! File: 5245C.PROP ! Database: PEPDB ! Date: 24-FEB-1994:02:50:36 coverpage: title_1: IMAGING THE HOT STELLAR CONTENT OF EARLY TYPE GALAXIES title_2: AS PART OF THE FOC/48 CAMPAIGN sci_cat: GALAXIES & CLUSTERS sci_subcat: STELLAR POPULATIONS proposal_for: GO cont_id: 3728 pi_title: PROF. pi_fname: FRANCESCO pi_lname: BERTOLA pi_inst: UNIVERSITY OF PADOVA pi_country: ITALY pi_phone: 39-49-8293436 hours_pri: 7.52 num_pri: 5 foc: Y funds_amount: 44001 funds_length: 12 funds_date: SEP-92 pi_position: PROF. OF ASTROPHYS. off_fname: ROBERTO off_lname: BARBON off_title: PROFESSOR off_inst: DEPT. OF ASTRONOMY,UNIVERSITY OF PADOVA off_addr_1: VICOLO OSSERVATORIO 5 off_city: PADOVA off_zip: I-35122 off_country: ITALY off_phone: 39-49-8293424 off_telex: 432071 ASTROS I ! end of coverpage abstract: line_1: WE PROPOSE TO IMAGE WITH THE FOC IN THE F/48 CONFIGURATION FIVE line_2: EARLY TYPE GALAXIES IN FOUR PASSBANDS CENTERED AT 1500 A, 2200 A, 2800 A line_3: AND 3400 A. WHEN COUPLED WITH PHOTOMETRY OBTAINED FROM THE GROUND OUR line_4: OBSERVATIONS WILL ALLOW US TO DERIVE COMPLETE SED OF THESE GALAXIES AS A line_5: FUNCTION OF THE DISTANCE FROM THE CENTER. THIS IS A KEY STEP TOWARDS THE line_6: UNDERSTANDING OF STELLAR POPULATIONS - IN PARTICULAR THE ONE RESPONSIBLE line_7: FOR THE UV EMISSION - IN EARLY TYPE GALAXIES AND WILL PROVIDE IMPORTANT line_8: INSIGHT IN THEIR FORMATION AND EVOLUTION. WE PLAN TO OBSERVE NGC 1399, line_9: NGC 2681, NGC 4552, NGC 5018 AND NGC 4627 WHICH SAMPLE A WIDE RANGE OF line_10: INTRINSIC PROPERTIES AS INDICATED BY PREVIOUS IUE OBSERVATIONS. FOR NGC line_11: 4627 THERE IS EVIDENCE OF ONGOING STAR FORMATION AND THE HST WILL BE line_12: ABLE TO SHOW THE CHARACTERISTIC CLUMPINESS. NGC 2681 HAD A STARBUST OF line_13: AGE GREATER THAN 1 GYR. NGC 4552 IS ONE OF THE MOST METAL RICH GALAXY line_14: KNOWN. NGC 1399 HAS THE SAME METALLICITY AND LUMINOSITY OF THE PREVIOUS line_15: GALAXY BUT IS A MUCH STRONGER X-RAY EMITTER. NGC 5018 IS A VERY GOOD line_16: CANDIDATE FOR ONGOING STAR FORMATION. line_17: WE BELIEVE IN THIS WAY WE CAN OBTAIN SED FOR THE TWO-DIMENSIONAL IMAGES line_18: OF EARLY TYPE GALAXIES FROM BROAD BAND IMAGING ALONE. THE CALIBRATION line_19: OF OUR FILTER SYSTEM WILL ALLOW US TO APPLY IT TO THE BIDIMENSIONAL line_20: ANALYSIS OF THE GENERAL SAMPLE OF EARLY TYPE GALAXIES. ! ! end of abstract general_form_proposers: lname: BERTOLA fname: FRANCESCO title: PROF. inst: DEPARTMENT OF ASTRONOMY PADOVA country: ITALY esa: Y ! lname: AMICO fname: PAOLA title: DR. inst: DEPARTMENT OF ASTRONOMY PADOVA country: ITALY esa: Y ! lname: BURSTEIN fname: DAVID title: PROF. inst: ARIZONA STATE UNIVERSITY country: U.S.A. ! lname: DI SEREGO ALIGHIERI fname: SPERELLO title: PROF. inst: OSSERVATORIO ASTROFISICO DI ARCETRI country: ITALY esa: Y ! lname: GREGGIO fname: LAURA title: DR. inst: DEPARTMENT OF ASTRONOMY BOLOGNA country: ITALY esa: Y ! lname: RENZINI fname: ALVIO title: PROF. inst: DEPARTMENT OF ASTRONOMY BOLOGNA country: ITALY esa: Y ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We plan to obtain four images for each of the five galaxies in four line_2: passbands centered at 1500 A, 2200 A, 2800 A and 3400 A in order to measure line_3: the main features of the UV spectral energy distribution (SED). line_4: These data, once calibrated and joined with analogous measurements at line_5: longer wavelengths made from the ground should provide the radial line_6: trend in the spectral energy distribution longward of 1200 A with an line_7: accuracy of 10%. In order to obtain this goal we need to reach a S/N line_8: of at least 20 in the measurement of the smoothly distributed line_9: luminosity within concentric rings centred on the nucleus with line_10: thickness of 0.5 arcsec going from the nucleus up to a distance of line_11: about 7 arcsec, close to the edge of the F/48 field of view. If the UV line_12: radiation is concentrated in clumps instead of being smoothly line_13: distributed (expected if the hot stars are young), these will be line_14: easier to detect. We estimate that we should be able to detect with line_15: S/N=5 an upper main sequence O5V star at the distance of our