DESI 2024 VII: cosmological constraints from the full-shape modeling of clustering measurements

Adame, A.G.; Aguilar, J.; Ahlen, S.; Alam, S.; Alexander, D.M.; Allende Prieto, C.; 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.; Carnero Rosell, A.; 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.G.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.-.; Landriau, M.; Lang, D.; Lasker, J.; Le Goff, J.M.; Le Guillou, L.; Leauthaud, A.; Levi, M.E.; T. S., L.; 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.; Zou, H.; Null, N.

doi:10.1088/1475-7516/2025/07/028

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 thoroughly validated in a series of supporting papers as summarised in [1]. We combine the full-shape information with DESI's DR1 constraints from the baryon acoustic oscillations (BAO) of these tracers. 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(m) = 0.2962 +/- 0.0095, and the amplitude of mass fluctuations to sigma(8) = 0.842 +/- 0.034. The addition of the cosmic microwave background (CMB) data tightens these constraints to Omega(m) = 0.3056 +/- 0.0049 and sigma(8) = 0.8121 +/- 0.0053, while further addition of the joint clustering and lensing analysis from the Dark Energy Survey Year-3 (DESY3) data further improves these measurements, and leads to a 0.4% determination of the Hubble constant, H-0 = (68.40 +/- 0.27) km s(-1) Mpc(-1). In models with a time-varying dark energy equation of state parametrised by w(0) and w(a), 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, improve the upper limits on the sum of the neutrino masses relative to the case when only the DR1 BAO was available, giving Sigma m(nu) < 0.071 eV at 95% confidence. We finally constrain deviations from general relativity represented by two modified gravity parameters. DESI (FS+BAO) data alone measure the parameter that controls the clustering of massive particles, mu(0) = 0.11(-0.54)(+0.45), in agreement with the zero value predicted by general relativity. 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 +/- 0.22 and Sigma(0) = 0.044 +/- 0.047, again in agreement with general relativity.

DESI 2024 VII: cosmological constraints from the full-shape modeling of clustering measurements / A.G. Adame, J. Aguilar, S. Ahlen, S. Alam, D.M. Alexander, C. Allende Prieto, M. Alvarez, O. Alves, A. Anand, U. Andrade, E. Armengaud, S. Avila, A. Aviles, H. Awan, B. Bahr-Kalus, S. Bailey, C. Baltay, A. Bault, J. Behera, S. Benzvi, F. Beutler, D. Bianchi, C. Blake, R. Blum, M. Bonici, S. Brieden, A. Brodzeller, D. Brooks, E. Buckley-Geer, E. Burtin, R. Calderon, R. Canning, A. Carnero Rosell, R. Cereskaite, J.L. Cervantes-Cota, S. Chabanier, E. Chaussidon, J. Chaves-Montero, D. Chebat, S. Chen, X. Chen, T. Claybaugh, S. Cole, A. Cuceu, T.M. Davis, K. Dawson, A. De La Macorra, A. De Mattia, N. Deiosso, A. Dey, B. Dey, Z. Ding, P. Doel, J. Edelstein, S. Eftekharzadeh, D.J. Eisenstein, W. Elbers, A. Elliott, P. Fagrelius, K. Fanning, S. Ferraro, J. Ereza, N. Findlay, B. Flaugher, A. Font-Ribera, D. Forero-Sánchez, J.E. Forero-Romero, C.S. Frenk, C. Garcia-Quintero, L.H. Garrison, E. Gaztañaga, H. Gil-Marín, S.G.A. Gontcho, A.X. Gonzalez-Morales, V. Gonzalez-Perez, C. Gordon, D. Green, D. Gruen, R. Gsponer, G. Gutierrez, J. Guy, B. Hadzhiyska, C. Hahn, M.M.S. Hanif, H.K. Herrera-Alcantar, K. Honscheid, C. Howlett, D. Huterer, V. Iršič, M. Ishak, R. Joyce, S. Juneau, N.G. Karaçaylı, R. Kehoe, S. Kent, D. Kirkby, H. Kong, S.E. Koposov, A. Kremin, A. Krolewski, O. Lahav, Y. Lai, T.-. Lan, M. Landriau, D. Lang, J. Lasker, J.M. Le Goff, L. Le Guillou, A. Leauthaud, M.E. Levi, T.S. Li, K. Lodha, C. Magneville, M. Manera, D. Margala, P. Martini, W. Matthewson, M. Maus, P. Mcdonald, L. Medina-Varela, A. Meisner, J. Mena-Fernández, R. Miquel, J. Moon, S. Moore, J. Moustakas, N. Mudur, E. Mueller, A. Muñoz-Gutiérrez, A.D. Myers, S. Nadathur, L. Napolitano, R. Neveux, J.A. Newman, N.M. Nguyen, J. Nie, G. Niz, H.E. Noriega, N. Padmanabhan, E. Paillas, N. Palanque-Delabrouille, J. Pan, S. Penmetsa, W.J. Percival, M.M. Pieri, M. Pinon, C. Poppett, A. Porredon, F. Prada, A. Pérez-Fernández, I. Pérez-Ràfols, D. Rabinowitz, A. Raichoor, C. Ramírez-Pérez, S. Ramirez-Solano, M. Rashkovetskyi, C. Ravoux, M. Rezaie, J. Rich, A. Rocher, C. Rockosi, N.A. Roe, A. Rosado-Marin, A.J. Ross, G. Rossi, R. Ruggeri, V. Ruhlmann-Kleider, L. Samushia, E. Sanchez, C. Saulder, E.F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, A. Shafieloo, R. Sharples, J. Silber, A. Slosar, A. Smith, D. Sprayberry, T. Tan, G. Tarlé, P. Taylor, S. Trusov, R. Vaisakh, D. Valcin, F. Valdes, G. Valogiannis, M. Vargas-Magaña, L. Verde, M. Walther, B. Wang, M.S. Wang, B.A. Weaver, N. Weaverdyck, R.H. Wechsler, D.H. Weinberg, M. White, M.J. Wilson, L. Yi, J. Yu, Y. Yu, S. Yuan, C. Yèche, E.A. Zaborowski, P. Zarrouk, H. Zhang, C. Zhao, R. Zhao, R. Zhou, T. Zhuang, H. Zou, N. Null. - In: JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS. - ISSN 1475-7516. - 2025:07(2025 Jul 09), pp. 1-54. [10.1088/1475-7516/2025/07/028]

