! File: 3094C.PROP ! Database: PEPDB ! Date: 18-FEB-1994:16:43:07 coverpage: title_1: RECOVERY OF THE HISTORICAL NOVA IN M14 - SPECTROSCOPY sci_cat: STELLAR ASTROPHYSICS proposal_for: SAT/FOS pi_title: PROF. pi_fname: BRUCE pi_lname: MARGON pi_inst: WASHINGTON, UNIVERSITY OF pi_country: USA pi_phone: 206-543-0089 keywords_1: NOVA, GLOBULAR CLUSTER hours_pri: 3.86 num_pri: 2 wf_pc: X foc: X fos: X pi_position: CHAIR AND PROFESSOR ! end of coverpage abstract: line_1: Imaging and spectroscopy will be used in an attempt to recover the line_2: historical nova in the globular cluster M14. Similar attempts line_3: from the ground are tantalizing, but inclusive. The proposed line_4: observations will also more generally test the feasibility of line_5: both HST spectroscopy and imaging in crowded fields. ! ! end of abstract general_form_proposers: lname: BEAVER fname: EDWARD inst: UC, SAN DIEGO country: USA ! lname: BURBIDGE fname: E. MARGARET inst: UC, SAN DIEGO country: USA ! lname: MARGON fname: BRUCE inst: WASHINGTON, UNIVERSITY OF country: USA ! lname: ANGEL fname: J. ROGER mi: P. inst: ARIZONA, UNIVERSITY OF country: USA ! lname: BARTKO fname: FRANK inst: MARTIN MARIETTA CORPORATION country: USA ! lname: DAVIDSEN fname: ARTHUR mi: F. inst: JOHNS HOPKINS UNIVERSITY country: USA ! lname: HARMS fname: RICHARD mi: J. inst: APPLIED RESEARCH CORPORATION country: USA ! lname: BOHLIN fname: RALPH inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: FORD fname: HOLLAND mi: C. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: The proposed observations will test the feasiblity of both line_2: spectroscopy and imaging in crowded fields through an attempt to line_3: recover the historical nova in the globular cluster M14. A wide line_4: variety of observing programs currently planned for HST rely on line_5: taking FOC or WF/PC images as EARLY ACQs for follow-up line_7: spectroscopy in confused or crowded fields. Due to the present HST line_9: image quality, there is considerable uncertainty about the line_10: feasiblity of such programs. A major hope in this regard is that line_11: (in certain situations), much of the original spatial resolution line_12: of such EARLY ACQ images can be recovered via image deconvolution line_13: or reconstruction techniques. It is especially those cases of high line_14: color contrast (e.g, a UV object in a field of red stars) that hold line_15: the most promise for these techniques. Additionally, spectra taken line_16: through small apertures in a wavelength regime where there is high line_17: color contrast between the object of interest and the confusing line_18: background, may also still allow much of the original science to line_19: be accomplished despite the current reduced capability for line_20: spatially resolved spectra. line_21: Globular clusters (hereafter, GCs) provide an excellent line_22: end-to-end test of such difficult imaging/spectroscopic programs. ! question: 2 section: 2 line_1: The large number of stars available allow an accurate empirical line_2: characterization of the PSF, and deconvolution/reconstruction line_3: techniques seem to work quite well in GCs. The range in magnitudes line_4: of the stars available allow useful tests on how faint one can line_5: push such image deconvolution/reconstruction techniques. Because line_6: much of the light from a typical GC is rather red (e.g., because line_7: of the dominance of K giants), even spectra of blue/UV objects may line_8: also still be feasible in crowded fields: the "background" from line_9: red stars being substantially suppressed at these blue/UV line_10: wavelengths. Among the blue/UV globular cluster objects of line_11: particular interest are those with bright accretion disks, such as line_12: are found in close, mass-transfer binaries (e.g., see GTO proposal line_13: no. 1053, from which this SAT proposal is derived). line_14: Recent theoretical work suggests that a small number of close line_15: binaries (defined here to be binaries with orbital periods of a line_16: few days or less) may dominate the dynamic evolution of GCs (e.g., line_17: Elson et al. 1987). Because of their high BINARY orbital line_18: velocities, just a handful of such close binaries in a GC can line_19: store as much kinetic energy as the combined kinetic energy line_20: associated with the CLUSTER orbital motions of all 100,000 line_21: single stars in the GC. This binary-orbital energy may line_22: be liberated by three-body encounters of single stars with