----- Submission 1 (Thu May 12 00:29:23 GMT 2005) -----
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Assigned ID: 159
----- Submission 1 (Fri Jan 21 08:26:29 GMT 2005) -----
Phase I Proposal 159 (ultrawds) successfully submitted.
----- Submission 3 (Fri Jan 21 20:57:19 GMT 2005) -----
Resolving Ultracool White Dwarf Binaries
We propose an ACS/HRC imaging survey of the coolest white dwarfs known in order to search for binarity. Current models fail to match observed spectral energy distributions of these sub-4000K stellar remnants, consistently predicting much lower luminosities than observed. A possible explanation is that they are binary in nature. Because these cool degenerates have no spectral features, the only way to investigate their apparent overluminosity is with very high resolution imaging, which can only be done with HST (these stars are far too faint to be observed with adaptive optics on the ground). Optical wavelengths are ideal because the spectral energy distributions of these old degenerates peak near 600 nm. With the F435W filter we will be able to partially resolve equally luminous binaries as close as 0.02", which corresponds to within 0.6 AU for over half of the 12 proposed target stars. The collected data will be critical in determining whether these stars represent the oldest white dwarfs in the solar neighborhood.
We will use the ACS/HRC with the F435W filter to obtain the highest spatial resolution possible while remaining near the peak in the spectral energy distribution of ultracool WDs. All of our targets have magnitudes at B-band less than around 21 mag and we will probe a full 3 magnitudes deeper for companions. In order to remove cosmic rays, hot pixels, detector blemishes, oversample the PSF, and minimize flat fielding errors we will dither 1.5 arcseconds (at 4 positions) as well as obtain two exposures at each dither position. In order to reach B=24 mag with a signal-to-noise ratio of 25, the exposure time calculator indicates a total integration time near 2400 seconds when an observation is split into 8 exposures. Together with the specified overheads, the orbit planner indicates we can reach very near to our depth goal in a single HST orbit. Therefore , we will use our 12 alloted orbits to probe as deeply as possible within each visibility window.
COOL STARS
12
false
0.0
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false
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SUPPORTED
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LATE-TYPE DEGENERATE
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ACS/HRC
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F435W
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F435W
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No
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LINE
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false
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4
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