%0 Generic %1 uddin2023carnegie %A Uddin, Syed A. %A Burns, Christopher R. %A Phillips, Mark M. %A Suntzeff, Nicholas B. %A Freedman, Wendy L. %A Brown, Peter J. %A Morrell, Nidia %A Hamuy, Mario %A Krisciunas, Kevin %A Wang, Lifan %A Hsiao, Eric Y. %A Goobar, Ariel %A Perlmutter, Saul %A Lu, Jing %A Stritzinger, Maximilian %A Anderson, Joseph P. %A Ashall, Chris %A Hoeflich, Peter %A Shappee, Benjamin J. %A Persson, S. E. %A Piro, Anthony L. %A Baron, Eddie %A Contreras, Carlos %A Galbany, Lluís %A Kumar, Sahana %A Shahbandeh, Melissa %A Davis, Scott %A Anais, Jorge %A Busta, Luis %A Campillay, Abdo %A Castellón, Sergio %A Corco, Carlos %A Diamond, Tiara %A Gall, Christa %A Gonzalez, Consuelo %A Holmbo, Simon %A Roth, Miguel %A Serón, Jacqueline %A Taddia, Francesco %A Torres, Simón %A Baltay, Charles %A Folatelli, Gastón %A Hadjiyska, Ellie %A Kasliwal, Mansi %A Nugent, Peter E. %A Rabinowitz, David %A Ryder, Stuart D. %A Schmidt, Brian P. %D 2023 %K tifr %T Carnegie Supernova Project-I and -II: Measurements of $H_0$ using Cepheid, TRGB, and SBF Distance Calibration to Type Ia Supernovae %U http://arxiv.org/abs/2308.01875 %X 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, $H_0$ using various distance calibrators: Cepheids, Tip of the Red Giant Branch (TRGB), and Surface Brightness Fluctuations (SBF). Combining all methods of calibrations, we derive $H_0=71.43 0.62 \ (stat) \pm 2.43 \ (sys) \ km \ s^-1 \ Mpc^-1$ from $B$-band, and $H_0=72.65 \pm 0.63 \ (stat) 2.88 \ (sys) \ km \ s^-1 \ Mpc^-1$ 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 an increased systematic error in $H_0$. As a result, 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 ($0.12\pm0.01$ mag), as defined by the intrinsic scatter ($\sigma_int$). We revisit SN~Ia Hubble residual-host mass correlations and recover previous results that these correlations do not change significantly between the optical and 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.

@misc{uddin2023carnegie, abstract = {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, $H_0$ using various distance calibrators: Cepheids, Tip of the Red Giant Branch (TRGB), and Surface Brightness Fluctuations (SBF). Combining all methods of calibrations, we derive $\rm H_0=71.43 \pm 0.62 \ (stat) \pm 2.43 \ (sys) \ km \ s^{-1} \ Mpc^{-1}$ from $B$-band, and $\rm H_0=72.65 \pm 0.63 \ (stat) \pm 2.88 \ (sys) \ km \ s^{-1} \ Mpc^{-1}$ 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 an increased systematic error in $H_0$. As a result, 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 ($0.12\pm0.01$ mag), as defined by the intrinsic scatter ($\sigma_{int}$). We revisit SN~Ia Hubble residual-host mass correlations and recover previous results that these correlations do not change significantly between the optical and 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.}, added-at = {2023-08-04T05:42:16.000+0200}, author = {Uddin, Syed A. and Burns, Christopher R. and Phillips, Mark M. and Suntzeff, Nicholas B. and Freedman, Wendy L. and Brown, Peter J. and Morrell, Nidia and Hamuy, Mario and Krisciunas, Kevin and Wang, Lifan and Hsiao, Eric Y. and Goobar, Ariel and Perlmutter, Saul and Lu, Jing and Stritzinger, Maximilian and Anderson, Joseph P. and Ashall, Chris and Hoeflich, Peter and Shappee, Benjamin J. and Persson, S. E. and Piro, Anthony L. and Baron, Eddie and Contreras, Carlos and Galbany, Lluís and Kumar, Sahana and Shahbandeh, Melissa and Davis, Scott and Anais, Jorge and Busta, Luis and Campillay, Abdo and Castellón, Sergio and Corco, Carlos and Diamond, Tiara and Gall, Christa and Gonzalez, Consuelo and Holmbo, Simon and Roth, Miguel and Serón, Jacqueline and Taddia, Francesco and Torres, Simón and Baltay, Charles and Folatelli, Gastón and Hadjiyska, Ellie and Kasliwal, Mansi and Nugent, Peter E. and Rabinowitz, David and Ryder, Stuart D. and Schmidt, Brian P.}, biburl = {https://www.bibsonomy.org/bibtex/2c0e564fd3d48c2eeefdebb92333fbebf/citekhatri}, description = {Carnegie Supernova Project-I and -II: Measurements of $H_0$ using Cepheid, TRGB, and SBF Distance Calibration to Type Ia Supernovae}, interhash = {e0ffc3ed9f6d5e4ada7ccd2e227c23d3}, intrahash = {c0e564fd3d48c2eeefdebb92333fbebf}, keywords = {tifr}, note = {cite arxiv:2308.01875Comment: Submitted to ApJ}, timestamp = {2023-08-04T05:42:16.000+0200}, title = {Carnegie Supernova Project-I and -II: Measurements of $H_0$ using Cepheid, TRGB, and SBF Distance Calibration to Type Ia Supernovae}, url = {http://arxiv.org/abs/2308.01875}, year = 2023 }