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Main Authors:	Zaborowski, E. A., Taylor, P., Honscheid, K., Cuceu, A., de Mattia, A., Krolewski, A., Rashkovetskyi, M., Ross, A. J., To, C., Aguilar, J., Ahlen, S., Anand, A., BenZvi, S., Bianchi, D., Brooks, D., Castander, F. J., Claybaugh, T., de la Macorra, A., Della Costa, J., Doel, P., Ferraro, S., Font-Ribera, A., Forero-Romero, J. E., Gaztañaga, E., Gutierrez, G., Herrera-Alcantar, H. K., Howlett, C., Huterer, D., Ishak, M., Joyce, R., Kirkby, D., Kisner, T., Kremin, A., Lahav, O., Lamman, C., Landriau, M., Guillou, L. Le, Manera, M., Martini, P., Meisner, A., Miquel, R., Moustakas, J., Nadathur, S., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Prada, F., Pérez-Ràfols, I., Rossi, G., Samushia, L., Sanchez, E., Schlegel, D., Schubnell, M., Seo, H., Silber, J., Sprayberry, D., Tarlé, G., Weaver, B. A., Zarrouk, P., Zhou, R., Zou, H.
Format:	Preprint
Published:	2025
Subjects:	Cosmology and Nongalactic Astrophysics
Online Access:	https://arxiv.org/abs/2510.19149
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_version_	1866915961612795904
author	Zaborowski, E. A. Taylor, P. Honscheid, K. Cuceu, A. de Mattia, A. Krolewski, A. Rashkovetskyi, M. Ross, A. J. To, C. Aguilar, J. Ahlen, S. Anand, A. BenZvi, S. Bianchi, D. Brooks, D. Castander, F. J. Claybaugh, T. de la Macorra, A. Della Costa, J. Doel, P. Ferraro, S. Font-Ribera, A. Forero-Romero, J. E. Gaztañaga, E. Gutierrez, G. Herrera-Alcantar, H. K. Howlett, C. Huterer, D. Ishak, M. Joyce, R. Kirkby, D. Kisner, T. Kremin, A. Lahav, O. Lamman, C. Landriau, M. Guillou, L. Le Manera, M. Martini, P. Meisner, A. Miquel, R. Moustakas, J. Nadathur, S. Niz, G. Palanque-Delabrouille, N. Percival, W. J. Prada, F. Pérez-Ràfols, I. Rossi, G. Samushia, L. Sanchez, E. Schlegel, D. Schubnell, M. Seo, H. Silber, J. Sprayberry, D. Tarlé, G. Weaver, B. A. Zarrouk, P. Zhou, R. Zou, H.
author_facet	Zaborowski, E. A. Taylor, P. Honscheid, K. Cuceu, A. de Mattia, A. Krolewski, A. Rashkovetskyi, M. Ross, A. J. To, C. Aguilar, J. Ahlen, S. Anand, A. BenZvi, S. Bianchi, D. Brooks, D. Castander, F. J. Claybaugh, T. de la Macorra, A. Della Costa, J. Doel, P. Ferraro, S. Font-Ribera, A. Forero-Romero, J. E. Gaztañaga, E. Gutierrez, G. Herrera-Alcantar, H. K. Howlett, C. Huterer, D. Ishak, M. Joyce, R. Kirkby, D. Kisner, T. Kremin, A. Lahav, O. Lamman, C. Landriau, M. Guillou, L. Le Manera, M. Martini, P. Meisner, A. Miquel, R. Moustakas, J. Nadathur, S. Niz, G. Palanque-Delabrouille, N. Percival, W. J. Prada, F. Pérez-Ràfols, I. Rossi, G. Samushia, L. Sanchez, E. Schlegel, D. Schubnell, M. Seo, H. Silber, J. Sprayberry, D. Tarlé, G. Weaver, B. A. Zarrouk, P. Zhou, R. Zou, H.
