0 Assigned ID: 5308 ----- Attempting Submission 1 (Tue Mar 26 02:52:53 GMT 2024) ----- The Exposure Configuration (instrument/detector) doesn't match the Pattern (instrument/detector). ORBIT PLANNER SERVER INTERNAL ERROR ----Submission 3 notes: 1. The individual exposure time for the PSF standard has been increased from 5 s to 7 s to avoid shutter vibrations dominating the PSF (and short enough to avoid saturation). 2. A short F606W exposure (20s) has been added to help model the bright nucleus in case it were saturated. ----Submission 2 notes: 1. The WFC3 UVIS and IR observations are grouped into a single visit of two orbits to reduce initial pointing overheads in the second orbit. 2. The "UVIS2-C1K1C-CTE" aperture is used instead of UVIS2 to place the target closer to the readout of the UVIS2 chip and substantially mitigate CTE losses. -894359850 ----- Attempting Submission 1 (Tue Aug 06 17:27:10 GMT 2024) ----- ----- Attempting Submission 2 (Mon Oct 28 15:23:35 GMT 2024) ----- ----- Attempting Submission 3 (Tue Oct 29 18:40:44 GMT 2024) ----- 1. the short UVIS exposure has been added at the end of the IR orbit to help model the bright nucleus in case it were saturated. 2. orbit planner error for unknown reason, even though the planner did run through. SDSS J1000+2233 is a broad-line quasar at z~0.4 with the peaks of its broad low-ionization lines blueshifted from the systemic velocity by ~8000 km/s, without obvious double-peaked broad line profiles characteristic of disk emitters. It represents one of the few best cases where a recoiling SMBH or a sub-parsec binary SMBH could be a viable interpretation of the blueshifted broad lines. We propose joint HST and Chandra observations to elucidate the nature of SDSS J1000+2233. HST WFC3 optical and IR imaging will potentially resolve spatically-offset nuclei supporting the scenario of a recoiling SMBH, and allow image decomposition to measure the properties of its host galaxy. HST STIS NUV spectroscopy will probe the broad UV emission line profiles to rule out (or confirm) the disk emitter scenario. Chandra X-ray imaging will pinpoint the location of the active SMBH to facilitate the HST imaging observations. The rejection or confirmation of the disk emitter hypothesis would provide valuable guidance for the searches of recoiling or binary SMBHs with kinematically-offset broad emission lines. Alternatively, detailed multi-wavelength coverage and host galaxy measurements will help understand the physical conditions leading to extreme broad line profiles that are rare even for disk emitters. The observations will have general implications for gravitational wave and multi-messenger astronomy, the understanding of galaxy evolution and SMBH formation, and/or astrophysical objects under extreme physical conditions. With a small investment of 6 HST hours and 25 ks of Chandra, the program could potentially confirm the general relativistic prediction of recoils from SMBH mergers. Overview: 1. We will use HST WFC3 to perform optical and near-IR imaging to potentially resolve close double nuclei at the 0.1" resolution, and to perform quasar-host imaging decomposition to derive host properties and stellar mass estimate from two-band color. 2. We will use HST STIS to obtain NUV spectroscopy to cover the UV broad emission lines from Ly to C III] to test the disk emitter scenario, and to facilitate photoionization modeling. More specifically: 1. For the WFC3 imaging, we choose the UVIS channel with the F606W filter to cover the restframe ~4000--5000 Angstrom. This band roughly samples the rest-frame B band for our target and probes the young stellar population in the host. We also choose the IR channel with the F110W (wide J) filter, which roughly samples the rest-frame I band for our target and probes the old stellar population in the host (mostly the bulge). The quasar light is expected to be at a minimum at this wavelength to facilitate quasar-host decomposition. The two-band (UVIS+IR) observations, after proper quasar-host decomposition, provide rest-frame optical color for the host to allow an estimate of the mass-to-light ratio (M/L) and hence the host stellar mass, based on stellar population synthesis models. The choice of these two bands