0 Assigned ID: 3758 ----- Attempting Submission 1 (Fri Mar 25 23:56:02 GMT 2022) ----- HST Phase I Proposal 3758 successfully submitted. Receipt: # 3758-1 ----- Attempting Submission 2 (Sat Mar 26 00:02:04 GMT 2022) ----- HST Phase I Proposal 3758 successfully submitted. Receipt: # 3758-2 ----- Attempting Submission 3 (Sat Mar 26 00:21:47 GMT 2022) ----- HST Phase I Proposal 3758 successfully submitted. Receipt: # 3758-3 ----- Attempting Submission 4 (Sat Mar 26 00:41:42 GMT 2022) ----- HST Phase I Proposal 3758 successfully submitted. Receipt: # 3758-4 STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS STIS EXPOSURE TIME ROUNDED DOWN TO NEAREST 0.1 SECONDS 2023-August-02: Removed 90s from science exposure time in visit 03 and 90s from the science exposure in visit 04 (03.003 and 04.003) in order to relax scheduling contraints given ORIENT updates. 351348852 ----- Attempting Submission 1 (Fri Jul 15 06:10:39 GMT 2022) ----- HST Phase II Proposal 17092 successfully submitted. Receipt: # 17092-1 ----- Attempting Submission 2 (Wed Jul 20 00:15:48 GMT 2022) ----- ----- Attempting Submission 3 (Fri Jul 28 12:53:07 GMT 2023) ----- HST Phase II Proposal 17092 successfully submitted. Receipt: # 17092-3 ----- Attempting Submission 4 (Fri Jul 28 12:59:14 GMT 2023) ----- HST Phase II Proposal 17092 successfully submitted. Receipt: # 17092-4 ----- Attempting Submission 5 (Wed Aug 02 14:57:13 GMT 2023) ----- All warnings related to automatic rounding down of exposure times due to CR-SPLITS by 0.1s, and should not impact program goals or execution. The Space Telescope Imaging Spectrograph (STIS) is currently the world's only available visible-light coronagraphic spectroscopy facility. The unique capabilities of R~500 optical spectroscopy at close angular separation (0.05-0.3") from a bright central object has been relatively unexplored with this mode and to-date are not yet fully calibrated. The goal of this program is to assess the achievable contrast, inner working angle, and fidelity of extracted spectra using the occulting fiducial F1 bar in the STIS 52x0.2 spectroscopic aperture. Targets will be two well-measured single A0V standard stars, in addition to a binary white dwarf companion system and PSF reference, wherein the faint companion has published images and low-resolution spectra against which STIS observations will be compared. Use of target offsets from the nominal bar acquisition positions, pushing the star as close as possible to the edge of the occulter, will allow us to determine the limits of coronagraphic performance achievable with this mode. The driving science benefit to the community is to provide well-calibrated contrast curves, an understanding of the noise properties and quality of extracted spectra in this mode. These measurements would have immediate utility for programs involving spectroscopy of imaged exoplanets, brown dwarfs, and close binary companions; circumstellar disks; jet-launching regions in young protostars; and AGN jets and host environments (i.e., any scientific case where optical spectra at very small angular separations are of interest). The proposed program will explore and calibrate the full capabilities of this unique mode made possible only with HST/STIS. ----------------------------- Overview ----------------------------- This calibration program involves six orbits to measure and calibrate the performance of the coronagraphic spectroscopy mode of STIS, via two main experiments: 1) Contrast Test: This experiment serves to determine the achievable contrast of the coronagraphic spectroscopy mode, involving observations of two early-type (A2V) stars, TYC 1262-187-1 and HD283593. These stars will each be acquired in imaging mode, then placed within the fiducial 52x0.2F1 aperture behind the F1 coronagraphic occulting bar. Then, each star will be offset toward the edge of bar by 100 mas or 200 mas using POS-TARGs, and deep observations will be taken in order to determine the sensitivity of the extracted spectra at close angular separation from the star. The stars will need to be observed in a standard coronagraphic sequence, i.e., in adjacent orbits. This is required to minimize the effects of breathing due to thermal fluctuations across the telescope structure, which has significant effects on PSF quality. The two observations will be used as calibration observations (PSF references) for each other in order to subtract the starlight in each exposure and allow deep observations of the circumstellar surroundings, and thus they may be observed in any order. 