0Assigned ID: 786
----- Attempting Submission 1 (Fri Mar 06 21:12:00 GMT 2020) -----
HST Phase I Proposal 786 successfully submitted.
Receipt: # 786-1
----- Attempting Submission 2 (Fri Mar 06 21:13:50 GMT 2020) -----
HST Phase I Proposal 786 successfully submitted.
Receipt: # 786-2
----- Attempting Submission 3 (Fri Mar 06 23:28:27 GMT 2020) -----The orientation parameter was computed using the offset values in Table 11.2 of the STIS Instrument Handbook.
Since the main purpose of the program is to spatially resolve the two cores, it is important that these offset
values are up to date. In additon, the two point-like cores are separated by 0.3-0.6 arcsec, and we have used the
point-source acq mode.
[v3] In this version we have changed the schedulability parameter to 100, wihch fixed the 5 previous visits that were
unschedulable, at the expense of reduced exposure time by 10-20%. This reduction in exposure time is acceptable
for our science.
[v4] In this version we have cleared the 'ON HOLD' parameter for all visits.
[v5] We have swapped two targets (#8 and #12) after being approved the swap request. We have recently found that the two old
targets are interlopers (i.e., star-quasar superpositions) based on our newly obtained spectra from Gemini. Replacing them with
new targets will help us improve the success rate of the program. To replace the two old targets, we have selected two new ones
based on the same criteria. These new targets were not included in the original proposal target list, because they were later
discovered (i.e., after the C28 deadline) to have double cores using new observations obtained from our ongoing HST/SNAP
imaging program (GO-15900). The two old targets to be replaced are (with the names representing the J2000 coordinates):
J131416.02-491218.2 and J185728.66+704811.4. The two new ones are: J053620.23+503826.2 are J074800.55+314648.0.
[v6]: We have added dithering (2 point along the slit with an offset of 1 arcsec) to help reject hot pixels.
We have also adopted the E1 aperture (located near row 900 of the CCD) to mitigate the down-stream CTE effects of cosmic rays and hot pixels.-1293100419----- Attempting Submission 1 (Mon Jun 22 15:35:03 GMT 2020) -----
----- Attempting Submission 2 (Sun Aug 23 01:57:59 GMT 2020) -----
HST Phase II Proposal 16210 successfully submitted.
Receipt: # 16210-2
----- Attempting Submission 3 (Tue Aug 25 14:13:22 GMT 2020) -----
----- Attempting Submission 4 (Mon Mar 29 16:40:45 GMT 2021) -----
----- Attempting Submission 5 (Wed Apr 14 17:26:13 GMT 2021) -----Spectroscopic Confirmation of High-Redshift Close Dual/Lensed Quasars from Gaia and HSTDual quasars are expected to be common in the hierarchical structure formation paradigm. Despite their significance, no confirmed dual quasar is known with <10 kpc separations at 1<z<3, in stark contrast to theoretical expectations. We propose STIS (G750L) slit spectroscopy for 14 double-core quasars to systematically discover close dual or lensed SMBHs at redshifts 1<z<3 for the first time. Our sample probes a new regime at higher redshifts and smaller merger separations than previous work - crucial for understanding the significance of mergers in triggering quasar activity in the cosmic "high noon". Our targets are selected using the new astrometric technique: when two close-by AGN vary stochastically, their combined light centroid shifts, which is detectable by Gaia. Follow-up HST imaging of Gaia-selected targets has uncovered double-cored morphology with nuclear separations of ~0.3"-0.6". The proposed STIS spectra will reject interlopers such as chance superpositions with stars/galaxies to unambiguously confirm the targets as dual or lensed quasars. The results will provide empirical constraints on the merger rate of supermassive black holes and therefore on the stochastic gravitational wave background from binary supermassive black holes.This program will perform STIS (G750L) slit spectroscopy for 14 double-core quasars to spectrally and spatially resolve the two cores.
We will use the 52x0.2" slit and the G750L aperture. The slit will be placed across both cores to obtain the spectrum for both components. The separation between the two cores is typically 0.3-0.6 arcsec, 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.
Each visit consists of 1 orbit, with one acquisition exposure followed by the science exposure, and the CCD flats.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 four papers published based on the HST observations. Dr. Shen is an expert in quasars and supermassive black holes; he has led four past HST observing programs and has extensive experiences in the analysis of quasar spectra that will be required to analyze and interpret the data. Dr. Zakamska is an expert in quasars; she has led multiple past HST programs and has extensive experiences in the analysis of quasar spectra. Mr. Chen's PhD thesis focuses on the study of binary and dual AGN; he works with Dr. Liu. Mr. Hwang is PI of the HST/WFC3 imaging program that discovered the double-core quasars being proposed as the STIS targets; he works with Dr. Zakamska.Supermassive Black Holes and Active Galaxies6falsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYQSOQUASARJ2000J2000GALAXYQSOQUASARJ2000J2000GALAXYQSOQUASARJ2000J2000GALAXYQSOQUASARJ2000J2000GALAXYQSOQUASARJ2000J2000GALAXYQSOQUASARJ2000J2000GALAXYQSOQUASARJ2000J2000GALAXYQSOQUASARJ2000J2000GALAXYQSOQUASARJ2000J2000GALAXYQSOQUASARJ2000J2000GALAXYQSOQUASARJ2000J2000GALAXYQSOQUASARJ2000J2000GALAXYQSOQUASARJ2000J2000GALAXYQSOQUASARJ2000J2000STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750L7751STIS/CCDSpectroscopicNoNoG750L7751POS-TARGDITHER1.0LINEfalsefalse290.0STIS-ALONG-SLIT1falseThe scheduling data was generated by CASM 29.0.CASM was run in Phase II mode.(Tic-Visit
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:visit-id "13"
:orbit-number 1
:pcs-time 393
:si-vis-utilization 3018
:al-overhead-at-end 72
:internal-dur-at-end 620
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3411
:pcs-gap 0
)true10The scheduling data was generated by CASM 29.0.CASM was run in Phase II mode.1627993769000179.14999999999998(Tic-Visit
:proposal-id 16210
:visit-id "14"
:proposal-version -1
:trans-version "20200619"
:date "14-Apr-2021 12:21:41.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 129232
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16210
:visit-id "14"
:obset-id "14"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16210
:visit-id "14"
:orbit-number 1
:pcs-time 393
:si-vis-utilization 2524
:al-overhead-at-end 0
:internal-dur-at-end 640
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2918
:pcs-gap 0
)true10