! $Id: 5485,v 11.1 1994/08/04 16:11:00 pepsa Exp $ coverpage: title_1: LONG PERIOD VARIABLES OF M81 sci_cat: GALAXIES & CLUSTERS sci_subcat: STELLAR POPULATIONS proposal_for: GO longterm: 2 cont_id: 4348 pi_fname: SHAUN pi_mi: M pi_lname: HUGHES pi_inst: 3100 pi_country: USA pi_phone: 818 395 4024 hours_pri: 3.00 num_pri: 2 wf_pc: Y time_crit: Y off_fname: EARL off_lname: FREISE off_title: DIRECTOR OF RESEARCH off_inst: 1590 off_addr_1: CALTECH off_addr_2: MS 213-6 off_city: PASADENA off_state: CA off_zip: 91125 off_country: USA off_phone: 818 395 6357 ! end of coverpage abstract: line_1: This is part of a very long term project to identify Long-Period line_2: Variables (LPVs) in external galaxies. Most LPVs are members of the line_3: Asymptotic Giant Branch (AGB), and hence one of the main reasons for line_4: studying the LPVs will be to understand the AGB, and how it varies in line_5: nearby galaxies. So far the only AGB LPVs to be identified in external line_6: galaxies are those in the Magellanic Clouds. Ground based programs are line_7: currently underway to identify the AGB LPVs in M31 and M32, and using line_8: HST to identify the LPVs in a galaxy beyond the local group will tell line_9: us how important a part galactic environment plays in the formation of line_10: AGB progenitor stars (ie initial main sequence masses of between line_11: 0.8 and 9 solar masses). An important bonus of studying LPVs is that line_12: they possess a precise PL relation, which will be a very useful check line_13: against the distance derived from Cepheids in the H_0 key project line_14: (Program No. 2227). ! ! end of abstract general_form_proposers: lname: HUGHES fname: SHAUN mi: M inst: 3100 country: USA ! lname: MOULD fname: JEREMY mi: R inst: 3100 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Our program aims to detect and measure accurate periods and line_2: magnitudes of Long-Period Variables (LPVs) in two M81 fields line_3: (denoted V30 and major axis). To avoid severe period aliases, line_4: we will need to obtain well-sampled light curves. The epochs line_5: of previous cycles' data have been used to search for gaps in line_6: LPV phase space, and the dates specified for cycle 4 have been line_7: carefully chosen to fill these gaps. However, as LPVs have line_8: periods of between 100 and 1000 days, we can tolerate a reasonably line_9: large scatter (+/- 10 days) about the ideal sampling times listed line_10: below. line_11: To ensure good phase coverage for the maximum number of stars line_12: it is very important for each epoch to be oriented orthogonally line_13: (ie +/- Nx90 deg) to the previous epochs' field orientations. line_14: We have obtained output from the RUN-ORIENT program to determine line_15: the allowable dates for the correct orientation for each exposure. line_16: This gives us 4 windows per year (one for each orientation), two of line_17: which last 60 days, and the other two lasting only 10 days. line_18: To obtain accurate periods, we shall need ~18 epochs in total. line_19: After the completion of cycle 3 in 1993 December, we expect to line_20: have 11 F785LP epochs (each of between 1600 and 1800 sec) of each line_21: of the two M81 fields, and therefore we shall need a further 7 line_22: epochs to complete the program. In cycle 4 we have been allocated line_23: enough time for 4 epochs (using the F814W filter, each being 300 sec). ! question: 3 section: 2 line_1: ! question: 4 section: 1 line_1: So far the only AGB LPVs to be identified in external galaxies line_2: are those in the Magellanic Clouds. Ground based programs are line_3: currently underway to identify the AGB LPVs in M32, which is at line_4: the limit of current ground-based observations. Using HST to line_5: identify the LPVs in a galaxy beyond the local group will tell line_6: us how important a part galactic environment plays in the formation line_7: of AGB progenitor stars (ie initial main sequence masses of 0.8 to line_8: 9 solar masses). An important bonus of studying LPVs is that line_9: they possess a precise P-L relation, which will be a very useful line_10: check against the distance derived from Cepheids in the H_0 key line_11: project (Program No. 2227). ! question: 5 section: 1 line_1: TIME CRITICAL: As described in Q3 above, the dates chosen in the line_2: EXPOSURE_LOGSHEET are such as to fill gaps in the LPV periods' line_3: phase space, while at the same time allowing orthogonal orientations line_4: to previous epochs, thereby maximising the sampling of