! File: 4392C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:09:54:36 coverpage: title_1: ABSORPTION LINE STUDIES OF THE HIGH VELOCITY title_2: CLOUD M II - CYCLE 3 SUPPLEMENTAL sci_cat: INTERSTELLAR MEDIUM sci_subcat: ABSORPTION LINES proposal_for: GO pi_title: DR. pi_fname: LAURA pi_lname: DANLY pi_inst: SPACE TELESCOPE SCIENCE INSTITUTE pi_country: USA pi_phone: 410-338-4422 hours_pri: 7.00 num_pri: 1 hrs: Y funds_amount: 61725 funds_length: 12 funds_date: JAN-94 off_fname: PETER off_lname: STOCKMAN off_title: ACTING DIRECTOR off_inst: SPACE TELESCOPE SCIENCE INSTITUTE off_addr_1: 3700 SAN MARTIN DRIVE off_city: BALTIMORE off_state: MD off_zip: 21218 off_country: USA off_phone: 410-338-4700 ! end of coverpage abstract: line_1: The extremely fortuitous alignment of HD 93521 and BD +38 2182 line_2: (~25 arcmin separation, z=1.5, 4.1 respectively) provides a rare line_3: opportunity to study the distribution and physical nature of gas line_4: in the milky way halo. Recent results from our IUE observations line_5: show that (1) the HVC M II is detected in absorption toward the line_6: more distant star, BD +38 2182, and (2) some evidence is found line_7: for spatial variations on scales less than 12 pc. Both of these line_8: observations have great implications for models of halo gas line_9: production. We wish to observe six setting on BD +38 2182 which, line_10: when added to the three other setting on this star that will be line_11: taken as part of our Cycle 2 program, make up a complete, line_12: complementary set of data by which to confirm and extend our line_13: studies. ! ! end of abstract general_form_proposers: lname: DANLY fname: LAURA title: DR. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: KUNTZ fname: KIP title: MR. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We propose to observe BD +38 2182 with three grating setting line_2: and two Echelle-B settings. The central wavelenths and species to line_3: be studied are listed after each setting. The set of observations is line_4: designed to complement the observations taken by L. Spitzer toward HD line_5: 93521 during his GTO program. line_6: \noindent line_7: BD +38 2182 (l=182.2, b=62.2, MK=B2V, V=11.2, d=4.6 kpc, z=4.1 kpc) line_8: \noindent line_9: G160M grating, SSA: line_10: \medskip line_11: $\lambda_c$=1312.0 \hskip 0.5cm t(exp)=45$^m$ \hskip 0.5cm Si I, O line_12: I, C I, Si II line_13: $\lambda_c$=1343.0 \hskip 0.5cm t(exp)=50$^m$ \hskip 0.5cm O I, C line_14: II, C II*, Cu II line_15: $\lambda_c$=1205.0 \hskip 0.5cm t(exp)=66$^m$ \hskip 0.5cm H I, C line_16: I, N I, Si II, Mn II, S III line_17: \noindent line_18: Echelle-B, SSA: line_19: \medskip ! question: 3 section: 2 line_1: $\lambda_c$=1805.0 \hskip 0.5cm t(exp)=1.4$^h$ \hskip 0.5cm S I, Si line_2: II, Ni II line_3: $\lambda_c$=2370.0 \hskip 0.5cm t(exp)=1.0$^h$ \hskip 0.5cm Fe II line_5: The first four settings toward BD +38 2182 are designed to achieve a line_6: 3$\sigma$ detection limit of 6 mA (S/N=30 for the grating settings and line_7: S/N=9 for the Echelle-B settings). Because of the good response at line_8: $\lambda$2370, we will integrate to achieve a S/N (=~25) which will line_9: give us a 3 mA detection limit. ! question: 3 section: 3 line_1: line_2: \bigskip line_3: These lines of sight will be combined with the data on BD +38 2182 line_4: that is obtained during our current Cycle 2 program (ID no. 3706). The line_5: Cycle two setups will cover the wavelength region around the high ions line_6: of C IV, Si IV, and N V. We will also get numerous other species with line_7: a range of ionization potential. In addition to studying the line_8: ionization and kinematic structure, we will have