! File: 4359C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:23:12:38 coverpage: title_1: PROBING THE HOT INTERSTELLAR MEDIUM title_2: OF THE LARGEST LMC SUPERGIANT SHELL CYC3-MED sci_cat: INTERSTELLAR MEDIUM sci_subcat: ABSORPTION LINES proposal_for: GO pi_fname: KLAAS pi_mi: S. pi_lname: DE BOER pi_inst: UNIVERSITAT BONN pi_country: GERMANY hours_pri: 5.00 num_pri: 2 hrs: Y ! end of coverpage abstract: line_1: We will measure absorptions due to interstellar CIV, OI and SiII on 4 lines of line_2: sight to stars located inside supershell LMC4 in the Large Magellanic Cloud. line_3: The equivalent widths and line profiles of the CIV absorptions are excellent line_4: probes for the determination of the temperature and structure of the coronal line_5: gas inside the LMC4 cavity, and thus of the energy content of the region. In line_6: addition, these measurements will determine the extent to which hot gas from line_7: the bubble flows into the LMC halo. We know that the bubble also contains line_8: neutral and low ionization species, and the proposed measurements of SiII and line_9: OI are essential to derive the relative importance of the hot versus the line_10: cool interstellar phases in supporting the LMC4 bubble. line_11: With these data we aim to test and calibrate existing models for the expansion line_12: of LMC4, improve insight in the disk-halo connection in (irregular) galaxies, line_13: and test scenarios for the creation of quasar absorption lines. ! ! end of abstract general_form_proposers: lname: DE BOER fname: KLAAS title: PI mi: S. inst: UNIVERSITAT BONN country: GERMANY esa: Y ! lname: BOMANS fname: DOMINIK mi: J. inst: UNIVERSITAT BONN country: GERMANY esa: Y ! lname: GREBEL fname: EVA mi: K. inst: UNIVERSITAT BONN country: GERMANY esa: Y ! lname: KOORNNEEF fname: JAN inst: STSCI country: USA esa: Y ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The table below contains the relevant data for our target stars. The line_2: positions of our stars over the face of LMC4 ist shown in Fig. 1. line_4: Star V Spec Typ F1300 F1550 grat. time(s) line_5: 130nm 155nm line_6: Sk-66 118 11.81 B2 Iab 2.4e-12 1.6e-12 G160M 600 3000 line_7: Sk-67 169 12.18 B0 I 1.1e-12 6.1e-13 G160M 1400 7000 line_9: F [erg* cm e-2*s e-1*A e-1] line_10: For each star we plan to obtain two spectra: line_11: 1. A spectrum with the G160M grating centered on 130.3 nm trough the LSA line_12: to aquire data line_13: with the high spectral resolution (through convolution techniques, e.g. line_14: Wahlgren et al. 1991) and modest S/N for the O I 130.2 nm and line_15: Si II 130.4 nm absorption lines. This provides information on the velocity line_16: structure of the neutral line_17: gas. Furthermore, comparison of the O I with 21-cm HI allows a direct line_18: interpretation of the depth structure. As substructures are already line_19: indicated in the IUE spectra, the velocity resolution with the G160M grating line_20: is sufficient to fully resolve them. The velocity range covered is -917 to line_21: 6649 km/s for Si II 130.4 nm and -459 to 7119 km/s for O I 130.2. ! question: 3 section: 2 line_1: As this exposure covers a wavelength range of 130.0 nm to 133.4 nm, we line_2: might get additional lines which provide information on cold and warm gas, line_3: namely Ni II 130.8 nm, Ni II 131.7 nm, C I 132.8 nm, Si II* 130.9 nm, and line_4: O I* 130.48 nm. These lines are weak, but will be useful in combination line_5: with the two lines we are actually aiming at. line_6: The second spectrum with the