! Proposal 5877, submission 2 ! PI: Steven Federman ! Received Fri Mar 10 15:38:54 EST 1995 ! From: pjames@astro.utoledo.edu ! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5877,v 8.1 1995/11/30 21:21:46 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: Alice Berman ! Phone: 410 338-4462 , E-mail: aberman@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Proposal_Information ! Section 4 Title: The ^11B/^10B Ratio in the Interstellar Medium Proposal_Category: GO Scientific_Category: Interstellar Medium Cycle: 5 Investigators PI_name: Steven Federman PI_Institution: University of Toledo CoI_Name: David Lambert CoI_Institution: University of Texas Contact: N CoI_Name: Yaron Sheffer CoI_Institution: University of Texas Contact: N CoI_Name: Jason Cardelli CoI_Institution: Villanova University Contact: N Abstract: ! Free format text (please update) We propose to measure the local interstellar ^11B/^10B ratio with the GHRS. These observations will provide the first measurements of the boron isotopic ratio beyond the solar system. The solar system ratio requires a source that enhances the ^11B/^10B ratio over that expected from spallation. Additional spallation via low energy galactic cosmic rays, whose flux is not directly measurable, may be the source. We will determine this flux from our data, and we will study the consequences of the derived flux on interstellar chemical processes and thermodynamics. Since production of ^11B is also possible in supernovae, our flux will be an upper limit. Questions ! Free format text (please update) Observing_Description: The targets were selected on the basis of the amount of neutral gas along the line of sight and of the simplicity of the absorption profile (in terms of velocity components) seen in high-resolution ground-based observations of K I (Hobbs 1974 ApJ 191 381) and of Na D (Welty, Hobbs & Kulkarni 1994 ApJ 436 152). Neutral potassium and sodium are found in appreciable quantities only in neutral gas because their ionization potentials are less than hydrogen's. For our investigation, most of the neutral material must reside in a single velocity component. Furthermore, the column density of hydrogen must be similar to that in the main component (v_helio = -15 km s^-1) toward Zeta Oph [N(H) = 1.32 * 10^21 cm^-2 (Savage, Cardelli & Sofia 1992 ApJ 401 706)]. The constraint derives from our detection of B II LAMBDA 1362 with an equivalent width of 1.78 +/- 0.29 mAngstrom in this velocity component (Federman et al. 1993). The design of our experiment revolves around our detection of B II toward Zeta Oph (Federman et al. 1993). Although not fully resolved even in the echelle mode, ECH-A can produce spectra revealing a broadened line with an asymmetry caused by the presence of the two isotopes. Synthetic spectra, based on our Zeta Oph results with G160M, clearly show absorption from both isotopes when ECH-A is utilized. A signal-to-noise ratio of 500 is required for our observations. Lower signal-to-noise ratios will mask the presence of any broadening and asymmetry. The synthesis was based on a shift of 13.3 mAngstrom (Joensson et al. 1994) and an isotopic ratio, ^11B/^10B = 4:1. We are also observing interstellar Ga II LAMBDA 1414 as a guide to the complexity of the component structure for our