! File: 3726C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:17:31:31 coverpage: title_1: GLOBULAR CLUSTERS IN M31 sci_cat: STELLAR POPULATIONS sci_subcat: GLOBULAR CLUSTERS proposal_for: GO pi_title: PROF. pi_fname: FLAVIO pi_lname: FUSI PECCI pi_inst: BOLOGNA OBSERVATORY pi_country: ITALY pi_phone: +39-51-259321 keywords_1: EXT-CLUSTER hours_pri: 2.50 num_pri: 2 foc: Y pi_position: PROFESSOR off_fname: BRUNO off_lname: MARANO off_title: DIRECTOR off_inst: BOLOGNA OBSERVATORY off_addr_1: VIA ZAMBONI 33 off_city: BOLOGNA off_zip: 40126 off_country: ITALY off_phone: +39-51-259404 off_telex: 520634 INFNBO I ! end of coverpage abstract: line_1: The original aim of this proposal was to observe 27 globular clusters line_2: in M31 using FOC/96 over a period of three years with the following line_3: scientific rationale: a) during cycle 2 and 3, B and UV images in order line_4: to obtain surface brightness profiles and blue upper parts of CMDs line_5: (e.g. Post-AGB and blue HB stars). This is essential for understanding line_6: the dynamical properties of the clusters and the galaxy, and the stellar line_7: population characteristics also in comparison with other LG galaxies line_8: (MW, MCs). 13 clusters are planned to be observed in cycle 1 in B and line_9: surface brightness profiles have been obtained. b) On the assumption that line_10: in cycle 4 HST is restored to its original optical performance, we proposed line_11: to observe 10 top-priority clusters using B and V filters, in order to line_12: obtain accurate (0.1 mag) CMDs down to the HB level. This would allow to line_13: derive the slope of the HB luminosity vs metallicity relation, a key line_14: ingredient in globular cluster distance and age determinations, with well line_15: known cosmological implications. Within this framework, the TAC has line_16: recommended that the time allocated to this proposal (2.5hrs) be used to line_17: observe one cluster in two filters during cycle 2, in order to line_18: test the feasibility and obtain the blue upper part of the CMD line_19: (i.e. UV-bright, Post-AGB and blue HB stars). ! ! end of abstract general_form_proposers: lname: FUSI PECCI fname: FLAVIO title: PI inst: BOLOGNA OBSERVATORY country: ITALY esa: Y ! lname: BATTISTINI fname: PIERLUIGI inst: UNIVERSITY OF BOLOGNA country: ITALY esa: Y ! lname: BENDINELLI fname: ORAZIO inst: UNIVERSITY OF BOLOGNA country: ITALY esa: Y ! lname: BONOLI fname: FABRIZIO inst: UNIVERSITY OF BOLOGNA country: ITALY esa: Y ! lname: CACCIARI fname: CARLA inst: BOLOGNA OBSERVATORY country: ITALY esa: Y ! lname: FEDERICI fname: LUCIANA inst: BOLOGNA OBSERVATORY country: ITALY esa: Y ! lname: PARMEGGIANI fname: GIANLUIGI inst: BOLOGNA OBSERVATORY country: ITALY esa: Y ! lname: ZAVATTI fname: FRANCO inst: UNIVERSITY OF BOLOGNA country: ITALY esa: Y ! lname: BUONANNO fname: ROBERTO inst: ROMA OBSERVATORY country: ITALY esa: Y ! lname: KING fname: IVAN mi: R. inst: UNIVERSITY OF CALIFORNIA, BERKELEY country: USA ! lname: WALTERBOS fname: RENE' inst: NEW MEXICO STATE UNIVERSITY country: USA ! lname: DJORGOVSKI fname: GEORGE mi: S. inst: CALTECH country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 0 line_1: ! question: 3 section: 0 line_1: Target: G351 (globular clusters in M31) line_2: Distance modulus (m-M)v = 24.4 line_3: Total integrated apparent magnitude of the cluster: V = 15.18 line_4: Integrated colour: B-V = 0.72 line_5: Angular size: 8 arcsec line_6: Reddening: E(B-V) = 0.10 + contribution within M31 (small) line_7: Proposed observations: FOC/96 with F342W and F140W (one exposure line_8: in each filter) line_9: The exposure times have been calculated in order to obtain line_10: approximately S/N=7 for a typical Post-AGB star with T=30,000K line_11: and logL/Lo=3.1, such as vZ1128 in M3, and S/N= 7-9 for line_12: a UV-bright star with T=22,500K and logL/Lo=3.1 such as K559 in line_13: M15. Fainter UV-bright stars will also be detectable, although line_14: with a lower S/N. ! question: 4 section: 0 line_1: Even in its present degraded optical situation, HST still has capabilities that line_2: are unmatched by ground-based instruments, namely the spatial resolution and line_3: the possibility of observing in the UV range. line_4: Post-AGB and Hot HB stars can efficiently be observed only in the UV range, line_5: and because the crowding is not severe in this wavelength range they can line_6: easily be detected and measured with a good degree of photometric accuracy. line_7: Observations in the U filter allow the construction of a CMD, which provides line_8: information on the hot stellar population of the cluster. ! question: 6 section: 0 line_1: For the data reduction a good knowledge of the PSF is important line_2: in order