We introduce a new method for measuring the Hubble parameter from low-redshift large-scale observations that is independent of the comoving sound horizon. The method uses the baryon-to-photon ratio determined by the primordial deuterium abundance, together with big bang nucleosynthesis calculations and the present-day cosmic microwave background (CMB) temperature, to determine the physical baryon density Ω\ud835\udc4f\u2062\u210e². The baryon fraction Ω\ud835\udc4f/Ω\ud835\udc5a is measured using the relative amplitude of the baryonic signature in galaxy clustering measured by the Baryon Oscillation Spectroscopic Survey, scaling the physical baryon density to the physical matter density. The physical density Ω\ud835\udc5a\u2062\u210e² is then compared with the geometrical density Ω\ud835\udc5a from Alcock-Paczynski measurements from baryon acoustic oscillations (BAO) and voids to give \ud835\udc3b0. Including type Ia supernovae and uncalibrated BAO, we measure \ud835\udc3b0=67.1+6.3−5.3 km s\u207b¹ Mpc\u207b¹. We find similar results when varying analysis choices, such as measuring the baryon signature from the reconstructed correlation function or excluding supernovae or voids. This measurement is currently consistent with both the distance-ladder and CMB \ud835\udc3b0 determinations, but near-future large-scale structure surveys will obtain 3 × to 4 × tighter constraints.
", "doi": "10.1103/physrevlett.134.101002", "issn": "0031-9007", "publisher": "American Physical Society", "publication": "Physical Review Letters", "publication_date": "2025-03-12", "series_number": "10", "volume": "134", "issue": "10", "pages": "101002" }, { "id": "authors:0m0v2-sz026", "collection": "authors", "collection_id": "0m0v2-sz026", "cite_using_url": "https://authors.library.caltech.edu/records/0m0v2-sz026", "type": "article", "title": "Measuring the baryon fraction using galaxy clustering", "author": [ { "family_name": "Krolewski", "given_name": "Alex", "orcid": "0000-0003-2183-7021", "clpid": "Krolewski-Alex" }, { "family_name": "Percival", "given_name": "Will J.", "orcid": "0000-0002-0644-5727" } ], "abstract": "The amplitude of the baryon signature in galaxy clustering depends on the cosmological baryon fraction. We consider two ways to isolate this signal in galaxy redshift surveys. First, we extend standard template-based baryon acoustic oscillation (BAO) models to include the amplitude of the baryonic signature by splitting the transfer function into baryon and cold dark matter components with freely varying proportions. Second, we include the amplitude of the split as an extra parameter in effective field theory of large scale structure (EFT) models of the full galaxy clustering signal. We find similar results from both approaches. For the Baryon Oscillation Spectroscopic Survey (BOSS) data we find fb\u2261\u03a9b/(\u03a9b+\u03a9c)=0.173\u00b10.027 for template fits postreconstruction, fb=0.153\u00b10.029 for template fits prereconstruction, and fb=0.154\u00b10.022 for EFT fits, with an estimated systematic error of 0.013 for all three methods. Using reconstruction only produces a marginal improvement for these measurements. Although significantly weaker than constraints on fb from the cosmic microwave background, these measurements rely on very simple physics and, in particular, are independent of the sound horizon. In a companion paper we show how they can be used, together with big bang nucleosynthesis measurements of the physical baryon density and geometrical measurements of the matter density from the Alcock-Paczynski effect, to constrain the Hubble parameter. While the constraints on H0 based on density measurements from BOSS are relatively weak, measurements from DESI and Euclid will lead to errors on H0 that can differentiate the cosmological and distance ladder H0 measurements.", "doi": "10.1103/physrevd.111.063526", "issn": "2470-0010", "publisher": "American Physical Society", "publication": "Physical Review D", "publication_date": "2025-03-12", "series_number": "6", "volume": "111", "issue": "6", "pages": "063526" }, { "id": "authors:kmvq2-nrb40", "collection": "authors", "collection_id": "kmvq2-nrb40", "cite_using_url": "https://authors.library.caltech.edu/records/kmvq2-nrb40", "type": "article", "title": "Impact and mitigation of spectroscopic systematics on DESI DR1 clustering measurements", "author": [ { "family_name": "Krolewski", "given_name": "A.", "orcid": "0000-0003-2183-7021", "clpid": "Krolewski-Alex" }, { "family_name": "Yu", "given_name": "J.", "orcid": "0009-0001-7217-8006" }, { "family_name": "Ross", "given_name": "A.J.", "orcid": "0000-0002-7522-9083" }, { "family_name": "Penmetsa", "given_name": "S." }, { "family_name": "Percival", "given_name": "W.J.", "orcid": "0000-0002-0644-5727" }, { "family_name": "Zhou", "given_name": "R.", "orcid": "0000-0001-5381-4372" }, { "family_name": "Wilson", "given_name": "M.J." }, { "family_name": "Hou", "given_name": "J.", "orcid": "0000-0001-6083-1947" }, { "family_name": "Aguilar", "given_name": "J.", "orcid": "0000-0003-0822-452X" }, { "family_name": "Ahlen", "given_name": "S.", "orcid": "0000-0001-6098-7247" }, { "family_name": "Brooks", "given_name": "D.", "orcid": "0000-0002-8458-5047" }, { "family_name": "Chaussidon", "given_name": "E.", "orcid": "0000-0001-8996-4874" }, { "family_name": "Claybaugh", "given_name": "T.", "orcid": "0000-0002-5024-6987" }, { "family_name": "de la Macorra", "given_name": "A.", "orcid": "0000-0002-1769-1640" }, { "family_name": "Dey", "given_name": "Biprateep", "orcid": "0000-0002-5665-7912" }, { "family_name": "Forero-Romero", "given_name": "J.E.", "orcid": "0000-0002-2890-3725" }, { "family_name": "Gontcho", "given_name": "S.Gontcho A.", "orcid": "0000-0003-3142-233X" }, { "family_name": "Guy", "given_name": "J.", "orcid": "0000-0001-9822-6793" }, { "family_name": "Honscheid", "given_name": "K." }, { "family_name": "Juneau", "given_name": "S.", "orcid": "0000-0002-0000-2394" }, { "family_name": "Kirkby", "given_name": "D.", "orcid": "0000-0002-8828-5463" }, { "family_name": "Kisner", "given_name": "T.", "orcid": "0000-0003-3510-7134" }, { "family_name": "Kremin", "given_name": "A.", "orcid": "0000-0001-6356-7424" }, { "family_name": "Lambert", "given_name": "A.", "orcid": "0009-0003-5658-2601" }, { "family_name": "Le Guillou", "given_name": "L.", "orcid": "0000-0001-7178-8868" }, { "family_name": "Levi", "given_name": "M.E.", "orcid": "0000-0003-1887-1018" }, { "family_name": "Martini", "given_name": "P.", "orcid": "0000-0002-4279-4182" }, { "family_name": "Meisner", "given_name": "A.", "orcid": "0000-0002-1125-7384" }, { "family_name": "Miquel", "given_name": "R.", "orcid": "0000-0002-6610-4836" }, { "family_name": "Moustakas", "given_name": "J.", "orcid": "0000-0002-2733-4559" }, { "family_name": "Myers", "given_name": "A.D." }, { "family_name": "Newman", "given_name": "J.A.", "orcid": "0000-0001-8684-2222" }, { "family_name": "Niz", "given_name": "G.", "orcid": "0000-0002-1544-8946" }, { "family_name": "Palanque-Delabrouille", "given_name": "N.", "orcid": "0000-0003-3188-784X" }, { "family_name": "Rossi", "given_name": "G." }, { "family_name": "Sanchez", "given_name": "E.", "orcid": "0000-0002-9646-8198" }, { "family_name": "Schlafly", "given_name": "E.F.", "orcid": "0000-0002-3569-7421" }, { "family_name": "Schlegel", "given_name": "D.", "orcid": "0000-0002-5042-5088" }, { "family_name": "Schubnell", "given_name": "M." }, { "family_name": "Seo", "given_name": "H.", "orcid": "0000-0002-6588-3508" }, { "family_name": "Sprayberry", "given_name": "D.", "orcid": "0000-0001-7583-6441" }, { "family_name": "Tarl\u00e9", "given_name": "G.", "orcid": "0000-0003-1704-0781" }, { "family_name": "Weaver", "given_name": "B.A." }, { "family_name": "Zhao", "given_name": "C.", "orcid": "0000-0002-1991-7295" } ], "abstract": "The large scale structure catalogs within DESI Data Release 1 (DR1) use nearly 6 million galaxies and quasars as tracers of the large-scale structure of the universe to measure the expansion history with baryon acoustic oscillations and the growth of structure with redshift-space distortions. In order to take advantage of DESI's unprecedented statistical power, we must ensure that the galaxy clustering measurements are unaffected by non-cosmological density fluctuations. One source of spurious fluctuations comes from variation in galaxy density with spectroscopic observing conditions, lowering the redshift efficiency (and thus galaxy density) in certain areas of the sky. We measure the uniformity of the redshift success rate for DESI luminous red galaxies (LRG), bright galaxies (BGS) and quasars (QSO), complementing the detailed discussion of emission line galaxy (ELG) systematics in a companion paper [1]. We find small but significant fluctuations of up to 3% in redshift success rate with the effective spectroscopic signal-to-noise, and create and describe weights that remove these fluctuations. We also describe the process to identify and remove data from certain poorly performing fibers from DESI DR1, and measure the stability of the redshift success rate with time. Finally, we find small but significant correlations of redshift success rate with position on the focal plane, survey speed, and number of exposures required, and show the impact of weights correcting these trends on the power spectrum multipoles and on cosmological parameters from BAO and RSD fits. These corrections change the best-fit parameters by <15% of their statistical errors, and thus contribute negligibly to the overall DESI error budget.
