%AJones, D.%AMandel, K.%AKirshner, R.%AThorp, S.%AChallis, P.%AAvelino, A.%ABrout, D.%ABurns, C.%AFoley, R.%APan, Y.%AScolnic, D.%ASiebert, M.%AChornock, R.%AFreedman, W.%AFriedman, A.%AFrieman, J.%AGalbany, L.%AHsiao, E.%AKelsey, L.%AMarion, G.%ANichol, R.%ANugent, P.%APhillips, M.%ARest, A.%ARiess, A.%ASako, M.%ASmith, M.%AWiseman, P.%AWood-Vasey, W.%BJournal Name: The Astrophysical Journal; Journal Volume: 933; Journal Issue: 2; Related Information: CHORUS Timestamp: 2024-01-16 14:45:12 %D2022%IDOI PREFIX: 10.3847 %JJournal Name: The Astrophysical Journal; Journal Volume: 933; Journal Issue: 2; Related Information: CHORUS Timestamp: 2024-01-16 14:45:12 %K %MOSTI ID: 10369031 %PMedium: X; Size: Article No. 172 %TCosmological Results from the RAISIN Survey: Using Type Ia Supernovae in the Near Infrared as a Novel Path to Measure the Dark Energy Equation of State %XAbstract

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 ≲z≲ 0.6) discovered by Pan-STARRS and the Dark Energy Survey. By comparing higher-zHST 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−2.5σsignificance 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 measureH0= 75.9 ± 2.2 km s−1Mpc−1from stars with geometric distance calibration in the hosts of eight SNe Ia observed in the NIR versusH0= 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 inwcould 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-zsamples, new light-curve models, calibration improvements, and eventually by building high-zsamples from the Roman Space Telescope.

%0Journal Article