objects line_16: in about 20 minutes in the F/48 + F150W + F130LP configuration. We line_17: have used the UV fluxes measured within the IUE large aperture (e.g. line_18: Burstein et al. 1988) and the assumption that the radial profiles in line_19: the UV are similar to those in the optical B and V bands to estimate line_20: the expected count rate and S/N ratio in each ring. For example for line_21: NGC 1399 in F/48 + F150W + F130LP we expect a count rate R_S = 4 cnt/s line_22: from the ring with thickness of 0.5 arcsec and mean radius of 7 arcsec line_23: (about 11000 pixel area). Since the background in this configuration ! question: 3 section: 2 line_1: is dominated by the detector dark counts (1.9E-3 cnt/s/px) the formula line_2: (1) on page 79 of the FOC Instrument Handbook (Version 2.0) shows that line_3: S/N=20 is reached in about 20 minutes. Rings at smaller radii all have line_4: higher S/N. Since our objects are all very red we have also evaluated line_5: the amount of red leak present in our UV exposures using the IUE line_6: spectra and the FOC total throughput curves obtained from the ST-ECF line_7: instrument database. The result is that about half of the radiation line_8: recorded in the F/48 + F150W + F130LP configuration is actually line_9: emitted at wavelengths above 2000A. The red leaks in the other filter line_10: configurations are considerably smaller. It is clear that the true line_11: spectral energy distribution will have to be spectrally deconvolved line_12: using our multiwavelength measurements and the FOC throughput curves. line_13: We can also use the IUE spectra to rescale the spectral energy line_14: distribution on an aperture equivalent to the IUE one. ! question: 4 section: 1 line_1: We need the unique imaging capability of HST in the ultraviolet, since this is line_2: the wavelength range where hot stars emit most of their radiation and are not line_3: ovewhelmed by the normal cold stars present in very large numbers in early- line_4: type galaxies. We also exploit the high spatial resolution of HST - still line_5: provided by the sharp core of the aberrated point spread function (PSF) - to line_6: search for the clumpiness in the spatial distribution of the UV radiation line_7: expected if the hot stars are young. We should be able to detect individually line_8: the massive young stars which might be present in our objects, thanks to the line_9: sharp core of the HST PSF and to the good discrimination against red stars in line_10: the UV. The IUE satellite, which we have used extensively to study the UV line_11: spectral energy distribution in early-type galaxies, cannot provide the line_12: detailed spatial information which is necessary to understand the nature of the line_13: hot stars present in these objects. In order to complement the HST observations line_14: it is planned to use the ground base telescopes at LA Silla and Steward line_15: Observatories to which members of our team have regular access. ! question: 5 section: 1 line_1: No special requests ! question: 7 section: 1 line_1: We plan to use the data from the pipeline calibration (RDPS) at STScI. line_2: Eventual recalibration is possible using IRAF/STSDAS and the instrument database line_3: (CDBS). Analysis of the data will be carried out within MIDAS and/or IRAF, line_4: available both in Padova and in Firenze. An important step in the reduction line_5: procedure will be the elimination of the effects of the filter red leak and the line_6: recalibration using IUE spectra. line_7: Members of our team will upgrade our algorithms and reduction procedures so as line_8: to deal with any unespected technical condition. ! question: 8 section: 1 line_1: The PI (F.B.) and A.R. are Co-Is in a scientifically related CYCLE 2 proposal line_2: (PI R. Windhorst) concerning the UV spectroscopy of moderate to high redshift line_3: RADIOGALAXIES. A. R. is PI of a scientifically related Cycle 2 proposal seeking line_4: to determine the evolution with redshift of the main characteristics of the UV line_5: rising branch of ellipticals. D.B. is P.I of two related Cycle 2 proposals. line_6: One is to study the