the ! question: 2 section: 3 line_1: binaries, and is likely to be the dominant source of kinetic line_2: energy needed to counterbalance the kinetic energy sinks of stars line_3: escaping from the GC. The GC binaries may be primordial, or may line_4: have formed later through encounter processes, especially during line_5: collapse of the cluster core. Elson et al. have pointed out the line_6: analogy of this energy source to thermonuclear fusion in stars: in line_7: this case, the GC collapses, forms binaries, and then "burns" the line_8: orbital kinetic energy via encounters. Although this provides an line_9: elegant theoretical picture, from an observational point of view, line_10: it should be noted that there are only a handful of confirmed line_11: close binaries known in GCs. Thus it remains highly desirable to line_12: observationally confirm some of the suspected, but less secure, line_13: candidate close binaries in globular clusters. line_14: A particularly interesting candidate GC close binary is the line_15: historical nova in M14, reported to have undergone an outburst in line_16: 1938 (e.g., see discussion in Hogg and Wehlau 1964, Shara et al. line_17: 1986). Shara et al. (1986) and Shara et al. (1990) have undertaken line_18: ground based work toward the recovery of the nova. From multicolor line_19: imaging, they've found a B=20 object which is ultraviolet (in U-B) line_20: compared to other stars in the cluster. Further, they have even line_21: taken a spectrum from the ground which possibly shows the presence line_22: of H-alpha emission from some object included in their slit. ! question: 2 section: 4 line_1: Unfortunately, the field is sufficiently crowded that Shara et al. line_2: are still unable to provide a precise optical identification from line_3: the ground, nor confirm with a high degree of certainty the line_4: presence of H-alpha emission. line_5: An attempt to recover the M14 nova with both HST imaging and line_6: spectroscopy will allow for direct comparison of HST observations line_7: with the already existing high quality (but inconclusive) ground line_8: based observations. The proposed HST images will be used to line_9: identify the old nova from its UV color and H-alpha emission. If a line_10: nova shell is present (which could be seen in the light of line_11: H-alpha), an expansion parallax may also be determinable, yielding line_12: an accurate distance to both the nova, and by its membership, the line_13: GC. For these reasons, we have chosen to take F342W and F430W line_14: images with the FOC plus an F656N image with the PC. The FOC and line_15: PC images will be examined to precisely locate a candidate of line_16: unusual color relative to other GC stars in the field. This may line_17: require use of sophisticated image deconvolution/reconstruction line_18: techniques; although the M14 nova is displaced from the core by line_19: about 30", the crowding is still high. Unfortunately, image line_20: deconvolution/reconstruction requires very high S/N, at least of line_21: order S/N=30 (Evans, private communication). We have chosen line_22: integration times of 2500s each in F342W and F430W to achieve such ! question: 2 section: 5 line_1: a S/N for the nova, while retaining an expected spatial resolution line_2: (after deconvolution/reconstruction) of at least 0.1-0.2". The line_3: F656N, H-alpha image will provide essential, strong confirmation line_4: of the candidate, and is needed to search for a possible nova line_5: shell. The 2500s exposure time chosen for the H-alpha image will line_6: provide comparable S/N, but at a poorer effective spatial line_7: resolution of about 0.2"-0.3" (i.e., we will have to further bin line_8: pixels to recover high S/N if deconvolution/reconstruction is line_9: required for the H-alpha image). Because we are looking for a UV line_10: bright object in a field of UV-weak stars (i.e, red K giants), the line_11: color contrast thus implied will further aid in analyzing the line_12: deconvolved images, and perhaps even allow recovery without the line_13: need for sophisticated deconvolution. line_14: A 2500sec confirming prism spectrum with the FOS will follow line_15: after the candidate has been selected from the FOC and PC images. line_16: Based on results from the FOS Simulator (corrected for the line_17: existing poorer HST PSF), we expect to get a S/N in the continuum line_18: of about 10 in such a 2500s exposure through the 0.5" aperture. line_19: The 0.5" aperture