DESI 2024 VII: cosmological constraints from the full-shape modeling of clustering measurements

Adame, A. G.;Aguilar, J.;Ahlen, S.;Alam, S.;Alexander, D. M.;Allende Prieto, C.;Alvarez, M.;Alves, O.;A. Anand;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.;D. Bianchi;Blake, C.;Blum, R.;Bonici, M.;Brieden, S.;Brodzeller, A.;Brooks, D.;Buckley-Geer, E.;Burtin, E.;Calderon, R.;Canning, R.;Carnero Rosell, A.;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.;Le Goff, J. M.;Le Guillou, L.;Leauthaud, A.;Levi, M. E.;Li, T. S.;Lodha, K.;Magneville, C.;M. Manera;Margala, D.;P. Martini;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.;F. Prada;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.;E. Sanchez;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.;Y. Yu;Yuan, S.;Yèche, C.;Zaborowski, E. A.;Zarrouk, P.;H. Zhang;Zhao, C.;Zhao, R.;Zhou, R.;Zhuang, T.;Zou, H.;null, null

2025

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 thoroughly validated in a series of supporting papers as summarised in [1]. We combine the full-shape information with DESI's DR1 constraints from the baryon acoustic oscillations (BAO) of these tracers. 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(m) = 0.2962 +/- 0.0095, and the amplitude of mass fluctuations to sigma(8) = 0.842 +/- 0.034. The addition of the cosmic microwave background (CMB) data tightens these constraints to Omega(m) = 0.3056 +/- 0.0049 and sigma(8) = 0.8121 +/- 0.0053, while further addition of the joint clustering and lensing analysis from the Dark Energy Survey Year-3 (DESY3) data further improves these measurements, and leads to a 0.4% determination of the Hubble constant, H-0 = (68.40 +/- 0.27) km s(-1) Mpc(-1). In models with a time-varying dark energy equation of state parametrised by w(0) and w(a), 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, improve the upper limits on the sum of the neutrino masses relative to the case when only the DR1 BAO was available, giving Sigma m(nu) < 0.071 eV at 95% confidence. We finally constrain deviations from general relativity represented by two modified gravity parameters. DESI (FS+BAO) data alone measure the parameter that controls the clustering of massive particles, mu(0) = 0.11(-0.54)(+0.45), in agreement with the zero value predicted by general relativity. 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 +/- 0.22 and Sigma(0) = 0.044 +/- 0.047, again in agreement with general relativity.

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	Parole chiave
	
				dark energy; experimentsredshift; surveyspower; spectrummodified; gravity
			
	Settori scientifico-disciplinari dell'articolo (validi dal 09/05/2024)
	
				Settore PHYS-05/A - Astrofisica, cosmologia e scienza dello spazio
			
	Data di pubblicazione
	
				9-lug-2025
			
	Rivista in ANCE
	
				JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
			
	DOI
	
				https://dx.doi.org/10.1088/1475-7516/2025/07/028
			
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				Article (author)
			
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				01 - Articolo su periodico

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