Type Ia supernovae (SNe Ia) are more precise standardizable candles when measured in the near-infrared (NIR) than in the optical. With this motivation, from 2012 to 2017 we embarked on the RAISIN program with the Hubble Space Telescope (HST) to obtain rest-frame NIR light curves for a cosmologically distant sample of 37 SNe Ia (0.2 ≲
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Abstract z ≲ 0.6) discovered by Pan-STARRS and the Dark Energy Survey. By comparing higher-z HST data with 42 SNe Ia atz < 0.1 observed in the NIR by the Carnegie Supernova Project, we construct a Hubble diagram from NIR observations (with only time of maximum light and some selection cuts from optical photometry) to pursue a unique avenue to constrain the dark energy equation-of-state parameter,w . We analyze the dependence of the full set of Hubble residuals on the SN Ia host galaxy mass and find Hubble residual steps of size ∼0.06-0.1 mag with 1.5σ −2.5σ significance depending on the method and step location used. Combining our NIR sample with cosmic microwave background constraints, we find 1 +w = −0.17 ± 0.12 (statistical + systematic errors). The largest systematic errors are the redshift-dependent SN selection biases and the properties of the NIR mass step. We also use these data to measureH 0= 75.9 ± 2.2 km s−1Mpc−1from stars with geometric distance calibration in the hosts of eight SNe Ia observed in the NIR versusH 0= 71.2 ± 3.8 km s−1Mpc−1using an inverse distance ladder approach tied to Planck. Using optical data, we find 1 +w = −0.10 ± 0.09, and with optical and NIR data combined, we find 1 +w = −0.06 ± 0.07; these shifts of up to ∼0.11 inw could point to inconsistency in the optical versus NIR SN models. There will be many opportunities to improve this NIR measurement and better understand systematic uncertainties through larger low-z samples, new light-curve models, calibration improvements, and eventually by building high-z samples from the Roman Space Telescope. -
Jones, D. O. ; Scolnic, D. M. ; Foley, R. J. ; Rest, A. ; Kessler, R. ; Challis, P. M. ; Chambers, K. C. ; Coulter, D. A. ; Dettman, K. G. ; Foley, M. M. ; et al ( , The Astrophysical Journal)