0 Assigned ID: 3809 ----- Attempting Submission 1 (Tue Sep 27 15:32:02 GMT 2022) ----- Comments for Submission 5: 1. Replaced Visit 07 with a new target (SDSSJ1625), since the old target (J0927) has recently been found to be unlikely a dual/lensed quasar. 2. Replaced Visit 03 with a new target (SDSSJ1608), since the old target (J0812) has recently been found a star/quasar superposition. --------------------------------- Comments for Submission 4: 1. Changed WFC3 dither spacing from integer to non-integer values for better PFS sampling. --------------------------------- Comments for Submission 3: 1. Visit 08 (with the replacement in Submission 2) has no guide stars (for STIS) even when schedulability is set to 100, and so has to be replaced by another new target (J0911). --------------------------------- Comments for Submission 2: 1. Visits 08 and 10 have no guide stars (for STIS) even when schedulability is set to 100, and so have to be replaced by new targets (J0032 and J1015). --------------------------------- Comments for Submission 1 1. Target SDSSJ0812-0040 is removed because it was recently discovered to be a star-quasar superposition after the proposal was submitted. Its allocated two orbits are replaced by Visits 11 and 12 for two newly discovered targets (after proposal submission; SDSSJ1059 and SDSSJ1118), which have scheduled WFC3 IR imaging, but still need STIS spectroscopy to achieve the science goals. Please advise if TTRB is needed. 2. Target SDSS0938+4216 has a duplicate WFC3 IR F160W image (recently scheduled after the proposal submission), and so one of its two allocated orbits is replaced by Visit 13 for a newly discovered target (SDSSJ1225) which has existing slit spectroscopy but still needs WFC3 IR F160W imaging to achieve the science goals. Please advise if TTRB is needed. -259971449 ----- Attempting Submission 1 (Tue Dec 13 00:47:14 GMT 2022) ----- ----- Attempting Submission 2 (Tue Dec 13 19:30:02 GMT 2022) ----- ----- Attempting Submission 3 (Tue Dec 13 21:34:16 GMT 2022) ----- ----- Attempting Submission 4 (Fri Dec 16 00:19:19 GMT 2022) ----- ----- Attempting Submission 6 (Fri Mar 17 16:16:28 GMT 2023) ----- The visit planner is running super slow from my end and almost stalling... If you could help run it locally would be really appreciated. Discovering Close Dual and Lensed SMBHs at Cosmic Noon STIS G430L slit spectroscopy and WFC3 F160W imaging are proposed to unambiguously confirm close (<5 kpc) dual and strong gravitationally lensed quasars at 1<z<3. The sample probes a new regime at higher redshifts, higher luminosities, and smaller separations than previous work. This poorly explored regime is crucial for understanding the impact of mergers in triggering SMBH accretion at Cosmic Noon, i.e., the peak quasar epoch. The targets are selected from Gaia using two new techniques. Targets have been carefully chosen to minimize interlopers from star-quasar superpositions. Ground-based follow-up AO-assisted NIR imaging has uncovered ~0.3"-0.7" double cores in each target, suggesting dual or lensed quasars, but the existing data are insufficient for determining their physical origins. The proposed new observations will unambiguously establish the targets as 1<z<3 sub-arcsecond dual or lensed quasars. STIS will detect spatially resolved spectra from each nucleus and measure SMBH and accretion properties (mass, mass ratio, and Eddington ratio) to put them into their cosmological context. WFC3 imaging will detect the much fainter extended host galaxy mergers against the bright quasars and possibly low surface brightness tidal features indicative of ongoing mergers in dual quasars, or foreground lenses in lensed quasars. The results will elucidate the unknown 1<z<3 sub-arcsec dual/lensed quasar population statistics. It will provide empirical constraints on the merger rate of 1<z<3 SMBHs and inform the prospects of binary SMBHs as targets for multi-messenger astronomy. Alternatively, discovery of small-scale lensed quasars would be equally interesting in its own right. This program will conduct WFC3/IR F160W imaging (for 7 targets) and STIS/G430L slit spectroscopy (for 8 targets) for a total sample of 11 candidate kpc-scale dual/lensed quasars at z~1--3. The targets have close double cores with separations of ~0.3"--0.7". The targets are a subset of a complete sample of high-fidelity double quasars at z>1 selected using two new techniques that have been developed recently (i.e., "varstrometry" and Gaia Multi Peak). Deep HST IR F160W imaging will detect the extended host galaxy mergers and low-surface-brightness tidal features (indicative of ongoing mergers) or foreground lenses to umambiguously distinguish between dual and lensed quasars. STIS slit spectroscopy will detect spatially resolved spectra simultaneously covering both nuclei. In dual quasars, the unresolved quasars will be carefully modeled (by PSFs) and subtracted in order to robustly reveal the (much fainter) extended host galaxies underlying each quasar. Furthermore, after carefully subtracting both the quasars (PSFs) and the host galaxies (using Sersic models), we may discover low surface brightntess tidal features as direct evidence for mergers. Alternatively, in lensed quasars, the unresolved lensed quasar images will be carefully modeled (using PSFs) and subtracted in order to either detect or put stringnet upper limits on the foreground lens galaxy. Using the structure decomposition constraints (on both the lensed images and the lens), we will perform strong lensing mass modeling tests in order to quantitatively assess the strong gravitational lensing scenario. The results will reveal bona-fide high-redshift kpc-scale dual quasars that are still