After the failure of ACS/HRC beginning 2007, I changed all visits that previously made use of ACS/HRC to WFPC2,
using PC1-FIX as aperture so that the cluster core is centred in the PC.
----- Submission 2 (Wed Jul 13 15:43:49 GMT 2005) -----
Phase II Proposal 10561 (M30_phase2) successfully submitted.
----- Submission 3 (Wed Jul 13 20:43:27 GMT 2005) -----
Phase II Proposal 10561 (M30_phase2) successfully submitted.
----- Submission 4 (Fri Jul 29 14:26:30 GMT 2005) -----
Phase II Proposal 10561 (M30_phase2) successfully submitted.
----- Submission 5 (Mon Jan 09 17:18:54 GMT 2006) -----
----- Attempting Submission 6 (Wed Mar 14 17:07:35 GMT 2007) -----
----- Attempting Submission 7 (Thu Mar 15 12:57:59 GMT 2007) -----
Phase II Proposal 10561 (10561.apt.txt) successfully submitted.
----- Attempting Submission 8 (Thu Mar 15 13:15:37 GMT 2007) -----
none
A deep UV imaging survey of the Globular Cluster M 30
We propose to carry out a deep FUV and NUV survey of M30 (NGC 7099) in order to find and study the hot and/or dynamically-formed stellar populations in the globular cluster. In particular, we will (i) search for the UV counterpart to a MSP binary, (ii) find and study the full population of cataclysmic variables in this cluster, (iii) study the UV properties of the cluster's extensive blue straggler population, (iv) detect the first set of white dwarfs in this cluster. Our survey will be sensitive to variability on time-scales from minutes to weeks, allowing us to search for variable stars in all of the FUV populations.
Our FUV imaging study of M30 requires 15 HST orbits, spread over 6 visits. Visits 1, 3, and 5 each consist of 3 consecutive HST orbits spend on FUV imaging with the ACS/SBC/F150LP detector/filter combination. Visits 2, 4, and 6 each consist of 2 orbits spend on NUV imaging with the ACS/HRC/F250W combination. We will keep each exposure in a series of identical exposures (i.e. for one detector/filter combination) as short as 5 min, so that there will be zero overheads between the exposures in each series. Visit 2 (NUV imaging) should occur 0-1 orbits after visit 1 (FUV imaging). Visit 3 (FUV) should follow about a week later, followed after 0-1 orbits by visit 4 (NUV). Visit 5 (FUV) should occur again about a week later, followed after 0-1 orbits by visit 6 (NUV). In this way, the visits will be spaced at intervals of a week, so that we will be sensitive to variability on time-scales from minutes to weeks.
12
false
0.0
false
false
false
false
false
false
SUPPORTED
STELLAR CLUSTER
GLOBULAR CLUSTER
MESSIER-030
J2000
00 00 0.0000
+00 00 0.00
J2000
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