0 Assigned ID: 811 ----- Attempting Submission 1 (Fri Apr 08 20:51:51 GMT 2016) ----- HST Phase I Proposal 811 (APT.apt.2016_04_08_01_53.aptbackup.2016_04_08_04_46.aptbackup.2016_04_08_06_17.aptbackup.2016_04_08_08_12.aptbackup.2016_04_08_16_36.aptbackup.2016_04_08_18_48.aptbackup) successfully submitted. Receipt: # 811-1 ----- Attempting Submission 2 (Fri Apr 08 21:00:19 GMT 2016) ----- HST Phase I Proposal 811 (APT.apt.2016_04_08_01_53.aptbackup.2016_04_08_04_46.aptbackup.2016_04_08_06_17.aptbackup.2016_04_08_08_12.aptbackup.2016_04_08_16_36.aptbackup.2016_04_08_18_48.aptbackup) successfully submitted. Receipt: # 811-2 ----- Attempting Submission 3 (Fri Apr 08 21:08:41 GMT 2016) ----- HST Phase I Proposal 811 (APT.apt.2016_04_08_01_53.aptbackup.2016_04_08_04_46.aptbackup.2016_04_08_06_17.aptbackup.2016_04_08_08_12.aptbackup.2016_04_08_16_36.aptbackup.2016_04_08_18_48.aptbackup) successfully submitted. Receipt: # 811-3 ----- Attempting Submission 4 (Fri Apr 08 21:10:18 GMT 2016) ----- HST Phase I Proposal 811 (APT.apt.2016_04_08_01_53.aptbackup.2016_04_08_04_46.aptbackup.2016_04_08_06_17.aptbackup.2016_04_08_08_12.aptbackup.2016_04_08_16_36.aptbackup.2016_04_08_18_48.aptbackup) successfully submitted. Receipt: # 811-4 PATTERN POSITION OUTSIDE APERTURE Our NGC205 STIS observation (Visit 2) has only ~1 month of schedulability. Please contact aseth@astro.utah.edu if this is going to be a problem to schedule. 1294368999 ----- Attempting Submission 1 (Mon Jul 18 18:15:28 GMT 2016) ----- Our dither pattern in Visit 3 moves the pointing out of the nominal E1 aperture -- however we don't think this will impact our observations and need to have separate dither positions. We have discussed this with Blair Porterfield. Measurements of black hole masses in massive early type galaxies have revealed that they tightly correlate with the properties of their host galaxies. At lower galaxy masses, almost no black hole mass measurements exist in early type galaxies, while existing measurements in later type galaxies show significant scatter. By finding and measuring the mass of black holes in low mass early type galaxies we can (1) constrain the fraction of low mass galaxies with black holes, an important measurement for understanding the formation of the first seed black holes, and (2) anchor the black hole mass scaling relations and quantify the scatter in these relations. We propose to make a robust dynamical estimation of the central black hole masses in three nearby, low mass early type galaxies. We request HST/STIS spectroscopy to constrain the variation in the stellar populations and mass-to-light ratio at high spatial resolution. We will combine this information with new and archival HST imaging to create accurate stellar mass maps of each galaxy. These will be combined with existing stellar kinematic maps from adaptive optics Gemini/NIFS and VLT/SINFONI data. The resulting analysis will enable us to dynamically measure black hole masses below the mass of any known central black holes. 1/ Purpose: ---------------------- Our observation includes of STIS spectroscopy of all three galaxies NGC 205 (2 orbits), NGC 5102 (4 orbits), and NGC 5206 (5 orbits) and WFC3 imaging (1 orbit) only for NGC 5102 to measure the spatial mass-to-light ratio variations within the NGC 205, NGC 5102, and NGC 5206 nuclei and enable a more robust masses determination of their black holes. We require that the total time for the imaging and spectroscopy will be observed within ~19 hours. 2/ Coordinates of the nucleus: ---------------------- For all images we have checked both the NED coordinates and those from 2MASS or the 2MASS large galaxy atlas. Some discrepancies exist at the <1" level for the centers of these galaxies, but given the size of the acquisition image (~5") we don't anticipate this lack of precision will cause any problems. 3/ STIS Spectroscopy: ------------------ We propose to obtain high spatial resolution observations of the stellar populations by obtaining STIS observations with the G430L gratings and the 52"x0.1" slit. we have chosen the 50CCD aperture to reduce CTE and used exposure times ~1000 sec to ensure good cosmic ray rejections. In total, we will obtain 5, 11, and 14 science exposures without any splits over 2, 4, and 5 orbits for NGC 205 (Visit 2), NGC 5102 (Visit 3), and NGC 5206 (iVisit 4), respectively. 