! Proposal 6494, submission 1 ! PI: Prof. K. O. Mason ! Received Sun Feb 11 10:39:59 EST 1996 ! From: kom@msslac.mssl.ucl.ac.uk ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6494,v 7.1 1996/11/21 14:18:39 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6494,v 7.1 1996/11/21 14:18:39 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: Manning ! Phone: 410-338-4456 , E-mail: manning@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: archive-0283.mason.prop ! Date generated: Fri Dec 22 16:47:41 EST 1995 ! Proposal_Information ! Section 4 Title: Changing perspectives on accretion disk winds Proposal_Category: GO Scientific_Category: BINARIES AND STAR FORMATION Cycle: 6 Investigators PI_name: Prof. K. O. Mason PI_Institution: Mullard Space Science Laboratory CoI_Name: Dr. J. E. Drew CoI_Institution: Imperial College of Science, Technology & Medicine Contact: ! Y or N (designate at most one contact) CoI_Name: C. Knigge CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Dr. J. Stone CoI_Institution: University of Maryland Contact: ! Y or N (designate at most one contact) CoI_Name: D. Proga CoI_Institution: Imperial College of Science, Technology & Medicine Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We seek to extend our highly successful study of wind-formed lines in disk-accreting CV by observing systems at higher orbital inclination than previously, thus probing the wind to greater heights above the disk. Our previous HST data, on the system UX UMa, point to a number of hitherto unexpected phenomena in the wind, including a thick layer at its base where very little acceleration apparently takes place. We have developed a model to explain these data, but there is a pressing need to test whether it is more generally applicable. The model predicts that there should be noticable differences in the appearance of the lines as the inclination is changed between about 70 and 80 degrees. The proposed target is RW Tri. We intend to perform time resolved UV spectroscopy through eclipse to probe the wind structure, and also to sample the light curve through the orbital cycle to test for asymmetries in the disk or the wind which would affect the interpretation of the eclipse light curves. Our goal is to build a full and self-consistent model for the wind in CV and to determine where and how the wind originates. We will then be in a position to investigate what drives the wind and the effect it has on the underlying accretion disk structure. Questions ! Free format text (please update) Observing_Description: Our scientific objectives call for time sequences of spectra which (i) follow the target through eclipse by the companion star and (ii) sample the rest of the orbital cycle to characterise orbital-phase-linked variations in the line profiles. Following our cycle 5 observations of UX UMa, we plan to observe RW Tri using the G140L grating on side~1 of the GHRS which gives the optimum balance between spectral resolution and wavelength coverage for this application. The sequences of observations are chosen to optimise coverage of the target orbital cycle with the sampling implied by the HST orbit. We propose to perform each sequence in two grating settings centered at 1293A and 1523A so as to cover a range of lines of different excitation (e.g. HeII 1640A, CIV 1550A, SiIV 1397A, and NV 1240A). The orbital period of RW~Tri is 5.57 hours. Each HST orbit will cover just over 0.1 orbital cycles in RW Tri, and the eclipse itself covers 0.12 cycles, or 40 minutes. The whole eclipse cannot be accomodated comfortably in one unocculted HST orbit and still allow the pre- and post-eclipse spectrum to be properly sampled. It is important to stress the need for good coverage immediately before and after eclipse to provide a solid reference with which to compare the changes in the spectrum during eclipse. Thus the observations are designed to cover eclipse ingress and eclipse egress on separate