002-0641-3231"
},
{
"family_name": "Holmes",
"given_name": "W.",
"clpid": "Holmes-Warren-A"
},
{
"family_name": "Hormuth",
"given_name": "F."
},
{
"family_name": "Hudelot",
"given_name": "P."
},
{
"family_name": "Jahnke",
"given_name": "K.",
"orcid": "0000-0003-3804-2137"
},
{
"family_name": "Kermiche",
"given_name": "S.",
"orcid": "0000-0002-0302-5735"
},
{
"family_name": "Kiessling",
"given_name": "A.",
"clpid": "Kiessling-Alina"
},
{
"family_name": "Kilbinger",
"given_name": "M.",
"orcid": "0000-0001-9513-7138"
},
{
"family_name": "Kitching",
"given_name": "T.",
"orcid": "0000-0002-4061-4598"
},
{
"family_name": "Kohley",
"given_name": "R."
},
{
"family_name": "K\u00fcmmel",
"given_name": "M."
},
{
"family_name": "Kunz",
"given_name": "M.",
"orcid": "0000-0003-1676-6126"
},
{
"family_name": "Kurki-Suonio",
"given_name": "H.",
"orcid": "0000-0002-4618-3063"
},
{
"family_name": "Ligori",
"given_name": "S.",
"orcid": "0000-0003-4172-4606"
},
{
"family_name": "Lilje",
"given_name": "P. B."
},
{
"family_name": "Lloro",
"given_name": "I.",
"orcid": "0000-0001-5966-1434"
},
{
"family_name": "Maiorano",
"given_name": "E.",
"orcid": "0000-0003-2593-4355"
},
{
"family_name": "Mansutti",
"given_name": "O.",
"orcid": "0000-0001-5758-4658"
},
{
"family_name": "Marggraf",
"given_name": "O.",
"orcid": "0000-0001-7242-3852"
},
{
"family_name": "Markovic",
"given_name": "K.",
"clpid": "Markovic-K"
},
{
"family_name": "Marulli",
"given_name": "F.",
"orcid": "0000-0002-8850-0303"
},
{
"family_name": "Massey",
"given_name": "R.",
"orcid": "0000-0002-6085-3780"
},
{
"family_name": "Maurogordato",
"given_name": "S."
},
{
"family_name": "Meneghetti",
"given_name": "M.",
"orcid": "0000-0003-1225-7084",
"clpid": "Meneghetti-Massimo"
},
{
"family_name": "Merlin",
"given_name": "E.",
"orcid": "0000-0001-6870-8900"
},
{
"family_name": "Meylan",
"given_name": "G."
},
{
"family_name": "Moresco",
"given_name": "M.",
"orcid": "0000-0002-7616-7136"
},
{
"family_name": "Moscardini",
"given_name": "L.",
"orcid": "0000-0002-3473-6716"
},
{
"family_name": "Munari",
"given_name": "E."
},
{
"family_name": "Niemi",
"given_name": "S. M."
},
{
"family_name": "Padilla",
"given_name": "C.",
"orcid": "0000-0001-7951-0166"
},
{
"family_name": "Paltani",
"given_name": "S.",
"orcid": "0000-0002-8108-9179"
},
{
"family_name": "Pasian",
"given_name": "F."
},
{
"family_name": "Pedersen",
"given_name": "K."
},
{
"family_name": "Pires",
"given_name": "S.",
"orcid": "0000-0002-0249-2104"
},
{
"family_name": "Poncet",
"given_name": "M."
},
{
"family_name": "Popa",
"given_name": "L."
},
{
"family_name": "Pozzetti",
"given_name": "L.",
"orcid": "0000-0001-7085-0412"
},
{
"family_name": "Raison",
"given_name": "F."
},
{
"family_name": "Rebolo",
"given_name": "R.",
"orcid": "0000-0003-3767-7085"
},
{
"family_name": "Rhodes",
"given_name": "J.",
"orcid": "0000-0002-4485-8549",
"clpid": "Rhodes-Jason-D"
},
{
"family_name": "Rix",
"given_name": "H.",
"orcid": "0000-0003-4996-9069"
},
{
"family_name": "Roncarelli",
"given_name": "M.",
"orcid": "0000-0001-9587-7822"
},
{
"family_name": "Rossetti",
"given_name": "E."
},
{
"family_name": "Saglia",
"given_name": "R.",
"orcid": "0000-0003-0378-7032"
},
{
"family_name": "Schneider",
"given_name": "P.",
"orcid": "0000-0002-5094-2245"
},
{
"family_name": "Secroun",
"given_name": "A.",
"orcid": "0000-0003-0505-3710"
},
{
"family_name": "Seidel",
"given_name": "G."
},
{
"family_name": "Serrano",
"given_name": "S."
},
{
"family_name": "Sirignano",
"given_name": "C."
},
{
"family_name": "Sirri",
"given_name": "G."
},
{
"family_name": "Stanco",
"given_name": "L."
},
{
"family_name": "Tallada-Cresp\u00ed",
"given_name": "P."
},
{
"family_name": "Taylor",
"given_name": "A. N."
},
{
"family_name": "Tereno",
"given_name": "I.",
"orcid": "0000-0002-4537-6218"
},
{
"family_name": "Toledo-Moreo",
"given_name": "R.",
"orcid": "0000-0002-2997-4859"
},
{
"family_name": "Torradeflot",
"given_name": "F."
},
{
"family_name": "Wang",
"given_name": "Y.",
"orcid": "0000-0002-4749-2984",
"clpid": "Wang-Yun"
},
{
"family_name": "Welikala",
"given_name": "N."
},
{
"family_name": "Weller",
"given_name": "J.",
"orcid": "0000-0002-8282-2010"
},
{
"family_name": "Zamorani",
"given_name": "G.",
"orcid": "0000-0002-2318-301X"
},
{
"family_name": "Zoubian",
"given_name": "J."
},
{
"family_name": "Andreon",
"given_name": "S.",
"orcid": "0000-0002-2041-8784"
},
{
"family_name": "Bardelli",
"given_name": "S.",
"orcid": "0000-0002-8900-0298"
},
{
"family_name": "Camera",
"given_name": "S.",
"orcid": "0000-0003-3399-3574"
},
{
"family_name": "Graci\u00e1-Carpio",
"given_name": "J.",
"orcid": "0000-0003-4689-3134"
},
{
"family_name": "Medinaceli",
"given_name": "E.",
"orcid": "0000-0002-4040-7783"
},
{
"family_name": "Mei",
"given_name": "S.",
"orcid": "0000-0002-2849-559X"
},
{
"family_name": "Polenta",
"given_name": "G.",
"orcid": "0000-0003-4067-9196"
},
{
"family_name": "Romelli",
"given_name": "E.",
"orcid": "0000-0003-3069-9222"
},
{
"family_name": "Sureau",
"given_name": "F."
},
{
"family_name": "Tenti",
"given_name": "M.",
"orcid": "0000-0002-4254-5901"
},
{
"family_name": "Vassallo",
"given_name": "T."
},
{
"family_name": "Zacchei",
"given_name": "A.",
"orcid": "0000-0003-0396-1192"
},
{
"family_name": "Zucca",
"given_name": "E.",
"orcid": "0000-0002-5845-8132"
},
{
"family_name": "Baccigalupi",
"given_name": "C.",
"orcid": "0000-0002-8211-1630"
},
{
"family_name": "Balaguera-Antol\u00ednez",
"given_name": "A.",
"orcid": "0000-0001-5028-3035"
},
{
"family_name": "Bernardeau",
"given_name": "F."
},
{
"family_name": "Biviano",
"given_name": "A.",
"orcid": "0000-0002-0857-0732"
},
{
"family_name": "Bolzonella",
"given_name": "M."
},
{
"family_name": "Bozzo",
"given_name": "E.",
"orcid": "0000-0002-7504-7423"
},
{
"family_name": "Burigana",
"given_name": "C.",
"orcid": "0000-0002-3005-5796"
},
{
"family_name": "Cabanac",
"given_name": "R.",
"orcid": "0000-0001-6679-2600"
},
{
"family_name": "Cappi",
"given_name": "A.",
"orcid": "0000-0002-9200-7167"
},
{
"family_name": "Carvalho",
"given_name": "C. S."
},
{
"family_name": "Casas",
"given_name": "S."
},
{
"family_name": "Castignani",
"given_name": "G.",
"orcid": "0000-0001-6831-0687"
},
{
"family_name": "Colodro-Conde",
"given_name": "C."
},
{
"family_name": "Coupon",
"given_name": "J."
},
{
"family_name": "Courtois",
"given_name": "H. M.",
"orcid": "0000-0003-0509-1776"
},
{
"family_name": "Di Ferdinando",
"given_name": "D."
},
{
"family_name": "Farina",
"given_name": "M."
},
{
"family_name": "Finelli",
"given_name": "F.",
"orcid": "0000-0002-6694-3269"
},
{
"family_name": "Flose-Reimberg",
"given_name": "P."
},
{
"family_name": "Fotopoulou",
"given_name": "S.",
"orcid": "0000-0002-9686-254X"
},
{
"family_name": "Galeotta",
"given_name": "S.",
"orcid": "0000-0002-3748-5115"
},
{
"family_name": "Ganga",
"given_name": "K."
},
{
"family_name": "Garc\u00eda-Bellido",
"given_name": "J.",
"orcid": "0000-0002-9370-8360"
},
{
"family_name": "Gaztanaga",
"given_name": "E.",
"orcid": "0000-0001-9632-0815"
},
{
"family_name": "Gozaliasl",
"given_name": "G.",
"orcid": "0000-0002-0236-919X"
},
{
"family_name": "Hook",
"given_name": "I.",
"orcid": "0000-0002-2960-978X"
},
{
"family_name": "Joachimi",
"given_name": "B."
},
{
"family_name": "Kansal",
"given_name": "V."
},
{
"family_name": "Keihanen",
"given_name": "E.",
"orcid": "0000-0003-1804-7715"
},
{
"family_name": "Kirkpatrick",
"given_name": "C. C."
