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1. class_sz I: Overview

Author: Bolliet B., Kusiak A., McCarthy F., Sabyr A., Surrao K., Hill J.C., Chluba J., Ferraro S., Hadzhiyska B., Han D., Macías-Pérez J.F., Madhavacheril M., Maniyar A., Mehta Y., Pandey S., Schaan E., Sherwin B., Mancini A. Spurio, and Zubeldia Í.
Subjects: Physics, QC1-999
Abstract: class_sz is a versatile, robust and efficient code, in C and Python, optimized to compute theoretical predictions for a wide range of observables relevant to cross-survey science in the Stage IV era. The code is public at https://github.com/CLASS-SZ/class_sz along with a series of tutorial notebooks (https://github.com/CLASS-SZ/notebooks). It will be presented in full detail in paper II. Here we give a brief overview of key features and usage.
Published: 2024
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2. DESI Spectroscopy of HETDEX Emission-line Candidates I: Line Discrimination Validation

Author: Landriau, Martin, Cooper, Erin Mentuch, Davis, Dustin, Gebhardt, Karl, Ciardullo, Robin, Armengaud, Éric, Dey, Arjun, Raichoor, Anand, Schlegel, David J., Wilson, Michael, Aguilar, J., Ahlen, S., Bianchi, D., Brooks, D., Claybaugh, T., de la Macorra, A., Ferraro, S., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Gutierrez, G., Hahn, C., Honscheid, K., Howlett, C., Ishak, M., Juneau, S., Kehoe, R., Kisner, T., Kremin, Anthony, Guillou, L. Le, Levi, Michael E., Manera, M., Meisner, A., Miquel, R., Moustakas, J., Nadathur, S., Pérez-Ràfols, I., Poppett, C., Prada, F., Rossi, G., Sanchez, E., Schubnell, M., Sprayberry, D., Tarlé, G., Weaver, B. A., Zhou, R., Zou, H., Farrow, Daniel J., Hill, Gary J., Jeong, Donghui, Liu, Chenxu, Saito, Shun, and Schneider, Donald P.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Hobby-Eberly Dark Energy Experiment (HETDEX) is an untargeted spectroscopic galaxy survey that uses Ly$\alpha$ emitting galaxies (LAEs) as tracers of 1.9 < z < 3.5 large scale structure. Most detections consist of a single emission line, whose identity is inferred via a Bayesian analysis of ancillary data. To determine the accuracy of these line identifications, HETDEX detections were observed with the Dark Energy Spectroscopic Instrument (DESI). In two DESI pointings, high confidence spectroscopic redshifts are obtained for 1157 sources, including 982 LAEs. The DESI spectra are used to evaluate the accuracy of the HETDEX object classifications, and tune the methodology to achieve the HETDEX science requirement of $\lesssim 2\%$ contamination of the LAE sample by low-redshift emission-line galaxies, while still assigning $96\%$ of the true Ly$\alpha$ emission sample with the correct spectroscopic redshift. We compare emission line measurements between the two experiments assuming a simple Gaussian line fitting model. Fitted values for the central wavelength of the emission line, the measured line flux and line widths are consistent between the surveys within uncertainties. Derived spectroscopic redshifts, from the two classification pipelines, when both agree as an LAE classification, are consistent to within $\langle \Delta z / (1 + z) \rangle = 6.9\times 10^{-5}$ with an rms scatter of $3.3\times 10^{-4}$., Comment: Submitted to AAS journals
Published: 2025

3. The Simons Observatory: Science Goals and Forecasts for the Enhanced Large Aperture Telescope

Author: Abitbol, M., Abril-Cabezas, I., Adachi, S., Ade, P., Adler, A. E., Agrawal, P., Aguirre, J., Ahmed, Z., Aiola, S., Alford, T., Ali, A., Alonso, D., Alvarez, M. A., An, R., Arnold, K., Ashton, P., Atkins, Z., Austermann, J., Azzoni, S., Baccigalupi, C., Lizancos, A. Baleato, Barron, D., Barry, P., Bartlett, J., Battaglia, N., Battye, R., Baxter, E., Bazarko, A., Beall, J. A., Bean, R., Beck, D., Beckman, S., Begin, J., Beheshti, A., Beringue, B., Bhandarkar, T., Bhimani, S., Bianchini, F., Biermann, E., Biquard, S., Bixler, B., Boada, S., Boettger, D., Bolliet, B., Bond, J. R., Borrill, J., Borrow, J., Braithwaite, C., Brien, T. L. R., Brown, M. L., Bruno, S. M., Bryan, S., Bustos, R., Cai, H., Calabrese, E., Calafut, V., Carl, F. M., Carones, A., Carron, J., Challinor, A., Chanial, P., Chen, N., Cheung, K., Chiang, B., Chinone, Y., Chluba, J., Cho, H. S., Choi, S. K., Chu, M., Clancy, J., Clark, S. E., Clarke, P., Clements, D. L., Connors, J., Contaldi, C., Coppi, G., Corbett, L., Cothard, N. F., Coulton, W., Crowley, K. D., Crowley, K. T., Cukierman, A., D'Ewart, J. M., Dachlythra, K., Datta, R., Day-Weiss, S., de Haan, T., Devlin, M., Di Mascolo, L., Dicker, S., Dober, B., Doux, C., Dow, P., Doyle, S., Duell, C. J., Duff, S. M., Duivenvoorden, A. J., Dunkley, J., Dutcher, D., Dünner, R., Edenton, M., Bouhargani, H. El, Errard, J., Fabbian, G., Fanfani, V., Farren, G. S., Fergusson, J., Ferraro, S., Flauger, R., Foster, A., Freese, K., Frisch, J. C., Frolov, A., Fuller, G., Galitzki, N., Gallardo, P. A., Ghersi, J. T. Galvez, Ganga, K., Gao, J., Garrido, X., Gawiser, E., Gerbino, M., Giardiello, S., Gill, A., Gilles, V., Giri, U., Gleave, E., Gluscevic, V., Goeckner-Wald, N., Golec, J. E., Gordon, S., Gralla, M., Gratton, S., Green, D., Groh, J. C., Groppi, C., Guan, Y., Gupta, N., Guðmundsson, J. E., Hagstotz, S., Hargrave, P., Haridas, S., Harrington, K., Harrison, I., Hasegawa, M., Hasselfield, M., Haynes, V., Hazumi, M., He, A., Healy, E., Henderson, S. W., Hensley, B. S., Hertig, E., Hervías-Caimapo, C., Higuchi, M., Hill, C. A., Hill, J. C., Hilton, G., Hilton, M., Hincks, A. D., Hinshaw, G., Hložek, R., Ho, A. Y. Q., Ho, S., Ho, S. P., Hoang, T. D., Hoh, J., Hornecker, E., Hornsby, A. L., Hoshino, D., Hotinli, S. C., Huang, Z., Huber, Z. B., Hubmayr, J., Huffenberger, K., Hughes, J. P., Lonappan, A. Idicherian, Ikape, M., Irwin, K., Iuliano, J., Jaffe, A. H., Jain, B., Jense, H. T., Jeong, O., Johnson, A., Johnson, B. R., Johnson, M., Jones, M., Jost, B., Kaneko, D., Karpel, E. D., Kasai, Y., Katayama, N., Keating, B., Keller, B., Keskitalo, R., Kim, J., Kisner, T., Kiuchi, K., Klein, J., Knowles, K., Kofman, A. M., Koopman, B. J., Kosowsky, A., Kou, R., Krachmalnicoff, N., Kramer, D., Krishak, A., Krolewski, A., Kusaka, A., Kusiak, A., La Plante, P., La Posta, A., Laguë, A., Lashner, J., Lattanzi, M., Lee, A., Lee, E., Leech, J., Lessler, C., Leung, J. S., Lewis, A., Li, Y., Li, Z., Limon, M., Lin, L., Link, M., Liu, J., Liu, Y., Lonergan, J., Louis, T., Lucas, T., Ludlam, M., Lungu, M., Lyons, M., MacCrann, N., MacInnis, A., Madhavacheril, M., Mak, D., Maldonado, F., Manduca, A., Mangu, A., Mani, H., Maniyar, A. S., Marques, G. A., Mates, J., Matsuda, F., Matsumura, T., Mauskopf, P., May, A., McCallum, N., McCarrick, H., McCarthy, F., McCulloch, M., McMahon, J., Meerburg, P. D., Mehta, Y., Melin, J., Mertens, J., Meyers, J., Middleton, A., Miller, A., Mirmelstein, M., Moodley, K., Moore, J., Morshed, M., Morton, T., Moser, E., Mroczkowski, T., Murata, M., Münchmeyer, M., Naess, S., Nakata, H., Namikawa, T., Nashimoto, M., Nati, F., Natoli, P., Negrello, M., Nerval, S. K., Newburgh, L., Nguyen, D. V., Nicola, A., Niemack, M. D., Nishino, H., Nishinomiya, Y., Orlando, A., Orlando, G., Orlowski-Scherer, J., Pagano, L., Page, L. A., Pandey, S., Papageorgiou, A., Paraskevakos, I., Partridge, B., Patki, R., Peel, M., Sarmiento, K. Perez, Perrotta, F., Phakathi, P., Piccirillo, L., Pierpaoli, E., Pinsonneault-Marotte, T., Pisano, G., Poletti, D., Puddu, R., Puglisi, G., Qu, F. J., Randall, M. J., Ranucci, C., Raum, C., Reeves, R., Reichardt, C. L., Remazeilles, M., Rephaeli, Y., Riechers, D., Robe, J., Robertson, M. F., Robertson, N., Rogers, K., Rojas, F., Romero, A., Rosenberg, E., Rotti, A., Rowe, S., Roy, A., Sadeh, S., Sailer, N., Sakaguri, K., Sakuma, T., Sakurai, Y., Salatino, M., Sanders, G. H., Sasaki, D., Rao, M. Sathyanarayana, Satterthwaite, T. P., Saunders, L., Scalcinati, L., Schaan, E., Schmitt, B., Schmittfull, M., Sehgal, N., Seibert, J., Seino, Y., Seljak, U., Shaikh, S., Shaw, E., Shellard, P., Sherwin, B., Shimon, M., Shroyer, J. E., Sierra, C., Sievers, J., Sifón, C., Sikhosana, P., Silva-Feaver, M., Simon, S. M., Sinclair, A., Smith, K., Sohn, W., Song, X., Sonka, R. F., Spergel, D., Spisak, J., Staggs, S. T., Stein, G., Stevens, J. R., Stompor, R., Storer, E., Sudiwala, R., Sugiyama, J., Surrao, K. M., Suzuki, A., Suzuki, J., Tajima, O., Takakura, S., Takeuchi, A., Tansieri, I., Taylor, A. C., Teply, G., Terasaki, T., Thomas, A., Thomas, D. B., Thornton, R., Trac, H., Tsan, T., Sang, E. Tsang King, Tucker, C., Ullom, J., Vacher, L., Vagnozzi, S., Vale, L., van Engelen, A., Van Lanen, J., van Marrewijk, J., Van Winkle, D. D., Vargas, C., Vavagiakis, E. M., Veenendaal, I., Vergès, C., Vissers, M., Viña, M., Wagoner, K., Walker, S., Walters, L., Wang, Y., Westbrook, B., Williams, J., Williams, P., Winch, H., Wollack, E. J., Wolz, K., Wong, J., Xu, Z., Yamada, K., Young, E., Yu, B., Yu, C., Zannoni, M., Zheng, K., Zhu, N., Zonca, A., and Zubeldia, I.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We describe updated scientific goals for the wide-field, millimeter-wave survey that will be produced by the Simons Observatory (SO). Significant upgrades to the 6-meter SO Large Aperture Telescope (LAT) are expected to be complete by 2028, and will include a doubled mapping speed with 30,000 new detectors and an automated data reduction pipeline. In addition, a new photovoltaic array will supply most of the observatory's power. The LAT survey will cover about 60% of the sky at a regular observing cadence, with five times the angular resolution and ten times the map depth of Planck. The science goals are to: (1) determine the physical conditions in the early universe and constrain the existence of new light particles; (2) measure the integrated distribution of mass, electron pressure, and electron momentum in the late-time universe, and, in combination with optical surveys, determine the neutrino mass and the effects of dark energy via tomographic measurements of the growth of structure at $z < 3$; (3) measure the distribution of electron density and pressure around galaxy groups and clusters, and calibrate the effects of energy input from galaxy formation on the surrounding environment; (4) produce a sample of more than 30,000 galaxy clusters, and more than 100,000 extragalactic millimeter sources, including regularly sampled AGN light-curves, to study these sources and their emission physics; (5) measure the polarized emission from magnetically aligned dust grains in our Galaxy, to study the properties of dust and the role of magnetic fields in star formation; (6) constrain asteroid regoliths, search for Trans-Neptunian Objects, and either detect or eliminate large portions of the phase space in the search for Planet 9; and (7) provide a powerful new window into the transient universe on time scales of minutes to years, concurrent with observations from Rubin of overlapping sky., Comment: 44 pages, 7 figures; abstract slightly abridged. Author contributions to this paper are available at https://simonsobservatory.org/wp-content/uploads/2025/02/Author-contribution-statement-20250228.pdf
Published: 2025

4. DESI 2024 IV: Baryon Acoustic Oscillations from the Lyman alpha forest

Author: Adame, AG, Aguilar, J, Ahlen, S, Alam, S, Alexander, DM, Alvarez, M, Alves, O, Anand, A, Andrade, U, Armengaud, E, Avila, S, Aviles, A, Awan, H, Bailey, S, Baltay, C, Bault, A, Bautista, J, Behera, J, BenZvi, S, Beutler, F, Bianchi, D, Blake, C, Blum, R, Brieden, S, Brodzeller, A, Brooks, D, Buckley-Geer, E, Burtin, E, Calderon, R, Canning, R, Rosell, A Carnero, Cereskaite, R, Cervantes-Cota, JL, Chabanier, S, Chaussidon, E, Chaves-Montero, J, Chen, S, Chen, X, Claybaugh, T, Cole, S, Cuceu, A, Davis, TM, Dawson, K, de la Cruz, R, de la Macorra, A, de Mattia, A, Deiosso, N, Dey, A, Dey, B, Ding, J, Ding, Z, Doel, P, Edelstein, J, Eftekharzadeh, S, Eisenstein, DJ, Elliott, A, Fagrelius, P, Fanning, K, Ferraro, S, Ereza, J, Findlay, N, Flaugher, B, Font-Ribera, A, Forero-Sánchez, D, Forero-Romero, JE, Garcia-Quintero, C, Gaztañaga, E, Gil-Marín, H, Gontcho, S Gontcho A, Gonzalez-Morales, AX, Gonzalez-Perez, V, Gordon, C, Green, D, Gruen, D, Gsponer, R, Gutierrez, G, Guy, J, Hadzhiyska, B, Hahn, C, Hanif, MMS, Herrera-Alcantar, HK, Honscheid, K, Howlett, C, Huterer, D, Iršič, V, Ishak, M, Juneau, S, Karaçaylı, NG, Kehoe, R, Kent, S, Kirkby, D, Kremin, A, Krolewski, A, Lai, Y, Lan, T-W, Landriau, M, Lang, D, Lasker, J, Le Goff, JM, and Le Guillou, L
Subjects: Particle and High Energy Physics, Astronomical Sciences, Physical Sciences, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics, Astronomical sciences, Particle and high energy physics
Abstract: Abstract: We present the measurement of Baryon Acoustic Oscillations (BAO) from the Lyman-α (Lyα) forest of high-redshift quasars with the first-year dataset of the Dark Energy Spectroscopic Instrument (DESI). Our analysis uses over 420 000 Lyα forest spectra and their correlation with the spatial distribution of more than 700 000 quasars. An essential facet of this work is the development of a new analysis methodology on a blinded dataset. We conducted rigorous tests using synthetic data to ensure the reliability of our methodology and findings before unblinding. Additionally, we conducted multiple data splits to assess the consistency of the results and scrutinized various analysis approaches to confirm their robustness. For a given value of the sound horizon (rd ), we measure the expansion at z eff = 2.33 with 2% precision, H(z eff) = ( 239.2 ± 4.8 ) (147.09 Mpc /rd ) km/s/Mpc. Similarly, we present a 2.4% measurement of the transverse comoving distance to the same redshift, DM (z eff) = ( 5.84 ± 0.14 ) (rd /147.09 Mpc) Gpc. Together with other DESI BAO measurements at lower redshifts, these results are used in a companion paper to constrain cosmological parameters.
Published: 2025

5. An analysis of parameter compression and Full-Modeling techniques with Velocileptors for DESI 2024 and beyond

Author: Maus, M, Chen, S, White, M, Aguilar, J, Ahlen, S, Aviles, A, Brieden, S, Brooks, D, Claybaugh, T, Cole, S, de la Macorra, A, Dey, Arjun, Doel, P, Ferraro, S, Findlay, N, Forero-Romero, JE, Gaztañaga, E, Gil-Marín, H, Gontcho, S Gontcho A, Hahn, C, Honscheid, K, Howlett, C, Ishak, M, Juneau, S, Kremin, A, Lai, Y, Landriau, M, Levi, ME, Manera, M, Miquel, R, Mueller, E, Myers, AD, Nadathur, S, Nie, J, Noriega, HE, Palanque-Delabrouille, N, Percival, WJ, Poppett, C, Ramirez-Solano, S, Rezaie, M, Rocher, A, Rossi, G, Sanchez, E, Schlegel, D, Schubnell, M, Seo, H, Sprayberry, D, Tarlé, G, Vargas-Magaña, M, Weaver, BA, Yuan, S, Zarrouk, P, Zhang, H, Zhou, R, and Zou, H
Subjects: Nuclear and Plasma Physics, Physical Sciences, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics, Astronomical sciences, Particle and high energy physics
Abstract: Abstract: In anticipation of forthcoming data releases of current and future spectroscopic surveys, we present the validation tests and analysis of systematic effects within velocileptors modeling pipeline when fitting mock data from the AbacusSummit N-body simulations. We compare the constraints obtained from parameter compression methods to the direct fitting (Full-Modeling) approaches of modeling the galaxy power spectra, and show that the ShapeFit extension to the traditional template method is consistent with the Full-Modeling method within the standard ΛCDM parameter space. We show the dependence on scale cuts when fitting the different redshift bins using the ShapeFit and Full-Modeling methods. We test the ability to jointly fit data from multiple redshift bins as well as joint analysis of the pre-reconstruction power spectrum with the post-reconstruction BAO correlation function signal. We further demonstrate the behavior of the model when opening up the parameter space beyond ΛCDM and also when combining likelihoods with external datasets, namely the Planck CMB priors. Finally, we describe different parametrization options for the galaxy bias, counterterm, and stochastic parameters, and employ the halo model in order to physically motivate suitable priors that are necessary to ensure the stability of the perturbation theory.
Published: 2025

