Per J. Anderson's helpful suggestions: added pos targs (0.08 offsets) to each UVIS orbit; readjusted UVIS Primary exposures to be closer to the same length -601714376 ----- Attempting Submission 1 (Fri Jul 04 14:55:38 GMT 2014) ----- ----- Attempting Submission 2 (Wed Jul 16 13:53:21 GMT 2014) ----- ----- Attempting Submission 3 (Wed Jul 23 19:18:55 GMT 2014) ----- ----- Attempting Submission 4 (Thu Jul 24 14:57:09 GMT 2014) ----- HST Phase II Proposal 13710 (m31_uv_bulge_phase2.apt) successfully submitted. ----- Attempting Submission 5 (Thu Jul 24 14:59:01 GMT 2014) ----- HST Phase II Proposal 13710 (m31_uv_bulge_phase2.apt) successfully submitted. ----- Attempting Submission 6 (Thu Jul 24 15:00:43 GMT 2014) ----- ----- Attempting Submission 7 (Fri Aug 29 16:54:58 GMT 2014) ----- ----- Attempting Submission 8 (Mon Oct 20 18:02:27 GMT 2014) ----- ----- Attempting Submission 9 (Tue Oct 21 08:37:57 GMT 2014) ----- ----- Attempting Submission 10 (Sat Nov 01 14:15:20 GMT 2014) ----- ----- Attempting Submission 11 (Mon Mar 02 23:48:45 GMT 2015) ----- 0 Assigned ID: 71 ----- Attempting Submission 1 (Tue Apr 08 15:53:27 GMT 2014) ----- HST Phase I Proposal 71 (m31uv_c22.apt) successfully submitted. ----- Attempting Submission 2 (Thu Apr 10 10:30:01 GMT 2014) ----- HST Phase I Proposal 71 (m31uv_c22.apt) successfully submitted. ----- Attempting Submission 3 (Fri Apr 11 11:04:26 GMT 2014) ----- HST Phase I Proposal 71 (m31uv_c22.apt) successfully submitted. ----- Attempting Submission 4 (Fri Apr 11 15:34:50 GMT 2014) ----- HST Phase I Proposal 71 (m31uv_c22.apt) successfully submitted. ----- Attempting Submission 5 (Fri Apr 11 19:32:57 GMT 2014) ----- HST Phase I Proposal 71 (m31uv_c22.apt) successfully submitted. ----- Attempting Submission 6 (Sat Apr 12 14:56:54 GMT 2014) ----- We aim to use HST observations of M31 to generate the definitive data set for modeling the population of the UV-bright stars that contribute to the UV flux in old stellar populations (i.e., the "UV excess" seen in some elliptical galaxies and spiral bulges). We propose to place stringent observational constraints on the post-AGB (P-AGB) and post-early AGB (PE-AGB) phases of stellar evolution using a UV survey of M31's bulge. M31 is a critical laboratory for testing these models, as it hosts an old, metal-rich stellar population with high stellar densities such that even rare evolutionary phases are well-represented. We will (1) assemble a catalog of UV-bright stars in the center of M31 in F336W and F225W, extending out to ~0.7 kpc, to sample stellar populations with different metallicities; and (2) image a smaller 0.9 sqr-arcmin strip with ACS/SBC in F140LP, to image the regions with the highest density of rapidly-evolving P-AGB stars. The FUV imaging will allow us to separate the P-AGB from the PE-AGB. These observations will include thousands of UV-bright stars, increasing the size of existing samples by orders of magnitude. These new observations will drive revisions in models for post-HB evolution, which we will merge into new isochrone libraries and stellar population synthesis codes. The revisions will have important implications for AGB evolution, spectral evolution models of galaxies, and for mass loss on the RGB. The observations will also have a direct impact on interpreting (1) the UV flux from old stellar populations; (2) the emission line flux from M31's nuclear spiral; and (3) models of dust heating by old stellar populations. Overview: Our observations consist of (1) 1 F225W+F336W WFC3/UVIS pointing oriented along the minor axis of the M31 bulge to get significantly better temperature sensitivity and depth than existing data; (2) 2 F140LP pointings (3200 arcsec^2) in the central region, where the density of the P-AGB stars are highest, to get optimal constraints on the hottest, rarest stars; (3) a third F225W+F336W WFC3/UVIS image, carried out in parallel with the primary SBC mosaic, to get additional area and better sampling of M31's radial metallicity and abundance gradient; (4) F502N, F658N, F555W, F625W ACS/WFC images taken in parallel with the primary WFC3/UVIS pointing to identify PNe, which will be used to calibrate PNe selection in the PHAT filter set, giving us more leverage on their separation from post-EHB stars in the bulge. Tiling Strategy: To sample the metallicity/abundance gradient in M31's bulge, we require 1 UVIS pointing. The primary pointing over the M31 center covers out to r ~0.5 kpc, comparable to where the UV-bright population gradient was identified in brighter PHAT data. For the SBC F140LP observations, we would ideally tile the whole area covered by the UVIS tiles. However, such a tiling is not feasible, given the SBC's smaller FOV. Moreover, given the rapid fall-off in the P-AGB population seen in the PHAT F275W data (see Rosenfield et al., 2012), observations far from the center become increasing inefficient. We therefore select a minimal set of 3 tiles arranged and sample the high density P-AGB regions (~0.27 kpc). Based on the PHAT F275W data, it is not possible to avoid the