},
{
"family_name": "Lindholm",
"given_name": "V."
},
{
"family_name": "Mainetti",
"given_name": "G."
},
{
"family_name": "Maino",
"given_name": "D.",
"orcid": "0000-0002-4761-1242"
},
{
"family_name": "Maoli",
"given_name": "R."
},
{
"family_name": "Martinelli",
"given_name": "M."
},
{
"family_name": "Martinet",
"given_name": "N.",
"orcid": "0000-0003-2786-7790"
},
{
"family_name": "Maturi",
"given_name": "M."
},
{
"family_name": "Metcalf",
"given_name": "R. B."
},
{
"family_name": "Morgante",
"given_name": "G."
},
{
"family_name": "Morisset",
"given_name": "N."
},
{
"family_name": "Nucita",
"given_name": "A.",
"orcid": "0000-0002-7926-3481"
},
{
"family_name": "Patrizii",
"given_name": "L.",
"orcid": "0000-0002-9712-977X"
},
{
"family_name": "Potter",
"given_name": "D."
},
{
"family_name": "Renzini",
"given_name": "A.",
"orcid": "0000-0002-7093-7355"
},
{
"family_name": "Riccio",
"given_name": "G.",
"orcid": "0000-0001-7020-1172"
},
{
"family_name": "S\u00e1nchez",
"given_name": "A. G.",
"orcid": "0000-0003-1198-831X"
},
{
"family_name": "Sapone",
"given_name": "D.",
"orcid": "0000-0001-7089-4503"
},
{
"family_name": "Schirmer",
"given_name": "M.",
"orcid": "0000-0003-2568-9994"
},
{
"family_name": "Schultheis",
"given_name": "M.",
"orcid": "0000-0002-6590-1657"
},
{
"family_name": "Scottez",
"given_name": "V."
},
{
"family_name": "Sefusatti",
"given_name": "E."
},
{
"family_name": "Teyssier",
"given_name": "R.",
"orcid": "0000-0001-7689-0933"
},
{
"family_name": "Tubio",
"given_name": "O."
},
{
"family_name": "Tutusaus",
"given_name": "I.",
"orcid": "0000-0002-3199-0399"
},
{
"family_name": "Valiviita",
"given_name": "J.",
"orcid": "0000-0001-6225-3693"
},
{
"family_name": "Viel",
"given_name": "M.",
"orcid": "0000-0002-2642-5707"
},
{
"family_name": "Hildebrandt",
"given_name": "H."
},
{
"literal": "Euclid Collaboration"
}
],
"abstract": "We present a new infrared survey covering the three Euclid deep fields and four other Euclid calibration fields using Spitzer Space Telescope's Infrared Array Camera (IRAC). We combined these new observations with all relevant IRAC archival data of these fields in order to produce the deepest possible mosaics of these regions. In total, these observations represent nearly 11 % of the total Spitzer Space Telescope mission time. The resulting mosaics cover a total of approximately 71.5 deg\u00b2 in the 3.6 and 4.5 \u03bcm bands, and approximately 21.8 deg\u00b2 in the 5.8 and 8 \u03bcm bands. They reach at least 24 AB magnitude (measured to 5\u03c3, in a 2\u2033.5 aperture) in the 3.6 \u03bcm band and up to \u223c5 mag deeper in the deepest regions. The astrometry is tied to the Gaia astrometric reference system, and the typical astrometric uncertainty for sources with 16\u2004Spitzer Space Telescope has now been decommissioned, these mosaics are likely to be the definitive reduction of these IRAC data. This survey therefore represents an essential first step in assembling multi-wavelength data on the Euclid deep fields, which are set to become some of the premier fields for extragalactic astronomy in the 2020s.",
"doi": "10.1051/0004-6361/202142361",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2022-02",
"volume": "658",
"pages": "Art. No. A126"
},
{
"id": "authors:b54x4-q4q64",
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"collection_id": "b54x4-q4q64",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220114-265237000",
"type": "article",
"title": "COSMOS2020: A Panchromatic View of the Universe to z \u223c 10 from Two Complementary Catalogs",
"author": [
{
"family_name": "Weaver",
"given_name": "J. R.",
"orcid": "0000-0003-1614-196X",
"clpid": "Weaver-John-R"
},
{
"family_name": "Kauffmann",
"given_name": "O. B.",
"orcid": "0000-0001-5283-4662"
},
{
"family_name": "Ilbert",
"given_name": "O.",
"orcid": "0000-0002-7303-4397"
},
{
"family_name": "McCracken",
"given_name": "H. J.",
"orcid": "0000-0002-9489-7765"
},
{
"family_name": "Moneti",
"given_name": "A."
},
{
"family_name": "Toft",
"given_name": "S.",
"orcid": "0000-0003-3631-7176"
},
{
"family_name": "Brammer",
"given_name": "G.",
"orcid": "0000-0003-2680-005X"
},
{
"family_name": "Shuntov",
"given_name": "M.",
"orcid": "0000-0002-7087-0701"
},
{
"family_name": "Davidzon",
"given_name": "I.",
"orcid": "0000-0002-2951-7519"
},
{
"family_name": "Hsieh",
"given_name": "B. C.",
"orcid": "0000-0001-5615-4904"
},
{
"family_name": "Laigle",
"given_name": "C."
},
{
"family_name": "Anastasiou",
"given_name": "A.",
"orcid": "0000-0001-8558-7709"
},
{
"family_name": "Jespersen",
"given_name": "C. K.",
"orcid": "0000-0002-8896-6496"
},
{
"family_name": "Vinther",
"given_name": "J.",
"orcid": "0000-0002-4418-752X"
},
{
"family_name": "Capak",
"given_name": "P.",
"orcid": "0000-0003-3578-6843"
},
{
"family_name": "Casey",
"given_name": "C. M.",
"orcid": "0000-0002-0930-6466"
},
{
"family_name": "McPartland",
"given_name": "C. J. R.",
"orcid": "0000-0003-0639-025X"
},
{
"family_name": "Milvang-Jensen",
"given_name": "B.",
"orcid": "0000-0002-2281-2785"
},
{
"family_name": "Mobasher",
"given_name": "B."
},
{
"family_name": "Sanders",
"given_name": "D. B.",
"orcid": "0000-0002-1233-9998"
},
{
"family_name": "Zalesky",
"given_name": "L.",
"orcid": "0000-0001-5680-2326"
},
{
"family_name": "Arnouts",
"given_name": "S."
},
{
"family_name": "Aussel",
"given_name": "H.",
"orcid": "0000-0002-1371-5705"
},
{
"family_name": "Dunlop",
"given_name": "J. S."
},
{
"family_name": "Faisst",
"given_name": "A.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Franx",
"given_name": "M.",
"orcid": "0000-0002-8871-3026"
},
{
"family_name": "Furtak",
"given_name": "L. J.",
"orcid": "0000-0001-6278-032X"
},
{
"family_name": "Fynbo",
"given_name": "J. P. U.",
"orcid": "0000-0002-8149-8298"
},
{
"family_name": "Gould",
"given_name": "K. M. L.",
"orcid": "0000-0003-4196-5960"
},
{
"family_name": "Greve",
"given_name": "T. R.",
"orcid": "0000-0002-2554-1837"
},
{
"family_name": "Gwyn",
"given_name": "S.",
"orcid": "0000-0001-8221-8406"
},
{
"family_name": "Kartaltepe",
"given_name": "J. S.",
"orcid": "0000-0001-9187-3605"
},
{
"family_name": "Kashino",
"given_name": "D.",
"orcid": "0000-0001-9044-1747"
},
{
"family_name": "Koekemoer",
"given_name": "A. M.",
"orcid": "0000-0002-6610-2048"
},
{
"family_name": "Kokorev",
"given_name": "V.",
"orcid": "0000-0002-5588-9156"
},
{
"family_name": "Le F\u00e8vre",
"given_name": "O.",
"orcid": "0000-0001-5891-2596"
},
{
"family_name": "Lilly",
"given_name": "S.",
"orcid": "0000-0002-6423-3597"
},
{
"family_name": "Masters",
"given_name": "D.",
"orcid": "0000-0001-5382-6138",
"clpid": "Masters-Daniel-C"
},
{
"family_name": "Magdis",
"given_name": "G.",
"orcid": "0000-0002-4872-2294"
},
{
"family_name": "Mehta",
"given_name": "V.",
"orcid": "0000-0001-7166-6035"
},
{
"family_name": "Peng",
"given_name": "Y."