3.1/ ACQ details: We have used existing HST WFPC2 & ACS/RHRC data of these galaxies on HLA to estimate the ACQ exposure times; specifically, F555W band for NGC 205 and NGC 5206, and the F547M band for NGC 5102. We calculate the magnitude in a 5x5 box to estimate the S/N in the STIS ETC, and to calculate saturation assuming this magnitude as a point source with a K0V Kurucz spectrum. For NGC205, NGC5206 & NGC5102 we get a ~V magnitude of 16.8, 17.1 & 14.7 respectively. This leads to minimum exposure times of 1s, 2s & 0.2s for each source, and saturation limits of 202s, 266s, and 29s. We choose 10s exposures for both ACQ and ACQ/PEAK exposures for NGC205 (increasing the ACQ/PEAK exposure time resulted in overfilling the first orbit), 10s ACQ exposures and 20s ACQ-PEAK in NGC5206, and 3s for ACQ and 6s for ACQ/PEAK in NGC5102. These exposure times should give us plenty of S/N and be <20% saturation in all cases. 3.2/ Exposure Times: Given the orbits available, we have tried to pack the visits with maximal efficiency. We find that packing three ~930s exposures per orbit, with the first orbit having the two acquisition exposures + 2 science exposures provides the maximal efficiency. In total we have 5 science frames in NGC205, 11 frames in NGC5102 and 14 science frames in NGC5206. These are designed to provide sufficient S/N out to radii of ~0.8". 3.3/ Dithers & CR-SPLIT: For NGC205 and NGC5102, no CR-SPLITs are used and integer pixel dithers are requested to ease combination of exposures without using multidrizzle. Larger dithers are used in NGC205 (since there are just 5 separate exposures). For NGC5206, we CR-SPLIT our exposures to get 7x2 science frames, each at a separate dither. This strategy is identical to our successful NGC404 STIS observations, but with larger dithers to ensure better subtraction using a median frame to mitigate detector artifcats.. 3.4/ Orientation: The position angles (E of N) desired for our observations are described below and are selected to roughly correspond to the major axis of the nuclear star clusters. We have added 45 degrees to these to determined the requested ORIENTs and included the 180 degree rotation of these to maximize schedulability, we note that NGC205 has minimal schedulability even with a relatively wide range of ORIENTs. NGC205 PA=135+-20 NGC 5102 PA=50+-10 NGC5206 PA=40+-20 4/ WFC3 Imaging for NGC 5102 ------------------------- For NGC5102, good archival imaging data is not available, so we requested 1 orbit of additional imaging. This will be used to measure the spatial stellar M/L ratio variability beyond the boundaries of the slit. We will obtain images in three filters (F336W, F547M, F814W), and four dithered exposures in each filter to ensure the highest possible spatial resolution for our observations. To manage so many exposures, we use the C512C subarray, which will give us information within the central 20" of the galaxy, sufficient for our mass-modeling purposes. The exposure times were simulated via ETC to make sure the S/N are still high enough (~10) out to the edge of the subarray field of (r ~ 10") and to ensure obtained images unsaturated. We used a variety of existing HST data and our adaptive optics data to estimate the colors in each band, and our requirements are met using 4x297s exposures in F336W, 4x120s exposures in F547M, 4x105s exposures in F814W. Massive Black Holes and their Hosts Galaxies 12 false false false false false false SUPPORTED GALAXY DWARF COMPACT DWARF ELLIPTICAL ELLIPTICAL NUCLEUS This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 GALAXY DWARF COMPACT DWARF ELLIPTICAL ELLIPTICAL NUCLEUS This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 GALAXY DWARF COMPACT DWARF ELLIPTICAL ELLIPTICAL NUCLEUS This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G430L 4300 WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F814W POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 1 false POS-TARG DITHER 1.523 LINE false false 5 90.0 STIS-ALONG-SLIT 2 false POS-TARG DITHER 0.711 LINE false false 11 90.0 STIS-ALONG-SLIT 3 false POS-TARG DITHER 1.016 LINE false false 7 90.0 STIS-ALONG-SLIT 4 false 1468864902171 /private/var/folders/_m/t72qk349343b2hlsz5bs5x4r0000gp/T/OPVisit6828353062558050935.xml The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. 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