sufficient data for a line_9: detailed analysis of the depletion patterns and abundances which line_10: should prove extremely interesting, especially in the High Velocity line_11: Cloud. ! question: 4 section: 1 line_1: The improvement in resolution and S/N that is made available through line_2: teh GHRS on HST is required to carry out the scientific aims of the line_3: proposal. We have fully analyzed the IUE spectra which provide some line_4: tantalizing hints at what is out there, particularly with regard to line_5: the HVC detection. However, the IUE is simply not able to provide the line_6: quality of data required to make a quantitative program of halo gas line_7: measurement as envisioned here, particularly for a star of V=11.2. Of line_8: course, the ultraviolet regime is required because of the wide range line_9: of ion species available for study that are not available from the line_10: ground. line_11: \medskip line_12: Observations of HD 93521 with Copernicus are available in the line_13: literature, and provide even more useful ions, including O VI. line_14: \medskip line_15: The PI also has observed this field using the 140' single dish radio line_16: telescope at NRAO-Greenbank (with E. Albert) and using the Westerbork line_17: Interferometric Radio Telescope (with B. Wakker and H. Van Woerden). line_18: These data are being analyzed currently to provide the best line_19: information on the small scale variations in the H I distribution. ! question: 4 section: 2 line_1: The ultraviolet fluxes for the G160M grating setting observations of line_2: BD +38 2182 were measured directly from our IUE line_3: spectra of the stars. No additional corrections (i.e. for line_4: interstellar extinction) are required. The count rates (in line_5: counts/sec/diode) were determined by multiplying the fluxes by the line_6: throughputs for the GHRS/G160M and for the LSA/SSA aperture ratio line_7: given in the GHRS Instrument Handbook (Version 3.0, January 1992). line_8: \medskip line_9: We were not able to measure directly the fluxes from BD +38 2182 line_10: longward of 2000$\AA$ as we do not have any LWP spectra of this star line_11: (it's magnitude and early spectral type made it unfeasible to observe line_12: in an IUE shift). To determine the flux, we scaled from IUE spectra line_13: toward a standard B2V star, HD 32612 (LWP 7007). The count rates were line_14: determined as above for the Echelle-B throughputs, and were also line_15: scaled by the normalized blaze function given in Figure 4-14 of the line_16: Handbook. line_17: \medskip line_18: For all the grating settings, the count-rates were above the line_19: instrumental background. Exposure times were determined by line_20: t=(S/N)$^2$/(count-rate). They are listed in Section 2. For the line_21: Echelle-B settings, the inter-order scattered light had to be included line_22: in the S/N calculations. In the cases of $\lambda$1805 and line_23: $\lambda$2602, the count-rates were low enough that the instrumental ! question: 4 section: 3 line_1: background had to also be considered. The exposure times listed in line_2: Section 2 were calculated according to Equation 4-8 in the Handbook, line_3: as explained. line_4: \medskip line_5: The S/N ratios were chosen to give limiting equivalent widths that line_6: would compare reasonably with the Echelle data taken by L. Spitzer in line_7: his GTO program. In order to make a meaningful comparison, we have line_8: tried to optimize our program to create a uniform data set, given the line_9: limitation that the Echelle-A is no longer available. line_10: \newpage ! question: 5 section: 1 line_1: none ! question: 6 section: 1 line_1: GHRS wavelength