},
{
"family_name": "Riechers",
"given_name": "D. A.",
"orcid": "0000-0001-9585-1462"
},
{
"family_name": "Salvato",
"given_name": "M.",
"orcid": "0000-0001-7116-9303"
},
{
"family_name": "Sawicki",
"given_name": "M.",
"orcid": "0000-0002-7712-7857"
},
{
"family_name": "Scarlata",
"given_name": "C.",
"orcid": "0000-0002-9136-8876"
},
{
"family_name": "Scoville",
"given_name": "N.",
"orcid": "0000-0002-0438-3323",
"clpid": "Scoville-N-Z"
},
{
"family_name": "Shirley",
"given_name": "R.",
"orcid": "0000-0002-1114-0135"
},
{
"family_name": "Silverman",
"given_name": "J. D.",
"orcid": "0000-0002-0000-6977"
},
{
"family_name": "Sneppen",
"given_name": "A.",
"orcid": "0000-0002-5460-6126"
},
{
"family_name": "Smolc\u0306i\u0107",
"given_name": "V.",
"orcid": "0000-0002-3893-8614"
},
{
"family_name": "Steinhardt",
"given_name": "C.",
"orcid": "0000-0003-3780-6801"
},
{
"family_name": "Stern",
"given_name": "D.",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-Daniel"
},
{
"family_name": "Tanaka",
"given_name": "M.",
"orcid": "0000-0002-5011-5178"
},
{
"family_name": "Taniguchi",
"given_name": "Y.",
"orcid": "0000-0003-2247-3741"
},
{
"family_name": "Teplitz",
"given_name": "H. I.",
"orcid": "0000-0002-7064-5424",
"clpid": "Teplitz-Harry-I"
},
{
"family_name": "Vaccari",
"given_name": "M.",
"orcid": "0000-0002-6748-0577"
},
{
"family_name": "Wang",
"given_name": "W.-H.",
"orcid": "0000-0003-2588-1265"
},
{
"family_name": "Zamorani",
"given_name": "G.",
"orcid": "0000-0002-2318-301X"
}
],
"abstract": "The Cosmic Evolution Survey (COSMOS) has become a cornerstone of extragalactic astronomy. Since the last public catalog in 2015, a wealth of new imaging and spectroscopic data have been collected in the COSMOS field. This paper describes the collection, processing, and analysis of these new imaging data to produce a new reference photometric redshift catalog. Source detection and multiwavelength photometry are performed for 1.7 million sources across the 2 deg2 of the COSMOS field, \u223c966,000 of which are measured with all available broadband data using both traditional aperture photometric methods and a new profile-fitting photometric extraction tool, The Farmer, which we have developed. A detailed comparison of the two resulting photometric catalogs is presented. Photometric redshifts are computed for all sources in each catalog utilizing two independent photometric redshift codes. Finally, a comparison is made between the performance of the photometric methodologies and of the redshift codes to demonstrate an exceptional degree of self-consistency in the resulting photometric redshifts. The i i < 27 reach a precision of 5%. Finally, these results are discussed in the context of previous, current, and future surveys in the COSMOS field. Compared to COSMOS2015, it reaches the same photometric redshift precision at almost one magnitude deeper. Both photometric catalogs and their photometric redshift solutions and physical parameters will be made available through the usual astronomical archive systems (ESO Phase 3, IPAC-IRSA, and CDS).",
"doi": "10.3847/1538-4365/ac3078",
"issn": "0067-0049",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2022-01",
"series_number": "1",
"volume": "258",
"issue": "1",
"pages": "Art. No. 11"
},
{
"id": "authors:g6267-tja67",
"collection": "authors",
"collection_id": "g6267-tja67",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210412-131332609",
"type": "article",
"title": "The ALPINE-ALMA [C\u2009II] Survey: kinematic diversity and rotation in massive star-forming galaxies at z ~ 4.4\u20135.9",
"author": [
{
"family_name": "Jones",
"given_name": "G. C.",
"orcid": "0000-0002-0267-9024",
"clpid": "Jones-Gareth-C"
},
{
"family_name": "Vergani",
"given_name": "D.",
"orcid": "0000-0003-0898-2216",
"clpid": "Vergani-Daniela"
},
{
"family_name": "Romano",
"given_name": "M.",
"orcid": "0000-0002-9948-3916",
"clpid": "Romano-Michael"
},
{
"family_name": "Ginolfi",
"given_name": "M.",
"orcid": "0000-0002-8231-821X",
"clpid": "Ginolfi-Michele"
},
{
"family_name": "Fudamoto",
"given_name": "Y.",
"orcid": "0000-0001-7440-8832",
"clpid": "Fudamoto-Yoshinobu"
},
{
"family_name": "B\u00e9thermin",
"given_name": "M.",
"orcid": "0000-0002-3915-2015",
"clpid": "B\u00e9thermin-Matthieu"
},
{
"family_name": "Fujimoto",
"given_name": "S.",
"orcid": "0000-0001-7201-5066",
"clpid": "Fujimoto-Seiji"
},
{
"family_name": "Lemaux",
"given_name": "B. C.",
"orcid": "0000-0002-1428-7036",
"clpid": "Lemaux-Brian-C"
},
{
"family_name": "Morselli",
"given_name": "L.",
"orcid": "0000-0003-0753-2571",
"clpid": "Morselli-Laura"
},
{
"family_name": "Capak",
"given_name": "P.",
"orcid": "0000-0003-3578-6843",
"clpid": "Capak-Peter"
},
{
"family_name": "Cassata",
"given_name": "P.",
"orcid": "0000-0002-6716-4400",
"clpid": "Cassata-Paolo"
},
{
"family_name": "Faisst",
"given_name": "A.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Le F\u00e8vre",
"given_name": "O.",
"orcid": "0000-0001-5891-2596",
"clpid": "Le-F\u00e8vre-Olivier"
},
{
"family_name": "Schaerer",
"given_name": "D.",
"orcid": "0000-0001-7144-7182",
"clpid": "Schaerer-Daniel"
},
{
"family_name": "Silverman",
"given_name": "J. D.",
"orcid": "0000-0002-0000-6977",
"clpid": "Silverman-John-D"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Boquien",
"given_name": "M.",
"orcid": "0000-0003-0946-6176",
"clpid": "Boquien-M\u00e9d\u00e9ric"
},
{
"family_name": "Cimatti",
"given_name": "A.",
"orcid": "0000-0002-4409-5633",
"clpid": "Cimatti-Andrea"
},
{
"family_name": "Dessauges-Zavadsky",
"given_name": "M.",
"orcid": "0000-0003-0348-2917",
"clpid": "Dessauges-Zavadsky-Miroslava"
},
{
"family_name": "Ibar",
"given_name": "E.",
"clpid": "Ibar-Eduardo"
},
{
"family_name": "Maiolino",
"given_name": "R.",
"orcid": "0000-0002-4985-3819",
"clpid": "Maiolino-Roberto"
},
{
"family_name": "Rizzo",
"given_name": "F.",
"clpid": "Rizzo-Francesca"
},
{
"family_name": "Talia",
"given_name": "M.",
"orcid": "0000-0003-4352-2063",
"clpid": "Talia-Margherita"
},
{
"family_name": "Zamorani",
"given_name": "G.",
"orcid": "0000-0002-2318-301X",
"clpid": "Zamorani-Giovanni"
}
],
"abstract": "While the kinematics of galaxies up to z \u223c 3 have been characterized in detail, only a handful of galaxies at high redshift (z > 4) have been examined in such a way. The Atacama Large Millimeter/submillimeter Array (ALMA) Large Program to INvestigate [C\u2009II] at Early times (ALPINE) survey observed a statistically significant sample of 118 star-forming main-sequence galaxies at z = 4.4\u20135.9 in [C\u2009II]158\u2009\u03bc\u03bcm emission, increasing the number of such observations by nearly 10\u00d7. A preliminary qualitative classification of these sources revealed a diversity of kinematic types (i.e. rotators, mergers, and dispersion-dominated systems). In this work, we supplement the initial classification by applying quantitative analyses to the ALPINE data: a tilted ring model (TRM) fitting code (^(3D)BAROLO), a morphological classification (Gini-M\u2082\u2080), and a set of disc identification criteria. Of the 75 [C\u2009II]-detected ALPINE galaxies, 29 are detected at sufficient significance and spatial resolution to allow for TRM fitting and the derivation of morphological and kinematic parameters. These 29 sources constitute a high-mass subset of the ALPINE sample (\u2060M\u2217 > 10^(9.5) M_\u2299). We robustly classify 14 of these sources (six rotators, five mergers, and three dispersion-dominated systems); the remaining sources showing complex behaviour. By exploring the G-M\u2082\u2080 of z > 4 rest-frame far-infrared and [C\u2009II] data for the first time, we find that our 1 arcsec \u223c 6\u2009kpc resolution data alone are insufficient to separate galaxy types. We compare the rotation curves and dynamical mass profiles of the six ALPINE rotators to the two previously detected z \u223c 4\u20136 unlensed main-sequence rotators, finding high rotational velocities (\u223c50\u2013250\u2009km\u2009s\u207b\u00b9) and a diversity of rotation curve shapes.",
"doi": "10.1093/mnras/stab2226",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2021-11",
"series_number": "3",
"volume": "507",
"issue": "3",
"pages": "3540-3563"
},
{
"id": "authors:jth25-h5s92",
"collection": "authors",
"collection_id": "jth25-h5s92",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211108-203838376",
"type": "article",
"title": "Further support for a trio of mass-to-light deviations in Abell 370: free-form grale lens inversion using BUFFALO strong lensing data",
"author": [
{
"family_name": "Ghosh",
"given_name": "Agniva",
"orcid": "0000-0001-5110-5433",
"clpid": "Ghosh-Agniva"
},
{
"family_name": "Williams",
"given_name": "Liliya L. R.",
"orcid": "0000-0002-6039-8706",
"clpid": "Williams-Liliya-L-R"
},
{
"family_name": "Liesenborgs",
"given_name": "Jori",
"orcid": "0000-0002-3648-8031",
"clpid": "Liesenborgs-Jori"
},
{
"family_name": "Acebron",
"given_name": "Ana",
"orcid": "0000-0003-3108-9039",
"clpid": "Acebron-Ana"
},
{
"family_name": "Jauzac",
"given_name": "Mathilde",
"orcid": "0000-0003-1974-8732",
"clpid": "Jauzac-Mathilde"
},
{
"family_name": "Koekemoer",
"given_name": "Anton M.",
"orcid": "0000-0002-6610-2048",
"clpid": "Koekemoer-Anton-M"
},
{
"family_name": "Mahler",
"given_name": "Guillaume",
"orcid": "0000-0003-3266-2001",
"clpid": "Mahler-Guillaume"
},
{
"family_name": "Niemiec",
"given_name": "Anna",
"orcid": "0000-0003-3791-2647",
"clpid": "Niemiec-Anna"
},
{
"family_name": "Steinhardt",
"given_name": "Charles",
"orcid": "0000-0003-3780-6801",
"clpid": "Steinhardt-Charles-L"
},
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Lagattuta",
