FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser Program is being resubmitted with slight modifications to the ORIENT angles, based on the new plan windows. 1438249305 ----- Attempting Submission 1 (Fri Jul 17 20:26:45 GMT 2015) ----- ----- Attempting Submission 2 (Thu Aug 20 19:31:20 GMT 2015) ----- APT is flagging short exposures without FLASHing, but the very bright targets will give plenty of background HST Observations of Astrophysically Important Visual Binaries We propose to continue our long-term program of astrometry of close visual binaries, with the primary goal of determining purely dynamical masses for 3 important main-sequence stars and 9 white dwarfs (WDs). A secondary aim is to set limits on third bodies in the systems down to planetary mass. Three of our targets are naked-eye stars with much fainter companions that are extremely difficult to image from the ground. Our other 2 targets are double WDs, whose small separations and faintness likewise make them difficult to measure using ground-based techniques. Observations have been completed for a 3rd double WD. The bright stars, to be imaged with WFC3, are: (1) Procyon (P = 40.83 yr), containing a bright F star and a much fainter WD companion. With the continued monitoring proposed here, we will obtain masses to an accuracy of better than 1%, providing a testbed for theories of both Sun-like stars and WDs. (2) Sirius (P = 50.14 yr), an A-type star also having a faint WD companion, Sirius B, the nearest and brightest of all WDs. (3) Mu Cas (P = 21.08 yr), a nearby metal-deficient G dwarf for which accurate masses will lead to the stars' helium contents, with cosmological implications. The faint double WDs, to be observed with FGS, are: (1) G 107-70 (P = 18.84 yr), and (2) WD 1818+126 (P = 12.19 yr). Our astrometry of these systems will add 4 accurate masses to the handful of WD masses that are directly known from dynamical measurements. The FGS measurements will also provide precise parallaxes for the systems, a necessary ingredient in the mass determinations. This is the Cycle 23 continuation of a program in which we are determining the orbits of visual binaries. The targets for Cycle 23 are Procyon, mu Cas, and Sirius. Procyon, mu Cas, and Sirius will be observed with WFC3/UVIS. For the two very bright stars, Procyon and Sirius, we will use the long-wavelength F953N filter to reduce the signal. Since even with this filter Procyon A and Sirius A would saturate in the minimum WFC3 exposure, we will let them saturate and use the diffraction spikes to centroid the bright components. For Procyon there will be a series of dithered 38-sec exposures, which will provide good unsaturated exposures for Procyon B at the same telescope pointing. For Sirius there will be a series of 6- and 12-sec dithered exposures. For mu Cas, we will use 1.5-sec exposures in F225W, which will not be saturated. These will be followed at each dither position with a 265-sec exposure, which will be well exposed for the cool dM companion. COOL STARS 12 false true false false 0.0 0.0 AVAILABLE STAR DA F3-F9 Coords are for center of gravity of binary. Accuracy confirmed by 2000 Nov 28 WFPC2 observations. 6/14/06: updated to ICRS system using galex website. ALPHA-CMI HR2943 J2000 J2000 B-V = 0.42 STAR G V-IV Coordinate accuracy confirmed by 2000-01 WFPC2 observations. 6/14/06: updated to ICRS system using galex website. HR321 HD6582 J2000 J2000 B-V = 0.70 STAR A0-A3 V-IV DA Coordinates are for center of mass of the Sirius A-B binary, determined from a WFPC2 observation in January 2008 and a WFC3 observation in September 2012.. ALPHA-CMA HR2491 J2000 J2000 WFC3/UVIS Imaging No No F953N WFC3/UVIS Imaging No No F953N WFC3/UVIS Imaging No No F225W FGS POS No F583W FGS POS No F583W POS-TARG DITHER 0.173 LINE 0.112 false true 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 1 false The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. /tmp/OPVisit6323156256602262870.xml ORIENT requirement is done so that companion star will not lie near diffraction spikes or charge bleeding from the very bright primary star. ORIENT updated 8/20/15 based on new plan windows. (Tic-Visit :proposal-id 14342 :visit-id "01" :proposal-version -1 :trans-version "20150609" :date "20-Aug-2015 15:28:23.0" :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 164752 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14342 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14342 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2868 :al-overhead-at-end 40 :internal-dur-at-end 217 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3213 :pcs-gap 0 ) true 1 0 The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. /tmp/OPVisit1313984307132844980.xml ORIENT requirement is done so that companion star will not lie near diffraction spikes or charge bleeding of primary star. ORIENT updated 8/20/15 based on new plan windows. (Tic-Visit :proposal-id 14342 :visit-id "02" :proposal-version -1 :trans-version "20150609" :date "20-Aug-2015 15:28:31.0" :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 109840 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14342 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14342 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3029 :al-overhead-at-end 43 :internal-dur-at-end 157 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3403 :pcs-gap 0 ) true 1 0 The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. /tmp/OPVisit7953813603085214289.xml ORIENT requirement is done so that companion star will not lie near diffraction spikes or charge bleeding from the very bright primary star. ORIENT updated 8/20/15 based on new plan windows. (Tic-Visit :proposal-id 14342 :visit-id "03" :proposal-version -1 :trans-version "20150609" :date "20-Aug-2015 15:28:38.0" :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 499088 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14342 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14342 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2756 :al-overhead-at-end 76 :internal-dur-at-end 582 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3221 :pcs-gap 0 ) true 1 0