G160M grating and LSA is centered on 155.0 nm to line_7: analyze the CIV doublet at 154.8 and 155.0 nm with the highest S/N possible; line_8: this will show the ubiquitousness of the hot gas and the velocity structure line_9: in the hot gas. Our spectrum covers a velocity line_10: range of -2510 to 3283 km/s for C IV 154.8nm and a range of -2893 to 2893 line_11: km/s for C IV 155.0 nm. line_12: For all observations we want to use the FP-SPLIT exposure mode with line_13: substepping by 1/4 diode steps to get spectra as well-sampled as possible. ! question: 4 section: 1 line_1: The absorption lines of the hot ISM are only observable in the UV. This is line_2: also true for lines with intrinsically large optical depth originating in line_3: the neutral ISM. line_4: Our experience with IUE shows that the absorption profiles in the direction line_5: to the center of supershell LMC4 usually are weak and often are heavily line_6: blended. The velocity resolution of the IUE satellite is incapable of line_7: resolving the LMC absorption in all its components. Faint lines cannot be line_8: resolved at all, and fine structure in stronger lines is only indicated. line_9: We can achieve a sufficiently high resolution and a high enough S/N for the line_10: detailed analysis of these components within an acceptable amount of observing line_11: time with the GHRS using its G160M grating. line_12: As G160M is situated at Side 2 of the line_13: GHRS, it is not affected by the current instrument problems. ! question: 7 section: 1 line_1: The data reduction will be carried out on the VMS and Ultrix clusters of the line_2: Astronomical Institutes of the University of Bonn and at the STScI. We will line_3: use STSDAS and MIDAS to perform the basic reduction steps. line_4: We will use the profile fitting packages of IRAF/STSDAS and/or MIDAS to line_5: produce cloud models to measure equivalent widths and central velocities of line_6: the lines. The data will provide us with detailed information on the line_7: velocities and temperatures of the gas clouds of LMC4, particularly in order line_8: to map the proposed outflow of gas into the halo of the LMC. line_9: We have ample experience in analyzing high dispersion UV spectra; two members line_10: of our group (KSdB and JK) have been working with the IUE since 1978, and on line_11: the ISM of the LMC in particular (see de Boer & Savage 1980, de Boer, Koornneef line_12: and Savage 1980, de Boer & Nash 1982, de Boer et al. 1985). The data will be line_13: analyzed together with IUE spectra to stars in this region of the LMC. ! question: 10 section: 1 line_1: No additional resources are needed to conduct the proposed project. All members line_2: of the team currently have unlimited access to DEC/VAX stations 3100, and line_3: higher. ! !end of general form text general_form_address: lname: DE BOER fname: KLAAS mi: S. category: PI inst: Universitat Bonn addr_1: STERNWARTE BONN addr_2: AUF DEM HUEGEL 71 city: 5300 BONN 1 country: GERMANY phone: [49]-(228)733655 telex: 8 86 440 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: SK-66118 name_2: GSC8891.03372 descr_1: B,113, descr_2: H,515,517,917 pos_1: PLATE-ID=06AF, pos_2: RA = 05H 30M 51.95S +/- 0.3", pos_3: DEC = -66D 54' 08.6" +/- 0.3" equinox: 2000 comment_1: GSC LABEL 'MULTIPLE' comment_2: IUE HIGH DIS. SPECTRUM fluxnum_1: 1 fluxval_1: V = 11.81 +/- 0.02 fluxnum_2: 2 fluxval_2: TYPE = B2 I fluxnum_3: 3 fluxval_3: E(B-V) = 0.07 +/- 0.05 fluxnum_4: 4 fluxval_4: B-V = -0.05 +/- 0.03 fluxnum_5: 5 fluxval_5: