Cross-calibration of HST, Euclid and Roman grism/prism through WFC3-IR faint spectrophotometric white dwarf standards near the North and South Ecliptic Poles

This proposal does not quite fall into the catagory of an HST calibration proposal. Rather, the proposal wishes to establish six hot White dwarfs as stable, spectrophotometric IR standards for use by Euclid and the Roman Space telescope, due from launch in 2022 and ~ 2026 respectively. As such, we have placed it in the "Large Scale Structure of the Universe" catagory. (Note that these comments still apply--as of Friday 9 April 2021 at 10.13am PST) 2139747178 Assigned ID: 1694 ----- Attempting Submission 1 (Thu Apr 08 19:53:42 GMT 2021) ----- HST Phase I Proposal 1694 successfully submitted. Receipt: # 1694-1 ----- Attempting Submission 2 (Thu Apr 08 23:35:28 GMT 2021) ----- HST Phase I Proposal 1694 successfully submitted. Receipt: # 1694-2 ----- Attempting Submission 3 (Fri Apr 09 14:20:21 GMT 2021) ----- HST Phase I Proposal 1694 successfully submitted. Receipt: # 1694-3 ----- Attempting Submission 4 (Fri Apr 09 17:13:43 GMT 2021) ----- this submission includes some changes to the preferred orient for visit 59. Hopefully, the Orient is not too restrictive. 1357128797 ----- Attempting Submission 1 (Thu Jul 29 17:55:44 GMT 2021) ----- ----- Attempting Submission 3 (Wed Oct 06 13:49:01 GMT 2021) ----- ----- Attempting Submission 4 (Tue Mar 01 17:23:00 GMT 2022) ----- Your proposal could not be saved. Submission aborted. Your proposal could not be saved. Submission aborted. ----- Attempting Submission 5 (Tue Aug 16 22:11:37 GMT 2022) ----- ----- Attempting Submission 6 (Wed Sep 14 13:24:04 GMT 2022) ----- Cross-calibration of HST, Euclid and Roman grism/prism through WFC3-IR faint spectrophotometric white dwarf standards near the North and South Ecliptic Poles One of the most exciting results in modern cosmology has been the discovery of the accelerated expansion of the Universe. It could be due to an unknown energy component (i.e., dark energy) or the modification of general relativity. In order to illuminate the unknown nature of the observed cosmic acceleration, ESA's Euclid and NASA's Roman Space Telescopes will be launched in 2022 and ~2026 respectively. They will complement each other in probing cosmic acceleration with high precision and accuracy, and need tight requirements on spectrophotometry to unprecedented accuracy. Accurate absolute spectrophotometry is vital to determine the fraction of baryonic matter turned into stars, for galaxy and supernovae surveys, and to enable legacy science. Extreme care must be taken to control systematic errors and biases. We propose to establish six hot White Dwarfs as stable, spectrophotometric IR standards for use by Euclid and Roman. The targets are suitable for spectrophotometry with the WFC3-IR grisms, and chosen to lie near both ecliptic poles within the Euclid and Roman CVZ. This allows for year-round accessibility. The stars lie within two planned, frequently repeated, Euclid deep fields, and in a likely location to be observed by Roman for calibration purposes. Although not formally an HST calibration proposal, our 11-orbit program will be vital in tying Euclid/Roman deep field spectra of faint galaxies to well-calibrated HST standards. It will also cross-calibrate the spectrophometry to broad-band IR colors of these faint high ecliptic-latitude sources. This proposed program is of critical importance to the successful calibration of both Euclid and Roman. WFC3/IR grism observations with G102 and G141 will cover the 0.8 - 1.7 micronm range with resolutions R = 200 and 150, respectively (Bohlin & Deustua 2019). Table 1 lists the six targets, Pan-STARRS r-band magnitude, the grism exposure times for S/N = 120 per resolution element, and the associated number of orbits. Grism exposure times were computed using the WFC3 Grism ETC with the default background values and aperture, using the CALSPEC standard WD1327-083 stiswfc 002.fits as the spectral template, normalized to the r-band AB magnitude of each target, and a desired S/N = 100 at 1.0 micron for G102 and 1.3 micron for G141. The resulting exposures times range from 151s to 2556s in G102, and from 135s