! Proposal 6546, submission 1 ! PI: Christopher Mauche ! Received Thu Feb 8 20:33:58 EST 1996 ! From: cmauche@igpp.llnl.gov ! 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: Dissecting the Wind and Disk of the Nova-like Variable V347 Puppis Proposal_Category: GO Scientific_Category: BINARIES AND STAR FORMATION Cycle: 6 Investigators PI_name: Christopher Mauche PI_Institution: Lawrence Livermore National Laboratory CoI_Name: Raymundo Baptista CoI_Institution: University of Saint Andrews Contact: N ! Y or N (designate at most one contact) CoI_Name: David Buckley CoI_Institution: South African Astronomical Observatory Contact: N ! Y or N (designate at most one contact) CoI_Name: Knox Long CoI_Institution: Space Telescope Science Institute Contact: N ! Y or N (designate at most one contact) CoI_Name: John Raymond CoI_Institution: Center for Astrophysics Contact: N ! Y or N (designate at most one contact) CoI_Name: Isaac Shlosman CoI_Institution: University of Kentucky Contact: N ! Y or N (designate at most one contact) CoI_Name: Peter Vitello CoI_Institution: Lawrence Livermore National Laboratory Contact: N ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) As evidenced by the P Cygni profiles of their ultraviolet resonance lines, high mass accretion rate CVs suffer mass loss in the form of high-velocity winds. Models of these line profiles are consistent with a disk origin of these winds, and hence demonstrate a close link between mass accretion and mass loss in CVs, just as applies in AGN and protostars. Our understanding of CVs has been advanced in unique and important ways by observations of systems in which the secondary eclipses the disk and wind. Such observations constraint the geometry and kinematics of the wind, provide the full spectral energy distribution across the face of the disk, allow an assessment of the contributions to the observed line profiles and continuum by the disk, the hot spot, and the heated face of the secondary. With its long period, high inclination, strong UV emission lines, and weak UV continuum, the bright nova-like variable V347 Pup is an ideal system in which to perform these studies. Recent optical and IUE observations reveal variations in the lines and continuum at all orbital phases including eclipse. Recent theoretical studies of the wind make a number of predictions which can be tested only with the large collecting area and high spectral and temporal resolution of HST. We propose to test these predictions and to perform the above disk and wind studies via simultaneous phase-resolved measurements with the FOS/BL G130H grating of the N V, Si IV, and C IV emission lines and 1140-1606 Angstrom continuum of V347 Pup. Questions ! Free format text (please update) Observing_Description: Subsection FOS/BL G130H: To cover the C IV Lambda 1550, Si IV Lambda 1400, and N V Lambda 1240 wind lines simultaneously with the highest possible spectral resolution, observations with the FOS/BL G130H grating are required. The spectral resolution of this grating is 0.96 Angstrom, over 4 times higher than that of IUE, and corresponds to a velocity width of ~200 km s^-1 or ~2% of the FWZI of the wind lines. We choose the upper 1" square aperture to avoid the "C IV" scratch on the photocathode, and to suppress geocoronal Lyman Alpha, which otherwise may affect the blue wing of N V. RAPID read-out is required because flickering is observed in CVs with timescales of order 10 seconds, the orbital period at the inner edge of the accretion disk. The recommended minimum READ-TIME of 7.4 s for the FOS with SUB-STEP=4 nicely fits our needs. Subsection Signal-to-noise ratio: Given the mean out-of-eclipse, eclipse, and hump spectra of V347 Pup shown in Figure 2, the sensitivity curves for the FOS/BL G130H grating in the FOS Handbook, and the transmittance of the 1" square aperture, the signal-to-noise ratio for the C IV, Si IV, and N V line profiles is as shown in Figure 4. An exposure of 100 s (~0.5% of the orbital period of V347 Pup) is assumed. In eclipse, the C IV, Si IV, and N V lines have signal-to-noise ratios of ~20, 8, and 9 diode^-1 (Angstrom^-1), respectively. Out of eclipse, these values are ~25, 13, and 13 diode^-1. Even higher values are realized during the