visits. The elipse-ingress and eclipse-egress visits are planned to consist of 4 and 2 contiguous HST orbits respectively, repeated in the two grating settings (4 visits in total). The four HST-orbit sequence will start just before phase 0.4 in the RW Tri orbit and sample phase regions near 0.4, 0.7, 0.0 (eclipse) and 0.25. This sequence will be timed to emphasise the eclipse ingress and the pre-eclipse region in the third of the four HST orbits. The two HST-orbit sequence will begin at about phase 0.8 and will monitor the eclipse during the second of the two HST orbits, emphasising eclipse egress and the post-eclipse region. The first orbit of a sequence is assumed to contain the target acquisition, so that the amount of science data in this orbit is curtailed. The phase in the RW~Tri binary cycle at which this first science data segment should start is specified using the PHASE command. Provided this observation starts on time as predicted by RPS2, subsequent orbits should occur at the intended RW~Tri binary phases, in particular the eclipse coverage should be satisfactory. However, if the time required to acquire the target differs from that predicted by RPS2, then the PHASE of the first science data will also need to be modified to reflect this. The binary phase of subsequent orbits will not change, however, so as a check we include as a comment the required starting phase of the second orbit of science data in each visit. The total number of HST orbits required for this programme is 12. As described above, this is determined by the orbital phase coverage needed and not by signal-to-noise requirements. RW~Tri is bright enough to yield phase and spectrally resolved spectra suitable for our needs. The continuum near 1500A should yield a flux of 6 x 10-14 erg cm-2 s-1 A-1 (based on the IUE ULDA), which will yield a S/N of 10 per diode in about 3 minutes (0.008 in phase). The peak flux of the CIV emission line (the brightest of the wind-formed resonance lines) is at least twice that of the continuum. Real_Time_Justification: Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: RWTRI Alternate_Names: RW-TRI Description: STAR,Nova-like,Interacting Binary Position: ! Most common specification format is RA=02H 25M 36.14S +/- 0.2", ! RA=0H 0M 0.00S +/- 0S, DEC=+28D 05' 51.3" +/- 0.2", ! DEC=0D 0' 0.0" +/- 0", PLATE-ID=01H7 ! 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=13.2 +/- 0.1 ! Include at least V and B-V B-V=0.0 F-LINE(1549)=2.0 +/- 0.5 E-13 W-LINE(1549)=20 +/- 5 F-CONT(1500)=6.0 +/- 1 E-14 F-LINE(1240)=1.4 +/- 0.5 E-13 W-LINE(1240)=8.0 +/- 3 F-CONT(1200)=6.0 +/- 1 E-14 A(V)=0.6 +/- 0.2 Comments: Eclipsing star - mid-eclipse V=15.6 !Solar_System_Targets ! Section 5.2 ! Target_Number: ! Target_Name: ! Description: ! Level_1: ! Satellite of Sun ! Level_2: ! Satellite of Level_1 ! Level_3: ! Satellite of Level_2 ! Ephem_Uncert: ! Needed for REQ EPHEM CORR sp req ! Acq_Uncert: ! Needed for SAVE and USE OFFSET sp reqs ! Window: ! Flux: ! Include at least V and B-V ! Comments: ! ! !Generic_Targets ! Section 5.3 ! Target_Number: ! Target_Name: ! Description: ! Criteria: ! Flux: ! Comments: ! ! !Scan_Data ! Appendix B ! Scan_Number: ! FGS_Scan: ! Cont_or_Dwell: ! Dwell_Points: ! Dwell_Secs: ! Scan_Width: ! Scan_Length: ! Sides_Angle: ! Number_Lines: ! Scan_Rate: ! First_Line_PA: ! Scan_Frame: ! Length_Offset: ! Width_Offset: ! 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: ! Section 7.1 ! Uncomment or copy visit level special requirements needed ! Most of these requirements (including ORIENT) will limit scheduling ! PCS MODE [Fine | Gyro] ! GUIDing TOLerance ! DROP TO GYRO IF NECESSARY [NO REACQuisition] ! ORIENTation TO ! ORIENTation TO FROM ! ORIENTation TO FROM NOMINAL ! SAME ORIENTation AS ! CVZ ! PARallel ! SCHEDulability ! AFTER [BY [TO ]] ! AFTER ! BEFORE ! BETWEEN AND GROUP 1-4 WITHIN 7D GROUP 1-2 WITHIN 1D PERIOD 0.231883297D AND ZERO-PHASE JD2441129.36487 ! SEQ WITHIN