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Carnegie Supernova Project-I and -II: Measurements of H₀ using Cepheid, TRGB, and SBF Distance Calibration to Type Ia Supernovae
Syed A. Uddin, Christopher R. Burns, Mark M. Phillips, Nicholas B. Suntzeff, Wendy L. Freedman, Peter J. Brown, Nidia Morrell, Mario Hamuy, Kevin Krisciunas, Lifan Wang, Eric Y. Hsiao, Ariel Goobar, Saul Perlmutter, Jing Lu, Maximilian Stritzinger, Joseph P. Anderson, Chris Ashall, Peter Hoeflich, Benjamin J. Shappee, S. E. Persson, Anthony L. Piro, Eddie Baron, Carlos Contreras, Lluís Galbany, Sahana Kumar, Melissa Shahbandeh, Scott Davis, Jorge Anais, Luis Busta, Abdo Campillay, Sergio Castellón, Carlos Corco, Tiara Diamond, Christa Gall, Consuelo Gonzalez, Simon Holmbo, Miguel Roth, Jacqueline Serón, Francesco Taddia, Simón Torres, Charles Baltay, Gastón Folatelli, Ellie Hadjiyska, Mansi Kasliwal, Peter E. Nugent, David Rabinowitz, Stuart D. Ryder
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We present an analysis of Type Ia Supernovae (SNe~Ia) from both the Carnegie Supernova Project~I (CSP-I) and II (CSP-II), and extend the Hubble diagram from the optical to the near-infrared wavelengths (uBgVriYJH). We calculate the Hubble constant, H₀, using various distance calibrators: Cepheids, Tip of the Red Giant Branch (TRGB), and Surface Brightness Fluctuations (SBF). Combining all methods of calibrations, we derive H₀=71.76 ±0.58 (stat) ±1.19 (sys) km s⁻¹ Mpc⁻¹ from B-band, and H₀=73.22 ±0.68 (stat) ±1.28 (sys) km s⁻¹ Mpc⁻¹ from H-band. By assigning equal weight to the Cepheid, TRGB, and SBF calibrators, we derive the systematic errors required for consistency in the first rung of the distance ladder, resulting in a systematic error of 1.2∼1.3 km s⁻¹ Mpc⁻¹ in H₀. As a result, relative to the statistics-only uncertainty, the tension between the late-time H₀ we derive by combining the various distance calibrators and the early-time H₀ from the Cosmic Microwave Background is reduced. The highest precision in SN~Ia luminosity is found in the Y band (0.12±0.01 mag), as defined by the intrinsic scatter (σᵢₙₜ). We revisit SN~Ia Hubble residual-host mass correlations and recover previous results that these correlations do not change significantly between the optical and the near-infrared wavelengths. Finally, SNe~Ia that explode beyond 10 kpc from their host centers exhibit smaller dispersion in their luminosity, confirming our earlier findings. Reduced effect of dust in the outskirt of hosts may be responsible for this effect.
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