This is a revision of the GO-10631 phaseII program. Exposure times were adjusted for primary and parallel observations to allow more flexible scheduling of visits. For most visits, this opened two windows in mid November and mid February. If this is possible, we would be very interested to see if the visible targets could be observed during these earlier windows. M31GC-B337-336 is the most important target in our program, and it would be very helpful to put visits 1 & 5 in the November window. That would give our group the most important data, which justifies a study by itself. ----- Submission 1 (Thu May 12 22:12:06 GMT 2005) ----- ----- Submission 2 (Fri Sep 16 15:56:32 GMT 2005) ----- Assigned ID: 457 ----- Submission 1 (Fri Jan 21 22:21:29 GMT 2005) ----- Phase I Proposal 457 (HBm31gc) successfully submitted. ----- Submission 4 (Fri Jan 21 22:49:18 GMT 2005) ----- Phase I Proposal 457 (HBm31gc) successfully submitted. ----- Submission 5 (Fri Jan 21 23:25:11 GMT 2005) ----- Phase I Proposal 457 (HBm31gc) successfully submitted. ----- Submission 6 (Sat Jan 22 00:15:14 GMT 2005) ----- Intermediate-Age Globular Clusters in M31 We propose deep ACS/WFC imaging of four halo M31 globular clusters in order to derive their horizontal branch morphologies. Our spectroscopic investigation of their integrated light identifies them as members of an intermediate-age population of globular clusters in M31. Since our spectroscopic results are based on the analysis of Balmer absorption lines, we need to secure our results against an artificial juvenation due to extreme horizontal branch morphologies. The proposed observations will allow a clear-cut answer to the question of whether spectroscopically derived intermediate-age estimates are due to genuinely younger ages or are the result of anomalously hot horizontal branch morphologies. Either way, our results will have important implications for spectroscopically derived ages and metallicities of distant stellar populations. Because of the high spatial resolution of the proposed ACS/WFC observations we will also derive accurate surface brightness profiles of our target globular clusters and investigate the influence of stellar density on horizontal branch morphology. Moreover, together with deep parallel WFPC2 fields we will study the metallicity dispersion of the background stellar population in M31 as a function of galactocentric radius.
We will observe resolved globular clusters in M31 in the two filters F435W and F606W, using the wide-field channel of ACS. To optimize the scientific output of the images two pointings (B337-336 and B058-049) contain more than one globular cluster. Another pointing contains one confirmed (B350) and one candidate globular cluster. The fourth pointing includes only one globular cluster (B292). For the fields with multiple objects we set orientation requirements to guarantee the best coverage of all targets. The B292 pointing additional orient constraints were added to avoid a bright star in the field of view. All roll angle requirements have little impact on the schedulability of the observations. Coordinated parallel observations in the filters F450W and F606W will be carried out with WFPC2 in order to sample the field stellar population of M31. In order to be as complete as possible for the much cooler WFPC2 targets, we choose to observe with WFPC2 in F450W when ACS is observing in the F606W filter, and in F606W when ACS will be taking integrations through the F435W filter. STELLAR POPULATIONS 12 false 0.0 false false false false false SUPPORTED EXT-CLUSTER GLOBULAR CLUSTER Coordinates were taken from Galleti et al. (2004, A&A 416, 917) B = 18.52 J2000 00 00 0.0000 +00 00 0.00 J2000 EXT-CLUSTER GLOBULAR CLUSTER Coordinates were taken from Galleti et al. (2004, A&A 416, 917) B = 15.81 J2000 00 41 53.0100 +40 47 8.63 J2000 EXT-CLUSTER GLOBULAR CLUSTER Coordinates were taken from Galleti et al. (2004, A&A 416, 917) B = 17.89 J2000 00 36 16.5900 +40 58 26.54 J2000 EXT-CLUSTER GLOBULAR CLUSTER Coordinates were taken from Galleti et al. (2004, A&A 416, 917) B = 17.36 J2000 00 42 28.3300 +40 24 50.18 J2000 ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F606W WFPC2 Imaging No F450W WFPC2 Imaging No F606W WFPC2 Imaging No F450W WFPC2 Imaging No F606W WFPC2 Imaging No F450W WFPC2 Imaging No F606W WFPC2 Imaging No F450W WFPC2 Imaging No F606W POS-TARG DITHER 0.171 LINE 0.171 false false 145.82 4 30.16 ACS-WFC-DITHER-BOX 1 false POS-TARG DITHER 0.17 LINE false false 3 47.23 ACS-WFC-DITHER-LINE 2 false /private/tmp/OPVisit41593.xml This visit includes a pair of clusters (B337 and B336) that can be simultaneously observed, placing the ACS field so that each clusters lies in one corner of the field of view. Consequently, four different roll angle windows, which are specified in the orientation requirements, are optimal to perform this observation. The first roll angle window (30-65 deg) should have lower priority, as a bright star is contaminating the coordinated parallel WFPC2 observations. Higher priority should therefore be given to the last three orient windows with roll angles >125 deg. The optimal orient angles are 47 and 227 degrees. We provide here the J2000 coordinates for the two globular clusters B337: 00 40 48.45, +42 12 11.45 and B336: 00 40 47.57, +42 08 41.38. 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The primary target is B058. To maximize schedulability the roll angles were optimized to include the clusters B058 and B049 only. The ideal roll angles of 97 and 277 deg include all three clusters within one ACS pointing. The J2000 coordinates of all three clusters are: B058: 00 41 53.01, +40 47 08.63; B049: 00 41 45.60, +40 49 53.73; B206D: 00 41 40.596, +40 50 06.90. 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Consequently, four different roll angle windows, which are specified in the orientation requirements, are optimal to perform this observation. The first roll angle window (30-65 deg) should have lower priority, as a bright star is contaminating the coordinated parallel WFPC2 observations. Higher priority should therefore be given to the last three orient windows with roll angles >125 deg. The optimal orient angles are 47 and 227 degrees. We provide here the J2000 coordinates for the two globular clusters B337: 00 40 48.45, +42 12 11.45 and B336: 00 40 47.57, +42 08 41.38. 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