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DESI DR2 Galaxy Luminosity Functions

Fuente: arXiv

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Bibliographic Details
Main Authors:	Moore, Samuel G., Cole, Shaun, Wilson, Michael, Norberg, Peder, Moustakas, John, Aguilar, J., Ahlen, S., Anand, A., Bianchi, D., Brooks, D., Castander, F. J., Claybaugh, T., Cuceu, A., de la Macorra, A., Dey, Arjun, Dey, Biprateep, Ferraro, S., Font-Ribera, A., Forero-Romero, J. E., Gaztanaga, E., Gontcho, S. Gontcho A, Gutierrez, G., Herrera-Alcantar, H. K., Honscheid, K., Ishak, M., Joyce, R., Juneau, S., Kehoe, R., Kisner, T., Koposov, S. E., Kremin, A., Lahav, O., Lamman, C., Landriau, M., Guillou, L. Le, Levi, M. E., Lucey, M., Manera, J. R., Meisner, A., Miquel, R., Nadathur, S., Percival, W. J., Poppett, C., Prada, F., Ross, A. J., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Seo, H., Silber, J., Sprayberry, D., Tarlé, G., Weaver, B. A., Wechsler, R. H., Zhou, R., Zou, H.
Format:	Preprint
Published:	2025
Subjects:	Astrophysics of Galaxies
Online Access:	Acceder al recurso
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_version_	1866910208432799744
author	Moore, Samuel G. Cole, Shaun Wilson, Michael Norberg, Peder Moustakas, John Aguilar, J. Ahlen, S. Anand, A. Bianchi, D. Brooks, D. Castander, F. J. Claybaugh, T. Cuceu, A. de la Macorra, A. Dey, Arjun Dey, Biprateep Ferraro, S. Font-Ribera, A. Forero-Romero, J. E. Gaztanaga, E. Gontcho, S. Gontcho A Gutierrez, G. Herrera-Alcantar, H. K. Honscheid, K. Ishak, M. Joyce, R. Juneau, S. Kehoe, R. Kisner, T. Koposov, S. E. Kremin, A. Lahav, O. Lamman, C. Landriau, M. Guillou, L. Le Levi, M. E. Lucey, M. Manera, J. R. Meisner, A. Miquel, R. Nadathur, S. Percival, W. J. Poppett, C. Prada, F. Ross, A. J. Rossi, G. Sanchez, E. Schlegel, D. Schubnell, M. Seo, H. Silber, J. Sprayberry, D. Tarlé, G. Weaver, B. A. Wechsler, R. H. Zhou, R. Zou, H.
author_facet	Moore, Samuel G. Cole, Shaun Wilson, Michael Norberg, Peder Moustakas, John Aguilar, J. Ahlen, S. Anand, A. Bianchi, D. Brooks, D. Castander, F. J. Claybaugh, T. Cuceu, A. de la Macorra, A. Dey, Arjun Dey, Biprateep Ferraro, S. Font-Ribera, A. Forero-Romero, J. E. Gaztanaga, E. Gontcho, S. Gontcho A Gutierrez, G. Herrera-Alcantar, H. K. Honscheid, K. Ishak, M. Joyce, R. Juneau, S. Kehoe, R. Kisner, T. Koposov, S. E. Kremin, A. Lahav, O. Lamman, C. Landriau, M. Guillou, L. Le Levi, M. E. Lucey, M. Manera, J. R. Meisner, A. Miquel, R. Nadathur, S. Percival, W. J. Poppett, C. Prada, F. Ross, A. J. Rossi, G. Sanchez, E. Schlegel, D. Schubnell, M. Seo, H. Silber, J. Sprayberry, D. Tarlé, G. Weaver, B. A. Wechsler, R. H. Zhou, R. Zou, H.
