0 Assigned ID: 4340 ----- Attempting Submission 1 (Wed May 24 14:22:05 GMT 2023) ----- HST Phase I Proposal 4340 successfully submitted. Receipt: # 4340-1 ----- Attempting Submission 2 (Wed May 24 21:04:32 GMT 2023) ----- HST Phase I Proposal 4340 successfully submitted. Receipt: # 4340-2 Updates the CCD exposures (G430L and G750L) to use 52x0.2E1 slit -1567632609 ----- Attempting Submission 1 (Wed Sep 13 20:55:13 GMT 2023) ----- HST Phase II Proposal 17523 successfully submitted. Receipt: # 17523-1 ----- Attempting Submission 2 (Thu Nov 09 15:32:57 GMT 2023) ----- In the last decade, significant progress in understanding the sizescale and structure of the inner regions of Active Galactic Nuclei has been brought about by high cadence continuum reverberation mapping campaigns. Measuring time lags between light curves at different wavelengths probes sizescales not possible through imaging. Results from these campaigns are now seriously challenging the scenario where X-rays drive variability in a standard optically thick, geometrically thin accretion disk at UV/optical wavelengths. Observational evidence suggests the presence of significant continuum emission from the broad line region (BLR). An 8-month multiwavelength continuum reverberation mapping campaign of the nearby bright Seyfert 1 NGC 7469 is on-going, utilizing NICER, Swift and ground-based monitoring. The UV and optical filter bands used for photometric monitoring include significant contamination by reprocessed emission from the broad-line region, including broad emission lines, Balmer continuum, and Fe II emission. To properly interpret the measured photometric lags therefore requires a careful assessment of the strength of each of these spectral components through the UV and optical. This can only be achieved with HST/STIS spectra covering from 1150 - 10000 Angstrom. Here we will obtain a simultaneous UV/optical spectrum of the AGN NGC 7469. These data are taken to support on-going multiwavelength monitoring of this source with NICER, Swift and ground-based data. That campaign is taking place from began in 2023 May 10 and will continue until 2024 Jan 12. As described in the Phase I proposal, we request that the HST observations take place before 2024 Jan 12. To maximize scheduling flexibility, we do not require any specific orientation or slit position angle. However, since this AGN is highly variable on timescales of days to weeks, it is critically important that the entire program be carried out in a single visit, so that we can obtain an accurate overall spectral shape for the AGN. The scientific goal of these observations is to determine the contribution of broad emission lines, Balmer continuum and Fe II emission to the various broadband filters used in the Swift and ground-based photometric monitoring. To achieve this a contemporaneous broadband spectrum will be obtained with HST using STIS and the G140L, G230L, G430L and G750L gratings. Two orbits have been approved in Phase I, and we will use the first orbit for target acquisition and the G140L exposures. The second orbit will be used for G230L, G430L and G750L. The AGN nucleus is very compact, and thus we will use the ACQTYPE=POINT for the STIS acquisition. We will use the 0.2 arcsec slit width for all spectroscopic exposures. For the CCD exposures, the E1 aperture position will be used to minimize CTE losses. With each grating, we will obtain dithered exposures using the STIS-ALONG-SLIT pattern to remove the effect of bad pixels and cosmic-ray hits in the CCD data and to maximize S/N in the MAMA data following Section 12.5.1 of the STIS Instrument Handbook. We will use the STIS/MAMA in ACCUM mode to maximize the on source integration time, and since the variability timescales are such that we do not expect any detectable variability during a single exposure. The total CCD exposure is less than 30 minutes (including overheads) and thus it is allowable to have both STIS MAMA and CCD exposures in the same orbit. We will use GAIN=4 for the CCD exposures to ensure that the peaks of the Halpha and [OIII] lines are well below the saturation level, based on STIS ETC calculations and a standard type I quasar spectrum. For G750L we will obtain fringe flats at the end of the orbit. Following Table 11.1 of the STIS Instrument Handbook, the 52X0.1 slit will be used for the G750L fringe flats. We choose not to use the 52X0.2E2 aperture position for the G750L observation of the AGN because this will negatively impact the throughput and measurement of the spectral shape when combined with the other grating settings. Edward Cackett (PI): Expert in reverberation mapping. Led HST/STIS reverberation campaign on the AGN NGC 4593. PI of Zowada Observatory monitoring of NGC 7469. Aaron Barth: Expert in reverberation mapping, with significant experience with HST/STIS spectral analysis of AGN. Rick Edelson: PI of the Swift NGC 7469 campaign. Mike Goad: Leader in photoionization modeling of the BLR and the BLR diffuse continuum. Juan Hernandez Santisteban: PI of the Las Cumbres Observatory monitoring of NGC 7469. Keith Horne: Expert in reverberation mapping. Kirk Korista: Leader in photoionization modeling of the BLR and the BLR diffuse continuum. Ethan Partington: PI of the NICER campaign monitoring NGC 7469 for 8 months. Supermassive Black Holes and Active Galaxies 6 false false false false false false false false SUPPORTED GALAXY ACCRETION DISK BLR SEYFERT This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 4E-14 erg/cm^2/s/A at 1500A from archival HST/FOS observations 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 POS-TARG DITHER 0.2 LINE false false 4 90.0 STIS-ALONG-SLIT 2 false POS-TARG DITHER 0.2 LINE false false 3 90.0 STIS-ALONG-SLIT 3 false 1704837409175 /System/Volumes/Data/solaris/user1/wskipper/OP-cache/17523-v01.xml The scheduling data was generated by CASM 32.1. CASM was run in Phase II mode. 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