0 Assigned ID: 977 ----- Attempting Submission 1 (Sat Mar 07 00:09:08 GMT 2020) ----- HST Phase I Proposal 977 successfully submitted. Receipt: # 977-1 ----- Attempting Submission 2 (Sat Mar 07 00:53:21 GMT 2020) ----- HST Phase I Proposal 977 successfully submitted. Receipt: # 977-2 FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser 0 ----- Attempting Submission 1 (Tue Jun 30 21:03:06 GMT 2020) ----- HST Phase II Proposal 16291 successfully submitted. Receipt: # 16291-1 ----- Attempting Submission 3 (Wed Jul 15 23:27:45 GMT 2020) ----- ----- Attempting Submission 4 (Fri Jul 17 23:07:35 GMT 2020) ----- ETC states that post-flash is too high, but these values were adopted to meet the new 20 e- per pixel background requirement. Spatially Resolving Outflows in a z~1 Extremely Red Quasar to Observe a Short-Lived Blowout Phase in Galaxy Evolution A key question in galaxy formation is how active galactic nuclei (AGN) interact with their host galaxies. Extremely Red Quasars (ERQs) are ideal objects to study this interaction since they are believed to be quasars caught in a short-lived phase where they are actively clearing gas from their host galaxy's central regions. Most known ERQs are at z=2-3, making it challenging to resolve details of their winds and host galaxies, even with HST. Here we propose to study the lowest redshift ERQ discovered to date (z~0.94) with the aim of directly resolving the high ionization outflow using narrow-band imaging of the [Ne V] line. The narrow band observations will provide a first look at the size and spatial distribution of a powerful quasar outflow during this key phase. The broad band observations will enable measurement of the host galaxy properties including Sersic index, evidence of merging, and recent (100 Myr) star formation. J0048-0046 provides the best possible chance to constrain the ionized gas outflow size of an ERQ, both due to its low redshift and its high level of nuclear obscuration. With the derived outflow size measurements, we can test our theories of galaxy formation and measure whether ERQ winds have enough kinetic power to blow the gas out of their hosts. These observations will also help contribute to building up a sample of ERQ hosts and outflow measurements that can be used to assess how ERQs outflows are driven and how the hosts of these galaxies evolve. We are proposing to measure the morphology and spatial extent of the quasar-driven wind in an Extremely Red Quasar at z=0.94 using WFC3-UVIS narrow-band imaging. We will trace the high ionization gas in the wind using the [Ne V] line at wavelengths of 6500-6630 in the observed frame. Broadband imaging will enable us to continuum subtract and measure the properties of the host galaxy. We are using the narrow F657N filter to isolate the broad [Ne V] line. F657N is well centered on the [Ne V] line and has a bandpass that spans the range of velocites we expect to observe. We conservatively estimate a 3 kpc (R ~ 0.38") outflow yielding a surface brightness of 1.3e-15 erg/s/A/cm^2. A line-dither pattern is used for the rejection of hot pixels and cosmic rays while improving spatial resolution. Unfortunately, both a 3-point and 4-point dither pattern introduces read noise that does not allow us to reach our target S/N. A post-flash of 13 e- is applied based on ETC calculations using the zodiacal background of the target and the most recent recommended background level of 20 e-. We will reach S/N ~ 5 per pixel centered on the brightest region of the outflow in 6 orbits. Broad-band imaging will allow us to correct for the stellar and QSO contiuum in the narrow-band F657N filter and allow us to measure properties of the host galaxy. The F606W filter will observe deep, off-band images with wavelengths close to our narrow-band filter. This will allow us to subtract off the continuum in the on-band images while introducing minimal noise. At radii where we expect the outflow to be present (R < 3 kpc), we will constrain the galaxy/qso continuum with a S/N >8 per pixel. The off-band image will also trace the properties of the host galaxy. A 5x5 pixel binning is appropriate for this diffuse outer-region and we can obtain S/N~3 per spatial bin with 2 orbits. To give us color information of the host galaxy, we use the F814W filter because it provides a better tracer of stellar mass. Since the host galaxy is ~2 times brighter in the F814W filter relative to F606W, we can acheive the same S/N in half the time required for F606W. Archival photometry indicates our target is mildly variable, possibly on time scales of days. As a consequence, we require broadband exposures with F606W for each visit so that the variable continuum can be accounted for when subtracting it from the narrow band. Doing so requires us to take half-orbit exposures in each of the broad bands for visits 1 and 2. A 3-point dither pattern for F606W is the most optimal as it will allow us to remain near our target S/N while also improving cosmic ray rejection and spatial resolution. A 2-point dither pattern for F814W is the safest since going above that many points reduces us to short sub-exposures that may not reach the required background level count of 20 e- per pixel. Due to the low background in our F657N, F606W, and F814W images CTE is a concern. The spatial extent of the outflow is expected to be small (< 10 pixels). We have therefore opted to place the targets close to the readout axis at the UVIS2-C1K1C-CTE position. In the advent of a 2-gyro operational mode, our science will be affected in two ways. Target visibility for this proposal is widely available from late October to mid December of 2020 with 3 gyros. This visibility during the fall is greatly diminished with only 2 gyros operational. Second, all exposures for visits 2 and 3 experience around 1-2 minutes of overrun which would affect our S/N, but not greatly. Our team has the scientific background and expertise to successfully carry out the proposed observations and analysis. We have been investigating outflows in a related population of objects - compact massive starbursts - for well over a decade and most of us are experienced users of HST. PI Christy Tremonti has devoted much of her career to studying star formation driven outflows and their potential to quench thier host galaxies. She has led three HST imaging programs of compact massive starbursts. Dr. Serena Perrortta is one of the leading experts on Extremely Red Quasars. She published a paper on the [O III] outflow properties of ERQs and explored correlations between