VizieR Online Data Catalog: Maps of dust distribution in M31 bulge (Dong+, 2016)

Dong, H.; Li, Z. Y.; Wang, Q. D.; Lauer, T. R.; Olsen, K. A. G.; Saha, A.; Dalcanton, J. J.; Groves, B. A.

April, 2016
ABSTRACT: 

275w.fit, f336w.fit, f390m.fit, f547m.fit and f665n.fit are the mosaics of HST WFC3/UVIS images at F275W (2704Å), F336W (3355Å), F390M (3897Å), F547M (5447Å), F665N (6656Å).f435w.fit, f475w.fit and f814w.fit are the mosaics of HST ACS/WFC images at F435W (4319Å), F475W (4747Å) and F814W (8057Å).
f110w.fit and f160w.fit are the mosaics of HST WFC3/IR images at F110W (1.15 micron) and F160W (1.54 micron).
Foreground Galactic extinction (E(B-V)=0.062, i.e. AV=0.17, Schlafly & Finkbeiner 2011) has been corrected from the ten HST images above. We have also downgraded the spatial resolution of these images to that of the F160W, the poorest one. The pixel size of these images are 0.13". Their units are ergs/s/cm2/Å.
These images have also been adaptively smoothed to make sure that each resolution element has at least 105solar mass.
extin.fit the extinction map (A_F547M) in units of magnitude.
frac.fit the map of the fraction of obscured starlight by the dusty clumps. The values are from 0 to 1.0 means that the dusty clumps re far behind the M31 bulge and 1 means that the clumps are in front of the M31 bulge pixind.fit the index image for the pixels suffers with significant extinction in the UV band (such as, F336W, F390M and F435W) (values = 1). For these pixels, the fractions of obscured starlight in frac.fit are very reliable.
(2 data files).