! File: 3815C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:20:27:37 coverpage: title_1: UV OBSERVATIONS OF THE HUBBLE-SANDAGE VARIABLES IN M31 AND M33 sci_cat: STELLAR ASTROPHYSICS sci_subcat: MASSIVE STARS proposal_for: GO pi_fname: ROBERTA pi_mi: M. pi_lname: HUMPHREYS pi_inst: UNIVERSITY OF MINNESOTA pi_country: USA pi_phone: 612-624-6530 hours_pri: 8.93 num_pri: 8 foc: Y 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 M31 and 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 M31 and 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: We plan to make UV images of all 8 stars in our list with the FOC, line_2: and then to use the FOS to obtain UV spectra of only 4, chosen after line_3: inspecting the FOC results. The rationale is as follows: line_4: --- line_5: Moderately long FOS integration times are needed for these objects. line_6: Therefore we feel that it is not realistic to attempt FOS observations line_7: of all 8 stars at this time. Moreover, some of the stars may be fainter line_8: than the assumed brightness and would thus be more expensive in terms of line_9: integration time. Thus it makes sense to obtain UV spectra of just 4 line_10: stars, most likely those which are brightest in the FOC images. line_11: --- line_12: Since we do not know the UV brightnesses, which probably fluctuate, line_13: we need the FOC to observe their fluxes around 2000 A. Eight FOC images line_14: are required to observe the eight stars. These may be regarded as early- line_15: acquisition images but they also have scientific value. They will provide line_16: rough limits on the temperatures of all 8 stars (by comparing the UV line_17: brightnesses with ground-based photometry) and they may also show if other, line_18: fainter hot stars are very near any of the H-S variables. We propose to line_19: use the FOC at F/96 with filter F190M (chosen to avoid excessive count line_20: rates). It appears that a format giving a 22" field with 0.022" x 0.044" line_21: pixels is satisfactory for our purposes (see comments in OSF). 2-minute line_22: integration times are sufficient to give good images and comfortably- line_23: better-than-minimal photometry. (continued:...) ! question: 3 section: 2 line_1: --- line_2: For each of 4 stars, we propose 3 FOS exposures using the 1" circular line_3: aperture: 70 minutes with grating G190H and the RD detector, 30 m with line_4: G270H/RD, and 30 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.) line_15: --- line_16: Altogether we propose 8 FOC exposures and 12 FOS exposures. Most likely line_17: the 4 stars chosen for FOS work will be those which are currently brightest line_18: at 2000 A, based on the FOC data. But an exception is possible, e.g. if a line_19: significant eruption is detected through ground-based observations. ! 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. If we get ST time to do the FOS observations, line_14: we hope to obtain ground-based spectra not too different in epoch. ! 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. First, it is highly desirable that line_4: the interval between FOC and FOS observations not be too long -- preferably line_5: not more than 2 months. Secondly, it is desirable to obtain the FOS line_6: observations during the months September--December, so that ground-based line_7: data can be obtained at nearly the same time -- even though this is not line_8: strictly a requirement. Finally, it is always possible that a major eruption line_9: of one of our target stars might be detected by ground-based work; if so line_10: then it would be desirable to obtain the FOS data as soon thereafter as line_11: 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: 7 section: 1 line_1: So far