Cannot find file /Users/bholwerd/Desktop/Proposals/HST/C25/UGC2885/hst-ugc2885-c25-v6.pdfversion 2, now with extra Jeremy-118796228Assigned ID: 630
----- Attempting Submission 1 (Fri Apr 07 16:39:53 GMT 2017) -----
HST Phase I Proposal 630 (UGC2885.apt) successfully submitted.
Receipt: # 630-1
----- Attempting Submission 2 (Fri Apr 07 19:26:51 GMT 2017) -----Broken up mosaic to place ACS on either side of galaxy. 3 dither positions per filter. 1 orbit per filter.
New setup suggested by STSCI and Rupali.658767406----- Attempting Submission 1 (Thu Jul 20 21:18:25 GMT 2017) -----
----- Attempting Submission 2 (Fri Sep 08 18:24:14 GMT 2017) -----The Cluster Population of UGC 2885UGC 2885 was discoverd to be the most extended disk galaxy [250 kpc diameter] by Vera Rubin in the 1980's. We ask for HST observations of UGC 2885 as it is close enough to resolve the GC population with HST but it is a substantially more extended disk than any studied before. LCDM galaxy assembly implies that the GC population comes from small accreted systems and the disk --and the clusters associated with it-- predominantly from gas accretion (matching angular momentum to the disk). Several scaling relations between the GC population and parent galaxy have been observed but these differ for disk and spheroidal (massive) galaxies.
We propose to observe this galaxy with HST in 4 point WFC3 mosaic with coordinated ACS parallels to probe both the disk and outer halo component of the GC population. GC populations have been studied extensively using HST color mosaics of local disk galaxies and these can serve as comparison samples. How UGC 2885 cluster populations relate to its stellar and halo mass, luminosity and with radius will reveal the formation history of extra-ordinary disk.
Our goals are twofold: our science goal is to map the luminosity, (some) size, and color distributions of the stellar and globular clusters in and around this disk. In absolute terms, we expect to find many GC but the relative relation of the GC population to this galaxy's mass (stellar and halo) and size will shed light on its formation history; similar to a group or cluster central elliptical or to a field galaxy (albeit one with a disk 10x the Milky Way's size)? Our secondary motive is to make an HST tribute image to the late Vera Rubin.The proposed observations are a straightforward three-filter 4-point mosaic of UGC 2885, oriented
along its major/minor axes. We ask for the F814W, F606W and F475W filters to follow closely
the database of previous studies on nearby low-inclination disk galaxies (e.g., Chandar et al.,
2010, 2015; Hudson et al., 2014).
WFC3 Mosaic
We ask for a 2 x 2 mosaic using WFC3, dithered between exposures and
oriented such that the ACS parallels are located at larger galactocentric radii.
ACS parallels
We ask for ACS parallels with the same filter set as the main WFC fields to
sample the halo cluster populations outside the immediate disk.
We ask for 180deg different orientation to position the ACS parallels on opposite
sides of the s
Exposure times
In a single orbit (40 min), a a signal-to-noise of ~5 is reached for 28.5
mag point sources in F606W. At the distance modulus to UGC 2885 (m - M = 34.49 mag),
this is sufficient to reach the turnover luminosity of the GC luminosity function.
Filter choices
Our choice of filters is based on experience with many other studies with HST
on nearby galaxies (Chandar et al., 2004, 2016; Barmby et al., 2006; Spitler et al., 2006; Harris
et al., 2009) and we opt for the same filters for consistency and to map the stellar populations in
these clusters. These filters cover the peak of the globular cluster SED; having
two colors improves discrimination between star clusters and background galaxies.
Dither Strategy
The WFC3-UVIS-MOSAIC-LINE approach is the most appropriate as the full UVIS channel of WEFC3 is to be used for the mosaic
and the ACS data.
offsets are defined as:
(0, 0) and (36.5, 71.5) pixels.
assuming a Pixel Size: 0.04 arcsec
1.46, 2.86" dither.
We assumed 2 dither positions is sufficient for cosmic ray rejection and chip gap masking.
Mosaic & Parallel Strategy
The mosaic was broken up in individual visits because it was imperative to place the ACS parallels on either side of the mosaic.
The single orbit is sufficient to reach the turnover of the GC luminosty function and a greater area covered would be beneficial in
the total GC population covered.Galaxies and the IGMStellar Populations6falsefalsefalsefalsefalsefalseSUPPORTEDGALAXYBULGEDISKSPIRALSPIRAL ARMSTAR FORMING REGIONThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYBULGEDISKSPIRALSPIRAL ARMSTAR FORMING REGIONThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYBULGEDISKSPIRALSPIRAL ARMSTAR FORMING REGIONThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYBULGEDISKSPIRALSPIRAL ARMSTAR FORMING REGIONThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYBULGEDISKSPIRALSPIRAL ARMSTAR FORMING REGIONThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/IRImagingNoNoF125WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF475WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF475WPOS-TARGDITHER0.135LINEfalsefalse346.84WFC3-UVIS-DITHER-LINE-3PT2false/private/var/folders/0k/z1mfxwb17qv56ltq6lg4h8y00000gn/T/OPVisit7751792595962434364.xmlThe scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.(Tic-Visit
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