calibrations for all spectra ! question: 7 section: 1 line_1: The proposers have had extensive experience with reducing spectral line_2: data, both optical and ultraviolet. Initial reduction, and, if line_3: necessary, recalibration shall be accomplished at Space Telescope line_4: Science Institute using the STSDAS software. Detailed analysis to line_5: determine column densities, velocities, and velocity widths of the line_6: absorption line profiles will be accomplished with the existing KDAF line_7: software package (an IDL based IUE-RDAF derivative). This procedure line_8: will ensure a reduction that adheres to Space Telescope standards, yet line_9: will allow easy comparison with existing IUE and optical data. Our line_10: Cycle 2 data will have already been delivered and our data reduction line_11: and analysis procedures will by then be routine. line_12: \smallskip The data on both the high ionization species {\it and} the line_13: weakly ionized and neutral species will be analyzed in the context of line_14: models for the production of gas in the halo. Based on our work from line_15: our Cycle 2 program, we will be developing (with other collaborators line_16: R. enjamin and P. Shapiro) and refining models for predicting the line_17: non-equilibrium radiative cooling, ionization, and recombination of line_18: halo gas (for descriptions, see Shapiro, P.R. and Benjamin, R. A. line_19: 1991, Publ. A.S.P., Vol. 103, in press; Shapiro, P. R. 1991, proc. line_20: from I.A.U. Symp. No. 144 on ``The Interstellar Disk-Halo Connection line_21: in Galaxies, p 417). We wish to determine if the observed column line_22: densities {\it and} kinematics give a self-consistent picture of both line_23: the heating and flow which are predicted according to the galactic ! question: 7 section: 2 line_1: fountain. Whatever results are obtained on the physical conditions of line_2: the gas will shed light as to its origin. ! question: 8 section: 1 line_1: This proposal is one of several programs (including three accepted GO line_2: programs; see Question 8) designed to study gas in the environments of line_3: galaxies. These programs have been tailored specifically to meet the line_4: objectives outlined in the P.I.'s (accepted) Hubble Fellowship line_5: proposal. The goal of the Hubble Fellowship research is to study gas line_6: which is in the vicinity of a variety of galaxies, and is therefore line_7: subjected to a range of interstellar and intergalactic environments. line_8: Central to this research is a detailed study of the production and line_9: maintenance of Milky Way halo gas, where we can expect to obtain the line_10: highest quality data and develop the most detailed models. Accurate line_11: means to interpret quantitative spectroscopic data are critical to the line_12: interpretation of QSO absorption lines. \medskip Related Cycle 3 line_13: proposals includ14: \bigskip Galacti15: \smallskip $\bullet$ ``New line_14: Probes for the Intermediate Velocity Arch" (Danly, L. and Kuntz, K.D.) line_15: \medskip $\bullet$ ``The Distance of High Velocity Clouds" (Wakker, line_16: B. P., Danly, L., Schwarz, U. J., and Van Woerden, H.) \bigskip line_17: Extragalactic: \smallskip $\bullet$ ``Quasar Absorption Line Studies line_18: of Starburst Galaxy Environments" (Norman, C.N., Blades, J.C., Danly, line_19: L., and Heckman, T) \medskip $\bullet$ ``The Structure of the Coma line_20: Cluster: A Search for Cool Absorbing Gas" (Urry, C.M., line_21: Branduardi-Raymont G., Danly, L., Fitchett, M.J., Mushotzky, R.F.) line_22: \medskip $\bullet$ ``An Investigation of Strong Local Ly$\alpha$ line_23: Systems" (Urry, C. M., Bowen D., Maraschi, L., Danly, L., Bruhweiler, ! question: 