6. A comparison of effective field theory models of redshift space galaxy power spectra for DESI 2024 and future surveys

Author: Maus, M, Lai, Y, Noriega, HE, Ramirez-Solano, S, Aviles, A, Chen, S, Fromenteau, S, Gil-Marín, H, Howlett, C, Vargas-Magaña, M, White, M, Zarrouk, P, Aguilar, J, Ahlen, S, Alves, O, Brieden, S, Brooks, D, Burtin, E, Claybaugh, T, Cole, S, Dawson, K, Icaza-Lizaola, M, de la Macorra, A, de Mattia, A, Doel, P, Ferraro, S, Findlay, N, Forero-Romero, JE, Gaztañaga, E, Gontcho, S Gontcho A, Hahn, C, Honscheid, K, Ishak, M, Kremin, A, Landriau, M, Le Guillou, L, Manera, M, Miquel, R, Mueller, E, Nadathur, S, Niz, G, Palanque-Delabrouille, N, Percival, WJ, Poppett, C, Prada, F, Rezaie, M, Rocher, A, Rossi, G, Sanchez, E, Schlegel, D, Schubnell, M, Sprayberry, D, Tarlé, G, Yuan, S, Zhao, R, Zhou, R, and Zou, H
Subjects: Nuclear and Plasma Physics, Physical Sciences, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics, Astronomical sciences, Particle and high energy physics
Abstract: Abstract: In preparation for the next generation of galaxy redshift surveys, and in particular the year-one data release from the Dark Energy Spectroscopic Instrument (DESI), we investigate the consistency of a variety of effective field theory models that describe the galaxy-galaxy power spectra in redshift space into the quasi-linear regime using 1-loop perturbation theory. These models are employed in the pipelines velocileptors, PyBird, and Folpsν . While these models have been validated independently, a detailed comparison with consistent choices has not been attempted. After briefly discussing the theoretical differences between the models we describe how to provide a more apples-to-apples comparison between them. We present the results of fitting mock spectra from the AbacusSummit suite of N-body simulations provided in three redshift bins to mimic the types of dark time tracers targeted by the DESI survey. We show that the theories behave similarly and give consistent constraints in both the forward-modeling and ShapeFit compressed fitting approaches. We additionally generate (noiseless) synthetic data from each pipeline to be fit by the others, varying the scale cuts in order to show that the models agree within the range of scales for which we expect 1-loop perturbation theory to be applicable. This work lays the foundation of Full-Shape analysis with DESI Y1 galaxy samples where in the tests we performed, we found no systematic error associated with the modeling of the galaxy redshift space power spectrum for this volume.
Published: 2025

7. The DESI-Lensing Mock Challenge: large-scale cosmological analysis of 3x2-pt statistics

Author: Blake, C., Garcia-Quintero, C., Ahlen, S., Bianchi, D., Brooks, D., Claybaugh, T., de la Macorra, A., DeRose, J., Dey, A., Doel, P., Emas, N., Ferraro, S., Forero-Romero, J. E., Gutierrez, G., Heydenreich, S., Honscheid, K., Howlett, C., Ishak, M., Joudaki, S., Jullo, E., Kehoe, R., Kirkby, D., Kremin, A., Krolewski, A., Landriau, M., Lange, J. U., Leauthaud, A., Levi, M. E., Manera, M., Miquel, R., Moustakas, J., Niz, G., Percival, W. J., Pérez-Ràfols, I., Porredon, A., Rossi, G., Ruggeri, R., Sanchez, E., Saulder, C., Schlegel, D., Sprayberry, D., Sun, Z., Tarlé, G., and Weaver, B. A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The current generation of large galaxy surveys will test the cosmological model by combining multiple types of observational probes. Realising the statistical promise of these new datasets requires rigorous attention to all aspects of analysis including cosmological measurements, modelling, covariance and parameter likelihood. In this paper we present the results of an end-to-end simulation study designed to test the analysis pipeline for the combination of the Dark Energy Spectroscopic Instrument (DESI) Year 1 galaxy redshift dataset and separate weak gravitational lensing information from the Kilo-Degree Survey, Dark Energy Survey and Hyper-Suprime-Cam Survey. Our analysis employs the 3x2-pt correlation functions including cosmic shear and galaxy-galaxy lensing, together with the projected correlation function of the spectroscopic DESI lenses. We build realistic simulations of these datasets including galaxy halo occupation distributions, photometric redshift errors, weights, multiplicative shear calibration biases and magnification. We calculate the analytical covariance of these correlation functions including the Gaussian, noise and super-sample contributions, and show that our covariance determination agrees with estimates based on the ensemble of simulations. We use a Bayesian inference platform to demonstrate that we can recover the fiducial cosmological parameters of the simulation within the statistical error margin of the experiment, investigating the sensitivity to scale cuts. This study is the first in a sequence of papers in which we present and validate the large-scale 3x2-pt cosmological analysis of DESI-Y1., Comment: 29 pages, 17 figures, accepted for publication in The Open Journal of Astrophysics
Published: 2024

8. Constraints on primordial non-Gaussianity from the cross-correlation of DESI Luminous Red Galaxies and $Planck$ CMB lensing

Author: Bermejo-Climent, J. R., Demina, R., Krolewski, A., Chaussidon, E., Rezaie, M., Ahlen, S., Bailey, S., Bianchi, D., Brooks, D., Burtin, E., Claybaugh, T., de la Macorra, A., Dey, Arjun, Doel, P., Farren, G., Ferraro, S., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Gutierrez, G., Hahn, C., Honscheid, K., Howlett, C., Kehoe, R., Kirkby, D., Kisner, T., Landriau, M., Guillou, L. Le, Levi, M. E., Manera, M., Meisner, A., Miquel, R., Moustakas, J., Newman, J. A., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Prada, F., Pérez-Ràfols, I., Rabinowitz, D., Ross, A. J., Rossi, G., Sanchez, E., Schlegel, D., Sprayberry, D., Tarlé, G., Weaver, B. A., White, M., Yèche, C., and Zarrouk, P.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use the angular cross-correlation between a Luminous Red Galaxy (LRG) sample from the DR9 DESI Legacy Survey and the $Planck$ PR4 CMB lensing maps to constrain the local primordial non-Gaussianity parameter $f_{\rm NL}$ using the scale-dependent galaxy bias effect. The galaxy sample covers $\sim$ 40% of the sky and contains galaxies up to $z \sim 1.4$, and is calibrated with the LRG spectra that have been observed for the DESI Survey Validation. We apply a nonlinear imaging systematics treatment based on neural networks to remove observational effects that could potentially bias the $f_{\rm NL}$ measurement. Our measurement is performed without blinding, but the full analysis pipeline is tested with simulations including systematics. Using the two-point angular cross-correlation between LRG and CMB lensing only ($C_\ell^{\kappa G}$) we find $f_{\rm NL} = 39_{-38}^{+40}$ at 68% confidence level, and our result is robust in terms of systematics and cosmology assumptions. If we combine this information with the autocorrelation of LRG ($C_\ell^{GG}$) applying a $\ell_{\rm min}$ scale cut to limit the impact of systematics, we find $f_{\rm NL} = 24_{-21}^{+20}$ at 68% confidence level. Our results motivate the use of CMB lensing cross-correlations for measuring $f_{\rm NL}$ with future datasets given its stability in terms of observational systematics compared to the angular auto-correlation., Comment: 13 pages, 11 figures, to be submitted to A&A
Published: 2024

9. Extensive analysis of reconstruction algorithms for DESI 2024 baryon acoustic oscillations

Author: Chen, X., Ding, Z., Paillas, E., Nadathur, S., Seo, H., Chen, S., Padmanabhan, N., White, M., de Mattia, A., McDonald, P., Ross, A. J., Variu, A., Rosell, A. Carnero, Hadzhiyska, B., Hanif, M. M. S, Forero-Sánchez, D., Ahlen, S., Alves, O., Andrade, U., BenZvi, S., Bianchi, D., Brooks, D., Chaussidon, E., Claybaugh, T., de la Macorra, A., Dey, Biprateep, Fanning, K., Ferraro, S., Font-Ribera, A., Forero-Romero, J. E., Garcia-Quintero, C., Gaztañaga, E., Gontcho, S. Gontcho A, Gutierrez, G., Hahn, C., Honscheid, K., Juneau, S., Kehoe, R., Kirkby, D., Kisner, T., Kremin, A., Levi, M. E., Meisner, A., Mena-Fernández, J., Miquel, R., Moustakas, J., Muñoz-Gutiérrez, A., Nikakhtar, F., Palanque-Delabrouille, N., Percival, W. J., Prada, F., Pérez-Ràfols, I., Rashkovetskyi, M., Rossi, G., Ruggeri, R., Sanchez, E., Saulder, C., Schlegel, D., Schubnell, M., Smith, A., Sprayberry, D., Tarlé, G., Valcin, D., Vargas-Magaña, M., Weaver, B. A., Yuan, S., and Zhou, R.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Reconstruction of the baryon acoustic oscillation (BAO) signal has been a standard procedure in BAO analyses over the past decade and has helped to improve the BAO parameter precision by a factor of ~2 on average. The Dark Energy Spectroscopic Instrument (DESI) BAO analysis for the first year (DR1) data uses the ``standard'' reconstruction framework, in which the displacement field is estimated from the observed density field by solving the linearized continuity equation in redshift space, and galaxy and random positions are shifted in order to partially remove nonlinearities. There are several approaches to solving for the displacement field in real survey data, including the multigrid (MG), iterative Fast Fourier Transform (iFFT), and iterative Fast Fourier Transform particle (iFFTP) algorithms. In this work, we analyze these algorithms and compare them with various metrics including two-point statistics and the displacement itself using realistic DESI mocks. We focus on three representative DESI samples, the emission line galaxies (ELG), quasars (QSO), and the bright galaxy sample (BGS), which cover the extreme redshifts and number densities, and potential wide-angle effects. We conclude that the MG and iFFT algorithms agree within 0.4% in post-reconstruction power spectrum on BAO scales with the RecSym convention, which does not remove large-scale redshift space distortions (RSDs), in all three tracers. The RecSym convention appears to be less sensitive to displacement errors than the RecIso convention, which attempts to remove large-scale RSDs. However, iFFTP deviates from the first two; thus, we recommend against using iFFTP without further development. In addition, we provide the optimal settings for reconstruction for five years of DESI observation. The analyses presented in this work pave the way for DESI DR1 analysis as well as future BAO analyses., Comment: 51 pages, 28 figures. Supporting publication of DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars
Published: 2024

10. Constraining primordial non-Gaussianity with DESI 2024 LRG and QSO samples

Author: Chaussidon, E., Yèche, C., de Mattia, A., Payerne, C., McDonald, P., Ross, A. J., Ahlen, S., Bianchi, D., Brooks, D., Burtin, E., Claybaugh, T., de la Macorra, A., Doel, P., Ferraro, S., Font-Ribera, A., Forero-Romero, J. E., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gutierrez, G., Guy, J., Honscheid, K., Howlett, C., Huterer, D., Kehoe, R., Kirkby, D., Kisner, T., Kremin, A., Guillou, L. Le, Levi, M. E., Manera, M., Meisner, A., Miquel, R., Moustakas, J., Newman, J. A., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Prada, F., Pérez-Ràfols, I., Ravoux, C., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Seo, H., Sprayberry, D., Tarlé, G., Vargas-Magaña, M., Weaver, B. A., Zhao, C., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We analyse the large-scale clustering of the Luminous Red Galaxy (LRG) and Quasar (QSO) sample from the first data release (DR1) of the Dark Energy Spectroscopic Instrument (DESI). In particular, we constrain the primordial non-Gaussianity (PNG) parameter $f_{\rm NL}^{\rm loc}$ via the large-scale scale-dependent bias in the power spectrum using $1,631,716$ LRGs ($0.6 < z < 1.1$) and $1,189,129$ QSOs ($0.8 < z < 3.1$). This new measurement takes advantage of the enormous statistical power at large scales of DESI DR1 data, surpassing the latest data release (DR16) of the extended Baryon Oscillation Spectroscopic Survey (eBOSS). For the first time in this kind of analysis, we use a blinding procedure to mitigate the risk of confirmation bias in our results. We improve the model of the radial integral constraint proposing an innovative correction of the window function. We also carefully test the mitigation of the dependence of the target selection on the photometry qualities by incorporating an angular integral constraint contribution to the window function, and validate our methodology with the blinded data. Finally, combining the two samples, we measure $f_{\rm NL}^{\rm loc} = {-3.6}_{-9.1}^{+9.0}$ at $68\%$ confidence, where we assume the universality relation for the LRG sample and a recent merger model for the QSO sample about the response of bias to primordial non-Gaussianity. Adopting the universality relation for the PNG bias in the QSO analysis leads to $f_{\rm NL}^{\rm loc} = 3.5_{-7.4}^{+10.7}$ at $68\%$ confidence. This measurement is the most precise determination of primordial non-Gaussianity using large-scale structure to date, surpassing the latest result from eBOSS by a factor of $2.3$.
Published: 2024

11. A Sound Horizon-Free Measurement of $H_0$ in DESI 2024

Author: Zaborowski, E. A., Taylor, P., Honscheid, K., Cuceu, A., de Mattia, A., Huterer, D., Krolewski, A., Martini, P., Ross, A. J., To, C., Torres, A., Ahlen, S., Bianchi, D., Brooks, D., Buckley-Geer, E., Burtin, E., Claybaugh, T., Cole, S., de la Macorra, A., Dey, Arjun, Dey, Biprateep, Doel, P., Ferraro, S., Font-Ribera, A., Forero-Romero, J. E., Gaztañaga, E., Gil-Marín, H., Gutierrez, G., Guy, J., Hahn, C., Howlett, C., Juneau, S., Kehoe, R., Kirkby, D., Kisner, T., Kremin, A., Landriau, M., Guillou, L. Le, Levi, M. E., Magneville, C., Meisner, A., Miquel, R., Moustakas, J., Palanque-Delabrouille, N., Percival, W. J., Prada, F., Pérez-Ràfols, I., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Seo, H., Sprayberry, D., Tarlé, G., Weaver, B. A., and Wechsler, R. H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The physical size of the sound horizon at recombination is a powerful source of information for early-time measurements of the Hubble constant $H_0$, and many proposed solutions to the Hubble tension therefore involve modifications to this scale. In light of this, there has been growing interest in measuring $H_0$ independently of the sound horizon. We present the first such measurement to use data from the Dark Energy Spectroscopic Instrument (DESI), jointly analyzing the full-shape galaxy power spectra of DESI luminous red galaxies, emission line galaxies, quasars, and the bright galaxy sample, in a total of six redshift bins. Information from the sound horizon scale is removed from our constraints via a rescaling procedure at the power spectrum level, with our sound horizon-marginalized measurement being driven instead primarily by the matter-radiation equality scale. This measurement is then combined with additional sound horizon-free information from Planck+ACT CMB lensing, uncalibrated type Ia supernovae, and the DESI Lyman-$\alpha$ forest. We agnostically combine with the DESY5, Pantheon+, and Union3 supernova datasets, with our tightest respective constraints being $H_0=66.7^{+1.7}_{-1.9},~67.9^{+1.9}_{-2.1},$ and $67.8^{+2.0}_{-2.2}$ km s-1 Mpc-1. This corresponds to a sub-3% sound horizon-free constraint of the Hubble constant, and is the most precise measurement of its kind to date. Even without including information from the sound horizon, our measurement is still in 2.2-3.0$\sigma$ tension with SH0ES. Additionally, the consistency between our result and other measurements that do rely on the sound horizon scale provides no evidence for new early-Universe physics (e.g. early dark energy). Future DESI data releases will allow unprecedented measurements of $H_0$ and place strong constraints on models that use beyond-$\Lambda$CDM physics to ameliorate the Hubble tension., Comment: 17+7 pages; 5 figures. Submitted to JCAP
Published: 2024

12. Modified Gravity Constraints from the Full Shape Modeling of Clustering Measurements from DESI 2024

Author: Ishak, M., Pan, J., Calderon, R., Lodha, K., Valogiannis, G., Aviles, A., Niz, G., Yi, L., Zheng, C., Garcia-Quintero, C., de Mattia, A., Medina-Varela, L., Cervantes-Cota, J. L., Andrade, U., Huterer, D., Noriega, H. E., Zhao, G., Shafieloo, A., Fang, W., Ahlen, S., Bianchi, D., Brooks, D., Burtin, E., Chaussidon, E., Claybaugh, T., Cole, S., de la Macorra, A., Dey, Arjun, Fanning, K., Ferraro, S., Font-Ribera, A., Forero-Romero, J. E., Gaztañaga, E., Gil-Marín, H., Gutierrez, G., Hahn, C., Honscheid, K., Howlett, C., Juneau, S., Kirkby, D., Kisner, T., Kremin, A., Landriau, M., Guillou, L. Le, Leauthaud, A., Levi, M. E., Meisner, A., Miquel, R., Moustakas, J., Newman, J. A., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Pérez-Ràfols, I., Ross, A. J., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Seo, H., Sprayberry, D., Tarlé, G., Vargas-Magana, M., Weaver, B. A., Wechsler, R. H., Yèche, C., Zarrouk, P., Zhou, R., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present cosmological constraints on deviations from general relativity (GR) from the first-year of clustering observations from the Dark Energy Spectroscopic Instrument (DESI) in combination with other datasets. We first consider the $\mu(a,k)$-$\Sigma(a,k)$ modified gravity (MG) parametrization (as well as $\eta(a,k)$) in flat $\Lambda$CDM and $w_0 w_a$CDM backgrounds. Using a functional form for time-only evolution gives $\mu_0= 0.11^{+0.44}_{-0.54}$ from DESI(FS+BAO)+BBN and a wide prior on $n_{s}$. Using DESI(FS+BAO)+CMB+DESY3+DESY5-SN, we obtain $\mu_0 = 0.05\pm 0.22$ and $\Sigma_0 = 0.008\pm 0.045$ in the $\Lambda$CDM background. In $w_0 w_a$CDM, we obtain $\mu_0 =-0.24^{+0.32}_{-0.28}$ and $\Sigma_0 = 0.006\pm 0.043$, consistent with GR, and we still find a preference of the data for dynamical dark energy with $w_0>-1$ and $w_a<0$. We then use binned forms in the two backgrounds starting with two bins in redshift and then combining them with two bins in scale for a total of 4 and 8 MG parameters, respectively. All MG parameters are found consistent with GR. We also find that the tension reported for $\Sigma_0$ with GR when using Planck PR3 goes away when we use the recent LoLLiPoP+HiLLiPoP likelihoods. As noted previously, this seems to indicate that the tension is related to the CMB lensing anomaly in PR3 which is also resolved when using these likelihoods. We then constrain the class of Horndeski theory in the effective field theory of dark energy. We consider both EFT-basis and $\alpha$-basis. Assuming a power law parametrization for the function $\Omega$, which controls non-minimal coupling, we obtain $\Omega_0 = 0.012^{+0.001}_{-0.012}$ and $s_0 = 0.996^{+0.54}_{-0.20}$ from DESI(FS+BAO)+DESY5SN+CMB in a $\Lambda$CDM background. Similar results are obtained when using the $\alpha$-basis, where we constrain $c_M<1.14$, and are all consistent with GR. [Abridged.], Comment: 55 pages, 13 figures. This DESI Collaboration Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers/). Added 3 figures and more discussions
Published: 2024

13. Characterization of DESI fiber assignment incompleteness effect on 2-point clustering and mitigation methods for DR1 analysis

Author: Bianchi, D., Hanif, M. M. S, Rosell, A. Carnero, Lasker, J., Ross, A. J., Pinon, M., de Mattia, A., White, M., Ahlen, S., Bailey, S., Brooks, D., Burtin, E., Chaussidon, E., Claybaugh, T., Cole, S., de la Macorra, A., Ferraro, S., Font-Ribera, A., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Gutierrez, G., Guy, J., Hahn, C., Honscheid, K., Howlett, C., Juneau, S., Kirkby, D., Kisner, T., Kremin, A., Landriau, M., Guillou, L. Le, Levi, M. E., McDonald, P., Meisner, A., Miquel, R., Moustakas, J., Palanque-Delabrouille, N., Percival, W. J., Prada, F., Pérez-Ràfols, I., Raichoor, A., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Sharples, R., Silber, J., Sprayberry, D., Tarlé, G., Vargas-Magaña, M., Weaver, B. A., Zarrouk, P., Zhou, R., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present an in-depth analysis of the fiber assignment incompleteness in the Dark Energy Spectroscopic Instrument (DESI) Data Release 1 (DR1). This incompleteness is caused by the restricted mobility of the robotic fiber positioner in the DESI focal plane, which limits the number of galaxies that can be observed at the same time, especially at small angular separations. As a result, the observed clustering amplitude is suppressed in a scale-dependent manner, which, if not addressed, can severely impact the inference of cosmological parameters. We discuss the methods adopted for simulating fiber assignment on mocks and data. In particular, we introduce the fast fiber assignment (FFA) emulator, which was employed to obtain the power spectrum covariance adopted for the DR1 full-shape analysis. We present the mitigation techniques, organised in two classes: measurement stage and model stage. We then use high fidelity mocks as a reference to quantify both the accuracy of the FFA emulator and the effectiveness of the different measurement-stage mitigation techniques. This complements the studies conducted in a parallel paper for the model-stage techniques, namely the $\theta$-cut approach. We find that pairwise inverse probability (PIP) weights with angular upweighting recover the "true" clustering in all the cases considered, in both Fourier and configuration space. Notably, we present the first ever power spectrum measurement with PIP weights from real data., Comment: 42 pages, 19 figures
Published: 2024

