Carnegie Supernova Project I and II: Measurements of H 0 Using Cepheid, Tip of the Red Giant Branch, and Surface Brightness Fluctuation Distance Calibration to Type Ia Supernovae
Gall, Christa; Ryder, Stuart D.; Morrell, Nidia; Freedman, Wendy L.; Baron, E.; Wang, Lifan; Shappee, Benjamin J.; Phillips, M. M.; Persson, S. E.; Krisciunas, Kevin; Suntzeff, Nicholas B.; Nugent, Peter E.; Taddia, Francesco; Piro, Anthony L.; Perlmutter, Saul; Kumar, Sahana; Baltay, Charles; Rabinowitz, David; Galbany, Lluís; Folatelli, Gastón; Hamuy, Mario; Brown, Peter J.; Shahbandeh, Melissa; Burns, Christopher R.; Contreras, Carlos; Roth, Miguel; Goobar, Ariel; Uddin, Syed A.; Anderson, Joseph P.; Kasliwal, Mansi; Stritzinger, Maximilian; Holmbo, Simon; Campillay, Abdo; Busta, Luis; Hoeflich, Peter; Ashall, Chris; Lu, Jing; Hsiao, Eric Y.; Castellón, Sergio; Davis, Scott; Anais, Jorge; Corco, Carlos; Diamond, Tiara; Gonzalez, Consuelo; Serón, Jacqueline; Torres, Simón; Hadjiyska, Ellie
United States, Chile, Sweden, Denmark, Germany, Spain, Argentina, Australia
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. *This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.