coverpage: title_1: UV OBSERVATIONS OF THE HUBBLE-SANDAGE VARIABLES IN M33 - title_2: Cycle 4 Carryover sci_cat: STELLAR ASTROPHYSICS sci_subcat: MASSIVE STARS proposal_for: GO/CAR cont_id: 3815 pi_fname: ROBERTA pi_mi: M. pi_lname: HUMPHREYS pi_inst: UNIVERSITY OF MINNESOTA pi_country: USA pi_phone: 612-624-6530 hours_pri: 1.96 num_pri: 1 fos: Y funds_amount: 62548 funds_length: 12 off_fname: RICK off_lname: DUNN off_title: ASSISTANT DIRECTOR off_inst: UNIVERSITY OF MINNESOTA off_addr_1: OFFICE OF RESEARCH AND TECHNOLOGY TRANSFER, off_addr_2: ADMINISTRATIVE SERVICES CENTER, off_addr_3: 1919 UNIVERSITY AVE. off_city: ST. PAUL off_state: MN off_zip: 55104 off_country: U.S.A. off_phone: 612-624-8526 ! end of coverpage abstract: line_1: The Hubble-Sandage variables in M33 are luminous blue variables (LBVs) line_2: -- very luminous, eruptively unstable stars in the same general class as S Dor, line_3: Eta Car, and P Cyg. UV observations of H-S variables will significantly line_4: enhance the limited information available to us concerning the evolution and line_5: structure of the most massive stars. line_6: ---- line_7: LBVs are important in several major astrophysical connections and are only line_8: beginning to be understood. Since the LBV stage of evolution is brief, only line_9: a few examples are available in our Galaxy and in the Magellanic Clouds, line_10: close enough for UV observations with IUE. Therefore our coverage of the line_11: wide parameter space embraced by LBVs has been so sparse that theoretical line_12: development has been hindered. line_13: ---- line_14: With the ST, we can significantly increase this coverage by adding the H-S line_15: variables in M33 to the set of "useful" LBVs. UV spectroscopy is line_16: needed to determine their temperatures, luminosities, and mass-loss rates. line_17: These parameters are required to clarify their relations to other LBVs and line_18: very massive stars in general, and to provide more information on evolutionary line_19: origin of LBVs, physical causes of the violent eruptions, and other problems. ! ! end of abstract general_form_proposers: lname: HUMPHREYS fname: ROBERTA title: PI mi: M. inst: UNIVERSITY OF MINNESOTA country: USA ! lname: DAVIDSON fname: KRIS inst: UNIVERSITY OF MINNESOTA country: USA ! lname: WALBORN fname: NOLAN mi: R. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: WOLF fname: BERNHARD inst: LANDESSTERNWARTE, HEIDELBERG country: GERMANY esa: Y ! lname: APPENZELLER fname: IMMO inst: LANDESSTERNWARTE, HEIDELBERG country: GERMANY esa: Y ! lname: STAHL fname: OTMAR inst: LANDESSTERNWARTE, HEIDELBERG country: GERMANY esa: Y ! lname: ZICKGRAF fname: FRANZ-JOSEF inst: LANDESSTERNWARTE, HEIDELBERG country: GERMANY esa: Y ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: (Edited to contain only carryover descriptions by Michelle Bullock) line_2: For each of 4 stars, we propose 3 FOS exposures using the 1" circular line_3: aperture: 39 minutes with grating G190H and the RD detector, 18 m with line_4: G270H/RD, and 20 m with G160L/BL. The G190H and G270H observations will line_5: produce good spectra in the range 1700--3200 A, with nominal S/N ratios line_6: of 20 to 30 for resolutions of 1 to 2 A (of course the S/N ratios will be line_7: better for stars that are brighter than assumed here, which we hope will be line_8: the case for at least two or three of them). A number of useful spectral line_9: lines occur in this wavelength interval. Unfortunately, in order to obtain line_10: continuum fluxes and slopes extending to wavelengths shorter than 1700 A, line_11: and in case certain important emission lines appear at such wavelengths, line_12: we must switch to the BL detector for the G160L observations, despite the line_13: overhead time