14. Mitigating Imaging Systematics for DESI 2024 Emission Line Galaxies and Beyond

Author: Rosado-Marín, A. J., Ross, A. J., Seo, H., Rezaie, M., Kong, H., de Mattia, A., Zhou, R., Aguilar, J., Ahlen, S., Alves, O., Bianchi, D., Brooks, D., Burtin, E., Chaussidon, E., Chen, X., Claybaugh, T., Dawson, K. S., de la Macorra, A., Dey, Arjun, Doel, P., Fanning, K., Ferraro, S., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Gutierrez, G., Hahn, C., Hanif, M. M. S, Howlett, C., Juneau, S., Kehoe, R., Kisner, T., Kremin, A., Krolewski, A., Landriau, M., Guillou, L. Le, Levi, M. E., Meisner, A., Mena-Fernández, J., Miquel, R., Moustakas, J., Newman, J. A., Paillas, E., Palanque-Delabrouille, N., Percival, W. J., Prada, F., Pérez-Ràfols, I., Raichoor, A., Rossi, G., Ruggeri, R., Sanchez, E., Schlafly, E. F., Schlegel, D., Schubnell, M., Sprayberry, D., Vargas-Magaña, M., Weaver, B. A., Yu, J., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Emission Line Galaxies (ELGs) are one of the main tracers that the Dark Energy Spectroscopic Instrument (DESI) uses to probe the universe. However, they are afflicted by strong spurious correlations between target density and observing conditions known as imaging systematics. We present the imaging systematics mitigation applied to the DESI Data Release 1 (DR1) large-scale structure catalogs used in the DESI 2024 cosmological analyses. We also explore extensions of the fiducial treatment. This includes a combined approach, through forward image simulations in conjunction with neural network-based regression, to obtain an angular selection function that mitigates the imaging systematics observed in the DESI DR1 ELGs target density. We further derive a line-of-sight selection function from the forward model that removes the strong redshift dependence between imaging systematics and low redshift ELGs. Combining both angular and redshift-dependent systematics, we construct a 3D selection function and assess the impact of all selection functions on clustering statistics. We quantify differences between these extended treatments and the fiducial treatment in terms of the measured 2-point statistics. We find that the results are generally consistent with the fiducial treatment and conclude that the differences are far less than the imaging systematics uncertainty included in DESI 2024 full-shape measurements. We extend our investigation to the ELGs at $0.6
Published: 2024

15. DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Measurements

Author: DESI Collaboration, Adame, A. G., Aguilar, J., Ahlen, S., Alam, S., Alexander, D. M., Prieto, C. Allende, Alvarez, M., Alves, O., Anand, A., Andrade, U., Armengaud, E., Avila, S., Aviles, A., Awan, H., Bahr-Kalus, B., Bailey, S., Baltay, C., Bault, A., Behera, J., BenZvi, S., Beutler, F., Bianchi, D., Blake, C., Blum, R., Bonici, M., Brieden, S., Brodzeller, A., Brooks, D., Buckley-Geer, E., Burtin, E., Calderon, R., Canning, R., Rosell, A. Carnero, Cereskaite, R., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Chebat, D., Chen, S., Chen, X., Claybaugh, T., Cole, S., Cuceu, A., Davis, T. M., Dawson, K., de la Macorra, A., de Mattia, A., Deiosso, N., Dey, A., Dey, B., Ding, Z., Doel, P., Edelstein, J., Eftekharzadeh, S., Eisenstein, D. J., Elbers, W., Elliott, A., Fagrelius, P., Fanning, K., Ferraro, S., Ereza, J., Findlay, N., Flaugher, B., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Frenk, C. S., Garcia-Quintero, C., Garrison, L. H., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gonzalez-Perez, V., Gordon, C., Green, D., Gruen, D., Gsponer, R., Gutierrez, G., Guy, J., Hadzhiyska, B., Hahn, C., Hanif, M. M. S, Herrera-Alcantar, H. K., Honscheid, K., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Joyce, R., Juneau, S., Karaçaylı, N. G., Kehoe, R., Kent, S., Kirkby, D., Kong, H., Koposov, S. E., Kremin, A., Krolewski, A., Lahav, O., Lai, Y., Lan, T. -W., Landriau, M., Lang, D., Lasker, J., Goff, J. M. Le, Guillou, L. Le, Leauthaud, A., Levi, M. E., Li, T. S., Lodha, K., Magneville, C., Manera, M., Margala, D., Martini, P., Matthewson, W., Maus, M., McDonald, P., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Miquel, R., Moon, J., Moore, S., Moustakas, J., Mudur, N., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Napolitano, L., Neveux, R., Newman, J. A., Nguyen, N. M., Nie, J., Niz, G., Noriega, H. E., Padmanabhan, N., Paillas, E., Palanque-Delabrouille, N., Pan, J., Penmetsa, S., Percival, W. J., Pieri, M. M., Pinon, M., Poppett, C., Porredon, A., Prada, F., Pérez-Fernández, A., Pérez-Ràfols, I., Rabinowitz, D., Raichoor, A., Ramírez-Pérez, C., Ramirez-Solano, S., Rashkovetskyi, M., Ravoux, C., Rezaie, M., Rich, J., Rocher, A., Rockosi, C., Roe, N. A., Rosado-Marin, A., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Samushia, L., Sanchez, E., Saulder, C., Schlafly, E. F., Schlegel, D., Schubnell, M., Seo, H., Shafieloo, A., Sharples, R., Silber, J., Slosar, A., Smith, A., Sprayberry, D., Tan, T., Tarlé, G., Taylor, P., Trusov, S., Vaisakh, R., Valcin, D., Valdes, F., Valogiannis, G., Vargas-Magaña, M., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, N., Wechsler, R. H., Weinberg, D. H., White, M., Wilson, M. J., Yi, L., Yu, J., Yu, Y., Yuan, S., Yèche, C., Zaborowski, E. A., Zarrouk, P., Zhang, H., Zhao, C., Zhao, R., Zhou, R., Zhuang, T., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present cosmological results from the measurement of clustering of galaxy, quasar and Lyman-$\alpha$ forest tracers from the first year of observations with the Dark Energy Spectroscopic Instrument (DESI Data Release 1). We adopt the full-shape (FS) modeling of the power spectrum, including the effects of redshift-space distortions, in an analysis which has been validated in a series of supporting papers. In the flat $\Lambda$CDM cosmological model, DESI (FS+BAO), combined with a baryon density prior from Big Bang Nucleosynthesis and a weak prior on the scalar spectral index, determines matter density to $\Omega_\mathrm{m}=0.2962\pm 0.0095$, and the amplitude of mass fluctuations to $\sigma_8=0.842\pm 0.034$. The addition of the cosmic microwave background (CMB) data tightens these constraints to $\Omega_\mathrm{m}=0.3056\pm 0.0049$ and $\sigma_8=0.8121\pm 0.0053$, while further addition of the the joint clustering and lensing analysis from the Dark Energy Survey Year-3 (DESY3) data leads to a 0.4% determination of the Hubble constant, $H_0 = (68.40\pm 0.27)\,{\rm km\,s^{-1}\,Mpc^{-1}}$. In models with a time-varying dark energy equation of state, combinations of DESI (FS+BAO) with CMB and type Ia supernovae continue to show the preference, previously found in the DESI DR1 BAO analysis, for $w_0>-1$ and $w_a<0$ with similar levels of significance. DESI data, in combination with the CMB, impose the upper limits on the sum of the neutrino masses of $\sum m_\nu < 0.071\,{\rm eV}$ at 95% confidence. DESI data alone measure the modified-gravity parameter that controls the clustering of massive particles, $\mu_0=0.11^{+0.45}_{-0.54}$, while the combination of DESI with the CMB and the clustering and lensing analysis from DESY3 constrains both modified-gravity parameters, giving $\mu_0 = 0.04\pm 0.22$ and $\Sigma_0 = 0.044\pm 0.047$, in agreement with general relativity. [Abridged.], Comment: This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers/). 55 pages, 10 figures
Published: 2024

16. DESI 2024 II: Sample Definitions, Characteristics, and Two-point Clustering Statistics

Author: DESI Collaboration, Adame, A. G., Aguilar, J., Ahlen, S., Alam, S., Alexander, D. M., Alvarez, M., Alves, O., Anand, A., Andrade, U., Armengaud, E., Avila, S., Aviles, A., Awan, H., Bailey, S., Baltay, C., Bault, A., Behera, J., BenZvi, S., Beutler, F., Bianchi, D., Blake, C., Blum, R., Brieden, S., Brodzeller, A., Brooks, D., Brown, Z., Buckley-Geer, E., Burtin, E., Calderon, R., Canning, R., Rosell, A. Carnero, Cereskaite, R., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Chen, S., Chen, X., Claybaugh, T., Cole, S., Cuceu, A., Davis, T. M., Dawson, K., de la Macorra, A., de Mattia, A., Deiosso, N., Demina, R., Dey, A., Dey, B., Ding, Z., Doel, P., Edelstein, J., Eftekharzadeh, S., Eisenstein, D. J., Elliott, A., Fagrelius, P., Fanning, K., Ferraro, S., Ereza, J., Findlay, N., Flaugher, B., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Frenk, C. S., Garcia-Quintero, C., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gonzalez-Perez, V., Gordon, C., Green, D., Gruen, D., Gsponer, R., Gutierrez, G., Guy, J., Hadzhiyska, B., Hahn, C., Hanif, M. M. S, Herrera-Alcantar, H. K., Honscheid, K., Hou, J., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Juneau, S., Karaçaylı, N. G., Kehoe, R., Kent, S., Kirkby, D., Kitaura, F. -S., Kong, H., Kremin, A., Krolewski, A., Lai, Y., Lan, T. -W., Landriau, M., Lang, D., Lasker, J., Goff, J. M. Le, Guillou, L. Le, Leauthaud, A., Levi, M. E., Li, T. S., Lodha, K., Magneville, C., Manera, M., Margala, D., Martini, P., Maus, M., McDonald, P., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Miquel, R., Moon, J., Moore, S., Moustakas, J., Mudur, N., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Napolitano, L., Neveux, R., Newman, J. A., Nguyen, N. M., Nie, J., Niz, G., Noriega, H. E., Padmanabhan, N., Paillas, E., Palanque-Delabrouille, N., Pan, J., Penmetsa, S., Percival, W. J., Pieri, M. M., Pinon, M., Poppett, C., Porredon, A., Prada, F., Pérez-Fernández, A., Pérez-Ràfols, I., Rabinowitz, D., Raichoor, A., Ramírez-Pérez, C., Ramirez-Solano, S., Rashkovetskyi, M., Ravoux, C., Rezaie, M., Rich, J., Rocher, A., Rockosi, C., Roe, N. A., Rosado-Marin, A., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Samushia, L., Sanchez, E., Saulder, C., Schlafly, E. F., Schlegel, D., Scholte, D., Schubnell, M., Seo, H., Sharples, R., Silber, J., Slosar, A., Smith, A., Sprayberry, D., Tan, T., Tarlé, G., Trusov, S., Vaisakh, R., Valcin, D., Valdes, F., Vargas-Magaña, M., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, N., Wechsler, R. H., Weinberg, D. H., White, M., Wilson, M. J., Yu, J., Yu, Y., Yuan, S., Yèche, C., Zaborowski, E. A., Zarrouk, P., Zhang, H., Zhao, C., Zhao, R., Zhou, R., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the samples of galaxies and quasars used for DESI 2024 cosmological analyses, drawn from the DESI Data Release 1 (DR1). We describe the construction of large-scale structure (LSS) catalogs from these samples, which include matched sets of synthetic reference `randoms' and weights that account for variations in the observed density of the samples due to experimental design and varying instrument performance. We detail how we correct for variations in observational completeness, the input `target' densities due to imaging systematics, and the ability to confidently measure redshifts from DESI spectra. We then summarize how remaining uncertainties in the corrections can be translated to systematic uncertainties for particular analyses. We describe the weights added to maximize the signal-to-noise of DESI DR1 2-point clustering measurements. We detail measurement pipelines applied to the LSS catalogs that obtain 2-point clustering measurements in configuration and Fourier space. The resulting 2-point measurements depend on window functions and normalization constraints particular to each sample, and we present the corrections required to match models to the data. We compare the configuration- and Fourier-space 2-point clustering of the data samples to that recovered from simulations of DESI DR1 and find they are, generally, in statistical agreement to within 2\% in the inferred real-space over-density field. The LSS catalogs, 2-point measurements, and their covariance matrices will be released publicly with DESI DR1., Comment: This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers/)
Published: 2024

17. DESI 2024 V: Full-Shape Galaxy Clustering from Galaxies and Quasars

Author: DESI Collaboration, Adame, A. G., Aguilar, J., Ahlen, S., Alam, S., Alexander, D. M., Alvarez, M., Alves, O., Anand, A., Andrade, U., Armengaud, E., Avila, S., Aviles, A., Awan, H., Bailey, S., Baltay, C., Bault, A., Behera, J., BenZvi, S., Beutler, F., Bianchi, D., Blake, C., Blum, R., Brieden, S., Brodzeller, A., Brooks, D., Buckley-Geer, E., Burtin, E., Calderon, R., Canning, R., Rosell, A. Carnero, Cereskaite, R., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Chen, S., Chen, X., Claybaugh, T., Cole, S., Cuceu, A., Davis, T. M., Dawson, K., de la Macorra, A., de Mattia, A., Deiosso, N., Dey, A., Dey, B., Ding, Z., Doel, P., Edelstein, J., Eftekharzadeh, S., Eisenstein, D. J., Elliott, A., Fagrelius, P., Fanning, K., Ferraro, S., Ereza, J., Findlay, N., Flaugher, B., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Garcia-Quintero, C., Garrison, L. H., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gonzalez-Perez, V., Gordon, C., Green, D., Gruen, D., Gsponer, R., Gutierrez, G., Guy, J., Hadzhiyska, B., Hahn, C., Hanif, M. M. S, Herrera-Alcantar, H. K., Honscheid, K., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Juneau, S., Karaçaylı, N. G., Kehoe, R., Kent, S., Kirkby, D., Kong, H., Koposov, S. E., Kremin, A., Krolewski, A., Lai, Y., Lan, T. -W., Landriau, M., Lang, D., Lasker, J., Goff, J. M. Le, Guillou, L. Le, Leauthaud, A., Levi, M. E., Li, T. S., Lodha, K., Magneville, C., Manera, M., Margala, D., Martini, P., Maus, M., McDonald, P., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Miquel, R., Moon, J., Moore, S., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Napolitano, L., Neveux, R., Newman, J. A., Nguyen, N. M., Nie, J., Niz, G., Noriega, H. E., Padmanabhan, N., Paillas, E., Palanque-Delabrouille, N., Pan, J., Penmetsa, S., Percival, W. J., Pieri, M. M., Pinon, M., Poppett, C., Porredon, A., Prada, F., Pérez-Fernández, A., Pérez-Ràfols, I., Rabinowitz, D., Raichoor, A., Ramírez-Pérez, C., Ramirez-Solano, S., Rashkovetskyi, M., Ravoux, C., Rezaie, M., Rich, J., Rocher, A., Rockosi, C., Rodríguez-Martínez, F., Roe, N. A., Rosado-Marin, A., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Samushia, L., Sanchez, E., Saulder, C., Schlafly, E. F., Schlegel, D., Schubnell, M., Seo, H., Sharples, R., Silber, J., Slosar, A., Smith, A., Sprayberry, D., Tan, T., Tarlé, G., Trusov, S., Vaisakh, R., Valcin, D., Valdes, F., Vargas-Magaña, M., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, N., Wechsler, R. H., Weinberg, D. H., White, M., Wilson, M. J., Yu, J., Yu, Y., Yuan, S., Yèche, C., Zaborowski, E. A., Zarrouk, P., Zhang, H., Zhao, C., Zhao, R., Zhou, R., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the measurements and cosmological implications of the galaxy two-point clustering using over 4.7 million unique galaxy and quasar redshifts in the range $0.1
Published: 2024

18. Analysis of DESI×DES using the Lagrangian effective theory of LSS

Author: Chen, S, DeRose, J, Zhou, R, White, M, Ferraro, S, Blake, C, Lange, JU, Wechsler, RH, Aguilar, J, Ahlen, S, Brooks, D, Claybaugh, T, Dawson, K, de la Macorra, A, Doel, P, Font-Ribera, A, Gaztañaga, E, Gontcho, S Gontcho A, Gutierrez, G, Honscheid, K, Howlett, C, Kehoe, R, Kirkby, D, Kisner, T, Kremin, A, Landriau, M, Le Guillou, L, Manera, M, Meisner, A, Miquel, R, Newman, JA, Niz, G, Palanque-Delabrouille, N, Percival, WJ, Prada, F, Rossi, G, Sanchez, E, Schlegel, D, Schubnell, M, Sprayberry, D, Tarlé, G, and Weaver, BA
Subjects: Nuclear and Plasma Physics, Physical Sciences
Abstract: In this work we use Lagrangian perturbation theory to analyze the harmonic space galaxy clustering signal of the Bright Galaxy Survey (BGS) and luminous red galaxies (LRGs) targeted by the dark energy spectroscopic instrument (DESI), combined with the galaxy-galaxy lensing signal measured around these galaxies using Dark Energy Survey Year 3 source galaxies. The BGS and LRG galaxies are extremely well characterized by DESI spectroscopy and, as a result, lens galaxy redshift uncertainty and photometric systematics contribute negligibly to the error budget of our "2×2-point"analysis. On the modeling side, this work represents the first application of the spinosaurus code, implementing an effective field theory model for galaxy intrinsic alignments, and we additionally introduce a new scheme (maiar) for marginalizing over the large uncertainties in the redshift evolution of the intrinsic alignment signal. Furthermore, this is the first application of a hybrid effective field theory model for galaxy bias based on the aemulus ν simulations. Our main result is a measurement of the amplitude of the lensing signal, S8=σ8(ωm/0.3)0.5=0.850-0.050+0.042, consistent with values of this parameter derived from the primary cosmic microwave background. This constraint is artificially improved by a factor of 51% if we assume a more standard, but restrictive parametrization for the redshift evolution and sample dependence of the intrinsic alignment signal, and 63% if we additionally assume the nonlinear alignment model. We show that when fixing the cosmological model to the best-fit values from Planck PR4 there is >5σ evidence for a deviation of the evolution of the intrinsic alignment signal from the functional form that is usually assumed in cosmic shear and galaxy-galaxy lensing studies.
Published: 2024

