Assigned ID: 363 ----- Attempting Submission 1 (Fri Feb 25 14:28:26 GMT 2011) ----- Visit 02 (HD 2133) has been updated based on our recent WFC3 image of the binary, and can now be taken off hold. -- by CoI H. E. Bond 4/11/2012 Visit 06 (HD 217411) has been updated based on our recent WFC3 image of the binary, and can now be taken off hold. -- by CoI H. E. Bond 6/12/2012 Target 1 (Sirius B): the position has been corrected more rigorously for parallax, and the effective proper motion has been updated for the anticipated observation date in February 2013. -- by CoI H. E. Bond 6/13/12 ----- Attempting Submission 1 (Tue Jul 12 03:28:15 GMT 2011) ----- ----- Attempting Submission 2 (Mon Jul 25 10:10:41 GMT 2011) ----- HST Phase II Proposal 12606 (sirius_like.apt) successfully submitted. ----- Attempting Submission 3 (Mon Jul 25 10:14:53 GMT 2011) ----- ----- Attempting Submission 4 (Mon Feb 13 22:41:59 GMT 2012) ----- HST Phase II Proposal 12606 (12606.apt) successfully submitted. ----- Attempting Submission 5 (Wed Feb 15 01:50:15 GMT 2012) ----- HST Phase II Proposal 12606 (12606.apt) successfully submitted. ----- Attempting Submission 6 (Thu Feb 16 20:42:53 GMT 2012) ----- HST Phase II Proposal 12606 (12606.apt) successfully submitted. ----- Attempting Submission 7 (Sun Feb 26 01:17:26 GMT 2012) ----- ----- Attempting Submission 8 (Sun Mar 11 00:38:48 GMT 2012) ----- ----- Attempting Submission 9 (Thu Apr 12 00:05:27 GMT 2012) ----- ----- Attempting Submission 10 (Wed Jun 13 00:07:58 GMT 2012) ----- ----- Attempting Submission 11 (Wed Jun 13 22:43:08 GMT 2012) ----- Targets were checked previously. This is only a resubmission with very minor changes. White dwarfs (WDs) are the remnants of all stars with initial masses less than 8Msun, and they provide important laboratories for the study of evolutionary processes and the behaviour of matter at extremes of temperature and density. Knowledge of the WD ages is also important in measuring the ages of stellar populations. However, such results depend on a thorough understanding of the evolution of WDs themselves and on predictions of the cooling rates. In turn, the masses, radii, and photospheric compositions affect these rates. We propose STIS observations of a sample of white dwarfs in resolved binary systems, for which Sirius B is the prototype, to obtain Balmer line profiles from which we can measure the effective temperature and surface gravity of each star. In addition, we will obtain an accurate radial velocity from the cores of the Halpha lines. These observations will provide improved fundamental information for each white dwarf yielding: a) the gravitational redshift and b) the optical flux normalization. Together these data will provide accurate mass and radius determinations. For Sirius B, in particular, it means the uncertainty in the spectroscopic mass will be on a par with that of the astrometric mass. By reducing the uncertainties in the V magnitude, log g and gravitational redshift to our expected levels, we find that spectroscopic mass and radius uncertainties will be respectively reduced to 3 per cent and 1.6 per cent. At these levels we can precisely test the theoretical M-R for the white dwarfs, distinguishing between a thick or thin H layer for the star and categorically rule out non-C/O core compositions. We are obtaining spectra of the Balmer lines of the white dwarf companions in 5 Sirius-like binaries (which are close visual binary systems consisting of a white dwarf and a bright main-sequence star). The STIS spectra will be obtained using the G430L and G750M gratings with the CCD detector. The G430L grating provides complete coverage of the Balmer line series from HBeta, yielding a resolution of 5.4 Angstroms which will be used for the determination of accurate Teff and log g of the white dwarf. The G430L grating does not yield adequate resolution (170km s-1 per pixel) for a sufficiently accurate radial-velocity measurement. Therefore, we will also obtain a pair of G750M exposures using the 52x2.0 arcsecond and 52x0.05 arcsecond slits, centered on Halpha, to obtain accurate radial velocities and photometry as discussed in the Scientific Justification, for both Sirius B and HD 2133. The 0.56 Å/pixel spectral resolution of the grating translates into 30km/s in velocity space and cross-correlation techniques can be used to improve the accuracy beyond this by a factor 10. The remaining three targets are more challenging with binary separations too small to use the standard slits without serious contamination from the primary. In these cases we will obtain our spectroscopic observations with the 52x0.2F1 setting, placing the primary behind the smaller of the two occulting bars, to provide the scattered light rejection we need. We will need S/N greater than 40 for the Teff and log g measurements as well as the radial velocity. Individual exposures can be easily obtained in one orbit of HST time, yielding a total request (with overheads) of 2 orbits for each target except Sirius B (1 orbit). For these close binaries where we cannot rely on useful STIS spectrophotometry, we will instead obtain WFC3 UVIS images for accurate photometry, with the F336W, F275W, F218W filters, where the contrast between the primary and secondary are substantially reduced. These magnitudes will be used to establish the photometric radii of the WDs. The separations of the targets are (with the exception of Sirius B) challenging. To optimise the contrast for