light curves. line_5: Because the periods of LPVs are 100 to 1000 days, reasonable line_6: tolerance about these dates (+/- 10 days) is allowed. ! question: 6 section: 1 line_1: No calibration exposures are required. ! ! question: 9 section: 1 line_1: 4348GO: Long Period Variables of M81. Hughes and Mould. line_3: 2227GO: The Extragalactic Distance Scale I. M81. H_0 team. line_4: 3905GO: The Extragalactic Distance Scale II. M81 & M101. H_0 team. line_5: 4658GO: The Extragalactic Distance Scale III. M101. H_0 team. line_7: The first program initiated the M81 LPV survey, and is for an line_8: anticipated 4 epochs in each of the two M81 fields in cycle 3 (with line_9: possibly two more epochs should the refurbishment mission be delayed). line_10: The last 3 programs are aimed at finding Cepheids in galaxies line_11: beyond the local group, and eventually out to the Virgo group. The line_12: first and nearest galaxy to be observed was M81, and in cycles 1 and line_13: 2, 18 and 6 epochs were obtained in F555W and F785LP, in two fields line_14: of M81. The F785LP frames will be used as part of the data for this line_15: LPV proposal. line_16: From the cycle 1 and 2 data, 37 Cepheid candidates have been line_17: identified. The entire data set has been calibrated against line_18: ground-based photometry (Palomar 200-inch) of the brightest stars in line_19: each of the fields. The Cepheid colors were used to estimate internal line_20: extinction, and have yielded an accurate distance to M81, the first line_21: step in measuring H_0 to better than 10%. ! question: 10 section: 1 line_1: A computer workstation, with associated hard disk and exabyte drive, line_2: will be used to reduce and analyse the data. ! !end of general form text general_form_address: lname: HUGHES fname: SHAUN mi: M category: PI inst: 3100 addr_1: PALOMAR OBSERVATORY addr_2: CALTECH, 105-24 city: PASADENA state: CA zip: 91125 country: USA phone: 818 395 4024 telex: smh@phobos.caltech.edu ! lname: category: CON ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC3031-FIELD name_2: NGC3031-MAJOR-AXIS descr_1: E,301,B,145,175 pos_1: RA=09H 51M 02.6S +/- 2", pos_2: DEC=+69D 23' 15" +/- 2" equinox: 1950 pm_or_par: N rv_or_z: V=80 comment_1: MAJOR-AXIS FIELD fluxnum_1: 1 fluxval_1: SURF(V)=25 +/- 1.0 fluxnum_2: 2 fluxval_2: SURF(I)=25 +/- 1.0 ! targnum: 2 name_1: NGC3031-V30 descr_1: E,301,B,145,175 pos_1: RA=09H 52M 03.5S +/- 2", pos_2: DEC=+69D 21' 18" +/- 2" equinox: 1950 pm_or_par: N rv_or_z: V=80 comment_1: V30 FIELD fluxnum_1: 1 fluxval_1: SURF(V)=25 +/- 1.0 fluxnum_2: 2 fluxval_2: SURF(I)=25 +/- 1.0 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 4.100 sequence_1: DEFINE sequence_2: ICYC4 targname: # config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 300S s_to_n: 10 fluxnum_1: 2 priority: # param_1: CR-SPLIT=NO req_1: AT 21-OCT-94 +/- 2D; req_2: ORIENT -56.6D +/- 0.2D; req_3: POS TARG +10, +10; comment_1: THIS POSITION PUTS TARGET ON APEX comment_2: AT V3PA = 123.4D (IE +0D OFF NOM) comment_3: ON DAY 1994.294 (1994 OCT 21) ! linenum: 4.200 sequence_1: DEFINE sequence_2: ICYC4 targname: # config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 300S s_to_n: 10 fluxnum_1: 2 priority: # param_1: CR-SPLIT=NO req_1: AFTER 4.1 BY 23D +/- 2D; req_2: SAME POS FOR 4.2 AS 4.1; comment_1: THIS IS ROTATED 0D WRT 4.1 comment_2: AT V3PA = 123.4D (IE +18D OFF NOM) comment_3: ON DAY 1994.317 (1994 NOV 13) ! linenum: 4.300 sequence_1: DEFINE sequence_2: ICYC4 targname: # config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 300S s_to_n: 10 fluxnum_1: 2 priority: # param_1: CR-SPLIT=NO req_1: AFTER 4.1 BY 74D +/- 2D; req_2: ORIENT -90.0D +/- 3.0D FROM 4.1; req_3: POS TARG +10, +10; comment_1: THIS IS ROTATED -90D WRT 4.1 comment_2: AT V3PA = 33.4D (IE -20D OFF NOM) comment_3: ON DAY 1995.003 (1995 JAN 3) ! linenum: 4.400 sequence_1: DEFINE sequence_2: ICYC4 targname: # config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 300S s_to_n: 10 fluxnum_1: 2 priority: # param_1: CR-SPLIT=NO req_1: AFTER 4.1 BY 163D +/- 2D; req_2: ORIENT +180.0D +/- 3.0D FROM 4.1; req_3: POS TARG +10, +10; comment_1: THIS IS ROTATED 180D WRT 4.1 comment_2: AT V3PA = 303.4D (IE -13D OFF NOM) comment_3: ON DAY 1995.092 (1995 APR 2) ! linenum: 40.000 sequence_1: USE sequence_2: ICYC4 targname: NGC3031-FIELD priority: 1 req_1: CYCLE 4 / 4.1 - 4.4; req_2: CYCLE 4 / 40 - 41 ! linenum: 41.000 sequence_1: USE sequence_2: ICYC4 targname: NGC3031-V30 priority: 2 ! ! end of exposure logsheet ! No scan data records found