! File: 4323C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:21:50:54 coverpage: title_1: THE GASEOUS ENVIRONMENT OF THE URSA MINOR DWARF title_2: SPHEROIDAL GALAXY: CYCLE3 MEDIUM sci_cat: GALAXIES & CLUSTERS sci_subcat: GAS & DUST proposal_for: GO pi_fname: EDWARD pi_mi: W pi_lname: OLSZEWSKI pi_inst: STEWARD OBSERVATORY pi_country: USA hours_pri: 8.76 num_pri: 2 fos: Y funds_length: 12 ! end of coverpage abstract: line_1: We propose to probe the interstellar gas content of the Ursa Minor dwarf line_2: spheroidal galaxy. We have discovered a V=18.5 QSO at approximately 1 line_3: core radius from the center of UMi. We will use the FOS to look for EUV line_4: absorption lines from gas in UMi. This technique complements ground-based line_5: H I measurements, and X-ray imaging. Some of the dSph, e.g., Carina, line_6: made a significant 2nd generation of stars a few Gyr ago, despite their line_7: current low limits on gas, low stellar densities, and low escape velocity. line_8: It is still a mystery why we do not detect significant gas lost during line_9: stellar evolution. This problem is compounded in the dSph because, unlike line_10: in the analogous globular cluster gas problem, the dSph gravitational line_11: potential is dominated by dark matter, which may confine the gas. line_12: Further, Silk, Wyse, and Shields (1987) have proposed that gas lost by line_13: galaxies at high redshift can cool and accrete onto dE galaxies. There line_14: may thus be large reservoirs of gas that can be detected by UV spectroscopy. line_15: We intend to use the G270H grating, which allows us to observe the Mg II line_16: doublet, Mg I, Fe II lines, and weak Fe I, Al I, Mn II, and Ti II lines. line_17: Because of the patchy nature of the Milky Way high velocity halo gas, we line_18: will also observe a brighter, nearby QSO to ensure that we can ascribe line_19: any detections to UMi. Finally we will take a low resolution, G160L, line_20: spectrum to see if the UMi QSO is clear of Lyman limits for future work. ! ! end of abstract general_form_proposers: lname: OLSZEWSKI fname: EDWARD title: PI mi: W inst: STEWARD OBSERVATORY country: USA ! lname: BECHTOLD fname: JILL mi: E inst: STEWARD OBSERVATORY country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We will be obtaining FOS spectra with the red side of FOS and the G270H grating line_2: and the .25" x 2" slit. There are two objects; our primary object is UMI-COS253 line_3: a QSO of V magnitude 18.6 behind the Ursa Minor dwarf spheroidal galaxy. The line_4: second object is a control QSO of estimated magnitude 17.0 nearby on the sky. line_5: Our intent is to look for absorption lines from the interstellar medium line_6: of the Ursa Minor dwarf spheroidal. The control QSO allows us to search for line_7: high velocity gas in the halo of the Milky Way. line_8: We are using the STSCI-recommended (Lucas, Keyes) 4-stage peakup procedure to line_9: acquire each object, as they are faint and probably variable. Exposure times line_10: for each step in the acquisition procedure were made using the FOS simulator, line_11: giving 1000 counts in each exposure with the mirrors line_12: and 3000 counts in each exposure with the slit. After this laborious line_13: peakup we will expose on the prime object for 289.8 minutes and on the control line_14: QSO for 41.7 minutes. Scaled to the Bahcall et al Key Project results line_15: this will give an equivalent width liit of about 0.25 Angstroms, which is what line_16: we need to do our science. ! question: 3 section: 2 line_1: All observations will use FOS/RD and G270H grating. ! question: 4 section: 1 line_1: Justify the need for HST line_2: Existing 21cm radio observations and Einstein X-ray observations are inadequate. line_3: Further, ROSAT PSPC observations would be unlikely to be sensitive enough for line_4: interesting limits on