2) Spectral Extraction Test: This experiment is designed to assess the fidelity of the extracted spectra at close angular separation (0.45") from the star. The target is a binary system consisting of a G-type star (HD114174) and its well-characterized white dwarf companion. The primary G-type star will be placed at the fiducial 52x0.2F1 position behind the bar with a designated ORIENT angle to place the white dwarf companion within the spectroscopic slit. Along with the binary, a PSF reference target of similar spectral type (HD115692) will be observed to subtract the PSF and recover the spectrum of the white dwarf by removing contributed starlight from the primary G-star behind the coronagraphic bar. ----------------------------- 2) Visit Structure ----------------------------- For the Contrast Test, we will obtain deep observations of each star at two separate POS-TARG offset positions. Given that the targets are isolated stars, no specific ORIENT angles are required. The observations are designed to be executed in subsequent orbits. For the Spectral Test, the binary system must be observed in subsequent orbits with the PSF reference. ----------------------------- ORIENT Constraints ----------------------------- This visit involves placing a close faint white dwarf companion to the primary star within the slit. The companion is predicted to be at a position angle of 178.5 deg and separation of ~0.45 arcsec (as of August 2023 based upon RV and astrometric orbital analysis, including an imaging epoch as recent as July 2022 with JWST), and the companion is moving closer to the primary star. Given the 45 deg relative angle of the STIS detector to the +U3 axis and the additional 1.3 deg offset to the 52x0.2F1 slit, we therefore request the ORIENT constraint to be within one of two sets of possible 20 degree ranges to place the companion either directly above or below the occulting bar within the slit (~225 +/- 10 deg. or ~45 +/- 10 deg., respectively). ----------------------------- Guide Stars ----------------------------- For stability with the PSF reference subtraction in both experiments, we require pointing and roll control with 2-FGS guiding. Single-FGS guiding is not sufficiently stable to perform PSF subtraction for coronagraphic spectroscopy. Dr. Kimberly Ward-Duong is an expert in high contrast imaging of stellar and substellar companions using both traditional and extreme AO on the ground and space-based observations. Her research has involved spectroscopy of low-mass stars, brown dwarfs, and exoplanets over wavelengths ranging from the NUV into the submillimeter, and she has significant experience working with the various coronagraphic modes of STIS as a previous STIS team member. Dr. John Debes has 10+ years of experience working on high contrast imaging of STIS, and over four years of experience working as manager of the STIS Instrument Branch at STScI. He is familiar with the detailed workings of STIS imaging and spectroscopic modes and will help with the Phase II design. Dr. Jonathan Aguilar is a staff scientist supporting coronagraphy for the MIRI instrument on JWST. He is an expert in both ground and space-based high-contrast imaging efforts, including P1640 and HST, and has extensive knowledge of post-processing pipelines to optimize high-contrast observations. William Balmer is a graduate student at the Johns Hopkins University studying high contrast observations of exoplanets and sub-stellar objects with Dr. Laurent Pueyo at the Space Telescope Science Institute. They have experience in optical/NIR photometry, spectroscopy, and interferometry. Dr. Katherine Follette is a leading expert in the field of direct imaging of accreting protoplanets and the search for young planets forming in transition disk systems. She has extensive experience working on the high contrast imaging of these systems, particularly in H-alpha observations. Jingyi Zhang is an undergraduate student whose research focuses on calibrating archival data using similar spectroscopic modes on STIS. She is working closely on the data reduction pipeline processing for STIS coronagraphic observations and post-processing and is working on finding new approaches to extract spectra. Exoplanets and Exoplanet Formation Exoplanets and Exoplanet Formation 0 true false false false false false false false SUPPORTED STAR F0-F2 This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 STAR A0-A3 V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR DC G V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR G V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. HD114174-PSF-REF J2000 J2000 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G750L 7751 1690522663073 /Users/kim/Research/Proposals/2022_HST_Cycle30/CS_calibration/OP-cache/STIS_CS_Calibration_PhaseII_v4-revJul2023-v01.xml Timing link suitability includes constraints ([Group (01 02) Within 0.3 days]) The scheduling data was generated by CASM 31.0. CASM was run in Phase II mode. (Tic-Visit :proposal-id 17092 :visit-id "01" :proposal-version -1 :trans-version "20220630" :date "28-Jul-2023 01:37:20.