VISIT 51 has been added to replace the failed VISIT 01. For each galaxy, it is preferred that the mosaiced visits share the same orientation angle when possible. If scheduling the observations with the current orientation angle restrictions proves too difficult, the field pointings can be changed to allow for a wider range of orientation angles at the cost of spatial coverage. Small pointing shifts towards the center of each galaxy could also be used in consultation with PI to help acquire guide stars. Small decreases to the exposure times could also be used to increase schedulability. ----- Submission 1 (Tue May 03 21:36:17 GMT 2005) ----- ----- Submission 2 (Tue May 17 17:43:51 GMT 2005) ----- Phase II Proposal 10582 (10582_N4365_N4697_resubmit) successfully submitted. ----- Submission 3 (Mon May 15 21:15:58 GMT 2006) ----- VISITS 01-12 have been completed already. I was told by Patricia Royle that only VISIT 51, which replaces the failed VISIT 01, needs to have been run under runAPT. Assigned ID: 80 ----- Submission 1 (Thu Jan 20 18:03:52 GMT 2005) ----- Probing The Galaxy-wide Globular Cluster - Low Mass X-ray Binary Connection in Early-type Galaxies The combination of high-resolution imaging from Hubble (HST) and Chandra (CXO) has completely revolutionized our understanding of extragalactic low-mass X-ray binaries (LMXBs) and globular clusters (GCs); however, studies have been limited by short X-ray exposures and relatively small fields. NGC 4697 amd NGC 4365 are relatively simple elliptical galaxies in the X-ray that will have deep CXO observations. We propose ACS observations in six flanking fields per galaxy to provide a study of the GC-LMXB connection in normal early-type galaxies with unprecedented depth, spatial resolution and areal coverage. Combined with existing central field observations, we will detect ~900 and ~2700 GCs GCs in most of NGC 4697 and all of NGC 4365. These two galaxies will have the greatest number of detected GC-LMXBs to date (~70 & 120). We will measure the fraction of LMXBs found in GCs, and the fraction of GCs which contain LMXBs, as a function of X-ray luminosity, galactocentric distance, color, GC half-light radius, and local GC specific frequency. We will test existing models of GC formation/evolution and LMXB formation/evolution. Using the radial profile of optical light, GCs, and LMXBS, we will determine the percentage of field LMXBs which may have originated in GCs.
Our science goal is to obtain a nearly complete census of globular clusters in NGC 4697 and NGC 4365, and make comparisons to the low-mass X-ray binary population using the ACS/WFC. For each galaxy, we will combine six new flanking fields with an existing central field to cover the isophotal 25 mag arcsec^-2 surface. We will observed the fields in the F475W (730s total exposure with a 2-point hot pixel dither pattern) and F850LP (1260s total exposure with a 3-point sub-pixel dither pattern). Our chosen dither patterns optimize the rejection of hot pixels and cosmic rays while maximizing total exposure time. Each flanking field is performed in one orbit. Orientation angle restrictions have been applied to maximize field coverage under 2-gyro pointing, while retaining sufficient overlap for astrometric registration of the fields. Combined with the exposure requirements, each galaxy is schedulable for ~20 days. For each galaxy, it is preferred that the mosaiced visits share the same orientation angle when possible. If scheduling the observations with the current orientation angle restrictions proves too difficult, the field pointings can be changed to allow for a wider range of orientation angles at the cost of spatial coverage. Small decreases to the exposure times could also be used to increase schedulability. GALAXIES 12 false 0.0 false false false false false SUPPORTED GALAXY ELLIPTICAL V=23.0, magnitude is that of a typical globular cluster in NGC 4697 J2000 12 48 27.1000 -05 45 35.67 J2000 GALAXY ELLIPTICAL V=23.0, magnitude is that of a typical globular cluster in NGC 4697 J2000 12 48 21.7000 -05 48 23.71 J2000 GALAXY ELLIPTICAL V=23.0, magnitude is that of a typical globular cluster in NGC 4697 J2000 12 48 31.3000 -05 50 56.74 J2000 GALAXY ELLIPTICAL V=23.0, magnitude is that of a typical globular cluster in NGC 4697 J2000 12 48 45.9000 -05 50 36.15 J2000 GALAXY ELLIPTICAL V=23.0, magnitude is that of a typical globular cluster in NGC 4697 J2000 12 48 50.9000 -05 47 47.70 J2000 GALAXY ELLIPTICAL V=23.0, magnitude is that of a typical globular cluster in NGC 4697 J2000 12 48 41.8000 -05 45 17.52 J2000 GALAXY ELLIPTICAL V=24.2, magnitude is that of a typical globular cluster in NGC 4697 J2000 12 24 17.6000 +07 21 10.20 J2000 GALAXY ELLIPTICAL V=24.2, magnitude is that of a typical globular cluster in NGC 4697 J2000 12 24 15.5000 +07 17 28.75 J2000 GALAXY ELLIPTICAL V=24.2, magnitude is that of a typical globular cluster in NGC 4697 J2000 12 24 25.7000 +07 15 35.14 J2000 GALAXY ELLIPTICAL V=24.2, magnitude is that of a typical globular cluster in NGC 4697 J2000 12 24 37.6000 +07 17 8.11 J2000 GALAXY ELLIPTICAL V=24.2, magnitude is that of a typical globular cluster in NGC 4697 J2000 12 24 42.1000 +07 20 17.03 J2000 GALAXY ELLIPTICAL V=24.2, magnitude is that of a typical globular cluster in NGC 4697 J2000 12 24 32.1000 +07 22 15.12 J2000 ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W 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