Mapping A Distant Protocluster Anchored by A Luminous Quasar in the Epoch of Reionization

0 Assigned ID: 441 ----- Attempting Submission 1 (Fri Mar 06 10:36:46 GMT 2020) ----- HST Phase I Proposal 441 successfully submitted. Receipt: # 441-1 ----- Attempting Submission 2 (Fri Mar 06 22:33:30 GMT 2020) ----- ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN repeating visit 01. The new visit is named as visit 51 within the J0910-G mosaic folder 1181903141 ----- Attempting Submission 1 (Thu Jun 11 23:36:20 GMT 2020) ----- HST Phase II Proposal 16187 successfully submitted. Receipt: # 16187-1 ----- Attempting Submission 2 (Thu Jun 25 17:31:47 GMT 2020) ----- ----- Attempting Submission 3 (Wed Feb 17 03:51:04 GMT 2021) ----- ----- Attempting Submission 4 (Fri Feb 19 15:06:45 GMT 2021) ----- ----- Attempting Submission 5 (Thu Mar 04 21:37:15 GMT 2021) ----- Your proposal could not be saved. Submission aborted. ----- Attempting Submission 6 (Wed Mar 09 21:38:53 GMT 2022) ----- warning and errors on already observed visits Mapping A Distant Protocluster Anchored by A Luminous Quasar in the Epoch of Reionization Theoretical models predict luminous quasars should reside in the most massive dark matter halos acting as signposts for large overdensities of galaxies in the young Universe. But despite two decades of searching, proto-clusters traced by quasars have not yet been uncovered in the epoch of reionization (EoR). Recent ALMA/JCMT sub-mm observations and Subaru narrow/broad band imaging of a luminous quasar at z=6.63 have revealed a spectacular overdensity of [CII] emitters, sub-mm galaxies (SMGs), and Lyman alpha emitters (LAEs), suggesting that it is the the most distant known proto-cluster harboring quasar activity, and the first such system discovered in the EoR. With two HST pointings we will map the inner region of this large scale structure, covering the quasar, six [CII] emitters, two LAEs, and seven SMGs. The high-resolution WFC3 images will measure the spectral energy distribution and the sizes of these galaxies, and resolve two putative galaxy merger systems. It will also enable accurate PSF subtraction to study the assembly of the massive and very large (>1 arcsec, from ALMA) quasar host galaxy. On larger scales, the combination of HST and Subaru deep imaging will identify more than 20 Lyman-break galaxies (LBGs) at z~6.6, and reveal the distribution of star forming galaxies. These rest-frame UV HST observations will trace the unobscured star formation, highly complimentary to the dust and gas emission traced by ALMA and JCMT. In addition, our proposed observations provide data essential for planning future JWST NIRSpec/MSA and IFU observations of this unique system to understand galaxy formation and evolution in the densest environments in the EoR. This program aims at observing a protocluster at z=6.63 with HST/WFC3 in two bands, F125W and F160W. We will perform two main pointings, one centered at the central quasar position, the other centered at a galaxy merger system. Each pointing has 8 primary orbits. In addition, we will observe a PSF star with one orbit in order to get an accurate PSF model for studying the quasar host galaxy. We requires some specific orientation range which does not reduce the visibility too much but significantly increase the number of galaxies covered by our HST observations. We also requires the orientation of PSF observations to be similar with the quasar pointing. 1. Mosaic centered at the galaxy merger system Visit 01, 02, 03, 04 We use 8 primary orbits (2x2 mosaicing) for this pointing to get deep imaging in F125W and F160W bands. The goal of this pointing is to detect the rest-frame UV emission from the galaxy merger system and other sub-milliter galaxies in the field. Each visit includes one orbit F125W imaging and one orbit F160W imaging observations. The galaxy merger system will be covered in all four mosaicing positions and thus will be in the deepest region of the final mosaiced image. 2. Mosaic centered at the quasar position Visit 05, 06, 07, 08 We use 4 primary orbits (2x2 mosaicing) for this pointing to get deep imaging in F125W and F160W bands. The goal of this pointing is to detect the rest-frame UV emission from sub-milliter galaxies in the vicinity of the quasar. Each visit includes one orbit shared by F125W and F160W imaging. The quasar will be covered in all four mosaicing positions and thus will be in the deepest region of the final mosaiced image. Different from the first mosaicing, we use shorter individual exposure to avoid saturating the central quasar. This observation will also be used for quasar host galaxy detection as detailed below. The orientation of this mosaic will be constrained to be similar (+/- 5 degrees) with visit 09 (see below). 3. Single pointing centered at the quasar position. Visit 09, 10 This pointing (4 primary orbits) aims at detecting the host galaxy of the central quasar which requires accurate PSF modeling. In order to minimize the thermal variation effects on the PSF model due to the orbital day/night cycle, we constructed our orbits to ensure that we fully sample each orbit in two bands. In order to accurately model the PSF, we will also observe one PSF star in these two bands with one orbit. The PSF star observation will also be observed in the same manner to minimize the thermal variation caused by the orbital day/night cycle. In addition, to minimize thermal variations due to spacecraft attitude, we request to observe our PSF star to be within five degrees in the orientation of the quasar observations. We also require that the quasar and PSF star observations to be collected in contiguous orbits. We further request that our observations should be scheduled immediately following another observation near the same celestial coordinates, thus minimizing thermal equilibration time in our first visit. 