as we can predict, the data reduction will use fairly routine methods. line_2: UV brightnesses estimated from the FOC images will probably use a sampling line_3: circle with r = about 0.3". Resolution enhancement in the FOC images will line_4: only be attempted if a field has an interesting close grouping of stars in line_5: it -- we cannot predict whether this will be the case. line_6: ...Analysis of P Cyg line profiles in the UV spectra obtained with the FOS line_7: will indicate the terminal velocity of the stellar wind and the mass-loss line_8: rate (provided that the velocities are not too small). The UV flux line_9: and UV spectral features, supported by ground-based photometry at visual and line_10: infrared wavelengths, will indicate the total energy distribution and line_11: bolometric luminosity of each FOS target star. Effective temperatures line_12: can be derived from the spectra in combination with model atmospheres. line_13: ..."Strange" UV spectra are possible for stars like these, e.g. with many line_14: emission lines; this is unpredictable and analysis would depend on details. ! 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: AF-AND name_2: M31-AF-AND descr_1: B,148,159 pos_1: RA = 0H 43M 33.06S +/- 0.03S, pos_2: DEC = +41D 12' 10.2" +/- 0.3", pos_3: PLATE-ID = 0738 equinox: J2000 comment_1: BRIGHTNESS IS VARIABLE. comment_2: SPECIAL FIELD (M31) 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 ! targnum: 2 name_1: AE-AND name_2: M31-AE-AND descr_1: B,148,159 pos_1: RA = 0H 43M 2.58S +/- 0.03S, pos_2: DEC = +41D 49' 11.9" +/- 0.3", pos_3: PLATE-ID = 0738 equinox: J2000 comment_1: BRIGHTNESS IS VARIABLE. comment_2: SPECIAL FIELD (M31). 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 ! targnum: 3 name_1: M31-004451+413037 name_2: M31-VAR-A1 descr_1: B,148,159 pos_1: RA = 0H 44M 50.58S +/- 0.03S, pos_2: DEC = +41D 30' 37.4" +/- 0.3", pos_3: PLATE-ID = 0738 equinox: J2000 comment_1: BRIGHTNESS IS VARIABLE. comment_2: SPECIAL FIELD (M31) comment_3: THERE IS A FAINTER STAR ABOUT 5" E. comment_4: 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 ! targnum: 4 name_1: M31-004419+412247 name_2: M31-VAR-15 descr_1: B,148,159 pos_1: RA = 0H 44M 19.46S +/- 0.03S, pos_2: DEC = +41D 22' 46.7" +/- 0.3", pos_3: PLATE-ID = 0738 equinox: J2000 comment_1: BRIGHTNESS IS VARIABLE. comment_2: SPECIAL FIELD (M31). comment_3: THERE ARE FAINTER STARS 4--6" AWAY, comment_4: TO S AND SW comment_5: 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 ! targnum: 5 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 ! targnum: 6 name_1: M33-013349+303809 name_2: M33-VAR-B descr_1: B,148,159 pos_1: RA = 1H 33M 49.22S +/- 0.03S, pos_2: DEC = +30D 38' 09.3" +/- 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 ! targnum: 7 name_1: M33-013335+303601 name_2: M33-VAR-C descr_1: B,148,159 pos_1: RA = 1H 33M 35.15S +/- 0.03S, pos_2: DEC = +30D 36' 00.6" +/- 0.3", pos_3: PLATE-ID = 00DV equinox: J2000 comment_1: BRIGHTNESS IS VARIABLE. comment_2: SPECIAL FIELD (M33). comment_3: THERE IS PROBABLY A FAINTER STAR comment_4: ABOUT 2" W. comment_5: 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 ! targnum: 8 name_1: M33-013418+303837 name_2: M33-VAR-2 descr_1: B,148,159 pos_1: RA = 1H 34M 18.36S +/- 0.03S, pos_2: DEC = +30D 38' 36.9" +/- 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 sequence_1: DEFINE sequence_2: HS-IMAGE targname: # config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F190M num_exp: 1 time_per_exp: 300S s_to_n: 60 fluxnum_1: 3 priority: 1 param_1: PIXEL = 50X25 req_1: CYCLE 2 comment_1: THESE FOC IMAGES OF THE 8 TARGETS comment_2: WILL BE USED TO DECIDE SUBSET OF 4 comment_3: TO BE OBS WITH FOS, HENCE MAY BE comment_4: REGARDED AS EARLY-ACQS. FLUXES