Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21360306j&link_type=abstract
American Astronomical Society, AAS Meeting #213, #603.06
Astronomy and Astrophysics
Astronomy
Scientific paper
Photometry in Sloan Digital Sky Survey (SDSS) g, r and i bands and 2MASS K-band images is presented of nearby (z<0.03) galaxy environments hosting a Type Ia (SNIa) or Ia peculiar (SNIaPec) supernova in the last 80 years. The g-r color was measured for 153 local galaxy environments of SNIa and SNIaPec using a photometric 6.3” diameter aperture (0.13-4.3kpc) centered about the supernova location. Of these regions, 40 have published B and V supernova peak apparent magnitudes. Comparing the g-r color of these host galaxy regions to the corresponding supernova (B-V)max color from the sample in Wang et al. (2006), there are redder g-r environment colors with increasing (B-V)max. This sample is cut to 27 by considering galaxies with inclinations < 66 degrees. The g-r colors are then binned into two weighted points of (B-V)max <0.3 and (B-V)max >0.3 giving a result of (g-r)<0.3=0.55 and (g-r)>0.3=0.72. When compared to the sample average color (g-r)ave=0.69, a z test shows that (g-r)<0.3 is significantly bluer, consistent with Wang et al. (2006) results. This suggests that supernovae in the sample come from similar stellar populations and dispersion in the (B-V)max values is due to reddening. However, a similar analysis with 2MASS K-band and i SDSS images using an aperture size of 10"(0.2-6.9kpc), reaches a different outcome. The relatively narrow range of i-K colors (2.2-2.7) is consistent with similar mean age stellar populations that define the SN local environment. However, unlike the previous case here, there is no correlation between the (B-V)max SNIa color and the local galaxy background i-K color. The distribution shows that its equally probable that (B-V)max is between the values of -0.1 to 0.3 as it is between 0.3 to 0.8. This result would suggest that there is an appreciable range in (B-V)max for similar mean age stellar populations.
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