hot gas, a statement made by scaling results from bright line_5: elliptical galaxies. The only absorption line accessible from the ground line_6: optically is Ca II H and K. Lack of detectable Ca II, however, is not definitive line_7: as it is a trace ionization state, and is known to be heavily depleted in the line_8: present day Milky Way ISM. All other lines of interest are accessible only in line_9: the EUV; our program objects are too faint for IUE. ! question: 4 section: 2 line_1: Justify exposure time line_2: Our exposure times were scaled from the HST FOS spectra presented by the line_3: Bahcall et al Key Project papers, and further scaled to fit the necessary line_4: acquisition procedures and total time awarded. ! question: 5 section: 1 line_1: No special scheduling requests. line_2: We reiterate here that we have consulted with people at STSCI and have been line_3: advised to use the 4-stage Peakup acquisition technique. ! question: 6 section: 1 line_1: We require no special calibration exposures. ! question: 7 section: 1 line_1: Plans for data reduction: line_2: The PI will go to STSCI to reduce the data. Reductions will be completed at line_3: Steward Observatory, using the STSDAS packages in IRAF. We have individual SUN line_4: workstations and servers, as well as the Steward SUN system. Analysis of the line_5: absorption line spectra will be carried out using the co-I's software which line_6: was developed to analyze ground-based QSO absorption line spectra. the software line_7: includes continuum fitting routines, automated line finding and identification line_8: routines, and a package to simulate absorption line spectra. ! question: 8 section: 1 line_1: Coordinates used in this Phase 2 submission come from GASP images reduced for line_2: us by James Lowenthal of Johns Hopkins. ! question: 9 section: 1 line_1: Olszewski is a co-I of a WFPC Cycle 1 Program number 2419, "Chronology of the line_2: formation of the Galactic Halo and Disk," robert Zinn, PI. It is NOT related to line_3: this Cycle 3 program. Data reduction is in progress. ! question: 10 section: 1 line_1: Each investigator owns their own Sun workstation and are connected into the line_2: extensive Steward computer network. it is customary for a small percentage of line_3: grant funding support to be contributed to the computer group which maintains line_4: the systems, updates software, and purchases paper and laser printer toner, etc. line_5: however, most of the funding for the computer group comes from the State of line_6: Arizona and from overhead. Ground-based observations in support of this project line_7: will be taken at the Multiple Mirror Telescope, run jointly by SAO and the line_8: University of Arizona. No funds are being requested in this proposal to support line_9: this part of the investigation. University of Arizona graduate students and line_10: undergraduate astronomy majors may become involved in this project, and are line_11: supported by departmental or NSF funds. ! !end of general form text general_form_address: lname: Olszewski fname: Edward mi: W category: PI inst: Steward Observatory addr_1: Steward Observatory addr_2: University of Arizona city: Tucson state: AZ zip: 85721 country: USA phone: (602)621-2288 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: UMI-COS253 descr_1: H,515 pos_1: RA = 15H 08M 40.34S +/- 0.1S, pos_2: DEC = +67D 17' 45.5" +/- 1.0", pos_3: PLATE-ID=00A9 equinox: J2000 rv_or_z: Z = 0.7 fluxnum_1: 1 fluxval_1: V = 18.66 fluxnum_2: 2 fluxval_2: B-V = 0.24 ! targnum: 2 name_1: B21503+691 descr_1: H,515 pos_1: RA = 15H 04M 12.71S +/- 0.1S, pos_2: DEC = +68D 56' 13.4" +/- 1.0", pos_3: PLATE-ID=01L5 equinox: J2000 rv_or_z: Z = 0.3 fluxnum_1: 1 fluxval_1: V = 17.0 fluxnum_2: 2 fluxval_2: B-V = 0.1 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: UMI-COS253 