Example data sets:
High resolution ACS BVHalpha image of M51 from archival HST coverage, overlayed with
HI radio contours from the Westerbork Synthesis Radio Telescope (courtesy of Robert Braun), contours are
spaced by sqrt(2) from 5.4 x 10^20 cm^-2 up to 1.8 x 10^21 cm^-2. Similar maps would be constructed
for additional 8 galaxies. The correlation between massive stars and the ISM can be probed
at single-star resolution. Click here for a higher-resolution version.
Identifying the progenitor of SN 2005cs in M51 using archival ACS BVI data:
co-I Maund and collaborators
co-Is Li, Van Dyk, Filippenko, Bloom, et al.
Complete ACS BVI coverage of M51 (Archival data)
Star cluster catalog in M51:
This is the masterlist of clusters used in Bastian et al. 2005 based on multi-band HST-WFPC2 imaging. The first digit of the id number
(i.e. 1 in 10015) is the chip on which the source was found (1 = PC,
2=WF2, 3=WF3, 4=WF4), reg is which 'region' (of the two WFPC2 pointings)
the source was found on. The x and y are the corrdianates on the chip. d
is the projected distance of the source from the galactic center. The
E(B-V), log age, and log mass are the best fitting values (and their
minimum and maximum) from comparison of the photometry to cluster (SSP)
models. M_V is the absolute magnitude, corrected for extinction and
distance to M51. The magnitudes of the source in different bands and
their respective errors is given. Finally the x and y positions of the
source is given in the reference frame of each chip (untruncated) and in
the componed WFPC2 mosaic.
Constructed: January 2007, by:
Avishay Gal-Yam ,
E-Mail: avishay@astro.caltech.edu