"given_name": "David",
"orcid": "0000-0002-7633-2883",
"clpid": "Lagattuta-David"
},
{
"family_name": "Natarajan",
"given_name": "Priyamvada",
"orcid": "0000-0002-5554-8896",
"clpid": "Natarajan-Priyamvada"
}
],
"abstract": "We use the Beyond Ultra-deep Frontier Fields and Legacy Observations (BUFFALO) strong lensing image catalogue of the merging galaxy cluster Abell 370 to obtain a mass model using free-form lens inversion algorithm GRALE. The improvement of the strong lensing data quality results in a lens plane rms of only 0.45 arcsec, about a factor of two lower than that of our existing HFF v4 reconstruction. We attribute the improvement to spectroscopic data and use of the full reprocessed HST mosaics. In our reconstructed mass model, we found indications of three distinct mass features in Abell 370: (i) a \u223c35 kpc offset between the northern BCG and the nearest mass peak, (ii) a \u223c100 kpc mass concentration of roughly critical density \u223c250 kpc east of the main cluster, and (iii) a probable filament-like structure passing N-S through the cluster. While (i) is present in some form in most publicly available reconstructions spanning the range of modelling techniques: parametric, hybrid, and free-form, (ii) and (iii) are recovered by only about half of the reconstructions. We tested our hypothesis on the presence of the filament-like structure by creating a synthetic cluster \u2013 Irtysh IIIc \u2013 mocking the situation of a cluster with external mass. We also computed the source plane magnification distributions. Using them, we estimated the probabilities of magnifications in the source plane, and scrutinized their redshift dependence. Finally, we explored the lensing effects of Abell 370 on the luminosity functions of sources at z_s = 9.0, finding it consistent with published results.",
"doi": "10.1093/mnras/stab1196",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2021-10",
"series_number": "4",
"volume": "506",
"issue": "4",
"pages": "6144-6158"
},
{
"id": "authors:qxcza-4bp53",
"collection": "authors",
"collection_id": "qxcza-4bp53",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211011-155239475",
"type": "article",
"title": "The ALPINE-ALMA [CII] survey. Dust mass budget in the early Universe",
"author": [
{
"family_name": "Pozzi",
"given_name": "F.",
"orcid": "0000-0002-7412-647X",
"clpid": "Pozzi-Francesca"
},
{
"family_name": "Calura",
"given_name": "F.",
"orcid": "0000-0002-6175-0871"
},
{
"family_name": "Fudamoto",
"given_name": "Y.",
"orcid": "0000-0001-7440-8832"
},
{
"family_name": "Dessauges-Zavadsky",
"given_name": "M.",
"orcid": "0000-0003-0348-2917"
},
{
"family_name": "Gruppioni",
"given_name": "C.",
"orcid": "0000-0002-5836-4056"
},
{
"family_name": "Talia",
"given_name": "M.",
"orcid": "0000-0003-4352-2063"
},
{
"family_name": "Zamorani",
"given_name": "G.",
"orcid": "0000-0002-2318-301X"
},
{
"family_name": "B\u00e9thermin",
"given_name": "M.",
"orcid": "0000-0002-3915-2015"
},
{
"family_name": "Cimatti",
"given_name": "A.",
"orcid": "0000-0002-4409-5633"
},
{
"family_name": "Enia",
"given_name": "A.",
"orcid": "0000-0002-0200-2857"
},
{
"family_name": "Khusanova",
"given_name": "Y.",
"orcid": "0000-0002-7220-397X"
},
{
"family_name": "Decarli",
"given_name": "R.",
"orcid": "0000-0002-2662-8803"
},
{
"family_name": "Le F\u00e8vre",
"given_name": "O.",
"orcid": "0000-0001-5891-2596"
},
{
"family_name": "Capak",
"given_name": "P.",
"orcid": "0000-0003-3578-6843",
"clpid": "Capak-Peter"
},
{
"family_name": "Cassata",
"given_name": "P.",
"orcid": "0000-0002-6716-4400"
},
{
"family_name": "Faisst",
"given_name": "A. L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Schaerer",
"given_name": "D.",
"orcid": "0000-0001-7144-7182"
},
{
"family_name": "Silverman",
"given_name": "J.",
"orcid": "0000-0002-0000-6977"
},
{
"family_name": "Bardelli",
"given_name": "S.",
"orcid": "0000-0002-8900-0298"
},
{
"family_name": "Boquien",
"given_name": "M.",
"orcid": "0000-0003-0946-6176",
"clpid": "Boquien-M"
},
{
"family_name": "Narayanan",
"given_name": "D.",
"orcid": "0000-0002-7064-4309"
},
{
"family_name": "Ginolfi",
"given_name": "M.",
"orcid": "0000-0002-8231-821X"
},
{
"family_name": "Hathi",
"given_name": "N. P.",
"orcid": "0000-0001-6145-5090"
},
{
"family_name": "Jones",
"given_name": "G. C.",
"orcid": "0000-0002-0267-9024"
},
{
"family_name": "Koekemoer",
"given_name": "A. M.",
"orcid": "0000-0002-6610-2048"
},
{
"family_name": "Lemaux",
"given_name": "B. C.",
"orcid": "0000-0002-1428-7036"
},
{
"family_name": "Loiacono",
"given_name": "F.",
"orcid": "0000-0002-8858-6784"
},
{
"family_name": "Maiolino",
"given_name": "R.",
"orcid": "0000-0002-4985-3819"
},
{
"family_name": "Riechers",
"given_name": "D. A.",
"orcid": "0000-0001-9585-1462"
},
{
"family_name": "Rodighiero",
"given_name": "G.",
"orcid": "0000-0002-9415-2296",
"clpid": "Rodighiero-Giulia"
},
{
"family_name": "Romano",
"given_name": "M.",
"orcid": "0000-0002-9948-3916"
},
{
"family_name": "Vallini",
"given_name": "L.",
"orcid": "0000-0002-3258-3672"
},
{
"family_name": "Vergani",
"given_name": "D.",
"orcid": "0000-0003-0898-2216"
},
{
"family_name": "Zucca",
"given_name": "E.",
"orcid": "0000-0002-5845-8132"
}
],
"abstract": "Aims. The dust content of normal galaxies and the dust mass density (DMD) at high-z (z\u2004>\u20044) are unconstrained given the source confusion and the sensitivity limitations of previous observations. The ALMA Large Program to INvestigate [CII] at Early times (ALPINE), which targeted 118 ultra-violet (UV)-selected star-forming galaxies at 4.4\u2004<\u2004z\u2004<\u20045.9, provides a new opportunity to tackle this issue for the first time with a statistically robust dataset. \n\nMethods. We exploited the rest-frame far-infrared (FIR) fluxes of 23 galaxies individually detected in their continuum emission, as well as stacked continuum images, to measure the dust content of the 118 UV-selected ALPINE galaxies. We focused on the dust scaling relations and, by comparison with predictions from chemical evolution models, we probed the evolutionary stage of UV-selected galaxies at high-z. By using the observed correlation between the UV luminosity and the dust mass, we estimated the DMD of UV-selected galaxies at z\u2004\u223c\u20045, weighting the galaxies by means of the UV luminosity function. The derived DMD is compared with the value we estimated from ten ALPINE galaxies blindly detected in the FIR continuum, at the redshift of the ALPINE targets. \n\nResults. Our ALMA survey allows the exploration for the first time of the dust content in normal star-forming galaxies at z\u2004>\u20044 in a statistically robust sample of sources. The comparison of the observed dust scaling relations with chemical evolution models suggests that ALPINE galaxies are not likely progenitors of disc galaxies, but of intermediate- and low-mass proto-spheroids, resulting in present-day bulges of spiral or elliptical galaxies. Interestingly, this conclusion is in line with the independent morphological analysis that shows that the majority (\u223c70%) of the dust-continuum detected galaxies have a disturbed morphology. The DMD obtained at z\u2004\u223c\u20045 from UV-selected sources is \u223c30% of the value obtained from blind FIR-selected sources, showing that the UV selection misses the most dust-rich, UV-obscured galaxies.",
"doi": "10.1051/0004-6361/202040258",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2021-09",
"volume": "653",
"pages": "Art. No. A84"
},
{
"id": "authors:3vkxz-myx52",
"collection": "authors",
"collection_id": "3vkxz-myx52",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211020-145122379",
"type": "article",
"title": "The ALPINE-ALMA [CII] survey. The contribution of major mergers to the galaxy mass assembly at z \u223c 5",
"author": [
{
"family_name": "Romano",
"given_name": "M.",
"orcid": "0000-0002-9948-3916",
"clpid": "Romano-Michael"
},
{
"family_name": "Cassata",
"given_name": "P.",
"orcid": "0000-0002-6716-4400"
},
{
"family_name": "Morselli",
"given_name": "L.",
"orcid": "0000-0003-0753-2571"
},
{
"family_name": "Jones",
"given_name": "G. C.",
"orcid": "0000-0002-0267-9024"
},
{
"family_name": "Ginolfi",
"given_name": "M.",
"orcid": "0000-0002-8231-821X"
},
{
"family_name": "Zanella",
"given_name": "A.",
"orcid": "0000-0001-8600-7008"
},
{
"family_name": "B\u00e9thermin",
"given_name": "M.",
"orcid": "0000-0002-3915-2015"
},
{
"family_name": "Capak",
"given_name": "P.",
"orcid": "0000-0003-3578-6843",
"clpid": "Capak-Peter"
},
{
"family_name": "Faisst",
"given_name": "A.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Le F\u00e8vre",
"given_name": "O.",
"orcid": "0000-0001-5891-2596"
},
{
"family_name": "Schaerer",
"given_name": "D.",
"orcid": "0000-0001-7144-7182"
},
{
"family_name": "Silverman",
"given_name": "J. D.",
"orcid": "0000-0002-0000-6977",
"clpid": "Silverman-J-D"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Bardelli",
"given_name": "S.",
"orcid": "0000-0002-8900-0298"
},
{
"family_name": "Boquien",
"given_name": "M.",
"orcid": "0000-0003-0946-6176"
},
{
"family_name": "Cimatti",
"given_name": "A.",
"orcid": "0000-0002-4409-5633"
},
{
"family_name": "Dessauges-Zavadsky",
"given_name": "M.",
"orcid": "0000-0003-0348-2917"
},
{
"family_name": "Enia",
"given_name": "A.",
"orcid": "0000-0002-0200-2857"
},
{
"family_name": "Fujimoto",
"given_name": "S.",
"orcid": "0000-0001-7201-5066"
},
{
"family_name": "Gruppioni",
"given_name": "C.",
"orcid": "0000-0002-5836-4056"
},
{
"family_name": "Hathi",
"given_name": "N. P.",
"orcid": "0000-0001-6145-5090"
},
{
"family_name": "Ibar",
"given_name": "E."
