0 Assigned ID: 501 ----- Attempting Submission 1 (Fri Apr 07 13:06:12 GMT 2017) ----- HST Phase I Proposal 501 (AndXIX_c25.apt) successfully submitted. Receipt: # 501-1 ----- Attempting Submission 2 (Fri Apr 07 16:06:32 GMT 2017) ----- HST Phase I Proposal 501 (AndXIX_c25.apt) successfully submitted. Receipt: # 501-2 ----- Attempting Submission 3 (Fri Apr 07 18:54:18 GMT 2017) ----- Submitting for PI who can't seem to connect to the servers here. -1488616950 ----- Attempting Submission 1 (Wed Jul 19 15:12:51 GMT 2017) ----- Unveiling the formation of Andromeda XIX - a uniquely diffuse Local Group galaxy We request 16 orbits of HST/ACS to obtain imaging in F606W and F814W of Andromeda (And) XIX, a truly unique galaxy. With an effective radius of 3.1 kpc, and a surface brightness of 29.3 mag per square arcsec, it is the only known Local Group analogue of the intriguing newly-discovered ultra diffuse galaxies found at higher redshift. And XIX contains significant substructure, and is one of only 3 low mass galaxies that is known to have prolate rotation. This suggests the possibility that And XIX formed as the result of a merger. Using deep, coordinated parallel HST/ACS and WFC3 imaging, we will efficiently test this formation scenario. Our proposed observations will allow us to measure detailed star formation histories for both the centre of And XIX, and its most significant substructure, the southern clump. If And XIX has been formed as the result of a merger, we expect to see significant differences between the star formation histories of both fields. If And XIX has formed through secular processes or tidal stripping, we expect to see no difference between the two fields. Either result will place a strong constraint on the formation of And XIX, and therefore also the most diffuse galaxies known. Our primary objective is to measure the star formation history (SFH) in the center of And XIX, as well as its most significant substructure, the southern clump. As the southern clump is separated from the center of And XIX by the distance between the ACS and WFC3 camera, this can be achieved with a coordinated parallel observation using these two instruments. We will therefore observe And XIX with one central ACS/WFC field and one parallel WFC3/UVIS field positioned in the southern clump. Field positioning To coordinate our parallel WFC3 observation in the southern clump substructure with our primary ACS field, we require a specific ORIENT. Using the Aladin tool in APT, we determine that both the central field and the substructure can be efficiently targeted with ORIENTs between 155 and 177 degrees. All visits require the same orientation, to ensure we sample the same region of And XIX with each visit, and this has been specified in our visit descriptions. Required depth Our depth constraints are set by the need to measure precision SFHs over the lifetime of And XIX. We employ the F814W and F606W filters (for both ACS and WFC3), which are well-suited for measuring the SFHs of nearby dwarf galaxies (e.g. Brown et al. 2015). To achieve our science goal, we require S/N > 8 at the oldest main sequence turn-off (Weisz et al. 2014) for And XIX. This S/N will permit us to reliably distinguish stars from background galaxies at this depth (Radburn-Smith, 2011). Simulations of And XIX in our phase 1 proposal indicate that the oMSTO in And XIX is located at F606W = 28.1 mag and F814W = 27.7 mag. Exposure times and observational strategy Using the ACS ETC, we determine that to reach a S/N = 8 at these depths, we require 7 orbits in F606W and 9 orbits in F814W, totalling16 orbits. To increase the schedulability of our observations, we have set schedulability to 60, giving a total of 36 days in cycle 25, for which these observations can be made. We will split each orbit between F606W and F814W, which will allow these observations to be used to obtain RR Lyrae light curves (e.g., Brown et al. 2004). While not a primary part of our science case, it does not detract from our use case and substantially enhances the archival value. To properly sample the lightcurves, we require our visits to be seprataed by between 4 hours and 3 days. Also, as RR Lyrae periods are ~12 hours, the visits must not be spaced by precisely N*0.5 days. Standard 4-point dither patterns will be used to achieve 0.5 pixel sampling. Stellar Populations 6 false false false false false false SUPPORTED GALAXY DWARF SPHEROIDAL This object was generated by the targetselector and retrieved from the SIMBAD database. 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