! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5809,v 1.1 1994/12/14 19:33:11 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: n/a ! Phone: n/a , E-mail: n/a ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: robert-752.prop ! Date generated: Wed Dec 14 14:33:04 EST 1994 ! Proposal_Information ! Section 4 Title: An HST Library of High Quality UV Spectra of Massive Stars Proposal_Category: AR Scientific_Category: Stellar Populations Cycle: 5 Investigators PI_name: Carmelle Robert PI_Institution: Space Telescope Science Institute CoI_Name: Claus Leitherer CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Timothy M. Heckman CoI_Institution: John Hopkins University Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We propose to build a high quality UV stellar library of hot, massive stars using FOS and GHRS spectra from the HST archives. The high signal-to-noise ratio and high spectral resolution achievable with the FOS and GHRS is a major factor in the uniqueness of the library. Spectra of hot, massive stars observed in different chemical environments also exist in the HST archives which will allow the creation of an extremely versatile library. UV spectral libraries of hot stars represent a fundamental tool for the study of the stellar population of star-forming regions. Hot, massive stars, which are difficult to identify directly in the optical -IR part of a composite spectrum, display on the other hand key signatures in the UV region. For example, O and Wolf-Rayet stars have broad, metallicity dependent spectral features of SiIV, CIV, and HeII due to their stellar winds. The study of stellar populations based on UV spectral synthesis requires therefore a high quality spectral library (S/N \buildrel > / ~ 30, resolution ~eq 200-300 km s^-1) of objects covering a broad range of stellar properties. A spectral library of high quality also represents a unique source of data for stellar atmosphere analysis. Questions ! Free format text (please update) Observing_Description: Real_Time_Justification: Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: Target_Name: Alternate_Names: Description: Position: ! Most common specification format is ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: 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: ! Include at least V and B-V Comments: 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 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: 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 ! ORIENTation TO ! ORIENTation TO FROM ! ORIENTation TO FROM NOMINAL ! SAME ORIENTation AS ! CVZ ! PARallel ! AFTER [BY [TO ]] ! AFTER ! BEFORE ! BETWEEN AND ! GROUP WITHIN