! Proposal 6796, submission 1 ! PI: Raymundo Baptista ! Received Thu Feb 15 16:07:40 EST 1996 ! From: rb8@st-andrews.ac.uk ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! ! Refer to the HST Phase II Proposal Instructions to fill this out ! ! Anything after a "!" is ignored, and may be deleted ! ! All keywords with multiple entries are comma delimited except the ! Visit_Requirements and Special_Requirements keywords which can be ! delimited with carriage returns or semi-colons, but not commas ! ! For help call your Program Coordinator: Alice Berman ! Phone: 410-338-4462, E-mail: aberman@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Proposal_Information ! Section 4 Title: Spectral Mapping of Accretion Disks in Cataclysmic Binaries: Bridging the CV Period Gap Proposal_Category: GO Scientific_Category: BINARIES AND STAR FORMATION Cycle: 6 Investigators PI_name: Raymundo Baptista PI_Institution: University of St Andrews CoI_Name: Keith Horne CoI_Institution: University of St Andrews Contact: ! Y or N (designate at most one contact) CoI_Name: Ivan Hubeny CoI_Institution: NASA Goddard Space Flight Center Contact: ! Y or N (designate at most one contact) CoI_Name: Knox Long CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Christopher Mauche CoI_Institution: Lawrence Livermore National Laboratory Contact: ! Y or N (designate at most one contact) CoI_Name: Rene Rutten CoI_Institution: Royal Greenwich Observatory - La Palma Contact: ! Y or N (designate at most one contact) CoI_Name: Richard Wade CoI_Institution: Pennsylvania State University Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) Maximum-entropy eclipse mapping techniques have advanced to the stage of delivering spatially-resolved spectra of accretion disks. By fitting disk model atmospheres to these spectra we are now able to determine the radial run of the temperature, surface density (which controls the local effective gravity of the disk), Mach number (which controls the strength of Balmer lines vs Balmer continuum), and the vertical temperature gradient in the disk (which controls whether the lines are in emission or absorption). Accretion disks in Cataclysmic Variables (CVs) cover a range of accretion rates and viscosity states. CVs show a bi-modal distribution of orbital periods, with systems clustering at periods of 1.5-2 hr or 3-5 hr, and a remarkable dearth of systems with periods between 2-3 hr. Our previous HST mapping experiments have framed accretion disks on both sides of this period gap, corresponding to the low and high accretion regimes. We now propose to look inside the gap by mapping the disk of V348 Pup (P_orb= 2.44 hr). There are evidences that its disk has different properties from those previously mapped by HST at shorter and longer periods. Observations of this type can drive fundamental new insights into the physics of accretion disks. Questions ! Free format text (please update) Observing_Description: We propose to observe 8 eclipses of V348 Pup. To have the broadest possible spectral coverage we will combine 4 visits with FOS/BL G160L (1150 to 2500 Angstrom) to 4 visits with FOS/RD PRISM (1800 to 8500 Angstrom). We are primarily interested in studying continuum and emission line time variability, and therefore we will use the FOS in the ``RAPID'' mode to obtain high temporal resolution. Ideally we would like to observe from binary phase -0.13 to +0.13 for each eclipse. This requires 39-min for V348 Pup (P_orb= 146 -min). We need to observe the eclipse 4 times (for each disperser) because this will distinguish between variations due to the eclipse of the WD and accretion disk and those due to flickering -- which is known to be present in this system at optical wavelengths -- and also because it allow us to increase the signal-to-noise ratio (S/N) of the eclipse light curves in each spectral bin by combining the 4 individual eclipses. The proposed sequence of observations consists of one HST orbit for a target acquisition with the ACQ/PEAK procedure (41 min), followed by a science exposure of 44 min in the next orbit. The second visit should be spaced by at least 3 days to allow the use of the ``reuse\_target\_offset'' procedure. All