! File: 4322C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:21:48:16 coverpage: title_1: RESOLUTION OF THE UPPER IMF IN THE MAGELLANIC CLOUDS:CY3HIGH sci_cat: HOT STARS sci_subcat: YOUNG CLUSTERS proposal_for: GO pi_fname: NOLAN pi_mi: R. pi_lname: WALBORN pi_inst: STSCI pi_country: USA hours_pri: 0.50 num_pri: 5 wf_pc: Y funds_length: 12 off_fname: HERVEY off_mi: S. off_lname: STOCKMAN off_title: DEPUTY DIRECTOR off_inst: 3470 off_addr_1: 3700 SAN MARTIN DRIVE off_city: BALTIMORE off_state: MD off_zip: 21218 off_country: USA off_phone: (410) 338-4730 ! end of coverpage abstract: line_1: Determination of the highly significant upper end of the initial mass line_2: function in extragalactic systems is subject to serious systematic error line_3: due to the combination of limited spatial resolution and the tendency of line_4: the most massive stars to occur in compact groups. These effects cause line_5: the luminosities to be overestimated and the numbers underestimated. line_6: The Magellanic Clouds provide the most favorable case, but even there line_7: compact systems remain a challenge. GTO observations of the 30 Doradus line_8: central cluster have demonstrated the substantial contribution which line_9: HST can make to the problem. This program will obtain UBV images with line_10: WF/PC of 5 important fields in the Magellanic Clouds other than the 30 line_11: Doradus cluster, in which recent ground-based and HST spectroscopy of line_12: extremely massive stars has been performed. It is absolutely vital to line_13: ascertain the multiplicity status of these images, even at the 0.1 arc line_14: sec level, for useful interpretation of the spectroscopic data. The use line_15: of 3 colors will enable reddening estimates to be made, and corrected line_16: color-magnitude diagrams and IMFs to be constructed, the latter with line_17: consultation of the spectroscopic results. The analysis of these images line_18: will provide a substantial advance over current knowledge of the upper line_19: IMF, and they represent an optimum use of HST in its present optical line_20: state, which would not be significantly enhanced by the refurbishment. ! ! end of abstract general_form_proposers: lname: WALBORN fname: NOLAN title: PI mi: R. inst: STSCI country: USA ! lname: MACKENTY fname: JOHN mi: W. inst: STSCI country: USA ! lname: SAHA fname: ABHIJIT inst: STSCI country: USA ! lname: WHITE fname: RICHARD mi: L. inst: STSCI country: USA ! lname: PARKER fname: JOEL mi: WM inst: NASA GODDARD SPACE FLIGHT CENTER country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Five fields in the Magellanic Clouds are observed with the line_2: WFPC to examine bright (V=12 to 16) magnitude O stars for line_3: multiplicity (and to determine magnitudes and colors of the line_4: separated components--if any). line_5: Each field is observed with either the PC or the WFC as line_6: determined by the size of the region with O stars. line_7: Each field is observed in U,B, and V. line_8: Exposure times are short (4 to 80 seconds). line_9: Two exposures in each filter are obtained to remove cosmic rays. line_10: It is critical that all 6 exposures of each field be obtained line_11: with the stars on the same pixels (SAME POS requirement). line_12: Preflash and Fine lock guiding are also required. line_13: The observations are grouped within 12H but it should be line_14: possible to obtain each field in 1 or 2 visibility periods line_15: as these fields are in or near the CVZ. line_16: Please direct change queries both to PI and John MacKenty x4559. ! question: 4 section: 1 line_1: All of these regions have been investigated from the line_2: ground. HST resolution is required to address the principal line_3: scientific objective: the multiplicity of the best current line_4: candidates for the most massive stars, those of type O3 line_5: in the Magellanic Clouds, and its implication for the upper line_6: IMF. In the case of NGC346, the PC images will provide an line_7: essential complement to FOS UV spectroscopic observations line_8: during Cycle 