Establishing a Network of DA White Dwarf SED Standards

Assigned ID: 629 ----- Attempting Submission 1 (Fri Feb 24 19:43:42 GMT 2012) ----- The targets that were not used were in the original list in Phase 1, and given ok by the TAC. We had to limit our targets because of restrictions on number of exposures due to buffer dumps. We want to keep the list of targets as they are. Added FLASH option to UV F360W and F475W exposures with WFC3/UVIS. Shortened other exposures by 5 sec to stay within the 2 orbit/target constraint. Added FlASH option. Visit B9 replaces Visit 09. 23Oct2012: Added FLASH to all visits. Shaved 5 sec off 2 longer exposures in orbits1 of each visit, and added 40s to the short u band single exp in the 2nd orbit of each visit. POS-TARG values in 2nd orbit (for dithering) changed from 0.15 to 1.50 in all visits. All orbits now look alike, except for target. resubmission ----- Attempting Submission 1 (Thu Jun 28 22:31:26 GMT 2012) ----- ----- Attempting Submission 2 (Wed Sep 19 21:12:33 GMT 2012) ----- ----- Attempting Submission 3 (Mon Sep 24 14:35:31 GMT 2012) ----- HST Phase II Proposal 12967 (HSt12967v2012-09-24.apt) successfully submitted. ----- Attempting Submission 4 (Mon Oct 01 18:05:56 GMT 2012) ----- ----- Attempting Submission 5 (Tue Oct 23 22:34:19 GMT 2012) ----- The targets that are not used in Phase II, were in the original Phase 1, and given OK by TAC. We had to limit the number of targets in implementation, because the buffer dumps severely limited the number of exposures we can do in an orbit. (so we made the exposures longer than necessary, but cut the numbers - which means we cannot do all the targets. 6 of the 60 warnings are caused by the above, and are so explained. The remaining 54 warnings are all due to the use of FLASH in WFC3, and is warning about possible leaked like in the other SIs. Not much we can do about that. Will check offline about whether that is likely to affect our ACS parallels -- I expect not, or we'd have known about it already. Establishing a Network of DA White Dwarf SED Standards Systematic uncertainties in photometric calibration are the dominant source of error in current type Ia supernova dark energy studies, as well as other forefront cosmology efforts, e.g. photo-redshift determinations for weak lensing mass tomography. Current and next-generation ground-based all-sky surveys require a network of calibration stars with 1) known SEDs (to properly and unambiguously take into account filter differences), and 2) that are on a common photometric zeropoint scale. HST affords us the ability to establish this essential network of faint primary photometric standards, exploiting the well-understood spectral energy distributions of DA white dwarf stars, without the complications of observing through the time-variable Earth's atmosphere. We have selected an initial set of equatorial DA targets that will have SNR ~200 in the LSST (and PanSTARRS and Dark Energy Survey) survey images, while avoiding saturation. This places primary photometric standards directly into in the multi-epoch all-sky LSST and other simailar databases. By using ground-based spectra, not for spectrophotometry, but to obtain the two parameters (temperature and log(g)) that determine the SED, we can use broadband HST photometry to set the overall flux scale for each source, and determine any applicable reddening. Thus calibrated, these standards can then be used as flux standards at wavelengths well beyond the range of HST, and in any arbitrary, but defined passband. This precision photometric heritage from HST will benefit essentially all existing and upcoming survey projects, and directly addresses one of the current barriers to understanding the nature of dark energy. We originally proposed to observe 15 DA white dwarfs and surrounding fields distributed around the celestial equator with purpose of establishing them as SED standards accessible to telescopes and surveys in both hemispheres. The targets are chosen from SDSS data, which provide an outstanding list of confirmed DA white dwarfs with well considered selection criteria (Prieto et al. 2009). We have adopted two of the sources identified by Prieto et al. (2009) that lie at appropriate declination, supplemented with other confirmed DA's with appropriate temperatures taken from Eisenstein et al. (2006). Our sample is optimal in that it spans a practical range of magnitudes and includes stars with temperatures ranging from 20,000 K to 80,000K. As pointed out in Holberg \& Bergeron (2006) having such a range of temperatures minimizes the possible effects of any temperature-dependent model biases. In Phase-I we asked for18 orbits based on exposure estimates, and nominal overheads. While constructing Phase-II we have been unable to fit all of the observations in because of the inefficiency introduced by data dumps, whose consequences were not clear in Phase-I planning. As a consequence, we have chosen 9 (of the original 15) best targets, and prepared the observing plan accordingly for both primary and parallel observations. We detail the observing descriptions below: PRIMARY OBSERVATIONS We will obtain imaging of our targets with WFC3 in 5 select bands: u,g,r,i and H. Our multiple exposures are designed to allow CR rejection in all bands, and have a small positional offset in all of these pass-bands. This complement of passbands is necessary for our goals. The Stromgren u (F336W) is chosen because it sits entirely shortward of the Balmer Jump (BJ), and so allows a way to measure it. For our targets, the BJ is sensitive to temperature, but in a different way than the Paschen continuum slope. This breaks any degeneracy between reddening and temperature, a critical function for our goal. The specific choice of Sloan g,r,i to measure the Paschen continuum provides a direct measure in bands being used in large surveys today (e.g. SDSS, PanSTARRS) and planned in the future (e.g. Dark Energy Survey with DECam, LSST). The H band anchors measurements as far longward as HST will allow. The exposure times chosen allow for S/N better than 200 for each of the targetted white dwarfs, while staying shorter than half of the time to saturation. The arrangements of the various exposures times (with their respective durations) within an orbit have been specially crafted to allow for the most efficient disposition of the data-dumps. Disrupting this sequence will insert "dead time" between exposures that severely compromise efficiency. The HST/WFC3 system response and CTE corrections needed are regularly monitored by the WFC3 instrument support group (which has Co-I representation on this proposal) to an accuracy of ~ 0.002 mag. We will rely on this to