small sparse dust lanes found in M31's bulge. However, the dust features are extremely narrow and well-localized such that they can be excluded from our analysis. In addition, we will use the exctiction measurements from Dong et al., 2014 who also identified and characterized 5 dusty clumps near the nucleus of M31. The second UVIS region comes essentially free as a parallel and samples r~1 kpc. Orientations were chosen to maximize schedulability and to arrange parallels to overlap eachother and existing multiwavelength data from PHAT. A test Phase II proposal including these constraints demonstrates that the 6 orbits of far-UV imaging (plus parallels) has 96 days per year of availability, while the 4 orbits of near-UV imaging has 61 days of availability. Filter Choices: With a target color error of ~0.05 mag, we calculate excellent temperature sensitivity for Teff<32,000K in F225W-F336W and for Teff<80,000K in F140LP-F336W; the former is adequate for constraining models of PE-AGB and AGBM stars, and for brighter P-AGB stars, and the latter is necessary to track P-AGB evolution fainter than F336W~24, where it would otherwise be blended with other evolutionary phases (i.e, PE-AGB, AGBM). We chose F140LP over other SBC filters to block strong airglow lines (Ly-alpha and O I) while retaining sufficient throughput. The target photometric error is roughly equivalent to STScI ETC's Optimal SNR~20 for PSF photometry. We set the exposure time to reach this SNR at F140LP=24.8, F225W=25.1, and F336W=26.3 (while these are the formal optimal SNR we expect, in practice the EHB crowding in the bulge will shift our limiting magnitudes slightly fainter; these depths are chosen to reveal the evolutionary phases of interest in each color-combination, while still being bright enough to avoid crowding from fainter, more numerous HB stars. The required exposure times can be reached in 4 orbits for the UVIS pointing (3 orbits for F225W and 1 orbit for F336W which we will co-add with the archival PHAT data) and 2 orbits for each of the two SBC pointings. Brown's previous FOC far-UV imaging found only 52 stars brighter than 23 VEGAMAG in a 14 x 14'' region that included the M31 center. Extrapolating from the PHAT data, we estimate we will obtain SNR=10 photometry of thousands of sources above F140LP=23.6 and F225W=24.0, including all PE-AGB and P-AGB stars above 10,000K and the brightest AGBM stars as well as ~10,000 UV-bright stars in our F225W+F336W images. Need for HST: HST is required for this project. The high stellar densities of M31's bulge cannot be resolved in the UV from the ground, likewise, the F225W and F140LP wavelengths can only be reliably detected from space. Parallels: We will use WFC3/UVIS in parallel with the primary ACS/SBC observations, using identical filters as the primary UVIS exposures; these parallels will give us additional areal and radial coverage. When running WFC3/UVIS in primary, we will use ACS to optimize the selection and analysis of PNe throughout the PHAT imaging area, giving us additional leverage on post-AGB evolution in the bulge of M31. To do this, we will carry out narrow band imaging of [OIII]5007 AA (F502N), Halpha (F658N; to discriminate from HII regions) and the corresponding continuum (F555W, F625W). While PHAT has coverage in F475W and F814W, adding F625W and F555W will sample the continuum at 2 intermediate points with high S/N. Any stellar continuum can be well modeled with these 4 points. Ancillary Science: In addition to our primary science goals, our observations will be extremely useful for further studies of M31's young nuclear cluster (Lauer et al., 2012), the contribution of old UV bright stars to dust heating (known to be unusual in M31's center), the possible ionization of the ISM by P-AGB and PE-AGB populations (which can potentially be confused with LINER emission from AGN), and possibly using the UV-upturn as an age indicator for elliptical galaxies (Dorman et al., 1995; Bressan et al., 1994) RESOLVED STELLAR POPULATIONS 12 Regular false true 0.0 0.0 false false false SUPPORTED GALAXY BULGE This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 GALAXY BULGE This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 GALAXY BULGE This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 GALAXY BULGE This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 ACS/SBC Imaging No No F140LP ACS/SBC Imaging No No F140LP ACS/SBC Imaging No No F140LP WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F225W WFC3/UVIS Imaging No No F225W ACS/WFC Imaging No No F502N ACS/WFC Imaging No No F658N ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F550M ACS/WFC Imaging No No F502N ACS/WFC Imaging No No F658N ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F550M POS-TARG DITHER 0.472 LINE false false 2 44.4 ACS-SBC-DITHER-LINE 1 false POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 2 false 1425336037213 Hst Same orient constraint links visits (01 02 03) The scheduling data was generated by CASM 23.0. 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