observations of each star we place a long slit perpendicular to the line joining the two stars, so that the scattered-light component can be determined and subtracted directly. The field will be acquired using the primary stars and we will then do a blind offset to each white dwarf, based on our accurate astrometry of the previous WFPC2 frames obtained in our various astrometric programmes and perform a peak-up on that to optimise its location in the narrow slit. The WFC3 UVIS images will be obtained by selecting a roll angle to prevent diffraction spikes from the saturated primary falling onto the white dwaf. For the STIS observations, we will use the 5x0.2F1-R setting and information from the WFC3 images to place the primary behind the occulting bar to allow uncontaminated observations of the white dwarf. To optimize the contrast for observations of each star we need to place a long slit perpendicular to the line joining the two stars (as demonstrated for Sirius B), so that the scattered light component can be determined and subtracted directly. We will be able to calculate the appropriate orientations from our previous WFPC2 images of the systems. HOT STARS 12 false 0.0 0.0 false false false false SUPPORTED STAR DA The RA and Dec of Sirius B are measured from WFC3 frames taken in 2011 October (epoch 2011.748) and corrected for parallax. The proper motion given here is the "effective" proper motion calculated by combining the Hipparcos motion of the center of mass of the Sirius system with the motion of Sirius B in the binary relative to the center of mass at an early 2013 epoch. HD-48915B WD0642-166 J2000 J2000 B=8.41 STAR DA F3-F9 Coordinates determined from WFPC2 frame taken in 1999. J2000 J2000 STAR DA This is the white dwarf companion of 14 Aur Ca. Offset measured from WFPC2 frame taken in 1999. J2000 STAR DA Target offset updated 4/11/12 based on recent WFC3 image. - CoI H. E. Bond J2000 STAR DA The offsets were updated on 2/16/12, based on measurements of a direct WFC3 image obtained in November 2011. -- CoI H. E. Bond HD27483B WD0418+137 J2000 STAR F3-F9 J2000 STAR F3-F9 HD27786 GSC2-NCE5031521 J2000 STAR DA J2000 J2000 STAR F3-F9 NA01007297 HD27483 J2000 STAR DA Target offsets updated based on measurements of recent WFC3 images obtained in this program. -- CoI H. E. Bond 6/12/12. STIS/CCD Spectroscopic No No G750M 6581 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750M 6581 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750M 6581 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750M 6581 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750M 6581 STIS/CCD Spectroscopic No No G430L 4300 WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F218W WFC3/UVIS Imaging No No F275W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F218W WFC3/UVIS Imaging No No F275W WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F218W WFC3/UVIS Imaging No No F275W POS-TARG DITHER 0.173 LINE 0.112 false true 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 1 false POS-TARG DITHER 0.40624 LINE false true 4 90.0 STIS-ALONG-SLIT 2 false POS-TARG DITHER 0.40624 LINE false true 2 90.0 STIS-ALONG-SLIT 3 false POS-TARG DITHER 0.40624 LINE false true 3 90.0 STIS-ALONG-SLIT 4 false The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. 1339625228478 /var/tmp/OPVisit2378921868073684781.xml SIRIUS B observation We know the position of Sirius B, about 9" away from Sirius A, so we go directly to Sirius B without offsetting from Sirius A. Consists of an acquisition image of Sirius B, a spectrum in G430M, a spectrum in G750M, an acquisition peakup in G750M, and a spectrum in G750M with slit of 0.05" ORIENT requirements are to place Sirius B halfway between the diffraction spikes of Sirius A (Tic-Visit :proposal-id 12606 :visit-id "01" :proposal-version -1 :trans-version "20120604" :date "13-Jun-2012 18:07:02.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 277024 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12606 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12606 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2701 :al-overhead-at-end 0 :internal-dur-at-end 379 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3244 :pcs-gap 0 ) true 1 0 1339625237280 The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. /var/tmp/OPVisit4085592575936798620.xml HD 2133 A and B observation. We use an ORIENT that places the slit perpendicular to the line joining the stars. We first acquire the bright HD 2133 A, and then do a dispersed peakup on A. We then do a blind offset to take spectra of B with the G430L and G750M gratings. ORIENTs updated 4/11/12 based on recent WFC3 images. - CoI H. E. Bond (Tic-Visit :proposal-id 12606 :visit-id "02" :proposal-version -1 :trans-version "20120604" :date "13-Jun-2012 18:07:15.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 110832 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12606 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12606 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3047 :al-overhead-at-end 0 :internal-dur-at-end 419 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3381 :pcs-gap 0 ) true 1 0 1339625263130 The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. /var/tmp/OPVisit5496646532704281606.xml HD27786B -2 Imaging in 3 filters with WFC3. Filters are F336W, F218W, F275W ORIENTs are specified to place white-dwarf companion away from diffraction spikes and bleeding column from bright primary 1330465580000 73.0 (Tic-Visit :proposal-id 12606 :visit-id "03" :proposal-version -1 :trans-version "20120604" :date "13-Jun-2012 18:07:36.