contents	The sound horizon scale $r_s$ is a key source of information for early-time $H_0$ measurements, and is therefore a common target of new physics proposed to solve the Hubble tension. We present a sub-2% measurement of the Hubble constant that is independent of this scale, using data from the first data release of the Dark Energy Spectroscopic Instrument (DESI DR1). Building on previous work, we remove dependency on the sound horizon size using a heuristic rescaling procedure at the power spectrum level. A key innovation is the inclusion of \emph{uncalibrated} (agnostic to $r_s$) post-reconstruction BAO measurements from DESI DR1, as well as using the CMB acoustic scale $θ_*$ as a high-redshift anchor. Uncalibrated type-Ia supernovae are often included as an independent source of $Ω_m$ information; here we demonstrate the robustness of our results by additionally considering two supernova-independent alternative datasets. We find somewhat higher values of $H_0$ relative to our previous work: $69.2^{+1.3}_{-1.4}$, $70.3^{+1.4}_{-1.2}$, and $69.6^{+1.3}_{-1.8}\,{\rm km\,s^{-1}\,Mpc^{-1}}$ respectively when including measurements from i) Planck/ACT CMB lensing $\times$ unWISE galaxies, ii) the DES Year 3 6$\times$2pt analysis, and iii) Planck/ACT CMB lensing + the DES Year 5 supernova analysis. These remarkably consistent constraints achieve better than 2% precision; they are among the most stringent sound horizon-independent measurements from LSS to date, and provide a powerful avenue for probing the origin of the Hubble tension.
format	Preprint
id	arxiv_https___arxiv_org_abs_2510_19149
institution	arXiv
publishDate	2025
record_format	arxiv
spellingShingle	$H_0$ Without the Sound Horizon (or Supernovae): A 2% Measurement in DESI DR1 Zaborowski, E. A. Taylor, P. Honscheid, K. Cuceu, A. de Mattia, A. Krolewski, A. Rashkovetskyi, M. Ross, A. J. To, C. Aguilar, J. Ahlen, S. Anand, A. BenZvi, S. Bianchi, D. Brooks, D. Castander, F. J. Claybaugh, T. de la Macorra, A. Della Costa, J. Doel, P. Ferraro, S. Font-Ribera, A. Forero-Romero, J. E. Gaztañaga, E. Gutierrez, G. Herrera-Alcantar, H. K. Howlett, C. Huterer, D. Ishak, M. Joyce, R. Kirkby, D. Kisner, T. Kremin, A. Lahav, O. Lamman, C. Landriau, M. Guillou, L. Le Manera, M. Martini, P. Meisner, A. Miquel, R. Moustakas, J. Nadathur, S. Niz, G. Palanque-Delabrouille, N. Percival, W. J. Prada, F. Pérez-Ràfols, I. Rossi, G. Samushia, L. Sanchez, E. Schlegel, D. Schubnell, M. Seo, H. Silber, J. Sprayberry, D. Tarlé, G. Weaver, B. A. Zarrouk, P. Zhou, R. Zou, H. Cosmology and Nongalactic Astrophysics The sound horizon scale $r_s$ is a key source of information for early-time $H_0$ measurements, and is therefore a common target of new physics proposed to solve the Hubble tension. We present a sub-2% measurement of the Hubble constant that is independent of this scale, using data from the first data release of the Dark Energy Spectroscopic Instrument (DESI DR1). Building on previous work, we remove dependency on the sound horizon size using a heuristic rescaling procedure at the power spectrum level. A key innovation is the inclusion of \emph{uncalibrated} (agnostic to $r_s$) post-reconstruction BAO measurements from DESI DR1, as well as using the CMB acoustic scale $θ_*$ as a high-redshift anchor. Uncalibrated type-Ia supernovae are often included as an independent source of $Ω_m$ information; here we demonstrate the robustness of our results by additionally considering two supernova-independent alternative datasets. We find somewhat higher values of $H_0$ relative to our previous work: $69.2^{+1.3}_{-1.4}$, $70.3^{+1.4}_{-1.2}$, and $69.6^{+1.3}_{-1.8}\,{\rm km\,s^{-1}\,Mpc^{-1}}$ respectively when including measurements from i) Planck/ACT CMB lensing $\times$ unWISE galaxies, ii) the DES Year 3 6$\times$2pt analysis, and iii) Planck/ACT CMB lensing + the DES Year 5 supernova analysis. These remarkably consistent constraints achieve better than 2% precision; they are among the most stringent sound horizon-independent measurements from LSS to date, and provide a powerful avenue for probing the origin of the Hubble tension.
title	$H_0$ Without the Sound Horizon (or Supernovae): A 2% Measurement in DESI DR1
topic	Cosmology and Nongalactic Astrophysics
url	https://arxiv.org/abs/2510.19149

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