},
{
"family_name": "Koekemoer",
"given_name": "A. M.",
"orcid": "0000-0002-6610-2048"
},
{
"family_name": "Lemaux",
"given_name": "B. C.",
"orcid": "0000-0002-1428-7036"
},
{
"family_name": "Rodighiero",
"given_name": "G.",
"orcid": "0000-0002-9415-2296"
},
{
"family_name": "Vergani",
"given_name": "D.",
"orcid": "0000-0003-0898-2216"
},
{
"family_name": "Zamorani",
"given_name": "G.",
"orcid": "0000-0002-2318-301X"
},
{
"family_name": "Zucca",
"given_name": "E.",
"orcid": "0000-0002-5845-8132"
}
],
"abstract": "Context. Galaxy mergers are thought to be one of the main mechanisms of the mass assembly of galaxies in the Universe, but there is still little direct observational evidence of how frequent they are at z\u2004\u2273\u20044. Recently, many works have suggested a possible increase in the fraction of major mergers in the early Universe, reviving the debate on which processes (e.g., cold accretion, star formation, mergers) most contribute to the mass build-up of galaxies through cosmic time.\nAims. To estimate the importance of major mergers in this context, we make use of the new data collected by the ALMA Large Program to INvestigate [CII] at Early times (ALPINE) survey, which attempted to observe the [CII] 158 \u03bcm emission line from a sample of 75 main-sequence star-forming galaxies at 4.4\u2004< \u2004z\u2004< \u20045.9.\nMethods. We used, for the first time, the morpho-kinematic information provided by the [CII] emission, along with archival multiwavelength data to obtain the fraction of major mergers (f_(MM)) at z\u2004\u223c\u20045. By combining the results from ALPINE with those at lower redshifts from the literature, we also studied the evolution of the merger fraction through cosmic time. We then used different redshift-evolving merger timescales (T_(MM)) to convert this fraction into the merger rate per galaxy (R_(MM)) and in the volume-averaged merger rate (\u0393_(MM)).\nResults. We find a merger fraction of f_(MM)\u2004\u223c\u20040.44 (0.34) at z\u2004\u223c\u20044.5 (5.5) from ALPINE. By combining our results with those at lower redshifts, we computed the cosmic evolution of the merger fraction which is described by a rapid increase from the local Universe to higher redshifts, a peak at z\u2004\u223c\u20043, and a slow decrease toward earlier epochs. Depending on the timescale prescription used, this fraction translates into a merger rate ranging between \u223c0.1 and \u223c4.0 Gyr\u207b\u00b9 at z\u2004\u223c\u20045, which in turn corresponds to an average number of major mergers per galaxy between 1 and 8 in \u223c12.5 yr (from z\u2004=\u20046 to the local Universe). When convolved with the galaxy number density at different epochs, the merger rate density becomes approximately constant over time at 1\u2004< \u2004z\u2004< 4, including values from 10\u207b\u2074 to 10\u207b\u00b3 Gyr\u22121 Mpc\u207b\u00b3, depending on the assumed T_(MM). We finally compare the specific star formation and star-formation rate density with the analogous quantities from major mergers, finding a good agreement at z\u2004> 4 if we assume a merger timescale that quickly decreases with increasing redshift.\nConclusions. Our new constraints on the merger fraction from the ALPINE survey at z\u2004\u223c\u20045 reveal the presence of a significant merging activity in the early Universe. Whether this population of mergers can provide a relevant contribution to the galaxy mass assembly at these redshifts and through the cosmic epochs is strongly dependent on the assumption of the merger timescale. However, our results show that an evolving T_(MM)\u2004\u221d\u2004(1 + z)\u207b\u00b2 agrees well with state-of-the-art cosmological simulations, suggesting a considerable role of mergers in the build-up of galaxies at early times.",
"doi": "10.1051/0004-6361/202141306",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2021-09",
"volume": "653",
"pages": "Art. No. A111"
},
{
"id": "authors:5755c-pdj45",
"collection": "authors",
"collection_id": "5755c-pdj45",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210916-143425405",
"type": "article",
"title": "The evolution of compact massive quiescent and star-forming galaxies derived from the R_e\u2013R_h and M_(star)\u2013M_h relations",
"author": [
{
"family_name": "Zanisi",
"given_name": "L.",
"clpid": "Zanisi-Lorenzo"
},
{
"family_name": "Shankar",
"given_name": "F.",
"orcid": "0000-0001-8973-5051",
"clpid": "Shankar-Francesco"
},
{
"family_name": "Fu",
"given_name": "H.",
"clpid": "Fu-H"
},
{
"family_name": "Rodriguez-Puebla",
"given_name": "A.",
"orcid": "0000-0002-0170-5358",
"clpid": "Rodriguez-Puebla-Aldo"
},
{
"family_name": "Avila-Reese",
"given_name": "V.",
"orcid": "0000-0002-3461-2342",
"clpid": "Avila-Reese-Vladimir"
},
{
"family_name": "Faisst",
"given_name": "A.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Daddi",
"given_name": "E.",
"orcid": "0000-0002-3331-9590",
"clpid": "Daddi-Emanuele"
},
{
"family_name": "Boco",
"given_name": "L.",
"clpid": "Boco-L"
},
{
"family_name": "Lapi",
"given_name": "A,",
"clpid": "Lapi-A"
},
{
"family_name": "Giavalisco",
"given_name": "M.",
"orcid": "0000-0002-7831-8751",
"clpid": "Giavalisco-Mauro"
},
{
"family_name": "Saracco",
"given_name": "P.",
"orcid": "0000-0003-3959-2595",
"clpid": "Saracco-Paolo"
},
{
"family_name": "Buitrago",
"given_name": "F.",
"orcid": "0000-0002-2861-9812",
"clpid": "Buitrago-Fernando"
},
{
"family_name": "Huertas-Company",
"given_name": "M.",
"orcid": "0000-0002-1416-8483",
"clpid": "Huertas-Company-Marc"
},
{
"family_name": "Puglisi",
"given_name": "A.",
"orcid": "0000-0001-9369-1805",
"clpid": "Puglisi-Annagrazia"
},
{
"family_name": "Dekel",
"given_name": "A.",
"orcid": "0000-0003-4174-0374",
"clpid": "Dekel-Avishai"
}
],
"abstract": "The mean size (effective radius R_e) of massive galaxies (MGs; M_(star) > 10^(11.2)M_\u2299) is observed to increase steadily with cosmic time. It is still unclear whether this trend originates from the size growth of individual galaxies (via, e.g. mergers and/or AGN feedback) or from the inclusion of larger galaxies entering the selection at later epochs (progenitor bias). We here build a data-driven, flexible theoretical framework to probe the structural evolution of MGs. We assign galaxies to dark matter haloes via stellar mass\u2013halo mass (SMHM) relations with varying high-mass slopes and scatters \u03c3_(SMHM) in stellar mass at fixed halo mass, and assign sizes to galaxies using an empirically motivated, constant and linear relationship between Re and the host dark matter halo radius Rh. We find that (1) the fast mean size growth of MGs is well reproduced independently of the shape of the input SMHM relation; (2) the numbers of compact MGs grow steadily until z \u2273 2 and fall off at lower redshifts, suggesting a lesser role of progenitor bias at later epochs; (3) a time-independent scatter \u03c3_(SMHM) is consistent with a scenario in which compact star-forming MGs transition into quiescent MGs in a few 10\u2078 yr with a negligible structural evolution during the compact phase, while a scatter increasing at high redshift implies significant size growth during the star-forming phase. A robust measurement of the size function of MGs at high redshift can set strong constraints on the scatter of the SMHM relation and, by extension, on models of galaxy evolution.",
"doi": "10.1093/mnras/stab1472",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2021-08",
"series_number": "3",
"volume": "505",
"issue": "3",
"pages": "4555-4570"
},
{
"id": "authors:qzchs-r4x74",
"collection": "authors",
"collection_id": "qzchs-r4x74",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210608-092348926",
"type": "article",
"title": "The ALPINE-ALMA [CII] survey. Obscured star formation rate density and main sequence of star-forming galaxies at z\u2004>\u20044",
"author": [
{
"family_name": "Khusanova",
"given_name": "Y.",
"orcid": "0000-0002-7220-397X",
"clpid": "Khusanova-Yana"
},
{
"family_name": "Bethermin",
"given_name": "M.",
"orcid": "0000-0002-3915-2015"
},
{
"family_name": "Le F\u00e8vre",
"given_name": "O.",
"orcid": "0000-0001-5891-2596"
},
{
"family_name": "Capak",
"given_name": "P.",
"orcid": "0000-0003-3578-6843",
"clpid": "Capak-Peter"
},
{
"family_name": "Faisst",
"given_name": "A. L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Schaerer",
"given_name": "D.",
"orcid": "0000-0001-7144-7182"
},
{
"family_name": "Silverman",
"given_name": "J. D.",
"orcid": "0000-0002-0000-6977"
},
{
"family_name": "Cassata",
"given_name": "P.",
"orcid": "0000-0002-6716-4400"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Ginolfi",
"given_name": "M.",
"orcid": "0000-0002-8231-821X"
},
{
"family_name": "Fudamoto",
"given_name": "Y.",
"orcid": "0000-0001-7440-8832"
},
{
"family_name": "Loiacono",
"given_name": "F.",