spectral energy distribution of extragalactic globular line_7: clusters and the nuclei of galaxies, including one of the galaxies proposed line_8: here (N1399). The other is to obtain mid-UV FOS spectra of AFG dwarf stars line_9: that can also be used as components of stellar population models. There is a line_10: clear complementarity among the five proposals. We have endeavored to construct line_11: these programs to make maximum use of HST resources. The scientific output of line_12: each of them would be enhanced by the successful completion of the other line_13: projects. ! question: 9 section: 1 line_1: P2791:PAGB STARS IN ELLIPTICAL AND BULGE DOMINATED NEARBY GALAXIES line_2: (P.I. F. Bertola) The GO cycle 1 program received 8.45 hours of spacecraft time, line_3: with HIGH priority. It is related to this project. line_4: P2579: THE CALIBRATION OF THE WHITE DWARF DISTANCE SCALE FOR GLOBULAR CLUSTERS. line_5: (PI A. Renzini) The GO cycle 1 program received 45.80 hours of spacecraft time, line_6: with SUPPLEMENTAL priority. The program then completed the Phase 2, and was line_7: cleared for the HST observations. Subsequent to the spherical aberration line_8: problem the PI asked to DEFER the program to the first HST cycle with fully line_9: recovered WF/PC capabilities. The project 2579 is not closely related to the line_10: present proposal. line_11: P2570: RECENT MASS EJECTION FROM PLANETARY NEBULA NUCLEI.(PI H. BOND) The line_12: GO cycle 1 program received 3.73 hours of spacecraft time, with HIGH priority. line_13: The program then completed the Phase 2, and was cleared for the HST line_14: observations, which are now are scheduled for the summer/fall 1991. line_15: The project is not related to the present proposal. line_16: P2298: STELLAR POPULATIONS OF GLOBULAR CLUSTERS AND GALAXIES line_17: (P.I. D. BURSTEIN) The GO Cycle 1 program received 15 hr. HIGH PRIORITY time. line_18: It is related to the present proposal. line_19: Up to now only the image of NGC 205 has been delivered and we are in the line_20: process of deriving the luminosity function of the stars in the field. ! question: 10 section: 1 line_1: Padova:VAX 8550 + MIDAS reduction package and SUN Sparcstation 2 line_2: Mod. GX + 1.5Gb disk + IRAF reduction package. line_3: ASU: DEC 5000-200 + DEC 3100 workstations, 2.6 Gbyte of disk; associated line_4: I/O devices; in a net with other workstations; access to Cray 4XMP. line_5: IRAF runs on both computers. ! !end of general form text general_form_address: lname: BERTOLA fname: FRANCESCO title: PROF. category: PI inst: DEPARTMENT OF ASTRONOMY addr_1: VICOLO OSSERVATORIO 5 city: PADOVA zip: I-35122 country: ITALY phone: 39-49-8293436 telex: 432071 ASTROS I ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC1399 descr_1: E,303 pos_1: RA = 03H 38M 29.09S +/- 0.1S, pos_2: DEC = -35D 27' 03.5" +/- 1", pos_3: PLATE-ID = 02IX equinox: J2000 rv_or_z: V = 1380 comment_1: THE DATA IN FLUX REFERENCE comment_2: NUMBERS 2 THROU 5 ARE FOR THE comment_3: IUE LARGE SCIENCE APERTURE, comment_4: EQUIVALENT TO A CIRCLE OF comment_5: 7.5 ARCSEC RADIUS. fluxnum_1: 1 fluxval_1: SURF(B) = 20.6 +/- 0.2 fluxnum_2: 2 fluxval_2: F(1500) = 11 +/- 2 E-15 fluxnum_3: 3 fluxval_3: F(2200) = 4.6 +/- 2 E-15 fluxnum_4: 4 fluxval_4: F(2750) = 7.6 +/- 2 E-15 fluxnum_5: 5 fluxval_5: F(3400) = 36 +/- 5 E-15 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.100 targname: NGC1399 config: FOC/48 opmode: IMAGE aperture: 512X1024 sp_element: F150W num_exp: 1 time_per_exp: 25M s_to_n: 20 fluxnum_1: 2 priority: 1 req_1: SAME ORIENT FOR 1.2-1.4 AS 1.1; req_2: CYCLE 2 / 1.1-1.4 ! linenum: 1.200 targname: NGC1399 config: FOC/48 opmode: IMAGE aperture: 512X1024 sp_element: F220W num_exp: 1 time_per_exp: 17M s_to_n: 20 fluxnum_1: 3 priority: 1 ! linenum: 1.300 targname: NGC1399 config: FOC/48 opmode: IMAGE aperture: 512X1024 sp_element: F275W num_exp: 1 time_per_exp: 10M s_to_n: 20 fluxnum_1: 4 priority: 1 ! linenum: 1.400 targname: NGC1399 config: FOC/48 opmode: IMAGE aperture: 512X1024 sp_element: F342W num_exp: 1 time_per_exp: 7M s_to_n: 20 fluxnum_1: 5 priority: 1 ! ! end of exposure logsheet ! No scan data records found