0Assigned ID: 234
----- Attempting Submission 1 (Thu Mar 05 15:58:57 GMT 2020) -----
HST Phase I Proposal 234 successfully submitted.
Receipt: # 234-1
----- Attempting Submission 2 (Fri Mar 06 16:45:12 GMT 2020) -----FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browserThis submission incorporates ORIENT constraints for visits 03, 05, 06, 07, and 12, as approved by the TTRB for Change Request 91877:
Visit 03 (NGC 1358): Exclude ORIENTS 150-190 and 320-350.
Visit 05 (IC 3639): Exclude ORIENTS 275-340.
Visit 06 (NGC 5135): Exclude ORIENTS 85-100.
Visit 07 (NGC 5427): Exclude ORIENTS 70-110.
Visit 12 (NGC 3227): Exclude ORIENTS 240-260.480540415----- Attempting Submission 1 (Fri Jun 26 00:15:12 GMT 2020) -----
----- Attempting Submission 2 (Wed Oct 07 13:32:50 GMT 2020) -----The following warnings are present in the submitted Phase II APT file and are explained below.
POST-FLASH:
All exposures issue a warning that the post-flash level may be too high.
The CS has confirmed that STScI recently increased the recommended level from 12e- to 20e-.
The post-flash levels have been selected to meet this updated recommendation.
POS-TARG & PATTERN:
Most exposures issue a warning to use caution when specifying a POS-TARG or PATTERN for quadrant filters.
No POS-TARGS are used in this program. Patterns are used to obtain the desired dither levels.
The specified dither spacing is generally 3x the default value for all quadrant filter observations.
This is designed to improve image quality without significant loss of spatial information due to filter vignetting.Are Narrow Line Region Outflows an Effective Mode of AGN Feedback?The ionizing radiation generated by accreting supermassive black holes can drive powerful outflows that may play a key role in galaxy evolution by evacuating the galactic bulge of gas. These outflows are observed in the narrow line regions (NLRs) of AGN and can only be accurately characterized using the high spatial-resolution imaging and spectroscopy afforded by HST. We will build a sample of 22 nearby AGN to determine the spatially-resolved extents, mass outflow rates, and kinetic luminosities of their NLR outflows. We will do this efficiently by obtaining new [O III] plus continuum images of 13 Seyfert galaxies and combining them with MAST archival long-slit STIS spectra and photoionization models to increase the current sample of 3 AGN by a factor of ~7. The mass outflow rates will provide direct measures of the removal of potential star-forming gas and the kinetic luminosities will identify the locations and amounts of energy deposited into the gas to disrupt star formation. We will then model the enclosed mass profiles of the host galaxies to find their bulge radii and determine the extent to which radiation can drive outflows in the gravitational potential of the galaxy. The sample spans a significant range in luminosity, black hole mass, and Eddington ratio, allowing us to map the dependence of these outflow parameters on AGN properties and thereby determine the effectiveness of NLR outflows as a feedback mechanism in nearby AGN. This study will provide a baseline for interpreting outflows in AGN at higher redshifts, particularly with JWST, and increase the legacy value of the archival STIS spectra by providing matching [O III] images for future NLR studies.The observations for this program consist of WFC3 UVIS imaging of 13 Seyfert AGN.
The goal is to obtain continuum-subtracted [O III] 5007A emission-line images of each AGN.
Abbreviated Summary from Phase I Proposal:
At the low redshifts of our targets (z < 0.02), WFC3/UVIS and its filters provide the best sensitivities for deep [O III] imaging at the high spatial resolution that is essential for meeting our science goals. For ten of our targets we select the FQ508N filter that is centered on the [O III] 5007 emission line at low redshifts. For the remaining targets, NGC 3227 and NGC 6300, we select the F502N filter that is most appropriate for sampling the [O III] 5007 emission line at z < 0.005.
We will also obtain short F547M images for each target in the same orbit as the [O III] images for proper continuum subtraction. The F547M images will also be helpful at small angular scales in combination with deep ground-based continuum images to determine the host galaxies enclosed mass profiles. Mrk 78 and NGC 5283 have small angular sizes and each also requires a deeper, single-orbit F547M image. While ground-based continuum images will be used for the remaining targets, the small angular sizes of these two AGN make accurate bulge-mass profile decomposition impossible even with adaptive-optics imaging.
We split the images into two exposures for the continuum and three exposures for the [O III] images to remove cosmic rays, bad pixels, and improve the image quality by sampling the PSF. While three exposures for the continuum images would allow for further improvement, the increased overheads reduce the resulting S/N in the faint regions below acceptable levels for determining precise ionized gas masses and would require an additional orbit per target due to buffer dump limitations. Thus we opt for two F547M exposures, which is sufficient to correct for cosmic rays with exposure times of < 1000s (Dahlen+ 2010). Finally, we will post-flash the images to obtain the desired 20e- per pixel background (Biretta+ 2013) in order to mitigate charge transfer efficiency losses.