largely illusive (but are predicted to be abundant by theory). For the WFC3 IR F160W imaging, we adopt the 256x256 subarray (30"x30" FOV, corresponding to ~250kpcx250kpc at z=2, more than enough to cover the double quasars and host galaxies). We adopt SPARS10 (NSAMP=15) to increase the dynamic range and account for potential saturation of bright cores, and the 4-step BOX dither (similar to the default WFC3-IR-DITHER-BOX-MIN but with increased spacing to meet the >10 pixel requirement to avoid persistence effects) for cosmic-ray and bad-pixel rejection, to better sample the PSF for optimal effective resolution. Since our primary goal is to detect the lens galaxy (or the lack thereof) rather than to accurately measure host galaxy morphology, this dither pattern is sufficient - nor do we require a dedicated PSF observation; we will use field stars and/or recent archival data to build an empirical PSF template. The IR depth assuming 412s on-source exposure is H~24 AB mag arcsec^-2 (3\sigma), sufficient to detect double cores and rule out lensing. For the STIS slit spectroscopy, we use the 52x0.2" slit and the G430L aperture. The slit will be placed across both cores to obtain the spectrum for both components. The separation between the two cores is ~0.3"--0.7", and we will use the point-source mode for acquisition. The conversion between the PA of the two cores and the ORIENT parameter is: ORIENT=PA+45.35 or ORIENT=PA+225.35 according to Table 11.2 of the STIS Instrument Handbook. Dr. Liu has expertise in HST data reduction for STIS, the prime instrument used in the proposed observations. She is an expert in dual AGN and has more than a dozen papers published in the past decade on the general topic of merging supermassive black holes; she has led four past HST observing programs with five papers published based on the HST observations. Dr. Gross has expertiese in multi-wavelength studies of dual AGN. He will be leading most of the proposed analysis. Dr. Shen is an expert in quasars and supermassive black holes; he has led six past HST observing programs and has extensive experiences in the analysis of quasar spectra that will be required to analyze and interpret the data. Mr. Chen's PhD thesis focuses on the study of binary and dual AGN under the guidance of Dr. Liu. Dr. Zakamska is an expert in quasars; she has led multiple past HST programs and has extensive experiences in the analysis of both quasar host galaxies and quasar spectra. Dr. Hwang has expertiese in Gaia astrometry and is the PI of the HST/WFC3 optical double-band imaging program that discovered some of the proposed targets. Supermassive Black Holes and Active Galaxies 3 false true false false false true false false SUPPORTED GALAXY QUASAR J2000 J2000 G=20.31, r=20.20, z=19.3 GALAXY QUASAR J2000 J2000 G=19.11, r = 19.43, z = 19.37 GALAXY QUASAR J2000 J2000 G=19.29 GALAXY QUASAR J2000 J2000 G=15.85, r = 15.73, z = 15.40 GALAXY QUASAR Replacement target for Visit 08 (both the original target J0938 and the first replacement J0032 have no guide stars available for STIS). J2000 J2000 r = 18.98, z = 18.71 GALAXY QUASAR J2000 J2000 r = 16.93, z = 16.26 GALAXY QUASAR Replacement target recently discovered after the proposal was submitted. It has WFC3 IR imaging scheduled, but lacks slit spectroscopy so STIS will be needed to achieve the science goals. J2000 J2000 r = 17.36, z=16.87 GALAXY QUASAR Replacement target recently discovered after the proposal was submitted. It has WFC3 IR imaging scheduled, but lacks slit spectroscopy so STIS will be needed to achieve the science goals. J2000 r = 18.75, z = 18.44 GALAXY QUASAR This is a new target (discovered after the proposal was submitted) to replace the WFC3 IR imaging for SDSSJ0938+4216 (which has a new duplicate WFC3 IR imaging most recently scheduled after the proposal submission). It already has spatially resolved spectroscopy (private communications), so no new STIS spectroscopy is needed, but deep IR imaging is still needed to achieve the science goals. J2000 z = 17.52 GALAXY QUASAR J2000 J2000 r = 18.98, z = 18.53 GALAXY QUASAR Replacement target for Visit 10 (the original target J0950 has no guide star available for STIS). J2000 r = 17.56, z = 17.40 GALAXY QUASAR NO Replacement target for Visit 07 J2000 r = 18.68 GALAXY QUASAR NO Replacement target for Visit 03 J2000 r = 19.50, z = 18.93 STIS/CCD Spectroscopic No No G430L 4300 WFC3/IR Imaging No No F160W STIS/CCD Spectroscopic No No G430L 4300 WFC3/IR Imaging No No F160W STIS/CCD Spectroscopic No No G430L 4300 WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F160W STIS/CCD Spectroscopic No No G430L 4300 WFC3/IR Imaging No No F160W STIS/CCD Spectroscopic No No G430L 4300 WFC3/IR Imaging No No F160W STIS/CCD Spectroscopic No No G430L 4300 WFC3/IR Imaging No No F160W STIS/CCD Spectroscopic No No G430L 4300 WFC3/IR Imaging No No F160W POS-TARG DITHER 1.365 increased dither spacing by 2.5x to avoid persistence effects LINE 0.975 false false 74.653 4 18.528 WFC3-IR-DITHER-BOX-MIN 1 false POS-TARG DITHER 1.0 LINE false false 2 90.0 STIS-ALONG-SLIT 2 false 1679667868000 102.10000000000002 (Tic-Visit :proposal-id 17287 :visit-id "01" :proposal-version -1 :trans-version "20220630" :date "16-Mar-2023 21:20:01.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 384032 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17287 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17287 :visit-id "01" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2566 :al-overhead-at-end 0 :internal-dur-at-end 436 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3200 :pcs-gap 0 ) true 1 0 The scheduling data was generated by CASM 31.0. 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