! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 6040,v 6.1 1995/11/10 14:36:38 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 11:27:52 EST 1994 ! Proposal_Information ! Section 4 Title: Ultra--high angular resolution of O3 stars in the Carina Nebula and in the LMC Proposal_Category: GO Scientific_Category: Hot Stars Cycle: 5 Investigators PI_name: R. Burg PI_Institution: Johns Hopkins University CoI_Name: M. G. Lattanzi CoI_Institution: Space Telescope Science Institute Contact: Y CoI_Name: N. R. Walborn CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: J. E. Pringle CoI_Institution: Institute of Astronomy Contact: ! Y or N (designate at most one contact) CoI_Name: J.L. Hershey CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: B.J. McLean CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: I.N. Evans CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) The upper mass limit for individual stars remains an open question of great importance in astronomy. Theory is not currently capable of placing a firm upper mass limit and, therefore, the problem is an observational one. O3 stars in giant HII regions are the hottest and presumably the most massive Population I stars. Of the 70 definite and possible members of this class, 59 are in the Magellanic Clouds (Walborn 1994). The Carina Nebula has the highest concentration of these stars in the Milky Way and hence provides the most accessible laboratory for the investigation of the most massive stars. The LMC has the most extreme examples; i.e., those objects which are candidates for the most massive star. We propose to use the Fine Guidance Sensor (FGS) in its interferometric mode to investigate a complete sample of six O3 stars in Carina and three extreme objects in the LMC in order to establish if these stars are massive single stars or if, like R136a in the LMC, they are multiple star systems. Questions ! Free format text (please update) Observing_Description: All of our proposed exposures use the TRANS mode of the astrometer FGS (FGS 3). As described in the FGS Instrument Handbook (Version 4.0), and in recently published papers (Bernacca et al. 1993, Lattanzi et al. 1994) this mode samples the interference fringe produced by the Koester's prism interferometer, the ``heart'' of the Fine Guidance Sensor. There are two Koester's prism interferometers in each FGS. These are fed by a beam--splitter to give sensitivity in two orthogonal directions, usually referred to as X and Y axes. Therefore, each FGS3 TRANS scan produces two fringes which can then be independently analyzed for signatures other than those characteristic of the FGS3 standard single star UP69. Indeed, deviations from the single star fringes are used to measure double, or multiple, stars projected separations. On--sky separation and position angle are easily derived from these measurements and telescope attitude data (Bernacca et al. 1993 and references therein). Accurate V magnitudes are also derived from the same counts used to construct the fringes and provided by the 4 photomultipliers (two per axis) which detect the photons from the Koester's prisms (Bucciarelli et al. 1994; Bernacca et al. 1994). Experience with observations very similar to those proposed here (Bernacca et al. 1993 and 1994; Lattanzi et al. 1994, and references therein) indicate that the FGS interferometers are capable of measuring separations smaller than 0.015 arcsec and position angles to better than 1 deg. We request one visit per target. Following the procedure for the calculation of the number of orbits given in the Cycle 5 Phase I Proposal Instructions volume, each visit comprises a guide star acquisition (12 min), the set--up time (including the selected filter) for TRANS mode (3 min), then the science exposure. Our science exposure consists of 30 TRANS scans of 2sec point1 on the sky each (i.e., 1sec point5 per FGS axis) sampled every 0sec point0008 (the pixel size per axis is 0sec point0006). Since each sample takes a fixed 0.025 sec, the 30 scans take 31.3 min, for a total of 12+3+31.3 = 46.3 min per visit. This is less than the visibility period per orbit. Therefore, we request one orbit per target. Recent observations (Lattanzi et al. 1994 and references therein) show that scans with the same pixel size, and through the PUPIL element give optimal resolution with minimum scan time. Consecutive scans are required for three reasons. First, spacecraft jitter can corrupt fringes. With multiple scans one can identify jitter--corrupted fringes and reject them. Second, analysis of multiple scans is the only reliable way to check on the repeatibility of a detection. Finally, multiple scans are co--added to increase the signal--to-- noise ratio (S/N). This is crucial for best resolution during the reductions and to allow for any star variability, and higher background due to diffuse light emission from nebulosity around the stars. Successful exposures should yield co--added fringes with typical