학술논문
The Dark Energy Survey Supernova Program: An updated measurement of the Hubble constant using the Inverse Distance Ladder
Document Type
Working Paper
Author
Camilleri, R.; Davis, T. M.; Hinton, S. R.; Armstrong, P.; Brout, D.; Galbany, L.; Glazebrook, K.; Lee, J.; Lidman, C.; Nichol, R. C.; Sako, M.; Scolnic, D.; Shah, P.; Smith, M.; Sullivan, M.; Sánchez, B. O.; Vincenzi, M.; Wiseman, P.; Allam, S.; Abbott, T. M. C.; Aguena, M.; Andrade-Oliveira, F.; Asorey, J.; Avila, S.; Bacon, D.; Bechtol, K.; Bocquet, S.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Rosell, A. Carnero; Carollo, D.; Carretero, J.; Castander, F. J.; Conselice, C.; da Costa, L. N.; Pereira, M. E. S.; Desai, S.; Diehl, H. T.; Everett, S.; Ferrero, I.; Flaugher, B.; Frieman, J.; García-Bellido, J.; Gaztanaga, E.; Giannini, G.; Gruendl, R. A.; Herner, K.; Hollowood, D. L.; Honscheid, K.; Huterer, D.; James, D. J.; Kent, S.; Kuehn, K.; Lahav, O.; Lee, S.; Lewis, G. F.; Lima, M.; Marshall, J. L.; Mena-Fernández, J.; Miquel, R.; Myles, J.; Ogando, R. L. C.; Palmese, A.; Pieres, A.; Malagón, A. A. Plazas; Romer, A. K.; Roodman, A.; Samuroff, S.; Sanchez, E.; Cid, D. Sanchez; Schubnell, M.; Sevilla-Noarbe, I.; Suchyta, E.; Suntzeff, N.; Swanson, M. E. C.; Tarle, G.; Tucker, B. E.; Walker, A. R.; Weaverdyck, N.
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Subject
Language
Abstract
We measure the current expansion rate of the Universe, Hubble's constant $H_0$, 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 $0.01\lt z \lt1.13$ anchored to the recent Baryon Acoustic Oscillation measurements from DESI spanning $0.30 \lt z_{\mathrm{eff}} \lt 2.33$. 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 $H_0=67.19^{+0.66}_{-0.64}\mathrm{~km} \mathrm{~s}^{-1} \mathrm{~Mpc}^{-1}$, in agreement with the value found by Planck without the need to assume Flat-$\Lambda$CDM. However the best-fitting expansion history differs from that of Planck, providing continued motivation to investigate these tensions.