19. ForestFlow: predicting the Lyman-$\alpha$ forest clustering from linear to nonlinear scales

Author: Chaves-Montero, J., Cabayol-Garcia, L., Lokken, M., Font-Ribera, A., Aguilar, J., Ahlen, S., Bianchi, D., Brooks, D., Claybaugh, T., Cole, S., de la Macorra, A., Ferraro, S., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Gutierrez, G., Honscheid, K., Kehoe, R., Kirkby, D., Kremin, A., Lambert, A., Landriau, M., Manera, M., Martini, P., Miquel, R., Muñoz-Gutiérrez, A., Niz, G., Pérez-Ràfols, I., Rossi, G., Sanchez, E., Schubnell, M., Sprayberry, D., Tarlé, G., and Weaver, B. A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: On large scales, the Lyman-$\alpha$ forest provides insights into the expansion history of the Universe, while on small scales, it imposes strict constraints on the growth history, the nature of dark matter, and the sum of neutrino masses. This work introduces ForestFlow, a novel framework that bridges the gap between large- and small-scale analyses, which have traditionally relied on distinct modeling approaches. Using conditional normalizing flows, ForestFlow predicts the two Lyman-$\alpha$ linear biases ($b_\delta$ and $b_\eta$) and six parameters describing small-scale deviations of the three-dimensional flux power spectrum ($P_\mathrm{3D}$) from linear theory as a function of cosmology and intergalactic medium physics. These are then combined with a Boltzmann solver to make consistent predictions, from arbitrarily large scales down to the nonlinear regime, for $P_\mathrm{3D}$ and any other statistics derived from it. Trained on a suite of 30 fixed-and-paired cosmological hydrodynamical simulations spanning redshifts from $z=2$ to 4.5, ForestFlow achieves 3 and 1.5\% precision in describing $P_\mathrm{3D}$ and the one-dimensional flux power spectrum ($P_\mathrm{1D}$) from linear scales to $k=5\,\mathrm{Mpc}^{-1}$ and $k_\parallel=4\,\mathrm{Mpc}^{-1}$, respectively. Thanks to its conditional parameterization, ForestFlow shows similar performance for ionization histories and two $\Lambda$CDM model extensions $\unicode{x2013}$ massive neutrinos and curvature $\unicode{x2013}$ even though none of these are included in the training set. This framework will enable full-scale cosmological analyses of Lyman-$\alpha$ forest measurements from the DESI survey., Comment: 18 pages, 12 figures. Accepted in A&A
Published: 2024
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20. Tracing the evolution of the cool gas in CGM and IGM environments through Mg II absorption from redshift z=0.75 to z=1.65 using DESI-Y1 data

Author: Wu, X., Cai, Z., Lan, T. -W., Zou, S., Anand, A., Dey, Biprateep, Li, Z., Aguilar, J., Ahlen, S., Brooks, D., Claybaugh, T., de la Macorra, A., Doel, P., Ferraro, S., Forero-Romero, J. E., Gontcho, S. Gontcho A, Honscheid, K., Juneau, S., Kehoe, R., Kisner, T., Lambert, A., Landriau, M., Guillou, L. Le, Manera, M., Meisner, A., Miquel, R., Moustakas, J., Newman, J. A., Prada, F., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Siudek, M., Sprayberry, D., Tarlé, G., Weaver, B. A., and Zou, H.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present a measurement of the mean absorption of cool gas traced by Mg II (${\lambda\lambda 2796, 2803}$) around emission line galaxies (ELGs), spanning spatial scales from 20 kpc to 10 Mpc. The measurement is based on cross-matching the positions of about 2.5 million ELGs at $z = 0.75-1.65$ and the metal absorption in the spectra of 1.4 million background quasars with data provided by the Year 1 sample of the Dark Energy Spectroscopic Instrument (DESI). The ELGs are divided into two redshift intervals: $0.75 < z < 1.0$ and $1.0 < z < 1.65$. We find that the composite spectra constructed by stacking the ELG-QSO pairs show evolution with redshift, with $z>1$ having a systematically higher signal of Mg II absorption. Within 1 Mpc, the covering fraction of the cool gas at $z > 1$ is higher than that of $z < 1$. The enhancement becomes less apparent especially if the projected distance $r_{p}>$1 Mpc. Also, ELGs with higher stellar mass and star formation rate (SFR) yield higher clustering of Mg II absorbers at $z<1$. For $z>1$, the covering fractions with different SFRs show little difference. The higher Mg II absorption at higher redshift also supports the observations of higher star formation at cosmic noon. Besides, the profile of Mg II absorption reveals a change of slope on scales of about 1 Mpc, consistent with the expected transition from a dark matter halo-dominated environment to a regime where clustering is dominated by halo-halo correlations. We estimate the cool gas density profile and derive the metal abundance at different redshifts. The growth of metal abundance suggests an increased presence of cool gas in the intergalactic medium (IGM) towards higher redshifts.
Published: 2024

21. Evidence for large baryonic feedback at low and intermediate redshifts from kinematic Sunyaev-Zel'dovich observations with ACT and DESI photometric galaxies

Author: Hadzhiyska, B., Ferraro, S., Guachalla, B. Ried, Schaan, E., Aguilar, J., Battaglia, N., Bond, J. R., Brooks, D., Calabrese, E., Choi, S. K., Claybaugh, T., Coulton, W. R., Dawson, K., Devlin, M., Dey, B., Doel, P., Duivenvoorden, A. J., Dunkley, J., Farren, G. S., Font-Ribera, A., Forero-Romero, J. E., Gallardo, P. A., Gaztañaga, E., Gontcho, S. Gontcho, Gralla, M., Guillou, L. Le, Gutierrez, G., Guy, J., Hill, J. C., Hložek, R., Honscheid, K., Juneau, S., Kisner, T., Kremin, A., Landriau, M., Liu, R. H., Louis, T., MacCrann, N., de Macorra, A., Madhavacheril, M., Manera, M., Meisner, A., Miquel, R., Moodley, K., Moustakas, J., Mroczkowski, T., Naess, S., Newman, J., Niemack, M. D., Niz, G., Page, L., Palanque-Delabrouille, N., Partridge, B., Percival, W. J., Prada, F., Qu, F. J., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Sehgal, N., Seo, H., Sifón, C., Spergel, D., Sprayberry, D., Staggs, S., Tarlé, G., Vargas, C., Vavagiakis, E. M., Weaver, B. A., Wollack, E. J., Zhou, R., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: Recent advances in cosmological observations have provided an unprecedented opportunity to investigate the distribution of baryons relative to the underlying matter. In this work, we robustly show that the gas is much more extended than the dark matter at 40$\sigma$ and the amount of baryonic feedback at $z \lesssim 1$ strongly disfavors low-feedback models such as that of state-of-the-art hydrodynamical simulation IllustrisTNG compared with high-feedback models such as that of the original Illustris simulation. This has important implications for bridging the gap between theory and observations and understanding galaxy formation and evolution. Furthermore, a better grasp of the baryon-dark matter link is critical to future cosmological analyses, which are currently impeded by our limited knowledge of baryonic feedback. Here, we measure the kinematic Sunyaev-Zel'dovich (kSZ) effect from the Atacama Cosmology Telescope (ACT), stacked on the luminous red galaxy (LRG) sample of the Dark Energy Spectroscopic Instrument (DESI) imaging survey. This is the first analysis to use photometric redshifts for reconstructing galaxy velocities. Due to the large number of galaxies comprising the DESI imaging survey, this is the highest signal-to-noise stacked kSZ measurement to date: we detect the signal at 13$\sigma$ and find that the gas is more spread out than the dark matter at $\sim$40$\sigma$. Our work opens up the possibility to recalibrate large hydrodynamical simulations using the kSZ effect. In addition, our findings point towards a way of alleviating inconsistencies between weak lensing surveys and cosmic microwave background (CMB) experiments such as the `low $S_8$' tension, and shed light on long-standing enigmas in astrophysics such as the `missing baryon' problem., Comment: 20 pages, 8 figures, submitting to PRL
Published: 2024

22. Not all lensing is low: An analysis of DESI$\times$DES using the Lagrangian Effective Theory of LSS

Author: Chen, S., DeRose, J., Zhou, R., White, M., Ferraro, S., Blake, C., Lange, J. U., Wechsler, R. H., Aguilar, J., Ahlen, S., Brooks, D., Claybaugh, T., Dawson, K., de la Macorra, A., Doel, P., Font-Ribera, A., Gaztañaga, E., Gontcho, S. Gontcho A, Gutierrez, G., Honscheid, K., Howlett, C., Kehoe, R., Kirkby, D., Kisner, T., Kremin, A., Landriau, M., Guillou, L. Le, Manera, M., Meisner, A., Miquel, R., Newman, J. A., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Prada, F., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Sprayberry, D., Tarlé, G., and Weaver, B. A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: In this work we use Lagrangian perturbation theory to analyze the harmonic space galaxy clustering signal of Bright Galaxy Survey (BGS) and Luminous Red Galaxies (LRGs) targeted by the Dark Energy Spectroscopic Instrument (DESI), combined with the galaxy--galaxy lensing signal measured around these galaxies using Dark Energy Survey Year 3 source galaxies. The BGS and LRG galaxies are extremely well characterized by DESI spectroscopy and, as a result, lens galaxy redshift uncertainty and photometric systematics contribute negligibly to the error budget of our ``$2\times2$-point'' analysis. On the modeling side, this work represents the first application of the \texttt{spinosaurus} code, implementing an effective field theory model for galaxy intrinsic alignments, and we additionally introduce a new scheme (\texttt{MAIAR}) for marginalizing over the large uncertainties in the redshift evolution of the intrinsic alignment signal. Furthermore, this is the first application of a hybrid effective field theory (HEFT) model for galaxy bias based on the $\texttt{Aemulus}\, \nu$ simulations. Our main result is a measurement of the amplitude of the lensing signal, $S_8=\sigma_8 \left(\Omega_m/0.3\right)^{0.5} = 0.850^{+0.042}_{-0.050}$, consistent with values of this parameter derived from the primary CMB. This constraint is artificially improved by a factor of $51\%$ if we assume a more standard, but restrictive parameterization for the redshift evolution and sample dependence of the intrinsic alignment signal, and $63\%$ if we additionally assume the nonlinear alignment model. We show that when fixing the cosmological model to the best-fit values from Planck PR4 there is $> 5 \sigma$ evidence for a deviation of the evolution of the intrinsic alignment signal from the functional form that is usually assumed in cosmic shear and galaxy--galaxy lensing studies., Comment: 53 pages, 25 figures, updated to match version accepted by PRD
Published: 2024

23. The Construction of Large-scale Structure Catalogs for the Dark Energy Spectroscopic Instrument

Author: Ross, A. J., Aguilar, J., Ahlen, S., Alam, S., Anand, A., Bailey, S., Bianchi, D., Brieden, S., Brooks, D., Burtin, E., Rosell, A. Carnero, Chaussidon, E., Claybaugh, T., Cole, S., Dawson, K., de la Macorra, A., de Mattia, A., Dey, Arjun, Dey, Biprateep, Doel, P., Fanning, K., Ferraro, S., Ereza, J., Font-Ribera, A., Forero-Romero, J. E., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Guy, J., Hahn, C., Heydenreich, S., Honscheid, K., Howlett, C., Ishak, M., Karim, T., Kirkby, D., Kisner, T., Kong, H., Kremin, A., Krolewski, A., Lambert, A., Landriau, M., Lasker, J., Guillou, L. Le, Levi, M. E., Manera, M., Martini, P., McDonald, P., Meisner, A., Miquel, R., Moon, J., Moustakas, J., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Napolitano, L., Newman, J. A., Nie, J., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Raichoor, A., Ravoux, C., Rezaie, M., Rosado-Marin, A., Rossi, G., Samushia, L., Sanchez, E., Schlafly, E. F., Schlegel, D., Seo, H., Smith, A., Sprayberry, D., Tarlé, G., Valcin, D., Vargas-Magaña, M., Weaver, B. A., Wilson, M., Yu, J., Zarrouk, P., Zhao, C., Zhou, R., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the technical details on how large-scale structure (LSS) catalogs are constructed from redshifts measured from spectra observed by the Dark Energy Spectroscopic Instrument (DESI). The LSS catalogs provide the information needed to determine the relative number density of DESI tracers as a function of redshift and celestial coordinates and, e.g., determine clustering statistics. We produce catalogs that are weighted subsamples of the observed data, each matched to a weighted `random' catalog that forms an unclustered sampling of the probability density that DESI could have observed those data at each location. Precise knowledge of the DESI observing history and associated hardware performance allows for a determination of the DESI footprint and the number of times DESI has covered it at sub-arcsecond level precision. This enables the completeness of any DESI sample to be modeled at this same resolution. The pipeline developed to create LSS catalogs has been designed to easily allow robustness tests and enable future improvements. We describe how it allows ongoing work improving the match between galaxy and random catalogs, such as including further information when assigning redshifts to randoms, accounting for fluctuations in target density, accounting for variation in the redshift success rate, and accommodating blinding schemes., Comment: Accepted (by JCAP) version of supporting publication of DESI 2024II: Sample definitions, characteristics, and two-point clustering statistics
Published: 2024

24. CMB lensing and Ly\alpha\ forest cross bispectrum from DESI's first-year quasar sample

Author: Karaçaylı, N. G., Martini, P., Weinberg, D. H., Ferraro, S., de Belsunce, R., Aguilar, J., Ahlen, S., Armengaud, E., Brooks, D., Claybaugh, T., de la Macorra, A., Dey, B., Doel, P., Fanning, K., Forero-Romero, J. E., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gutierrez, G., Guy, J., Honscheid, K., Kirkby, D., Kisner, T., Kremin, A., Lambert, A., Landriau, M., Guillou, L. Le, Levi, M. E., Manera, M., Meisner, A., Miquel, R., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Newman, J. A., Nie, J., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Ravoux, C., Rezaie, M., Ross, A. J., Rossi, G., Sanchez, E., Schlafly, E. F., Schlegel, D., Seo, H., Sprayberry, D., Tan, T., Tarlé, G., Weaver, B. A., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The squeezed cross-bispectrum \bispeconed\ between the gravitational lensing in the Cosmic Microwave Background and the 1D \lya\ forest power spectrum can constrain bias parameters and break degeneracies between $\sigma_8$ and other cosmological parameters. We detect \bispeconed\ with $4.8\sigma$ significance at an effective redshift $z_\mathrm{eff}=2.4$ using Planck PR3 lensing map and over 280,000 quasar spectra from the Dark Energy Spectroscopic Instrument's first-year data. We test our measurement against metal contamination and foregrounds such as Galactic extinction and clusters of galaxies by deprojecting the thermal Sunyaev-Zeldovich effect. We compare our results to a tree-level perturbation theory calculation and find reasonable agreement between the model and measurement., Comment: 13 pages excluding references, 8 figures
Published: 2024

25. Systematic Effects in Galaxy-Galaxy Lensing with DESI

Author: Lange, J. U., Blake, C., Saulder, C., Jeffrey, N., DeRose, J., Beltz-Mohrmann, G., Emas, N., Garcia-Quintero, C., Hadzhiyska, B., Heydenreich, S., Ishak, M., Joudaki, S., Jullo, E., Krolewski, A., Leauthaud, A., Medina-Varela, L., Porredon, A., Rossi, G., Ruggeri, R., Xhakaj, E., Yuan, S., Aguilar, J., Ahlen, S., Brooks, D., Claybaugh, T., de la Macorra, A., Doel, P., Fanning, K., Ferraro, S., Font-Ribera, A., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Juneau, S., Kehoe, R., Kisner, T., Kremin, A., Landriau, M., Levi, M. E., Manera, M., Miquel, R., Moustakas, J., Mueller, E., Myers, A. D., Nie, J., Niz, G., Palanque-Delabrouille, N., Poppett, C., Rezaie, M., Sanchez, E., Schubnell, M., Seo, H., Silber, J., Sprayberry, D., Tarlé, G., Vargas-Magaña, M., Wechsler, R. H., Zhou, Z., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Dark Energy Spectroscopic Instrument (DESI) survey will measure spectroscopic redshifts for millions of galaxies across roughly $14,000 \, \mathrm{deg}^2$ of the sky. Cross-correlating targets in the DESI survey with complementary imaging surveys allows us to measure and analyze shear distortions caused by gravitational lensing in unprecedented detail. In this work, we analyze a series of mock catalogs with ray-traced gravitational lensing and increasing sophistication to estimate systematic effects on galaxy-galaxy lensing estimators such as the tangential shear $\gamma_{\mathrm{t}}$ and the excess surface density $\Delta\Sigma$. We employ mock catalogs tailored to the specific imaging surveys overlapping with the DESI survey: the Dark Energy Survey (DES), the Hyper Suprime-Cam (HSC) survey, and the Kilo-Degree Survey (KiDS). Among others, we find that fiber incompleteness can have significant effects on galaxy-galaxy lensing estimators but can be corrected effectively by up-weighting DESI targets with fibers by the inverse of the fiber assignment probability. Similarly, we show that intrinsic alignment and lens magnification are expected to be statistically significant given the precision forecasted for the DESI year-1 data set. Our study informs several analysis choices for upcoming cross-correlation studies of DESI with DES, HSC, and KiDS., Comment: 18 pages, 13 figures, version accepted for publication
Published: 2024
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26. An analysis of parameter compression and full-modeling techniques with Velocileptors for DESI 2024 and beyond

Author: Maus, M., Chen, S., White, M., Aguilar, J., Ahlen, S., Aviles, A., Brieden, S., Brooks, D., Claybaugh, T., Cole, S., de la Macorra, A., Dey, Arjun, Doel, P., Ferraro, S., Findlay, N., Forero-Romero, J. E., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Hahn, C., Honscheid, K., Howlett, C., Ishak, M., Juneau, S., Kremin, A., Lai, Y., Landriau, M., Levi, M. E., Manera, M., Miquel, R., Mueller, E., Myers, A. D., Nadathur, S., Nie, J., Noriega, H. E., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Ramirez-Solano, S., Rezaie, M., Rocher, A., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Seo, H., Sprayberry, D., Tarlé, G., Vargas-Magaña, M., Weaver, B. A., Yuan, S., Zarrouk, P., Zhang, H., Zhou, R., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: In anticipation of forthcoming data releases of current and future spectroscopic surveys, we present the validation tests and analysis of systematic effects within \texttt{velocileptors} modeling pipeline when fitting mock data from the \texttt{AbacusSummit} N-body simulations. We compare the constraints obtained from parameter compression methods to the direct fitting (Full-Modeling) approaches of modeling the galaxy power spectra, and show that the ShapeFit extension to the traditional template method is consistent with the Full-Modeling method within the standard $\Lambda$CDM parameter space. We show the dependence on scale cuts when fitting the different redshift bins using the ShapeFit and Full-Modeling methods. We test the ability to jointly fit data from multiple redshift bins as well as joint analysis of the pre-reconstruction power spectrum with the post-reconstruction BAO correlation function signal. We further demonstrate the behavior of the model when opening up the parameter space beyond $\Lambda$CDM and also when combining likelihoods with external datasets, namely the Planck CMB priors. Finally, we describe different parametrization options for the galaxy bias, counterterm, and stochastic parameters, and employ the halo model in order to physically motivate suitable priors that are necessary to ensure the stability of the perturbation theory., Comment: 56 pages, 23 figures. Supporting publication of DESI 2024 V: Analysis of the full shape of two-point clustering statistics from galaxies and quasars
Published: 2024

27. A comparison of effective field theory models of redshift space galaxy power spectra for DESI 2024 and future surveys

Author: Maus, M., Lai, Y., Noriega, H. E., Ramirez-Solano, S., Aviles, A., Chen, S., Fromenteau, S., Gil-Marín, H., Howlett, C., Vargas-Magaña, M., White, M., Zarrouk, P., Aguilar, J., Ahlen, S., Alves, O., Brieden, S., Brooks, D., Burtin, E., Claybaugh, T., Cole, S., Dawson, K., Icaza-Lizaola, M., de la Macorra, A., de Mattia, A., Doel, P., Ferraro, S., Findlay, N., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Hahn, C., Honscheid, K., Ishak, M., Kremin, A., Landriau, M., Guillou, L. Le, Manera, M., Miquel, R., Mueller, E., Nadathur, S., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Rezaie, M., Rocher, A., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Sprayberry, D., Tarlé, G., Yuan, S., Zhao, R., Zhou, R., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: In preparation for the next generation of galaxy redshift surveys, and in particular the year-one data release from the Dark Energy Spectroscopic Instrument (DESI), we investigate the consistency of a variety of effective field theory models that describe the galaxy-galaxy power spectra in redshift space into the quasi-linear regime using 1-loop perturbation theory. These models are employed in the pipelines \texttt{velocileptors}, \texttt{PyBird}, and \texttt{Folps$\nu$}. While these models have been validated independently, a detailed comparison with consistent choices has not been attempted. After briefly discussing the theoretical differences between the models we describe how to provide a more apples-to-apples comparison between them. We present the results of fitting mock spectra from the \texttt{AbacusSummit} suite of N-body simulations provided in three redshift bins to mimic the types of dark time tracers targeted by the DESI survey. We show that the theories behave similarly and give consistent constraints in both the forward-modeling and ShapeFit compressed fitting approaches. We additionally generate (noiseless) synthetic data from each pipeline to be fit by the others, varying the scale cuts in order to show that the models agree within the range of scales for which we expect 1-loop perturbation theory to be applicable. This work lays the foundation of Full-Shape analysis with DESI Y1 galaxy samples where in the tests we performed, we found no systematic error associated with the modeling of the galaxy redshift space power spectrum for this volume., Comment: 33 pages, 12 figures. Supporting publication of DESI 2024 V: Analysis of the full shape of two-point clustering statistics from galaxies and quasars
Published: 2024