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 183056 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12606 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12606 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2883 :al-overhead-at-end 40 :internal-dur-at-end 237 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3267 :pcs-gap 0 ) true 1 0 1339625275265 The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. /var/tmp/OPVisit3486927461687761017.xml 14 Aur Cb STIS observation Acquire bright star 14 Aur Ca. Offset to faint companion and do acq peakup. Obtain spectra in G750M (0.5" and 0.05" slits) and G430L (0.5" slit). ORIENT specification is to place slit perpendicular to line joining the two stars. (Tic-Visit :proposal-id 12606 :visit-id "04" :proposal-version -1 :trans-version "20120604" :date "13-Jun-2012 18:07:51.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 147696 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12606 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12606 :visit-id "04" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2826 :al-overhead-at-end 0 :internal-dur-at-end 379 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3160 :pcs-gap 0 ) true 1 0 1339625304195 The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. /var/tmp/OPVisit633223757518179435.xml HD 217411 Imaging in 3 filters with WFC3. Filters are F336W, F275W, F218W ORIENTs are specified to place companion away from diffraction spikes from primary 1338076057000 247.29761284544804 (Tic-Visit :proposal-id 12606 :visit-id "05" :proposal-version -1 :trans-version "20120604" :date "13-Jun-2012 18:08:17.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 201360 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12606 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12606 :visit-id "05" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2895 :al-overhead-at-end 40 :internal-dur-at-end 257 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3233 :pcs-gap 0 ) true 1 0 1339625314568 The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. /var/tmp/OPVisit4929005706800700075.xml HD 217411 B STIS observation. We use an ORIENT that places the slit perpendicular to the line joining the stars. We first acquire the bright A component, and then do an offset to the companion fainter B white dwarf. Spectra are taken with the G430L and G750M gratings. ORIENTS updated based on recent WFC3 images. -- CoI H. E. Bond 6/12/12 (Tic-Visit :proposal-id 12606 :visit-id "06" :proposal-version -1 :trans-version "20120604" :date "13-Jun-2012 18:08:31.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 147648 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12606 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12606 :visit-id "06" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2721 :al-overhead-at-end 0 :internal-dur-at-end 340 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3069 :pcs-gap 0 ) true 1 0 1339625323914 The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. /var/tmp/OPVisit8797051120870357049.xml Imaging in 3 filters with WFC3. Filters are F275W, F218W, F336W PA is 10.62D offset = 221.38D Total angle = 232 1322336533000 360.0 (Tic-Visit :proposal-id 12606 :visit-id "07" :proposal-version -1 :trans-version "20120604" :date "13-Jun-2012 18:08:42.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1732464 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12606 :visit-id "07" :obset-id "07" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12606 :visit-id "07" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2096 :al-overhead-at-end 118 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3239 :pcs-gap 0 ) true 1 0 1339625332506 The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. /var/tmp/OPVisit5109753828839084871.xml HR 1358 STIS observation Acquire bright star. Blind offset to faint companion. Obtain spectra in G750M and G430L/ ORIENT specification is to place slit perpendicular to line joining the two stars. (Tic-Visit :proposal-id 12606 :visit-id "08" :proposal-version -1 :trans-version "20120604" :date "13-Jun-2012 18:08:50.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 148208 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12606 :visit-id "08" :obset-id "08" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12606 :visit-id "08" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2793 :al-overhead-at-end 0 :internal-dur-at-end 379 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3129 :pcs-gap 0 ) true 1 0 1339625359283 The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. /var/tmp/OPVisit3870113679963677892.xml HD 2133 Imaging in 3 filters with WFC3. Filters are F336W, F275W, F218W ORIENTs are specified to place companion away from diffraction spikes from primary 1333938328000 192.8 (Tic-Visit :proposal-id 12606 :visit-id "09" :proposal-version -1 :trans-version "20120604" :date "13-Jun-2012 18:09:12.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 201360 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 12606 :visit-id "09" :obset-id "09" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 12606 :visit-id "09" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3195 :al-overhead-at-end 40 :internal-dur-at-end 257 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3635 :pcs-gap 0 ) true 1 0