0 Assigned ID: 194 ----- Attempting Submission 1 (Thu Apr 06 04:00:54 GMT 2017) ----- HST Phase I Proposal 194 (linerprop.apt) successfully submitted. Receipt: # 194-1 ----- Attempting Submission 2 (Fri Apr 07 21:18:44 GMT 2017) ----- The BOT does not find any sources at this position since this is the center of a nearby large galaxy. However, I have used a 1996 HST FOS UV/optical spectrum of the M81 nucleus (taken with the FOS 0.86" aperture) to run exposure time calculations in the STIS ETC and the nuclear UV source is well below any count rate limits for the STIS MAMAs. Revised submission on 2017 Oct 20 to change IR filter from F160W to F153M. -1332124818 ----- Attempting Submission 1 (Wed Jul 19 18:34:47 GMT 2017) ----- HST Phase II Proposal 15123 (15123phase2.apt) successfully submitted. Receipt: # 15123-1 ----- Attempting Submission 2 (Fri Oct 20 20:24:01 GMT 2017) ----- Probing the accretion flow and emission-line regions of M81, the nearest broad-lined low-luminosity AGN The nucleus of M81 is an object of singular importance as a template for low-luminosity accretion flows onto supermassive black holes. We propose to obtain a complete, small-aperture, high S/N STIS UV/optical spectrum of the M81 nucleus and multi-filter WFC3 imaging covering the UV through near-IR. Such data have never previously been obtained with HST; the only prior archival UV/optical spectra of M81 have low S/N, incomplete wavelength coverage, and are strongly contaminated by starlight. Combined with new Chandra X-ray data, our proposed observations will comprise the definitive reference dataset on the spectral energy distribution of this benchmark low-luminosity AGN. These data will provide unique new constraints on the possible contribution of a truncated thin accretion disk to the AGN emission spectrum, clarifying a fundamental property of low-luminosity accretion flows. The data will additionally provide new insights into broad-line region structure and black hole mass scaling relationships at the lowest AGN luminosities, and spatially resolved diagnostics of narrow-line region excitation conditions at unprecedented spatial resolution to assess the impact of the AGN on the ionization state of the gas in the host galaxy bulge. This program is designed to obtain complete UV and optical spectroscopy plus multi-band near-UV through near-IR imaging of the nucleus of M81. We will obtain STIS spectroscopy in the 0.2 arcsec slit in the G140L, G230L, G430L, and G750L grating settings, plus the G750M grating with central wavelength 6581 A to obtain a medium-resolution spectrum of the H-alpha + [NII] blend. This program also includes a coordinated Chandra HETG observation of M81 in order to obtain the spectral energy distribution from X-rays through UVOIR wavelengths. In order to minimize the impact of AGN variability on the spectral energy distribution measurement, we have grouped the HST visits to be observed within a 14 day window. If it is possible for all visits to be scheduled within an even shorter time window, that would be very beneficial for the science, so we request that the observations be scheduled within the shortest time span that is feasible to obtain. The HST visits can be carried out in any sequence, within the specified time window. We have also used the SAME-ORIENT-AS keyword to require that all of the STIS visits should be carried out at the same spacecraft orientation, in order to sample the same portion of the AGN narrow-line region within the STIS slit. We will also request that the Chandra observation be obtained during the same 14 day window if possible. Each STIS visit will begin with a standard STIS target acquisition. The AGN nucleus is compact and bright, and we select ACQTYPE=POINT because this has been used successfully for past STIS acquisitions of the M81 nucleus in programs 7350 and 7351. For the UV spectroscopy, we have 4 orbits for G140L and 1 orbit for G230L. These are broken up into two separate visits: one visit with 3 orbits of G140L, and one visit with 1 orbit of G140L and one orbit of G230L. The MAMA observations will be dithered using the STIS-ALONG-SLIT pattern following the recommendation of Section 12.5.1 of the STIS instrument handbook. For the MAMA observations, ACCUM mode will be used instead of TIME-TAG because the higher overheads required for memory buffer dumps for dithered TIME-TAG observations would lead to a reduction in the on-source integration time. The STIS CCD observations will be carried out in a separate visit, with one orbit for G750M observations and one orbit for G430L and G750L. In each case, we will obtain 5 exposures dithered with STIS-ALONG-SLIT in order to optimize the cosmic-ray cleaning to produce a high S/N spectrum. For G750L we will obtain CCDFLAT exposures at the end of the orbit. CCDFLATs will be done using the 52X0.1 slit as recommended for point sources in Table 11.1 of the STIS Instrument Handbook. For the G750L observation of M81, we choose not to use the E2 aperture position since this would negatively impact the overall throughput and would negatively impact the spectral and spatial matching with the G430L grating observation. With WFC3, we will obtain observations in F218W, F438W, F547M, and F814W (UVIS), and F153M (IR). Short exposure times will be used in order to avoid saturation of the bright nuclear point source in the optical filters. In order to fit all WFC3 observations into one orbit and