28. Weak lensing combined with the kinetic Sunyaev Zel'dovich effect: A study of baryonic feedback

Author: Bigwood, L., Amon, A., Schneider, A., Salcido, J., McCarthy, I. G., Preston, C., Sanchez, D., Sijacki, D., Schaan, E., Ferraro, S., Battaglia, N., Chen, A., Dodelson, S., Roodman, A., Pieres, A., Ferte, A., Alarcon, A., Drlica-Wagner, A., Choi, A., Navarro-Alsina, A., Campos, A., Ross, A. J., Rosell, A. Carnero, Yin, B., Yanny, B., Sanchez, C., Chang, C., Davis, C., Doux, C., Gruen, D., Rykoff, E. S., Huff, E. M., Sheldon, E., Tarsitano, F., Andrade-Oliveira, F., Bernstein, G. M., Giannini, G., Diehl, H. T., Huang, H., Harrison, I., Sevilla-Noarbe, I., Tutusaus, I., Elvin-Poole, J., McCullough, J., Zuntz, J., Blazek, J., DeRose, J., Cordero, J., Prat, J., Myles, J., Eckert, K., Bechtol, K., Herner, K., Secco, L. F., Gatti, M., Raveri, M., Kind, M. Carrasco, Becker, M. R., Troxel, M. A., Jarvis, M., MacCrann, N., Friedrich, O., Alves, O., Leget, P. -F., Chen, R., Rollins, R. P., Wechsler, R. H., Gruendl, R. A., Cawthon, R., Allam, S., Bridle, S. L., Pandey, S., Everett, S., Shin, T., Hartley, W. G., Fang, X., Zhang, Y., Aguena, M., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Carretero, J., Castander, F. J., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kuehn, K., Lahav, O., Lee, S., Marshall, J. L., Mena-Fernandez, J., Miquel, R., Muir, J., Paterno, M., Malagon, A. A. Plazas, Porredon, A., Romer, A. K., Samuroff, S., Sanchez, E., Cid, D. Sanchez, Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Weaverdyck, N., Weller, J., Wiseman, P., and Yamamoto, M.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: Extracting precise cosmology from weak lensing surveys requires modelling the non-linear matter power spectrum, which is suppressed at small scales due to baryonic feedback processes. However, hydrodynamical galaxy formation simulations make widely varying predictions for the amplitude and extent of this effect. We use measurements of Dark Energy Survey Year 3 weak lensing (WL) and Atacama Cosmology Telescope DR5 kinematic Sunyaev-Zel'dovich (kSZ) to jointly constrain cosmological and astrophysical baryonic feedback parameters using a flexible analytical model, `baryonification'. First, using WL only, we compare the $S_8$ constraints using baryonification to a simulation-calibrated halo model, a simulation-based emulator model and the approach of discarding WL measurements on small angular scales. We find that model flexibility can shift the value of $S_8$ and degrade the uncertainty. The kSZ provides additional constraints on the astrophysical parameters and shifts $S_8$ to $S_8=0.823^{+0.019}_{-0.020}$, a higher value than attained using the WL-only analysis. We measure the suppression of the non-linear matter power spectrum using WL + kSZ and constrain a mean feedback scenario that is more extreme than the predictions from most hydrodynamical simulations. We constrain the baryon fractions and the gas mass fractions and find them to be generally lower than inferred from X-ray observations and simulation predictions. We conclude that the WL + kSZ measurements provide a new and complementary benchmark for building a coherent picture of the impact of gas around galaxies across observations.
Published: 2024

29. Semi-analytical covariance matrices for two-point correlation function for DESI 2024 data

Author: Rashkovetskyi, M., Forero-Sánchez, D., de Mattia, A., Eisenstein, D. J., Padmanabhan, N., Seo, H., Ross, A. J., Aguilar, J., Ahlen, S., Alves, O., Andrade, U., Brooks, D., Burtin, E., Chen, X., Claybaugh, T., Cole, S., de la Macorra, A., Ding, Z., Doel, P., Fanning, K., Ferraro, S., Font-Ribera, A., Forero-Romero, J. E., Garcia-Quintero, C., Gil-Marín, H., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gutierrez, G., Honscheid, K., Howlett, C., Juneau, S., Kremin, A., Guillou, L. Le, Manera, M., Medina-Varela, L., Mena-Fernández, J., Miquel, R., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Nie, J., Niz, G., Paillas, E., Percival, W. J., Poppett, C., Pérez-Fernández, A., Rezaie, M., Rosado-Marin, A., Rossi, G., Ruggeri, R., Sanchez, E., Saulder, C., Schlegel, D., Schubnell, M., Sprayberry, D., Tarlé, G., Weaver, B. A., Yu, J., Zhao, C., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Physics - Data Analysis, Statistics and Probability
Abstract: We present an optimized way of producing the fast semi-analytical covariance matrices for the Legendre moments of the two-point correlation function, taking into account survey geometry and mimicking the non-Gaussian effects. We validate the approach on simulated (mock) catalogs for different galaxy types, representative of the Dark Energy Spectroscopic Instrument (DESI) Data Release 1, used in 2024 analyses. We find only a few percent differences between the mock sample covariance matrix and our results, which can be expected given the approximate nature of the mocks, although we do identify discrepancies between the shot-noise properties of the DESI fiber assignment algorithm and the faster approximation (emulator) used in the mocks. Importantly, we find a close agreement (<=8% relative differences) in the projected errorbars for distance scale parameters for the baryon acoustic oscillation measurements. This confirms our method as an attractive alternative to simulation-based covariance matrices, especially for non-standard models or galaxy sample selections, making it particularly relevant to the broad current and future analyses of DESI data., Comment: This DESI Publication is part of the 2024 series using the first year of observations (see https://data.desi.lbl.gov/doc/papers/). 41 pages, 4 figures. Major rewrite after v2. Accepted to JCAP. Code available at https://github.com/oliverphilcox/RascalC and https://github.com/cosmodesi/RascalC-scripts/tree/DESI2024. Figure and table data available at https://zenodo.org/doi/10.5281/zenodo.10895161
Published: 2024
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30. DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations

Author: DESI Collaboration, Adame, A. G., Aguilar, J., Ahlen, S., Alam, S., Alexander, D. M., Alvarez, M., Alves, O., Anand, A., Andrade, U., Armengaud, E., Avila, S., Aviles, A., Awan, H., Bahr-Kalus, B., Bailey, S., Baltay, C., Bault, A., Behera, J., BenZvi, S., Bera, A., Beutler, F., Bianchi, D., Blake, C., Blum, R., Brieden, S., Brodzeller, A., Brooks, D., Buckley-Geer, E., Burtin, E., Calderon, R., Canning, R., Rosell, A. Carnero, Cereskaite, R., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Chen, S., Chen, X., Claybaugh, T., Cole, S., Cuceu, A., Davis, T. M., Dawson, K., de la Macorra, A., de Mattia, A., Deiosso, N., Dey, A., Dey, B., Ding, Z., Doel, P., Edelstein, J., Eftekharzadeh, S., Eisenstein, D. J., Elliott, A., Fagrelius, P., Fanning, K., Ferraro, S., Ereza, J., Findlay, N., Flaugher, B., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Frenk, C. S., Garcia-Quintero, C., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gonzalez-Perez, V., Gordon, C., Green, D., Gruen, D., Gsponer, R., Gutierrez, G., Guy, J., Hadzhiyska, B., Hahn, C., Hanif, M. M. S, Herrera-Alcantar, H. K., Honscheid, K., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Juneau, S., Karaçaylı, N. G., Kehoe, R., Kent, S., Kirkby, D., Kremin, A., Krolewski, A., Lai, Y., Lan, T. -W., Landriau, M., Lang, D., Lasker, J., Goff, J. M. Le, Guillou, L. Le, Leauthaud, A., Levi, M. E., Li, T. S., Linder, E., Lodha, K., Magneville, C., Manera, M., Margala, D., Martini, P., Maus, M., McDonald, P., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Miquel, R., Moon, J., Moore, S., Moustakas, J., Mudur, N., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Napolitano, L., Neveux, R., Newman, J. A., Nguyen, N. M., Nie, J., Niz, G., Noriega, H. E., Padmanabhan, N., Paillas, E., Palanque-Delabrouille, N., Pan, J., Penmetsa, S., Percival, W. J., Pieri, M. M., Pinon, M., Poppett, C., Porredon, A., Prada, F., Pérez-Fernández, A., Pérez-Ràfols, I., Rabinowitz, D., Raichoor, A., Ramírez-Pérez, C., Ramirez-Solano, S., Ravoux, C., Rashkovetskyi, M., Rezaie, M., Rich, J., Rocher, A., Rockosi, C., Roe, N. A., Rosado-Marin, A., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Samushia, L., Sanchez, E., Saulder, C., Schlafly, E. F., Schlegel, D., Schubnell, M., Seo, H., Shafieloo, A., Sharples, R., Silber, J., Slosar, A., Smith, A., Sprayberry, D., Tan, T., Tarlé, G., Taylor, P., Trusov, S., Ureña-López, L. A., Vaisakh, R., Valcin, D., Valdes, F., Vargas-Magaña, M., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, N., Wechsler, R. H., Weinberg, D. H., White, M., Yu, J., Yu, Y., Yuan, S., Yèche, C., Zaborowski, E. A., Zarrouk, P., Zhang, H., Zhao, C., Zhao, R., Zhou, R., Zhuang, T., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present cosmological results from the measurement of baryon acoustic oscillations (BAO) in galaxy, quasar and Lyman-$\alpha$ forest tracers from the first year of observations from the Dark Energy Spectroscopic Instrument (DESI), to be released in the DESI Data Release 1. DESI BAO provide robust measurements of the transverse comoving distance and Hubble rate, or their combination, relative to the sound horizon, in seven redshift bins from over 6 million extragalactic objects in the redshift range $0.1-1$ and $w_a<0$. This preference is 2.6$\sigma$ for the DESI+CMB combination, and persists or grows when SN~Ia are added in, giving results discrepant with the $\Lambda$CDM model at the $2.5\sigma$, $3.5\sigma$ or $3.9\sigma$ levels for the addition of Pantheon+, Union3, or DES-SN5YR datasets respectively. For the flat $\Lambda$CDM model with the sum of neutrino mass $\sum m_\nu$ free, combining the DESI and CMB data yields an upper limit $\sum m_\nu < 0.072$ $(0.113)$ eV at 95% confidence for a $\sum m_\nu>0$ $(\sum m_\nu>0.059)$ eV prior. These neutrino-mass constraints are substantially relaxed in models beyond $\Lambda$CDM. [Abridged.], Comment: This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers). 68 pages, 15 figures. Version accepted for publication in JCAP
Published: 2024

31. DESI 2024 IV: Baryon Acoustic Oscillations from the Lyman Alpha Forest

Author: DESI Collaboration, Adame, A. G., Aguilar, J., Ahlen, S., Alam, S., Alexander, D. M., Alvarez, M., Alves, O., Anand, A., Andrade, U., Armengaud, E., Avila, S., Aviles, A., Awan, H., Bailey, S., Baltay, C., Bault, A., Bautista, J., Behera, J., BenZvi, S., Beutler, F., Bianchi, D., Blake, C., Blum, R., Brieden, S., Brodzeller, A., Brooks, D., Buckley-Geer, E., Burtin, E., Calderon, R., Canning, R., Rosell, A. Carnero, Cereskaite, R., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Chen, S., Chen, X., Claybaugh, T., Cole, S., Cuceu, A., Davis, T. M., Dawson, K., de la Cruz, R., de la Macorra, A., de Mattia, A., Deiosso, N., Dey, A., Dey, B., Ding, J., Ding, Z., Doel, P., Edelstein, J., Eftekharzadeh, S., Eisenstein, D. J., Elliott, A., Fagrelius, P., Fanning, K., Ferraro, S., Ereza, J., Findlay, N., Flaugher, B., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Garcia-Quintero, C., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gonzalez-Perez, V., Gordon, C., Green, D., Gruen, D., Gsponer, R., Gutierrez, G., Guy, J., Hadzhiyska, B., Hahn, C., Hanif, M. M. S, Herrera-Alcantar, H. K., Honscheid, K., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Juneau, S., Karaçayli, N. G., Kehoe, R., Kent, S., Kirkby, D., Kremin, A., Krolewski, A., Lai, Y., Lan, T. -W., Landriau, M., Lang, D., Lasker, J., Goff, J. M. Le, Guillou, L. Le, Leauthaud, A., Levi, M. E., Li, T. S., Linder, E., Lodha, K., Magneville, C., Manera, M., Margala, D., Martini, P., Maus, M., McDonald, P., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Miquel, R., Moon, J., Moore, S., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Napolitano, L., Neveux, R., Newman, J. A., Nguyen, N. M., Nie, J., Niz, G., Noriega, H. E., Padmanabhan, N., Paillas, E., Palanque-Delabrouille, N., Pan, J., Penmetsa, S., Percival, W. J., Pieri, M. M., Pinon, M., Poppett, C., Porredon, A., Prada, F., Pérez-Fernández, A., Pérez-Ràfols, I., Rabinowitz, D., Raichoor, A., Ramírez-Pérez, C., Ramirez-Solano, S., Rashkovetskyi, M., Ravoux, C., Rezaie, M., Rich, J., Rocher, A., Rockosi, C., Roe, N. A., Rosado-Marin, A., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Samushia, L., Sanchez, E., Saulder, C., Schlafly, E. F., Schlegel, D., Schubnell, M., Seo, H., Sharples, R., Silber, J., Sinigaglia, F., Slosar, A., Smith, A., Sprayberry, D., Tan, T., Tarlé, G., Trusov, S., Vaisakh, R., Valcin, D., Valdes, F., Vargas-Magaña, M., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, N., Wechsler, R. H., Weinberg, D. H., White, M., Yu, J., Yu, Y., Yuan, S., Yèche, C., Zaborowski, E. A., Zarrouk, P., Zhang, H., Zhao, C., Zhao, R., Zhou, R., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the measurement of Baryon Acoustic Oscillations (BAO) from the Lyman-$\alpha$ (Ly$\alpha$) forest of high-redshift quasars with the first-year dataset of the Dark Energy Spectroscopic Instrument (DESI). Our analysis uses over $420\,000$ Ly$\alpha$ forest spectra and their correlation with the spatial distribution of more than $700\,000$ quasars. An essential facet of this work is the development of a new analysis methodology on a blinded dataset. We conducted rigorous tests using synthetic data to ensure the reliability of our methodology and findings before unblinding. Additionally, we conducted multiple data splits to assess the consistency of the results and scrutinized various analysis approaches to confirm their robustness. For a given value of the sound horizon ($r_d$), we measure the expansion at $z_{\rm eff}=2.33$ with 2\% precision, $H(z_{\rm eff}) = (239.2 \pm 4.8) (147.09~{\rm Mpc} /r_d)$ km/s/Mpc. Similarly, we present a 2.4\% measurement of the transverse comoving distance to the same redshift, $D_M(z_{\rm eff}) = (5.84 \pm 0.14) (r_d/147.09~{\rm Mpc})$ Gpc. Together with other DESI BAO measurements at lower redshifts, these results are used in a companion paper to constrain cosmological parameters., Comment: This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers). Minor changes in v4, version accepted for publication in JCAP
Published: 2024
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32. Optimal Reconstruction of Baryon Acoustic Oscillations for DESI 2024

Author: Paillas, E., Ding, Z., Chen, X., Seo, H., Padmanabhan, N., de Mattia, A., Ross, A. J., Nadathur, S., Howlett, C., Aguilar, J., Ahlen, S., Alves, O., Andrade, U., Brooks, D., Buckley-Geer, E., Burtin, E., Chen, S., Claybaugh, T., Cole, S., Dawson, K., de la Macorra, A., Dey, Arjun, Doel, P., Fanning, K., Ferraro, S., Forero-Romero, J. E., Garcia-Quintero, C., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gutierrez, G., Hahn, C., Hanif, M. M. S, Honscheid, K., Ishak, M., Kehoe, R., Kremin, A., Landriau, M., Guillou, L. Le, Levi, M. E., Manera, M., Martini, P., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Miquel, R., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Newman, J. A., Nie, J., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Pérez-Fernández, A., Rashkovetskyi, M., Rezaie, M., Rosado-Marin, A., Rossi, G., Ruggeri, R., Sanchez, E., Saulder, C., Schlafly, E. F., Schlegel, D., Schubnell, M., Sprayberry, D., Tarlé, G., Valcin, D., Vargas-Magaña, M., Yu, J., Yuan, S., Zhou, R., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Baryon acoustic oscillations (BAO) provide a robust standard ruler to measure the expansion history of the Universe through galaxy clustering. Density-field reconstruction is now a widely adopted procedure for increasing the precision and accuracy of the BAO detection. With the goal of finding the optimal reconstruction settings to be used in the DESI 2024 galaxy BAO analysis, we assess the sensitivity of the post-reconstruction BAO constraints to different choices in our analysis configuration, performing tests on blinded data from the first year of DESI observations (DR1), as well as on mocks that mimic the expected clustering and selection properties of the DESI DR1 target samples. Overall, we find that BAO constraints remain robust against multiple aspects in the reconstruction process, including the choice of smoothing scale, treatment of redshift-space distortions, fiber assignment incompleteness, and parameterizations of the BAO model. We also present a series of tests that DESI followed in order to assess the maturity of the end-to-end galaxy BAO pipeline before the unblinding of the large-scale structure catalogs., Comment: Supporting publication of DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars
Published: 2024

33. Validation of the DESI 2024 Ly$\alpha$ forest BAO analysis using synthetic datasets

Author: Cuceu, Andrei, Herrera-Alcantar, Hiram K., Gordon, Calum, Martini, Paul, Guy, Julien, Font-Ribera, Andreu, Gonzalez-Morales, Alma X., Karim, M. Abdul, Aguilar, J., Ahlen, S., Armengaud, E., Bault, A., Brooks, D., Claybaugh, T., de la Macorra, A., Doel, P., Fanning, K., Ferraro, S., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Gutierrez, G., Honscheid, K., Howlett, C., Karaçaylı, N. G., Kirkby, D., Kremin, A., Landriau, M., Goff, J. M. Le, Guillou, L. Le, Levi, M. E., Manera, M., Meisner, A., Miquel, R., Moustakas, J., Muñoz-Gutiérrez, A., Myers, A. D., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Pérez-Ràfols, I., Ramírez-Pérez, C., Ravoux, C., Rezaie, M., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Seo, H., Sprayberry, D., Tan, T., Tarlé, G., Vargas-Magaña, M., Walther, M., Weaver, B. A., Zhou, R., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The first year of data from the Dark Energy Spectroscopic Instrument (DESI) contains the largest set of Lyman-$\alpha$ (Ly$\alpha$) forest spectra ever observed. This data, collected in the DESI Data Release 1 (DR1) sample, has been used to measure the Baryon Acoustic Oscillation (BAO) feature at redshift $z=2.33$. In this work, we use a set of 150 synthetic realizations of DESI DR1 to validate the DESI 2024 Ly$\alpha$ forest BAO measurement. The synthetic data sets are based on Gaussian random fields using the log-normal approximation. We produce realistic synthetic DESI spectra that include all major contaminants affecting the Ly$\alpha$ forest. The synthetic data sets span a redshift range $1.8
Published: 2024

34. DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars

Author: DESI Collaboration, Adame, A. G., Aguilar, J., Ahlen, S., Alam, S., Alexander, D. M., Alvarez, M., Alves, O., Anand, A., Andrade, U., Armengaud, E., Avila, S., Aviles, A., Awan, H., Bailey, S., Baltay, C., Bault, A., Behera, J., BenZvi, S., Beutler, F., Bianchi, D., Blake, C., Blum, R., Brieden, S., Brodzeller, A., Brooks, D., Buckley-Geer, E., Burtin, E., Calderon, R., Canning, R., Rosell, A. Carnero, Cereskaite, R., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Chen, S., Chen, X., Claybaugh, T., Cole, S., Cuceu, A., Davis, T. M., Dawson, K., de la Macorra, A., de Mattia, A., Deiosso, N., Dey, A., Dey, B., Ding, Z., Doel, P., Edelstein, J., Eftekharzadeh, S., Eisenstein, D. J., Elliott, A., Fagrelius, P., Fanning, K., Ferraro, S., Ereza, J., Findlay, N., Flaugher, B., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Garcia-Quintero, C., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gonzalez-Perez, V., Gordon, C., Green, D., Gruen, D., Gsponer, R., Gutierrez, G., Guy, J., Hadzhiyska, B., Hahn, C., Hanif, M. M. S, Herrera-Alcantar, H. K., Honscheid, K., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Juneau, S., Karaçaylı, N. G., Kehoe, R., Kent, S., Kirkby, D., Kremin, A., Krolewski, A., Lai, Y., Lan, T. -W., Landriau, M., Lang, D., Lasker, J., Goff, J. M. Le, Guillou, L. Le, Leauthaud, A., Levi, M. E., Li, T. S., Linder, E., Lodha, K., Magneville, C., Manera, M., Margala, D., Martini, P., Maus, M., McDonald, P., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Miquel, R., Moon, J., Moore, S., Moustakas, J., Mudur, N., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Napolitano, L., Neveux, R., Newman, J. A., Nguyen, N. M., Nie, J., Niz, G., Noriega, H. E., Padmanabhan, N., Paillas, E., Palanque-Delabrouille, N., Pan, J., Penmetsa, S., Percival, W. J., Pieri, M., Pinon, M., Poppett, C., Porredon, A., Prada, F., Pérez-Fernández, A., Pérez-Ràfols, I., Rabinowitz, D., Raichoor, A., Ramírez-Pérez, C., Ramirez-Solano, S., Rashkovetskyi, M., Rezaie, M., Rich, J., Rocher, A., Rockosi, C., Roe, N. A., Rosado-Marin, A., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Samushia, L., Sanchez, E., Saulder, C., Schlafly, E. F., Schlegel, D., Schubnell, M., Seo, H., Sharples, R., Silber, J., Slosar, A., Smith, A., Sprayberry, D., Swanson, J., Tan, T., Tarlé, G., Trusov, S., Vaisakh, R., Valcin, D., Valdes, F., Vargas-Magaña, M., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, N., Wechsler, R. H., Weinberg, D. H., White, M., Yu, J., Yu, Y., Yuan, S., Yèche, C., Zaborowski, E. A., Zarrouk, P., Zhang, H., Zhao, C., Zhao, R., Zhou, R., and Zou, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the DESI 2024 galaxy and quasar baryon acoustic oscillations (BAO) measurements using over 5.7 million unique galaxy and quasar redshifts in the range 0.1
Published: 2024

35. The Early Data Release of the Dark Energy Spectroscopic Instrument

Author: Collaboration, DESI, Adame, AG, Aguilar, J, Ahlen, S, Alam, S, Aldering, G, Alexander, DM, Alfarsy, R, Prieto, C Allende, Alvarez, M, Alves, O, Anand, A, Andrade-Oliveira, F, Armengaud, E, Asorey, J, Avila, S, Aviles, A, Bailey, S, Balaguera-Antolínez, A, Ballester, O, Baltay, C, Bault, A, Bautista, J, Behera, J, Beltran, SF, BenZvi, S, Silva, L Beraldo E, Bermejo-Climent, JR, Berti, A, Besuner, R, Beutler, F, Bianchi, D, Blake, C, Blum, R, Bolton, AS, Brieden, S, Brodzeller, A, Brooks, D, Brown, Z, Buckley-Geer, E, Burtin, E, Cabayol-Garcia, L, Cai, Z, Canning, R, Cardiel-Sas, L, Rosell, A Carnero, Castander, FJ, Cervantes-Cota, JL, Chabanier, S, Chaussidon, E, Chaves-Montero, J, Chen, S, Chen, X, Chuang, C, Claybaugh, T, Cole, S, Cooper, AP, Cuceu, A, Davis, TM, Dawson, K, de Belsunce, R, de la Cruz, R, de la Macorra, A, Della Costa, J, de Mattia, A, Demina, R, Demirbozan, U, DeRose, J, Dey, A, Dey, B, Dhungana, G, Ding, J, Ding, Z, Doel, P, Doshi, R, Douglass, K, Edge, A, Eftekharzadeh, S, Eisenstein, DJ, Elliott, A, Ereza, J, Escoffier, S, Fagrelius, P, Fan, X, Fanning, K, Fawcett, VA, Ferraro, S, Flaugher, B, Font-Ribera, A, Forero-Romero, JE, Forero-Sánchez, D, Frenk, CS, Gänsicke, BT, García, LÁ, García-Bellido, J, Garcia-Quintero, C, Garrison, LH, Gil-Marín, H, Golden-Marx, J, and Gontcho, S Gontcho A
Subjects: Astronomical Sciences, Physical Sciences, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics
Abstract: The Dark Energy Spectroscopic Instrument (DESI) completed its 5 month Survey Validation in 2021 May. Spectra of stellar and extragalactic targets from Survey Validation constitute the first major data sample from the DESI survey. This paper describes the public release of those spectra, the catalogs of derived properties, and the intermediate data products. In total, the public release includes good-quality spectral information from 466,447 objects targeted as part of the Milky Way Survey, 428,758 as part of the Bright Galaxy Survey, 227,318 as part of the Luminous Red Galaxy sample, 437,664 as part of the Emission Line Galaxy sample, and 76,079 as part of the Quasar sample. In addition, the release includes spectral information from 137,148 objects that expand the scope beyond the primary samples as part of a series of secondary programs. Here, we describe the spectral data, data quality, data products, Large-Scale Structure science catalogs, access to the data, and references that provide relevant background to using these spectra.
Published: 2024

36. Baryon Acoustic Oscillation Theory and Modelling Systematics for the DESI 2024 results

Author: Chen, Shi-Fan, Howlett, Cullan, White, Martin, McDonald, Patrick, Ross, Ashley J., Seo, Hee-Jong, Padmanabhan, Nikhil, Aguilar, J., Ahlen, S., Alam, S., Alves, O., Andrade, U., Blum, R., Brooks, D., Chen, X., Cole, S., Davis, T. M., Dawson, K., de la Macorra, A., Dey, Arjun, Ding, Z., Doel, P., Ferraro, S., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Garcia-Quintero, C., Gaztañaga, E., Gontcho, S. Gontcho A, Hanif, M. M. S, Honscheid, K., Kisner, T., Kremin, A., Lambert, A., Landriau, M., Levi, M. E., Manera, M., Meisner, A., Mena-Fernández, J., Miquel, R., Muñoz-Gutiérrez, A., Paillas, E., Palanque-Delabrouille, N., Percival, W. J., Prada, F., Pérez-Fernández, A., Rashkovetskyi, M., Rezaie, M., Rosado-Marin, A., Rossi, G., Ruggeri, R., Sanchez, E., Schlegel, D., Silber, J., Tarlé, G., Vargas-Magaña, M., Weaver, B. A., Yu, J., Yuan, S., Zhou, R., and Zhou, Z.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: This paper provides a comprehensive overview of how fitting of Baryon Acoustic Oscillations (BAO) is carried out within the upcoming Dark Energy Spectroscopic Instrument's (DESI) 2024 results using its DR1 dataset, and the associated systematic error budget from theory and modelling of the BAO. We derive new results showing how non-linearities in the clustering of galaxies can cause potential biases in measurements of the isotropic ($\alpha_{\mathrm{iso}}$) and anisotropic ($\alpha_{\mathrm{ap}}$) BAO distance scales, and how these can be effectively removed with an appropriate choice of reconstruction algorithm. We then demonstrate how theory leads to a clear choice for how to model the BAO and develop, implement and validate a new model for the remaining smooth-broadband (i.e., without BAO) component of the galaxy clustering. Finally, we explore the impact of all remaining modelling choices on the BAO constraints from DESI using a suite of high-precision simulations, arriving at a set of best-practices for DESI BAO fits, and an associated theory and modelling systematic error. Overall, our results demonstrate the remarkable robustness of the BAO to all our modelling choices and motivate a combined theory and modelling systematic error contribution to the post-reconstruction DESI BAO measurements of no more than $0.1\%$ ($0.2\%$) for its isotropic (anisotropic) distance measurements. We expect the theory and best-practices laid out to here to be applicable to other BAO experiments in the era of DESI and beyond., Comment: 30 pages, 18 figures, 1 table, updated to match version accepted by MNRAS
Published: 2024

37. class_sz I: Overview

Author: Bolliet, B., Kusiak, A., McCarthy, F., Sabyr, A., Surrao, K., Hill, J. C., Chluba, J., Ferraro, S., Hadzhiyska, B., Han, D., Macías-Pérez, J. F., Madhavacheril, M., Maniyar, A., Mehta, Y., Pandey, S., Schaan, E., Sherwin, B., Mancini, A. Spurio, and Zubeldia, Í.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: class_sz is a versatile and robust code in C and Python that can compute theoretical predictions for a wide range of observables relevant to cross-survey science in the Stage IV era. The code is public at https://github.com/CLASS-SZ/class_sz along with a series of tutorial notebooks (https://github.com/CLASS-SZ/notebooks). It will be presented in full detail in paper II. Here we give a brief overview of key features and usage., Comment: to appear in Proc. of the mm Universe 2023 conference, Grenoble (France), June 2023, published by F. Mayet et al. (Eds), EPJ Web of conferences, EDP Sciences
Published: 2023

38. Validation of the Scientific Program for the Dark Energy Spectroscopic Instrument

Author: Collaboration, DESI, Adame, AG, Aguilar, J, Ahlen, S, Alam, S, Aldering, G, Alexander, DM, Alfarsy, R, Prieto, C Allende, Alvarez, M, Alves, O, Anand, A, Andrade-Oliveira, F, Armengaud, E, Asorey, J, Avila, S, Aviles, A, Bailey, S, Balaguera-Antolínez, A, Ballester, O, Baltay, C, Bault, A, Bautista, J, Behera, J, Beltran, SF, BenZvi, S, Silva, L Beraldo E, Bermejo-Climent, JR, Berti, A, Besuner, R, Beutler, F, Bianchi, D, Blake, C, Blum, R, Bolton, AS, Brieden, S, Brodzeller, A, Brooks, D, Brown, Z, Buckley-Geer, E, Burtin, E, Cabayol-Garcia, L, Cai, Z, Canning, R, Cardiel-Sas, L, Rosell, A Carnero, Castander, FJ, Cervantes-Cota, JL, Chabanier, S, Chaussidon, E, Chaves-Montero, J, Chen, S, Chen, X, Chuang, C, Claybaugh, T, Cole, S, Cooper, AP, Cuceu, A, Davis, TM, Dawson, K, de Belsunce, R, de la Cruz, R, de la Macorra, A, de Mattia, A, Demina, R, Demirbozan, U, DeRose, J, Dey, A, Dey, B, Dhungana, G, Ding, J, Ding, Z, Doel, P, Doshi, R, Douglass, K, Edge, A, Eftekharzadeh, S, Eisenstein, DJ, Elliott, A, Escoffier, S, Fagrelius, P, Fan, X, Fanning, K, Fawcett, VA, Ferraro, S, Ereza, J, Flaugher, B, Font-Ribera, A, Forero-Sánchez, D, Forero-Romero, JE, Frenk, CS, Gänsicke, BT, García, LÁ, García-Bellido, J, Garcia-Quintero, C, Garrison, LH, Gil-Marín, H, Golden-Marx, J, Gontcho, S Gontcho A, and Gonzalez-Morales, AX
Subjects: Astronomical Sciences, Physical Sciences, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics
Abstract: The Dark Energy Spectroscopic Instrument (DESI) was designed to conduct a survey covering 14,000 deg2 over 5 yr to constrain the cosmic expansion history through precise measurements of baryon acoustic oscillations (BAO). The scientific program for DESI was evaluated during a 5 month survey validation (SV) campaign before beginning full operations. This program produced deep spectra of tens of thousands of objects from each of the stellar Milky Way Survey (MWS), Bright Galaxy Survey (BGS), luminous red galaxy (LRG), emission line galaxy (ELG), and quasar target classes. These SV spectra were used to optimize redshift distributions, characterize exposure times, determine calibration procedures, and assess observational overheads for the 5 yr program. In this paper, we present the final target selection algorithms, redshift distributions, and projected cosmology constraints resulting from those studies. We also present a One-Percent Survey conducted at the conclusion of SV covering 140 deg2 using the final target selection algorithms with exposures of a depth typical of the main survey. The SV indicates that DESI will be able to complete the full 14,000 deg2 program with spectroscopically confirmed targets from the MWS, BGS, LRG, ELG, and quasar programs with total sample sizes of 7.2, 13.8, 7.46, 15.7, and 2.87 million, respectively. These samples will allow exploration of the Milky Way halo, clustering on all scales, and BAO measurements with a statistical precision of 0.28% over the redshift interval z < 1.1, 0.39% over the redshift interval 1.1 < z < 1.9, and 0.46% over the redshift interval 1.9 < z < 3.5.
Published: 2024

39. Cosmology from Cross-Correlation of ACT-DR4 CMB Lensing and DES-Y3 Cosmic Shear

Author: Shaikh, S., Harrison, I., van Engelen, A., Marques, G. A., Abbott, T. M. C., Aguena, M., Alves, O., Amon, A., An, R., Bacon, D., Battaglia, N., Becker, M. R., Bernstein, G. M., Bertin, E., Blazek, J., Bond, J. R., Brooks, D., Burke, D. L., Calabrese, E., Rosell, A. Carnero, Carretero, J., Cawthon, R., Chang, C., Chen, R., Choi, A., Choi, S. K., da Costa, L. N., Pereira, M. E. S., Darwish, O., Davis, T. M., Desai, S., Devlin, M., Diehl, H. T., Doel, P., Doux, C., Elvin-Poole, J., Farren, G. S., Ferraro, S., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., Gatti, M., Giannini, G., Giardiello, S., Gruen, D., Gruendl, R. A., Gutierrez, G., Hill, J. C., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huffenberger, K. M., Huterer, D., James, D. J., Jarvis, M., Jeffrey, N., Jense, H. T., Knowles, K., Kim, J., Kramer, D., Lahav, O., Lee, S., Lima, M., MacCrann, N., Madhavacheril, M. S., Marshall, J. L., McCullough, J., Mehta, Y., Mena-Fernández, J., Miquel, R., Mohr, J. J., Moodley, K., Myles, J., Navarro-Alsina, A., Newburgh, L., Niemack, M. D., Omori, Y., Pandey, S., Partridge, B., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Prat, J., Qu, F. J., Robertson, N., Rollins, R. P., Roodman, A., Samuroff, S., Sánchez, C., Sanchez, E., Cid, D. Sanchez, Secco, L. F., Sehgal, N., Sheldon, E., Sherwin, B. D., Shin, T., Smith, C. Sifón M., Suchyta, E., Swanson, M. E. C., Tarle, G., Troxel, M. A., Tutusaus, I., Vargas, C., Weaverdyck, N., Wiseman, P., Yamamoto, M., and Zuntz, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Cross-correlation between weak lensing of the Cosmic Microwave Background (CMB) and weak lensing of galaxies offers a way to place robust constraints on cosmological and astrophysical parameters with reduced sensitivity to certain systematic effects affecting individual surveys. We measure the angular cross-power spectrum between the Atacama Cosmology Telescope (ACT) DR4 CMB lensing and the galaxy weak lensing measured by the Dark Energy Survey (DES) Y3 data. Our baseline analysis uses the CMB convergence map derived from ACT-DR4 and $\textit{Planck}$ data, where most of the contamination due to the thermal Sunyaev Zel'dovich effect is removed, thus avoiding important systematics in the cross-correlation. In our modelling, we consider the nuisance parameters of the photometric uncertainty, multiplicative shear bias and intrinsic alignment of galaxies. The resulting cross-power spectrum has a signal-to-noise ratio $= 7.1$ and passes a set of null tests. We use it to infer the amplitude of the fluctuations in the matter distribution ($S_8 \equiv \sigma_8 (\Omega_{\rm m}/0.3)^{0.5} = 0.782\pm 0.059$) with informative but well-motivated priors on the nuisance parameters. We also investigate the validity of these priors by significantly relaxing them and checking the consistency of the resulting posteriors, finding them consistent, albeit only with relatively weak constraints. This cross-correlation measurement will improve significantly with the new ACT-DR6 lensing map and form a key component of the joint 6x2pt analysis between DES and ACT., Comment: 26 pages, 30 figures (including appendices). Data associated with this article is available at https://github.com/itrharrison/actdr4kappa-x-desy3gamma-data
Published: 2023
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40. The Early Data Release of the Dark Energy Spectroscopic Instrument

