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Main Authors:	Elbers, W., Aviles, A., Noriega, H. E., Chebat, D., Menegas, A., Frenk, C. S., Garcia-Quintero, C., Gonzalez, D., Ishak, M., Lahav, O., Naidoo, K., Niz, G., Yèche, C., Abdul-Karim, M., Ahlen, S., Alves, O., Andrade, U., Armengaud, E., Behera, J., BenZvi, S., Bianchi, D., Brieden, S., Brodzeller, A., Brooks, D., Burtin, E., Calderon, R., Canning, R., Rosell, A. Carnero, Casas, L., Castander, F. J., Charles, M., Chaussidon, E., Chaves-Montero, J., Claybaugh, T., Cole, S., Cooper, A. P., Cuceu, A., Dawson, K. S., de la Macorra, A., de Mattia, A., Deiosso, N., Dey, A., Dey, B., Ding, Z., Doel, P., Eisenstein, D. J., Ferraro, S., Font-Ribera, A., Forero-Romero, J. E., Garrison, L. H., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gutierrez, G., He, S., Herbold, M., Herrera-Alcantar, H. K., Howlett, C., Huterer, D., Juneau, S., Kehoe, R., Kirkby, D., Kisner, T., Kremin, A., Lamman, C., Landriau, M., Guillou, L. Le, Leauthaud, A., Levi, M. E., Li, Q., Lodha, K., Magneville, C., Manera, M., Martini, P., Matthewson, W. L., Meisner, A., Mena-Fernández, J., Miquel, R., Moustakas, J., Nadathur, S., Newman, J. A., Paillas, E., Palanque-Delabrouille, N., Percival, W. J., Pieri, M. M., Poppett, C., Prada, F., Pérez-Ràfols, I., Rabinowitz, D., Ramírez-Pérez, C., Rashkovetskyi, M., Ravoux, C., Rivera-Morales, H., Rohlf, J., Ross, A. J., Rossi, G., Ruhlmann-Kleider, V., Samushia, L., Sanchez, E., Schlegel, D., Schubnell, M., Seo, H., Sinigaglia, F., Sprayberry, D., Tan, T., Tarlé, G., Taylor, P., Turner, W., Vargas-Magaña, M., Verde, L., Walther, M., Weaver, B. A., Whitford, A., Wolfson, M., Zarrouk, P., Zhao, C., Zhou, R., Zou, H.
Format:	Preprint
Published:	2025
Subjects:	Cosmology and Nongalactic Astrophysics
Online Access:	https://arxiv.org/abs/2503.14744
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author	Elbers, W. Aviles, A. Noriega, H. E. Chebat, D. Menegas, A. Frenk, C. S. Garcia-Quintero, C. Gonzalez, D. Ishak, M. Lahav, O. Naidoo, K. Niz, G. Yèche, C. Abdul-Karim, M. Ahlen, S. Alves, O. Andrade, U. Armengaud, E. Behera, J. BenZvi, S. Bianchi, D. Brieden, S. Brodzeller, A. Brooks, D. Burtin, E. Calderon, R. Canning, R. Rosell, A. Carnero Casas, L. Castander, F. J. Charles, M. Chaussidon, E. Chaves-Montero, J. Claybaugh, T. Cole, S. Cooper, A. P. Cuceu, A. Dawson, K. S. de la Macorra, A. de Mattia, A. Deiosso, N. Dey, A. Dey, B. Ding, Z. Doel, P. Eisenstein, D. J. Ferraro, S. Font-Ribera, A. Forero-Romero, J. E. Garrison, L. H. Gaztañaga, E. Gil-Marín, H. Gontcho, S. Gontcho A Gonzalez-Morales, A. X. Gutierrez, G. He, S. Herbold, M. Herrera-Alcantar, H. K. Howlett, C. Huterer, D. Juneau, S. Kehoe, R. Kirkby, D. Kisner, T. Kremin, A. Lamman, C. Landriau, M. Guillou, L. Le Leauthaud, A. Levi, M. E. Li, Q. Lodha, K. Magneville, C. Manera, M. Martini, P. Matthewson, W. L. Meisner, A. Mena-Fernández, J. Miquel, R. Moustakas, J. Nadathur, S. Newman, J. A. Paillas, E. Palanque-Delabrouille, N. Percival, W. J. Pieri, M. M. Poppett, C. Prada, F. Pérez-Ràfols, I. Rabinowitz, D. Ramírez-Pérez, C. Rashkovetskyi, M. Ravoux, C. Rivera-Morales, H. Rohlf, J. Ross, A. J. Rossi, G. Ruhlmann-Kleider, V. Samushia, L. Sanchez, E. Schlegel, D. Schubnell, M. Seo, H. Sinigaglia, F. Sprayberry, D. Tan, T. Tarlé, G. Taylor, P. Turner, W. Vargas-Magaña, M. Verde, L. Walther, M. Weaver, B. A. Whitford, A. Wolfson, M. Zarrouk, P. Zhao, C. Zhou, R. Zou, H.