comment_5: ARE VARIABLE. S/N IS IDEALIZED, comment_6: REFERS TO ENTIRE STAR IMAGE. ! linenum: 20.000 sequence_1: DEFINE sequence_2: HS-SPECT targname: # config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 30S fluxnum_1: 1 fluxnum_2: 2 priority: 1 req_1: GROUP 20-50 NO GAP; req_2: ONBOARD ACQ FOR 30-50; req_3: CYCLE 2 / 20-50 comment_1: 30S EXP TIME IS OPTIMAL comment_2: FOR STAR SLIGHTLY comment_3: FAINTER THAN ASSUMED comment_4: V=17.0; MIGHT REDUCE comment_5: ACQ EXP TIME ON BASIS comment_6: OF FOC IMAGE... ! linenum: 30.000 sequence_1: DEFINE sequence_2: HS-SPECT targname: # config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1650-2311 num_exp: 1 time_per_exp: 62M 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. ! linenum: 40.000 sequence_1: DEFINE sequence_2: HS-SPECT targname: # config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2225-3281 num_exp: 1 time_per_exp: 28M s_to_n: 27 fluxnum_1: 3 fluxnum_2: 1 fluxnum_3: 2 priority: 1 comment_1: SEE COMMENT FOR LINE 30 ! linenum: 50.000 sequence_1: DEFINE sequence_2: HS-SPECT targname: # config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G160L wavelength: 1150-2524 num_exp: 1 time_per_exp: 24M s_to_n: 13 fluxnum_1: 3 fluxnum_2: 2 priority: 1 comment_1: SEE COMMENT FOR LINE 30 ! linenum: 110.000 sequence_1: USE sequence_2: HS-IMAGE targname: AF-AND comment_1: SEE COMMENTS FOR LINE 10. comment_2: RE SCHEDULING, SEE TEXT QUESTIONS comment_3: 5 AND 8; OPTIMAL WOULD BE FOC comment_4: IMAGING BETWEEN MID-JULY AND MID- comment_5: SEPT, ALLOWING FOS OBS IN FALL 92. ! linenum: 120.000 sequence_1: USE sequence_2: HS-IMAGE targname: AE-AND comment_1: SEE COMMENTS FOR LINE 10 ! linenum: 130.000 sequence_1: USE sequence_2: HS-IMAGE targname: M31-004451+413037 comment_1: SEE COMMENTS FOR LINE 10 ! linenum: 140.000 sequence_1: USE sequence_2: HS-IMAGE targname: M31-004419+412247 comment_1: SEE COMMENTS FOR LINE 10 ! linenum: 150.000 sequence_1: USE sequence_2: HS-IMAGE targname: M33-013411+303438 comment_1: SEE COMMENTS FOR LINE 10 ! linenum: 160.000 sequence_1: USE sequence_2: HS-IMAGE targname: M33-013349+303809 comment_1: SEE COMMENTS FOR LINE 10 ! linenum: 170.000 sequence_1: USE sequence_2: HS-IMAGE targname: M33-013335+303601 comment_1: SEE COMMENTS FOR LINE 10 ! linenum: 180.000 sequence_1: USE sequence_2: HS-IMAGE targname: M33-013418+303837 comment_1: SEE COMMENTS FOR LINE 10 ! linenum: 210.000 sequence_1: USE sequence_2: HS-SPECT targname: AF-AND req_1: COND IF 110 BRIGHT ENOUGH; req_2: SELECT 4 OF 210 OR 220 OR req_3: 230 OR 240 OR 250 OR req_4: 260 OR 270 OR 280 comment_1: SEE COMMENT LINENUM 110. comment_2: FOR S/N, SEE SEQ DEF. ! linenum: 220.000 sequence_1: USE sequence_2: HS-SPECT targname: AE-AND req_1: COND IF 120 BRIGHT ENOUGH comment_1: SEE SELECT, LINE 210 ! linenum: 230.000 sequence_1: USE sequence_2: HS-SPECT targname: M31-004451+413037 req_1: COND IF 130 BRIGHT ENOUGH; comment_1: SEE SELECT, LINE 210 ! linenum: 240.000 sequence_1: USE sequence_2: HS-SPECT targname: M31-004419+412247 req_1: COND IF 140 BRIGHT ENOUGH; comment_1: SEE SELECT, LINE 210 ! linenum: 250.000 sequence_1: USE sequence_2: HS-SPECT targname: M33-013411+303438 req_1: COND IF 150 BRIGHT ENOUGH; comment_1: SEE SELECT, LINE 210 ! linenum: 260.000 sequence_1: USE sequence_2: HS-SPECT targname: M33-013349+303809 req_1: COND IF 160 BRIGHT ENOUGH; comment_1: SEE SELECT, LINE 210 ! linenum: 270.000 sequence_1: USE sequence_2: HS-SPECT targname: M33-013335+303601 req_1: COND IF 170 BRIGHT ENOUGH; comment_1: SEE SELECT, LINE 210 ! linenum: 280.000 sequence_1: USE sequence_2: HS-SPECT targname: M33-013418+303837 req_1: COND IF 180 BRIGHT ENOUGH; comment_1: SEE SELECT, LINE 210 ! ! end of exposure logsheet ! No scan data records found