Author: DESI Collaboration, Adame, A. G., Aguilar, J., Ahlen, S., Alam, S., Aldering, G., Alexander, D. M., Alfarsy, R., Prieto, C. Allende, Alvarez, M., Alves, O., Anand, A., Andrade-Oliveira, F., Armengaud, E., Asorey, J., Avila, S., Aviles, A., Bailey, S., Balaguera-Antolínez, A., Ballester, O., Baltay, C., Bault, A., Bautista, J., Behera, J., Beltran, S. F., BenZvi, S., Silva, L. Beraldo e, Bermejo-Climent, J. R., Berti, A., Besuner, R., Beutler, F., Bianchi, D., Blake, C., Blum, R., Bolton, A. S., Brieden, S., Brodzeller, A., Brooks, D., Brown, Z., Buckley-Geer, E., Burtin, E., Cabayol-Garcia, L., Cai, Z., Canning, R., Cardiel-Sas, L., Rosell, A. Carnero, Castander, F. J., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Chen, S., Chen, X., Chuang, C., Claybaugh, T., Cole, S., Cooper, A. P., Cuceu, A., Davis, T. M., Dawson, K., de Belsunce, R., de la Cruz, R., de la Macorra, A., Della Costa, J., de Mattia, A., Demina, R., Demirbozan, U., DeRose, J., Dey, A., Dey, B., Dhungana, G., Ding, J., Ding, Z., Doel, P., Doshi, R., Douglass, K., Edge, A., Eftekharzadeh, S., Eisenstein, D. J., Elliott, A., Escoffier, S., Fagrelius, P., Fan, X., Fanning, K., Fawcett, V. A., Ferraro, S., Ereza, J., Flaugher, B., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Frenk, C. S., Gänsicke, B. T., García, L. Á., García-Bellido, J., Garcia-Quintero, C., Garrison, L. H., Gil-Marín, H., Golden-Marx, J., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gonzalez-Perez, V., Gordon, C., Graur, O., Green, D., Gruen, D., Guy, J., Hadzhiyska, B., Hahn, C., Han, J. J., Hanif, M. M. S, Herrera-Alcantar, H. K., Honscheid, K., Hou, J., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Jacques, A., Jana, A., Jiang, L., Jimenez, J., Jing, Y. P., Joudaki, S., Jullo, E., Juneau, S., Kizhuprakkat, N., Karaçaylı, N. G., Karim, T., Kehoe, R., Kent, S., Khederlarian, A., Kim, S., Kirkby, D., Kisner, T., Kitaura, F., Kneib, J., Koposov, S. E., Kovács, A., Kremin, A., Krolewski, A., L'Huillier, B., Lahav, O., Lambert, A., Lamman, C., Lan, T. -W., Landriau, M., Lang, D., Lange, J. U., Lasker, J., Leauthaud, A., Guillou, L. Le, Levi, M. E., Li, T. S., Linder, E., Lyons, A., Magneville, C., Manera, M., Manser, C. J., Margala, D., Martini, P., McDonald, P., Medina, G. E., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Meneses-Rizo, J., Mezcua, M., Miquel, R., Montero-Camacho, P., Moon, J., Moore, S., Moustakas, J., Mueller, E., Mundet, J., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Napolitano, L., Neveux, R., Newman, J. A., Nie, J., Nikutta, R., Niz, G., Norberg, P., Noriega, H. E., Paillas, E., Palanque-Delabrouille, N., Palmese, A., Zhiwei, P., Parkinson, D., Penmetsa, S., Percival, W. J., Pérez-Fernández, A., Pérez-Ràfols, I., Pieri, M., Poppett, C., Porredon, A., Pothier, S., Prada, F., Pucha, R., Raichoor, A., Ramírez-Pérez, C., Ramirez-Solano, S., Rashkovetskyi, M., Ravoux, C., Rocher, A., Rockosi, C., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Sabiu, C. G., Said, K., Saintonge, A., Samushia, L., Sanchez, E., Saulder, C., Schaan, E., Schlafly, E. F., Schlegel, D., Scholte, D., Schubnell, M., Seo, H., Shafieloo, A., Sharples, R., Sheu, W., Silber, J., Sinigaglia, F., Siudek, M., Slepian, Z., Smith, A., Soumagnac, M. T., Sprayberry, D., Stephey, L., Suárez-Pérez, J., Sun, Z., Tan, T., Tarlé, G., Tojeiro, R., Ureña-López, L. A., Vaisakh, R., Valcin, D., Valdes, F., Valluri, M., Vargas-Magaña, M., Variu, A., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, N., Wechsler, R. H., White, M., Xie, Y., Yang, J., Yèche, C., Yu, J., Yuan, S., Zhang, H., Zhang, Z., Zhao, C., Zheng, Z., Zhou, R., Zhou, Z., Zou, H., Zou, S., and Zu, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Dark Energy Spectroscopic Instrument (DESI) completed its five-month Survey Validation in May 2021. Spectra of stellar and extragalactic targets from Survey Validation constitute the first major data sample from the DESI survey. This paper describes the public release of those spectra, the catalogs of derived properties, and the intermediate data products. In total, the public release includes good-quality spectral information from 466,447 objects targeted as part of the Milky Way Survey, 428,758 as part of the Bright Galaxy Survey, 227,318 as part of the Luminous Red Galaxy sample, 437,664 as part of the Emission Line Galaxy sample, and 76,079 as part of the Quasar sample. In addition, the release includes spectral information from 137,148 objects that expand the scope beyond the primary samples as part of a series of secondary programs. Here, we describe the spectral data, data quality, data products, Large-Scale Structure science catalogs, access to the data, and references that provide relevant background to using these spectra., Comment: 43 pages, 7 figures, 17 tables, accepted for publication in the Astronomical Journal
Published: 2023
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41. Validation of the Scientific Program for the Dark Energy Spectroscopic Instrument

Author: DESI Collaboration, Adame, A. G., Aguilar, J., Ahlen, S., Alam, S., Aldering, G., Alexander, D. M., Alfarsy, R., Prieto, C. Allende, Alvarez, M., Alves, O., Anand, A., Andrade-Oliveira, F., Armengaud, E., Asorey, J., Avila, S., Aviles, A., Bailey, S., Balaguera-Antolínez, A., Ballester, O., Baltay, C., Bault, A., Bautista, J., Behera, J., Beltran, S. F., BenZvi, S., Silva, L. Beraldo e, Bermejo-Climent, J. R., Berti, A., Besuner, R., Beutler, F., Bianchi, D., Blake, C., Blum, R., Bolton, A. S., Brieden, S., Brodzeller, A., Brooks, D., Brown, Z., Buckley-Geer, E., Burtin, E., Cabayol-Garcia, L., Cai, Z., Canning, R., Cardiel-Sas, L., Rosell, A. Carnero, Castander, F. J., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Chen, S., Chuang, C., Claybaugh, T., Cole, S., Cooper, A. P., Cuceu, A., Davis, T. M., Dawson, K., de Belsunce, R., de la Cruz, R., de la Macorra, A., de Mattia, A., Demina, R., Demirbozan, U., DeRose, J., Dey, A., Dey, B., Dhungana, G., Ding, J., Ding, Z., Doel, P., Doshi, R., Douglass, K., Edge, A., Eftekharzadeh, S., Eisenstein, D. J., Elliott, A., Escoffier, S., Fagrelius, P., Fan, X., Fanning, K., Fawcett, V. A., Ferraro, S., Ereza, J., Flaugher, B., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Frenk, C. S., Gänsicke, B. T., García, L. Á., García-Bellido, J., Garcia-Quintero, C., Garrison, L. H., Gil-Marín, H., Golden-Marx, J., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gonzalez-Perez, V., Gordon, C., Graur, O., Green, D., Gruen, D., Guy, J., Hadzhiyska, B., Hahn, C., Han, J. J., Hanif, M. M. S, Herrera-Alcantar, H. K., Honscheid, K., Hou, J., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Jana, A., Jiang, L., Jimenez, J., Jing, Y. P., Joudaki, S., Joyce, R., Jullo, E., Juneau, S., Kizhuprakkat, N., Karaçaylı, N. G., Karim, T., Kehoe, R., Kent, S., Khederlarian, A., Kim, S., Kirkby, D., Kisner, T., Kitaura, F., Kneib, J., Koposov, S. E., Kovács, A., Kremin, A., Krolewski, A., L'Huillier, B., Lahav, O., Lambert, A., Lamman, C., Lan, T. -W., Landriau, M., Lang, D., Lange, J. U., Lasker, J., Guillou, L. Le, Leauthaud, A., Levi, M. E., Li, T. S., Linder, E., Lyons, A., Magneville, C., Manera, M., Manser, C. J., Margala, D., Martini, P., McDonald, P., Medina, G. E., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Meneses-Rizo, J., Mezcua, M., Miquel, R., Montero-Camacho, P., Moon, J., Moore, S., Moustakas, J., Mueller, E., Mundet, J., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Napolitano, L., Neveux, R., Newman, J. A., Nie, J., Niz, G., Norberg, P., Noriega, H. E., Paillas, E., Palanque-Delabrouille, N., Palmese, A., Zhiwei, P., Parkinson, D., Penmetsa, S., Percival, W. J., Pérez-Fernández, A., Pérez-Ràfols, I., Pieri, M., Poppett, C., Porredon, A., Prada, F., Pucha, R., Raichoor, A., Ramírez-Pérez, C., Ramirez-Solano, S., Rashkovetskyi, M., Ravoux, C., Rocher, A., Rockosi, C., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Sabiu, C. G., Said, K., Saintonge, A., Samushia, L., Sanchez, E., Saulder, C., Schaan, E., Schlafly, E. F., Schlegel, D., Scholte, D., Schubnell, M., Seo, H., Shafieloo, A., Sharples, R., Sheu, W., Silber, J., Sinigaglia, F., Siudek, M., Slepian, Z., Smith, A., Sprayberry, D., Stephey, L., Suárez-Pérez, J., Sun, Z., Tan, T., Tarlé, G., Tojeiro, R., Ureña-López, L. A., Vaisakh, R., Valcin, D., Valdes, F., Valluri, M., Vargas-Magaña, M., Variu, A., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, N., Wechsler, R. H., White, M., Xie, Y., Yang, J., Yèche, C., Yu, J., Yuan, S., Zhang, H., Zhang, Z., Zhao, C., Zheng, Z., Zhou, R., Zhou, Z., Zou, H., Zou, S., and Zu, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Dark Energy Spectroscopic Instrument (DESI) was designed to conduct a survey covering 14,000 deg$^2$ over five years to constrain the cosmic expansion history through precise measurements of Baryon Acoustic Oscillations (BAO). The scientific program for DESI was evaluated during a five month Survey Validation (SV) campaign before beginning full operations. This program produced deep spectra of tens of thousands of objects from each of the stellar (MWS), bright galaxy (BGS), luminous red galaxy (LRG), emission line galaxy (ELG), and quasar target classes. These SV spectra were used to optimize redshift distributions, characterize exposure times, determine calibration procedures, and assess observational overheads for the five-year program. In this paper, we present the final target selection algorithms, redshift distributions, and projected cosmology constraints resulting from those studies. We also present a `One-Percent survey' conducted at the conclusion of Survey Validation covering 140 deg$^2$ using the final target selection algorithms with exposures of a depth typical of the main survey. The Survey Validation indicates that DESI will be able to complete the full 14,000 deg$^2$ program with spectroscopically-confirmed targets from the MWS, BGS, LRG, ELG, and quasar programs with total sample sizes of 7.2, 13.8, 7.46, 15.7, and 2.87 million, respectively. These samples will allow exploration of the Milky Way halo, clustering on all scales, and BAO measurements with a statistical precision of 0.28% over the redshift interval $z<1.1$, 0.39% over the redshift interval $1.1
Published: 2023
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42. The Kinematic Sunyaev-Zel'dovich Effect with ACT, DES, and BOSS: a Novel Hybrid Estimator

Author: Mallaby-Kay, M., Amodeo, S., Hill, J. C., Aguena, M., Allam, S., Alves, O., Annis, J., Battaglia, N., Battistelli, E. S., Baxter, E. J., Bechtol, K., Becker, M. R., Bertin, E., Bond, J. R., Brooks, D., Calabrese, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Choi, A., Crocce, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Doux, C., Drlica-Wagner, A., Dunkley, J., Elvin-Poole, J., Everett, S., Ferraro, S., Ferrero, I., Frieman, J., Gallardo, P. A., García-Bellido, J., Giannini, G., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., James, D. J., Kosowsky, A., Kuehn, K., Lokken, M., Louis, T., Marshall, J. L., McMahon, J., Mena-Fernández, J., Menanteau, F., Miquel, R., Moodley, K., Mroczkowski, T., Naess, S., Niemack, M. D., Ogando, R. L. C., Page, L., Pandey, S., Pieres, A., Malagón, A. A. Plazas, Raveri, M., Rodriguez-Monroy, M., Rykoff, E. S., Samuroff, S., Sanchez, E., Schaan, E., Sevilla-Noarbe, I., Sheldon, E., Sifón, C., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., To, C., Vargas, C., Vavagiakis, E. M., Weaverdyck, N., Weller, J., Wiseman, P., and Yanny, B.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The kinematic and thermal Sunyaev-Zel'dovich (kSZ and tSZ) effects probe the abundance and thermodynamics of ionized gas in galaxies and clusters. We present a new hybrid estimator to measure the kSZ effect by combining cosmic microwave background temperature anisotropy maps with photometric and spectroscopic optical survey data. The method interpolates a velocity reconstruction from a spectroscopic catalog at the positions of objects in a photometric catalog, which makes it possible to leverage the high number density of the photometric catalog and the precision of the spectroscopic survey. Combining this hybrid kSZ estimator with a measurement of the tSZ effect simultaneously constrains the density and temperature of free electrons in the photometrically selected galaxies. Using the 1000 deg2 of overlap between the Atacama Cosmology Telescope (ACT) Data Release 5, the first three years of data from the Dark Energy Survey (DES), and the Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 12, we detect the kSZ signal at 4.8${\sigma}$ and reject the null (no-kSZ) hypothesis at 5.1${\sigma}$. This corresponds to 2.0${\sigma}$ per 100,000 photometric objects with a velocity field based on a spectroscopic survey with 1/5th the density of the photometric catalog. For comparison, a recent ACT analysis using exclusively spectroscopic data from BOSS measured the kSZ signal at 2.1${\sigma}$ per 100,000 objects. Our derived constraints on the thermodynamic properties of the galaxy halos are consistent with previous measurements. With future surveys, such as the Dark Energy Spectroscopic Instrument and the Rubin Observatory Legacy Survey of Space and Time, we expect that this hybrid estimator could result in measurements with significantly better signal-to-noise than those that rely on spectroscopic data alone., Comment: 19 pages, 15 figures - matches published version
Published: 2023
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43. Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument

Author: Abareshi, B., Aguilar, J., Ahlen, S., Alam, Shadab, Alexander, David M., Alfarsy, R., Allen, L., Prieto, C. Allende, Alves, O., Ameel, J., Armengaud, E., Asorey, J., Aviles, Alejandro, Bailey, S., Balaguera-Antolínez, A., Ballester, O., Baltay, C., Bault, A., Beltran, S. F., Benavides, B., BenZvi, S., Berti, A., Besuner, R., Beutler, Florian, Bianchi, D., Blake, C., Blanc, P., Blum, R., Bolton, A., Bose, S., Bramall, D., Brieden, S., Brodzeller, A., Brooks, D., Brownewell, C., Buckley-Geer, E., Cahn, R. N., Cai, Z., Canning, R., Rosell, A. Carnero, Carton, P., Casas, R., Castander, F. J., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chuang, C., Circosta, C., Cole, S., Cooper, A. P., da Costa, L., Cousinou, M. -C., Cuceu, A., Davis, T. M., Dawson, K., de la Cruz-Noriega, R., de la Macorra, A., de Mattia, A., Della Costa, J., Demmer, P., Derwent, M., Dey, A., Dey, B., Dhungana, G., Ding, Z., Dobson, C., Doel, P., Donald-McCann, J., Donaldson, J., Douglass, K., Duan, Y., Dunlop, P., Edelstein, J., Eftekharzadeh, S., Eisenstein, D. J., Enriquez-Vargas, M., Escoffier, S., Evatt, M., Fagrelius, P., Fan, X., Fanning, K., Fawcett, V. A., Ferraro, S., Ereza, J., Flaugher, B., Font-Ribera, A., Forero-Romero, J. E., Frenk, C. S., Fromenteau, S., Gänsicke, B. T., Garcia-Quintero, C., Garrison, L., Gaztañaga, E., Gerardi, F., Gil-Marín, H., Gontcho, S. Gontcho A, Gonzalez-Morales, Alma X., Gonzalez-de-Rivera, G., Gonzalez-Perez, V., Gordon, C., Graur, O., Green, D., Grove, C., Gruen, D., Gutierrez, G., Guy, J., Hahn, C., Harris, S., Herrera, D., Herrera-Alcantar, Hiram K., Honscheid, K., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Jelinsky, P., Jiang, L., Jimenez, J., Jing, Y. P., Joyce, R., Jullo, E., Juneau, S., Karaçaylı, N. G., Karamanis, M., Karcher, A., Karim, T., Kehoe, R., Kent, S., Kirkby, D., Kisner, T., Kitaura, F., Koposov, S. E., Kovács, A., Kremin, A., Krolewski, Alex, L'Huillier, B., Lahav, O., Lambert, A., Lamman, C., Lan, Ting-Wen, Landriau, M., Lane, S., Lang, D., Lange, J. U., Lasker, J., Guillou, L. Le, Leauthaud, A., Van Suu, A. Le, Levi, Michael E., Li, T. S., Magneville, C., Manera, M., Manser, Christopher J., Marshall, B., McCollam, W., McDonald, P., Meisner, Aaron M., Mezcua, J. Mena-Fernández M., Miller, T., Miquel, R., Montero-Camacho, P., Moon, J., Martini, J. Paul, Meneses-Rizo, J., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, Andrea, Myers, Adam D., Nadathur, S., Najita, J., Napolitano, L., Neilsen, E., Newman, Jeffrey A., Nie, J. D., Ning, Y., Niz, G., Norberg, P., Noriega, Hernán E., O'Brien, T., Obuljen, A., Palanque-Delabrouille, N., Palmese, A., Zhiwei, P., Pappalardo, D., Peng, X., Percival, W. J., Perruchot, S., Pogge, R., Poppett, C., Porredon, A., Prada, F., Prochaska, J., Pucha, R., Pérez-Fernández, A., Pérez-Ráfols, I., Rabinowitz, D., Raichoor, A., Ramirez-Solano, S., Ramírez-Pérez, César, Ravoux, C., Reil, K., Rezaie, M., Rocher, A., Rockosi, C., Roe, N. A., Roodman, A., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Sabiu, C. G., Safonova, S., Said, K., Saintonge, A., Catonga, Javier Salas, Samushia, L., Sanchez, E., Saulder, C., Schaan, E., Schlafly, E., Schlegel, D., Schmoll, J., Scholte, D., Schubnell, M., Secroun, A., Seo, H., Serrano, S., Sharples, Ray M., Sholl, Michael J., Silber, Joseph Harry, Silva, D. R., Sirk, M., Siudek, M., Smith, A., Sprayberry, D., Staten, R., Stupak, B., Tan, T., Tarlé, Gregory, Tie, Suk Sien, Tojeiro, R., Ureña-López, L. A., Valdes, F., Valenzuela, O., Valluri, M., Vargas-Magaña, M., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, C., Wechsler, R., Wilson, Michael J., Yang, J., Yu, Y., Yuan, S., Yèche, Christophe, Zhang, H., Zhang, K., Zhao, Cheng, Zhou, Rongpu, Zhou, Zhimin, Zou, H., Zou, J., Zou, S., and Zu, Y.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Dark Energy Spectroscopic Instrument (DESI) has embarked on an ambitious five-year survey to explore the nature of dark energy with spectroscopy of 40 million galaxies and quasars. DESI will determine precise redshifts and employ the Baryon Acoustic Oscillation method to measure distances from the nearby universe to z > 3.5, as well as measure the growth of structure and probe potential modifications to general relativity. In this paper we describe the significant instrumentation we developed for the DESI survey. The new instrumentation includes a wide-field, 3.2-deg diameter prime-focus corrector that focuses the light onto 5020 robotic fiber positioners on the 0.812 m diameter, aspheric focal surface. The positioners and their fibers are divided among ten wedge-shaped petals. Each petal is connected to one of ten spectrographs via a contiguous, high-efficiency, nearly 50 m fiber cable bundle. The ten spectrographs each use a pair of dichroics to split the light into three channels that together record the light from 360 - 980 nm with a resolution of 2000 to 5000. We describe the science requirements, technical requirements on the instrumentation, and management of the project. DESI was installed at the 4-m Mayall telescope at Kitt Peak, and we also describe the facility upgrades to prepare for DESI and the installation and functional verification process. DESI has achieved all of its performance goals, and the DESI survey began in May 2021. Some performance highlights include RMS positioner accuracy better than 0.1", SNR per \sqrt{\AA} > 0.5 for a z > 2 quasar with flux 0.28e-17 erg/s/cm^2/A at 380 nm in 4000s, and median SNR = 7 of the [OII] doublet at 8e-17 erg/s/cm^2 in a 1000s exposure for emission line galaxies at z = 1.4 - 1.6. We conclude with highlights from the on-sky validation and commissioning of the instrument, key successes, and lessons learned. (abridged), Comment: 78 pages, 32 figures, submitted to AJ
Published: 2022
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44. THE NOT-WEIGHT-BASED DOSING STRATEGY OF DELNIDO CARDIOPLEGIA IS SAFE AND EFFECTIVE IN ACHIEVING MYOCARDIAL PROTECTION IN CARDIAC SURGERIES WITH STANDARD AND PROLONGED CROSS-CLAMP: PRELIMINARY RESULTS FROM I.R.DE.N. REGISTRY

