Compact oddballs in COSMOS: The Faint End of the z>6 Quasar Luminosity Function and the Growth of Ionized Bubbles

0 Assigned ID: 3543 ----- Attempting Submission 1 (Fri Mar 25 20:58:16 GMT 2022) ----- HST Phase I Proposal 3543 successfully submitted. Receipt: # 3543-1 ----- Attempting Submission 2 (Fri Mar 25 23:23:18 GMT 2022) ----- HST Phase I Proposal 3543 successfully submitted. Receipt: # 3543-2 ----- Attempting Submission 3 (Fri Mar 25 23:53:01 GMT 2022) ----- April 21, 2023: Resubmission after failed visits 03 and 07. Visits 03 and 07 have been duplicated (new ID numbers 53 and 57) after failing due to guiding error. April 14, 2023: Resubmission after failed visits 13 and 14. Visits 13 and 14 have been duplicated (new ID numbers 63 and 64) after failing due to guiding error. January 30, 2023: Resubmission of Phase II. Replaced F606W autoimage with a manual F814W autoimage before exposure 2 with same PA for each visit. I was not able to set the exposure of 180s (as it is automatically done for the F606W autoimage) because of time overrun. The maximal exposure I was able to set is 156s. 696964817 ----- Attempting Submission 1 (Tue Jul 12 12:32:54 GMT 2022) ----- ----- Attempting Submission 2 (Mon Jan 30 18:28:17 GMT 2023) ----- ----- Attempting Submission 3 (Fri Apr 14 18:25:28 GMT 2023) ----- ----- Attempting Submission 4 (Fri Apr 21 21:33:21 GMT 2023) ----- Compact oddballs in COSMOS: The Faint End of the z>6 Quasar Luminosity Function and the Growth of Ionized Bubbles Finding galaxies with an active galactic nucleus (AGN), or quasars, in the early Universe is the forefront of today's astronomical research. While luminous quasars have been well characterized, the number density of low-luminosity (<1E45 erg/s) quasars at z>6 is still uncertain. Constraining their numbers will tremendously advance our understanding of the processes which lead to the reionization of our Universe as well as the formation of the first supermassive black holes. Through stringent selection criteria including color and size, we have identified a complete sample of 7 low-luminosity quasar candidates in the 1.64 deg2 COSMOS field. Here we propose to use ACS/G800L slitless spectroscopy to confirm their redshifts via Ly-alpha and to study the spatial morphology of the emission. We will use the power of the grism to simultaneously measure Ly-alpha emission from color-selected star-forming galaxies within the ionized bubble of the quasar. This will allow us to (i) place the first constraints on the faint end of the quasar luminosity function at z>6, (ii) quantify the importance of low-luminosity quasars in the reionization process and place constraints on models of early supermassive black hole formation, (iii) study the relationship between Ly-alpha sizes and UV luminosities of low-luminosity quasars, a tracer of the size of the ionized bubbles and the clumping factor of the gas and (iv) measure star-formation in smaller halos in the local neighborhood of the quasars and statistically the Ly-alpha emitter density in the bubbles, compared to the field to further constrain the interplay between low-mass and high-mass halos in the growth of large scale structure. There are no significant modifications of the observing strategy compare to Phase 1 submission. Below, we add more details in addition to the methods outlined in the proposal. We use G800L grism observations to confirm the redshifts of 7 low-luminosity quasar candidtes via Ly-alpha emission, as well as to study the environment around these galaxies. For each of the targets, we require 2 orbits, which are split in two visits. For each orbit, we require a 180s auto-image in F814W. We then can fit four 430 second exposures in G800L. We dither each of these observations within one orbit using the default ACS-WFC-DITHER-BOX dither pattern with POS-TARG pairs (0",0"), (0.247",0.094"), (0.124",0.232"), and (0.124",0.138") for optimal half-pixel sampling