that this entails. (Since the resulting count rates are low, line_14: we do not attempt to obtain good resolution at the shortest wavelengths.) ! question: 4 section: 1 line_1: IUE observations of some of the visually brightest Hubble-Sandage variables line_2: have been attempted. The results have been just marginal detections even line_3: with IUE exposure times of 6 or 7 hours; they give only a few DN above line_4: background and poor S/N even for wide-band flux estimates at the wavelengths line_5: where IUE is most sensitive (Humpheys et al. 1984, 1988). These efforts line_6: have demonstrated that measurements of these stars' spectral features and line_7: accurate short-UV-wavelength fluxes cannot be done with IUE; they also line_8: confirm that the typical UV fluxes assumed in this proposal are realistic. line_9: --- line_10: Many ground-based visual-wavelength observations of H-S variables have been line_11: made since the early 1970's (see refs. in the scientific justification). line_12: Their blue-visual spectra show strong similarities to the LBVs in our line_13: Galaxy and in the LMC. ! question: 5 section: 1 line_1: No special scheduling is absolutely required; however, since our target line_2: stars do vary over timescales of years or months, advantageous scheduling line_3: would be helpful in several respects. Firstly, it is desirable to obtain line_4: the FOS observations during the months September--December, so that line_5: ground-based data can be obtained at nearly the same time -- even though line_6: this is not strictly a requirement. Secondly, it is always possible line_7: that a major eruption of one of our target stars might be detected by line_8: ground-based work; if so then it would be desirable to obtain the FOS line_9: data as soon thereafter as practicable. ! question: 6 section: 1 line_1: There are no special calibration requirements. line_2: A small "special catalog" of acquisition stars may be advisable; line_3: if so, we will provide the needed data (most likely just a few line_4: altered flags for the sets of GSC stars in these M31 and M33 fields). ! ! question: 8 section: 1 line_1: Considerations outlined in question 5 are pertinent. Since it is desirable line_2: (though not necessary) to take ground-based data at about the same time as line_3: the FOS data, September--January is the optimum time for these ST observations. line_4: Ground-based photometric and spectroscopic monitoring of the Hubble-Sandage line_5: variables will continue. We can obtain visual and near-IR (UBVRI + JHK) line_6: photometry of the H-S variables with the University of Minnesota 1.5-m line_7: telescope on Mt. Lemmon, and moderate-to-high-resolution blue-visual-red line_8: spectra with the Calar Alto 3.5-m telescope. September--January is of line_9: course the prime season for ground-based observations of M31 and M33. line_10: ---- line_11: We have measured accurate TARGET POSITIONS on a set of 4m-prime-focus line_12: plates, using appropriate sets of GSC stars to set up the coordinate line_13: grids. These same plates may provide altered flags for a few GSC line_14: stars which may be dangerous to use for acquisition. (Target positions line_15: were measured in February 1992; as of mid-March, the GSC star line_16: re-evaluations are not yet completed but probably will be within line_17: a few weeks.) ! question: 9 section: 1 line_1: -- Davidson is PI and Humphreys, Walborn and Wolf are CoI's on GO 2338, line_2: "Spectroscopy of the speckle-resolved Eta Car point sources." This is line_3: indirectly related in the sense that Eta Carinae is an LBV and so are line_4: the H-S variables. line_5: -- Davidson and Walborn are assisting D. Ebbets on Ebbets' GTO 1186, line_6: "Imagery and UV spectroscopy of matter