0Assigned ID: 464
----- Attempting Submission 1 (Fri Apr 11 13:24:59 GMT 2014) -----Dear Miranda & Hugues,
here is the revised Phase II with the visits 1, 6, 7, and 10 switched to STIS / G140L as per PCR 78976.
(second attempt)
Boris2001970976----- Attempting Submission 1 (Fri Jul 18 15:24:39 GMT 2014) -----
----- Attempting Submission 2 (Thu Nov 13 15:08:03 GMT 2014) -----Testing the single degenerate channel for supernova IaThe progenitors of supernova Ia are close binaries containing white dwarfs. Of crucial importance to the evolution of these systems is how much material the white dwarf can stably accrete and hence grow in mass. This occurs during a short-lived intense phase of mass transfer known as the super soft source (SSS) phase. The short duration of this phase and large extinction to soft X-rays means that only a handful are known in our Galaxy. Far more can be learned from the underlying SSS progenitor population of close white dwarf plus FGK type binaries. Unfortunately, these systems are hard to find since the main-sequence stars completely outshine the white dwarfs at optical wavelengths. Because of this, there are currently no known close white dwarf binaries with F, G or early K type companions, making it impossible to determine the contribution of the single degenerate channel towards supernova Ia. Using the GALEX and RAVE surveys we have now identified the first large sample of FGK stars with UV excesses, a fraction of which are these illusive, close systems. Following an intense ground based spectroscopic investigation of these systems, we have identified 5 definite close binaries, with periods of less than a few days. Here we apply for COS spectroscopic observations to measure the mass and temperature of the white dwarfs in order to determine the future evolution of these systems. This will provide a crucial test for the single degenerate channel towards supernova Ia.The aim of this proposal is to obtain far-ultraviolet COS spectra of white dwarfs in close binary systems with F, G or early K type main-sequence companions in order to measure their masses and determine if they are viable supernova Ia projenitors. Ground based spectroscopy has already been used to determine the masses of the main-sequence stars and the orbital periods, which span from 12 hours to 10s of days. All our targets have good GALEX photometry and are photometrically stable, therefore we have been able to determine the best setup (acquisition and resolution) for each system.
Our observations are straight-forward. Target acquisition, depending on the target brightness, will be done with NUV imaging, or in dispersed light using the G130M grating. At present, the coordinates and proper motions are drawn from the PPMXL catalogue, which has proven to be reliable and accurate to fractions of an arcsec, hence we do not precede the observations with a search pattern. For our faintest object, LAMOST J1445+1236, we will use the lower resolution G140L grating, for all other targets we use the higher resolution G130M grating. We will make use of all 4 FP-POS positions.
One target, TYC 7218-934-1, is particularly interesting as it appears to be an eccentric binary. In order to confirm this we will observe the system twice in order to detect the Doppler shift of the white dwarf and confirm that it is definitely part of the binary (rather than being a wide member of a main-sequence binary). We separate the two observations by ~9 days (2/3rds of an orbit) in order to ensure that the white dwarf will have a Doppler shift between the two observations.HOT STARSDefaultfalsefalsefalsefalsefalseSUPPORTEDSTARCOMPOSITE SPECTRAL TYPEDAF3-F9This object was generated by the targetselector and retrieved from the SIMBAD database.RAVE-J0019-3712J2000J2000FUV=17.961, NUV=15.593STARCOMPOSITE SPECTRAL TYPEDAF3-F9This object was generated by the targetselector and retrieved from the SIMBAD database.RAVE-J0253-7352J2000J2000FUV=16.809, NUV=15.118STARCOMPOSITE SPECTRAL TYPEDAK V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.2MASS-J11222735+5236348J2000J2000FUV=16.268, NUV=16.699STARCOMPOSITE SPECTRAL TYPEDAG V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.RAVE-J1151-3104J2000J2000FUV=17.137, NUV=16.221STARCOMPOSITE SPECTRAL TYPEDAG V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=18.626, NUV=16.886STARCOMPOSITE SPECTRAL TYPEDAF3-F9This object was generated by the targetselector and retrieved from the SIMBAD database.RAVE-J1502-2941J2000J2000FUV=17.754, NUV=15.419STARCOMPOSITE SPECTRAL TYPEDAG V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=14.376, NUV=14.978STARCOMPOSITE SPECTRAL TYPEDAG V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.RAVE-J2013-2951J2000J2000FUV=15.337, NUV=14.732STARCOMPOSITE SPECTRAL TYPEDAF3-F9This object was generated by the targetselector and retrieved from the SIMBAD database.RAVE-J2355-6803J2000J2000FUV=17.746, NUV=14.646COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105/tmp/OPVisit2266316667883468456.xmlThe scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.(Tic-Visit
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