4. Single pointing centered at a PSF star Visit 11 The observation closely following Visit 09 and 10 but with much shorter individual exposures to avoid saturation. We use the subarray for the PSF observations. Our team members have done pioneering work in the areas of high-redshift quasars, BH/galaxy coevolution, reionization and quasar clustering. We also have extensive experience in using HST, especially with WFC3 (the proposed instrument) and ACS imaging. Team members have led several tens successful HST programs in those areas in previous cycles, resulted in a large number of publications. Dr. Banados is an expert on quasar searching, quasar environment and quasar host galaxy studies. Dr. Bian is an expert in high redshift galaxies, especially high redshift Lyman break galaxies. Dr. Davies is an expert on cosmic reionization and cosmological simulations. Dr. Decarli is an expert on sub-millimeter observations, quasar host galaxies and high contrast imaging analysis. Prof. Fan is an observational cosmologist and has led several past HST programs on high redshift quasars and galaxies. He is also an expert on studying the most distant galaxies and quasars, quasar host galaxies and the cosmic reionization. Dr. Farina is an export on quasar host galaxy and quasar environment. He has extensive experience with PSF modeling and PSF subtraction. Prof. Hennawi is an expert on quasar clustering, cosmic reionization, and computational simulations. Prof. Hennawi have many expertise on studies focus on understanding the nature of quasars and galaxies at high- redshift. Dr. Jiangtao Li is an expert on multi-wavelength observations of galaxies, especially on X-ray observations of the extended hot gas in the CGM/IGM. Dr. Mazzucchelli is an expert on high redshift quasars and quasar environments. Dr. Venemans is an expert on sub-millimeter observations, quasar host galaxies and distant quasar studies. Dr. Walter is an expert on sub-millimeter observations, high redshift galaxies, and quasar host galaxies. Dr. Wang is an expert on high redshift quasar studies. He has expertise in HST data reduction for ACS and WFC3. Dr. Wang also has experience with PSF modeling and PSF subtraction, and high contract imaging analysis. Prof. Wu is an expoert on high redshift quasar studies including both high redshift quasar searching, quasar and host galaxy coevolution and supermassive black hole physics. Dr. Yang is an expert on high redshift quasars, quasar/galaxy luminosity function, and galaxy photometric redshifts measurements. Ms. Jones is a graduate student of Prof. Fan. She will help on the PSF subtraction and quasar host galaxy studies. Mr. Yue is an graduate student of Prof. Fan, Mr Yue has experience with PSF subtraction and high contrast imaging analysis. Supermassive Black Holes and Active Galaxies Large Scale Structure of the Universe 6 false false false false false false false SUPPORTED GALAXY QUASAR J2000 J2000 J=28.6 AB GALAXY ULTRALUMINOUS IR GAL J2000 J2000 J=28.6 AB STAR M V-IV J2000 J2000 J=16.95, H=16.272, Ks=15.34 WFC3/IR Imaging No No F125W WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F125W WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F125W WFC3/IR Imaging No No F160W 1646861488036 Hst Same orient constraint links visits (01 02 03 04 53) The scheduling data was generated by CASM 30.1. 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CASM was run in Phase II mode. /private/var/folders/jn/c8t6q4fd2vs64sp7y1322sq00000gn/T/OPVisit4525892388355841132.xml 1614076813000 60.09 (Tic-Visit :proposal-id 16187 :visit-id "09" :proposal-version -1 :trans-version "20211222" :date "09-Mar-2022 14:31:39.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 2942224 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16187 :visit-id "09" :obset-id "09" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16187 :visit-id "09" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2755 :al-overhead-at-end 0 :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 16187 :visit-id "09" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2730 :al-overhead-at-end 0 :internal-dur-at-end 709 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 2 0 1646861501436 The scheduling data was generated by CASM 30.1. CASM was run in Phase II mode. /private/var/folders/jn/c8t6q4fd2vs64sp7y1322sq00000gn/T/OPVisit4254310869317622988.xml 1614259823000 60.09 (Tic-Visit :proposal-id 16187 :visit-id "10" :proposal-version -1 :trans-version "20211222" :date "09-Mar-2022 14:31:41.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 2942224 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16187 :visit-id "10" :obset-id "10" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16187 :visit-id "10" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2755 :al-overhead-at-end 0 :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 16187 :visit-id "10" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2730 :al-overhead-at-end 0 :internal-dur-at-end 709 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 2 0 1646861504174 The scheduling data was generated by CASM 30.1. CASM was run in Phase II mode. /private/var/folders/jn/c8t6q4fd2vs64sp7y1322sq00000gn/T/OPVisit9292567713708396134.xml 1613322085000 61.09 (Tic-Visit :proposal-id 16187 :visit-id "11" :proposal-version -1 :trans-version "20211222" :date "09-Mar-2022 14:31:43.0" :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 567136 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16187 :visit-id "11" :obset-id "11" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16187 :visit-id "11" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2650 :al-overhead-at-end 0 :internal-dur-at-end 701 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 1 0 1646861506580 The scheduling data was generated by CASM 30.1. CASM was run in Phase II mode. /private/var/folders/jn/c8t6q4fd2vs64sp7y1322sq00000gn/T/OPVisit6885992672025385570.xml 1646580235000 65.09 (Tic-Visit :proposal-id 16187 :visit-id "61" :proposal-version -1 :trans-version "20211222" :date "09-Mar-2022 14:31:46.0" :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 567136 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16187 :visit-id "61" :obset-id "61" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16187 :visit-id "61" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2650 :al-overhead-at-end 0 :internal-dur-at-end 701 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 1 0