ensure that the observations of our targets are uniform and self-consistent at this level. Other stars in the file of WFC3 will also be calibrated to the HST standardized Sloan u,g,r and i bands, and the near IR H band. Since the WFC3 state of calibration through the standard calibration programs is accurate to 0.002 mag, these additional stars will serve as secondary standards in this system. PARALLEL OBSERVATIONS: In fields adjacent to the WD that the ACS lands on with no prior contraint on ORIENT, we still expect to see several stars brighter than 21, for which S/N better than 100 can be obtained. These will mostly be K dwarfs, but also some G stars, and an occassional F. The original plan to obtain photometry in the SDSS g,r,i,z passbands has been compromised by the afore-mentioned data-dump overhead limitation, and we have chosen to proceed with only the g and i bands. Thes eobservations will give as photometry tied to the current calibration of HST (and ACS in particular), which is based on 3 bright DA white dwarfs. For ground based astronomy concerned about atmospheric extinction effects on measured color, the ACS stars will be observed in the same field, and so simultaneously, as the white dwarfs (ground based FOVs are typically large enough to include the angular separation between WFC3 and ACS). The ACS ETC shows that our planned expsosures will obtain S/N better than 100 for stars at g=21.7 with spectral classes ranging from F0V through M5V. The HST/ACS system reponse and CTE correction prescription are also monitored by the ACS instrument support group, which again has Co-I representation on this proposal. The photometric stability that can be attained is also $\sim .002$ mag, which will ensure adequate photometric uniformity for our coordinated parallel fields.These measurements will supplement the standardization stars in the primary WFC3 fields. Although now limited only to g and i (due to the data dump issue), the ACS photometry will extend deeper, with S/N ~ 100 to nearly g=22. COSMOLOGY 0 false 0.0 4.5 false false false false SUPPORTED STAR DA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 Sloan g =19.1 +/- .05 STAR DA This object was generated by the targetselector and retrieved from the SIMBAD database.This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 Sloan g =19.8 +/- .05 STAR DA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 Sloan g =18.9 +/- .05 STAR DA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 Sloan g =19.7 +/- .05 STAR DA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 Sloan g =18.9 +/- .05 STAR DA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 Sloan g = 18.7 +/- .05 STAR DA J2000 J2000 Sloan g = 17.0 +/- .05 STAR DA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 Sloan g =19.0 +/- .05 STAR DA J2000 J2000 Sloan g =15.7 +/- .05 STAR DA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 Sloan g = 18.8 +/- .05 STAR DA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 Sloan g =18.9 +/- .05 STAR DA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 Sloan g =18.7 +/- .05 STAR DA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 Sloan g = 18.2 +/- 0.05 STAR DA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 Sloan g = 19.7 STAR DA This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F775W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F775W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F775W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F775W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F775W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F775W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F775W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F775W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F775W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F775W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F775W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F775W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F775W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F775W WFC3/IR Imaging No No F160W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F775W WFC3/IR Imaging No No F160W ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W ACS/WFC Imaging No No F850LP ACS/WFC Imaging No No F475W ACS/WFC Imaging No No F625W ACS/WFC Imaging No No F775W ACS/WFC Imaging No No F850LP 1351030390801 The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. /Users/saha/STScI-Cyc20/OP-cache/PH2-V19-v01.xml ORIENT restrictions are to avoid blooming and cross talk from brighter stars on WFC3. 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CASM was run in Phase II mode. /Users/saha/STScI-Cyc20/OP-cache/PH2-V19-v04.xml ORIENT restrictions are to avoid blooming and cross talk from brighter stars on WFC3. 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CASM was run in Phase II mode. /Users/saha/STScI-Cyc20/OP-cache/PH2-V19-v05.xml ORIENT restrictions are to avoid blooming and cross talk from brighter stars on WFC3. 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CASM was run in Phase II mode. /Users/saha/STScI-Cyc20/OP-cache/PH2-V19-v06.xml ORIENT restrictions are to avoid blooming and cross talk from brighter stars on WFC3. 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CASM was run in Phase II mode. /Users/saha/STScI-Cyc20/OP-cache/PH2-V19-v07.xml ORIENT restrictions are to avoid blooming and cross talk from brighter stars on WFC3. 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CASM was run in Phase II mode. /Users/saha/STScI-Cyc20/OP-cache/PH2-V19-vB9.xml ORIENT restrictions are to avoid blooming and cross talk from brighter stars on WFC3. This visit replaces the original Visit 09. Post flash added to the UV exposures. (Tic-Visit :proposal-id 12967 :visit-id "B9" :proposal-version -1 :trans-version "20120604" :date "23-Oct-2012 15:18:55.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 4442208 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12967 :visit-id "B9" :obset-id "B9" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12967 :visit-id "B9" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2680 :al-overhead-at-end 125 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) (Tic-Orbit :proposal-id 12967 :visit-id "B9" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2768 :al-overhead-at-end 124 :internal-dur-at-end 1015 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) true 2 0 1351029827425 The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. /Users/saha/STScI-Cyc20/OP-cache/PH2-V19-v08.xml ORIENT restrictions are to avoid blooming and cross talk from brighter stars on WFC3. 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