"orcid": "0000-0002-8858-6784"
},
{
"family_name": "Amorin",
"given_name": "R.",
"orcid": "0000-0001-5758-1000"
},
{
"family_name": "Bardelli",
"given_name": "S.",
"orcid": "0000-0002-8900-0298"
},
{
"family_name": "Boquien",
"given_name": "M.",
"orcid": "0000-0003-0946-6176"
},
{
"family_name": "Cimatti",
"given_name": "A.",
"orcid": "0000-0002-4409-5633"
},
{
"family_name": "Dessauges-Zavadsky",
"given_name": "M.",
"orcid": "0000-0003-0348-2917"
},
{
"family_name": "Gruppioni",
"given_name": "C.",
"orcid": "0000-0002-5836-4056"
},
{
"family_name": "Hathi",
"given_name": "N. P.",
"orcid": "0000-0001-6145-5090"
},
{
"family_name": "Jones",
"given_name": "G. C.",
"orcid": "0000-0002-0267-9024"
},
{
"family_name": "Koekemoer",
"given_name": "A. M.",
"orcid": "0000-0002-6610-2048"
},
{
"family_name": "Lagache",
"given_name": "G.",
"orcid": "0000-0003-1492-2519"
},
{
"family_name": "Maiolino",
"given_name": "R.",
"orcid": "0000-0002-4985-3819"
},
{
"family_name": "Lemaux",
"given_name": "B. C.",
"orcid": "0000-0002-1428-7036"
},
{
"family_name": "Oesch",
"given_name": "P.",
"orcid": "0000-0001-5851-6649"
},
{
"family_name": "Pozzi",
"given_name": "F.",
"orcid": "0000-0002-7412-647X"
},
{
"family_name": "Riechers",
"given_name": "D. A.",
"orcid": "0000-0001-9585-1462"
},
{
"family_name": "Romano",
"given_name": "M.",
"orcid": "0000-0002-9948-3916"
},
{
"family_name": "Talia",
"given_name": "M.",
"orcid": "0000-0003-4352-2063"
},
{
"family_name": "Toft",
"given_name": "S.",
"orcid": "0000-0003-3631-7176"
},
{
"family_name": "Vergani",
"given_name": "D.",
"orcid": "0000-0003-0898-2216"
},
{
"family_name": "Zamorani",
"given_name": "G.",
"orcid": "0000-0002-2318-301X"
},
{
"family_name": "Zucca",
"given_name": "E.",
"orcid": "0000-0002-5845-8132"
}
],
"abstract": "Star formation rate (SFR) measurements at z\u2004>\u20044 have relied mostly on the rest-frame far-ultraviolet (FUV) observations. The corrections for dust attenuation based on the IRX-\u03b2 relation are highly uncertain and are still debated in the literature. Hence, rest-frame far-infrared (FIR) observations are necessary to constrain the dust-obscured component of the SFR. In this paper, we exploit the rest-frame FIR continuum observations collected by the ALMA Large Program to INvestigate [CII] at Early times (ALPINE) to directly constrain the obscured SFR in galaxies at 4.4\u2004<\u2004z\u2004<\u20045.9. We used stacks of continuum images to measure average infrared luminosities taking both detected and undetected sources into account. Based on these measurements, we measured the position of the main sequence of star-forming galaxies and the specific SFR (sSFR) at z\u2004\u223c\u20044.5 and z\u2004\u223c\u20045.5. We find that the main sequence and sSFR do not significantly evolve between z\u2004\u223c\u20044.5 and z\u2004\u223c\u20045.5, as opposed to lower redshifts. We developed a method to derive the obscured SFR density (SFRD) using the stellar masses or FUV-magnitudes as a proxy of FIR fluxes measured on the stacks and combining them with the galaxy stellar mass functions and FUV luminosity functions from the literature. We obtain consistent results independent of the chosen proxy. We find that the obscured fraction of SFRD is decreasing with increasing redshift, but even at z\u2004\u223c\u20045.5 it constitutes around 61% of the total SFRD.",
"doi": "10.1051/0004-6361/202038944",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2021-05",
"volume": "649",
"pages": "Art. No. A152"
},
{
"id": "authors:bg9ss-5ps35",
"collection": "authors",
"collection_id": "bg9ss-5ps35",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210303-074449231",
"type": "article",
"title": "Illuminating the Dark Side of Cosmic Star Formation Two Billion Years after the Big Bang",
"author": [
{
"family_name": "Talia",
"given_name": "Margherita",
"orcid": "0000-0003-4352-2063",
"clpid": "Talia-Margherita"
},
{
"family_name": "Cimatti",
"given_name": "Andrea",
"orcid": "0000-0002-4409-5633",
"clpid": "Cimatti-Andrea"
},
{
"family_name": "Giulietti",
"given_name": "Marika",
"orcid": "0000-0002-1847-4496",
"clpid": "Giulietti-Marika"
},
{
"family_name": "Zamorani",
"given_name": "Gianni",
"orcid": "0000-0002-2318-301X",
"clpid": "Zamorani-Gianni"
},
{
"family_name": "B\u00e9thermin",
"given_name": "Matthieu",
"orcid": "0000-0002-3915-2015",
"clpid": "B\u00e9thermin-Matthieu"
},
{
"family_name": "Faisst",
"given_name": "Andreas",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Le F\u00e8vre",
"given_name": "Olivier",
"orcid": "0000-0001-5891-2596",
"clpid": "Le-F\u00e8vre-Olivier"
},
{
"family_name": "Smol\u010di\u0107",
"given_name": "Vernesa",
"orcid": "0000-0002-3893-8614",
"clpid": "Smol\u010di\u0107-Vernesa"
}
],
"abstract": "How and when did galaxies form and assemble their stars and stellar mass? The answer to these questions, so crucial to astrophysics and cosmology, requires the full reconstruction of the so-called cosmic star formation rate density (SFRD), i.e., the evolution of the average star formation rate per unit volume of the universe. While the SFRD has been reliably traced back to 10\u201311 billion years ago, its evolution is still poorly constrained at earlier cosmic epochs, and its estimate is mainly based on galaxies luminous in the ultraviolet and with low obscuration by dust. This limited knowledge is largely due to the lack of an unbiased census of all types of star-forming galaxies in the early universe. We present a new approach to finding dust-obscured star-forming galaxies based on their emission at radio wavelengths coupled with the lack of optical counterparts. Here, we present a sample of 197 galaxies selected with this method. These systems were missed by previous surveys at optical and near-infrared wavelengths, and 22 of them are at very high redshift (i.e., z > 4.5). The contribution of these elusive systems to the SFRD is substantial and can be as high as 40% of the previously known SFRD based on UV-luminous galaxies. The mere existence of such heavily obscured galaxies in the first two billion years after the Big Bang opens new avenues to investigate the early phases of galaxy formation and evolution, and to understand the links between these systems and the massive galaxies that ceased their star formation at later cosmic times.",
"doi": "10.3847/1538-4357/abd6e3",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2021-03-01",
"series_number": "1",
"volume": "909",
"issue": "1",
"pages": "Art. No. 23"
},
{
"id": "authors:85d28-5rm77",
"collection": "authors",
"collection_id": "85d28-5rm77",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210222-100902465",
"type": "article",
"title": "The Fundamental Plane of Massive Quiescent Galaxies at z \u223c 2",
"author": [
{
"family_name": "Stockmann",
"given_name": "Mikkel",
"orcid": "0000-0001-5983-6273",
"clpid": "Stockmann-Mikkel"
},
{
"family_name": "J\u00f8rgensen",
"given_name": "Inger",
"orcid": "0000-0003-3002-1446",
"clpid": "J\u00f8rgensen-Inger"
},
{
"family_name": "Toft",
"given_name": "Sune",
"orcid": "0000-0003-3631-7176",
"clpid": "Toft-Sune"
},
{
"family_name": "Conselice",
"given_name": "Christopher J.",
"orcid": "0000-0003-1949-7638",
"clpid": "Conselice-Christopher-J"
},
{
"family_name": "Faisst",
"given_name": "Andreas",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Margalef-Bentabol",
"given_name": "Berta",
"orcid": "0000-0001-8702-7019",
"clpid": "Margalef-Bentabol-Berta"
},
{
"family_name": "Gallazzi",
"given_name": "Anna",
"orcid": "0000-0002-9656-1800",
"clpid": "Gallazzi-Anna"
},
{
"family_name": "Zibetti",
"given_name": "Stefano",
"orcid": "0000-0003-1734-8356",
"clpid": "Zibetti-Stefano"
},
{
"family_name": "Brammer",
"given_name": "Gabriel B.",
"orcid": "0000-0003-2680-005X",
"clpid": "Brammer-Gabriel-B"
},
{
"family_name": "G\u00f3mez-Guijarro",
"given_name": "Carlos",
"orcid": "0000-0002-4085-9165",
"clpid": "G\u00f3mez-Guijarro-Carlos"
},
{
"family_name": "Hirschmann",
"given_name": "Michaela",
"orcid": "0000-0002-3301-3321",
"clpid": "Hirschmann-Michaela"
},
{
"family_name": "Lagos",
"given_name": "Claudia D.",
"orcid": "0000-0003-3021-8564",
"clpid": "Lagos-Claudia-D"
},
{
"family_name": "Valentino",
"given_name": "Francesco M.",
"orcid": "0000-0001-6477-4011",
"clpid": "Valentino-Francesco-M"
},
{
"family_name": "Zabl",
"given_name": "Johannes",
"orcid": "0000-0002-9842-6354",
"clpid": "Zabl-Johannes"
}
],