8 section: 2 line_1: F. C., Falomo, R., Grady, C.) ! question: 9 section: 1 line_1: No. 3706 -- ``The Nature of Gaseous Loops in the Milky Way Halo" line_2: No. 2644 -- ``The Environments of Starburst Galaxies: Absorption Line line_3: Studies of Galactic Outflows" line_4: \bigskip line_5: The nature of both of these programs is described in Question 8. In line_6: particular, No. 3706 is closely related to the current line_7: proposed program, and is described in the Scientific Justification. ! question: 9 section: 2 line_1: No. 3706 -- one spectrum has been taken and is being analyzed. line_2: No. 2644 -- one spectrum has been taken and is being analyzed. ! !end of general form text general_form_address: lname: Danly fname: Laura title: Dr. category: PI inst: Space Telescope Science Institute addr_1: 3700 San Martin Drive city: Baltimore state: Md zip: 21218 country: USA phone: 410-338-4422 from_date: 01-JAN-94 to_date: 01-JAN-95 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: BD+38D2182 name_2: GSC03009-02485 descr_1: G,508,509,510 descr_2: A,110 pos_1: PLATE-ID=01R8, pos_2: RA= 10H 49M 12.9S +/- 0.1S, pos_3: DEC= +38D 0' 14.5" +/- 1" equinox: J2000 rv_or_z: V=79 fluxnum_1: 1 fluxval_1: V=11.2, TYPE=B2V, E(B-V)=0.02 fluxnum_2: 2 fluxval_2: B-V=-0.22 fluxnum_3: 3 fluxval_3: F-CONT(1240) = 36 E-13 fluxnum_4: 4 fluxval_4: F-CONT(1300) = 24 E-13 fluxnum_5: 5 fluxval_5: F-CONT(1400) = 22 E-13 fluxnum_6: 6 fluxval_6: F-CONT(1800) = 12 E-13 fluxnum_7: 7 fluxval_7: F-CONT(2400) = 7 E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: BD+38D2182 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 3.6S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3/ 1.0 - 5.2; req_2: ONBOARD ACQ FOR 1.10 - 5.20 comment_1: STEP-TIME = 0.4 ! linenum: 1.100 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1312 num_exp: 1 time_per_exp: DEF priority: 1 req_1: CALIB FOR 1.2; req_2: SEQ 1.1-1.2 NO GAP ! linenum: 1.200 targname: BD+38D2182 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1312 num_exp: 1 time_per_exp: 40M s_to_n: 28 fluxnum_1: 4 priority: 1 param_1: FP-SPLIT=STD ! linenum: 2.100 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1343 num_exp: 1 time_per_exp: DEF priority: 1 req_1: CALIB FOR 2.2; req_2: SEQ 2.1-2.2 NO GAP ! linenum: 2.200 targname: BD+38D2182 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1343 num_exp: 2 time_per_exp: 25M s_to_n: 28 fluxnum_1: 4 priority: 1 param_1: FP-SPLIT=STD ! linenum: 3.100 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1205 num_exp: 1 time_per_exp: DEF priority: 1 req_1: CALIB FOR 3.2; req_2: SEQ 3.1-3.2 NO GAP ! linenum: 3.200 targname: BD+38D2182 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1205 num_exp: 2 time_per_exp: 30M s_to_n: 30 fluxnum_1: 3 priority: 1 param_1: FP-SPLIT=STD ! linenum: 4.100 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1805 num_exp: 1 time_per_exp: DEF priority: 1 param_1: STEP-PATT=8 req_1: CALIB FOR 4.2; req_2: SEQ 4.1-4.2 NO GAP ! linenum: 4.200 targname: BD+38D2182 config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-B wavelength: 1805 num_exp: 3 time_per_exp: 30M s_to_n: 9 fluxnum_1: 4 priority: 1 param_1: FP-SPLIT=STD param_2: STEP-PATT=8 param_3: CENSOR=YES ! linenum: 5.100 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 2370 num_exp: 1 time_per_exp: DEF priority: 1 param_1: STEP-PATT=6 req_1: CALIB FOR 5.2; req_2: SEQ 5.1-5.2 NO GAP ! linenum: 5.200 targname: BD+38D2182 config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-B wavelength: 2370 num_exp: 2 time_per_exp: 30M s_to_n: 25 fluxnum_1: 7 priority: 1 param_1: FP-SPLIT=STD param_2: STEP-PATT=6 ! ! end of exposure logsheet ! No scan data records found