author_facet	Elbers, W. Aviles, A. Noriega, H. E. Chebat, D. Menegas, A. Frenk, C. S. Garcia-Quintero, C. Gonzalez, D. Ishak, M. Lahav, O. Naidoo, K. Niz, G. Yèche, C. Abdul-Karim, M. Ahlen, S. Alves, O. Andrade, U. Armengaud, E. Behera, J. BenZvi, S. Bianchi, D. Brieden, S. Brodzeller, A. Brooks, D. Burtin, E. Calderon, R. Canning, R. Rosell, A. Carnero Casas, L. Castander, F. J. Charles, M. Chaussidon, E. Chaves-Montero, J. Claybaugh, T. Cole, S. Cooper, A. P. Cuceu, A. Dawson, K. S. de la Macorra, A. de Mattia, A. Deiosso, N. Dey, A. Dey, B. Ding, Z. Doel, P. Eisenstein, D. J. Ferraro, S. Font-Ribera, A. Forero-Romero, J. E. Garrison, L. H. Gaztañaga, E. Gil-Marín, H. Gontcho, S. Gontcho A Gonzalez-Morales, A. X. Gutierrez, G. He, S. Herbold, M. Herrera-Alcantar, H. K. Howlett, C. Huterer, D. Juneau, S. Kehoe, R. Kirkby, D. Kisner, T. Kremin, A. Lamman, C. Landriau, M. Guillou, L. Le Leauthaud, A. Levi, M. E. Li, Q. Lodha, K. Magneville, C. Manera, M. Martini, P. Matthewson, W. L. Meisner, A. Mena-Fernández, J. Miquel, R. Moustakas, J. Nadathur, S. Newman, J. A. Paillas, E. Palanque-Delabrouille, N. Percival, W. J. Pieri, M. M. Poppett, C. Prada, F. Pérez-Ràfols, I. Rabinowitz, D. Ramírez-Pérez, C. Rashkovetskyi, M. Ravoux, C. Rivera-Morales, H. Rohlf, J. Ross, A. J. Rossi, G. Ruhlmann-Kleider, V. Samushia, L. Sanchez, E. Schlegel, D. Schubnell, M. Seo, H. Sinigaglia, F. Sprayberry, D. Tan, T. Tarlé, G. Taylor, P. Turner, W. Vargas-Magaña, M. Verde, L. Walther, M. Weaver, B. A. Whitford, A. Wolfson, M. Zarrouk, P. Zhao, C. Zhou, R. Zou, H.
contents	The Dark Energy Spectroscopic Instrument (DESI) Collaboration has obtained robust measurements of baryon acoustic oscillations (BAO) in the redshift range, $0.1 < z < 4.2$, based on the Lyman-$α$ forest and galaxies from Data Release 2 (DR2). We combine these measurements with external cosmic microwave background (CMB) data from Planck and ACT to place our tightest constraints yet on the sum of neutrino masses. Assuming the cosmological $Λ$CDM model and three degenerate neutrino states, we find $\sum m_ν<0.0642$ eV (95%) with a marginalized error of $σ(\sum m_ν)=0.020$ eV. We also constrain the effective number of neutrino species, finding $N_\rm{eff} = 3.23^{+0.35}_{-0.34}$ (95%), in line with the Standard Model prediction. When accounting for neutrino oscillation constraints, we find a preference for the normal mass ordering and an upper limit on the lightest neutrino mass of $m_l < 0.023$ eV (95%). However, we determine using frequentist and Bayesian methods that our constraints are in tension with the lower limits derived from neutrino oscillations. Correcting for the physical boundary at zero mass, we report a 95% Feldman-Cousins upper limit of $\sum m_ν<0.053$ eV, breaching the lower limit from neutrino oscillations. Considering a more general Bayesian analysis with an effective cosmological neutrino mass parameter, $\sum m_{ν,\rm{eff}}$, that allows for negative energy densities and removes unsatisfactory prior weight effects, we derive constraints that are in $3σ$ tension with the same oscillation limit. In the absence of unknown systematics, this finding could be interpreted as a hint of new physics not necessarily related to neutrinos. The preference of DESI and CMB data for an evolving dark energy model offers one possible solution. In the $w_0w_a$CDM model, we find $\sum m_ν<0.163$ eV (95%), relaxing the neutrino tension. [Abridged]
format	Preprint
id	arxiv_https___arxiv_org_abs_2503_14744
institution	arXiv
publishDate	2025
record_format	arxiv
