Calibrating the Universe: Faint White Dwarf Standard Stars at the Ecliptic Poles for Cross-calibration of HST, Euclid and Roman.apt

0 Assigned ID: 4545 ----- Attempting Submission 1 (Wed May 24 19:48:40 GMT 2023) ----- HST Phase I Proposal 4545 successfully submitted. Receipt: # 4545-1 ----- Attempting Submission 2 (Wed May 24 23:23:54 GMT 2023) ----- The number of orbits used exceeds the number allocated ORBITAL VISIBILITY OVERRUN MISSING FRINGE FLAT CALIBRATION ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN MISSING FRINGE FLAT CALIBRATION MISSING FRINGE FLAT CALIBRATION ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN MISSING FRINGE FLAT CALIBRATION MISSING FRINGE FLAT CALIBRATION MISSING FRINGE FLAT CALIBRATION MISSING FRINGE FLAT CALIBRATION MISSING FRINGE FLAT CALIBRATION MISSING FRINGE FLAT CALIBRATION MISSING FRINGE FLAT CALIBRATION MISSING FRINGE FLAT CALIBRATION MISSING FRINGE FLAT CALIBRATION MISSING FRINGE FLAT CALIBRATION MISSING FRINGE FLAT CALIBRATION MISSING FRINGE FLAT CALIBRATION MISSING FRINGE FLAT CALIBRATION MISSING FRINGE FLAT CALIBRATION STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL MISSING FRINGE FLAT CALIBRATION MISSING FRINGE FLAT CALIBRATION MISSING FRINGE FLAT CALIBRATION MISSING FRINGE FLAT CALIBRATION G750L fringe flats are in the occultation along with all Wavecals per Phase 1 TAC approval. 2024jun26-Added visit 8R per HOPR 92868. 2024jun27-Added visit 5R per HOPR 92872 2024Oct10 - Added visit 50 per HOPR 92933 -723609458 ----- Attempting Submission 1 (Tue Sep 12 19:16:42 GMT 2023) ----- ----- Attempting Submission 2 (Wed Jun 26 14:17:43 GMT 2024) ----- HST Phase II Proposal 17442 successfully submitted. Receipt: # 17442-2 ----- Attempting Submission 3 (Thu Jun 27 13:30:49 GMT 2024) ----- ----- Attempting Submission 4 (Thu Oct 10 19:13:39 GMT 2024) ----- G750L fringe flats are in the occultation along with all Wavecals per Phase 1 TAC approval. Calibrating the Universe: Faint White Dwarf Standard Stars at the Ecliptic Poles for Cross-calibration of HST, Euclid and Roman.apt One of the most exciting results in modern cosmology has been the discovery of the accelerated expansion of the Universe. ESA's Euclid and NASA's Roman Space Telescopes are designed to illuminate the unknown nature of the observed cosmic acceleration, with launch dates in 2023 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 as importantly, enable legacy science. Extreme care must be taken to control systematic errors and biases. We propose to establish five DA White Dwarfs located near the ecliptic poles, within the Euclid and Roman continuous viewing zones, as spectrophotometric standards. This allows for year-round accessibility. The stars lie within two of the Euclid deep fields, and in a likely location to be observed by Roman for calibration purposes. Our program will double the number of CALSPEC white dwarf standards at V > 16 mag, and will be vital in tying Euclid/Roman deep field spectra of faint galaxies to well-calibrated HST standards.This proposed program is of critical importance to the successful calibration of both Euclid and Roman. STIS spectroscopy with the G430L and G750L gratings formally cover the wavelength range between 2900 A and 10270 A. The exposure times for the WD targets are calculated for SNR=100 at 4500 A for G430L and at 7500 A for G750L; templates for each target are drawn from the Tremblay+ 3D model grid for logg=8 that match the Gentile Fusillo+ 2019 catalog values for Teff. For the faintest star, the CALSPEC spectrum of WD1307_083_stiswfc_004.fits scaled to WDJ040027.30-502542.04's r(ABmag) was used to calculate the exposure times, for a slightly lower average SNR over each grating to keep the number of orbits at a more reasonable number (7, instead of 13) and still have accurate spectrophotometry. Our team brings together experts from all areas of space-based spectroscopy spanning the full range from optical and IR ground-based spectroscopy, space based spectroscopy and imaging with HST, Gaia, Euclid and Roman. Philip Appleton (Caltech/IPAC, Co-PI) is a senior research scientist, and has experience in radio and infrared spectroscopy. His research interest is in galaxies and galaxy evolution and specializes in observational evidence for atomic and molecular shock-heating and cooling in galaxies and AGN. 