", "doi": "10.1088/1475-7516/2025/01/147", "issn": "1475-7516", "publisher": "IOP Publishing", "publication": "Journal of Cosmology and Astroparticle Physics", "publication_date": "2025-01-01", "series_number": "01", "volume": "2025", "issue": "01", "pages": "147" }, { "id": "authors:jpmnx-b6762", "collection": "authors", "collection_id": "jpmnx-b6762", "cite_using_url": "https://authors.library.caltech.edu/records/jpmnx-b6762", "type": "article", "title": "No evidence for parity violation in BOSS", "author": [ { "family_name": "Krolewski", "given_name": "Alex", "orcid": "0000-0003-2183-7021", "clpid": "Krolewski-Alex" }, { "family_name": "May", "given_name": "Simon", "orcid": "0000-0002-2781-6304" }, { "family_name": "Smith", "given_name": "Kendrick", "orcid": "0000-0002-2088-3125" }, { "family_name": "Hopkins", "given_name": "Hans", "orcid": "0009-0002-1199-8876" } ], "abstract": "Recent studies have found evidence for parity violation in the BOSS spectroscopic galaxy survey, with statistical significance as high as 7σ. These analyses assess the significance of the parity-odd four-point correlation function (4PCF) with a statistic called X2. This statistic is biased if the parity-even eight-point correlation function (8PCF) of the data differs from the mock catalogs. We construct new statistics X2×,X2null that separate the parity violation signal from the 8PCF bias term, allowing them to be jointly constrained. Applying these statistics to BOSS, we find that the parity violation signal ranges from 0 to 2.5σ depending on analysis choices, whereas the 8PCF bias term is ~ 6σ. We conclude that there is no compelling evidence for parity violation in BOSS. Our new statistics can be used to search for parity violation in future surveys, such as DESI, without 8PCF biases.
", "doi": "10.1088/1475-7516/2024/08/044", "issn": "1475-7516", "publisher": "IOP Publishing", "publication": "Journal of Cosmology and Astroparticle Physics", "publication_date": "2024-08-01", "series_number": "08", "volume": "2024", "issue": "08", "pages": "044" }, { "id": "authors:vk8t0-ttr56", "collection": "authors", "collection_id": "vk8t0-ttr56", "cite_using_url": "https://authors.library.caltech.edu/records/vk8t0-ttr56", "type": "article", "title": "Constraining primordial non-Gaussianity from DESI quasar targets and Planck CMB lensing", "author": [ { "family_name": "Krolewski", "given_name": "Alex", "orcid": "0000-0003-2183-7021", "clpid": "Krolewski-Alex" }, { "family_name": "Percival", "given_name": "Will J.", "orcid": "0000-0002-0644-5727" }, { "family_name": "Ferraro", "given_name": "Simone", "orcid": "0000-0003-4992-7854" }, { "family_name": "Chaussidon", "given_name": "Edmond", "orcid": "0000-0001-8996-4874" }, { "family_name": "Rezaie", "given_name": "Mehdi", "orcid": "0000-0001-5589-7116" }, { "family_name": "Aguilar", "given_name": "Jessica Nicole", "orcid": "0000-0003-0822-452X" }, { "family_name": "Ahlen", "given_name": "Steven", "orcid": "0000-0001-6098-7247" }, { "family_name": "Brooks", "given_name": "David", "orcid": "0000-0002-8458-5047" }, { "family_name": "Dawson", "given_name": "Kyle" }, { "family_name": "de la Macorra", "given_name": "Axel", "orcid": "0000-0002-1769-1640" }, { "family_name": "Doel", "given_name": "Peter", "orcid": "0000-0002-6397-4457" }, { "family_name": "Fanning", "given_name": "Kevin", "orcid": "0000-0003-2371-3356" }, { "family_name": "Font-Ribera", "given_name": "Andreu", "orcid": "0000-0002-3033-7312" }, { "family_name": "a Gontcho", "given_name": "Satya