0Assigned ID: 987
----- Attempting Submission 1 (Fri Apr 07 22:17:40 GMT 2017) -----This version has been updated to use postargs instead of patterns for all dither steps;
every exposure is at a different position, based on a six-point dither pattern, plus
half and quarter pixel offets between visits.
This latest submission has substituted one orbit of F438W for one of the F336W orbits, and spread the three F438W exposures
over three of the visits. The F814W exposures have also been reordered to accompany the F438W exposures. The two outermost
dither points have been moved to make a more compact array of pointings.-721631702----- Attempting Submission 1 (Thu Jul 20 09:29:20 GMT 2017) -----
HST Phase II Proposal 15169 (g1phot_submit1.apt) successfully submitted.
Receipt: # 15169-1
----- Attempting Submission 2 (Fri Jul 21 12:41:35 GMT 2017) -----
----- Attempting Submission 3 (Wed Oct 11 03:20:04 GMT 2017) -----
----- Attempting Submission 4 (Tue Oct 30 05:34:15 GMT 2018) -----Resolving Multiple Stellar Populations in G1The most luminous and massive compact stellar system in the Local Group is G1, a satellite of M31. It has been speculated that G1 is the remnant nucleus of a tidally stripped dwarf elliptical galaxy. As such, G1 is key to understanding both the evolution of dwarf galaxies and the hierarchical assembly of bright spirals. Recently, new U-B-V-I broad band imaging techniques have revealed multiple stellar populations in Milky Way globular clusters. We propose to obtain new deep WFC3/UVIS F336W and F814W images, to be combined with archival WFC3 data, to probe the star formation and enrichment history of G1. This study will yield new and definitive insights into the origin and evolution of G1, the relationship of globular clusters to dwarf galaxies, and the formation of luminous spirals like M31 and the Milky Way.We will observe G1 with F336W for 10 orbits. Estimating
2400s open shutter time per orbit, this will result in a 24ks
exposure. To take advantage of drizzling resolution gains, we will
obtain three dithered exposures each orbit, and dither between orbits.
The WFC3 ETC estimates that for a GIII spectral type at
U=27.0, we will achieve S/N=15 (optimally extracted), including
Galactic reddening and average sky brightness. At the distance of G1,
m-M=24.4, this reaches the base of the red HB in
G1, and well below, still with S/N of 8-10.
To reach a similar depth as the other WFC3 broad band data for G1, we
will use two orbits for F814W. These will be divided into six
exposures, dithered for optimum resolution recovery and CR rejection.
With this exposure time, F814W data will reach S/N of 20 for a GIII
spectral type 1.5 magnitudes below the level of the HB (I=25.5), and
comparable S/N even for blue HB stars with colors of ~ 0. This
is a good match to the depth of the existing WFC3 data in F438W and
F606W, and will allow a robust implementation of the CUBI technique.
During the 12 orbits of WFC3 observations, parallel ACS exposures of a
nearby field will be obtained to characterize the stellar population in the
surrounding halo of M31. We will divide the time evenly between the F606W
and F814W filters. For these exposure times, the
ACS ETC calculates S/N of 5 for a K0III star with V= 29.75.Stellar Populations6falsefalsefalsefalsefalsefalsefalseSUPPORTEDEXT-CLUSTERGLOBULAR CLUSTERYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF475WACS/WFCImagingNoNoF814WThe scheduling data was generated by CASM 26.0.CASM was run in Phase II mode.154247677600098.0(Tic-Visit
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