GO: Calibrating the Black-Hole Mass Scaling Relations using Reverberation-Mapped Active Galaxies with Velocity-Resolved Measurements

0 Assigned ID: 3089 ----- Attempting Submission 1 (Fri Mar 25 00:27:07 GMT 2022) ----- HST Phase I Proposal 3089 successfully submitted. Receipt: # 3089-1 ----- Attempting Submission 2 (Fri Mar 25 22:35:16 GMT 2022) ----- HST Phase I Proposal 3089 successfully submitted. Receipt: # 3089-2 ----- Attempting Submission 3 (Fri Mar 25 23:38:49 GMT 2022) ----- 0 ----- Attempting Submission 1 (Sun Jul 10 17:37:10 GMT 2022) ----- HST Phase II Proposal 17103 successfully submitted. Receipt: # 17103-1 ----- Attempting Submission 2 (Mon Jul 11 10:02:32 GMT 2022) ----- HST Phase II Proposal 17103 successfully submitted. Receipt: # 17103-2 ----- Attempting Submission 3 (Mon Jul 11 12:51:06 GMT 2022) ----- HST Phase II Proposal 17103 successfully submitted. Receipt: # 17103-3 ----- Attempting Submission 4 (Fri Jul 15 14:29:56 GMT 2022) ----- ----- Attempting Submission 5 (Wed Oct 19 21:44:53 GMT 2022) ----- GO: Calibrating the Black-Hole Mass Scaling Relations using Reverberation-Mapped Active Galaxies with Velocity-Resolved Measurements Reverberation mapping (RM) determines the mass of black holes (MBH) in active galactic nuclei (AGNs) by resolving the BH gravitational sphere of influence "in time". The resulting relationship between broad-line region (BLR) radius and AGN luminosity (the "R-L relation") is the foundation of virtually all MBH measurements beyond the local universe. Recent RM campaigns with high-quality data (cadence and S/N) yielded velocity-resolved time lags and independent BH masses for a sample of 29 objects, spanning a wide range of AGN luminosities and BH masses (6.4<log MBH/Msun<9.1). Integral-field spectroscopy was obtained with state-of-the-art instruments (Keck/KCWI and VLT/MUSE) for 11 objects for a robust measurement of stellar-velocity dispersion. HST images are essential to: (i) separate the nuclear luminosity from that of the host and thus calibrate the R-L relation over a wide mass range; (ii) determine the correlations between MBH and host-galaxy properties, such as bulge and host-galaxy luminosities, bulge effective-radii, and morphology (frequency of pseudo-bulges, bars, and mergers). Archival HST images are available for 18 objects (see our AR proposal ID 3094), we propose here for the remaining 11. This sample has the most accurate MBH measurements beyond the local universe and will provide a fundamental local benchmark for studies of the evolution of massive black holes and their host galaxies across cosmic time. Measuring the distribution and scatter of f factors and looking for other dependencies to go beyond the sample-average f factor will help to better constrain the single-epoch BH mass. 11 objects will be observed with WFC3/UVIS in F814W to maximize the contrast between AGN and host, avoiding strong AGN emission lines, while taking full advantage of the high resolution of UVIS. The ETC indicates saturation for the brightest objects after 10-70s. To obtain the dynamic range needed for an accurate decomposition of the host galaxy and the AGN, the long exposures will be complemented by short, unsaturated ones. A two-point dither pattern with semi-integer pixel offsets will be used which allow to reject cosmic rays and hot pixels and increase the sampling of the PSF and to bridge the gap between the WFC3 UVIS detectors. To allow for individual flash settings, we will use Pos Targ for dithering rather than the default dither pattern (WFC3-UVIS-GAP-LINE). One short (10 sec) and two long exposures (~500-600 sec depending on orbital visibility) at both dither locations will be taken. The short exposure will be taken with Blade=A. A sequence of "short-long-long-dither-long-long-short" will result in minimal additional overhead as the buffer can be dumped during the long exposure or at the end of the orbit. Our program does not have any orient restrictions. All objects will be observed with one orbit each. All visits have multiple scheduling opportunities during cycle 30. Thus, we expect any impact of potentially going to reduced-gyro mode to be minimal. The team has significant expertise in the structural analysis of AGN host galaxies, and galaxies in general, in particular using HST images. Members of the team have led several HST observing campaigns and published multiple papers. Dr. Vardha N. Bennert was the PI of a recently completed (and published) HST SNAP program observing local AGNs with single-epoch MBH estimations. She has also been leading the analysis of Keck/KCWI spectra that complement the HST images proposed here. Dr. Aaron Barth is the PI of one of the reverberation-mapping project that forms the basis of this proposal, the so-called Lick AGN Monitoring Project 2016 (LAMP2016). Dr. Barth is also the PI of an ongoing HST ACS imaging campaign of a large sample of local AGNs. Dr. Vivian U led the analysis of the published LAMP2016 data. The dynamical modeling is carried out by Dr. Tommaso Treu and his graduate student Lizvette Villafana. Dr. Simon Birrer is the developer of the Lenstronomy code that will be used for the detailed host-galaxy analysis. Dr. Xuheng Ding has recently applied Lenstronomy to a sample of high-redshift broad-line AGNs to study the evolution of the BH mass-host-galaxy scaling relations. With Birrer's and Ding's help, Bennert has applied Lenstronomy to the sample of local broad-line AGNs obtained in her recent HST SNAP program. Nico Winkel is a graduate student and expert on IFU spectroscopic observations complementary to this HST proposal. Dr. Knud Jahnke is an expert on quasar host galaxy morphologies and image decomposition, and has PI'd several HST programs. He has been studying the co-evolution of BHs and host galaxies since 1996. Bennert, Malkan, and Treu have been studying the co-evolution of BHs and spheroids since 2004, developing many of the techniques that enable this work. Barth, Bennert, Malkan and Treu have been measuring BH masses through reverberation mapping for many years, including several successful Lick observing campaigns. Our LAMP team has established itself as one of the leading groups through both datasets of high S/N and cadence as well as new analysis strategies. Barth, Treu and Malkan provide the team with excellent access to Keck telescope time. The team is in a superb position to accomplish the goals stated in this proposal. Graduate student Raymond Remigio (UC Irvine) will be working on the Keck/KCWI ground-based data under supervision of Dr. U. Supermassive Black Holes and Active Galaxies 6 false false false false false false false false AVAILABLE GALAXY SEYFERT YES J2000 J2000 z=0.026; log MBH/Msun = 7.25 GALAXY SEYFERT YES J2000 J2000 z=0.0573; log MBH/Msun = 8.0 GALAXY SEYFERT YES J2000 J2000 z=0.0417; log MBH/Msun=7.5 GALAXY SEYFERT YES J2000 J2000 z=0.034; log MBH/Msun = 6.94 GALAXY SEYFERT YES J2000 J2000 z=0.0418; log MBH/Msun=7.40 GALAXY SEYFERT YES J2000 J2000 z=0.0305 , log MBH/Msun = 7.58 GALAXY SEYFERT YES J2000 J2000 z=0.0364; log MBH/Msun=7.67 GALAXY SEYFERT YES J2000 J2000 z=0.0361; log MBH/Msun=7.80 GALAXY SEYFERT YES J2000 J2000 z=0.062, log MBH/Msun =7.36 GALAXY SEYFERT YES J2000 J2000 z=0.070; log MBH/Msun=7.46 GALAXY SEYFERT YES J2000 J2000 z=0.066; log MBH/Msun =7.15 WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F814W 1657380771496 The scheduling data was generated by CASM 30.3. 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