S/N > 60. Two of our targets are too bright to be observed with the PUPIL element and the neutral density filter (F5ND) is required. This filter as been very little used with TRANS observations and some degradation of the fringes is expected. Also, it is necessary to have F5ND fringes of the FGS single star standard UP69. Routine TRANS mode calibration observations on UP69 run by the STScI do not foresee the F5ND filter. We have therefore added one calibration orbit on UP69. Length, pixel size, and number of scans in the calibration visit are the same as for the science observations. This calibration should be placed as close in time as possible to the F5ND science observations. Should the STScI Cycle 5 calibration plan for TRANS mode include the F5ND filter, the calibrations orbit requested would not be necessary. Real_Time_Justification: None. Calibration_Justification: ! Move appropriate text from Real_Time_Justification !The F5ND filter has not been calibrated by the Observatory. !This filter is needed for 2 of the 7 targets in our list. Additional_Comments: !If the Observatory decides, as a result of the calibration requirements !for the FGS in Cycle, to proceed with the routine calibrations of the !F5ND filter Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: HDE269810 Alternate_Names: Description: EXT-STAR, Giant O Position: RA = 05H 35M 13.93S +/- 0.1S, DEC = -67D 33' 26.7" +/- 1", PLATE-ID=06B0 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=12.3 +/- 0.1, B-V=-0.23, TYPE=O3III ! Include at least V and B-V Comments: Target_Number: 2 Target_Name: LMC-053705-662136 Alternate_Names: Sk-66 172 Description: EXT-STAR, Giant O Position: RA = 05H 37M 05.57S +/- 0.1S, DEC = -66D 21' 35.4" +/- 1", PLATE-ID=06B0 ! Most common specification format is 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=13.1 +/- 0.1, B-V=-0.12, TYPE=O3III ! Include at least V and B-V Comments: Target_Number: 3 Target_Name: LMC-045659-662438 Alternate_Names: LH10-3209, GSC8889-00615 Description: EXT-STAR, Giant O Position: RA= 04H 56M 58.92S +/- 0.1S, DEC = -66D 24' 39.0" +/- 1", PLATE-ID=06AF ! Most common specification format is 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=12.66 +/- 0.01, B-V=-0.11 +/- 0.01, TYPE=O3III ! Include at least V and B-V Comments: Target_Number: 4 Target_Name: HD93129A Alternate_Names: GSC8626-02805 Description: STAR, Supergiant O Position: RA = 10H 43M 57.30S +/- 0.1S, DEC = -59D 32' 51.2" +/- 1", PLATE-ID=ZZZQ ! Most common specification format is 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=7.3 +/- 0.1, B-V=0.22 ! Include at least V and B-V Comments: Target HD93129B is TRANSed together with HD93129A Target_Number: 5 Target_Name: HD93205 Alternate_Names: GSC8626-02810 Description: STAR, Main Sequence O Position: RA = 10H 44M 33.90S +/- 0.1S, DEC = -59D 44' 15.2" +/- 1", PLATE-ID=ZZZQ ! Most common specification format is 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=7.8 +/- 0.1, B-V=0.05 ! Include at least V and B-V Comments: Target_Number: 6 Target_Name: HD93250 Alternate_Names: GSC8626-02075 Description: STAR, Main Sequence O Position: RA = 10H 44M 45.13S +/- 0.1S, DEC = -59D 33' 55.0" +/- 1", PLATE-ID=ZZZQ ! Most common specification format is 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=7.4 +/- 0.1, B-V=0.15 ! Include at least V and B-V Comments: Target_Number: 7 Target_Name: HD303308 Alternate_Names: GSC8626-02808 Description: STAR, Main Sequence O Position: RA = 10H 45M 06.05S +/- 0.1S, DEC = -59D 40' 06.1" +/- 1", PLATE-ID=ZZZQ ! Most common specification format is 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=8.2 +/- 0.1, B-V=0.13 ! Include at least V and B-V Comments: Target_Number: 8 Target_Name: HD93128 Alternate_Names: Description: STAR, Main Sequence O Position: RA = 10H 43M 54.00S +/- 0.1S, DEC = -59D 32' 56.0" +/- 1", PLATE-ID=ZZZQ ! Most common specification format is 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=8.8 +/- 0.1, B-V=0.24 ! Include at least V and B-V Comments: Target_Number: 9 Target_Name: Mk42 Alternate_Names: Description: EXT-STAR, Supergiant O Position: RA=05H 38M 42.22S +/- 0.05S, DEC=-69D 05' 55.3" +/- 0.1" Equinox: J2000 RV_or_Z: RA_PM: Dec_PM: Epoch: Annual_Parallax: Flux: V=12.7 +/- 0.1, B-V=0.0 +/- 0.1 Comments: ! Target_Number: 9 ! Target_Name: NGC188-004242+851414 !Alternate_Names: Upgren 69 ! Description: STAR, Main Sequence O ! Position: RA = 9.46625D +/- 0.0004D, DEC = 84.9632778D +/- 0.002D, PLATE-ID=ZZZZ ! Most common specification format is ! Equinox: 1950 ! 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=9.58 +/- 0.05, B-V=0.5 ! Include at least V and B-V ! Comments: Calibration star, please put it on hold !********************************************************************* Scan_Data ! Appendix B !*************************************************************************** ! 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 F ! 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