Gontcho" }, { "family_name": "Guy", "given_name": "Julien", "orcid": "0000-0001-9822-6793" }, { "family_name": "Honscheid", "given_name": "Klaus", "orcid": "0000-0002-6550-2023" }, { "family_name": "Kehoe", "given_name": "Robert", "orcid": "0000-0002-7101-697X" }, { "family_name": "Kisner", "given_name": "Theodore", "orcid": "0000-0003-3510-7134" }, { "family_name": "Kremin", "given_name": "Anthony", "orcid": "0000-0001-6356-7424" }, { "family_name": "Landriau", "given_name": "Martin", "orcid": "0000-0003-1838-8528" }, { "family_name": "Levi", "given_name": "Michael E.", "orcid": "0000-0003-1887-1018" }, { "family_name": "Martini", "given_name": "Paul", "orcid": "0000-0002-4279-4182" }, { "family_name": "Meisner", "given_name": "Aaron M.", "orcid": "0000-0002-1125-7384" }, { "family_name": "Miquel", "given_name": "Ramon", "orcid": "0000-0002-6610-4836" }, { "family_name": "Nie", "given_name": "Jundan", "orcid": "0000-0001-6590-8122" }, { "family_name": "Poppett", "given_name": "Claire", "orcid": "0000-0003-0512-5489" }, { "family_name": "Ross", "given_name": "Ashley J.", "orcid": "0000-0002-7522-9083" }, { "family_name": "Rossi", "given_name": "Graziano" }, { "family_name": "Schubnell", "given_name": "Michael" }, { "family_name": "Seo", "given_name": "Hee-Jong", "orcid": "0000-0002-6588-3508" }, { "family_name": "Tarl\u00e9", "given_name": "Gregory", "orcid": "0000-0003-1704-0781" }, { "family_name": "Vargas-Maga\u00f1a", "given_name": "Mariana", "orcid": "0000-0003-3841-1836" }, { "family_name": "Weaver", "given_name": "Benjamin Alan" }, { "family_name": "Y\u00e8che", "given_name": "Christophe", "orcid": "0000-0001-5146-8533" }, { "family_name": "Zhou", "given_name": "Rongpu", "orcid": "0000-0001-5381-4372" }, { "family_name": "Zhou", "given_name": "Zhimin", "orcid": "0000-0002-4135-0977" } ], "abstract": "We detect the cross-correlation between 2.7 million DESI quasar targets across 14,700 deg2 (180 quasars deg-2) and Planck 2018 CMB lensing at ∼30σ. We use the cross-correlation on very large scales to constrain local primordial non-Gaussianity via the scale dependence of quasar bias. The DESI quasar targets lie at an effective redshift of 1.51 and are separated into four imaging regions of varying depth and image quality. We select quasar targets from Legacy Survey DR9 imaging, apply additional flux and photometric redshift cuts to improve the purity and reduce the fraction of unclassified redshifts, and use early DESI spectroscopy of 194,000 quasar targets to determine their redshift distribution and stellar contamination fraction (2.6%). Due to significant excess large-scale power in the quasar autocorrelation, we apply weights to mitigate contamination from imaging systematics such as depth, extinction, and stellar density. We use realistic contaminated mocks to determine the greatest number of systematic modes that we can fit, before we are biased by overfitting and spuriously remove real power. We find that linear regression with one to seven imaging templates removed per region accurately recovers the input cross-power, fNL and linear bias. As in previous analyses, our fNL constraint depends on the linear primordial non-Gaussianity bias parameter, b\u03d5= 2( b - p ) δc assuming universality of the halo mass function. We measure fNL= -26+45-40 with p= 1.6 (fNL= -18+29-27 with p= 1.0), and find that this result is robust under several systematics tests. Future spectroscopic quasar cross-correlations with Planck lensing can tighten the fNL constraints by a factor of 2 if they can remove the excess power on large scales in the quasar auto power spectrum.
