! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 6311,v 4.1 1995/06/16 16:58:02 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: Denise Taylor ! Phone: 410 338-4824 , E-mail: dctaylor@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Date generated: Sun Dec 18 11:52:26 EST 1994 ! Proposal_Information ! Section 4 Title: The Structure of Nova Shells Proposal_Category: GO Scientific_Category: Interstellar Medium Cycle: 4 Investigators PI_name: Michael Shara 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: Dina Prialnik CoI_Institution: Tel-Aviv University 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: David Zurek CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) Recent WFPC2 observations of the recurrent nova T Pyxidis show that the ejected material from the previous eruptions is neither uniform nor isotropic. Rather, the ejecta is distributed in hundreds of unresolved knots. If this result is the norm for all nova ejecta then all previous mass estimates and ejection models for nova shells are probably incorrect. Observationally determined masses of nova shells provide a very important test to the nova theory. We are proposing to use WFPC2 to determine if 1) all nova shells are in fact broken into knots, and, for the closest shells, 2) to determine the size distribution of these knots. In addition WFPC2 observations of T Pyxidis will enable us to determine whether the clumpy shell is expanding. Finally, we are asking for a reendorsement (granted in cycles 1 and 4) to observe the effects of the next eruption of T Pyx (once in a generation and now several years overdue) on its multitude of circumstellar knots. Questions ! Free format text (please update) Observing_Description: We will image the structure of nova shell around T Pyx with WFPC2 using narrow-band filter (NII) corresponding to the brightest spectral feature seen in shell spectra. Real_Time_Justification: None Calibration_Justification: Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: T-PYXIDIS Alternate_Names: Description: STAR,RECURRENT NOVA,SHELL Position: RA=9H 04M 41.500S +/- 0.02S,DEC=-32D 22' 47.00" +/- 0.2",PLATE-ID=04J9 Equinox: 2000 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=14.0 +/- 1.0 ! Include at least V and B-V Comments: ! 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 ! GUIDing TOLerance ! ORIENTation 45D TO 225D ! ORIENTation TO FROM ! ORIENTation TO FROM NOMINAL ! SAME ORIENTation AS ! CVZ ! PARallel ! AFTER [BY [TO ]] ! AFTER ! BEFORE ! BETWEEN AND ! GROUP WITHIN