ejected from Eta Carinae." line_7: Above comments apply to this project also. line_8: -- Davidson is a CoI on R. Dufour's GO 2416, "Imagery and spectroscopy line_9: of super metal poor galaxies." This is related only if some line_10: LBV-like stars are found in GR8 or I Zw 18 (unlikely). line_11: -----results from above-listed programs:----- line_12: Several good WFC and PC images of Eta Car were made in 1991, and line_13: good FOS data were obtained for project 2338 in August 1991. These line_14: all require rather tricky analyses, which are not yet completed as line_15: of mid-March 1992. Similar remarks apply to the data obtained for line_16: Dufour's program number 2416. line_17: There are no real publications yet, except that several of the line_18: images were used in poster papers at the January 1992 AAS meeting. ! question: 10 section: 1 line_1: The Graduate School of the University of Minnesota provided $12,000 toward line_2: the purchase of a Sun computer for the original proposal for these line_3: observations submitted in 1988. A network of Sun computers now exists line_4: in the Minnesota Astronomy department. We have IRAF running on this line_5: system. However, since these machines are very heavily used, Humphreys line_6: is requesting funds for a dedicted work station. line_7: The data analysis facilities of ESO/ST-ECF are available to Wolf, line_8: Appenzeller, Stahl, and Zickgraf. They have also the MIDAS data line_9: reduction package on the machines at the Landessternwarte, Heidelberg. ! !end of general form text general_form_address: lname: HUMPHREYS fname: ROBERTA mi: M. category: PI inst: UNIVERSITY OF MINNESOTA addr_1: ASTRONOMY DEPT. addr_2: UNIVERSITY OF MINNESOTA addr_3: 116 CHURCH ST. S.E. city: MINNEAPOLIS state: MN zip: 55455 country: USA phone: 612-624-6530 ! ! end of general_form_address records fixed_targets: ! targnum: 1 name_1: M33-013411+303438 name_2: M33-VAR-83 descr_1: B,148,159 pos_1: RA = 1H 34M 10.92S +/- 0.03S, pos_2: DEC = +30D 34' 37.6" +/- 0.3", pos_3: PLATE-ID = 00DV equinox: J2000 comment_1: BRIGHTNESS IS VARIABLE. comment_2: SPECIAL FIELD (M33). comment_3: GS VERSION 1.1 (NOT 1.0) fluxnum_1: 1 fluxval_1: V = 17.0 +/- 1.0 fluxnum_2: 2 fluxval_2: B-V = 0.0 +/- 0.2 fluxnum_3: 3 fluxval_3: F-CONT(2000) = 4 +/- 3 E-15 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 10.000 targname: M33-013411+303438 config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 20S fluxnum_1: 1 fluxnum_2: 2 priority: 1 req_1: CYCLE 4 / 10-40; req_2: ONBOARD ACQ FOR 11; linenum: 11.000 targname: M33-013411+303438 config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR param_1: SEARCH-SIZE-X=4 param_2: SEARCH-SIZE-Y=4 param_3: SCAN-STEP-X=0.172 param_4: SCAN-STEP-Y=0.172 num_exp: 1 time_per_exp: 7S priority: 1 req_1: ONBOARD ACQ FOR 20-40; linenum: 20.000 targname: M33-013411+303438 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: 39M s_to_n: 27 fluxnum_1: 3 priority: 1 comment_1: QUOTED S/N RATIOS FOR FOS ACCUM comment_2: REFER TO 1/2 DIODE, AND ARE VERY comment_3: CRUDE BECAUSE ASSUMED FLUXES ARE comment_4: ROUGH. comment_5: WOULD LIKE 1650 - 2311 comment_6: WAVELENGTH COVERAGE. ! linenum: 30.000 targname: M33-013411+303438 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H num_exp: 1 time_per_exp: 18M s_to_n: 27 fluxnum_1: 3 fluxnum_2: 1 fluxnum_3: 2 priority: 1 comment_1: SEE COMMENT FOR LINE 20 comment_2: ABOUT S/N. WOULD LIKE comment_3: 2225-3281. ! linenum: 40.000 targname: M33-013411+303438 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G160L num_exp: 1 time_per_exp: 20M s_to_n: 13 fluxnum_1: 3 fluxnum_2: 2 priority: 1 comment_1: SEE COMMENT FOR LINE 20 comment_2: ABOUT S/N. WOULD LIKE comment_3: 1150-2524 ! ! end of exposure logsheet ! No scan data records found