0Assigned ID: 2520
----- Attempting Submission 1 (Sat Apr 10 00:01:23 GMT 2021) -----This resubmission includes Visit 10:
i.e., 1 orbit observation of the target J1030+0524.
The previous Visit (#04) of this target suffered a delayed guide-star reacquisition,
leading to degraded data.
This has been approved via: HOPR 92184
As a reminder: we opted for a common strategy for all targets.
We kept the some ORIENT constraints set in the previous submission.
The target with such constraints that still need to be scheduled are:
J1030+0524
P340-18
These constraints are set to limit the effect of difraction spikes of brigth
nearby stars over the target of our observations.-536705039----- Attempting Submission 1 (Thu Jul 29 14:05:23 GMT 2021) -----
----- Attempting Submission 2 (Fri Sep 17 13:59:32 GMT 2021) -----
----- Attempting Submission 3 (Fri Sep 17 20:54:43 GMT 2021) -----
HST Phase II Proposal 16740 successfully submitted.
Receipt: # 16740-3
----- Attempting Submission 4 (Tue Apr 05 07:29:43 GMT 2022) -----The host galaxies of the first QSOsThe mere presence of hundreds of luminous quasars at cosmic dawn (redshift z>6, age of the Universe <1 Gyr) represents a puzzle to mechanisms of formation and early growth of massive black holes and galaxies. The central engine of these quasars is a black hole of ~1e9 solar masses. In the local universe, such massive black holes only reside in the most massive galaxies. Detailed optical IFU observations VLT/MUSE have indeed revealed massive and extended gaseous reservoirs fueling intense episodes of star formation in z>6 quasar hosts. At the same time, high-resolution ALMA observations unveiled highly massive and star forming galaxies. However, to date, the host starlight remain elusive at such early cosmic times, due to surface brightness and wavelength range limitations.
Here we propose to perform a survey of a sample of 9 QSOs at z>6 to image their host galaxy starlight in the rest-frame optical emission (which is a robust tracer of the stellar mass). For all these objects deep MUSE and ALMA observations shows the presence of extended gas reservoirs and dust. The ultimate goal of the project is to have direct constraints on the stellar distribution in these early active galaxies, and relate this information to the spatial distribution of gas and dust. This will allow us to investigate the interplay between star formation and the gas cycle in these systems.We aim to characterize the rest-frame UV properties of 9 faint (J>26) host galaxies located underneath the central (unresolved) emission of 9 bright (J<21) QSOs at z>6.
To achieve the required accuracy in the PSF modelling and in the detection of the low surface brightness emission from the QSO hosts we will image each field for one orbit with WFC3/IR F140W to achieve an AB magnitude of ~27 at 5-sigma. We will use the default 4-step box dither pattern (WFC3-IR-DITHER-BOX-MIN) with an increased dither step to avoid possible self-persistence issues due to the bright QSOs. This dither step will give adequate subpixel sampling to reconstruct nyquist-sampled (2pix/FWHM) images and it is a commonly used patthern for high-redshift studies, easing the search for PSF reference with the same sampling for PSF subtraction purposes.
Each visit is divided in 4 Sub Exposures to facilitate the removal of cosmic rays.The team comprises of world-wide research leaders in the field of high-redshift quasars. The PI of this project, Dr. Farina, has pushed the study of the nebular emission around QSOs to z>6. The Co-PI, Dr. Decarli, has extensively studied high-z host galaxies in terms of stellar emission and of their gas and dust content. They published 27 first author papers on the subject in the last 10 years.