in both x and y, with overall dimensions large enough to help reject the larger detector artifacts. Furthermore, we place the targets in the 1/3 closest to the chip gap. We do this to avoid edge-effects but at the same time to put the target as central as possible to study the surrounding environment at an even radius. We split the observation of each target in two visits to be able to take two spectra (of 1 orbit) at different ORIENT angles to mitigate the issue of potential overlapping dispersions. For most of the target, we use the ORIENT angles of 80-90 degrees and 110-120 degrees. These angles provide enough difference and at the same time fall into favorable ORIENT angles for efficient observations of the COSMOS field. For three targets (667155, 747548, 772319), we restrict the ORIENT angles more significantly in order to avoid overlap with the dispersion from nearby bright targets. Dr. Faisst is an expert in early galaxy formation and evolution and has expertise in HST data reduction for ACS and WFC3 imaging. He led and co-led several past HST observing programs. He also has experience in the reduction and analysis of spectra of high-redshift galaxies. Drs. Chary and Helou are experts in quasars and AGN in the early Universe. Dr. Chary is also an expert on high-z galaxy evolution and reionization and is the lead for spectral decontamination of Euclid grism spectra and for the joint survey processing effort. Dr. Brammer has valuable expertise in the reduction and analysis of HST grism observations as well as is an expert in the field of early galaxy formation. Dr. Koekemoer (STScI) brings well-established observational expertise in HST imaging and spectroscopy, and scientific expertise in AGN and galaxy evolution. With his extensive expertise with HST, he will also supervise the phase II planning of this program. Ph.D. student Weaver has experience in the extraction of photometry and SED fitting, which will be required to measure the UV properties of the galaxies and quasars. Dr. Fajardo-Acosta is an expert in the study of cool stars and proper motions, and has experience in photometry, spectroscopy, and discrimination of stellar and extragalactic objects. Supermassive Black Holes and Active Galaxies 6 false false false false false false false SUPPORTED GALAXY QUASAR 10 01 37.8461 +02 44 47.70 offset -0.5" in RA J2000 J2000 F814W magnitude: 25.7 AB GALAXY QUASAR 10 01 25.5142 +02 45 33.34 offset -0.5" in RA J2000 J2000 F814W magnitude: 25.3 AB GALAXY QUASAR 10 00 47.2067 +02 02 2.17 offset of -0.5" in RA J2000 J2000 F814W magnitude: 25.4 AB GALAXY QUASAR 09 59 8.2437 +01 43 0.72 offset 0.5" in RA J2000 J2000 F814W magnitude: 25.2 AB GALAXY QUASAR 09 58 31.0377 +02 14 50.63 offset 0.5" in RA This source is close to a brighter source in the south, therefore the ORIENT values are different than for the other sources as well as tighter constrained. J2000 J2000 F814W magnitude: 25.6 AB GALAXY QUASAR 09 58 10.6045 +02 16 31.83 offset -0.5" in RA Some bright objects nearby, therefore ORIENT is different compared to other sources and also more constrained. J2000 J2000 F814W magnitude: 25.6 AB GALAXY QUASAR 09 57 47.8332 +02 31 24.32 offset 0.5" in RA Some bright objects nearby, therefore ORIENT is different compared to other sources and also more constrained. J2000 J2000 F814W magnitude: 25.7 AB ACS/WFC Spectroscopic No No G800L ACS/WFC Spectroscopic No No G800L ACS/WFC Spectroscopic No No G800L ACS/WFC Spectroscopic No No G800L ACS/WFC Spectroscopic No No G800L ACS/WFC Spectroscopic No No G800L ACS/WFC Spectroscopic No No G800L ACS/WFC Spectroscopic No No G800L ACS/WFC Spectroscopic No No G800L ACS/WFC Spectroscopic No No G800L ACS/WFC Spectroscopic No No G800L ACS/WFC Spectroscopic No No G800L ACS/WFC Spectroscopic No No G800L ACS/WFC Spectroscopic No No G800L 1681494120198 The scheduling data was generated by CASM 30.3. 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