config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 3S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 2; req_2: CYCLE 3 / 1-5; req_3: SEQ 1-5 NO GAP; req_4: SPATIAL SCAN; comment_1: EXPOSURE TIME DETERMINED comment_2: FROM FOS SIMULATOR comment_3: FIRST PART OF 4-STAGE comment_4: PEAKUP; THIS 4-STAGE comment_5: PEAKUP RECOMMENDED comment_6: BY STSCI ! linenum: 2.000 targname: UMI-COS253 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 5S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 3; req_2: SPATIAL SCAN; comment_1: EXPOSURE TIME DETERMINED comment_2: FROM FOS SIMULATOR comment_3: SECOND STAGE OF comment_4: 4-STAGE PEAKUP ! linenum: 3.000 targname: UMI-COS253 config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 8S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP=0.35, param_2: SEARCH-SIZE=3 req_1: ONBOARD ACQ FOR 4; comment_1: EXPOSURE TIME DETERMINED comment_2: FROM FOS SIMULATOR comment_3: THIRD STAGE OF comment_4: 4-STAGE PEAKUP ! linenum: 4.000 targname: UMI-COS253 config: FOS/RD opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 90S fluxnum_1: 1 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 5; req_2: SPATIAL SCAN comment_1: EXPOSURE TIME DETERMINED comment_2: FROM FOS SIMULATOR comment_3: 4TH AND FINAL STAGE OF comment_4: 4-STAGE PEAKUP comment_5: ACQUISITION ! linenum: 5.000 targname: UMI-COS253 config: FOS/RD opmode: ACCUM aperture: 0.25X2.0 sp_element: G270H wavelength: 2225 - 3293 num_exp: 1 time_per_exp: 285.57M s_to_n: 30 fluxnum_1: 1 priority: 1 comment_1: EXPOSURE TIME CALCULATED comment_2: BY FOS SIMULATOR comment_3: FINALLY, THE EXPOSURE ! linenum: 6.000 targname: B21503+691 config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 7; req_2: CYCLE 3 / 6-10; req_3: SEQ 6-10 NO GAP; req_4: SPATIAL SCAN; comment_1: EXPOSURE TIME DETERMINED comment_2: FROM FOS SIMULATOR comment_3: FIRST STAGE OF comment_4: 4-STAGE PEAKUP ! linenum: 7.000 targname: B21503+691 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 1.5S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 8; req_2: SPATIAL SCAN; comment_1: EXPOSURE TIME DETERMINED comment_2: FROM FOS SIMULATOR comment_3: SECOND STAGE OF comment_4: 4-STAGE PEAKUP ! linenum: 8.000 targname: B21503+691 config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 2S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP=0.35, param_2: SEARCH-SIZE=3 req_1: ONBOARD ACQ FOR 9; comment_1: EXPOSURE TIME DETERMINED comment_2: FROM FOS SIMULATOR comment_3: THIRD STAGE OF comment_4: 4-STAGE PEAKUP ! linenum: 9.000 targname: B21503+691 config: FOS/RD opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: MIRROR num_exp: 1 time_per_exp: 6S fluxnum_1: 1 priority: 1 param_1: TYPE=UP req_1: ONBOARD ACQ FOR 10; req_2: SPATIAL SCAN; comment_1: EXPOSURE TIME DETERMINED comment_2: FROM FOS SIMULATOR comment_3: 4TH AND FINAL STAGE OF comment_4: 4-STAGE PEAKUP comment_5: ACQUISITION ! linenum: 10.000 targname: B21503+691 config: FOS/RD opmode: ACCUM aperture: 0.25X2.0 sp_element: G270H wavelength: 2225 - 3293 num_exp: 1 time_per_exp: 45.87M s_to_n: 30 fluxnum_1: 1 priority: 1 comment_1: EXPOSURE TIME CALCULATED comment_2: BY FOS SIMULATOR comment_3: FINALLY, THE EXPOSURE ! ! end of exposure logsheet scan_data: line_list: 1,6 fgs_scan: cont_dwell: D dwell_pnts: 3 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 2.8000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 0.0000 scan_frame: S/C len_offset: 1.4 wid_offset: 0.0 ! line_list: 2,7 fgs_scan: cont_dwell: D dwell_pnts: 6 dwell_secs: 1.00 scan_width: 0.7000 scan_length: 3.5000 sides_angle: 90.0000 number_lines: 2 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 1.75 wid_offset: 0.35 ! line_list: 4,9 fgs_scan: cont_dwell: D dwell_pnts: 7 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 0.4000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 0.2 wid_offset: ! ! end of scan data