Version 1596863689Assigned ID: 871
----- Attempting Submission 1 (Fri Apr 11 21:30:32 GMT 2014) -----Fixed all of the known issues and pending changes with the original.
There were some orient changes and many little tweaks to exposure times and positions.
This is an updated version to fill the orbits which use single guide stars, and also substituting
F350LP for F475X for all five targets.539078143----- Attempting Submission 1 (Thu Jul 24 17:46:38 GMT 2014) -----
----- Attempting Submission 2 (Thu Jul 31 21:51:40 GMT 2014) -----
----- Attempting Submission 3 (Thu Dec 18 06:25:29 GMT 2014) -----Morphological Transformation in the Coma ClusterThis proposal seeks to document the various stages of ram pressure stripping of bright
spiral galaxies evolving in the rich Coma cluster environment. Based on two ram pressure
stripping examples we have already found in Coma, we have selected an additional five
targets which manifest signs of ICM-ISM interactions. These seven objects are distributed
in a ring around the inner core of Coma, sampling different locations in the cluster and
each can be expected to show a different phase of evolution of the stripping process. We
propose WFC3 UVIS imaging to reveal the details of the interactions. From these
observations, we will be able to piece together a coherent picture of the processes which
drive morphological transformation and evolution of disk galaxies in rich environments.
The ionization and global star formation patterns, both spatial and temporal, will reveal
and characterize the ISM-ICM interactions driving the evolution of galaxies in clusters
and altering their morphologies.Primary WFC3 Imaging:
We will observe the five targets for two orbits each, dividing the time evenly between the extra-wide WFC3 filters F475X and F600LP. Each orbit will be subdivided into four dither positions to reject CRs and optimally sample the PSF. We will weight the exposure time to favor F600LP because F475X is more sensitive: 3 x 500 seconds exposures in F475X and 5 x 700 seconds in F600LP.
With 1500s total exposure in F475X, we will reach S/N of 14 for B=27, and with 3500s in F600LP, S/N of 12 for R=27, assuming typical colors of young star clusters. These correspond to M_v = -8 at the distance of Coma (100 Mpc, m-M=35.0). This is well down the cluster luminosity function,
assuming they will be comparable to cluster populations studied elsewhere, such as in the Antennae (Whitmore et al.\ 2010) where > 1000 clusters have been found down to these levels. Every individual exposure will be dithered to facilitate reduction with astrodrizzle routines.
Parallel ACS Imaging:
During our primary WFC3 observations, we will use the parallel ACS time to take F475W and F814W images. These are the filters used by the Coma Treasury Survey, and these ACS parallel observations will sample new regions in the Coma cluster, adding to the coverage of the Treasury imaging. With two orbits per field, these observations can exactly match the exposure times of the Treasury program which also devoted two orbits to each field. These new images will be useful for detecting intergalactic globular clusters, any tidal debris, and dwarf galaxies, all of which are also associated with the transformation and destruction of galaxies during the formation of rich clusters.UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTURE0falsefalse0.00.0falsefalsefalseSUPPORTEDGALAXYSPIRALThis object was generated by the targetselector and retrieved from the NED database.J2000J2000GALAXYSPIRALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSPIRALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSPIRALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSPIRALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISImagingNoNoF475XWFC3/UVISImagingNoNoF600LPWFC3/UVISImagingNoNoF475XWFC3/UVISImagingNoNoF600LPWFC3/UVISImagingNoNoF475XWFC3/UVISImagingNoNoF600LPWFC3/UVISImagingNoNoF475XWFC3/UVISImagingNoNoF600LPWFC3/UVISImagingNoNoF475XWFC3/UVISImagingNoNoF600LPACS/WFCImagingNoNoF475WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF475WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF475WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF475WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF475WACS/WFCImagingNoNoF814WThe scheduling data was generated by CASM 22.2.CASM was run in Phase II mode./Users/michael/pro/hst/c22/ngsl2/phase2/OP-cache/ultrawidecoma-v01.xml(Tic-Visit
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