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 258064 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17092 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17092 :visit-id "01" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2764 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3157 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17092 :visit-id "01" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2764 :al-overhead-at-end 0 :internal-dur-at-end 561 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3157 :pcs-gap 0 ) true 2 0 Using the E1 pseudo-aperture to avoid CTE effects. 1690523753197 /Users/kim/Research/Proposals/2022_HST_Cycle30/CS_calibration/OP-cache/STIS_CS_Calibration_PhaseII_v4-revJul2023-v02.xml Timing link suitability includes constraints ([Group (01 02) Within 0.3 days]) The scheduling data was generated by CASM 31.0. CASM was run in Phase II mode. (Tic-Visit :proposal-id 17092 :visit-id "02" :proposal-version -1 :trans-version "20220630" :date "28-Jul-2023 01:55:39.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 294864 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17092 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17092 :visit-id "02" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2768 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3165 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17092 :visit-id "02" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2769 :al-overhead-at-end 0 :internal-dur-at-end 580 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3165 :pcs-gap 0 ) true 2 0 Using the E1 pseudo-aperture to avoid CTE effects. 1690980188954 /private/var/folders/mv/dnh3zwd138x8994mysrnnsch0000gn/T/OPVisit16477060446145340734.xml Timing link suitability includes constraints ([Group (03 04) Within 0.1 days]) The scheduling data was generated by CASM 31.0. CASM was run in Phase II mode. This visit involves placing a close faint white dwarf companion to the primary star within the slit. The companion is predicted to be at a position angle of 178.5 deg and separation of ~0.45 arcsec (as of August 2023), and is moving closer to the primary star. Given the 45 deg relative angle of the STIS detector to the +U3 axis and the additional 1.3 deg offset to the 52x0.2F1 slit, we therefore request the ORIENT constraint to be within one of two sets of possible 20 degree ranges to place the companion either directly above or below the occulting bar within the slit (~225 deg. or ~45 deg., respectively). (Tic-Visit :proposal-id 17092 :visit-id "03" :proposal-version -1 :trans-version "20220630" :date "02-Aug-2023 08:42:48.0" :trans-errors '(:WARNINGS 10 :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 239648 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17092 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17092 :visit-id "03" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2661 :al-overhead-at-end 0 :internal-dur-at-end 640 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3145 :pcs-gap 0 ) true 1 0 Using the E1 pseudo-aperture to avoid CTE effects. 1690980269630 /private/var/folders/mv/dnh3zwd138x8994mysrnnsch0000gn/T/OPVisit18374999338650226293.xml Timing link suitability includes constraints ([Group (03 04) Within 0.1 days]) The scheduling data was generated by CASM 31.0. CASM was run in Phase II mode. (Tic-Visit :proposal-id 17092 :visit-id "04" :proposal-version -1 :trans-version "20220630" :date "02-Aug-2023 08:44:17.0" :trans-errors '(:WARNINGS 0 :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 129232 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17092 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17092 :visit-id "04" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2662 :al-overhead-at-end 0 :internal-dur-at-end 640 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3145 :pcs-gap 0 ) true 1 0 Revised 2023-07-27 to use F25ND3 aperture based upon corrected ETC calculations Using the E1 pseudo-aperture to avoid CTE effects.