Author: Ferraro, S., Calanni, C., Damiano, A., Barbaro, M., Cotugno, M., Comentale, G., and Pilato, E.
Published: 2024
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45. Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument

Author: Collaboration, DESI, Abareshi, B, Aguilar, J, Ahlen, S, Alam, Shadab, Alexander, David M, Alfarsy, R, Allen, L, Prieto, C Allende, Alves, O, Ameel, J, Armengaud, E, Asorey, J, Aviles, Alejandro, Bailey, S, Balaguera-Antolínez, A, Ballester, O, Baltay, C, Bault, A, Beltran, SF, Benavides, B, BenZvi, S, Berti, A, Besuner, R, Beutler, Florian, Bianchi, D, Blake, C, Blanc, P, Blum, R, Bolton, A, Bose, S, Bramall, D, Brieden, S, Brodzeller, A, Brooks, D, Brownewell, C, Buckley-Geer, E, Cahn, RN, Cai, Z, Canning, R, Capasso, R, Rosell, A Carnero, Carton, P, Casas, R, Castander, FJ, Cervantes-Cota, JL, Chabanier, S, Chaussidon, E, Chuang, C, Circosta, C, Cole, S, Cooper, AP, da Costa, L, Cousinou, M-C, Cuceu, A, Davis, TM, Dawson, K, de la Cruz-Noriega, R, de la Macorra, A, de Mattia, A, Della Costa, J, Demmer, P, Derwent, M, Dey, A, Dey, B, Dhungana, G, Ding, Z, Dobson, C, Doel, P, Donald-McCann, J, Donaldson, J, Douglass, K, Duan, Y, Dunlop, P, Edelstein, J, Eftekharzadeh, S, Eisenstein, DJ, Enriquez-Vargas, M, Escoffier, S, Evatt, M, Fagrelius, P, Fan, X, Fanning, K, Fawcett, VA, Ferraro, S, Ereza, J, Flaugher, B, Font-Ribera, A, Forero-Romero, JE, Frenk, CS, Fromenteau, S, Gänsicke, BT, Garcia-Quintero, C, Garrison, L, Gaztañaga, E, Gerardi, F, Gil-Marín, H, Gontcho, S Gontcho A, Gonzalez-Morales, Alma X, and Gonzalez-de-Rivera, G
Subjects: Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract: The Dark Energy Spectroscopic Instrument (DESI) embarked on an ambitious 5 yr survey in 2021 May to explore the nature of dark energy with spectroscopic measurements of 40 million galaxies and quasars. DESI will determine precise redshifts and employ the baryon acoustic oscillation method to measure distances from the nearby universe to beyond redshift z > 3.5, and employ redshift space distortions to measure the growth of structure and probe potential modifications to general relativity. We describe the significant instrumentation we developed to conduct the DESI survey. This includes: a wide-field, 3.°2 diameter prime-focus corrector; a focal plane system with 5020 fiber positioners on the 0.812 m diameter, aspheric focal surface; 10 continuous, high-efficiency fiber cable bundles that connect the focal plane to the spectrographs; and 10 identical spectrographs. Each spectrograph employs a pair of dichroics to split the light into three channels that together record the light from 360-980 nm with a spectral resolution that ranges from 2000-5000. We describe the science requirements, their connection to the technical requirements, the management of the project, and interfaces between subsystems. DESI was installed at the 4 m Mayall Telescope at Kitt Peak National Observatory and has achieved all of its performance goals. Some performance highlights include an rms positioner accuracy of better than 0.″1 and a median signal-to-noise ratio of 7 of the [O ii] doublet at 8 × 10-17 erg s-1 cm-2 in 1000 s for galaxies at z = 1.4-1.6. We conclude with additional highlights from the on-sky validation and commissioning, key successes, and lessons learned.
Published: 2022

46. Superclustering with the Atacama Cosmology Telescope and Dark Energy Survey. I. Evidence for Thermal Energy Anisotropy Using Oriented Stacking

Author: Lokken, M, Hložek, R, van Engelen, A, Madhavacheril, M, Baxter, E, DeRose, J, Doux, C, Pandey, S, Rykoff, ES, Stein, G, To, C, Abbott, TMC, Adhikari, S, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Battaglia, N, Bernstein, GM, Bertin, E, Bond, JR, Brooks, D, Calabrese, E, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Cawthon, R, Choi, A, Costanzi, M, Crocce, M, da Costa, LN, da Silva Pereira, ME, De Vicente, J, Desai, S, Dietrich, JP, Doel, P, Dunkley, J, Everett, S, Evrard, AE, Ferraro, S, Flaugher, B, Fosalba, P, Frieman, J, Gallardo, PA, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Giannantonio, T, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hill, JC, Hilton, M, Hincks, AD, Hinton, SR, Hollowood, DL, Honscheid, K, Hoyle, B, Huang, Z, Hughes, JP, Huterer, D, Jain, B, James, DJ, Jeltema, T, Kuehn, K, Lima, M, Maia, MAG, Marshall, JL, McMahon, J, Melchior, P, Menanteau, F, Miquel, R, Mohr, JJ, Moodley, K, Morgan, R, Nati, F, Page, L, Ogando, RLC, Palmese, A, Paz-Chinchón, F, Malagón, AA Plazas, Pieres, A, Romer, AK, Rozo, E, Sanchez, E, Scarpine, V, Schillaci, A, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Sheldon, E, Shin, T, Sifón, C, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, MEC, Tarle, G, and Thomas, D
Subjects: Nuclear and Plasma Physics, Physical Sciences, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: The cosmic web contains filamentary structure on a wide range of scales. On the largest scales, superclustering aligns multiple galaxy clusters along intercluster bridges, visible through their thermal Sunyaev-Zel'dovich signal in the cosmic microwave background. We demonstrate a new, flexible method to analyze the hot gas signal from multiscale extended structures. We use a Compton y-map from the Atacama Cosmology Telescope (ACT) stacked on redMaPPer cluster positions from the optical Dark Energy Survey (DES). Cutout images from the y-map are oriented with large-scale structure information from DES galaxy data such that the superclustering signal is aligned before being overlaid. We find evidence of an extended quadrupole moment of the stacked y signal at the 3.5σ level, demonstrating that the large-scale thermal energy surrounding galaxy clusters is anisotropically distributed. We compare our ACT × DES results with the Buzzard simulations, finding broad agreement. Using simulations, we highlight the promise of this novel technique for constraining the evolution of anisotropic, non-Gaussian structure using future combinations of microwave and optical surveys.
Published: 2022

47. Cross-correlation of Dark Energy Survey Year 3 lensing data with ACT and Planck thermal Sunyaev-Zel’dovich effect observations. II. Modeling and constraints on halo pressure profiles

Author: Pandey, S, Gatti, M, Baxter, E, Hill, JC, Fang, X, Doux, C, Giannini, G, Raveri, M, DeRose, J, Huang, H, Moser, E, Battaglia, N, Alarcon, A, Amon, A, Becker, M, Campos, A, Chang, C, Chen, R, Choi, A, Eckert, K, Elvin-Poole, J, Everett, S, Ferte, A, Harrison, I, Maccrann, N, Mccullough, J, Myles, J, Alsina, A Navarro, Prat, J, Rollins, RP, Sanchez, C, Shin, T, Troxel, M, Tutusaus, I, Yin, B, Aguena, M, Allam, S, Andrade-Oliveira, F, Bernstein, GM, Bertin, E, Bolliet, B, Bond, JR, Brooks, D, Calabrese, E, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Cawthon, R, Costanzi, M, Crocce, M, da Costa, LN, Pereira, MES, De Vicente, J, Desai, S, Diehl, HT, Dietrich, JP, Doel, P, Dunkley, J, Evrard, AE, Ferraro, S, Ferrero, I, Flaugher, B, Fosalba, P, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Giannantonio, T, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Herner, K, Hincks, AD, Hinton, SR, Hollowood, DL, Honscheid, K, Hughes, JP, Huterer, D, Jain, B, James, DJ, Jeltema, T, Krause, E, Kuehn, K, Lahav, O, Lima, M, Lokken, M, Madhavacheril, MS, Maia, MAG, Mcmahon, JJ, Melchior, P, Menanteau, F, Miquel, R, Mohr, JJ, Moodley, K, Morgan, R, Nati, F, Niemack, MD, Page, L, and Palmese, A
Subjects: Nuclear and Plasma Physics, Physical Sciences, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Quantum Physics, Nuclear & Particles Physics, Mathematical physics, Astronomical sciences, Particle and high energy physics
Abstract: Hot, ionized gas leaves an imprint on the cosmic microwave background via the thermal Sunyaev-Zel'dovich (tSZ) effect. The cross-correlation of gravitational lensing (which traces the projected mass) with the tSZ effect (which traces the projected gas pressure) is a powerful probe of the thermal state of ionized baryons throughout the Universe and is sensitive to effects such as baryonic feedback. In a companion paper (Gatti et al. Phys. Rev. D 105, 123525 (2022)PRVDAQ2470-0010), we present tomographic measurements and validation tests of the cross-correlation between Galaxy shear measurements from the first three years of observations of the Dark Energy Survey and tSZ measurements from a combination of Atacama Cosmology Telescope and Planck observations. In this work, we use the same measurements to constrain models for the pressure profiles of halos across a wide range of halo mass and redshift. We find evidence for reduced pressure in low-mass halos, consistent with predictions for the effects of feedback from active Galactic nuclei. We infer the hydrostatic mass bias (BM500c/MSZ) from our measurements, finding B=1.8±0.1 when adopting the Planck-preferred cosmological parameters. We additionally find that our measurements are consistent with a nonzero redshift evolution of B, with the correct sign and sufficient magnitude to explain the mass bias necessary to reconcile cluster count measurements with the Planck-preferred cosmology. Our analysis introduces a model for the impact of intrinsic alignments (IAs) of galaxy shapes on the shear-tSZ correlation. We show that IA can have a significant impact on these correlations at current noise levels.
Published: 2022

48. Cross-correlation of Dark Energy Survey Year 3 lensing data with ACT and Planck thermal Sunyaev-Zel’dovich effect observations. I. Measurements, systematics tests, and feedback model constraints

Author: Gatti, M, Pandey, S, Baxter, E, Hill, JC, Moser, E, Raveri, M, Fang, X, DeRose, J, Giannini, G, Doux, C, Huang, H, Battaglia, N, Alarcon, A, Amon, A, Becker, M, Campos, A, Chang, C, Chen, R, Choi, A, Eckert, K, Elvin-Poole, J, Everett, S, Ferte, A, Harrison, I, Maccrann, N, Mccullough, J, Myles, J, Alsina, A Navarro, Prat, J, Rollins, RP, Sanchez, C, Shin, T, Troxel, M, Tutusaus, I, Yin, B, Abbott, T, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Bernstein, G, Bertin, E, Bolliet, B, Bond, JR, Brooks, D, Burke, DL, Calabrese, E, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Cawthon, R, Costanzi, M, Crocce, M, da Costa, LN, da Silva Pereira, ME, De Vicente, J, Desai, S, Diehl, HT, Dietrich, JP, Doel, P, Dunkley, J, Evrard, AE, Ferraro, S, Ferrero, I, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Giannantonio, T, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Herner, K, Hincks, AD, Hinton, SR, Hollowood, DL, Honscheid, K, Hughes, JP, Huterer, D, Jain, B, James, DJ, Krause, E, Kuehn, K, Kuropatkin, N, Lahav, O, Lidman, C, Lima, M, Lokken, M, Madhavacheril, MS, Maia, MAG, Marshall, JL, Mcmahon, JJ, Melchior, P, Moodley, K, Mohr, JJ, Morgan, R, and Nati, F
Subjects: Nuclear and Plasma Physics, Physical Sciences, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Quantum Physics, Nuclear & Particles Physics, Mathematical physics, Astronomical sciences, Particle and high energy physics
Abstract: We present a tomographic measurement of the cross-correlation between thermal Sunyaev-Zel'dovich (TSZ) maps from Planck and the Atacama Cosmology Telescope and weak galaxy lensing shears measured during the first three years of observations of the Dark Energy Survey. This correlation is sensitive to the thermal energy in baryons over a wide redshift range and is therefore a powerful probe of astrophysical feedback. We detect the correlation at a statistical significance of 21σ, the highest significance to date. We examine the TSZ maps for potential contaminants, including cosmic infrared background and radio sources, finding that cosmic infrared background has a substantial impact on our measurements and must be taken into account in our analysis. We use the cross-correlation measurements to test different feedback models. In particular, we model the TSZ using several different pressure profile models calibrated against hydrodynamical simulations. Our analysis marginalizes over redshift uncertainties, shear calibration biases, and intrinsic alignment effects. We also marginalize over ωm and σ8 using Planck or DES priors. We find that the data prefer the model with a low amplitude of the pressure profile at small scales, compatible with a scenario with strong active galactic nuclei feedback and ejection of gas from the inner part of the halos. When using a more flexible model for the shear profile, constraints are weaker, and the data cannot discriminate between different baryonic prescriptions.
Published: 2022

49. Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument

Author: Abareshi, B, Aguilar, J, Ahlen, S, Alam, Shadab, Alexander, David M, Alfarsy, R, Allen, L, Prieto, C Allende, Alves, O, Ameel, J, Armengaud, E, Asorey, J, Aviles, Alejandro, Bailey, S, Balaguera-Antolínez, A, Ballester, O, Baltay, C, Bault, A, Beltran, SF, Benavides, B, BenZvi, S, Berti, A, Besuner, R, Beutler, Florian, Bianchi, D, Blake, C, Blanc, P, Blum, R, Bolton, A, Bose, S, Bramall, D, Brieden, S, Brodzeller, A, Brooks, D, Brownewell, C, Buckley-Geer, E, Cahn, RN, Cai, Z, Canning, R, Rosell, A Carnero, Carton, P, Casas, R, Castander, FJ, Cervantes-Cota, JL, Chabanier, S, Chaussidon, E, Chuang, C, Circosta, C, Cole, S, Cooper, AP, Costa, L da, Cousinou, M-C, Cuceu, A, Davis, TM, Dawson, K, Cruz-Noriega, R de la, Macorra, A de la, Mattia, A de, Costa, J Della, Demmer, P, Derwent, M, Dey, A, Dey, B, Dhungana, G, Ding, Z, Dobson, C, Doel, P, Donald-McCann, J, Donaldson, J, Douglass, K, Duan, Y, Dunlop, P, Edelstein, J, Eftekharzadeh, S, Eisenstein, DJ, Enriquez-Vargas, M, Escoffier, S, Evatt, M, Fagrelius, P, Fan, X, Fanning, K, Fawcett, VA, Ferraro, S, Ereza, J, Flaugher, B, Font-Ribera, A, Forero-Romero, JE, Frenk, CS, Fromenteau, S, Gänsicke, BT, Garcia-Quintero, C, Garrison, L, Gaztañaga, E, Gerardi, F, Gil-Marín, H, Gontcho, S Gontcho A, Gonzalez-Morales, Alma X, Gonzalez-de-Rivera, G, Gonzalez-Perez, V, and Gordon, C
Subjects: astro-ph.IM, astro-ph.CO
Abstract: The Dark Energy Spectroscopic Instrument (DESI) has embarked on an ambitiousfive-year survey to explore the nature of dark energy with spectroscopy of 40million galaxies and quasars. DESI will determine precise redshifts and employthe Baryon Acoustic Oscillation method to measure distances from the nearbyuniverse to z > 3.5, as well as measure the growth of structure and probepotential modifications to general relativity. In this paper we describe thesignificant instrumentation we developed for the DESI survey. The newinstrumentation includes a wide-field, 3.2-deg diameter prime-focus correctorthat focuses the light onto 5020 robotic fiber positioners on the 0.812 mdiameter, aspheric focal surface. The positioners and their fibers are dividedamong ten wedge-shaped petals. Each petal is connected to one of tenspectrographs via a contiguous, high-efficiency, nearly 50 m fiber cablebundle. The ten spectrographs each use a pair of dichroics to split the lightinto three channels that together record the light from 360 - 980 nm with aresolution of 2000 to 5000. We describe the science requirements, technicalrequirements on the instrumentation, and management of the project. DESI wasinstalled at the 4-m Mayall telescope at Kitt Peak, and we also describe thefacility upgrades to prepare for DESI and the installation and functionalverification process. DESI has achieved all of its performance goals, and theDESI survey began in May 2021. Some performance highlights include RMSpositioner accuracy better than 0.1", SNR per \sqrt{\AA} > 0.5 for a z > 2quasar with flux 0.28e-17 erg/s/cm^2/A at 380 nm in 4000s, and median SNR = 7of the [OII] doublet at 8e-17 erg/s/cm^2 in a 1000s exposure for emission linegalaxies at z = 1.4 - 1.6. We conclude with highlights from the on-skyvalidation and commissioning of the instrument, key successes, and lessonslearned. (abridged)
Published: 2022

50. Cross-correlation of DES Y3 lensing and ACT/${\it Planck}$ thermal Sunyaev Zel'dovich Effect I: Measurements, systematics tests, and feedback model constraints

Author: Gatti, M., Pandey, S., Baxter, E., Hill, J. C., Moser, E., Raveri, M., Fang, X., DeRose, J., Giannini, G., Doux, C., Huang, H., Battaglia, N., Alarcon, A., Amon, A., Becker, M., Campos, A., Chang, C., Chen, R., Choi, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferte, A., Harrison, I., Maccrann, N., Mccullough, J., Myles, J., Alsina, A. Navarro, Prat, J., Rollins, R. P., Sanchez, C., Shin, T., Troxel, M., Tutusaus, I., Yin, B., Abbott, T., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bernstein, G., Bertin, E., Bolliet, B., Bond, J. R., Brooks, D., Burke, D. L., Calabrese, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cawthon, R., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. da Silva, DeVicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Dunkley, J., Evrard, A. E., Ferraro, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garcıa-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Herner, K., Hincks, A. D., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hughes, J. P., Huterer, D., Jain, B., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Lima, M., Lokken, M., Madhavacheril, M. S., Maia, M. A. G., Marshall, J. L., Mcmahon, J. J., Melchior, P., Moodley, K., Mohr, J. J., Morgan, R., Nati, F., Niemack, M. D., Page, L., Palmese, A., Paz-Chinchon, F., Pieres, A., Malagon, A. A. Plazas, Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Schaan, E., Secco, L. F., Serrano, S., Sheldon, E., Sherwin, B. D., Sifon, C., Smith, M., Soares-Santos, M., Spergel, D., Suchyta, E., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., Weller, J., Wilkinson, R. D., Wollack, E. J., and Xu, Z.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a tomographic measurement of the cross-correlation between thermal Sunyaev-Zeldovich (tSZ) maps from ${\it Planck}$ and the Atacama Cosmology Telescope (ACT) and weak galaxy lensing shears measured during the first three years of observations of the Dark Energy Survey (DES Y3). This correlation is sensitive to the thermal energy in baryons over a wide redshift range, and is therefore a powerful probe of astrophysical feedback. We detect the correlation at a statistical significance of $21\sigma$, the highest significance to date. We examine the tSZ maps for potential contaminants, including cosmic infrared background (CIB) and radio sources, finding that CIB has a substantial impact on our measurements and must be taken into account in our analysis. We use the cross-correlation measurements to test different feedback models. In particular, we model the tSZ using several different pressure profile models calibrated against hydrodynamical simulations. Our analysis marginalises over redshift uncertainties, shear calibration biases, and intrinsic alignment effects. We also marginalise over $\Omega_{\rm m}$ and $\sigma_8$ using ${\it Planck}$ or DES priors. We find that the data prefers the model with a low amplitude of the pressure profile at small scales, compatible with a scenario with strong AGN feedback and ejection of gas from the inner part of the halos. When using a more flexible model for the shear profile, constraints are weaker, and the data cannot discriminate between different baryonic prescriptions., Comment: submitted to PRD
Published: 2021
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