0Assigned ID: 3349
----- Attempting Submission 1 (Fri Mar 25 17:21:23 GMT 2022) -----
HST Phase I Proposal 3349 successfully submitted.
Receipt: # 3349-1
----- Attempting Submission 2 (Fri Mar 25 20:19:00 GMT 2022) -----
HST Phase I Proposal 3349 successfully submitted.
Receipt: # 3349-2PARALLELS SIGNIFICANTLY EXTEND ALIGNMENT TIME
PARALLELS SIGNIFICANTLY EXTEND ALIGNMENT TIMEResubmission with Visit Z1 as part of HOPR 92593.
This replaces orbit 1 from Visit 1 and orbit 1 from Visit 7, both of which failed.2069667466----- Attempting Submission 1 (Thu Jul 07 10:59:27 GMT 2022) -----
----- Attempting Submission 2 (Mon Aug 14 20:18:56 GMT 2023) -----There are 15 warnings. 1 for every visit that says the Parallels significantly extend the alignment time.
This is true, and is performed to extract the maximium time from the orbit for the ACS parallel observations. This gives us about 1 extra minute of integration time per orbit (>30 mins in total for the program), compared to the quantized integration times we can obtain from WFC/IR
The Visit Planner runs fine for Visit Z1, which is the one for which we are resubmittingAGN variability at cosmic dawn: a census of the youngest supermassive black holesThe origin and growth of the first supermassive black holes (SMBH) has become one of the most pressing unsolved problems in astrophysics. SMBHs are present in the nuclei of most massive galaxies and impact many aspects of galaxy evolution, including feedback, morphological transformations, and cosmic reionization. Several scenarios can explain how the seeds of SMBHs may have been planted, but without accurate and direct observational estimates of their comoving number density, it is hard to distinguish between them.
Under popular formation scenarios, SMBHs undergo their period of most rapid growth at high-redshift, beyond z=6. However, at this distance only the most luminous quasars have been identified, which reveal a very biased picture of the universe. AGN at intermediate luminosities (M_UV=-21 to -18, hereafter IL-AGN) must also be present, and are probably growing rapidly at z~6-10. These objects go undetected in current deep NIR imaging surveys, where they masquerade instead as star-forming galaxies. We argue here that the most reliable, yet unexplored, way to test all these highest-redshift systems for AGN activity is through variability. We therefore request 30 orbits to re-image the Hubble Ultra Deep Field with WFC3/IR/F140W, a decade after the first epoch was taken. This time delay, redshift, target restframe wavelength, and luminosity regime are all optimal for identifying AGN variability. We will make the first estimate of the comoving number density of SMBHs in the early universe, with target numbers sufficient to discriminate between black hole seeding scenarios.This is a 30-orbit imaging program. The goals are to obtain:
1. a single deep image of the Hubble Ultradeep Field with WFC3/IR/F140W
2. in parallel obtain a deep ACS/F814W image of the the HUDF05-P2 field.
The scientific objective is to test for variability of sources in both fields. Alignment with the previous campaign (UDF12; GO 12498) and acquisition of the parallel field demand an orient constraint of 264 degrees.
There are 15 visits, each of two orbits.
Each visit contains four primary exposures and four parallel, each of approximately 1/2 orbit duration. Primary (WFC3/F140W imaging) uses a SPARS100 sequence with 13 (first per orbit) and 14 (second per orbit) samples. ACS/F814W exposure times are then tuned to the maximum duration of the orbit.
We use a 4-point dither pattern within each visit, specified at the exposure level by POS-TARGs. This aims to improve the sampling of the WFC3/IR PSF and mitigate the effects of its large pixel size. The pattern is also offset by a sufficiently large amount to move persistent pixels to different locations on the sky in each exposure.
In addition, each of these 15 sets of 4-point dithers is also offset onto a larger-scale grid, where the offsets are ~3" along the +y ACS/WFC direction to cover the chip gap and other large defects on the WFC3/IR detector (such as the "death star" which has a diameter of 50 pixels, or ~6.4"). This also mitigates the effects of persistence further, by providing offset sufficiently large to move large-scale persistent structures to different locations on the sky. Both the small-scale 4-point dithers as well as the larger-scale grid are designed to build upon and complement the dither patterns that were used in a previous WFC3/IR UDF programs [11563; PI Illingworth and 12498; PI Ellis), thereby ensuring as much continuity as possible between 2012 and 2022 to deliver the most homogeneous data and optimized search for transient objects.All investigators are experts in various aspects of galaxy evolution, and have extensive experience of HST observations and data analysis.
Prof. Matthew Hayes has ~20 years experience working with HST imaging in almost all configurations and is specialist in galaxy evolution and high redshift surveys. He has acted as PI for 10 HST programs since cycle 19.