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 is 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 involved with plans (led by Lee Armus at IPAC) to develop data reduction pipelines for the grism/prism data on Roman. Ralph Bohlin (STScI): is a senior calibration astronomer at STScI and has been involved in many HST calibration campaigns with the current generation of instruments: STIS, ACS, WFC3. He is an expert in absolute calibration of space telescopes, especially HST. Susana Deustua (NIST, PI) is a calibration scientist whose research areas are supernova cosmology and the calibration of large surveys and missions in astronomy, and she is experienced with HST spectroscopy and imaging using STIS, WFC3, ACS and COS. She leads the NIST Stars project, an international collaboration to provide SI-traceable flux calibration of standard stars, and she is PI of CANDLE (Calibration using an Artificial star with NIST-traceable Distribution of Luminous Energy) a program to develop space-based artificial stars for astronomy. She has been involved with the Roman Space Telescope since 2015 and is an active member of the Roman calibration working group. Mischa Schirmer (MPIA) is the Euclid Lead Calibration Scientist and responsible for Euclid's overall calibration scheme and execution. Previously, he 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. Pier-Emmanuel Tremblay (U. Warwick) is an expert in white dwarf evolution, 3D model atmospheres and the determination of their fundamental parameters, such as temperature, surface gravity, mass and age. He is interested in white dwarfs and stars as physics laboratories and probes of Galactic and planet formation history. Stellar Physics and Stellar Types Large Scale Structure of the Universe 0 true false false false false false false false AVAILABLE STAR WDO NO J2000 J2000 17.927Rpmag STAR WDO J2000 J2000 16.647Rpmag STAR WDO J2000 J2000 16.936Rpmag STAR WDO NO J2000 J2000 17.3966Rpmg STAR WDO J2000 J2000 17.655Rpmag STAR WDO NO J2000 J2000 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G430L 4300 The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. 1728586684402 STIS GD153 1706133997000 296.9098064004993 (Tic-Visit :proposal-id 17442 :visit-id "01" :proposal-version -1 :trans-version "20240604" :date "10-Oct-2024 14:58:04.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 202848 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17442 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17442 :visit-id "01" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2696 :al-overhead-at-end 116 :internal-dur-at-end 1244 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3028 :pcs-gap 0 ) true 1 1 S/N > 100 at > 3000 A S/N > 100 at < 9500 A Manual fringe flat used instead of default to get higher S/N. 1728586685415 The scheduling data was generated by CASM 32.1.1. 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Manual fringe flat used instead of default to get higher S/N. 1728586690975 The scheduling data was generated by CASM 32.1.1. 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Manual fringe flat used instead of default to get higher S/N. 1730226212743 The scheduling data was generated by CASM 32.1.3. CASM was run in Phase II mode. /private/var/folders/b9/jx3rgsbx0tgf9j1xp52tw6km0005ml/T/OPVisit10697057236701650567.xml This submission of 2024oct10 is for a repeat of the failed 2nd orbit of Visit 10 per HOPR 92933 of 2024Aug9 & is late, because I just received notification of HOPR approval today. (Tic-Visit :proposal-id 17442 :visit-id "50" :proposal-version -1 :trans-version "20240627" :date "29-Oct-2024 14:23:32.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 166048 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17442 :visit-id "50" :obset-id "50" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17442 :visit-id "50" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2769 :al-overhead-at-end 116 :internal-dur-at-end 1204 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3151 :pcs-gap 0 ) true 1 0 Manual fringe flat used instead of default to get higher S/N. 1728586696313 The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. 1722836033000 135.5034710175645 (Tic-Visit :proposal-id 17442 :visit-id "11" :proposal-version -1 :trans-version "20240604" :date "10-Oct-2024 14:58:16.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 166048 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17442 :visit-id "11" :obset-id "11" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17442 :visit-id "11" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2737 :al-overhead-at-end 116 :internal-dur-at-end 1204 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3119 :pcs-gap 0 ) true 1 0 1728586696812 The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. Repeat of 3rd orbit per HOPR 92872 1722527242000 242.35185875769338 (Tic-Visit :proposal-id 17442 :visit-id "12" :proposal-version -1 :trans-version "20240604" :date "10-Oct-2024 14:58:16.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 166048 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17442 :visit-id "12" :obset-id "12" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17442 :visit-id "12" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2681 :al-overhead-at-end 116 :internal-dur-at-end 1204 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3062 :pcs-gap 0 ) true 1 0 Manual fringe flat used instead of default to get higher S/N.