(LAST) Re-submission 3 of Windhorst et al. HST Cy 27 AR Legacy proposal with title: SKY-SURF: Panchromatic constraints on the Extragalactic Background Light and Zodical Light sources through all-sky foreground measurements Please confirm its receipt. Thanks! -1420398677 Assigned ID: 78 ----- Attempting Submission 1 (Tue Apr 02 10:11:23 GMT 2019) ----- HST Phase I Proposal 78 (zodiar_cy27.apt) successfully submitted. Receipt: # 78-1 ----- Attempting Submission 2 (Wed Apr 03 22:15:49 GMT 2019) ----- HST Phase I Proposal 78 (zodiar_cy27.apt) successfully submitted. Receipt: # 78-2 ----- Attempting Submission 3 (Fri Apr 05 23:43:18 GMT 2019) ----- HST Phase I Proposal 78 (zodiar_cy27.apt) successfully submitted. Receipt: # 78-3 ----- Attempting Submission 4 (Fri Apr 05 23:44:17 GMT 2019) ----- More than 95% of all photons in the HST Archive come from <5 AU. Yet, no precise panchromatic all-sky HST measurement of foregrounds exists. Project SKY-SURF will use HST's unique capability as absolute photometer to measure the absolute ~0.2-1.7 micron all-sky surface brightness (SB) from 57,302 ACS and WFC3 datasets in ~1100 fields. This Legacy dataset will constrain the diffuse UV-nearIR sky components: Zodiacal Light (ZL; inner solar system), Kuiper Belt Objects (KBOs; outer solar system), Diffuse Galactic Light (DGL), and Extragalactic Background Light (EBL). SKY-SURF will: (1) construct optimized panchromatic object catalogs, and an all-sky model of the (time-dependent) ZL, plus the DGL at ~10 deg resolution in the UV,U,B,V,r,i,z,Y,J,H filters free of discrete objects; (2) determine the integrated EBL to <3% by measuring panchromatic galaxy counts over 1100 HST fields, averaging over cosmic-variance effects on the EBL, as most of the EBL comes from 18-25 mag galaxies. We will use SKY-SURF's panchromatic ZL+DGL model to: (3) help recalibrate the direct EBL measurements to <4%; (4) assess how much DIFFUSE EBL can exist beyond the (extrapolated) discrete galaxy counts: Intra-galaxy Halo Light, Intra-Group Light, Intra-Cluster Light, etc.; (5) constrain the count-slope of very faint KBOs and grains in the outer solar system at R>28 mag, sampling their size-distribution from 1 km-0.1 mm; constrain the KBO flux-integral as a small excess on top of the Zodi foreground around Ecliptic latitude b_Ecl~0. (6) release to MAST panchromatic legacy products: optimized object catalogs, absolutely calibrated sky-SB data, and models of the ZL(t), DGL, and EBL. Team Experience and Tasks --- # 78: ``SKY-SURF: Panchromatic constraints on the Extragalactic Background Light and Zodical Light sources through all-sky foreground measurements. PI Dr. R. Windhorst (ASU): has been working on and with HST since 1986. Interdisciplinary Scientist for JWST since 2002. Expert in distant galaxies and cosmology. He has a keen interest in HST on-orbit Zodiacal foreground levels (Windhorst et al. 1994, 1998, 2011), the EBL and maximum SB-levels allowed by Pop III stars and their stellar-mass black hole accretion disks (Windhorst et al. 2018). He will have overall management responsibility for the data selection, retrieval, analysis, and timely dissemination of the data products from this AR Legacy program. He will help students and co-I's with the analysis of ZL, DGL, KBO and EBL data, and with writing the papers. Co-I Dr. R. Jansen (ASU): 20+ years expertise in HST data reduction and analysis. PI of the Cycle 25 HST North Ecliptic Pole Time Domain Survey. He will optimize the sky-background estimation software, train the students in its use and quality control of the results. Lead a paper on this aspect. Co-I Dr. S. Cohen (ASU): 20+ years expertise in HST data reduction and analysis. He will help the students with the data processing, SB calibrations, independent assessment of measurement quality, and writing the papers. 1 Graduate student + 2 Undergraduate students (TBD; ASU): will work with PI and Co-I's to retrieve the data from the Archive (Co-I's and GRA will help mentor the UGs after training by the PI), prepare for and perform the ACS+WFC3 data processing. They will run the PROFOUND+PROFIT object finders (instead of ``SExtractor'') for optimized total-flux fitting and panchromatic object catalogs. They will help with the analysis and help write and present the papers. Co-Is Dr. N. Grogin, J. MacKenty, N. Pirzkal (STScI): Experts on the HST orbital brightness levels (Zodi, Earthshine, straylight). They will help pre-select and verify all LOW-SKY or SHADOW images from the past HST scheduling database, help analyze SKY-SURF's sky-SB signals, and help write the team papers. Co-I Dr. S. Casertano & R. Ryan (STScI): experts in HST WFPC2, ACS and WFC3 data analysis. They will help the students interface with MAST, and with resolving pipeline calibration issues, including SI zeropoint monitoring vs. time, which is critical for our project. Co-I Dr. A. Koekemoer (STScI): expert in HST image drizzling. He will automate & optimize the ACS+WFC3 processing beyond the standard products, preserving all subtracted sky-levels during MultiDrizzle. (This is not default, but also critical for our project!). Co-I Dr. S. Kenyon (CfA): expert in the modeling of solar system debris and the Kuiper Belt Objects (KBO) size distribution. He will lead the modeling analysis and interpretation of the zodiacal foreground and KBO signal, and lead a paper on this. Co-Is Dr. R. Arendt, E. Dwek & A. Kashlinsky (NASA GSFC): experts in the analysis and modeling of Zodiacal light (ZL), Diffuse Galactic Light (DGL) and Extragalactic Background Light (EBL), respectively. Arendt will develop the time-dependent ZL model ZL(lambda, t, l_Ecl, b_Ecl), and characterize the DGL. Dwek will generate a physical model of the Zodiacal cloud consistent with the IR emission, and examine the correlation between the DGL and Galactic thermal dust emission. Kashlinsky will study the diffuse EBL that is allowed after these foregrounds are removed. Each will lead papers on this. Co-I Dr. S. Driver & A. Robotham (UCRAR, Australia): experts in very large databases and their scientific analysis, such as the GAMA survey. They will contribute their expertise in EBL and modeling (Driver et al. 2016), as well as the optimized object finder PROFOUND and optimized total-flux extractor PROFIT (Robotham et al. 2017, 2018), and will help write EBL papers. This is at no cost to NASA, they are funded by the Australian Research Council. Cosmology Galaxies and the IGM 0 Legacy false false false false true SUPPORTED