"abstract": "We examine the Fundamental Plane (FP) and mass-to-light ratio (M/L) scaling relations using the largest sample of massive quiescent galaxies at 1.5 < z < 2.5 to date. The FP (r_e, \u03c3_e, I_e) is established using 19 UVJ quiescent galaxies from COSMOS with Hubble Space Telescope H F160W rest-frame optical sizes and X-shooter absorption line-measured stellar velocity dispersions. For a very massive, log(M_*/M_\u2299), subset of eight quiescent galaxies at z > 2, from Stockmann et al., we show that they cannot passively evolve to the local Coma cluster relation alone and must undergo significant structural evolution to mimic the sizes of local massive galaxies. The evolution of the FP and M/L scaling relations, from z = 2 to present day, for this subset are consistent with passive aging of the stellar population and minor merger structural evolution into the most massive galaxies in the Coma cluster and other massive elliptical galaxies from the MASSIVE Survey. Modeling the luminosity evolution from minor merger-added stellar populations favors a history of merging with \"dry\" quiescent galaxies.",
"doi": "10.3847/1538-4357/abce66",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2021-02-20",
"series_number": "2",
"volume": "908",
"issue": "2",
"pages": "Art. No. 135"
},
{
"id": "authors:vgsgx-d6576",
"collection": "authors",
"collection_id": "vgsgx-d6576",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210210-124713447",
"type": "article",
"title": "The ALPINE\u2013ALMA [C II] survey. Luminosity function of serendipitous [C II] line emitters at z \u223c 5",
"author": [
{
"family_name": "Loiacono",
"given_name": "Federica",
"orcid": "0000-0002-8858-6784",
"clpid": "Loiacono-Federica"
},
{
"family_name": "Decarli",
"given_name": "Roberto",
"orcid": "0000-0002-2662-8803"
},
{
"family_name": "Gruppioni",
"given_name": "Carlotta"
},
{
"family_name": "Talia",
"given_name": "Margherita",
"orcid": "0000-0003-4352-2063"
},
{
"family_name": "Cimatti",
"given_name": "Andrea",
"orcid": "0000-0002-4409-5633"
},
{
"family_name": "Zamorani",
"given_name": "Gianni",
"orcid": "0000-0002-2318-301X"
},
{
"family_name": "Pozzi",
"given_name": "Francesca",
"orcid": "0000-0002-7412-647X"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Lemaux",
"given_name": "Brian C.",
"orcid": "0000-0002-1428-7036"
},
{
"family_name": "Riechers",
"given_name": "Dominik A.",
"orcid": "0000-0001-9585-1462"
},
{
"family_name": "Le F\u00e8vre",
"given_name": "Olivier",
"orcid": "0000-0001-5891-2596"
},
{
"family_name": "B\u00e9thermin",
"given_name": "Matthieu",
"orcid": "0000-0002-3915-2015"
},
{
"family_name": "Capak",
"given_name": "Peter",
"orcid": "0000-0003-3578-6843",
"clpid": "Capak-Peter"
},
{
"family_name": "Cassata",
"given_name": "Paolo",
"orcid": "0000-0002-6716-4400"
},
{
"family_name": "Faisst",
"given_name": "Andreas",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Schaerer",
"given_name": "Daniel",
"orcid": "0000-0001-7144-7182"
},
{
"family_name": "Silverman",
"given_name": "John D.",
"orcid": "0000-0002-0000-6977"
},
{
"family_name": "Bardelli",
"given_name": "Sandro",
"orcid": "0000-0002-8900-0298"
},
{
"family_name": "Boquien",
"given_name": "M\u00e9d\u00e9ric",
"orcid": "0000-0003-0946-6176"
},
{
"family_name": "Burkutean",
"given_name": "Sandra"
},
{
"family_name": "Dessauges-Zavadsky",
"given_name": "Miroslava",
"orcid": "0000-0003-0348-2917"
},
{
"family_name": "Fudamoto",
"given_name": "Yoshinobu",
"orcid": "0000-0001-7440-8832"
},
{
"family_name": "Fujimoto",
"given_name": "Seiji",
"orcid": "0000-0001-7201-5066"
},
{
"family_name": "Ginolfi",
"given_name": "Michele",
"orcid": "0000-0002-9122-1700"
},
{
"family_name": "Hathi",
"given_name": "Nimish P.",
"orcid": "0000-0001-6145-5090"
},
{
"family_name": "Jones",
"given_name": "Gareth C.",
"orcid": "0000-0002-0267-9024"
},
{
"family_name": "Khusanova",
"given_name": "Yana"
},
{
"family_name": "Koekemoer",
"given_name": "Anton M.",
"orcid": "0000-0002-6610-2048"
},
{
"family_name": "Lagache",
"given_name": "Guilaine",
"orcid": "0000-0003-1492-2519"
},
{
"family_name": "Lubin",
"given_name": "Lori M.",
"orcid": "0000-0003-4249-5315"
},
{
"family_name": "Massardi",
"given_name": "Marcella"
},
{
"family_name": "Oesch",
"given_name": "Pascal",
"orcid": "0000-0001-5851-6649"
},
{
"family_name": "Romano",
"given_name": "Michael",
"orcid": "0000-0002-9948-3916"
},
{
"family_name": "Vallini",
"given_name": "Livia",
"orcid": "0000-0002-3258-3672"
},
{
"family_name": "Vergani",
"given_name": "Daniela",
"orcid": "0000-0003-0898-2216"
},
{
"family_name": "Zucca",
"given_name": "Elena",
"orcid": "0000-0002-5845-8132"
}
],
"abstract": "We present the first [C II] 158 \u03bcm luminosity function (LF) at z\u2004\u223c\u20045 from a sample of serendipitous lines detected in the ALMA Large Program to INvestigate [C II] at Early times (ALPINE). A study of the 118 ALPINE pointings revealed several serendipitous lines. Based on their fidelity, we selected 14 lines for the final catalog. According to the redshift of their counterparts, we identified eight out of 14 detections as [C II] lines at z\u2004\u223c\u20045, along with two as CO transitions at lower redshifts. The remaining four lines have an elusive identification in the available catalogs and we considered them as [C II] candidates. We used the eight confirmed [C II] and the four [C II] candidates to build one of the first [C II] LFs at z\u2004\u223c\u20045. We found that 11 out of these 12 sources have a redshift very similar to that of the ALPINE target in the same pointing, suggesting the presence of overdensities around the targets. Therefore, we split the sample in two (a \"clustered\" and \"field\" subsample) according to their redshift separation and built two separate LFs. Our estimates suggest that there could be an evolution of the [C II] LF between z\u2004\u223c\u20045 and z\u2004\u223c\u20040. By converting the [C II] luminosity to the star-formation rate, we evaluated the cosmic star-formation rate density (SFRD) at z\u2004\u223c\u20045. The clustered sample results in a SFRD \u223c10 times higher than previous measurements from UV\u2013selected galaxies. On the other hand, from the field sample (likely representing the average galaxy population), we derived a SFRD \u223c1.6 higher compared to current estimates from UV surveys but compatible within the errors. Because of the large uncertainties, observations of larger samples will be necessary to better constrain the SFRD at z\u2004\u223c\u20045. This study represents one of the first efforts aimed at characterizing the demography of [C II] emitters at z\u2004\u223c\u20045 using a mm selection of galaxies.",
"doi": "10.1051/0004-6361/202038607",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2021-02",
"volume": "646",
"pages": "Art. No. A76"
},
{
"id": "authors:1s15m-8zd64",
"collection": "authors",
"collection_id": "1s15m-8zd64",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200824-123559194",
"type": "article",
"title": "The ALPINE-ALMA [C II] Survey: [C II] 158 \u03bcm Emission Line Luminosity Functions at z ~ 4\u20136",
"author": [
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Sajina",
"given_name": "A.",
"orcid": "0000-0002-1917-1200"
},
{
"family_name": "Loiacono",
"given_name": "F.",
"orcid": "0000-0002-8858-6784"
},
{
"family_name": "Lagache",
"given_name": "G.",
"orcid": "0000-0003-1492-2519"
},
{
"family_name": "B\u00e9thermin",
"given_name": "M.",
"orcid": "0000-0002-3915-2015"
},
{
"family_name": "Faisst",
"given_name": "A.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Ginolfi",
"given_name": "M.",
"orcid": "0000-0002-8231-821X"
},
{
"family_name": "Le F\u00e8vre",
"given_name": "O.",
"orcid": "0000-0001-5891-2596",
"clpid": "Le-F\u00e8vre-Olivier"
},
{
"family_name": "Gruppioni",
"given_name": "C.",
"orcid": "0000-0002-5836-4056"
},
{
"family_name": "Capak",
"given_name": "P. L.",
"orcid": "0000-0003-3578-6843",
"clpid": "Capak-Peter"
},
{
"family_name": "Cassata",
"given_name": "P.",
"orcid": "0000-0002-6716-4400"
},
{
"family_name": "Schaerer",
"given_name": "D.",
"orcid": "0000-0001-7144-7182"
},
{
"family_name": "Silverman",
"given_name": "J. D.",
"orcid": "0000-0002-0000-6977"
},
{
"family_name": "Bardelli",
"given_name": "S.",
"orcid": "0000-0002-8900-0298"
},
{
"family_name": "Dessauges-Zavadsky",
"given_name": "M.",
"orcid": "0000-0003-0348-2917"
},
{
"family_name": "Cimatti",
"given_name": "A.",
"orcid": "0000-0002-4409-5633"
},
{
"family_name": "Hathi",
"given_name": "N. P.",
"orcid": "0000-0001-6145-5090"
},
{
"family_name": "Lemaux",
"given_name": "B. C.",
"orcid": "0000-0002-1428-7036"
},
{
"family_name": "Ibar",
"given_name": "E."
},
{
"family_name": "Jones",
"given_name": "G. C.",
"orcid": "0000-0002-0267-9024"
},
{
"family_name": "Koekemoer",
"given_name": "A. M.",
"orcid": "0000-0002-6610-2048"
},
{
"family_name": "Oesch",
"given_name": "P. A.",
"orcid": "0000-0001-5851-6649"
},
{
"family_name": "Talia",
"given_name": "M.",
"orcid": "0000-0003-4352-2063"
},
{
"family_name": "Pozzi",
"given_name": "F.",
"orcid": "0000-0002-7412-647X"
},
{
"family_name": "Riechers",
"given_name": "D. A.",
"orcid": "0000-0001-9585-1462"
},
{
"family_name": "Tasca",
"given_name": "L. A."
