Near-infrared Supernova Ia Distances: Host Galaxy Extinction and Mass-step Corrections Revisited

Creators: Johansson, J.; Cenko, S. B.; Fox, O. D.; Dhawan, S.; Goobar, A.; Stanishev, V.; Butler, N.; Lee, W. H.; Watson, A. M.; Fremling, U. C.; Kasliwal, M. M.; Nugent, P. E.; Petrushevska, T.; Sollerman, J.; Yan, L.; Burke, J.; Hosseinzadeh, G.; Howell, D. A.; McCully, C.; Valenti, S.

Abstract

We present optical and near-infrared (NIR, Y-, J-, H-band) observations of 42 Type Ia supernovae (SNe Ia) discovered by the untargeted intermediate Palomar Transient Factory survey. This new data set covers a broad range of redshifts and host galaxy stellar masses, compared to previous SN Ia efforts in the NIR. We construct a sample, using also literature data at optical and NIR wavelengths, to examine claimed correlations between the host stellar masses and the Hubble diagram residuals. The SN magnitudes are corrected for host galaxy extinction using either a global total-to-selective extinction ratio, R_V = 2.0, for all SNe, or a best-fit R_V for each SN individually. Unlike previous studies that were based on a narrower range in host stellar mass, we do not find evidence for a "mass step," between the color- and stretch-corrected peak J and H magnitudes for galaxies below and above log(M∗/M⊙) = 10. However, the mass step remains significant (3σ) at optical wavelengths (g, r, i) when using a global R_V, but vanishes when each SN is corrected using their individual best-fit R_V. Our study confirms the benefits of the NIR SN Ia distance estimates, as these are largely exempted from the empirical corrections dominating the systematic uncertainties in the optical.

Additional Information

© 2021. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 May 24; revised 2021 October 11; accepted 2021 October 12; published 2021 December 24. We are grateful for valuable comments from Jakob Nordin and feedback from the CSP team (Chris Burns, Eric Hsiao, Mark Phillips, and Shuvo Uddin). We thank Melissa L. Graham for helping to obtain follow-up observations with Las Cumbres Observatory in 2013. A.G. acknowledges support from the Swedish Research Council under Dnr VR 2016-03274 and 2020-03444. T.P. acknowledges the financial support from the Slovenian Research Agency (grants I0-0033, P1-0031, J1-8136 and Z1-1853). Research by S.V. is supported by NSF grants AST-1813176 and AST-2008108. This work makes use of observations from the Las Cumbres Observatory network. The LCO team was supported by NSF grants AST-1313484 and AST-1911225. The intermediate Palomar Transient Factory project is a scientific collaboration among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin, Milwaukee, the Oskar Klein Center, the Weizmann Institute of Science, the TANGO Program of the University System of Taiwan, and the Kavli Institute for the Physics and Mathematics of the Universe. LANL participation in iPTF is supported by the US Department of Energy as a part of the Laboratory Directed Research and Development program. Software: FPipe (Fremling et al. 2016), QUBA pipeline (Valenti et al. 2011), lcogtsnpipe (Valenti et al. 2016), IRAF (Tody 1993), astrometry.net (Lang et al. 2010), swarp (Bertin 2010), (Becker 2015), SNooPy (Burns et al. 2011).

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