avoid buffer dump overheads, we will use subarray readouts for the UVIS and IR detectors. Subarray readouts are acceptable in this case because our primary goal is to measure the AGN point source flux, and the HST archive already contains extensive full-frame observations of M81 in multiple filters. There are no orientation constraints for the WFC3 visit, but it should be done as close in time to the STIS observations as is feasible, within the specified 14-day window. Massive Black Holes And Their Host Galaxies 6 false true false false false 15 true SUPPORTED GALAXY ACCRETION DISK BLR LINER NLR NUCLEUS Coordinates are from ICRF2 catalog (Fey et al 2015, AJ, 150, 58) and were checked against SDSS and 2MASS images for consistency. J2000 J2000 STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G750M 6581 WFC3/UVIS Imaging No No F218W WFC3/UVIS Imaging No No F438W WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F814W WFC3/IR Imaging No No F153M POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 2 false POS-TARG DITHER 0.572 LINE 0.365 false false 74.653 4 18.528 WFC3-IR-DITHER-BOX-MIN 3 false POS-TARG DITHER 0.4 LINE false false 3 90.0 STIS-ALONG-SLIT 5 false POS-TARG DITHER 0.1 LINE false false 5 90.0 STIS-ALONG-SLIT 6 false /data/barth/proposals/hst/cycle25/phase2/15123-m81/OP-cache/15123phase2-v01.xml Timing link suitability includes constraints ([Group (01 02 03 04) Within 14.0 days]) Hst Same orient constraint links visits (01 02 03) The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. All 4 visits should be done within a total span of 14 days, and a shorter total span is strongly preferred in order to minimize the impact of source variability. Please schedule all visits as close in time to one another as is feasible. Visits 1, 2, and 3 should be done at the same spacecraft orientation to obtain the same STIS slit positioning on the target. (Tic-Visit :proposal-id 15123 :visit-id "01" :proposal-version -1 :trans-version "20170613" :date "19-Jul-2017 11:04:17.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 696320 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15123 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15123 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3212 :al-overhead-at-end 85 :internal-dur-at-end 132 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3546 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15123 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3322 :al-overhead-at-end 85 :internal-dur-at-end 132 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3546 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15123 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3322 :al-overhead-at-end 85 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3546 :pcs-gap 0 ) true 3 0 ACQ exposure time of 10 s was used previously in GO-7350, producing ~17000 counts within a 3x3 checkbox at the galaxy nucleus. /data/barth/proposals/hst/cycle25/phase2/15123-m81/OP-cache/15123phase2-v02.xml Timing link suitability includes constraints ([Group (01 02 03 04) Within 14.0 days]) Hst Same orient constraint links visits (01 02 03) The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 15123 :visit-id "02" :proposal-version -1 :trans-version "20170613" :date "19-Jul-2017 11:04:26.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 487584 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15123 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15123 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3212 :al-overhead-at-end 85 :internal-dur-at-end 132 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3546 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15123 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3322 :al-overhead-at-end 85 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3546 :pcs-gap 0 ) true 2 0 /data/barth/proposals/hst/cycle25/phase2/15123-m81/OP-cache/15123phase2-v03.xml Timing link suitability includes constraints ([Group (01 02 03 04) Within 14.0 days]) Hst Same orient constraint links visits (01 02 03) The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 15123 :visit-id "03" :proposal-version -1 :trans-version "20170613" :date "19-Jul-2017 11:05:33.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 386880 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15123 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15123 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3209 :al-overhead-at-end 75 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3546 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15123 :visit-id "03" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3324 :al-overhead-at-end 0 :internal-dur-at-end 640 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3546 :pcs-gap 0 ) true 2 0 /tmp/OPVisit6739316041085586905.xml Timing link suitability includes constraints ([Group (01 02 03 04) Within 14.0 days]) The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 15123 :visit-id "04" :proposal-version -1 :trans-version "20170613" :date "20-Oct-2017 13:21:17.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 345872 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15123 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15123 :visit-id "04" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3213 :al-overhead-at-end 0 :internal-dur-at-end 459 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3546 :pcs-gap 0 ) true 1 0