},
{
"family_name": "Toft",
"given_name": "S.",
"orcid": "0000-0003-3631-7176"
},
{
"family_name": "Vallini",
"given_name": "L.",
"orcid": "0000-0002-3258-3672"
},
{
"family_name": "Vergani",
"given_name": "D.",
"orcid": "0000-0003-0898-2216"
},
{
"family_name": "Zamorani",
"given_name": "G.",
"orcid": "0000-0002-2318-301X"
},
{
"family_name": "Zucca",
"given_name": "E.",
"orcid": "0000-0002-5845-8132"
}
],
"abstract": "We present the [C II] 158 \u03bcm line luminosity functions (LFs) at z ~ 4\u20136 using the ALMA observations of 118 sources, which are selected to have UV luminosity M_(1500\u00c5) < \u221220.2 and optical spectroscopic redshifts in COSMOS and ECDF-S. Of the 118 targets, 75 have significant [C II] detections and 43 are upper limits. This is by far the largest sample of [C II] detections, which allows us to set constraints on the volume density of [C II] emitters at z ~ 4\u20136. But because this is a UV-selected sample, we are missing [C II]-bright but UV-faint sources, making our constraints strict lower limits. Our derived LFs are statistically consistent with the z ~ 0 [C II] LF at 10^(8.25)\u201310^(9.75) L_\u2299. We compare our results with the upper limits of the [C II] LF derived from serendipitous sources in the ALPINE maps. We also infer the [C II] LFs based on published far-IR and CO LFs at z ~ 4\u20136. Combining our robust lower limits with these additional estimates, we set further constraints on the true number density of [C II] emitters at z ~ 4\u20136. These additional LF estimates are largely above our LF at L_([CII]) > 10\u2079 L_\u2299, suggesting that UV-faint but [C II]-bright sources likely make significant contributions to the [C II] emitter volume density. When we include all the LF estimates, we find that available model predictions underestimate the number densities of [C II] emitters at z ~ 4\u20136. Finally, we set a constraint on the molecular gas mass density at z ~ 4\u20136, with \u03c1_(mol) ~ (2\u20137) \u00d7 10\u2077 M_\u2299 Mpc\u207b\u00b3. This is broadly consistent with previous studies.",
"doi": "10.3847/1538-4357/abc41c",
"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. 147"
},
{
"id": "authors:bca2p-7dp74",
"collection": "authors",
"collection_id": "bca2p-7dp74",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200720-071439633",
"type": "article",
"title": "ALMA characterizes the dust temperature of z \u223c 5.5 star-forming galaxies",
"author": [
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Fudamoto",
"given_name": "Yoshinobu",
"orcid": "0000-0001-7440-8832",
"clpid": "Fudamoto-Yoshinobu"
},
{
"family_name": "Oesch",
"given_name": "Pascal A.",
"orcid": "0000-0001-5851-6649",
"clpid": "Oesch-Pascal-A"
},
{
"family_name": "Scoville",
"given_name": "Nick",
"orcid": "0000-0002-0438-3323",
"clpid": "Scoville-N-Z"
},
{
"family_name": "Riechers",
"given_name": "Dominik A.",
"orcid": "0000-0001-9585-1462",
"clpid": "Riechers-Domink-A"
},
{
"family_name": "Pavesi",
"given_name": "Riccardo",
"orcid": "0000-0002-2263-646X",
"clpid": "Pavesi-Riccardo"
},
{
"family_name": "Capak",
"given_name": "Peter",
"orcid": "0000-0003-3578-6843",
"clpid": "Capak-Peter"
}
],
"abstract": "The infrared (IR) spectral energy distributions (SEDs) of main-sequence galaxies in the early Universe (z > 4) is currently unconstrained as IR continuum observations are time-consuming and not feasible for large samples. We present Atacama Large Millimetre Array Band 8 observations of four main-sequence galaxies at z \u223c 5.5 to study their IR SED shape in detail. Our continuum data (rest-frame 110\u2009\u03bcm\u2060, close to the peak of IR emission) allows us to constrain luminosity-weighted dust temperatures and total IR luminosities. With data at longer wavelengths, we measure for the first time the emissivity index at these redshifts to provide more robust estimates of molecular gas masses based on dust continuum. The Band 8 observations of three out of four galaxies can only be reconciled with optically thin emission redward of rest-frame 100\u03bcm\u2060. The derived dust peak temperatures at z \u223c 5.5 (\u206030\u221243K\u2060) are elevated compared to average local galaxies, however, \u223c10K below what would be predicted from an extrapolation of the trend at z < 4. This behaviour can be explained by decreasing dust abundance (or density) towards high redshifts, which would cause the IR SED at the peak to be more optically thin, making hot dust more visible to the external observer. From the 850-\u03bcm dust continuum, we derive molecular gas masses between 10\u00b9\u2070 and 10\u00b9\u00b9M\u2299 and gas fractions (gas over total mass) of 30\u221280 per cent (gas depletion times of 100\u2212220 Myr\u2060). All in all, our results provide a first measured benchmark SED to interpret future millimetre observations of normal, main-sequence galaxies in the early Universe.",
"doi": "10.1093/mnras/staa2545",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2020-11",
"series_number": "3",
"volume": "498",
"issue": "3",
"pages": "4192-4204"
},
{
"id": "authors:nx8hh-cmw64",
"collection": "authors",
"collection_id": "nx8hh-cmw64",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191002-135305171",
"type": "article",
"title": "The ALPINE-ALMA [C\u2009II] survey: a triple merger at z \u223c 4.56",
"author": [
{
"family_name": "Jones",
"given_name": "G. C.",
"orcid": "0000-0002-0267-9024",
"clpid": "Jones-Gareth-C"
},
{
"family_name": "B\u00e9thermin",
"given_name": "M.",
"orcid": "0000-0002-3915-2015"
},
{
"family_name": "Fudamoto",
"given_name": "Y.",
"orcid": "0000-0001-7440-8832"
},
{
"family_name": "Ginolfi",
"given_name": "M.",
"orcid": "0000-0002-8231-821X"
},
{
"family_name": "Capak",
"given_name": "P.",
"orcid": "0000-0003-3578-6843",
"clpid": "Capak-Peter"
},
{
"family_name": "Cassata",
"given_name": "P.",
"orcid": "0000-0002-6716-4400"
},
{
"family_name": "Faisst",
"given_name": "A.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Le Fevre",
"given_name": "O.",
"orcid": "0000-0001-5891-2596"
},
{
"family_name": "Schaerer",
"given_name": "D.",
"orcid": "0000-0001-7144-7182"
},
{
"family_name": "Silverman",
"given_name": "J.",
"orcid": "0000-0002-0000-6977"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Bardelli",
"given_name": "S.",
"orcid": "0000-0002-8900-0298"
},
{
"family_name": "Boquien",
"given_name": "M.",
"orcid": "0000-0003-0946-6176"
},
{
"family_name": "Cimatti",
"given_name": "A.",
"orcid": "0000-0002-4409-5633"
},
{
"family_name": "Dessauges-Zavadsky",
"given_name": "M.",
"orcid": "0000-0003-0348-2917"
},
{
"family_name": "Giavalisco",
"given_name": "M.",
"orcid": "0000-0002-7831-8751"
},
{
"family_name": "Gruppioni",
"given_name": "C.",
"orcid": "0000-0002-5836-4056"
},
{
"family_name": "Ibar",
"given_name": "E."
},
{
"family_name": "Khusanova",
"given_name": "Y.",
"orcid": "0000-0002-7220-397X"
},
{
"family_name": "Koekemoer",
"given_name": "A. M.",
"orcid": "0000-0002-6610-2048"
},
{
"family_name": "Lemaux",
"given_name": "B. C.",
"orcid": "0000-0002-1428-7036"
},
{
"family_name": "Loiacono",
"given_name": "F.",
"orcid": "0000-0002-8858-6784"
},
{
"family_name": "Maiolino",
"given_name": "R.",
"orcid": "0000-0002-4985-3819"
},
{
"family_name": "Oesch",
"given_name": "P. A.",
"orcid": "0000-0001-5851-6649"
},
{
"family_name": "Pozzi",
"given_name": "F.",
"orcid": "0000-0002-7412-647X"
},
{
"family_name": "Riechers",
"given_name": "D.",
"orcid": "0000-0001-9585-1462"
},
{
"family_name": "Rodighiero",
"given_name": "G.",
"orcid": "0000-0002-9415-2296"
},
{
"family_name": "Talia",
"given_name": "M.",
"orcid": "0000-0003-4352-2063"
},
{
"family_name": "Vallini",
"given_name": "L.",
"orcid": "0000-0002-3258-3672"
},
{
"family_name": "Vergani",
"given_name": "D.",
"orcid": "0000-0003-0898-2216"
},
{
"family_name": "Zamorani",
"given_name": "G.",
"orcid": "0000-0002-2318-301X"
},
{
"family_name": "Zucca",
"given_name": "E.",
"orcid": "0000-0002-5845-8132"
}
],
"abstract": "We report the detection of [C\u2009II] \u03bb158 \u03bc\u03bcm emission from a system of three closely separated sources in the Cosmic Evolution Survey (COSMOS) field at z \u223c 4.56 , as part of the Atacama Large Millimeter/submillimeter Array (ALMA) Large Program to INvestigate C\u2009II at Early times (ALPINE). The two most luminous sources are closely associated, both spatially (1.6 arcsec \u223c 11 kpc) and in velocity (\u223c100 km s\u207b\u00b9), while the third source is slightly more distant (2.8 arcsec \u223c 18 kpc, \u223c300 km s\u207b\u00b9). The second most luminous source features a slight velocity gradient, while no significant velocity gradient is seen in the other two sources. Using the observed [C\u2009II] luminosities, we derive a total log_(10)(SFR_([CII])[M\u2299yr\u207b\u00b9])=2.8\u00b10.2\u2060, which may be split into contributions of 59, 31, and 10 per cent from the central, east, and west sources, respectively. Comparison of these [C\u2009II] detections to recent zoom-in cosmological simulations suggests an ongoing major merger. We are thus witnessing a system in a major phase of mass build-up by merging, including an ongoing major merger and an upcoming minor merger, which is expected to end up in a single massive galaxy by z \u223c 2.5.",
"doi": "10.1093/mnrasl/slz154",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2020-01",
"series_number": "1",
"volume": "491",
"issue": "1",
"pages": "L18-L23"
}
]