The only trouble we had was in understanding that the "angle" value for plotting apertures in the Aladin
previewer is not the same as the U3 orientation we specify in the proposal; it would be nice if they were
the same. Once we determined the difference, we were able to complete the phase II proposal with no
problems.
----- Attempting Submission 1 (Wed May 09 16:47:27 GMT 2007) -----
Re-worked version of proposal 443 to use WFPC2 instead of ACS/WFC.
Assigned ID: 1124
----- Attempting Submission 1 (Wed Feb 07 14:47:09 CST 2007) -----
White dwarfs in the open star cluster NGC 188
White dwarf cooling sequences represent the only ways in which we can determine ages of Galactic components such as the disk and the halo, and they are an independent check on main sequence ages of globular star clusters. These age measurements rely heavily on theoretical cooling models, many of which disagree by as much as a few gigayears for the coolest white dwarfs. Further, observations of the white dwarf sequence in the super metal-rich open cluster NGC 6791 have found a white dwarf age several gigayears younger than the accepted cluster age determined by main-sequence fitting. The white dwarf sequence of the solar-metallicity, 7-Gyr old open cluster NGC 188 can provide some much-needed insight into these uncertainties, but previous HST observations were too shallow to detect the oldest, faintest white dwarfs in the cluster. We propose deep imaging of two fields at the center of the cluster with the following goals: (1) To detect the end of the white dwarf cooling sequence, providing a much-needed empirical data point for cool white dwarf evolutionary models, (2) to compare the white dwarf luminosity function of NGC 188 with that of NGC 6791 to determine if the odd white dwarf sequence in the latter cluster is due to the cluster's high metallicity or due to a shortcoming in theoretical models, and (3) to determine via photometry the masses of white dwarfs formed by solar-mass stars, a quantity not yet empirically measured.
Our observations represent a second epoch of imaging of two fields in the open cluster NGC 188 first imaged in GO 7371. The three primary goals of the observations are: (1) In one deep field, obtain V and I photometry with S/N~14 for white dwarfs as faint as V=27.2 (0.2 mag fainter than the faintest expected white dwarfs in this 7 Gyr-old cluster); (2) In a second, shallower field, obtain accurate V and I photometry for white dwarfs as faint as V=26.5 for comparison with the anomalous white dwarf luminosity function of the open cluster NGC 6791; and (3) To obtain measurements of proper motions of white dwarfs imaged in both fields in both epochs.
In order to maximize the overlap of these observations with the first epoch imaging and in order to minimize the impact of distortions on proper motion measurements, we constrain the ORIENT of each field to within 10 degrees of the first epoch orientation; multiple visits to each field are constrained to be at the same ORIENT as the first visit.
As several exposures will be taken in each filter at each field, we have set CR-SPLIT=NO. Both BOX and LINE dither patterns were selected for the purposes of sub-sampling the WF PSF and to aid in cosmic ray and hot pixel rejection.
RESOLVED STELLAR POPULATIONS
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The V-magnitude indicate the faintest objects we wish to detect in this field.
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The V-magnitude indicate the faintest objects we wish to detect in this field.
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