hump phase. The signal-to-noise ratio of the continuum is low (~4 for C IV) because the continuum flux is low (recall that the low continuum flux is critical to the study of the wind). The signal-to-noise ratio of the continuum can be increased by a factor of 5 (to ~20 for C IV) by binning the spectrum into 25 Angstrom bins. Subsection Sequence of observations: HST observations of V347 Pup are severely constrained by the 5.56 hr orbital period of the binary. First, occultations of the disk and wind last ~70 min, longer than the visibility of 56 min for a source at this declination. Almost all of the predicted action on the wind lines occurs in ~+/- 7% of the orbital period of the binary (see Fig. 3) or ~47 min, but to observe the full ingress and egress of the disk, including the hot spot, and to obtain spectra well away from eclipse in order to measure the undisturbed line profiles, a minimum of 2 HST orbits are required to cover the eclipse. To separate flickering variations from orbital variations, two or more eclipses should be observed. Second, there is a near 2:7 resonance between the orbital periods of HST and V347 Pup. To observe all binary phases, 7 consecutive HST orbits are required. Beginfigure Signal-to-noise ratio for the C IV, Si IV, and N V line profiles of V347 Pup: mean out-of-eclipse (bold solid curves), eclipse (lower solid curves), and hump (upper dashed curves). Calculation assumes 100 s exposures. Endfigure To meet the above constraints and requirements, we propose to observe V347 Pup during two visits. These visits should be spaced by greater than 4 days, but by less than 3-4 weeks, so that the "reuse_target_offset" procedure can be used. During the first visit of 5 consecutive orbits, the following orbital phases should be observed: 0.71-0.86, 1.00-1.15, 1.29-1.44, 1.58-1.73, 1.86-1.01. The 2nd and 5th HST orbits sample the egress from and ingress to eclipse, respectively; the 1st orbit samples the hump phase. During the second visit of 5 consecutive orbits, the following orbital phases should be observed: 0.85-1.00, 1.14-1.29, 1.43-1.58, 1.71-1.86, 2.00-2.15. The 1st and 5th HST orbits sample the ingress to and egress from eclipse, respectively; the 4th orbit samples the hump phase. With this observing strategy, the eclipse and hump phases are observed twice; all other phases are observed once (see graphic below). Note that the registry of the phases of the above sequences could be shifted by +/-~ 0.02, if necessary. Also, the phasings of the first visit could be repeated during the second visit, if necessary. Subsection Target Acquisition: On the first visit, we will allocate 2 orbits for careful target acquisition into the upper 1" square aperture (after consultation with the FOS team). On the second visit, we will employ the "reuse_target_offset" procedure to cut down on overheads. The total number of orbits for this project is thus 12. NOTICE: We find that target acquisition can be accomplished in 1 orbit, so we have used the 2nd orbit of the 1st visit for FOS exposures. If target acquistion turns out to require more than 1 orbit, the 1st FOS exposure can be shortened to pack that orbit. Note that the phase requirement is placed only on the 2nd and subsequent orbits of the 1st visit. Real_Time_Justification: The requested observations are time critical as they must cover specific orbital phases. However, the orbital ephemeris is known to high precision, so the conditions can be specified well in advance. We request two visits to the source to observe 2 eclipse sequences to separate flickering variations from orbital variations. To allow the use of the "reuse_target_offset" procedure, the second visit should follow the first after 4 days but within 3-4 weeks. The timing of the second visit is further constrained by the near 2:7 resonance between the orbital periods of HST and V347 Pup. NOTICE: If timely scheduling of the 2nd visit is not possible with the required phase constraints, one could steal 1 orbit from the 1st visit and start from scratch during the 2nd visit with a new target acquisition, thereby negating the constraint of the "reuse_target_offset" procedure. HOWEVER: this change should be considered ON HOLD for PI approval. The possibility of simultaneous or near-simultaneous ground- based optical photometry and/or spectroscopy is being pursued with colleagues in the southern hemisphere. Co-I D. Buckley (South Africa) and colleague D. Sullivan (New Zealand) have extensive experience observing this source. NOTICE: Optimal simultaneous ground-based coverage requires the following additional constraints: BETWEEN 01-DEC-96 AND 10-JAN-97 and BETWEEN 18:45 U.T. AND 02:45 U.T. Upon the advise of A. Berman (02/06/96), we have not added these constraints below. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: V347PUPPIS Alternate_Names: LB1800 Description: STAR, NOVA-LIKE, INTERACTING BINARY Position: ! Most common specification format is RA=06H 10M 33.54S +/- 0.5S, ! RA=0H 0M 0.00S +/- 0S, DEC=-48D 44' 26.1" +/- 0.5", ! DEC=0D 0' 0.0" +/- 0", PLATE-ID=01CH ! 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 = 13.4 +/- 0.2 ! Include at least V and B-V B-V = 0.3 +/- 0.2 F-CONT(1470) = 2.5 +/- 1.5E-14 F-LINE(1549) = 7.5 +/- 1.5E-12 W-LINE(1549) = 11.8 +/- 2.4 Comments: Eclipsing nova-like variable; flux values apply away from eclipse. Typical flux values in eclipse are as follows: V=15.7+/-0.2, B-V=1.0+/-0.2, F-CONT(1470)=0.3+/-0.2E-14, F-LINE(1549)=4.0+/-0.5E-12, W-LINE(1549)=8.0+/-1.0. Star will be acquired out of eclipse. ! This is a template for a single visit containing a single exposure ! Repeat exposure and visit blocks as needed Visits ! Section 6 Visit_Number: 1 Visit_Requirements: PERIOD 0.231936060D AND ZERO-PHASE JD2446836.96176 ORIENT 338D TO 338D On_Hold_Comments: Visit_Comments: FOS exposures must follow one after the other over 6 orbits. Phase requirements for the set follow from the 7th (critical) orbit. To allow simultaneous ground-based optical observations, we request that these observations are scheduled during the November, September, or December/January scheduling windows, in that order of preference. Exposure_Number: 1 ! Section 6.5 Target_Name: V347PUPPIS Config: FOS/BL Opmode: ACQ/PEAK ! acquire target 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 2 ! Section 7.2 Comments: Exposure_Number: 2 ! Section 6.5 Target_Name: V347PUPPIS Config: FOS/BL Opmode: ACQ/PEAK ! acquire target 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 3 ! Section 7.2 Comments: Exposure_Number: 3 ! Section 6.5 Target_Name: V347PUPPIS Config: FOS/BL Opmode: ACQ/PEAK ! acquire target 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 4 ! Section 7.2 Comments: Exposure_Number: 4 ! Section 6.5 Target_Name: V347PUPPIS Config: FOS/BL Opmode: ACQ/PEAK ! acquire target 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: 1S Special_Requirements: ONBOARD ACQ FOR 5-10 ! Section 7.2 SAVE OFFSET 1 Comments: Exposure_Number: 5 ! Section 6.5 Target_Name: V347PUPPIS Config: FOS/BL ! FOS exposures Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: G130H Wavelength: Optional_Parameters: READ-TIME=7.40, SUB-STEP=4, COMB=YES, STEP-PATT=SINGLE, STEP-TIME=0.3 Number_of_Iterations: 1 Time_Per_Exposure: 2405.0S Special_Requirements: NO SPLIT Comments: If target acquisition takes longer than the currently estimated 1 orbit, this exposure can be shortened to pack the orbit. Exposure_Number: 6 ! Section 6.5 Target_Name: V347PUPPIS Config: FOS/BL ! FOS exposures Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: G130H Wavelength: Optional_Parameters: READ-TIME=7.40, SUB-STEP=4, COMB=YES, STEP-PATT=SINGLE, STEP-TIME=0.3 Number_of_Iterations: 1 Time_Per_Exposure: 2405.0S Special_Requirements: NO SPLIT ! Section 7.2 Comments: Expand exposure to pack orbit. Exposure_Number: 7 ! Section 6.5 Target_Name: V347PUPPIS Config: FOS/BL ! FOS exposures Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: G130H Wavelength: Optional_Parameters: READ-TIME=7.40, SUB-STEP=4, COMB=YES, STEP-PATT=SINGLE, STEP-TIME=0.3 Number_of_Iterations: 1 Time_Per_Exposure: 2405.0S Special_Requirements: PHASE 0.99 TO 0.01! Section 7.2 NO SPLIT Comments: Expand exposure to pack orbit. CRITICAL ORBIT: Contains the egress of the eclipse of the accretion disk and wind. Exposure_Number: 8 ! Section 6.5 Target_Name: V347PUPPIS Config: FOS/BL ! FOS exposures Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: G130H Wavelength: Optional_Parameters: READ-TIME=7.40, SUB-STEP=4, COMB=YES, STEP-PATT=SINGLE, STEP-TIME=0.3 Number_of_Iterations: 1 Time_Per_Exposure: 2405.0S Special_Requirements: NO SPLIT ! Section 7.2 Comments: Expand exposure to pack orbit. Exposure_Number: 9 ! Section 6.5 Target_Name: V347PUPPIS Config: FOS/BL ! FOS exposures Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: G130H Wavelength: Optional_Parameters: READ-TIME=7.40, SUB-STEP=4, COMB=YES, STEP-PATT=SINGLE, STEP-TIME=0.3 Number_of_Iterations: 1 Time_Per_Exposure: 2405.0S Special_Requirements: NO SPLIT ! Section 7.2 Comments: Expand exposure to pack orbit. Exposure_Number: 10 ! Section 6.5 Target_Name: V347PUPPIS Config: FOS/BL ! FOS exposures Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: G130H Wavelength: Optional_Parameters: READ-TIME=7.40, SUB-STEP=4, COMB=YES, STEP-PATT=SINGLE, STEP-TIME=0.3 Number_of_Iterations: 1 Time_Per_Exposure: 2405.0S Special_Requirements: NO SPLIT ! Section 7.2 Comments: Expand exposure to pack orbit. IMPORTANT ORBIT: Contains the ingress of the eclipse of the accretion disk and wind. Visits ! Section 6 Visit_Number: 2 Visit_Requirements: PERIOD 0.231936060D AND ZERO-PHASE JD2446836.96176 ORIENT 338D TO 338D On_Hold_Comments: Visit_Comments: Visit Number 2 should follow as soon after Visit Number 1 as the phase requirements and the USE OFFSET feature allows. Note that if timely scheduling of Visit Number 2 is not possible with these constraints, it may be acceptable to steal 1 orbit from Visit Number 1 and to reacquire the target from scratch. Please consult the PI before making this change. FOS exposures must follow one after the other over 5 orbits. Phase requirements for the set should follow from the 5th (critical) orbit. To allow simultaneous ground-based optical observations, we request that these observations are scheduled during the November, September, or December/January scheduling windows, in that order of preference. Exposure_Number: 1 ! Section 6.5 Target_Name: V347PUPPIS Config: FOS/BL ! FOS exposures Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: G130H Wavelength: Optional_Parameters: READ-TIME=7.40, SUB-STEP=4, COMB=YES, STEP-PATT=SINGLE, STEP-TIME=0.3 Number_of_Iterations: 1 Time_Per_Exposure: 2405.0S Special_Requirements: NO SPLIT ! Section 7.2 USE OFFSET 1 Comments: Expand exposure to pack orbit. IMPORTANT ORBIT: Contains the ingress of the eclipse of the accretion disk and wind. Exposure_Number: 2 ! Section 6.5 Target_Name: V347PUPPIS Config: FOS/BL ! FOS exposures Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: G130H Wavelength: Optional_Parameters: READ-TIME=7.40, SUB-STEP=4, COMB=YES, STEP-PATT=SINGLE, STEP-TIME=0.3 Number_of_Iterations: 1 Time_Per_Exposure: 2405.0S Special_Requirements: NO SPLIT ! Section 7.2 USE OFFSET 1 Comments: Expand exposure to pack orbit. Exposure_Number: 3 ! Section 6.5 Target_Name: V347PUPPIS Config: FOS/BL ! FOS exposures Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: G130H Wavelength: Optional_Parameters: READ-TIME=7.40, SUB-STEP=4, COMB=YES, STEP-PATT=SINGLE, STEP-TIME=0.3 Number_of_Iterations: 1 Time_Per_Exposure: 2405.0S Special_Requirements: NO SPLIT ! Section 7.2 USE OFFSET 1 Comments: Expand exposure to pack orbit. Exposure_Number: 4 ! Section 6.5 Target_Name: V347PUPPIS Config: FOS/BL ! FOS exposures Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: G130H Wavelength: Optional_Parameters: READ-TIME=7.40, SUB-STEP=4, COMB=YES, STEP-PATT=SINGLE, STEP-TIME=0.3 Number_of_Iterations: 1 Time_Per_Exposure: 2405.0S Special_Requirements: NO SPLIT ! Section 7.2 USE OFFSET 1 Comments: Expand exposure to pack orbit. Exposure_Number: 5 ! Section 6.5 Target_Name: V347PUPPIS Config: FOS/BL ! FOS exposures Opmode: RAPID Aperture: 1.0-PAIR-A Sp_Element: G130H Wavelength: Optional_Parameters: READ-TIME=7.40, SUB-STEP=4, COMB=YES, STEP-PATT=SINGLE, STEP-TIME=0.3 Number_of_Iterations: 1 Time_Per_Exposure: 2405.0S Special_Requirements: PHASE 0.99 TO 0.01! Section 7.2 NO SPLIT USE OFFSET 1 Comments: Expand exposure to pack orbit. CRITICAL ORBIT: Contains the egress of the eclipse of the accretion disk and wind. Data_Distribution ! Defaults indicated; change if desired Medium: 8MM ! 8MM or 6250BPI or 1600BPI Blocking_Factor: 10 ! 10 or 1 ! 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