Prof. Hennawi has played a leading role in the study of quasars as cosmological probes. He wrote 13 first-author publications on this subject, and led a large and prolific group studying virtually any properties of quasars, in particular clustering, duty cycle, diffuse nebular emission, absorption properties of the intervening intergalactic medium. Dr. Walter, Dr. Venemans, Dr. Wang, Dr. Banados, Dr. Mazzucchelli, prof. Fan are responsible for the discovery and characterization of >75% of the z>6 quasars known to date, including the most distant quasar at z=7.6. Dr. Walter, Dr. Decarli, Dr. Venemans, Dr. Novak, Dr. Neeleman have led ground-breaking studies of star formation and of the interstellar medium in high-redshift galaxies and quasar host galaxies (including sub-arcsecond resolution ALMA maps).Supermassive Black Holes and Active GalaxiesGalaxies6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDGALAXYQSOQUASARNOTwo bright stars located withing the WFC3/IR FoV at:
21:32:30.15 +12:17:26.0 (i_AB~9.8mag)
21:32:35.21 +12:17:52.9 (i_AB~11.7mag)
Nearby galaxy with K_AB=20.3mag located 1.6 arcsec NNE from the target QSO.J2000J2000J_AB=19.74GALAXYQSOQUASARNOJ2000J2000J_AB=19.51GALAXYQSOQUASARNOOne bright star located at the edge of the WFC3/IR FoV at:
23:29:12.23 -03:02:29.05 (i_AB~10.2mag)J2000J2000J_AB=21.56GALAXYQSOQUASARNOOne bright star located within the WFC3/IR FoV at:
10:30:25.59, +05:24:25.71 (i_AB~12.5mag)J2000J2000J_AB=19.79GALAXYQSOQUASARNOJ2000J2000J_AB=19.32GALAXYQSOQUASARNOJ2000J2000J_AB=19.85GALAXYQSOQUASARNOOne bright star located withing the WFC3/IR FoV at:
22:40:48.77 -18:39:27.7 (i_AB~15.7mag)J2000J2000J_AB=20.28GALAXYQSOQUASARNOJ2000J2000J_AB=19.93GALAXYQSOQUASARNOOne fairly faint star located close to the target:
22:28:43.03 +01:10:38.89 (i_AB~18.1mag)J2000J2000J_AB=20.90WFC3/IRImagingNoNoF140WWFC3/IRImagingNoNoF140WWFC3/IRImagingNoNoF140WWFC3/IRImagingNoNoF140WWFC3/IRImagingNoNoF140WWFC3/IRImagingNoNoF140WWFC3/IRImagingNoNoF140WWFC3/IRImagingNoNoF140WWFC3/IRImagingNoNoF140WPOS-TARGDITHER4.004LINE4.015falsefalse74.653418.528WFC3-IR-DITHER-BOX-MIN1false/home/ema/Dropbox/Astronomy/Proposals/HST/202104_HostHighZQSOs/PhaseII/OP-cache/HST29_Host_PhaseII_v2-v01.xmlThe scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.Two bright stars located withing the WFC3/IR FoV at:
21:32:30.15 +12:17:26.0 (i_AB~9.8mag)
21:32:35.21 +12:17:52.9 (i_AB~11.7mag)
The separation from our target of the first star is 53.2arcsec and with an on-sky position angle (East of North) of PA=236.72degree.
The separation from our target of the second star is 29.68arcsec and with an on-sky position angle (East of North) of PA=94.56degree.
Following the secition 6.2.2 (Target Orientation Visit-level Special Requirements) of the HST documentation we thus select to avoid angles within ORIENT - PA(star) equal to 135deg and 315deg (with a buffer of +/-10deg) and those with ORIENT - PA(star) equal to 0deg, 90deg, 180deg, and 270deg. This implies that the following ORIENT ranges are *not* suitable for our observations:
1st star
1.7 deg < ORIENT < 21.7 deg
46.7 deg < ORIENT < 66.7 deg
136.7 deg < ORIENT < 156.7 deg
181.7 deg < ORIENT < 201.7 deg
226.7 deg < ORIENT < 246.7 deg
316.7 deg < ORIENT < 336.7 deg
2nd star
39.6 deg < ORIENT < 59.6 deg
84.6 deg < ORIENT < 104.6 deg
174.6 deg < ORIENT < 194.6 deg
219.6 deg < ORIENT < 239.6 deg
264.6 deg < ORIENT < 284.6 deg
354.6 deg < ORIENT < 14.6 deg
Nearby galaxy with K_AB=20.3mag located 1.6 arcsec NNE from the target QSO. This will be resolved by HST and thus the impact of the diffraction spikes will be minimal.1649555875000264.6(Tic-Visit
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The separation from our target of this star is 66.5arcsec and with an on-sky position angle (East of North) of PA=117.05degree.