consecutive visits will than consist of one science exposure of 41/42 mins per orbit. The 8 exposures should be spaced as closely as possible in time (and by no more than 3-4 weeks to permit use of ``reuse\_target\_offset'') consistent with the requirement to obtain the appropriate phase coverage. The exposure times are dictated by the time to cover the eclipse of V348 Pup. We estimate a count rate of 0.17 counts/s/Angstrom at 1850 Angstrom using continuum fluxes from an IUE spectrum (SWP 44676, 1.3* 10^-14 ergs/cm^2/s/Angstrom) and the latest sensitivity data on the FOS using the 0.9 arcsec (1.0) aperture. Thus 50 Angstrom wide bandpasses will yield UV light curves with a S/N of 10 in 12 s integrations. The C IV line has a flux of 7* 10^-13 ergs/cm^2/s and will produce 65 counts/s (S/N = 8). These numbers increase by a factor 2 by combining the 4 individual eclipses in average eclipse light curves. Real_Time_Justification: These observations are time-critical and must cover specific orbital phases. The orbital ephemeris of V348 Pup is well known so the conditions can be specified well in advance. The target is not a dwarf nova and therefore it does not undergo the periodic outbursts associated with those objects. However, since it is expected to present some low amplitude variations (~lt 0.5 mag), all 8 observations should be scheduled as close as possible in time to minimize the effects of secular variations and the joining together of the light curves from the various eclipses. Whole eclipses must be observed whenever possible. Calibration_Justification: Additional_Comments: The 8 science exposures should be obtained by alternating between exposures using the FOS/BL,G160L and FOS/RD,PRISM configurations. To allow simultaneous ground-based optical observations, we prefer that these observations are scheduled (in order of preference) during the October/November, September, or December/January scheduling windows. Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: V348-PUPPIS Alternate_Names: 1H0709-36 Description: STAR, NOVA-LIKE, INTERACTING BINARY, ACCRETION DISK Position: ! Most common specification format is RA=07H 12M 32.90S +/- 0.5", ! RA=0H 0M 0.00S +/- 0S, DEC=-36D 05' 39.6" +/- 0.5", ! DEC=0D 0' 0.0" +/- 0", PLATE-ID=02CS ! PLATE-ID=0000 Equinox: J2000 RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V = 15.6 +/- 0.4 ! Include at least V and B-V U-B = -0.65 +/- 0.15 B-V = +0.15 +/- 0.15 V-R = +0.15 +/- 0.15 F-CONT(1850) = 1.3 +/- 0.5 E-14 Comments: Eclipsing nova-like variable; flux ranges reflect the range of variations outside of eclipses. Target acquisition will occur outside of eclipse. Visits ! Section 6 Visit_Number: 1 Visit_Requirements: PERIOD 0.101838911D AND ZERO-PHASE JD2447210.12101 Visit_Comments: To allow simultaneous ground-based optical observations, we prefer that these observations are scheduled (in order of preference) during the October/November, September, or December/January scheduling windows. Exposure_Number: 10 ! Target acquisition, first step Target_Name: V348-PUPPIS Config: FOS/RD Opmode: ACQ/PEAK Aperture: 4.3 Sp_Element: MIRROR Wavelength: Optional_Parameters: SCAN-STEP-Y=1.23, SEARCH-SIZE-X=1, SEARCH-SIZE-Y=3 Number_of_Iterations: 1 Time_Per_Exposure: 1S Special_Requirements: ONBOARD ACQ FOR 20 Exposure_Number: 20 ! Target acquisition, second step Target_Name: V348-PUPPIS Config: FOS/RD Opmode: ACQ/PEAK Aperture: 1.0-PAIR-A Sp_Element: MIRROR Wavelength: Optional_Parameters: SCAN-STEP-X=0.61, SCAN-STEP-Y=0.61, SEARCH-SIZE-X=6, SEARCH-SIZE-Y=2 Number_of_Iterations: 1 Time_Per_Exposure: 1S Special_Requirements: ONBOARD ACQ FOR 30 Exposure_Number: 30 ! Target acquisition, third step Target_Name: V348-PUPPIS Config: FOS/RD Opmode: ACQ/PEAK Aperture: 0.5-PAIR-A Sp_Element: MIRROR Wavelength: Optional_Parameters: SCAN-STEP-X=0.29, SCAN-STEP-Y=0.29, SEARCH-SIZE-X=3, SEARCH-SIZE-Y=3 Number_of_Iterations: 1 Time_Per_Exposure: 1S Special_Requirements: ONBOARD ACQ FOR 40 Exposure_Number: 40 ! Target acquisition, final step Target_Name: V348-PUPPIS Config: FOS/RD Opmode: ACQ/PEAK Aperture: 0.25-PAIR-A Sp_Element: MIRROR Wavelength: Optional_Parameters: SCAN-STEP-X=0.11, SCAN-STEP-Y=0.11, SEARCH-SIZE-X=4, SEARCH-SIZE-Y=4 Number_of_Iterations: 1 Time_Per_Exposure: 4S Special_Requirements: ONBOARD ACQ FOR 50; SAVE OFFSET OFF-1 Comments: If possible, use occultation time to switch Sp_Element to PRISM and Aperture to 4.3 to save time for next orbit exposure. Exposure_Number: 50 ! First science exposure Target_Name: V348-PUPPIS Config: FOS/RD Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: PRISM Wavelength: Optional_Parameters: SUB-STEP=2, READ-TIME=5, COMB=YES, STEP-PATT=SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 2530S Special_Requirements: NO SPLIT; PHASE 0.86 TO 0.14 Comments: Try to center exposure on phase 0.0 Uninterrupted eclipse coverage required. Visit_Number: 2 Visit_Requirements: PERIOD 0.101838911D AND ZERO-PHASE JD2447210.12101 AFTER 1 BY 3D TO 28D SEQ 2-8 WITHIN 25D Visit_Comments: Use of USE OFFSET constrain separation with respect to first visit. All visits thereafter should be scheduled as close as possible in time consistent with the PHASE requirements, and in a sequence alternating exposures with FOS/BL,G160L and FOS/RD,PRISM. To allow simultaneous ground-based optical observations, we prefer that these observations are scheduled (in order of preference) during the October/November, September, or December/January scheduling windows. Exposure_Number: 1 ! First science exposure Target_Name: V348-PUPPIS Config: FOS/BL Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: G160L Wavelength: Optional_Parameters: SUB-STEP=2, READ-TIME=5, COMB=YES, STEP-PATT=SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 2375S Special_Requirements: NO SPLIT; PHASE 0.87 TO 0.13 USE OFFSET OFF-1 Comments: Try to center exposure on phase 0.0. Uninterrupted eclipse coverage required. Visit_Number: 3 Visit_Requirements: PERIOD 0.101838911D AND ZERO-PHASE JD2447210.12101 AFTER 1 BY 3D TO 28D Visit_Comments: Use of USE OFFSET constrain separation with respect to first visit. All visits thereafter should be scheduled as close as possible in time consistent with the PHASE requirements, and in a sequence alternating exposures with FOS/BL,G160L and FOS/RD,PRISM. To allow simultaneous ground-based optical observations, we prefer that these observations are scheduled (in order of preference) during the October/November, September, or December/January scheduling windows. Exposure_Number: 1 ! First science exposure Target_Name: V348-PUPPIS Config: FOS/RD Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: PRISM Wavelength: Optional_Parameters: SUB-STEP=2, READ-TIME=5, COMB=YES, STEP-PATT=SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 2305S Special_Requirements: NO SPLIT; PHASE 0.87 TO 0.13 USE OFFSET OFF-1 Comments: Try to center exposure on phase 0.0. Uninterrupted eclipse coverage required. Visit_Number: 4 Visit_Requirements: PERIOD 0.101838911D AND ZERO-PHASE JD2447210.12101 AFTER 1 BY 3D TO 28D Visit_Comments: Use of USE OFFSET constrain separation with respect to first visit. All visits thereafter should be scheduled as close as possible in time consistent with the PHASE requirements, and in a sequence alternating exposures with FOS/BL,G160L and FOS/RD,PRISM. To allow simultaneous ground-based optical observations, we prefer that these observations are scheduled (in order of preference) during the October/November, September, or December/January scheduling windows. Exposure_Number: 1 ! First science exposure Target_Name: V348-PUPPIS Config: FOS/BL Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: G160L Wavelength: Optional_Parameters: SUB-STEP=2, READ-TIME=5, COMB=YES, STEP-PATT=SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 2375S Special_Requirements: NO SPLIT; PHASE 0.87 TO 0.13 USE OFFSET OFF-1 Comments: Try to center exposure on phase 0.0. Uninterrupted eclipse coverage required. Visit_Number: 5 Visit_Requirements: PERIOD 0.101838911D AND ZERO-PHASE JD2447210.12101 AFTER 1 BY 3D TO 28D Visit_Comments: Use of USE OFFSET constrain separation with respect to first visit. All visits thereafter should be scheduled as close as possible in time consistent with the PHASE requirements, and in a sequence alternating exposures with FOS/BL,G160L and FOS/RD,PRISM. To allow simultaneous