to 2586s in G141 and are listed in the table Filter exposure time calculations were made using the IR imaging ETC with default background values and apertures, using the CALSPEC standard WD1327-083 stiswfc 002.fits as the template, normalized to the targets r-band magnitude, for S/N = 100. Exposure times are less than 70s in F160W, less than 17s in F110W and less than 38s in F098M. Imaging exposures will be acquired using a 3 point dither pattern to mitigate detector effects. The orbit number per target includes the on-target grism exposures as well as direct imaging in filters F098M, F110W and F160W. Acquisition overheads, filter wheel changes and readout time are included in the orbit estimates, for total of 11 orbits. The roll angles will be chosen such that no spectra contamination occurs from neigh- boring sources. GD153 observations will be scheduled in time between the northern and southern star visits to guarantee a contemporaneous reference star that is on the CALSPEC calibration system.. Our team brings together experts from all areas of IR space-based spectroscopy spanning the full range from optical and IR ground-based spectroscopy, space based spectroscopy and imaging with HST , Euclid and Roman. Philip Appleton PI: (Caltech/IPAC) is a senior research scientist, and has experience in radio and infared spectroscopy. He was an Associate Professor of Astrophysics at Iowa State University from 1986-2001. He worked (2001-2009) at the Spitzer Science Center to help calibrate the Infrared Spectrograph on Spitzer. He later was a US calibration liaison scientist for the PACS spectrometer on Herschel, and became the Project Scientist/Task Lead for the NASA Herschel Science Center from 2009 to 2016. He is currently at the Euclid NASA Science Center/IPAC Caltech, where he in involved in absolute calibration with Euclid. He is a member of the Euclid Calibration Working Group, and is Deputy Head of Science at IPAC. He is also involved with plans (led by Lee Armus at IPAC) to develop data reduction pipelines for the grism/prism data on Roman. His research interest is in galaxies and galaxy evolution, and specialises in observational evidence for atomic and molecular shock-heating and cooling in galaxies and AGN. Susana Deustua (STScI) Co-Principal Investigator: is an calibration scientist whose research areas are supernova cosmology and the calibration of large surveys and missions in astronomy, and is experienced with spectroscopy and imaging with WFC3. Currently, she is an active member of the Roman calibration working group and is PI of an absolute flux calibration project. She will be in charge of the WFC3 data reduction. Lee Armus (Caltech/IPAC): is a senior research scientist. He is lead scientist for the Roman project at IPAC, and lead of the IPAC Roman slitless spectroscopy development team. This includes slitless spectroscopy pipeline development. He has PI'ed several large projects and has a long history of work in calibrating and using IR spectrographs. Ralph Bohlin (STScI): is a senior calibration astronomer at STScI and has been involved in many HST calibration campaigns, including the WFC3 grisms. He is an expert in absolute calibration of space telescopes, especially HST. Stefano Castenarto (STScI): is an observatory scientist and WFI Instrument Scientist; He has over 20 years experience with calibration of HST instruments, and formerly was Project Scientist for Data Quality for HST. He currently co-leads of the Roman/WFI Calibration Working Group. Ranga-Ram Chary(Caltech/IPAC): is a senior research scientist and Euclid U.S. Science Team PI at the Euclid NASA Science Center. he is a member of the Euclid Collaboration, working on decontamination of the Euclid grism spectra. James Colbert (Caltech/IPAC): is a member of both the NASA Euclid Science Center and WFIRST Science Operations Center teams and Euclid Collaboration member. His expertise is in near-infrared grism spectroscopy, involved in both simulation and developing software pipelines. Yannick Copin (Universite Claude Bernard, Lyon): is an associate professor and Deputy Lead Scientist of the Euclid Operational Unit SIR (Spectroscopy) team, and has considerable experience in optical