Papers › The Dark Energy Survey Supernova Program: An updated measurement of the Hubble...
The Dark Energy Survey Supernova Program: An updated measurement of the Hubble constant using the Inverse Distance Ladder
R. Camilleri, T. M. Davis, S. R. Hinton, P. Armstrong, D. Brout, L. Galbany, K. Glazebrook, J. Lee, C. Lidman, R. C. Nichol, M. Sako, D. Scolnic, P. Shah, M. Smith, M. Sullivan, B. O. Sánchez, M. Vincenzi, P. Wiseman, S. Allam, T. M. C. Abbott, M. Aguena, F. Andrade-Oliveira, J. Asorey, S. Avila, D. Bacon, K. Bechtol, S. Bocquet, D. Brooks, E. Buckley-Geer, D. L. Burke, A. Carnero Rosell, D. Carollo, J. Carretero, F. J. Castander, C. Conselice, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, S. Everett, I. Ferrero, B. Flaugher, J. Frieman, J. García-Bellido, E. Gaztanaga, G. Giannini, R. A. Gruendl, K. Herner, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, S. Kent, K. Kuehn, O. Lahav, S. Lee, G. F. Lewis, M. Lima, J. L. Marshall, J. Mena-Fernández, R. Miquel, J. Myles, R. L. C. Ogando, A. Palmese, A. Pieres, A. A. Plazas Malagón, A. K. Romer, A. Roodman, S. Samuroff, E. Sanchez, D. Sanchez Cid, M. Schubnell, I. Sevilla-Noarbe, E. Suchyta, N. Suntzeff, M. E. C. Swanson, G. Tarle, B. E. Tucker, A. R. Walker, N. Weaverdyck
The archive published only this paper's code-link row. Authors, date and abstract are from arXiv's metadata (CC0), read from the Kaggle arXiv metadata snapshot of 2026-09-12 where its title matched the archive's; the title is the archive's.
We measure the current expansion rate of the Universe, Hubble's constant H₀, by calibrating the absolute magnitudes of supernovae to distances measured by Baryon Acoustic Oscillations. This `inverse distance ladder' technique provides an alternative to calibrating supernovae using nearby absolute distance measurements, replacing the calibration with a high-redshift anchor. We use the recent release of 1829 supernovae from the Dark Energy Survey spanning 0.01z 1.13 anchored to the recent Baryon Acoustic Oscillation measurements from DESI spanning 0.30 z_(eff) 2.33. To trace cosmology to z=0, we use the third-, fourth- and fifth-order cosmographic models, which, by design, are agnostic about the energy content and expansion history of the universe. With the inclusion of the higher-redshift DESI-BAO data, the third-order model is a poor fit to both data sets, with the fourth-order model being preferred by the Akaike Information Criterion. Using the fourth-order cosmographic model, we find H₀=67.19^(+0.66)_(-0.64) km s⁻¹ Mpc⁻¹, in agreement with the value found by Planck without the need to assume Flat-ΛCDM. However the best-fitting expansion history differs from that of Planck, providing continued motivation to investigate these tensions.
Code
Repository list and official/mentioned flags are the archive's, frozen 2025-07-28. Reachability, where shown, is from one Syntology probe window (2026-09-16 to 2026-09-18); repositories not probed show nothing. GitHub stars are not tracked.
Code Syntology ran Syntology
Not run by Syntology. Nothing on this page verifies that the listed code works.
Results from the paper archive 2025-07-28
No leaderboard rows for this paper in the archive.
Report a problem or propose a change · a person checks every report against the paper or source before anything changes; decisions are listed on /corrections