sight lines beyond what is possible from K I and Na D. Of particular note is that the B II and Ga II lines have similar strengths. Like boron, gallium is predominantly singly ionized; these two elements have similar reference (solar) abundances and they have similar depletions in the main component toward Zeta Oph. Absorption from Ga II based on ECH-A data only appears in this component (Cardelli, Ebbets & Savage 1991 ApJ 383 L23). Moreover, the oscillator strengths for B II LAMBDA 1362 and Ga II LAMBDA 1414 are similar. Cardelli et al. (1991) clearly detected the Ga II line from spectra with a signal-to-noise ratio of ~ 100. We based our exposure times on a S/N of 500 so that the Ga II line can be used as a template for component structure and instrumental profile in our analysis of B II LAMBDA 1362. Gallium has 2 isotopes as well as hyperfine components; we expect insignificant wavelength shifts and any resulting changes to the line profile from their presence. Of all the known interstellar lines, gallium absorption is the most similar to boron's, and even with some uncertainty arising from the presence of Ga isotopes and hyperfine structure, the Ga II line is the best template for our analysis. The exposure times were derived in the following way. Each of our stars was observed with OAO-2 and their fluxes were presented by Code & Meade (1979 ApJS 39 195). The fluxes at LAMBDA LAMBDA 1362, 1414 were derived from interpolation and were multiplied by the sensitivity of ECH-A in orders 41 and 40, respectively, taking into consideration the blaze function, the efficiency using STEP- PATT=7 (4 samples per diode), and the loss in sensitivity when using the Small Science Aperture (SSA). (The SSA is required for the highest possible resolution afforded by the GHRS.) For signal-to-noise ratios of 500 per pixel, the total exposure times were obtained for the B and Ga observations by multiplying the exposure time per diode by 4 for FP-SPLIT=4. The calculations also included the effects of scattered light. In deriving the number of orbits per target, we assumed BRIGHT=RETURN would be used with mirror N1 for a total acquisition time of 37^m per star. For this initial survey, we will observe three stars. Real_Time_Justification: None. Calibration_Justification: None. Additional_Comments: Should the need arise for more detailed descriptions of the line profile, we will obtain ultra-high-resolution spectra (LAMBDA/DELTA LAMBDA ~ 600,000) on K I LAMBDA 7699 from McDonald Observatory. ! This text block was moved from the Real_Time_Justification section 6/9/95. Fixed_Targets ! Coordinates updated from Hipparcos 6/6/95 - AFB Target_Number: 1 Target_Name: HD38771 Alternate_Names: KAPPA-ORI, GSC5351-00760 Description: ISM, HI CLOUD, STAR, B0-B2 III-I, Position: RA = 05H 47M 45.38S +/- 0.01S, DEC = -09D 40' 10.8" +/- 0.1" Equinox: J2000 RV_or_Z: V = +21.0 RA_PM: -0.0002 Dec_PM: -0.005 Epoch: 2000.000 Annual_Parallax: 0.015 Flux: V = 2.07 B-V = -0.17 E(B-V) = 0.07 F-CONT(1362) = 1.78 E-8 F-CONT(1414) = 1.42 E-8 Comments: THIS IS A BRIGHT STAR. Coordinates are from Hipparcos INCA ! Original values: ! Position: RA = 5H 45M 23.0S +/- 0.003S, ! DEC = -9D 41' 9.5" +/- 0.04" ! Equinox: 1950.0 ! Epoch: 1950.0 ! Flux: V = 2.06 Target_Number: 2 Target_Name: HD143275 Alternate_Names: DELTA-SCO, GSC6779-02194 Description: ISM, HI CLOUD, STAR, B0-B2 V-IV, Position: RA = 16H 00M 20.01S +/- 0.01S, DEC = -22D 37' 18.0" +/- 0.1" Equinox: J2000 RV_or_Z: V = -7.0 RA_PM: -0.0007 Dec_PM: -0.025 Epoch: 2000.000 Annual_Parallax: Flux: V = 2.28 B-V = -0.12 E(B-V) = 0.16 F-CONT(1362) = 1.47 E-8 F-CONT(1414) = 1.21 E-8 Comments: THIS IS A BRIGHT STAR. Coordinates are from Hipparcos INCA ! Original values: ! Position: RA = 15H 57M 22.3S +/- 0.003S, ! DEC = -22D 28' 51.4" +/- 0.04", ! Equinox: 1950.0 ! Epoch: 1950.0 ! Flux: V = 2.32 Target_Number: 3 Target_Name: HD149757 Alternate_Names: ZETA-OPH, GSC5632-01042 Description: ISM, HI CLOUD, MOLECULAR CLOUD, STAR, MAIN SEQUENCE O, Position: RA = 16H 37M 9.54S +/- 0.01S, DEC = -10D 34' 1.6" +/- 0.1" Equinox: J2000 RV_or_Z: V = -15.0 RA_PM: -0.0008 Dec_PM: -0.023 Epoch: 2000.000 Annual_Parallax: 0.003 Flux: V = 2.58 B-V = +0.02 E(B-V) = 0.32 F-CONT(1362) = 4.58 E-9 F-CONT(1414) = 4.29 E-9 Comments: THIS IS A BRIGHT STAR. Coordinates are from Hipparcos INCA ! Original values: ! Position: RA = 16H 34M 24.1S +/- 0.003S, ! DEC = -10D 28' 2.8" +/- 0.04", ! Equinox: 1950.0 ! Epoch: 1950.0 ! Flux: V = 2.56 ! 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: On_Hold_Comments: Visit_Comments: Exposure_Number: 10 Target_Name: HD38771 Config: HRS Opmode: ACQ Aperture: 2.0 Sp_Element: MIRROR-A1 Wavelength: Optional_Parameters: BRIGHT=RETURN, SEARCH-SIZE=3 Number_of_Iterations: 1 Time_Per_Exposure: 1.8S Special_Requirements: ONBOARD ACQ FOR 11 Comments: CENTER IN LSA, BRIGHTEST STAR IN FIELD TIME-STEP=0.2S Exposure_Number: 11 Target_Name: HD38771 Config: HRS Opmode: ACQ/PEAKUP Aperture: 0.25 Sp_Element: MIRROR-A1 Wavelength: Optional_Parameters: SEARCH-SIZE=5 Number_of_Iterations: 1 Time_Per_Exposure: 5.0S Special_Requirements: ONBOARD ACQ FOR 12 Comments: TIME-STEP=0.2S Exposure_Number: 12 Target_Name: HD38771 Config: HRS Opmode: ACQ/PEAKUP Aperture: 0.25 Sp_Element: MIRROR-A1 Wavelength: Optional_Parameters: SEARCH-SIZE=5 Number_of_Iterations: 1 Time_Per_Exposure: 5.0S Special_Requirements: ONBOARD ACQ FOR 13-16 Comments: TIME-STEP=0.2S Exposure_Number: 13 Target_Name: HD38771 Config: HRS Opmode: ACCUM Aperture: 0.25 Sp_Element: ECH-A Wavelength: 1360.5 Optional_Parameters: FP-SPLIT=STD, STEP-PATT=7, COMB=FOUR, DOPPLER=DEF Number_of_Iterations: 1 Time_Per_Exposure: 435.2S Special_Requirements: Comments: Exposure_Number: 14 Target_Name: HD38771 Config: HRS Opmode: ACCUM Aperture: 0.25 Sp_Element: ECH-A Wavelength: 1361.0 Optional_Parameters: FP-SPLIT=STD, STEP-PATT=7, COMB=FOUR, DOPPLER=DEF Number_of_Iterations: 2 Time_Per_Exposure: 326.4S Special_Requirements: Comments: Exposure_Number: 15 Target_Name: HD38771 Config: HRS Opmode: ACCUM Aperture: 0.25 Sp_Element: ECH-A Wavelength: 1412.7 Optional_Parameters: FP-SPLIT=STD, STEP-PATT=7, COMB=FOUR, DOPPLER=DEF Number_of_Iterations: 2 Time_Per_Exposure: 326.4S Special_Requirements: Comments: Exposure_Number: 16 Target_Name: HD38771 Config: HRS Opmode: ACCUM Aperture: 0.25 Sp_Element: ECH-A Wavelength: 1413.3 Optional_Parameters: FP-SPLIT=STD, STEP-PATT=7, COMB=FOUR, DOPPLER=DEF Number_of_Iterations: 2 Time_Per_Exposure: 326.4S Special_Requirements: Comments: Visit_Number: 2 Visit_Requirements: ! 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