0
Assigned ID: 677
----- Attempting Submission 1 (Fri Apr 07 17:38:05 GMT 2017) -----
The number of orbits used exceeds the number allocated
duplicated visit 08 to 58. Repeat due to WFC3 suspend
-2144860975
----- Attempting Submission 1 (Wed Jul 19 08:27:01 GMT 2017) -----
----- Attempting Submission 2 (Wed Jan 09 17:05:10 GMT 2019) -----
----- Attempting Submission 3 (Mon Jan 14 16:30:29 GMT 2019) -----
All problems stem from the fact that I had to re-ran the orbit planner on visits that had already been executed.
Only visit 57, a new visit account of a HOPR, is relevant and it requests the same orient as visit 17 which
has already happened.
The Globular Cluster Systems of Local Group Dwarf Galaxies
We propose to obtain deep ACS and WFC3 imaging of 26 globular clusters (GCs) lying in three Local Group dwarf galaxies -- NGC 147, NGC 185 and NGC 6822. These three galaxies possess the richest dwarf galaxy GC systems known within the Local Group and our sample represents their entire GC populations. We will characterize, in unprecedented detail, the properties of the GCs in these low mass systems and construct a reference dataset against which to compare the properties of suspected accreted families of GCs in the M31 and Milky Way halos. Our deep imaging will allow us to derive the properties of the constituent stellar populations (e.g. metallicities, HB morphologies) of the GCs, as well as their structural parameters and line-of-sight distances, and quantify the variation within and between GC systems in galaxies of the dE and dIrr classes. In addition, our imaging will facilitate the construction of deep colour-magnitude diagrams for a wide swathe of the field populations in these dwarf galaxies, from which we will extract detailed star formation histories. This will enable us to analyse spatial variations in their stellar mass assembly histories (complementing previous deep single field studies of these systems) and quantitatively compare the history of star formation as traced by field stars and GCs.
The aim of this program is to conduct resolved imaging of 26 globular clusters in three Local Group dwarf galaxies -- NGC 147, NGC 185, and NGC 6822. Using these observations we will construct a colour-magnitude diagram for each target cluster, facilitating measurement of their constituent stellar populations, structures, and line-of-sight distances. Parallel imaging will allow us to (i) increase the efficiency of the program, and (ii) obtain data on the field populations in these galaxies, through which we will study their star formation histories at various locations.
We will utilise both ACS/WFC and WFC3/UVIS. For both imagers we will observe using the F606W and F814W filters. These offer maximum throughput and match the vast majority of extant HST imaging of M31 and Galactic globular clusters.
WFC3/UVIS will be used as the primary imager in cases where the crowding is greatest, due to its slightly better pixel scale. To achieve the required depth (~2 mag below the horizontal branch), visits with WFC3/UVIS as the primary imager will cover 3 orbits (one with F606W and two with F814W). Visits with ACS/WFC as the primary imager can achieve the necessary depth in 2 orbits (one each with F606W and F814W).
Some visits have a constrained roll angle so that target clusters can be observed in both the primary and parallel fields. These are:
- Visits 01 and 02, which each have 2 clusters in the primary field and 1 in the parallel field;
- Visits 03 and 08, which each have 1 cluster in the primary field and 1 in the parallel field;
- Visit 07, which has 2 clusters in the primary field and 3 in the parallel field;
Each of these visits uses WFC3/UVIS as the primary imager and ACS/WFC as the parallel imager. All appear to be schedulable at various intervals through the Cycle; the most limited is Visit 07 which will allow us to simultaneously observe 5 of our target objects.
The remaining visits target a single cluster in the primary field and reserve the parallel observation for sampling the field star populations of the host galaxy. These visits use ACS/WFC as the primary imager and mostly have unconstrained roll angle. In a few cases (V5, V10, V11, V13) we have imposed a weak restriction on the allowed orientation to try and avoid bright foreground stars in either the primary or parallel fields. This does not adversely affect the schedulability of these visits.
We will conduct three exposures on any given orbit. The individual exposure times range between ~750-950 seconds, depending on the visibility of the target. We have used the "auto-adjust" feature in APT to maximise the exposure time per orbit. We have used the ETC to check that the resulting exposure times are appropriate (i.e., stars in the target clusters do not saturate in any given frame, and the total exposure time per filter allows us to reach ~2 magnitudes below the horizontal branch at S/N ~ 10 for any given target).
For visits using WFC3/UVIS as the primary imager, we will utilise the WFC3-UVIS-MOSAIC-LINE dither pattern with 3 points, which will allow us to fill in the inter-chip gap for both the primary field and the parallel field being observed with ACS/WFC. For visits using ACS/WFC as the primary imager, we will use the ACS-WFC-DITHER-LINE pattern with 3 points, which will allow us to fill in the inter-chip gap for the primary field. In all cases where ACS/WFC is the primary imager, the parallel field will sample only the field star populations of the host galaxy, so the presence of the chip gap in the parallel field is not problematic.
Stellar Populations
6
false
false
false
false
false
false
0.0
0.0
false
SUPPORTED
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 1.0
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 1.0
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 0.9
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 1.0
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 1.1
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 0.9
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 1.0
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 1.0
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 1.0
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 1.0
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 1.0
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 1.0
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 1.0
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 0.8
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 0.9
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 0.9
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 1.0
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 0.8
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 0.9
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 1.0
EXT-CLUSTER
GLOBULAR CLUSTER
J2000
J2000
(V-I) = 0.9
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
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No
F814W
POS-TARG
DITHER
3.034
LINE
false
false
3
85.29
ACS-WFC-DITHER-LINE
1
false
POS-TARG
DITHER
DITHER
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3.264
WFC3-UVIS-DITHER-BOX
false
81.785
false
0.112
0.173
3
63.697
POS-TARG
WFC3-UVIS-MOSAIC-LINE
23.884
2
false
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