spellingShingle	Constraints on Neutrino Physics from DESI DR2 BAO and DR1 Full Shape Elbers, W. Aviles, A. Noriega, H. E. Chebat, D. Menegas, A. Frenk, C. S. Garcia-Quintero, C. Gonzalez, D. Ishak, M. Lahav, O. Naidoo, K. Niz, G. Yèche, C. Abdul-Karim, M. Ahlen, S. Alves, O. Andrade, U. Armengaud, E. Behera, J. BenZvi, S. Bianchi, D. Brieden, S. Brodzeller, A. Brooks, D. Burtin, E. Calderon, R. Canning, R. Rosell, A. Carnero Casas, L. Castander, F. J. Charles, M. Chaussidon, E. Chaves-Montero, J. Claybaugh, T. Cole, S. Cooper, A. P. Cuceu, A. Dawson, K. S. de la Macorra, A. de Mattia, A. Deiosso, N. Dey, A. Dey, B. Ding, Z. Doel, P. Eisenstein, D. J. Ferraro, S. Font-Ribera, A. Forero-Romero, J. E. Garrison, L. H. Gaztañaga, E. Gil-Marín, H. Gontcho, S. Gontcho A Gonzalez-Morales, A. X. Gutierrez, G. He, S. Herbold, M. Herrera-Alcantar, H. K. Howlett, C. Huterer, D. Juneau, S. Kehoe, R. Kirkby, D. Kisner, T. Kremin, A. Lamman, C. Landriau, M. Guillou, L. Le Leauthaud, A. Levi, M. E. Li, Q. Lodha, K. Magneville, C. Manera, M. Martini, P. Matthewson, W. L. Meisner, A. Mena-Fernández, J. Miquel, R. Moustakas, J. Nadathur, S. Newman, J. A. Paillas, E. Palanque-Delabrouille, N. Percival, W. J. Pieri, M. M. Poppett, C. Prada, F. Pérez-Ràfols, I. Rabinowitz, D. Ramírez-Pérez, C. Rashkovetskyi, M. Ravoux, C. Rivera-Morales, H. Rohlf, J. Ross, A. J. Rossi, G. Ruhlmann-Kleider, V. Samushia, L. Sanchez, E. Schlegel, D. Schubnell, M. Seo, H. Sinigaglia, F. Sprayberry, D. Tan, T. Tarlé, G. Taylor, P. Turner, W. Vargas-Magaña, M. Verde, L. Walther, M. Weaver, B. A. Whitford, A. Wolfson, M. Zarrouk, P. Zhao, C. Zhou, R. Zou, H. Cosmology and Nongalactic Astrophysics The Dark Energy Spectroscopic Instrument (DESI) Collaboration has obtained robust measurements of baryon acoustic oscillations (BAO) in the redshift range, $0.1 < z < 4.2$, based on the Lyman-$α$ forest and galaxies from Data Release 2 (DR2). We combine these measurements with external cosmic microwave background (CMB) data from Planck and ACT to place our tightest constraints yet on the sum of neutrino masses. Assuming the cosmological $Λ$CDM model and three degenerate neutrino states, we find $\sum m_ν<0.0642$ eV (95%) with a marginalized error of $σ(\sum m_ν)=0.020$ eV. We also constrain the effective number of neutrino species, finding $N_\rm{eff} = 3.23^{+0.35}_{-0.34}$ (95%), in line with the Standard Model prediction. When accounting for neutrino oscillation constraints, we find a preference for the normal mass ordering and an upper limit on the lightest neutrino mass of $m_l < 0.023$ eV (95%). However, we determine using frequentist and Bayesian methods that our constraints are in tension with the lower limits derived from neutrino oscillations. Correcting for the physical boundary at zero mass, we report a 95% Feldman-Cousins upper limit of $\sum m_ν<0.053$ eV, breaching the lower limit from neutrino oscillations. Considering a more general Bayesian analysis with an effective cosmological neutrino mass parameter, $\sum m_{ν,\rm{eff}}$, that allows for negative energy densities and removes unsatisfactory prior weight effects, we derive constraints that are in $3σ$ tension with the same oscillation limit. In the absence of unknown systematics, this finding could be interpreted as a hint of new physics not necessarily related to neutrinos. The preference of DESI and CMB data for an evolving dark energy model offers one possible solution. In the $w_0w_a$CDM model, we find $\sum m_ν<0.163$ eV (95%), relaxing the neutrino tension. [Abridged]
title	Constraints on Neutrino Physics from DESI DR2 BAO and DR1 Full Shape
topic	Cosmology and Nongalactic Astrophysics
url	https://arxiv.org/abs/2503.14744

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