spectrophotometry. Jeffrey Kruk (NASA/GSFC); is Research Astrophysicist and is currently Deputy Senior Project Scientist for the Roman Space Telescope. Dan Masters (Caltech/IPAC): is a Scientific Research Associate Member of the Euclid Consortium, and key member of the OU-PHZ team leading the photometric redshift calibration effort for Euclid. He is also a member of the Roman cosmology science investigation team (SIT), and Member of the SPHEREx science team and SPHEREx IPAC pipeline development team and is working on the photometric calibration for that mission. Sangeeta Malhotra (GSFC): is Research Astrophysicist who is an expert in galaxy evolution, especially in studies of medium to high redshift galaxies. She is closely involved in the grism and prism development for the Roman Space Telescope. She has been involved in infrared spectroscopy for many year. Mischer Schirmer (MPIA): is the Euclid Lead Calibration Scientist and responsible for Euclid's overall calibration scheme and execution. Previously, MS was responsible for the near-infrared imaging and spectroscopic instruments at the Gemini-South observatory (2011-2017) and the William Herschel Telescope (2004-2008), supporting the hardware as well as developing data processing software. Marco Scodeggio (CNR;IASFC): is Lead Scientist of the Euclid Operational Unit SIR (Spectroscopy) team and has considerable experience in optical and IR spectroscopy of galaxies in large surveys and galaxy evolution. Daniel Scolnic (Duke U./Dept. of Physics): is an expert in absolute calibration, particularly focusing on cross-calibration between surveys. He led the calibration working group for Roman. He participates in many of the international collaborations that are collecting astronomical survey measurements in unprecedented quantity and quality, including Pan-STARRS; the Dark Energy Survey (DES); the Large Synoptic Survey Telescope (LSST); and the Roman Space Telescope. Daniel Stern (JPL): is a Senior Research Scientist at JPL and is member of the Complimentary Observations Group (COG) for Euclid and was part of the WFIRST (now Roman) STDT. As a member of the COG, Stern is involved in complimentary data being obtained in support of the Euclid mission. Harry Teplitz (Caltech/IPAC): is the Science Lead for the Euclid NASA Science Center at IPAC, and has extensive experience with HST imaging and grism spectroscopy. He is PI of programs including UVUDF & UVCANDELS; senior team member for the WFC3 Infrared Spectroscopy Parallels survey (WISPs; PI=Malkan). Yun Wang (Caltech/IPAC): is a Senior Research Scientist in the Euclid NASA Science Center, and Deputy Coordinator of Euclid Galaxy Clustering Science Working Group, BAO/RSD Science Topic Lead for Roman Large Scale Structure of the Universe 0 false false false false false false false SUPPORTED STAR WDO NO J2000 J2000 17.927Rpmag STAR WDO J2000 J2000 17.655Rpmag STAR WDO NO J2000 J2000 17.3966Rpmg STAR WDO J2000 J2000 16.936Rpmag STAR WDO J2000 J2000 16.647Rpmag STAR WDO J2000 J2000 15.425Rpmag STAR WDO J2000 J2000 WFC3/IR Spectroscopic No No G102 WFC3/IR Spectroscopic No No G141 WFC3/IR Imaging No No F098M WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F110W WFC3/IR Spectroscopic No No G102 WFC3/IR Spectroscopic No No G141 WFC3/IR Imaging No No F098M WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F110W WFC3/IR Spectroscopic No No G102 WFC3/IR Spectroscopic No No G141 WFC3/IR Imaging No No F098M WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F110W WFC3/IR Spectroscopic No No G102 WFC3/IR Spectroscopic No No G141 WFC3/IR Imaging No No F098M WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F110W WFC3/IR Spectroscopic No No G102 WFC3/IR Spectroscopic No No G141 WFC3/IR Imaging No No F098M WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F110W WFC3/IR Spectroscopic No No G102 WFC3/IR Spectroscopic No No G141 WFC3/IR Imaging No No F098M WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F110W WFC3/IR Spectroscopic No No G102 WFC3/IR Spectroscopic No No G141 WFC3/IR Imaging No No F098M WFC3/IR Imaging No No F160W WFC3/IR Imaging No No F110W 1663161504537 The scheduling data was generated by CASM 30.3. 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