to obtain as accurate as possible photometric information line_3: on individual stars. Given the very limited amount of time granted line_4: to the program, however, we plan to use the PSFs available in the line_5: library either from theoretical models or from previous standard line_6: calibration observations. ! question: 7 section: 0 line_1: Data reduction and analysis will be performed mainly: a) in Rome as far line_2: as the properties of individual stars are concerned, and b) in Bologna line_3: for features of the integrated surface brightness. We also expect to spend line_4: a significant amount of time (1-2 months) at the STScI and/or ST-ECF for line_5: getting acquainted with particular aspects/problems, especially during line_6: the initial phase of data reduction. line_7: To achieve the goals of a), we have already started checks and simulations line_8: using both synthetic and HST-SV images and the photometric package ROMAFOT line_9: (Buonanno et al. 1983, integrated with some routines by Bendinelli et al.), line_10: which has been recently optimized for HST image reduction taking into account line_11: both PSF features and problems related to sampling and flat-fielding. line_12: Star photometry will also be performed using the Malumuth technique which line_13: exploits the bright small cores of HST images to achieve better star line_14: separation near the cluster centers. line_15: REFERENCES line_16: Buonanno,R., Buscema,G., Corsi.C.E., Ferraro,I., Iannicola,G.,1983, Astron. line_17: Astrophys. 126, 278 line_18: Malumuth, E.M., Neill,J.D., Lindler,D.J., Heap,S.R., 1990, B.A.A.S. 22, 1276 ! question: 8 section: 0 line_1: We plan to measure accurate target positions using GASP frames. line_2: This can be done at ST-ECF, as it was done in previous occasions. ! question: 9 section: 0 line_1: GO Program 2583: Surface Photometry of a Sample of Globular line_2: Clusters in M31. line_3: This program is strictly related to the present project. line_4: Only part of the observations have been taken at the present time. line_5: The data are extremely good for the purpose of deriving surface line_6: photometry, and the preliminary reduction shows excellent surface line_7: brightness profiles. The results will be presented at the line_8: forthcoming HST Workshop in Baia Chia (Sardinia, Italy, June-July line_9: 1992), and a paper is in preparation. ! question: 10 section: 0 line_1: Computing: line_2: Bologna: one VAX 8530, one VAX 8800, 3 Microvaxes, 3 DEC 3100 Workstations, line_3: 3Gby mass memory, one Gould-DeAnza image processor, one Microvax GPX line_4: workstation, in addition to numerous peripherals. Access to the Cray2 of the line_5: Bologna University is also available. line_6: Rome: 4 Microvaxes and numerous peripherals. line_7: Berkeley: private MicrovaxGPX with 8 Mby + 210 Mby disk, VAX 200 workstation line_8: Caltech: Several VAX-class computers, including one private Microvax GPX. line_9: One Convex C-1. line_10: NMSU (Las Cruces): private Sun Sparc 1+ station with peripherals. line_11: Access to the 3.5-m Apache Point Observatory. line_12: The facilities of the ST-ECF are also available, if needed. line_13: Research Assistants and Students: there are typically 10 graduate students in line_14: Astronomy in Bologna, part of which already working on HST-related projects. line_15: Research assistance will be secured. line_16: Funds: our personal Research Grants are sufficient to cover all the expenses line_17: conceivably required to complete this project. line_18: A separate request for funding will be submitted by our U.S. co-investigators. ! !end of general form text general_form_address: lname: FUSI PECCI fname: FLAVIO title: PROF. category: PI inst: BOLOGNA OBSERVATORY addr_1: VIA ZAMBONI 33 city: BOLOGNA zip: 40126 country: ITALY phone: +39-51-259321 telex: 520634 INFNBO I ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: G351 name_2: BO405 descr_1: D, 201 pos_1: RA = 00H 49M 39.78S +/- 0.3", pos_2: DEC = +41D 35' 29.4" +/- 0.3", pos_3: PLATE-ID = 01JV equinox: 2000 comment_1: FLUX1= CLUSTER INTEGR. V comment_2: FOR ACQ ONLY comment_3: FLUX2,3 REFER TO PAGB STAR comment_4: B=24.0, B-V=-0.40 fluxnum_1: 1 fluxval_1: V=15.18 +/- 0.1, B-V=0.72 fluxnum_2: 2 fluxval_2: F(1360)=26 +/- 1 E-18 fluxnum_3: 3 fluxval_3: F(3360)=24 +/- 1 E-19 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: G351 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F342W num_exp: 1 time_per_exp: 1680S s_to_n: 7 fluxnum_4: 3 priority: 1 req_1: CYCLE 2 ! linenum: 2.000 targname: G351 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F140W num_exp: 1 time_per_exp: 4560S s_to_n: 7 fluxnum_2: 2 priority: 1 req_1: CYCLE 2 ! ! end of exposure logsheet ! No scan data records found