0 Assigned ID: 975 ----- Attempting Submission 1 (Fri Apr 07 22:06:42 GMT 2017) ----- HST Phase I Proposal 975 (cycle25_phase1.apt) successfully submitted. Receipt: # 975-1 Use of the UVIS-M1K1C-SUB aperture for the F438W/F555W observations is not ideal, but all other alternative configurations require either guide star re-acquisition or buffer dumps. The choice still applies to this resubmission. -982448730 ----- Attempting Submission 1 (Tue Jul 18 01:28:30 GMT 2017) ----- ----- Attempting Submission 2 (Wed Dec 05 23:49:42 GMT 2018) ----- Stellar Luminosity Profiles for Precision Measurements of Black Hole Mass in Early-Type Galaxies We have obtained ALMA CO(2-1) data for a sample of nearby early-type galaxies, of which nine are detected in CO at high S/N and show rotation-dominated kinematics. We are in the process of modeling the kinematics of these molecular gas disks to derive accurate measurements of the black hole masses in these galaxies. Near-IR imaging is essential in order to measure the stellar luminosity profiles for these galaxies with dusty circumnuclear disks, and WFC3/IR imaging data is available or pending for only two of our CO disk galaxies. We propose to obtain WFC3/IR and UVIS data for the remaining seven galaxies. Gas mass measurements suggest that the dust extinction may reach ~1 mag in the H-band, and we are developing a modeling method to recover pixel-by-pixel extinction maps for these dust disks and produce dust-corrected stellar luminosity profiles using imaging in filters from the B to H bands. Using the dust-corrected stellar luminosity profiles together with the ALMA kinematic data, we will be able to determine black hole masses with precisions reaching ~10%. We request a single orbit for each of the seven galaxies. We propose to obtain WFC3/UVIS F438W or F555W observations, as well as WFC3/IR F110W and F160W observations to measure the stellar surface brightness profiles of seven early type galaxies possessing circumnuclear dust disks: NGC 1332, NGC 3268, NGC 3557, NGC 4697, NGC 4786, NGC 5838, and NGC 6861. We require a single orbit for each target to complete this imaging. These observations will complement existing optical broadband imaging, allowing us to model spatially resolved dust obscuration across optical to near-IR wavelengths. Based on their declinations, these galaxies have visibility periods between 53 and 56 minutes. The largest single overhead in each orbit will be six minutes for guide star acquisition, along with small telescope movements to dither the telescope and changes between WFC3 detectors/filters. We will mosaic the field around each galaxy in the F160W filter using a 2x2 pattern with offsets of ~40 arcsec. This mosaic places the central bright region of the galaxy within the overlap region between all four pointings and covers a total 3.5x3.5 arcmin^2 field. The F160W images will be taken with NSAMP=10 in the STEP50 mode, providing sufficient integration times to map the stellar surface brightness profiles out to the mosaic edges as well as taking enough reads at early times (<30 seconds) to allow up-the-ramp sampling to avoid saturating on the galaxy nuclei as well as to reject cosmic rays. The resulting mosaics will have a total galaxy center integration time of 1000 s in the F160W filter. At the outskirts of the mosaic, these observations will probe down to a limiting H-band surface brightness of ~22.3 mag/arcsec^2 in a 5x5pixel region. The F110W images will be obtained in a two-point WFC3-IR-DITHER-LINE pattern, centered on the nuclei, also with NSAMP=10 in the STEP50 mode, permitting a total of 500 s integration in the inner ~2x2 arcmin^2 field. As for the F160W images, these SAMP-SEQ and NSAMP values allow up-the-ramp sampling to reject cosmic rays and avoid nuclear saturation. The final set of observations for each galaxy will be either F438W or F555W WFC3/UVIS images (depending on whether archival HST B or V data are already available) in a four-point WFC3-UVIS-BOX-MIN pattern centered on the nucleus. To avoid saturating the galaxy centers, these broadband images are intentionally short (~130 s at each dither location); the emergence of restrictive buffer dumps when utilizing the full array leads us to request only a subarray for these UVIS observations. If using the optimal subarray (UVIS2-C1K1C-SUB), the guide star needs to be reacquired between the WFC3/IR and UVIS patterns, regardless of the ordering of previous IR observations. Instead, we select the UVIS2-M1K1C-SUB subarray for these F438W/F555W observations. Sufficient FLASH is included in each observation to mitigate CTE losses when using this subarray. As the stellar surface brightness profiles for each galaxy will be derived from their F160W mosaics, and the additional broadband imaging is needed to model the dust obscuration in the <5 arcsec radius dust disks, the smaller field of view and slightly worse CTE of this WFC3/UVIS subarray will not negatively impact this project. This UVIS pattern leads to ~500 s total integration in a ~50x50 arcsec^2 region about each galaxy center. Massive Black Holes And Their Host Galaxies 6 false false false false false false false SUPPORTED GALAXY DUST LANE LENTICULAR NUCLEUS This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 GALAXY DUST LANE ELLIPTICAL NUCLEUS This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 GALAXY DUST LANE ELLIPTICAL NUCLEUS This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 GALAXY DUST LANE ELLIPTICAL NUCLEUS This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 GALAXY DUST LANE ELLIPTICAL NUCLEUS This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 GALAXY DUST LANE LENTICULAR NUCLEUS This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 GALAXY DUST LANE LENTICULAR NUCLEUS This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F438W WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F555W WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F438W WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F555W WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F438W WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F555W WFC3/IR Imaging No No F110W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F438W POS-TARG DITHER 0.636 LINE false false 2 41.788 WFC3-IR-DITHER-LINE 2 false POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 3 false The scheduling data was generated by CASM 26.2.2. 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