! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 6079,v 6.1 1996/06/27 19:01:50 pepsa Exp $ ! ! 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: Dustin Manning ! Phone: 410 338-4456 , E-mail: manning@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Date generated: Sun Dec 18 19:15:13 EST 1994 ! Proposal_Information ! Section 4 Title: UV Eclipse Spectroscopy of Accretion Disk Winds Proposal_Category: GO Scientific_Category: Hot Stars Cycle: 5 Investigators PI_name: K.O. Mason PI_Institution: Mullard Space Science Laboratory CoI_Name: J.E. Drew CoI_Institution: Oxford University Contact: ! Y or N (designate at most one contact) CoI_Name: C. Knigge CoI_Institution: Oxford University Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We shall monitor wind-formed UV lines in the highly inclined disk-accreting CV, UX UMa as they are eclipsed by the companion star. By measuring the way in which lines from several different ionic species change in shape and strength as the wind is progressively covered, we will probe its ionisation structure as well as its geometry and kinematics. The data will be compared with the results of Monte Carlo simulation of the line profiles to provide quantitative constraints on outflow collimation, acceleration, and mass- loss rate. Our goal is to build a full and self consistent model for the wind and to determine where in the system the wind originates (e.g. white dwarf, boundary layer, or disk). We will then be in a position to investigate what drives the wind and the effect it has on the underlying accretion disk structure. The proposal builds on highly successful observations of UX UMa begun by us in Cycle 2 in a restricted wavelength range. Repairs to the GHRS now permit its full potential for such a study to be realised. Questions ! Free format text (please update) Observing_Description: Our scientific objectives call for time sequences of spectra which follow the target through eclipse by the companion star. Thus the length of observation is determined by the duration of eclipse rather than by signal to noise considerations. We plan to use the G140L grating on side 1 of the GHRS which gives the optimum balance between spectral resolution and wavelength coverage for this application. The combination will yield 0.7Angstrom per pixel, sufficient to resolve, and derive separate eclipse light curves for, all the major features of the lines (for example the FWHM of the narrow absorption features seen in CIV is about 2Angstrom). The lines to be observed range from CIII 1175Angstrom at the shortward extreme to HeII 1640Angstrom at the longward extreme. This can be covered with two grating settings, centered at about 1293Angstrom and 1523Angstrom. The continuum eclipse of UX UMa lasts for about 20 minutes, the eclipse of the lines for about 30-40 minutes. This can be contained within one spacecraft orbit. To guard against variability unrelated to the binary motion, we propose to observe two eclipses at each grating setting. To maximise coverage of the eclipse, we would in some cases acquire the target in the previous spacecraft orbit. The remainder of the acquisition orbit would be used to obtain an unambiguous out- of-eclipse spectrum for comparison with the spectrum during eclipse. This is an essential reference. Our previous work has demonstrated the existance of orbital-phase related changes in the line profiles outside of eclipse. These are presently unexplained, but may have important consequences for the modelling of the wind and the changes during eclipse. We therefore plan one contiguous series of 4 spacecraft orbits where we monitor