! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6723,v 16.1 1996/08/05 16:04:56 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: Karla Peterson ! Phone: 410-338-4774 , E-mail: peterson@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. Proposal_Information ! Section 4 Title: Physical conditions near high galactic latitude molecular clouds Proposal_Category: GO Scientific_Category: INTERSTELLAR MEDIUM Cycle: 6 Investigators PI_name: Chris Blades PI_Institution: Space Telescope Science Institute CoI_Name: Meena Sahu CoI_Institution: Space Telescope Science Institute Contact: Y ! Y or N (designate at most one contact) CoI_Name: Lida He CoI_Institution: Rensselaer Polytechnic Institute Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) Ultra high resolution observations (R ~ 10^6) of the high latitude stars HD 28497, HD 89688, HD 141569 and HD 151741, show complex NaI (D1 and D2) and Ca II K interstellar absorption line profiles. Due to their location near high galactic latitude molecular clouds, these stars are well- suited background sources for detailed spectroscopic studies of molecular clouds as well as gas in the near halo. The optical data show that the column densities are low and the clouds are well resolved with a wide range of physical conditions, making these rich and important sightlines for ultraviolet studies. We would like to study the distribution and physical characteristics of the neutral (HI), ionized (HII) and highly ionized (hot) gas associated with the individual absorbing components observed in the NaI and CaII absorption line profiles. HST GHRS spectra of the interstellar absorption lines of MgI, CI, SiII, FeII, MgII, CrII, ZnII, SiIV, CIV and NV will allow us to trace the extent of the neutral, ionized and hot gas and will be used to estimate kinetic temperatures, electron densities, pressures, the depletions of the various elements in the HI gas, and the composition of the grains. Further, these observations will determine if high galactic latitude molecular clouds are indeed embedded in the hot local interstellar medium as suggested by X-ray observations and how the physical conditions in these clouds differ from other diffuse interstellar clouds. Questions ! Free format text (please update) Observing_Description: We plan to obtain high S/N HST GHRS echelle spectra with the highest wavelength resolution possible. To achieve this, the observations will be made with the SSA and by sampling the data using four substep bins per diode. The FP-Split option will be utilized to get a better estimate of the fixed pattern noise and thus improve S/N. The lines we would like to observe are listed in the table below together with their wavelengths and the echelle setting required for the observation. The program would require four ECH-A wavelength settings and five ECH-B settings per star. The exposure times have been computed based on the UV fluxes for the stars (from published literature) and taking into account the effects of reduced GHRS echelle blaze efficiences and the reduced SSA efficiency (GHRS Handbook, Version 6.0). For S/N ~ 100:1, we need exposure times for ECH-A settings ranging from 12 to 40 minutes and ECH-B settings ranging from 6 to 20 minutes. If we take into account the target acquisition and exposure overheads and specify that the change from ECH-A to ECH-B be done during the occultation period, we would require a total of 5 orbits for HD 28497 and 6 orbits each for the other three stars. This would imply that a total of 23 orbits would be necessary to complete our proposed observations. begintabularlll SPECIES & Lambda Angstrom \ & ECHELLE SETTING, & &, CIV & 1548.19 & ECH-A36, & 1550.77 & ECH-A36, SiIV&1393.76 & ECH-A40, &1402.77 & ECH-A40, CI & around 1278 & ECH-A44, MgII&1239.93 & ECH-A45, NV & 1238.82 & ECH-A45, & 1242.8& ECH-A45, MgI & 2852.96 & ECH-B20, & 2026.48 & ECH- B28, FeII& 2600.17& ECH-B22, & 2374.46& ECH-B24, CrII& 2062.23& ECH-B27, & 2066.16& ECH-B27, ZnII& 2026.14& ECH- B28, & 2062.66& ECH-B27, SiII& 1808.01 & ECH-B31, & & , endtabular Real_Time_Justification: None None Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number:1 Target_Name:HD28497 Alternate_Names:SAO149674, HR1423, GSC5320-1896 Description:Star, B0-B2 V-IV Position: RA=04H 29M 6.92S +/-0.01S, DEC=-13D 02' 54.1" +/-0.1" Equinox:J2000 RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch:2000 Annual_Parallax: Flux:V=5.6 +/- 0.3, B-V= -0.20 +/-0.05, Type=B2V, E(B-V) = 0.10 Comments:Coordinates are from Hipparcos INCA, F(1400)=5.1E-10, F(2000)=2.44E-10 Target_Number:2 Target_Name:HD89688 Alternate_Names:SAO118248, HR4064, GSC0246-01238 Description:Star Position: RA = 10H 21M 2.00S +/- 0.01S, DEC = 02D 17' 22.8" +/- 0.1", Equinox: J2000 RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch:2000 Annual_Parallax: Flux:V=6.68 +/- 0.3, B-V= -0.08 +/-0.01, Type=B3V, E(B-V) = 0.16 Comments:Coordinates are from Hipparcos INCA, F(1400)=4.5E-11, F(2000)=3.1E-11 ! 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 WITHIN