Carnegie Supernova Project I and II: Measurements of H <sub>0</sub> Using Cepheid, Tip of the Red Giant Branch, and Surface Brightness Fluctuation Distance Calibration to Type Ia Supernovae*
S. A. Uddin, C. R. Burns, M. M. Phillips, N. B. Suntzeff, Wendy L. Freedman, P. J. Brown, N. Morrell, M. Hamuy, K. Krisciunas, Lifan Wang, E. Y. Hsiao, A. Goobar, S. Perlmutter, Jing Lü, M. Stritzinger, J. P. Anderson, C. Ashall, P. Hoêflich, B. J. Shappee, S. E. Persson, Anthony L. Piro, E. Baron, C. Contreras, L. Galbany, Sahana Kumar, Melissa Shahbandeh, Scott Davis, J. Anais, L. Busta, A. Campillay, S. Castellón, C. Corco, T. Diamond, C. Gall, C. González, S. Holmbo, Miguel Roth, J. Serón, F. Taddia, Simón Torres, C. Baltay, G. Folatelli, E. Hadjiyska, M. M. Kasliwal, P. Nugent, D. Rabinowitz, S. D. Ryder
Abstract
Abstract We present an analysis of Type Ia supernovae (SNe Ia) from the Carnegie Supernova Project I and II and extend the Hubble diagram from optical to near-infrared wavelengths ( uBgVriYJH ). We calculate the Hubble constant, H 0 , using various distance calibrators: Cepheids, the tip of the red giant branch (TRGB), and surface brightness fluctuations (SBFs). Combining all methods of calibration, we derive H 0 = 71.76 ± 0.58 (stat) ± 1.19 (sys) km s −1 Mpc −1 from the B band and H 0 = 73.22 ± 0.68 (stat) ± 1.28 (sys) km s −1 Mpc −1 from the 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 H 0 . As a result, relative to the statistics-only uncertainty, the tension between the late-time H 0 we derive by combining the various distance calibrators and the early-time H 0 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 ( σ int ). We revisit SN Ia Hubble residual-host mass correlations and recover previous results that these correlations do not change significantly between the optical and 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. A reduced effect of dust in the outskirts of hosts may be responsible for this effect.