Sept 9, 2014: This is a further revised submission. Visits not already scheduled have been given time windows so that the visits to the bright calibrators (vists 51,52,53, 61-3, an 71-73 can be
taken at appropriate times over the course of the obsevations of the "unknowns". This was done at the advice of the schedulers and proposal coordinator at STScI.
This is a revised submission. The changes were primarily motivated to minimize the usage of the WFC3
CSM mechanism. The rearrangement of exposures necessitated related changes, most significantly a change in the strategy for the coordinated parallels, since the rearrangement of
primary visits forces new constraints on the buffer dumps from the parallel ACS exposures.
changed subarray for H-band images of standard stars to increas the number of NSAMP, while keeping
total observing time the same-1709146907----- Attempting Submission 1 (Wed Jul 23 00:25:37 GMT 2014) -----
----- Attempting Submission 2 (Mon Aug 25 20:34:57 GMT 2014) -----
----- Attempting Submission 3 (Wed Aug 27 13:48:53 GMT 2014) -----
----- Attempting Submission 4 (Mon Sep 08 19:46:59 GMT 2014) -----Establishing a Network of Next Generation SED standards with DA White DwarfsPhotometric calibration uncertainties are the dominant source of error in current type Ia supernova dark energy studies, and other forefront cosmology efforts, e.g., photo-redshifts for weak lensing mass tomography. Modern 'all-sky' surveys require a network of calibration stars with 1) known SEDs (to properly and unambiguously account for filter differences), and 2) that are on a common photometric zero-point scale. HST enables us to establish this essential network of faint spectrophotometric standards, by eliminating the time-variable Earth's atmosphere, and by exploiting the well-understood energy distributions of DA white dwarfs. We have selected a set of DA WD targets that will have SNR ~200 in the LSST (and PanSTARRS and Dark Energy Survey) survey images, while avoiding saturation. This means they will be included in the surveys, and will directly calibrate the data products. By using ground-based spectra of Balmer lines 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 benefits essentially all existing and upcoming surveys, standardizes (spectro)photometry across observatories and facilities, and directly addresses one of the current barriers to understanding the nature of dark energy. In our Cycle 20 program we achieve sub-percent accuracy. Here we propose improvements in experimental design from lessons learned.Experimental Procedure:
1. Obtain WFC3 photometry on the system of Bohlin DA white dwarf standards of our faint prospective white dwarf standard stars in several bands ranging from the near UV through the near IR, which is the spectral region maximally sensitive to temperature and gravity in the star.
2. Obtain and analyze ground based spectra of these proto-standard white dwarfs: from Balmer line fits derive Te and log g using the same models used for the Bohlin standards. Using the SEDs predicted by the same models, synthesize the photometry in the observed pass-bands to obtain the intrinsic Spectral Energy Distribution (SED) of the star.
3. Compare the observed and synthetic photometry from 1) and 2) above. They should match for each prospective white dwarf standard, allowing ony for a) a small reddening adjustment due to interstellar extinction, and b) a single common zero-point shift for all bands. Binarity of (or presence of orbiting debris in) the white dwarf can drive a mis-match: observed magnitudes will be relatively brighter than the synthetic values in the red.
Primary Targets:
We have 3 classes of targets:
A) The 9 targets we observed in Cycle 20, for which we need (and have been awarded) some additional observations as stated in our Phase 1 proposal. These are done in visits lasting only 1 orbit. In this Phase-2 proposal they are to be found in Visits 20 through 28.
B) The 14 additional targets awarded in Cycle 22, which are 3 orbits in duration. These are in Visits 01 through 14 in this Phase 2 proposal.
C) Observations of the 3 Bohlin SED standards for monitoring WFC3 response through the duration over which this program executes. Each of the 3 targets is to be observed 3 times (with one orbit visits) totalling 9 visits: once near the beginning of the observing program, once when about half the other targets have been observed, and finally near or right after all the other targets have been observed. The visits for these observations are to be found in Visits 51-53, 61-63, and 71-73. We have put in timing requirements using the "AFTER nn by TT" construction for the visits, on the assumption that it will take about 1.5 years to get all the observations. But the driving principle is what is stated here.
Primary Observations:
We propose to obtain imaging of our targets with WFC3 in select bands: Sloan gri, Stromgren u, F275W, and the near-ir H band. We seek to attain S/N of 200 or better in each passband. This complement of passbands is necessary for our goals. The Stromgren u sits clear of the Balmer Jump, and the specific choice of Sloan gri to measure the Paschen continuum provides a direct measure in bands being used in large surveys today (e.g. SDSS, PanSTARRS, Dark Energy Survey with DECam, and in the future, LSST). The H band anchors measurements as far longward as HST will allow. The F275W passband will alert us to cases where there may be non-standard reddening - which if left unaccounted for, would make any UV extrapolation of the arriving SED less reliable.
Orient constraints: some of our targets are as faint as 19 mag, and because we are trying to get the highest possible s/n, we have put in ORIENT constraints so that brighter objects that fall on the same detector do not "bleed" onto our primary white dwarf target or surrounding pixels.
The Parallel Observations:
In the adjacent ACS fields, with no prior constraint on ORIENT, we 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. With such parallel observation, we will obtain photometry in the SDSS g, r, and i passbands, tied to the current calibration of HST (based on the 3 bright Bohlin SED standard DA white dwarfs ): this does not cause any overflow in the orbits required (which are based solely on the primary observations). For ground based imaging concerned about atmospheric extinction effects on measured color, the ACS stars as well as the DA-WD standard and stars around it will typically be observed simultaneously in the same image (FOVs of ground based survey facilities are large enough for this). The ACS exposures are longer (fewer passbands) and so go deeper than the WFC3 observations. Thus these extra stars from the ACS field will more than double the number of usefully measured stars, especially for tracking gray extinction and aerosol effects from the ground. The photometric stability that can be attained is ~.002 mag, ensuring adequate photometric uniformity for our target fields.DefaultfalsefalsefalsefalsefalseSUPPORTEDSTARDAJ2000Sloan r = 19.8STARDAJ2000Sloan r=19.7STARDAJ2000Sloan g=16.4STARDAJ2000Sloan g=15.7STARDAJ2000Sloan g=19.6STARDAJ2000Sloan r=18.44STARDAThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000STARDAThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000STARDAThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000STARDAJ2000Sloan r=19.1STARDAJ2000Sloan r=18.9STARDAJ2000B=18.2STARDAJ2000Sloan r=18.9STARDAJ2000Sloan r=18.7STARDAJ2000Sloan r=19.0STARDAJ2000Sloan r=18.8STARDAJ2000Sloan r=18.7STARDAJ2000STARDAJ2000Sloan g=18.36STARDAJ2000Sloan g=17.98STARDAJ2000Sloan g=17.85STARDAJ2000Sloan g=18.40STARDAJ2000Sloan g=17.71STARDAJ2000Sloan g=17.45STARDAJ2000Sloan g=16.50STARDAJ2000Sloan g=18.06The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode./Users/saha/HSTPROP/C22/PHASE2/REWORK/OP-cache/Rev3_go13711-vP1.xml(Tic-Visit
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Visit 52 should be done when about half the visits from 01 thru 28 have been executed,
and Visit 53 should be done as close as possble to the execution of the last of the visits from visits 01 thru 28.
The "AFTER ... BY ... " constructions in visits 52 and 53 assume a total observational timeline of 1.5 years. This comment describes our need better than (and supercedes) the "AFTER ... BY ... " requirements.1410185424000267.5748693775962(Tic-Visit
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