ground-based optical observations, we prefer that these observations are scheduled (in order of preference) during the October/November, September, or December/January scheduling windows. Exposure_Number: 1 ! First science exposure Target_Name: V348-PUPPIS Config: FOS/RD Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: PRISM Wavelength: Optional_Parameters: SUB-STEP=2, READ-TIME=5, COMB=YES, STEP-PATT=SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 2305S Special_Requirements: NO SPLIT; PHASE 0.87 TO 0.13 USE OFFSET OFF-1 Comments: Try to center exposure on phase 0.0. Uninterrupted eclipse coverage required. Visit_Number: 6 Visit_Requirements: PERIOD 0.101838911D AND ZERO-PHASE JD2447210.12101 AFTER 1 BY 3D TO 28D Visit_Comments: Use of USE OFFSET constrain separation with respect to first visit. All visits thereafter should be scheduled as close as possible in time consistent with the PHASE requirements, and in a sequence alternating exposures with FOS/BL,G160L and FOS/RD,PRISM. To allow simultaneous ground-based optical observations, we prefer that these observations are scheduled (in order of preference) during the October/November, September, or December/January scheduling windows. Exposure_Number: 1 ! First science exposure Target_Name: V348-PUPPIS Config: FOS/BL Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: G160L Wavelength: Optional_Parameters: SUB-STEP=2, READ-TIME=5, COMB=YES, STEP-PATT=SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 2375S Special_Requirements: NO SPLIT; PHASE 0.87 TO 0.13 USE OFFSET OFF-1 Comments: Try to center exposure on phase 0.0. Uninterrupted eclipse coverage required. Visit_Number: 7 Visit_Requirements: PERIOD 0.101838911D AND ZERO-PHASE JD2447210.12101 AFTER 1 BY 3D TO 28D Visit_Comments: Use of USE OFFSET constrain separation with respect to first visit. All visits thereafter should be scheduled as close as possible in time consistent with the PHASE requirements, and in a sequence alternating exposures with FOS/BL,G160L and FOS/RD,PRISM. To allow simultaneous ground-based optical observations, we prefer that these observations are scheduled (in order of preference) during the October/November, September, or December/January scheduling windows. Exposure_Number: 1 ! First science exposure Target_Name: V348-PUPPIS Config: FOS/RD Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: PRISM Wavelength: Optional_Parameters: SUB-STEP=2, READ-TIME=5, COMB=YES, STEP-PATT=SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 2305S Special_Requirements: NO SPLIT; PHASE 0.87 TO 0.13 USE OFFSET OFF-1 Comments: Try to center exposure on phase 0.0. Uninterrupted eclipse coverage required. Visit_Number: 8 Visit_Requirements: PERIOD 0.101838911D AND ZERO-PHASE JD2447210.12101 AFTER 1 BY 3D TO 28D Visit_Comments: Use of USE OFFSET constrain separation with respect to first visit. All visits thereafter should be scheduled as close as possible in time consistent with the PHASE requirements, and in a sequence alternating exposures with FOS/BL,G160L and FOS/RD,PRISM. To allow simultaneous ground-based optical observations, we prefer that these observations are scheduled (in order of preference) during the October/November, September, or December/January scheduling windows. Exposure_Number: 1 ! First science exposure Target_Name: V348-PUPPIS Config: FOS/BL Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: G160L Wavelength: Optional_Parameters: SUB-STEP=2, READ-TIME=5, COMB=YES, STEP-PATT=SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 2375S Special_Requirements: NO SPLIT; PHASE 0.87 TO 0.13 USE OFFSET OFF-1 Comments: Try to center exposure on phase 0.0. Uninterrupted eclipse coverage required. 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: PI_Address ! STSCI or PI_Address or ! PI Address from Phase I is: ! ! School of Physics & Astronomy ! North Haugh ! St. Andrews ! KY16 9SS ! Scotland, UK ! Ship_Via: UPS ! UPS (2-day) or OVERNIGHT ! Overnight shipping done at PI expense Recipient_Email: ! Needed if Ship_To: is not PI_Address ! ! Let us know what you think of this template and software! ! Please send a list of your likes and dislikes to your Program Coordinator