Are Type Ia Supernovae in Rest-frame H Brighter in More Massive Galaxies?
Metadatos
Mostrar el registro completo del ítemEditorial
Institute of Physics
Materia
Supernova: general Cosmology: dark energy
Fecha
2021-10-02Referencia bibliográfica
Published version: Kara A. Ponder... [et al]. 2021 ApJ 923 197. [https://doi.org/10.3847/1538-4357/ac2d99]
Patrocinador
National Science Foundation (NSF) AST-1311862; PITT PACC; Berkeley Center for Cosmological Physics; United States Department of Energy (DOE) DE-AC02-05CH11231 DE-AC02-05CH1123 DE-AC02-76SF00515; European Commission 839090; National Aeronautics & Space Administration (NASA); Alfred P. Sloan Foundation; United States Department of Energy (DOE); Participating Institutions; Center for High-Performance Computing at the University of Utah; SDSS Collaboration, including the Brazilian Participation Group; Carnegie Institution for Science, Carnegie Mellon University; Chilean Participation Group; French Participation Group; Smithsonian Institution; Harvard-Smithsonian Center for Astrophysics; Instituto de Astrofisica de Canarias; Johns Hopkins University; Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo; United States Department of Energy (DOE); Leibniz Institut fur Astrophysik Potsdam (AIP); Max-Planck-Institut fur Astronomie (MPIA Heidelberg) Max-Planck-Institut fur Astrophysik (MPA Garching) Max-Planck-Institut fur Extraterrestrische Physik (MPE); National Astronomical Observatories of China; New Mexico State University; New York University; University of Notre Dame; Observatario Nacional/MCTI; Ohio State University; Pennsylvania State University; Shanghai Astronomical Observatory; United Kingdom Participation Group; Universidad Nacional Autonoma de Mexico; University of Arizona; University of Colorado Boulder; University of Oxford; University of Portsmouth; University of Utah; University of Virginia; University of Washington; University of Wisconsin; Vanderbilt University; Yale University; United States Department of Energy (DOE); National Science Foundation (NSF); Spanish Government; UK Research & Innovation (UKRI); Science & Technology Facilities Council (STFC); UK Research & Innovation (UKRI); Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Inovacao e Pesquisa (Finep); Fundacao Carlos Chagas Filho de Amparo Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio De Janeiro (FAPERJ); Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ); Spanish Government; German Research Foundation (DFG); Collaborating Institutions in the Dark Energy Survey; National Energy Research Scientific Computing Center; United States Department of Energy (DOE); National Science Foundation (NSF) NSF - Directorate for Mathematical & Physical Sciences (MPS) AST-0950945; Association of Universities for Research in Astronomy, Inc., under NASA NAS5-26555 National Aeronautics & Space Administration (NASA) NNX09AF08GResumen
We analyze 143 Type Ia supernovae (SNe Ia) observed in H band (1.6-1.8 mu m) and find that SNe Ia are intrinsically brighter in H band with increasing host galaxy stellar mass. We find that SNe Ia in galaxies more massive than 10(10)(.4)(3) M-circle dot are 0.13 +/- 0.04 mag brighter in H than SNe Ia in less massive galaxies. The same set of SNe Ia observed at optical wavelengths, after width-color-luminosity corrections, exhibit a 0.10 +/- 0.03 mag offset in the Hubble residuals. We observe an outlier population (vertical bar Delta H-max vertical bar > 0.5 mag) in the H band and show that removing the outlier population moves the mass threshold to 10(10.65) M-circle dot and reduces the step in H band to 0.08 +/- 0.04 mag, but the equivalent optical mass step is increased to 0.13 +/- 0.04 mag. We conclude that the outliers do not drive the brightness-host-mass correlation. Less massive galaxies preferentially host more higher-stretch SNe Ia, which are intrinsically brighter and bluer. It is only after correction for width-luminosity and color- luminosity relationships that SNe Ia have brighter optical Hubble residuals in more massive galaxies. Thus, finding that SNe Ia are intrinsically brighter in H in more massive galaxies is an opposite correlation to the intrinsic (prewidth-luminosity correction) optical brightness. If dust and the treatment of intrinsic color variation were the main driver of the host galaxy mass correlation, we would not expect a correlation of brighter H-band SNe Ia in more massive galaxies.