0
Assigned ID: 658
----- Attempting Submission 1 (Fri Apr 11 18:25:06 GMT 2014) -----
HST Phase I Proposal 658 (emission-v4.apt) successfully submitted.
----- Attempting Submission 2 (Fri Apr 11 19:10:30 GMT 2014) -----
HST Phase I Proposal 658 (emission-v7.apt) successfully submitted.
----- Attempting Submission 3 (Fri Apr 11 19:26:09 GMT 2014) -----
HST Phase I Proposal 658 (emission-v8.apt) successfully submitted.
----- Attempting Submission 4 (Fri Apr 11 20:33:04 GMT 2014) -----
HST Phase I Proposal 658 (emission-v9-submitted.apt) successfully submitted.
----- Attempting Submission 5 (Fri Apr 11 21:10:33 GMT 2014) -----
HST Phase I Proposal 658 (emission-v10-submit.apt) successfully submitted.
----- Attempting Submission 6 (Fri Apr 11 22:07:49 GMT 2014) -----
HST Phase I Proposal 658 (emission-v11-submit.apt) successfully submitted.
----- Attempting Submission 7 (Fri Apr 11 22:15:08 GMT 2014) -----
HST Phase I Proposal 658 (emission-v12-submit.apt) successfully submitted.
----- Attempting Submission 8 (Fri Apr 11 22:41:24 GMT 2014) -----
HST Phase I Proposal 658 (emission-v14-submit.apt) successfully submitted.
----- Attempting Submission 9 (Fri Apr 11 23:28:46 GMT 2014) -----
HST Phase I Proposal 658 (emission-v15-submit.apt) successfully submitted.
----- Attempting Submission 10 (Fri Apr 11 23:54:16 GMT 2014) -----
HST Phase I Proposal 658 (emission-v16-submit.apt) successfully submitted.
----- Attempting Submission 11 (Fri Apr 11 23:59:53 GMT 2014) -----
HST Phase I Proposal 658 (emission-v16-submit.apt) successfully submitted.
The number of orbits used exceeds the number allocated
copy of visit 01 -> 07. lost to safing
-436508393
----- Attempting Submission 1 (Thu Jul 24 14:30:40 GMT 2014) -----
----- Attempting Submission 2 (Mon Aug 04 20:02:04 GMT 2014) -----
----- Attempting Submission 3 (Wed Sep 10 00:08:45 GMT 2014) -----
----- Attempting Submission 4 (Tue Oct 21 14:07:14 GMT 2014) -----
Emission Line Stars in Andromeda
Elucidating the physics that drives production of emission lines in a wide variety of stellar sources is hampered by the relatively small, heterogeneous available samples. We propose to construct a large, deep, homogeneous sample of more than 10,000 emission line stars in M31, by adding H-alpha imaging to existing data from the Panchromatic Hubble Andromeda Treasury (PHAT), in regions targeted to contain large numbers of massive young stellar clusters. This program will deliver the statistics needed to determine the prevalence of Be disk systems as a function of age and the rate of dramatic disk-loss/disk-renewal episodes. The survey will also provide a key opportunity to identify Symbiotic stars from a well characterized dataset, and diagnose why the current rate of observed symbiotic stars is several orders of magnitude less than that predicted by theory. Our program will also serve as a critical, deep legacy product for the broader community interested in other emission line stars such as Wolf-Rayet stars, PNe, and luminous M(e) stars.
Our observing strategy is to obtain deep H-alpha imaging, and matched F625W imaging. There are 6 targets, and 6 visits. Each target is vidted once with UVIS as the primary and ACS as the parallel. The orients are fixed so that the 2 targets are observed with each visit, resulting in double the depth. We dither each visit to obtain Nyquist pixel sampling in H-alpha for the ACS imaging, and improved pixel sampling for the UVIS imaging as well.
RESOLVED STELLAR POPULATIONS
Default
false
false
false
false
false
SUPPORTED
GALAXY
SPIRAL
J2000
J2000
GALAXY
SPIRAL
J2000
J2000
GALAXY
SPIRAL
J2000
J2000
GALAXY
SPIRAL
J2000
J2000
GALAXY
SPIRAL
J2000
J2000
GALAXY
SPIRAL
J2000
J2000
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F625W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F625W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F625W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F625W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F625W
ACS/WFC
Imaging
No
No
F658N
ACS/WFC
Imaging
No
No
F625W
WFC3/UVIS
Imaging
No
No
F657N
WFC3/UVIS
Imaging
No
No
F625W
WFC3/UVIS
Imaging
No
No
F657N
WFC3/UVIS
Imaging
No
No
F625W
WFC3/UVIS
Imaging
No
No
F657N
WFC3/UVIS
Imaging
No
No
F625W
WFC3/UVIS
Imaging
No
No
F657N
WFC3/UVIS
Imaging
No
No
F625W
WFC3/UVIS
Imaging
No
No
F657N
WFC3/UVIS
Imaging
No
No
F625W
WFC3/UVIS
Imaging
No
No
F657N
WFC3/UVIS
Imaging
No
No
F625W
Timing link suitability includes constraints ([02 After 01 by 180.0 to 365.0 days])
The scheduling data was generated by CASM 22.2.
CASM was run in Phase II mode.
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