", "doi": "10.1088/1475-7516/2024/03/021", "issn": "1475-7516", "publisher": "IOP Publishing", "publication": "Journal of Cosmology and Astroparticle Physics", "publication_date": "2024-03-01", "series_number": "03", "volume": "2024", "issue": "03", "pages": "021" }, { "id": "authors:0dgnm-kac94", "collection": "authors", "collection_id": "0dgnm-kac94", "cite_using_url": "https://authors.library.caltech.edu/records/0dgnm-kac94", "type": "article", "title": "The Integrated Sachs Wolfe effect: unWISE and Planck constraints on dynamical dark energy", "author": [ { "family_name": "Krolewski", "given_name": "Alex", "orcid": "0000-0003-2183-7021", "clpid": "Krolewski-Alex" }, { "family_name": "Ferraro", "given_name": "Simone", "orcid": "0000-0003-4992-7854" } ], "abstract": "CMB photons redshift and blueshift as they move through gravitational potentials \u03a6 while propagating across the Universe. If the potential is not constant in time, the photons will pick up a net redshift or blueshift, known as the Integrated Sachs-Wolfe (ISW) effect. In thez\u226a 1000 universe, \u03a6\u0307 is nonzero on large scales when the Universe transitions from matter to dark energy domination. This effect is only detectable in cross-correlation with large-scale structure atz\u223c 1. In this paper we present a 3.2\u03c3detection of the ISW effect using cross-correlations between unWISE infrared galaxies and Planck CMB temperature maps. We use 3 tomographic galaxy samples spanning 0 <z< 2, allowing us to fully probe the dark energy domination era and the transition into matter domination. This measurement is consistent with \u039bCDM (AISW= 0.96 \u00b1 0.30). We study constraints on a particular class of dynamical dark energy models (where the dark energy equation of state is different in matter and dark energy domination), finding that unWISE-ISW improves constraints from type Ia supernovae due to improved constraints on the time evolution of dark energy. When combining with BAO measurements, we obtain the tightest constraints on specific dynamical dark energy models. In the context of a phenomenological model for freezing quintessence, the Mocker model, we constrain the dark energy density within 10% atz< 2 using ISW, BAO and supernovae. Moreover, the ISW measurement itself provides an important independent check when relaxing assumptions about the theory of gravity, as it is sensitive to the gravitational potential rather than the expansion history.
", "doi": "10.1088/1475-7516/2022/04/033", "issn": "1475-7516", "publisher": "IOP Publishing", "publication": "Journal of Cosmology and Astroparticle Physics", "publication_date": "2022-04-01", "series_number": "04", "volume": "2022", "issue": "04", "pages": "033" }, { "id": "authors:a6g60-h6372", "collection": "authors", "collection_id": "a6g60-h6372", "cite_using_url": "https://authors.library.caltech.edu/records/a6g60-h6372", "type": "article", "title": "Cosmological constraints from unWISE and Planck CMB lensing tomography", "author": [ { "family_name": "Krolewski", "given_name": "Alex", "orcid": "0000-0003-2183-7021", "clpid": "Krolewski-Alex" }, { "family_name": "Ferraro", "given_name": "Simone", "orcid": "0000-0003-4992-7854" }, { "family_name": "White", "given_name": "Martin", "orcid": "0000-0001-9912-5070" } ], "abstract": "A number of recent, low-redshift, lensing measurements hint at a universe in which the amplitude of lensing is lower than that predicted from the \u039bCDM model fit to the data of the Planck CMB mission. Here we use the auto- and cross-correlation signal of unWISE galaxies and Planck CMB lensing maps to infer cosmological parameters at low redshift. In particular, we consider three unWISE samples (denoted as \"blue\", \"green\" and \"red\") at median redshifts z \u223c 0.6, 1.1 and 1.5, which fully cover the Dark Energy dominated era. Our cross-correlation measurements, with combined significance S/N \u223c 80, are used to infer the amplitude of low-redshift fluctuations, \u03c38; the fraction of matter in the Universe, \u03a9m; and the combination S8 \u2261 \u03c38(\u03a9m/0.3)0.5 to which these low-redshift lensing measurements are most sensitive. The combination of blue, green and red samples gives a value Sm = 0.784 \u00b1 0.015, that is fully consistent with other low-redshift lensing measurements and in 2.4\u03c3 tension with the CMB predictions from Planck. This is noteworthy, because CMB lensing probes the same physics as previous galaxy lensing measurements, but with very different systematics, thus providing an excellent complement to previous measurements.