Prof. Jonathan Tan is an expert on theoretical models of supermassive black hole formation and early universe star formation. Specifically for this application his simulations motivate the search for variable AGN at these early times.
Prof. Richard Ellis is a leading researcher in galaxy evolution and observations of the highest redshift systems. Specifically here, he led the HUDF12 campaign of WFC3/IR imaging in the same field: our so-called 'Epoch one' data.
Dr. Aayush Saxena is an expert in modelling the growth and evolution of SMBHs in the early Universe and is experienced with multi-wavelength studies of AGN at high redshifts.
Prof. Zhi-Yun Li is an expert on theoretical models of accretion disks and outflows, with this physics relevant to understanding AGN accretion and variability.
Dr. Jens Melinder is a data scientist specialized in HST imaging, predominantly concerned with star-forming galaxies, and has developed a large number of custom tools for processing HST imaging data.
Prof. Pierluigi Monaco is an expert on cosmic structure formation and cosmological simulations of SMBH seeding and evolution.
Mr. Jasbir Singh is a Ph.D. student working on SMBH seeding simulations with Profs. Monaco and Tan.
Dr. Nilanjan Banik is an expert on SMBH seeding models.
Dr. Ragnhild Lunnan is an expert on stellar-mass transient events, with a focus on core-collapse and superluminous supernovae, and will aid in the identification and light curve analysis of any potential supernova "interlopers".
Dr. Benjamin Keller is an expert in numerical simulations of galaxy formation and feedback processes. He will provide theoretical constraints for this project and apply the observational results to build more realistic models for SMBH formation in future cosmological simulations.
Mr. Vieri Cammelli is a Ph.D. student focusing on the study of the connection between the physical and observational properties of Supermassive Black Holes and their host galaxies with Prof. Monaco and Prof. Tan.
Dr. Maya Petkova is an expert on numerical modelling of ionising radiation. In the context of this project, her models will be used to improve SMBH seeding simulations.Supermassive Black Holes and Active Galaxies6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYHIGH REDSHIFT GALAXYQUASARSTARBURSTJ2000J2000WFC3/IRImagingNoNoF140WACS/WFCImagingNoNoF850LPThe scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.1691123419000264.0(Tic-Visit
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:visit-id "13"
:obset-id "13"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17073
:visit-id "13"
:orbit-number 1
:pcs-time 383
:si-vis-utilization 2675
: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 3058
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 17073
:visit-id "13"
:orbit-number 2
:pcs-time 392
:si-vis-utilization 2666
:al-overhead-at-end 0
:internal-dur-at-end 1075
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3058
:pcs-gap 0
)true20The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.1691944988000264.0(Tic-Visit
:proposal-id 17073
:visit-id "14"
:proposal-version -1
:trans-version "20220516"
:date "07-Jul-2022 12:00:23.0"
:trans-errors '(:WARNINGS 1 :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 2146592
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17073
:visit-id "14"
:obset-id "14"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17073
:visit-id "14"
:orbit-number 1
:pcs-time 383
:si-vis-utilization 2675
: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 3058
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 17073
:visit-id "14"
:orbit-number 2
:pcs-time 392
:si-vis-utilization 2666
:al-overhead-at-end 0
:internal-dur-at-end 1075
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3058
:pcs-gap 0
)true20The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.1691238730000264.0(Tic-Visit
:proposal-id 17073
:visit-id "15"
:proposal-version -1
:trans-version "20220516"
:date "07-Jul-2022 12:00:23.0"
:trans-errors '(:WARNINGS 1 :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 2146592
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17073
:visit-id "15"
:obset-id "15"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17073
:visit-id "15"
:orbit-number 1
:pcs-time 383
:si-vis-utilization 2675
: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 3058
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 17073
:visit-id "15"
:orbit-number 2
:pcs-time 392
:si-vis-utilization 2666
:al-overhead-at-end 0
:internal-dur-at-end 1075
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3058
:pcs-gap 0
)true20The scheduling data was generated by CASM 31.0.CASM was run in Phase II mode./tmp/OPVisit10473155564367709502.xmlCombination of Visit 01 and Visit 07 as HOPR 92593(Tic-Visit
:proposal-id 17073
:visit-id "Z1"
:proposal-version -1
:trans-version "20220630"
:date "14-Aug-2023 22:17:43.0"
:trans-errors '(:WARNINGS 1 :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 2146592
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 17073
:visit-id "Z1"
:obset-id "Z1"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 17073
:visit-id "Z1"
:orbit-number 1
:pcs-time 383
:si-vis-utilization 2675
: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 3058
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 17073
:visit-id "Z1"
:orbit-number 2
:pcs-time 392
:si-vis-utilization 2666
:al-overhead-at-end 0
:internal-dur-at-end 1075
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3058
:pcs-gap 0
)true20