THEHUBBLE SPACE TELESCOPECLUSTER SUPERNOVA SURVEY. III. CORRELATED PROPERTIES OF TYPE Ia SUPERNOVAE AND THEIR HOSTS AT 0.9 <z< 1.46

Abstract

Using the sample of Type Ia supernovae (SNe Ia) discovered by the Hubble Space Telescope (HST) Cluster Supernova Survey and augmented with HST-observed SNe Ia in the Great Observatories Origins Deep Survey (GOODS) fields, we search for correlations between the properties of SNe and their host galaxies at high redshift. We use galaxy color and quantitative morphology to determine the red sequence in 25 clusters and develop a model to distinguish passively evolving early-type galaxies from star-forming galaxies in both clusters and the field. With this approach, we identify 6 SN Ia hosts that are early-type cluster members and 11 SN Ia hosts that are early-type field galaxies. We confirm for the first time at z > 0.9 that SNe Ia hosted by early-type galaxies brighten and fade more quickly than SNe Ia hosted by late-type galaxies. We also show that the two samples of hosts produce SNe Ia with similar color distributions. The relatively simple spectral energy distributions expected for passive galaxies enable us to measure stellar masses of early-type SN hosts. In combination with stellar mass estimates of late-type GOODS SN hosts from Thomson & Chary, we investigate the correlation of host mass with Hubble residual observed at lower redshifts. Although the sample is small and the uncertainties are large, a hint of this relation is found at z > 0.9. By simultaneously fitting the average cluster galaxy formation history and dust content to the red-sequence scatters, we show that the reddening of early-type cluster SN hosts is likely E(B − V ) 0.06. The similarity of the field and cluster early-type host samples suggests that field early-type galaxies that lie on the red sequence may also be minimally affected by dust. Hence, the early-type-hosted SNe Ia studied here occupy a more favorable environment to use as well-characterized high-redshift standard candles than other SNe Ia.

Assembly of the Red Sequence in Infrared-Selected Galaxy Clusters From the Irac Shallow Cluster Survey

“…Specifically, σ C = S MAD = MAD/0.6745, since a normally distributed quantity will have MAD = 0.6745σ . Where the samples overlap, our measurements of σ U −V are consistent with those measured by Meyers et al (2012), except for ISCS J1438.1+3414 (z = 1.413). At z 1.3, the addition of the HST WFC3/F160W data permits an improved k-correction, and so we believe the present calculation to be reliable.…”

“…The scatter measurements in the bottom panel of Figures 7 and 8 show the same general trend with redshift as the median color measurements of the top two panels: clusters in this sample at higher redshift indicate an earlier formation epoch. Therefore, the time elapsed since the last major star-forming episode appears roughly constant, yielding a luminosity-weighted average age of ≈2.3 ± 0.6 Gyr, consistent with the timescales inferred from rest-frame optical color scatters by Meyers et al (2012) using the models of van Dokkum & Franx (2001) for seven of these clusters. Note.…”

“…If we posit that galaxies follow an evolutionary path from star-forming disks, through quenching, and ultimately to red-and-dead galaxies, then it is not clear that ETGs at higher redshift will have significantly more dust obscuration than those at z 1. Meyers et al (2012) analyzed the ETGs in a set of clusters that includes seven members of the ISCS and found that these galaxies, some of which are on the red sequences in the present work, likely experience little dust reddening:…”

The abundance and colours of galaxies in high-redshift clusters in the cold dark matter cosmology

“…Some observations at high redshift appear to be consistent with high-redshift galaxies having a small dust attenuation (e.g. Meyers et al 2012). If we assume therefore that there is indeed negligible dust attenuation in high-redshift cluster galaxies, then from equation (3) we can see that too large an optical depth might indicate that the predicted sizes of such galaxies are too small, the amount of cold gas in the galaxies is too high or the metallicity of the cold gas is too high, or a combination of all three.…”

BAHAMAS: NEW ANALYSIS OF TYPE Ia SUPERNOVAE REVEALS INCONSISTENCIES WITH STANDARD COSMOLOGY

“…There is strong evidence that the absolute magnitude (after corrections) of SNe Ia correlates with host galaxy mass (e.g., Sullivan et al 2006;Meyers et al 2012). Current results indicate that more massive galaxies (…”