The observations consist of WFC3 UVIS imaging of 13 Seyfert AGN, each using one of four visit setups:
Visit Setup #1 - (9 Targets: UGC 01395, NGC 788, NGC 1358, NGC 1667, IC 3639, NGC 5135, NGC 5427, NGC 5695, NGC 7682)
These AGN will be observed for 1 orbit each using the FQ508N and F547M filters for [O III] and continuum images, respectively.
The visit has two F547M and three FQ508N exposures using two and three point dither patterns with three times the default spacing.
The F547M exposures are 350s in duration, with the FQ508N exposures filling the orbit, typically each ~ 460-510s.
Visit Setup #2 - (1 Target: NGC 5283)
This AGN will be observed over 2 orbits using the FQ508N and F547M filters for [O III] and continuum images, respectively.
The first orbit consists of three F547M exposures filling the orbit using a WFC3-UVIS-DITHER-LINE-3PT pattern.
The second orbit consits of three FQ508N exposures filling the orbit using a WFC3-UVIS-DITHER-LINE-3PT pattern.
The F547M and FQ508N exposures are ~ 940s in duration, filling two orbits, with three times the default point spacing.
Visit Setup #3 - (1 Target: MRK 78)
This AGN will be observed for 1 orbit using the F547M filter for continuum imaging and there is archival FOC [O III] imaging.
The visit has three exposures using a WFC3-UVIS-DITHER-LINE-3PT pattern with three times the default point spacing.
The F547M exposures are ~ 940s in duration, fully filling the orbit.
Visit Setup #4 - (2 Targets: NGC 3227, NGC 6300)
These AGN will be observed for 1 orbit each using the F502N and F547M filters for [O III] and continuum images, respectively.
The visit has two F547M and three FQ508N exposures using WFC3-UVIS-GAP-LINE patterns to encompass these low-redshift, extended objects.
For NGC 3227, a short ~ 20s F547M exposure is included to account for saturation near the bright Type I AGN nucleus.
The F547M exposures are 350s in duration, with the FQ508N exposures filling the orbit, typically each ~ 440-580s.
Requested Statement on the Impact of Reduced Gyro Operations: None of the observations in this program have orientation requirements and should be schedulable in 2 or even 1 gyro-modes. If required, the exposure times could be reduced by tens of seconds with a negligible impact on the signal-to-noise of the images if additional time is required for guide star acquisition and related orbital maneuvers.Mitchell Revalski refined the techniques for spatially-resolved mass outflows with HST for publications on two other AGN (Mrk 34 and Mrk 573) as part of his dissertation, and will apply these techniques to the larger sample. D. Michael Crenshaw developed the original technique for determining spatially-resolved mass outflow rates with HST observations of NGC 4151. Henrique Schmitt is an expert at HST imaging and analysis and will process and analyze the [O III] and continuum images. Travis Fischer will provide experience with STIS spectral fitting and analysis. Steven Kraemer will provide expertise on photoionization modeling and interpretation of the results. Marc Rafelski is an expert at HST imaging and analysis, including the use of custom WFC3/UVIS calibrations, having led the effort for their development. Beena Meena is a graduate student that will be in charge of the observations, data reduction, and analysis of complementary long-slit spectra with the Apache Point Observatory 3.5-meter telescope, which will be used to trace the rotation curves into the host galaxies. Garrett Polack will assist in the reduction and analysis of the existing APO and STIS spectra as part of an undergraduate research project.Supermassive Black Holes and Active Galaxies6falsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYSEYFERTThis object was generated by the targetselector and retrieved from the NED database.J2000J2000GALAXYSEYFERTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSEYFERTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSEYFERTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSEYFERTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSEYFERTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSEYFERTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSEYFERTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSEYFERTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSEYFERTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSEYFERTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSEYFERTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSEYFERTThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISImagingNoNoFQ508NWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoFQ508NWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoFQ508NWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoFQ508NWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF502NWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoFQ508NWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoFQ508NWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoFQ508NWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoFQ508NWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoFQ508NWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoF502NWFC3/UVISImagingNoNoF547MWFC3/UVISImagingNoNoFQ508NWFC3/UVISImagingNoNoF547MPOS-TARGDITHER0.435The specified point spacing is three times the default value of 0.145LINEfalsefalse246.84WFC3-UVIS-DITHER-LINE1falsePOS-TARGDITHER0.405The specified point spacing is three times the default value of 0.135LINEfalsefalse346.84WFC3-UVIS-DITHER-LINE-3PT2falsePOS-TARGDITHERDITHER42.414The specified point spacing is the default value of 2.414WFC3-UVIS-DITHER-BOXfalse81.785false0.1120.173285.759POS-TARGWFC3-UVIS-GAP-LINE23.8843falsePOS-TARGDITHERDITHER42.414The specified point spacing is the default value of 2.414WFC3-UVIS-DITHER-BOXfalse81.785false0.1120.173385.759POS-TARGWFC3-UVIS-GAP-LINE23.8844falseThe scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.(Tic-Visit
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