", "doi": "10.1088/1475-7516/2021/12/028", "issn": "1475-7516", "publisher": "IOP Publishing", "publication": "Journal of Cosmology and Astroparticle Physics", "publication_date": "2021-12-01", "series_number": "12", "volume": "2021", "issue": "12", "pages": "028" }, { "id": "authors:sded3-pkd41", "collection": "authors", "collection_id": "sded3-pkd41", "cite_using_url": "https://authors.library.caltech.edu/records/sded3-pkd41", "type": "article", "title": "Accelerating computation of the density-field filtering scale \u03c3(R) and non-linear mass by an order of magnitude", "author": [ { "family_name": "Krolewski", "given_name": "Alex", "orcid": "0000-0003-2183-7021", "clpid": "Krolewski-Alex" }, { "family_name": "Slepian", "given_name": "Zachary", "orcid": "0000-0002-1208-119X" } ], "abstract": "The non-linear mass is a characteristic scale in halo formation that has many applications across cosmology. Naively, computing it requires repeated numerical integration to calculate the variance of the power spectrum on different scales and determine which scales exceed the threshold for non-linear collapse. We accelerate calculation of both the non-linear mass and the rms amplitude of the power spectrum σ(R) by working in configuration space and approximating the correlation function as a polynomial at r ≤ 5 h\u207b¹ Mpc. This enables an analytic rather than numerical solution for the non-linear mass, accurate across a variety of cosmologies to 0.1–$1{{\\ \\rm per\\ cent}}$ in mass (depending on redshift) and 20–60× faster than the standard numerical method. We also present a further acceleration of the non-linear mass (400–1000× faster than the standard method) in which we determine the polynomial coefficients using a Taylor expansion in the cosmological parameters rather than re-fitting a polynomial to the correlation function. Our method is also 500× faster than the standard method for σ(R) for a typical case of NR = 100 desired R values, with timing essentially independent of NR. Our approach can be used for quick calculation of the halo mass function, halo mass–bias relation, and cosmological calculations involving the non-linear mass.
", "doi": "10.1093/mnras/staa3525", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2020-11-18", "series_number": "4", "volume": "500", "issue": "4", "pages": "4439-4447" }, { "id": "authors:cpwez-y9487", "collection": "authors", "collection_id": "cpwez-y9487", "cite_using_url": "https://authors.library.caltech.edu/records/cpwez-y9487", "type": "article", "title": "unWISE tomography of Planck CMB lensing", "author": [ { "family_name": "Krolewski", "given_name": "Alex", "orcid": "0000-0003-2183-7021", "clpid": "Krolewski-Alex" }, { "family_name": "Ferraro", "given_name": "Simone", "orcid": "0000-0003-4992-7854" }, { "family_name": "Schlafly", "given_name": "Edward F.", "orcid": "0000-0002-3569-7421" }, { "family_name": "White", "given_name": "Martin", "orcid": "0000-0001-9912-5070" } ], "abstract": "CMB lensing tomography, or the cross-correlation between CMB lensing maps and large-scale structure tracers over a well-defined redshift range, has the potential to map the amplitude and growth of structure over cosmic time, provide some of the most stringent tests of gravity, and break important degeneracies between cosmological parameters. In this work, we use the unWISE galaxy catalog to provide three samples at median redshifts z \u223c 0.6, 1.1 and 1.5, fully spanning the Dark Energy dominated era, together with the most recent Planck CMB lensing maps. We obtain a combined cross-correlation significance S/N = 79.3 over the range of scales 100 < \u2113 < 1000. We measure the redshift distribution of unWISE sources by a combination of cross-matching with the COSMOS photometric catalog and cross-correlation with BOSS galaxies and quasars and eBOSS quasars. We also show that magnification bias must be included in our analysis and perform a number of null tests. In a companion paper, we explore the derived cosmological parameters by modeling the non-linearities and propagating the redshift distribution uncertainties.", "doi": "10.1088/1475-7516/2020/05/047", "issn": "1475-7516", "publisher": "IOP Publishing", "publication": "Journal of Cosmology and Astroparticle Physics", "publication_date": "2020-05-26", "series_number": "05", "volume": "2020", "issue": "05", "pages": "047-047" } ]