U-B = -0.86 +/- 0.03 fluxnum_6: 6 fluxval_6: F(1300) = 2.4 +/- 0.2 E-12 fluxnum_7: 7 fluxval_7: F(1550) = 1.6 +/- 0.2 E-12 ! targnum: 2 name_1: SK-67169 name_2: GSC8891.03638 descr_1: B,113, descr_2: H,515,517,917 pos_1: PLATE-ID=06AF, pos_2: RA = 05H 31M 51.62S +/- 0.3", pos_3: DEC = -67D 02' 21.8" +/- 0.3" equinox: 2000 comment_1: GSC LABLE 'MULTIPLE comment_2: IUE HIGH DISP SPECTRA fluxnum_1: 1 fluxval_1: V = 12.18 +/- 0.02 fluxnum_2: 2 fluxval_2: TYPE = B0 I fluxnum_3: 3 fluxval_3: E(B-V) = 0.07 +/- 0.05 fluxnum_4: 4 fluxval_4: B-V = -0.12 +/- 0.03 fluxnum_5: 5 fluxval_5: U-B = -0.90 +/- 0.03 fluxnum_6: 6 fluxval_6: F(1300) = 1.1 +/- 0.2 E-12 fluxnum_7: 7 fluxval_7: F(1550) = 6.1 +/- 0.2 E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.010 targname: SK-66118 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 5S fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 fluxnum_4: 4 priority: 1 param_1: SEARCH-SIZE = 5, param_2: BRIGHT = RETURN, param_3: LOCATE = YES req_1: ONBOARD ACQ FOR 1.02, 1.03; req_2: CYCLE 3 comment_1: ACQ FOR SK-66 118 comment_2: CROWDED FIELD comment_3: SHAPLEY CONSTELLATION III IN THE LMC comment_4: BRIGHTEST STAR IN 10" REGION comment_5: STEP-TIME = 0.2S ! linenum: 1.020 targname: SK-66118 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1303 num_exp: 2 time_per_exp: 300S s_to_n: 34 s_to_n_time: 590S fluxnum_1: 6 priority: 1 param_1: STEP-PATT = 5, param_2: FP-SPLIT = FOUR, param_3: COMB = FOUR, param_4: DOPPLER = ON req_1: CYCLE 3 comment_1: SPECTRA REGION OF SIII 1304 A comment_2: NEUTRAL GAS AND COLD GAS comment_3: OI, SIII, NIII, CII, CII*, CI comment_4: VELOCITY STRUCTURE OF THE SHELL ! linenum: 1.030 targname: SK-66118 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1550 num_exp: 4 time_per_exp: 632S s_to_n: 50 s_to_n_time: 2481S fluxnum_1: 7 priority: 1 param_1: STEP-PATT = 5, param_2: FP-SPLIT = FOUR, param_3: COMB = FOUR, param_4: DOPPLER = ON, req_1: CYCLE 3 comment_1: SPECTRAL REGION OF THE CIV DOUBLETT comment_2: SEARCH FOR INTERSTELLAR CIV FROM THE comment_3: HOT INTERIOR OF SUPERGIANT SHELL LMC4 comment_4: WEAK LINES ! linenum: 2.010 targname: SK-67169 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 5S fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 fluxnum_4: 4 priority: 1 param_1: SEARCH-SIZE = 5, param_2: BRIGHT = RETURN, param_3: LOCATE = YES req_1: ONBOARD ACQ FOR 2.02, 2.03; req_2: CYCLE 3 comment_1: ACQ FOR SK-67 169 comment_2: CROWDED FIELD comment_3: SHAPLEY CONSTELLATION III IN THE LMC comment_4: BRIGHTEST STAR IN THE 10" REGION comment_5: STEP-TIME = 0.2S ! linenum: 2.020 targname: SK-67169 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1303 num_exp: 2 time_per_exp: 650S s_to_n: 34 s_to_n_time: 1300S fluxnum_1: 6 priority: 1 param_1: STEP-PATT = 5, param_2: FP-SPLIT = FOUR, param_3: COMB = FOUR, param_4: DOPPLER = ON req_1: CYCLE 3 comment_1: SPECTRA REGION OF SIII 1304 A comment_2: NEUTRAL GAS AND COLD GAS comment_3: OI, SIII, NIII, CII, CII*, CI comment_4: VELOCITY STRUCTURE OF THE SHELL ! linenum: 2.030 targname: SK-67169 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1550 num_exp: 6 time_per_exp: 1150S s_to_n: 51 s_to_n_time: 6800S fluxnum_1: 7 priority: 1 param_1: STEP-PATT = 5, param_2: FP-SPLIT = FOUR, param_3: COMB = FOUR, param_4: DOPPLER = ON req_1: CYCLE 3 comment_1: SPECTRAL REGION OF THE CIV DOUBLETT comment_2: SEARCH FOR INTERSTELLAR CIV FROM THE comment_3: HOT INTERIOR OF SUPERGIANT SHELL LMC4 comment_4: WEAK LINES ! ! end of exposure logsheet ! No scan data records found