outflow velocity, color, Eddington ratio, and bolometric luminosity. She led Keck/OSIRIS observations designed to constrain the sizes of [OIII] winds in z=2.5 ERQs. These observations did not resolve the wind, motivating the current proposal. Dr. Paul Sell and Aleks Diamond-Stanic are experts on deriving galaxy structural parameters from HST data (Diamond-Stanic et al. 2012, Sell et al. 2014). They will play a leading role in the host galaxy analysis. Dr. John Moustakas is an expert on SED fitting. His knowledge and tools will be invaluable in constraining the host galaxy stellar mass and SFR from our 2-band HST imaging. Dr. Gregory Mosby is an expert on stellar population analysis of quasar host galaxies. Dr. Alison Coil has been studying galaxy and AGN formation and evolution from large surveys, and will help us place our results in the context of other AGN populations. Dr. Jim Geach has expertise studying AGN winds with radio/sub-mm data and will be involved proposals to follow-up this target with ALMA. Dr. David Rupke is an expert on studying starburst and AGN-driven galactic winds at low redshift. Dr. Ryan Hickox is an expert on multiwavelength AGN observations and in the star formation-AGN connection. Cameren Swiggum: Undergraduate student at University of Wisconsin - Madison. He has been studying this source for nearly two years and is the first author on a paper in preparation regarding this unusual quasar. Supermassive Black Holes and Active Galaxies 6 false false false false false false false SUPPORTED GALAXY QUASAR YES J2000 J2000 WFC3/UVIS Imaging No No F657N WFC3/UVIS Imaging No No F606W WFC3/UVIS Imaging No No F814W POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 1 false POS-TARG DITHER 0.145 LINE false false 2 46.84 WFC3-UVIS-DITHER-LINE 2 false POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 3 false /private/var/folders/58/m3km1yk15rgcq0hfq011tfk80002ks/T/OPVisit9600364703156348975.xml The scheduling data was generated by CASM 29.0. CASM was run in Phase II mode. 1612410690000 70.775319349086 (Tic-Visit :proposal-id 16291 :visit-id "01" :proposal-version -1 :trans-version "20200619" :date "22-Jun-2021 10:21:47.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 2309968 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16291 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16291 :visit-id "01" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2756 :al-overhead-at-end 116 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16291 :visit-id "01" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2749 :al-overhead-at-end 125 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16291 :visit-id "01" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2749 :al-overhead-at-end 125 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 3 0 /private/var/folders/58/m3km1yk15rgcq0hfq011tfk80002ks/T/OPVisit6383912359740356936.xml The scheduling data was generated by CASM 29.0. CASM was run in Phase II mode. 1612496473000 70.918621578254 (Tic-Visit :proposal-id 16291 :visit-id "02" :proposal-version -1 :trans-version "20200619" :date "22-Jun-2021 10:21:48.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 2598720 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16291 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16291 :visit-id "02" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2758 :al-overhead-at-end 116 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16291 :visit-id "02" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2749 :al-overhead-at-end 125 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16291 :visit-id "02" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2749 :al-overhead-at-end 125 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 3 0 /private/var/folders/58/m3km1yk15rgcq0hfq011tfk80002ks/T/OPVisit7431711070805507040.xml The scheduling data was generated by CASM 29.0. CASM was run in Phase II mode. (Tic-Visit :proposal-id 16291 :visit-id "03" :proposal-version -1 :trans-version "20200619" :date "22-Jun-2021 10:21:49.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 2598720 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16291 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16291 :visit-id "03" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2758 :al-overhead-at-end 116 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16291 :visit-id "03" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2749 :al-overhead-at-end 125 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16291 :visit-id "03" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2749 :al-overhead-at-end 125 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 3 0 The scheduling data was generated by CASM 29.0. CASM was run in Phase II mode. /private/var/folders/58/m3km1yk15rgcq0hfq011tfk80002ks/T/OPVisit13384311140309157812.xml (Tic-Visit :proposal-id 16291 :visit-id "04" :proposal-version -1 :trans-version "20200619" :date "22-Jun-2021 10:21:50.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 2309968 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16291 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16291 :visit-id "04" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2756 :al-overhead-at-end 116 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16291 :visit-id "04" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2749 :al-overhead-at-end 125 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16291 :visit-id "04" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2749 :al-overhead-at-end 125 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 3 0 The scheduling data was generated by CASM 29.0. CASM was run in Phase II mode. /private/var/folders/58/m3km1yk15rgcq0hfq011tfk80002ks/T/OPVisit4799756794226214365.xml (Tic-Visit :proposal-id 16291 :visit-id "05" :proposal-version -1 :trans-version "20200619" :date "22-Jun-2021 10:21:50.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 2598720 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16291 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16291 :visit-id "05" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2758 :al-overhead-at-end 116 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16291 :visit-id "05" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2749 :al-overhead-at-end 125 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16291 :visit-id "05" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2749 :al-overhead-at-end 125 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 3 0