High-precision asteroseismology of the accreting white dwarf in GW Lib through simultaneous HST and K2 observations

0 Assigned ID: 1330 ----- Attempting Submission 1 (Tue Jan 31 17:09:36 GMT 2017) ----- HST Phase I Proposal 1330 (gwlib.apt) successfully submitted. Receipt: # 1330-1 ----- Attempting Submission 2 (Tue Jan 31 21:50:03 GMT 2017) ----- The number of orbits used exceeds the number allocated Hi Amber & Nick, I fixed the broken orbits in Visit 02, on my APT all visits do now fit nicely into the orbit constraint. Best wishes, Boris -143542256 ----- Attempting Submission 1 (Fri Mar 17 17:16:55 GMT 2017) ----- ----- Attempting Submission 2 (Fri Jul 21 21:17:35 GMT 2017) ----- ----- Attempting Submission 3 (Sat Jul 29 21:52:24 GMT 2017) ----- HST Phase II Proposal 14912 (14912.apt) successfully submitted. Receipt: # 14912-3 ----- Attempting Submission 4 (Mon Jul 31 20:46:43 GMT 2017) ----- The warning regarding the orbit allocation is probably due to the S/C and BOP visits. High-precision asteroseismology of the accreting white dwarf in GW Lib through simultaneous HST and K2 observations Our insight into the interior structures of stars is, literally, superficial, as most information is derived from observations the stellar photosphere, which represents only a tiny fraction of the total mass. Asteroseismology, the study of stellar pulsations, has the power to probe deep below the surface. For white dwarfs, asteroseismology can measure the composition of the degenerate core, the masses of the non-degenerate He and H layers, and rotation rates. This research area is rapidly progressing thanks to the uninterrupted long time-series observations obtained by Kepler/K2. GW Lib is the prototypical pulsating white dwarf in a cataclysmic variable, enabling the most definitive analysis of how accretion of mass, angular momentum, and energy affects the internal structure of the star. GW Lib falls into the footprint of K2 Campaign 15 (Aug-Nov 2017), and we will obtain 80 days of photometry every 58.8s which we will use to carry out the most detailed asteroseismological analysis of this star possible for the foreseeable future. In order to make full use of this unmatched photometric dataset, we request three HST/COS visits of GW Lib spread throughout Campaign 15 to (1) accurately measure the effective temperature, (2) unambiguously identify the pulsation modes, and (3) constrain the surface eigenfunctions of this rapidly rotating star. Concurrent measurement of these properties is essential for a complete seismological analysis and requires UV observations due to optical contamination from accretion. These mid-cycle observations will conclude our 15-year HST campaign on this pulsating white dwarf, from quiescence through its 2007 outburst and back into quiescence. The goal of this proposal is to obtain COS G140L ultraviolet spectroscopy of the pulsating white dwarf in the cataclysmic variable GW Lib simultaneous with the K2 Campaign 15 observations of this star. Campaign 15 will run from August 23 - November 20, 2017. GW Lib has been observed with STIS (Program 8103) and COS (Programs 11639, 12231, 12870, 13807). The previous COS observations with the G140L grating are: LB1A01020, LBJ501010, LB1A01020, LBJ501010, LC1V07010, LCJ301010 Our science goals require to cover the Ly alpha absorption of the white dwarf, thus we choose the 1105A central wavelength. Target acquisition is done in dispersed light, as in our previous COS observations. GW Lib is a catacylsmic variable, hence there is the possibility that it goes into a dwarf nova outburst. This is extremely unlikely, as the outburst period of the system is ~25 years, and the last outburst was in 2007. Nevertheless, we will follow the standard procedure for COS observations of cataclysmic variables, i.e. we will provide intense ground-based monitoring of the system right up to the HST observations (~24h), and STScI/GSFC will then remove the safety pin (=coordinate offset) for the observations to go ahead. This has been practiced ~40 times in HST program 12870. One caveat is that GW Lib will be visible from the ground only until ~mid September, so we have defined the observations as follows: Visit #1 should be about 5 days after the beginning of Campaign 15 (to ensure that K2 has settled in the field), and then Visit #2 and #3 will follow ~5 and ~10 days later. We are currently investigating if we could use Swift to provide the brightness measurements required to ensure the safety of COS, in which case Visit #3 could be pushed back towards October or November. 2017-July-21: change to ACQ/IMAGE acquisitions. 2017-July-29: fixed small orbit overruns in Visit 01 and 03 Stellar Physics Stellar Physics 6 false true false false false false AVAILABLE STAR DWARF NOVA NO GW Lib was observed with COS/G140L as part of programs 11639, 12231, 12870 and 13807, data sets: LB1A01020 LBJ501010 LC1V07010 LCJ301010 J2000 UNIDENTIFIED BLANK FIELD NO This target is a blank piece of sky which is the bright object safe pointing and is 9.817 arcseconds away at a PA 38.4 degrees from GW-LIB. GW Lib was observed with COS/G140L as part of programs 11639, 12231, 12870 and 13807, data sets: LB1A01020 LBJ501010 LC1V07010 LCJ301010 COS/FUV Spectroscopic No No G140L 1105 1501532449740 Timing link suitability includes constraints ([02 After 01 by 5.0 to 8.0 days] [01 After 1A by at least 3.0 days]) The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. /tmp/OPVisit4151751834786045586.xml This should be scheduled in evening-local time. Flags need to be cleared during the work day. This visit uses ACQ/IMAGE - needs the offsets etc. to be fixed. 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CASM was run in Phase II mode. /home/astro/btg/OP-cache/14912-v1B.xml This visit is for BOP checking the safe target only and should not execute onboard HST. 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CASM was run in Phase II mode. /tmp/OPVisit4509442792823697111.xml This visit allocates and sets up the safe position offset slot for visit 01 which will use that slot. This S/C visit should go earlier in the week while visit 01 will be at least 3 days later. Note: weekends are to be avoided since the CS must clear the target within 24 hours of HST execution. 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CASM was run in Phase II mode. /tmp/OPVisit7117851979915110226.xml This should be scheduled in evening-local time. Flags need to be cleared during the work day. This visit uses ACQ/IMAGE - needs the offsets etc. to be fixed. 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CASM was run in Phase II mode. /home/astro/btg/OP-cache/14912-v2B.xml This visit is for BOP checking the safe target only and should not execute onboard HST. 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CASM was run in Phase II mode. /tmp/OPVisit8548153887863754243.xml This visit allocates and sets up the safe position offset slot for visit 02 which will use that slot. This S/C visit should go earlier in the week while visit 02 will be at least 3 days later. Note: weekends are to be avoided since the CS must clear the target within 24 hours of HST execution. 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Flags need to be cleared during the work day. This visit uses ACQ/IMAGE - needs the offsets etc. to be fixed. 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CASM was run in Phase II mode. /home/astro/btg/OP-cache/14912-v3B.xml This visit is for BOP checking the safe target only and should not execute onboard HST. 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CASM was run in Phase II mode. /tmp/OPVisit2859931857477989809.xml This visit allocates and sets up the safe position offset slot for visit 03 which will use that slot. This S/C visit should go earlier in the week while visit 03 will be at least 3 days later. Note: weekends are to be avoided since the CS must clear the target within 24 hours of HST execution. 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