1. ! question: 5 section: 1 line_1: No special realtime data or special scheduling line_2: is required. Note that these targets are in or near line_3: the CVZ and an increase in spacecraft efficiency is line_4: possible if they are scheduled to utilize this fact. ! question: 6 section: 1 line_1: No special calibration required. ! question: 7 section: 1 line_1: The proposal team constitutes a strong complementary mix of line_2: expertise. NRW is an expert on the spatial and stellar line_3: spectroscopic morphology of the regions to be observed. line_4: JWM is the principal WF/PC specialist at the STScI, who line_5: will be responsible for Phase II specifications and initial line_6: calibration/reduction considerations. AS has extensive line_7: experience with stellar photometric measurements in HST line_8: images. JWmP has just completed a major PhD thesis line_9: investigation of CCD photometry and the IMF in 30 Doradus, line_10: and he was the first author of the N11 study as well. RLW line_11: is an image-deconvolution expert with considerable line_12: experience involving HST images. The photometry will be line_13: done with the original images using PSF-Fitting line_14: techniques, but Lucy deconvolutions will be performed on line_15: all of them, possibly for object-list input to the line_16: photometry, and definitely for presentation. Reddening line_17: corrections and IMF results will be derived by standard line_18: techniques already employed in the analysis of prior line_19: ground-based data. Complete catalogues of all images line_20: measured will be prepared and published. ! question: 9 section: 1 line_1: NRW (CoI): 1186, Imagery and UV Spectroscopy of Matter line_2: Ejected from Eta Carinae line_3: NRW " : 2233, The Physics of Massive O-Stars in line_4: Different Parent Galaxies line_5: NRW " : 2338, Spectroscopy of the Speckle-Resolved Eta line_6: Carinae Point Sources line_7: NRW " : 3815, UV Observations of the Hubble-Sandage line_8: Variables in M31 and M33 line_9: JWM (PI) : 3698, A Snapshot Survey of the Nuclear Regions line_10: of 102 Markarian Galaxies line_11: JWM (CoI) : 3538, UV Spectroscopy of Extended Emission-Line line_12: Regions Around QSOs line_13: AS (CoI) : 2547, Calibration of Supernovae of Type I as line_14: Standard Candles line_15: Program 2233 will obtain FOS UV spectroscopy of several line_16: stars in NGC 346 to be imaged here. ! question: 10 section: 1 line_1: Much of the work will be supported through the associated line_2: grant requests, which include 1 month of scientist and 3 line_3: months of research assistant salaries as well as computer line_4: equipment and support. We have access to substantial line_5: data-analysis facilities and support personnel at the STScI line_6: in addition. JWM heads the STScI WF/PC technical support line_7: group, while AS and RLM also have considerable experience line_8: in the analysis of HST images. ! !end of general form text general_form_address: lname: WALBORN fname: NOLAN mi: R. category: PI inst: STScI addr_1: 3700 SAN MARTIN DRIVE city: BALTIMORE state: MD zip: 21218 country: USA phone: (410) 338-4915 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC346 descr_1: D,203 pos_1: PLATE-ID=06B1, pos_2: RA= 00H59M02.0S +/-1S, pos_3: DEC= -72D10'31" +/- 1" equinox: 2000 fluxnum_1: 1 fluxval_1: V = 14 ! targnum: 2 name_1: HD32228 name_2: LUCKE-HODGE9 descr_1: D,203 pos_1: RA= 04H56M34.5S +/-1S, pos_2: DEC= -66D28'25" +/- 1" equinox: 2000 fluxnum_1: 1 fluxval_1: V = 14 ! targnum: 3 name_1: LUCKE-HODGE10 descr_1: D,203 pos_1: RA= 04H56M50.6S +/-1S, pos_2: DEC= -66D24'35" +/- 1" equinox: 2000 fluxnum_1: 1 fluxval_1: V = 14 ! targnum: 4 name_1: NGC2044 name_2: 30DORADUS-C descr_1: D,203 pos_1: RA= 05H35M54.0S +/-1S, pos_2: DEC= -69D11'48" +/- 1" equinox: 2000 fluxnum_1: 1 fluxval_1: V = 14 ! targnum: 5 name_1: 30DORADUS-B descr_1: D,203 pos_1: RA= 05H37M44.0S +/-1S, pos_2: DEC= -69D09'55" +/- 1" equinox: 2000 fluxnum_1: 1 fluxval_1: V = 14 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.100 sequence_1: DEF SEQPC targname: # config: PC opmode: IMAGE aperture: PCALL sp_element: F336W num_exp: 1 time_per_exp: 40S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES req_1: GROUP 1.1-1.6 WITHIN 12H; req_2: PCS MODE F /1.1-1.6; req_3: SAME POS FOR 1.2-1.6 AS 1.1; ! linenum: 1.200 sequence_1: DEF SEQPC targname: # config: PC opmode: IMAGE aperture: PCALL sp_element: F336W num_exp: 1 time_per_exp: 80S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES ! linenum: 1.300 sequence_1: DEF SEQPC targname: # config: PC opmode: IMAGE aperture: PCALL sp_element: F439W num_exp: 1 time_per_exp: 20S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES ! linenum: 1.400 sequence_1: DEF SEQPC targname: # config: PC opmode: IMAGE aperture: PCALL sp_element: F439W num_exp: 1 time_per_exp: 40S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES ! linenum: 1.500 sequence_1: DEF SEQPC targname: # config: PC opmode: IMAGE aperture: PCALL sp_element: F569W num_exp: 1 time_per_exp: 7S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES ! linenum: 1.600 sequence_1: DEF SEQPC targname: # config: PC opmode: IMAGE aperture: PCALL sp_element: F569W num_exp: 1 time_per_exp: 14S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES ! linenum: 2.100 sequence_1: DEF SEQWFC targname: # config: WFC opmode: IMAGE aperture: WFALL sp_element: F336W num_exp: 1 time_per_exp: 16S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES req_1: GROUP 2.1-2.6 WITHIN 12H; req_2: PCS MODE F /2.1-2.6; req_3: SAME POS FOR 2.2-2.6 AS 2.1; ! linenum: 2.200 sequence_1: DEF SEQWFC targname: # config: WFC opmode: IMAGE aperture: WFALL sp_element: F336W num_exp: 1 time_per_exp: 30S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES ! linenum: 2.300 sequence_1: DEF SEQWFC targname: # config: WFC opmode: IMAGE aperture: WFALL sp_element: F439W num_exp: 1 time_per_exp: 10S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES ! linenum: 2.400 sequence_1: DEF SEQWFC targname: # config: WFC opmode: IMAGE aperture: WFALL sp_element: F439W num_exp: 1 time_per_exp: 20S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES ! linenum: 2.500 sequence_1: DEF SEQWFC targname: # config: WFC opmode: IMAGE aperture: WFALL sp_element: F569W num_exp: 1 time_per_exp: 4S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES ! linenum: 2.600 sequence_1: DEF SEQWFC targname: # config: WFC opmode: IMAGE aperture: WFALL sp_element: F569W num_exp: 1 time_per_exp: 8S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES ! linenum: 3.100 sequence_1: DEF SEQ6PC targname: # config: PC opmode: IMAGE aperture: PC6 sp_element: F336W num_exp: 1 time_per_exp: 40S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES req_1: GROUP 3.1-3.6 WITHIN 12H; req_2: PCS MODE F /3.1-3.6; req_3: SAME POS FOR 3.2-3.6 AS 3.1; ! linenum: 3.200 sequence_1: DEF SEQ6PC targname: # config: PC opmode: IMAGE aperture: PC6 sp_element: F336W num_exp: 1 time_per_exp: 80S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES ! linenum: 3.300 sequence_1: DEF SEQ6PC targname: # config: PC opmode: IMAGE aperture: PC6 sp_element: F439W num_exp: 1 time_per_exp: 20S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES ! linenum: 3.400 sequence_1: DEF SEQ6PC targname: # config: PC opmode: IMAGE aperture: PC6 sp_element: F439W num_exp: 1 time_per_exp: 40S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES ! linenum: 3.500 sequence_1: DEF SEQ6PC targname: # config: PC opmode: IMAGE aperture: PC6 sp_element: F569W num_exp: 1 time_per_exp: 7S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES ! linenum: 3.600 sequence_1: DEF SEQ6PC targname: # config: PC opmode: IMAGE aperture: PC6 sp_element: F569W num_exp: 1 time_per_exp: 14S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES ! linenum: 11.000 sequence_1: USE SEQPC targname: NGC346 req_1: CYCLE 3/11-15; ! linenum: 12.000 sequence_1: USE SEQ6PC targname: HD32228 ! linenum: 13.000 sequence_1: USE SEQWFC targname: LUCKE-HODGE10 ! linenum: 14.000 sequence_1: USE SEQWFC targname: NGC2044 ! linenum: 15.000 sequence_1: USE SEQWFC targname: 30DORADUS-B ! ! end of exposure logsheet ! No scan data records found