0
Assigned ID: 1053
----- Attempting Submission 1 (Fri Apr 07 22:53:50 GMT 2017) -----
We are observing faint globular clusters within extended low-surface-brightness galaxies. We chose to place our targets at WFC1-FIXED since they are extended. Please let us know if there is a better choice for our science. Many thanks.
1557064424
----- Attempting Submission 1 (Thu Jul 13 22:11:48 GMT 2017) -----
Weighing Ultra-Diffuse Galaxies: Bridging the environmental gap
Interest in ultra-low-surface brightness galaxies has been reignited by the discovery of a substantial population of ultra-diffuse galaxies (UDGs) in dense clusters. These galaxies are characterized by dwarf-like stellar masses spread across giant-galaxy sizes, and their prolonged survival in clusters suggests that they may be extremely dark-matter dominated. The dark matter halos of a handful of UDGs in dense clusters have been "weighed" by the detection of rich globular cluster (GC) systems (~20-100 GCs), and indeed, their inferred mass-to-light ratios (M/L > 1000) are unprecedented for their stellar masses. More recently, galaxies with UDG-like properties have been discovered in much lower-density environments. However, the connection between UDGs across the full range of halo environments remains uncertain. Do extreme mass-to-light ratios persist throughout this population regardless of environment? Or, is this a unique characteristic of UDGs in galaxy clusters? Thanks to the depth and wide-area coverage afforded by our ongoing Hyper Suprime-Cam (HSC) Survey, we are carrying out the first truly blind search for UDGs to address this question. We currently have a sample of ~300 UDG candidates in environments ranging from the field to intermediate-mass groups. We propose to use ACS/WFC imaging to study the GC systems of 10 UDGs selected for their association with poor groups that span a range in environment a factor of ~10 to 100 less dense than Coma. Our program has the potential, for the first time, to establish a connection between the extremely dark-matter dominated UDGs in dense galaxy clusters and those being discovered in much lower-density environments.
Observing Plan: We will spend the first full orbit on the F814W band, dividing the exposure into two dithers. After guide-star acquisition (6 min), read-out (6.5 min), and one dither (0.5 min), we are left with 40 min of exposure time, assuming a typical 53 min orbit. We will divide that time evenly into two 1200 sec exposures, using the ACS-WFC-DITHER-LINE pattern. In the second orbit, guide star aquisition takes only 4 min, so we have a total of 42 min of exposure on F606W, allowing us to reach comparable depths in the two filters.
Stellar Populations
Galaxies and the IGM
6
false
false
false
false
false
false
SUPPORTED
GALAXY
DWARF ELLIPTICAL
LSB
YES
J2000
J2000
GALAXY
DWARF ELLIPTICAL
LSB
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J2000
J2000
GALAXY
DWARF ELLIPTICAL
LSB
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J2000
J2000
GALAXY
DWARF ELLIPTICAL
LSB
J2000
J2000
GALAXY
DWARF ELLIPTICAL
LSB
J2000
J2000
GALAXY
DWARF ELLIPTICAL
LSB
J2000
J2000
GALAXY
DWARF ELLIPTICAL
LSB
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J2000
J2000
GALAXY
DWARF ELLIPTICAL
LSB
YES
J2000
J2000
GALAXY
DWARF ELLIPTICAL
LSB
YES
J2000
J2000
GALAXY
DWARF ELLIPTICAL
LSB
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J2000
J2000
ACS/WFC
Imaging
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No
F814W
ACS/WFC
Imaging
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No
F814W
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No
F814W
ACS/WFC
Imaging
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No
F814W
ACS/WFC
Imaging
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No
F814W
ACS/WFC
Imaging
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No
F814W
ACS/WFC
Imaging
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No
F814W
ACS/WFC
Imaging
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No
F814W
ACS/WFC
Imaging
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No
F814W
ACS/WFC
Imaging
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F814W
ACS/WFC
Imaging
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No
F606W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
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No
F606W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F606W
POS-TARG
DITHER
3.034
LINE
false
false
2
85.29
ACS-WFC-DITHER-LINE
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