! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! Id: 6098 ! ! For help call your Program Coordinator: Max Mutchler ! Phone: 410 338-1321 , E-mail: mutchler@stsci.edu Proposal_Information Title: Eclipse Mapping and Tomography of the UV Line Emitting Regions of DQ Herculis Proposal_Category: GO Scientific_Category: Hot Stars Cycle: 5 Investigators PI_name: Michael Eracleous PI_Institution: Space Telescope Science Institute CoI_Name: Mario Livio CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Robert Williams CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Keith Horne CoI_Institution: University of Saint Andrews Contact: ! Y or N (designate at most one contact) CoI_Name: Joseph Patterson CoI_Institution: Columbia University Contact: ! Y or N (designate at most one contact) CoI_Name: Phillip Martell CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Kirk Korista CoI_Institution: University of Kentucky Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) The old nova DQ Herculis is a cataclysmic binary which offers a rare combination of two important properties: (1) eclipses and (2) coherent periodic signals. We propose to exploit these properties in order to answer two fundamental questions: (1) to determine the origin of the UV emission lines and pulsations, and (2) to establish definitively the presence or absence of a wind, and to determine its origin. Our approach will be to use the behavior of the UV continuum and emission lines as the binary rotates, through eclipse, and over the rapid (71 s) oscillation cycle to construct eclipse maps and Doppler tomograms of the line emitting regions, and thus to locate the origin of the lines and to test for the presence of a wind. Since emission lines are an essential tool for probing the physical conditions and kinematics of cataclysmic variables, the importance of establishing their origin can hardly be overestimated. A system such as DQ Her, which is thought to lack an inner accretion disk, will also provide a crucial test for models of wind and outflow formation. Questions ! Free format text (please update) Observing_Description: We will use the FOS with the BLUE digicon detector and the G130H grating in RAPID mode, to obtain spectra with a time resolution of 5 s. The above setup will give us coverage of the region 1150 - 1606 A (see Figure 1), with a dispersion of 0.25~\AA~pix\m1\ (quarterstepping over diodes). We will employ the 1\asecb.0 aperture, with which we will achieve a spectral resolution of 0.96~\AA, corresponding to a velocity resolution of 190~\kms\ at the \CIV\ line. This resolution is adequate for our study of the line profiles and their variability over the orbital rapid oscillation cycles. To study the kinematics of the line emitting gas over the rapid oscillation cycle, the time-resolved spectra will be folded about the known pulse period, to maximize the signal-to-noise ratio (hereafter $S/N$). Real_Time_Justification: In order to apply our Doppler tomographic and eclipse mapping techniques we need coverage of one complete orbital cycle, including two eclipses. The binary orbital period of our target is 4.64 hours and the duration of the eclipse is 55 minutes. Because this binary orbital period is almost an integer multiple of the 96-minute orbital period of the spacecraft, we need to visit the target twice with the FOS. In the second visit we will observe the binary phases not covered in the first visit due to earth occultation. The visibility window of the target is 55 minutes, which just barely accommodates a full eclipse (some observing time will be lost to re-acquisition of guide stars). Therefore, in order to achieve the desired coverage we need to observe for 4 spacecraft orbits on each visit. In the first visit we will begin our observation at binary orbital phase 0.56 and observe continuously for 4 spacecraft orbits. This will give us coverage of half of the orbital cycle, and two incomplete eclipses. We will return 23 hours later, after the observing window has shifted in phase by 47 minutes, to repeat the same sequence of observations and fill in the gaps left in the first visit. With this observing plan we will achieve complete coverage of the binary orbit, with a total, on-source exposure time of 330 minutes (19,800 s). Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: DQ-HER Alternate_Names: NOVA-HERCULIS-1934 Description: STAR, INTERACTING BINARY Position: RA=18H 07M 30.38S +/- 0.1S, DEC=+45D 51' 31.8" +/- 0.5", PLATE-ID=00TB Equinox: 2000 RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: 1983.352 Annual_Parallax: Flux: V=14.65 +/- 0.10 ! Include at least V and B-V B-V=0.14 +/- 0.05 F-CONT(1450)=1.1 +/- 0.1 E-14 F-LINE(1550)=2.0 +/- 0.2 E-13 W-LINE(1550)=10 +/- 2 Comments: THE STAR IS AN ECLIPSING BINARY. THE MAGNITUDE AT MID-ECLIPSE DROPS TO V=17.1, B-V=0.2. ACQUISITION MUST OCCUR OUT OF ECLIPSE. Visits Visit_Number: 1 Visit_Requirements: PERIOD 0.193620897d AND ZERO-PHASE JD2434954.9438 GROUP 1-2 WITHIN 7D Visit_Comments: Exposure_Number: 1 Target_Name: DQ-HER Config: FOS/BL Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Wavelength: Optional_Parameters: ! TYPE=UP Number_of_Iterations: 1 Time_Per_Exposure: 10S Special_Requirements: ONBOARD ACQ FOR 2 PHASE 0.78 TO 0.80 Comments: Exposure_Number: 2 Target_Name: DQ-HER Config: FOS/BL Opmode: RAPID Aperture: 1.0 Sp_Element: G130H Wavelength: Optional_Parameters: READ-TIME=6.3 Number_of_Iterations: 1 Time_Per_Exposure: 10332S Special_Requirements: !---------------------------------------------------------------------------- Visit_Number: 2 Visit_Requirements: PERIOD 0.193620897d AND ZERO-PHASE JD2434954.9438 GROUP 1-2 WITHIN 7D Visit_Comments: THE TIMING OF THE OBSERVATIONS WITH THE RED AND BLUE DETECTORS IS VERY CRUCIAL. DO NOT CHANGE THE ORDER OF THE FOS/RD AND FOS/BL OBSERVATIONS. Exposure_Number: 1 Target_Name: DQ-HER Config: FOS/RD Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Wavelength: Optional_Parameters: ! TYPE=UP Number_of_Iterations: 1 Time_Per_Exposure: 10S Special_Requirements: ONBOARD ACQ FOR 2-3 PHASE 0.57 TO 0.59 Exposure_Number: 2 Target_Name: DQ-HER Config: FOS/RD Opmode: RAPID Aperture: 1.0 Sp_Element: G190H Wavelength: Optional_Parameters: READ-TIME=6.3 Number_of_Iterations: 1 Time_Per_Exposure: 9954S Special_Requirements: Comments: CHANGE DETECTORS AND GRATINGS DURING EARTH OCCULTATION. APERTURE STAYS THE SAME. Exposure_Number: 3 Target_Name: DQ-HER Config: FOS/BL Opmode: RAPID Aperture: 1.0 Sp_Element: G130H Wavelength: Optional_Parameters: READ-TIME=6.3 Number_of_Iterations: 1 Time_Per_Exposure: 11088S Special_Requirements: !============================================================================= Data_Distribution ! Defaults indicated; change if desired Medium: 8MM ! 8MM or 6250BPI or 1600BPI Blocking_Factor: 10 ! 10 or 1 ! Only astronomers with very old 9- ! track tape drives should consider ! a blocking factor of 1 Ship_To: Mike Eracleous ! STSCI or PI_Address or Will pick-up ! PI Address from Phase I is: ! ! 3700 San Martin Drive, ! Baltimore, MD 21218 ! ! Ship_Via: UPS ! UPS (2-day) or OVERNIGHT ! Overnight shipping done at PI expense Recipient_Email: ! Needed if Ship_To: is not PI_Address !