0 Assigned ID: 1544 ----- Attempting Submission 2 (Fri Mar 01 16:51:14 GMT 2013) ----- HST Phase I Proposal 1544 (S0_CSS_apt_v3.pdf.apt) successfully submitted. ----- Attempting Submission 3 (Fri Mar 01 22:25:24 GMT 2013) ----- The position and orientation of the WFC3/UVIS and IR detectors are chosen such that UGC 12591 is covered entirely by both the UVIS and the IR chanels and the UVIS chip gap does not cross the galaxy. This will benefit both the scientific and the outreach quality of the images. Also, the lower UVIS detector covers a nearby (in projection) galaxy, which may be (have been) interacting with UGC 12591. 1160857489 ----- Attempting Submission 1 (Mon Jun 17 11:22:16 GMT 2013) ----- These warnings can be ignored as they do not affect the scientific goals or orbit planning of the proposal. We propose to determine the formation history of UGC12591 - the most massive known field S0 galaxy in the nearby Universe (D ~ 98Mpc). Its maximum rotational velocity of 483 km/s yields a dynamical mass within 50 kpc of 2x10^12 solar masses. Given its field location, this poses the question of how such a massive bulge can grow in isolation? To trace the UGC12591 star formation and assembly history we will use the properties of its globular clusters (GCs) and massive compact stellar systems which are expected in huge numbers given its mass. In particular, GCs are well known to be among the best indicators of major (merger) galaxy formation episodes, capturing the physical conditions at the time of their formation. With the wide spectral coverage of the proposed obesrvations, we will 1) search for multiple/intermediate-age GC populations and 2) measure whether the specific frequency of the metal-rich GCs relative to the bulge luminosity is enhanced. If any of these points are confirmed, this would strongly favor a merger-driven (gas-rich) as opposed to "passive" bulge growth (secular evolution). The only possible way to derive robust photometric GC ages and metallicities at the distance of UGC12591 in a reasonable amount of time is by employing the efficiency of HST/WFC3 and the age-metallicity sensitive V, I, H filter combination (F606W, F814W, F160W). In four orbits we will observe the brighter half of the GC population of UGC12591, which will enable us to derive GC population peak age and metallicity (+/- 20%). The results from this proposal will offer an important leap forward in our understanding of the assembly history of extremely massive isolated S0 galaxies. Observations will be performed with the UVIS & IR F606W, F814W, F160W filter set (i.e. V, I, H) to allow a robust GC age and metallicity derivation. Exposure times are estimated based on the STScI ETC and a custom made script to account for the local background surface brightness. To reach V<27.5mag with S/N>5, a BC03 G2V spectrum, E(B-V)=0.114mag, an "elliptical galaxy" background surface brightness of mu_V = 21 mag/arcsec^2 (typical for a few arcsec from the galaxy center), and zodiacal light calculated from the UGC 12591 position, we obtain the following exposure times: 2500, 3000 and 5700 seconds in WFC3/UVIS F606W, F814W , and IR F160W, respectively. Three-point dither-line pattern for the F606W and F814W and four-point for F160W will allow a good sampling of the PSF, and facilitate cosmic-ray and detectors artifacts removal. With the APT Phase II orbit planner optimization, and accounting for overheads, we were able to accommodate the following exposure time splits: 3x873 = 2619 and 3x913 = 2739 seconds for F606W and F814W, and 4x1400 seconds (NSAMP = 14, STEP200) in F160W. We note that beyond the central mu_V = 21 mag/arcsec^2 the S/N will be higher, i.e. at radius where the majority of the GCs are located in a galaxy. UGC 12591 is perfectly covered by one WFC3 pointing to about 2x of its D25 = 1.23' (RC3). The position and min and maxorient (230-265 degrees) were chosen such that the galaxy is entirely covered by one of the WFC3/UVIS detectors as well as the nearby satellite galaxy in the other. For proper analysis of the UGC 12591 evolution history, it is important to keep the observations within the specified position and orientation. To estimate background contamination from unresolved distant galaxies and foreground Galactic stars, we will use in coordinated parallel the ACS/WFC camera in F606W and F814W filters. The high spatial resolution of both WFC3 (0.04"/pix) and ACS (0.05"/pix) will already allow to significantly reduce the number of background contamination, unachievable with ground-based observations. Their exposure time splits have been adjusted such that the total integration time for each filter reaches S/N~10 at V=27.5mag. UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTURE 12 false false false false false SUPPORTED GALAXY ELLIPTICAL LENTICULAR This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 GALAXY ELLIPTICAL LENTICULAR This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 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/IR Imaging No No F160W ACS/WFC Imaging No No F606W ACS/WFC Imaging No No F814W POS-TARG DITHER 0.145 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE 1 false POS-TARG DITHER 0.636 LINE false false 4 41.788 WFC3-IR-DITHER-LINE 2 false 1370539456738 /Users/iskren/Work/Documents/Proposals/HST/Cycle21/S0s/OP-cache/S0_CSS_PhaseII-v01.xml The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. 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