Following the secition 6.2.2 (Target Orientation Visit-level Special Requirements) of the HST documentation we thus select to avoid angles within ORIENT - PA(star) equal to 135deg and 315deg (with a buffer of +/-10deg) and those with ORIENT - PA(star) equal to 0deg, 90deg, 180deg, and 270deg. This implies that the following ORIENT ranges are *not* suitable for our observations:
17.1 deg < ORIENT < 37.1 deg
62.1 deg < ORIENT < 82.1 deg
107.1 deg < ORIENT < 127.1 deg
197.1 deg < ORIENT < 217.1 deg
242.1 deg < ORIENT < 262.1 deg
287.1 deg < ORIENT < 307.1 deg(Tic-Visit
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The separation from our target of this star is 36.9arcsec and with an on-sky position angle (East of North) of PA=217.55degree.
Following the secition 6.2.2 (Target Orientation Visit-level Special Requirements) of the HST documentation we thus select to avoid angles within ORIENT - PA(star) equal to 135deg and 315deg (with a buffer of +/-10deg) and those with ORIENT - PA(star) equal to 0deg, 90deg, 180deg, and 270deg. This implies that the following ORIENT ranges are *not* suitable for our observations:
27.6 deg < ORIENT < 47.6 deg
117.6 deg < ORIENT < 137.6 deg
162.6 deg < ORIENT < 182.6 deg
207.6 deg < ORIENT < 227.6 deg
297.6 deg < ORIENT < 317.6 deg
342.6 deg < ORIENT < 2.6 deg164642688800082.84386080162972(Tic-Visit
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)true10The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.One bright star located withing the WFC3/IR FoV at: 22:40:48.77 -18:39:27.7 (i_AB~15.7mag)
The separation from our target of this star is 16.4arcsec and with an on-sky position angle (East of North) of PA=348.68degree.
Following the secition 6.2.2 (Target Orientation Visit-level Special Requirements) of the HST documentation we thus select to avoid angles within ORIENT - PA(star) equal to 135deg and 315deg (with a buffer of +/-10deg) and those with ORIENT - PA(star) equal to 0deg, 90deg, 180deg, and 270deg. This implies that the following ORIENT ranges are *not* suitable for our observations:
68.7 deg < ORIENT < 88.7 deg
113.7 deg < ORIENT < 133.7 deg
158.7 deg < ORIENT < 178.7 deg
248.7 deg < ORIENT < 268.7 deg
293.7 deg < ORIENT < 313.7 deg
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)true10The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.One fairly faint star located close to the target: 22:28:43.03 +01:10:38.89 (i_AB~18.1mag)
The separation from our target of this star is 10.1arcsec and with an on-sky position angle (East of North) of PA=311.46degree.
Following the secition 6.2.2 (Target Orientation Visit-level Special Requirements) of the HST documentation we thus select to avoid angles within ORIENT - PA(star) equal to 135deg and 315deg (with a buffer of +/-10deg) and those with ORIENT - PA(star) equal to 0deg, 90deg, 180deg, and 270deg. This implies that the following ORIENT ranges are *not* suitable for our observations:
31.5 deg < ORIENT < 51.5 deg
76.5 deg < ORIENT < 96.5 deg
121.5 deg < ORIENT < 141.5 deg
211.5 deg < ORIENT < 231.5 deg
256.5 deg < ORIENT < 276.5 deg
301.5 deg < ORIENT < 321.5 deg163806983400068.7591037907755(Tic-Visit
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Following the secition 6.2.2 (Target Orientation Visit-level Special Requirements) of the HST documentation we thus select to avoid angles within ORIENT - PA(star) equal to 135deg and 315deg (with a buffer of +/-10deg) and those with ORIENT - PA(star) equal to 0deg, 90deg, 180deg, and 270deg. This implies that the following ORIENT ranges are *not* suitable for our observations:
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