is such that complications with TP-AGB stars on host SED are not an issue for the M/L estimation. For the F110W observation, we will use the subarray to minimize overhead and avoid buffer dump. We will use the 4-step BOX dither between exposures to facilitate cosmic-ray and bad-pixel rejection, to better sample the PSF, and to improve the effective image resolution. For the F606W observations, we will use the full array to cover the largest field of view to include as many field stars as possible to register for absolute astrometry by comparing to deep ground based imaging from the DECal Legacy Survey. To achieve the best PSF possible with HST, desirable for identifying close double nuclei, we will adopt a 4-point dither pattern to over-sample the PSF. We use one orbit each in the WFC3 IR and UVIS bands to accommodate these dither patterns and to reach the depth desirable to detect faint extended host features. There are no field stars in the same field-of-view that are bright enough to use as PSF templates. For robust PSF modeling, we thus use a separate orbit to observe a bright white dwarf in addition to the WFC3 observations of the science target. We will combine the UVIS and IR observations in the same orbit, with the same filter configurations and dither patterns as for our science target. It is important to observe the PSF star in the same cycle to minimize the impact of instrument PSF variations across cycles. 2. NUV spectroscopy is used to explore the UV broad lines to test the disk emitter hypothesis. We choose STIS NUV-MAMA with the G230L grating for the broad spectral coverage from Lya to C III] in one setting. The moderate spectral resolution R~500 is sufficient to resolve the broad UV emission lines and their potential offset of ~8000 km/s. We will orient the 52"x0.2" slit to cover both nuclei should they be discovered from the WFC3 imaging, and therefore request the NUV spectroscopy to be taken at least 17 days (to allow time for analysis and resubmission of the observation and to be non-disruptive) after the WFC3 imaging for us to properly set up the slit position. We use 3 orbits for the NUV spectroscopy taking into account an estimated overhead of 35 min (including initial guide-star acquisition 5.6 min, target acquisition 6.0 min, two additional automatic wavecal for series of identical exposures extending more than 40 min at 4.0 min each, and two guide-star reacquisitions at 3.7 min each, and additional overhead such as CR-split/buffer dump). PI Shen works on a broad range of topics on AGN and SMBHs, and is experienced with spectral analysis of quasars, observational tests of recoiling and binary SMBHs, disk emitters, and the phenomenology and physics of SMBH accretion. Co-I Guo works on AGN science and is experienced with spectral analysis of quasars and photoionization modeling of AGN spectra. Co-I Li works on HST imaging analysis of quasar hosts and is experienced with GALFIT and measurements of host properties from broad-band photometry and spectroscopy. Co-I Eracleous is an expert on AGN and a leading expert on disk emitters, and is experienced with multi-wavelength observations of AGN. Co-PI Liu works on observational searches for sub-parsec binary SMBHs and recoiling SMBHs with various methods including the kinematically-offset broad emission line technique. Supermassive Black Holes and Active Galaxies Galaxies 6 false true true false false false false true PRIMARY 25 0 0 0 0 true SUPPORTED GALAXY QSO J2000 J2000 NUV=19.72, r=18.44, H=15.8 CALIBRATION POINT SPREAD FUNCTION J2000 J2000 J=14.831 WFC3/UVIS Imaging No No F606W WFC3/IR Imaging No No F110W STIS/NUV-MAMA Spectroscopic No No G230L 2376 WFC3/IR Imaging No No F110W WFC3/UVIS Imaging No No F606W POS-TARG DITHER 1.716 LINE 1.095 false false 74.653 4 18.528 WFC3-IR-DITHER-BOX-MIN 1 false POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 2 false POS-TARG DITHER 0.15 LINE false false 2 90.0 STIS-ALONG-SLIT 3 false 1730225939087 Timing link suitability includes constraints ([03 After 01 by 60.0 to 365.0 days]) The scheduling data was generated by CASM 32.1.3. 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CASM was run in Phase II mode. 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