Changed filters for Visits 22 and 24 to avoid saturation.
----- Attempting Submission 2 (Tue Sep 27 22:35:24 GMT 2011) -----
A Precise Mass-Luminosity-Temperature Relation for Young Stars
The fundamental properties of young stars (masses, luminosities, and temperatures) are very poorly understood in comparison to their older field counterparts. The standard method for calibrating these properties is to monitor the orbits of binary systems and measure their dynamical masses, but only a handful of well-determined dynamical masses are known for low-mass (<1 Msun) stars. We are conducting an ongoing monitoring campaign to expand the sample of precise visual binary masses from ~5 to ~50 using a new high-resolution imaging technique (nonredundant mask interferometry) to monitor very short-period systems that can't be resolved with other techniques. However, the inaccessibility of these systems makes it difficult to determine component properties from the ground.
We propose a 16-orbit WFC3/UVIS imaging campaign to observe 16 systems that are near maximum separation. We know precise component positions at any epoch from our orbit fits, so we can exploit the stable HST PSF to deconvolve the optical photometry for these systems, even though they are separated by <60 mas. Furthermore, the targets' brightness and the speed of the subarrayed WFC3/UVIS let us obtain observations in 11 filters within a single orbit, efficiently characterizing each component's broadband SEDs from the near-UV to the far-red and measuring emission line fluxes in Halpha and Ca H&K. These comprehensive SEDs will yield component temperatures and identify any excesses on the individual stars resulting from accretion and activity. Our results will place the the individual stars unambiguously on the HR diagram, allowing direct comparison of our dynamical masses to theoretical predictions.
The goal of this program is to obtain multicolor images of a large sample of close (<0.06 arcseconds) binary systems. We have orbits for these binary systems from monitoring in the near-infrared, so we can precisely estimate their position/PA at the epoch of the HST images, allowing us to deconvolve out the brightness of each component. The goal is to obtain as many filters per orbit as possible, generally aiming for a peak pixel value of 20% of well depth on most filters, and at least S/N=100 on blue filters and narrowband filters. Our primary concern is making sure that our targets (most of which are bright) do not saturate.
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