contents	We present galaxy luminosity functions (LFs) for the Dark Energy Spectroscopic Instrument (DESI) DR2 Bright Galaxy Survey (BGS) in the g,r,z, and w1 bands over 0.002<z<0.6. Our analysis uses updated k-corrections and evolutionary corrections, including new polynomial k-correction fits derived from BGS Year1 data that supersede earlier GAMA-based prescriptions. Exploiting the statistical power of DESI, we measure LFs to very faint magnitudes, reaching M_r-5log h = -10. Independent measurements from the North and South survey regions show excellent agreement around the LF knee, but the very small statistical uncertainties reveal that simple analytic forms fail to capture the full LF shape. The bright end departs from a pure exponential decline, while the faint end exhibits complex, non-power-law behaviour, including a pronounced upturn at M_r-5log h > -15, which is stronger for red galaxies than for blue. We show that our LFs are largely complete for galaxies with surface brightness mu_50<25, and that an apparent steepening fainter than -13 is driven primarily by local overdensity and fragmentation of large galaxies. A systematic North-South offset at the brightest magnitudes is traced to red galaxies and may reflect shallower North photometry underestimating extended early-type profiles, although this remains inconclusive. We therefore also provide LFs based on model-Petrosian magnitudes. Redshift-splitting reveals small but significant residuals, indicating limitations of a simple global evolutionary model. Using the redshift limits of Loveday (2011) we find excellent agreement with GAMA, with substantially reduced statistical errors. These measurements provide a precise reference for studies of environmental and population-dependent LFs and for testing galaxy formation models.
format	Preprint
id	arxiv_https___arxiv_org_abs_2511_01803
institution	arXiv
publishDate	2025
record_format	arxiv
spellingShingle	DESI DR2 Galaxy Luminosity Functions Moore, Samuel G. Cole, Shaun Wilson, Michael Norberg, Peder Moustakas, John Aguilar, J. Ahlen, S. Anand, A. Bianchi, D. Brooks, D. Castander, F. J. Claybaugh, T. Cuceu, A. de la Macorra, A. Dey, Arjun Dey, Biprateep Ferraro, S. Font-Ribera, A. Forero-Romero, J. E. Gaztanaga, E. Gontcho, S. Gontcho A Gutierrez, G. Herrera-Alcantar, H. K. Honscheid, K. Ishak, M. Joyce, R. Juneau, S. Kehoe, R. Kisner, T. Koposov, S. E. Kremin, A. Lahav, O. Lamman, C. Landriau, M. Guillou, L. Le Levi, M. E. Lucey, M. Manera, J. R. Meisner, A. Miquel, R. Nadathur, S. Percival, W. J. Poppett, C. Prada, F. Ross, A. J. Rossi, G. Sanchez, E. Schlegel, D. Schubnell, M. Seo, H. Silber, J. Sprayberry, D. Tarlé, G. Weaver, B. A. Wechsler, R. H. Zhou, R. Zou, H. Astrophysics of Galaxies We present galaxy luminosity functions (LFs) for the Dark Energy Spectroscopic Instrument (DESI) DR2 Bright Galaxy Survey (BGS) in the g,r,z, and w1 bands over 0.002<z<0.6. Our analysis uses updated k-corrections and evolutionary corrections, including new polynomial k-correction fits derived from BGS Year1 data that supersede earlier GAMA-based prescriptions. Exploiting the statistical power of DESI, we measure LFs to very faint magnitudes, reaching M_r-5log h = -10. Independent measurements from the North and South survey regions show excellent agreement around the LF knee, but the very small statistical uncertainties reveal that simple analytic forms fail to capture the full LF shape. The bright end departs from a pure exponential decline, while the faint end exhibits complex, non-power-law behaviour, including a pronounced upturn at M_r-5log h > -15, which is stronger for red galaxies than for blue. We show that our LFs are largely complete for galaxies with surface brightness mu_50<25, and that an apparent steepening fainter than -13 is driven primarily by local overdensity and fragmentation of large galaxies. A systematic North-South offset at the brightest magnitudes is traced to red galaxies and may reflect shallower North photometry underestimating extended early-type profiles, although this remains inconclusive. We therefore also provide LFs based on model-Petrosian magnitudes. Redshift-splitting reveals small but significant residuals, indicating limitations of a simple global evolutionary model. Using the redshift limits of Loveday (2011) we find excellent agreement with GAMA, with substantially reduced statistical errors. These measurements provide a precise reference for studies of environmental and population-dependent LFs and for testing galaxy formation models.
title	DESI DR2 Galaxy Luminosity Functions
topic	Astrophysics of Galaxies
url	https://arxiv.org/abs/2511.01803