the eclipse in the first and fourth orbits (the orbital period of UX UMa is very close to an exact number (three) of HST orbits) and the more general orbital changes in between. Allowing for coverage of four eclipses, and for acquisition and out-of- eclipse spectra, we require a total of 8 spacecraft orbits to observe UX UMa. Though the exposure time is determined by phase coverage rather than the source flux, it is important to note that UX UMa is one of the brightest high inclination nova-like CV. The continuum near 1500Angstrom\ should yield a flux of 2* 10^-13 erg cm^-2s^-1AA^-1 (based on the IUE ULDA). This translates to a S/N of 10 per diode in about 1.5 minutes (0.005 in phase). This is adequate for our purposes as demonstrated by our cycle 2 observations of UX UMa (made with the G160M grating on side 2 of GHRS prior to the COSTAR repair mission). The peak flux in the CIV emission line (the brightest of the wind-formed resonance lines) is about twice that of the continuum. Real_Time_Justification: The observations must occur at a specific phase in the orbital cycle of the binary in order to sample the eclipse. The binary period of UX UMa is 0.196671278 days, and observations of the eclipse should start at about phase 0.93+/-0.02. The eclipse should be centered in the spacecraft viewing window as well as possible. Supporting ground based photometry may be arranged, but is not essential and should not influence the HST scheduling. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: UXUMA Alternate_Names: UX-UMA Description: STAR,Nova-like,Interacting Binary Position: !Most common specification format is RA=13H 36M 40.97S +/- 0.02S, ! RA=0H 0M 0.00S +/- 0S, DEC=+51D 54' 50.2" +/- 0.3", ! DEC=0D 0' 0.0" +/- 0", PLATE-ID=00XN ! PLATE-ID=0000 Equinox: J2000 Flux: V=12.7 +/- 0.3 ! Include at least V and B-V B-V=0.0 F-LINE(1549)=5 +/- 1 E-13 W-LINE(1549)=15 +/- 5 F-CONT(1549)=2 +/- 0.3 E-13 F-LINE(1640)=2 +/- 0.2 E-13 W-LINE(1640)=10 +/- 3 F-CONT(1640)=2 +/- 0.3 E-13 A(V)=0.06 +/- 0.06 Comments: Eclipsing variable star - mid-eclipse V=14.1 ! 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 0.196671278D AND ZERO-PHASE JD2443904.87872 On_Hold_Comments: Visit_Comments: Exact timings adjustable in consultation with PI to accomodate actual HST orbit schedule most efficiently. Exposure_Number: 1 ! Section 6.5 Target_Name: UXUMA Config: HRS Opmode: ACQ Aperture: 2.0 Sp_Element: MIRROR-N1 Wavelength: Optional_Parameters: BRIGHT=RETURN LOCATE=DEF Number_of_Iterations: 1 Time_Per_Exposure: 9S Special_Requirements: ONBOARD ACQuisition FOR 2-7 Comments: Exposure_Number: 2 ! Section 6.5 Target_Name: UXUMA Config: HRS Opmode: RAPID Aperture: 2.0 Sp_Element: G140L Wavelength: 1293 Optional_Parameters: SAMPLE-TIME=5 Number_of_Iterations: 1 Time_Per_Exposure: 29M Special_Requirements: END ORBIT PHASE 0.91 TO 0.95 Comments: Exposure_Number: 3 ! Section 6.5 Target_Name: UXUMA Config: HRS Opmode: RAPID Aperture: 2.0 Sp_Element: G140L Wavelength: 1523 Optional_Parameters: SAMPLE-TIME=5 Number_of_Iterations: 1 Time_Per_Exposure: 30M Special_Requirements: Comments: Exposure_Number: 4 ! Section 6.5 Target_Name: UXUMA Config: HRS Opmode: RAPID Aperture: 2.0 Sp_Element: G140L Wavelength: 1293 Optional_Parameters: SAMPLE-TIME=5 Number_of_Iterations: 1 Time_Per_Exposure: 10M Special_Requirements: END ORBIT Comments: Exposure_Number: 5 ! Section 6.5 Target_Name: UXUMA Config: HRS Opmode: RAPID Aperture: 2.0 Sp_Element: G140L Wavelength: 1293 Optional_Parameters: SAMPLE-TIME=5 Number_of_Iterations: 1 Time_Per_Exposure: 10M Special_Requirements: Comments: Exposure_Number: 6 ! Section 6.5 Target_Name: UXUMA Config: HRS Opmode: RAPID Aperture: 2.0 Sp_Element: G140L Wavelength: 1523 Optional_Parameters: SAMPLE-TIME=5 Number_of_Iterations: 1 Time_Per_Exposure: 30M Special_Requirements: END ORBIT Comments: Exposure_Number: 7 ! Section 6.5 Target_Name: UXUMA Config: HRS Opmode: RAPID Aperture: 2.0 Sp_Element: G140L Wavelength: 1523 Optional_Parameters: SAMPLE-TIME=5 Number_of_Iterations: 1 Time_Per_Exposure: 45M Special_Requirements: END ORBIT Comments: This exposure should be centered on eclipse automatically if exposure 2 is, since HST and UXUMA orbital periods close to an exact multiple. Extra acquisition time in first orbit has been allowed for. Visits ! Section 6 Visit_Number: 2 Visit_Requirements: GROUP 2-3 WITHIN 3D PERIOD 0.196671278D AND ZERO-PHASE JD2443904.87872 On_Hold_Comments: Visit_Comments: Exact timings adjustable in consultation with PI to accomodate actual HST orbit schedule most efficiently. Exposure_Number: 8 ! Section 6.5 Target_Name: UXUMA Config: HRS Opmode: ACQ Aperture: 2.0 Sp_Element: MIRROR-N1 Wavelength: Optional_Parameters: BRIGHT=RETURN LOCATE=DEF Number_of_Iterations: 1 Time_Per_Exposure: 9S Special_Requirements: ONBOARD ACQ FOR 9-11 Comments: Exposure_Number: 9 ! Section 6.5 Target_Name: UXUMA Config: HRS Opmode: RAPID Aperture: 2.0 Sp_Element: G140L Wavelength: 1523 Optional_Parameters: SAMPLE-TIME=5 Number_of_Iterations: 1 Time_Per_Exposure: 12M Special_Requirements: Comments: Exposure_Number: 10 ! Section 6.5 Target_Name: UXUMA Config: HRS Opmode: RAPID Aperture: 2.0 Sp_Element: G140L Wavelength: 1293 Optional_Parameters: SAMPLE-TIME=5 Number_of_Iterations: 1 Time_Per_Exposure: 12M Special_Requirements: END ORBIT Comments: Exposure_Number: 11 ! Section 6.5 Target_Name: UXUMA Config: HRS Opmode: RAPID Aperture: 2.0 Sp_Element: G140L Wavelength: 1523 Optional_Parameters: SAMPLE-TIME=5 Number_of_Iterations: 1 Time_Per_Exposure: 45M Special_Requirements: END ORBIT PHASE 0.91 TO 0.95 Comments: Visits ! Section 6 Visit_Number: 3 Visit_Requirements: PERIOD 0.196671278D AND ZERO-PHASE JD2443904.87872 On_Hold_Comments: Visit_Comments: Exact timings adjustable in consultation with PI to accomodate actual HST orbit schedule most efficiently. Exposure_Number: 12 ! Section 6.5 Target_Name: UXUMA Config: HRS Opmode: ACQ Aperture: 2.0 Sp_Element: MIRROR-N1 Wavelength: Optional_Parameters: BRIGHT=RETURN LOCATE=DEF Number_of_Iterations: 1 Time_Per_Exposure: 9S Special_Requirements: ONBOARD ACQ FOR 13-15 Comments: Exposure_Number: 13 ! Section 6.5 Target_Name: UXUMA Config: HRS Opmode: RAPID Aperture: 2.0 Sp_Element: G140L Wavelength: 1293 Optional_Parameters: SAMPLE-TIME=5 Number_of_Iterations: 1 Time_Per_Exposure: 12M Special_Requirements: Comments: Exposure_Number: 14 ! Section 6.5 Target_Name: UXUMA Config: HRS Opmode: RAPID Aperture: 2.0 Sp_Element: G140L Wavelength: 1523 Optional_Parameters: SAMPLE-TIME=5 Number_of_Iterations: 1 Time_Per_Exposure: 12M Special_Requirements: END ORBIT Comments: Exposure_Number: 15 ! Section 6.5 Target_Name: UXUMA Config: HRS Opmode: RAPID Aperture: 2.0 Sp_Element: G140L Wavelength: 1293 Optional_Parameters: SAMPLE-TIME=5 Number_of_Iterations: 1 Time_Per_Exposure: 45M Special_Requirements: END ORBIT PHASE 0.91 TO 0.95 Comments: 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: ! ! ! Note: this is PI address, but not clear from listing below whether ! Institution also included in default PI Address - this is needed ! It does include Institution (N.Fulton-11/20/95) ! ! Holmbury St. Mary,Dorking, ! Surrey RH5 6NT,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! ! 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