0Assigned ID: 2048
----- Attempting Submission 1 (Fri Apr 09 17:34:13 GMT 2021) -----
HST Phase I Proposal 2048 successfully submitted.
Receipt: # 2048-1
----- Attempting Submission 2 (Fri Apr 09 21:23:51 GMT 2021) -----Updated Jun 3, 2022 - use Gaia DR2 coordinates, PMs and epoch for objects after verifying in target confirmation PDF-1489911663----- Attempting Submission 1 (Thu Jul 29 15:05:17 GMT 2021) -----
HST Phase II Proposal 16764 successfully submitted.
Receipt: # 16764-1
----- Attempting Submission 2 (Fri Jul 30 15:23:59 GMT 2021) -----
----- Attempting Submission 3 (Mon Aug 30 19:55:53 GMT 2021) -----
HST Phase II Proposal 16764 successfully submitted.
Receipt: # 16764-3
----- Attempting Submission 4 (Wed Sep 01 18:34:50 GMT 2021) -----
----- Attempting Submission 5 (Fri Jun 03 15:55:06 GMT 2022) -----
HST Phase II Proposal 16764 successfully submitted.
Receipt: # 16764-5
----- Attempting Submission 6 (Fri Jun 03 20:21:21 GMT 2022) -----Ralph Bohlin will verifyThe Stars Like Dust: Inferring a Probabilistic Extinction Law from STIS UV Spectroscopy of the Cosmic Flux StandardsOur understanding of dust, encoded in our knowledge of the extinction law, is one of the leading sources of systematic bias impacting cosmology today. We propose to measure the extinction law, and its variation, directly through STIS FUV and NUV spectroscopy of 21 faint white dwarf stars, the Cosmic Flux Standards. These standards have SEDs that are exceptionally well-constrained by high S/N legacy HST panchromatic imaging, detailed ground-based optical spectroscopy, and temporal monitoring to assess variability. These Cosmic Flux Standards extend the CALSPEC system down to V~19.5 mag, and has been demonstrated that measurements of these standards will allow 1% absolute photometric calibration and 0.5% relative calibration, suitable for major upcoming projects such as the Vera Rubin Observatory and Nancy Grace Roman Space Telescope. These observations will allow a direct measurement of the extinction law by comparing the STIS spectrophotometry to the unreddened SEDs of the Cosmic Flux Standards, allowing a population inference of the extinction law, as well as line-of-sight estimates to each object. This probabilistic model of the extinction law will directly address dust as a source of systematic error, and the STIS FUV and NUV observations will also extend the validity of the standards to 1,150 Angstrom in preparation for future UV space-missions.The observational sample for this proposal is selected from the Cosmic Flux Standards set of DAWDs. The selection critiera are A_V values from 0 to 1, and observed F275W mag (AB) between 15-18 mag. ETC values for the MAMA gratings are calculated by using the STIS ETC v29.1.1. The CALSPEC spectrum for GD153 is the template, normalized to the F275W magnitude and extinction for each target, using R_V =3.1. Default background values and settings are used.
STIS FUV-MAMA Observations Spectra will be obtained with the G140L grating, the 52x2 arcsec slit, covering the wavelength range between 1150 Angstrom and 1700 Angstrom, R=1000 (0.6 Angstrom/pixel). Exposure times are estimated for SNR 20 at 1500 Angstrom (per resolution element).
Exposure times for the DAWDs are between 100 seconds and 900 seconds, except for the faintest source, at 1600 seconds.
STIS NUV-MAMA Observations Spectra are with the G230L grating and the 52x2 arcsec slit, covering the wavelength range between 1570 Angstrom and 3180 Angstrom with R=500 (1.58 A/pixel). The ISM UV bump at 2175 A is near the middle of the spectral region. Exposure times are estimated for SNR 20 at 2200 Angstrom (per resolution element). These SNRs of 100 per 100 Angstrom bin are sufficient for the purpose of quantifying the UV bump, i.e., measuring its profile and fitting the observed UV SED with stellar model plus reddening.Collectively, the team has expertise in stellar astrophysics, cosmology with Type Ia supernovae (SNe Ia), the
cosmological distance scale, large surveys and photometric calibration. Team members are experienced in the observation, reduction and analysis of ground and space-based imaging and spectroscopy, and have expertise in the establishment of flux standard stars. The team includes well known WD stellar atmosphere experts Drs. Rauch and Hubeny, ISM astronomer Dr. Points, supernova investigators Drs. Matheson and Rest, LSST scientist Dr. Axelrod, and HST scientists Drs. calamida, Bohlin, MacKenty and Sabbi.
Primary investigators for this proposal are:
Dr. Bohlin, STScI calibration scientist since 1982 who has worked on absolute flux calibrations for over forty
years, and developed CALSPEC.
Dr. Calamida, STSCI scientist and WFC3 deputy branch manager, lead author of one paper on the DAWD Cosmic Flux Standards, and whose main scientific interests are studying the advanced phases of stellar evolution in old stellar populations and photometric calibration.
Dr. Deustua, is an astrophysicist and STScI calibration scientist who has for a long time been addressing the calibration needs for dark energy science, and cross-calibration of large surveys and missions in astronomy. She is a member of one of the teams that discovered the accelerating expansion of the universe, with expertise on the impact of instrument systematics on supernova measurements, and is PI of the NISTStars absolute flux calibration project.
Dr. Holberg, expert on white dwarf models with considerable experience observing white dwarfs in the UV,
with such missions as IUE, FUSE, EUVE, and HST.
Dr. Narayan works on understanding the properties of dark energy using SNe Ia surveys, as well as working on photometric calibration and is the lead author of two papers on the DAWD Cosmic Flux Standards.
Dr. Olszewski is an expert on stellar photometry and spectroscopy. He led the effort to discover and observe
spectroscopically the Southern white dwarfs used in this work.
Dr. Saha, well known for research on the cosmological distance scale as well as variable stars and stellar
populations, and, PI of three HST proposals (15113, 13711,12967) to develop a network of faint, WD standard
stars, upon which effort this proposal is based.
Dr. Stubbs is an astrophysicist who has long been pursuing methods to enhance spectrophotometric calibration of astronomical measurements. He was a member of one of the teams who discovered the accelerating cosmic expansion, and is keen to improve our ability to understand the nature of dark energy. This entails addressing calibration issues that dominate the systematic error budget for using type Ia SNe to map out the expansion history.Stellar Physics and Stellar TypesIntergalactic Medium and the Circumgalactic Medium6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTARDAWDONOJ2000J2000STARDAWDONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARDAWDONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARDAWDONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARDAWDONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARDAWDONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARDAWDONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARDAWDONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARDAWDONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARDAWDONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARDAWDONOJ2000J2000STARDAWDONOJ2000J2000STARDAWDONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARDAWDONOJ2000J2000STARDAWDONOJ2000J2000STARDAWDONOJ2000J2000STARDAWDONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARDAWDONOJ2000J2000STARDAWDONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARDAWDONOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARDANOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/NUV-MAMASpectroscopicNoNoG230L2376The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.(Tic-Visit
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