is chosen over the 1" aperture to limit line_20: "background" contamination from the nearby stars. This prism line_21: spectrum includes the spectral range of about 2200-7000A, and line_22: should provide strong spectral confirmation of the candidate ! question: 2 section: 6 line_1: chosen from the images; e.g., we expect to see strong Balmer as line_3: well as UV emission lines. At least in the blue/UV portion of this line_4: spectrum, we expect a marked improvement over the existing ground line_5: based spectrum because of significant reduction in contamination line_6: from nearby stars (precise positioning and a small aperture), and line_7: because of suppression of the contaminating (red) background light line_8: in the blue/UV. ! question: 3 section: 1 line_1: FOC and WF/PC images of globular cluster nova were line_2: obtained as EARLY ACQ for FOS spectra in proposal 3002. line_3: This proposal performs the follow-on spectroscopy based on line_4: those images. line_6: Note that we will be doing a pseudo-EARLY ACQ. We will need line_7: the same guide stars for both parts of this proposal (72H line_8: separation). We will also need to perform a realtime slew line_9: after the guide star acquisition of part 2 (hence the REQ line_10: UPLINK on line 6), but prior to the INT ACQ exposure. We line_11: will then need the standard donwlink/uplink for the INT ACQ. ! question: 5 section: 1 line_1: The SV prerequisite programs for all FOS observations in line_2: this program are: line_4: Prop ID 2195..FOS Target Acquisition Tests...first line_5: successful binary search acquisition. ! question: 7 section: 1 line_1: Data reduction will be performed at the ST ScI, and the analysis will be line_2: performed using FOS IDT computer facilities. ! question: 8 section: 1 line_1: Candidate for spectroscopy will all appear in FOC and WF/PC images. If line_2: identical guide stars are available for both observations, FOS acquisition line_3: could be significantly faster and more reliable. If not, we will offset from line_4: arbitrary anonymous bright stars in field. ! question: 10 section: 1 line_1: Data analysis, research assistant support, and funding will be provided under line_2: NASA's FOS GTO contract(s). ! !end of general form text general_form_address: lname: MARGON fname: BRUCE category: PI inst: WASHINGTON, UNIVERSITY OF ! lname: DOWNES fname: RONALD category: CON inst: UC, SAN DIEGO addr_1: GODDARD SPACE FLIGHT CENTER addr_2: CODE 936 city: GREENBELT state: MD zip: 20771 country: USA phone: 301 286-4384 ! lname: ANDERSON fname: SCOTT category: CON inst: UNIVERSITY OF WASHINGTON addr_1: ASTRONOMY DEPARTMENT, FM-20 city: SEATTLE state: WA zip: 98195 country: USA phone: 206 685-2392 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC6402-B descr_1: OFFSET STAR B IN GLOBULAR CLUSTER descr_2: WITH OLD NOVA pos_1: RA= 17H 37M 38.36S +/-0.02S, pos_2: DEC = -03D 14' 37.1" +/-0.3", pos_3: PLATE-ID=009I equinox: 2000 comment_1: COORDINATES FROM GSSS, comment_2: REGION S804. ! targnum: 2 name_1: NGC6402-NOVA descr_1: OLD NOVA IN GLOBULAR CLUSTER pos_1: RA-OFF = -0.144S +/- 0.01S, pos_2: DEC-OFF = -4.27" +/- 0.1", pos_3: FROM 1 equinox: 2000 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: NGC6402-B config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 180S priority: 1 req_3: SEQ 1-5 NO GAP; req_4: CYCLE 0/1-10; comment_1: OBTAIN A MAP OF THE comment_2: FIELD AS A EARLY ACQ comment_3: AS DONE BY GHRS. ! linenum: 2.000 targname: NGC6402-B config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ priority: ^ req_1: POS TARG 2.15,2.15 ! linenum: 3.000 targname: NGC6402-B config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ priority: ^ req_1: POS TARG 2.15,-2.15 ! linenum: 4.000 targname: NGC6402-B config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ priority: ^ req_1: POS TARG -2.15,-2.15 ! linenum: 5.000 targname: NGC6402-B config: ^ opmode: ^ aperture: ^ sp_element: ^ num_exp: ^ time_per_exp: ^ priority: ^ req_1: POS TARG -2.15,2.15 ! linenum: 6.000 targname: NGC6402-B config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 180S priority: 1 req_1: REQ UPLINK; req_2: INT ACQ FOR 7; req_3: AFTER 5 BY 72H+/-12H; comment_1: USE THE SAME GUIDE STARS comment_2: AS LINES 1-5. A REALTIME comment_3: SLEW IS NEEDED PRIOR TO comment_4: THIS EXPOSURE BASED ON comment_5: THE IMAGES TAKEN IN LINES comment_6: 1-5 (SEE GF QUESTION 3). ! linenum: 7.000 targname: NGC6402-B config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S priority: 1 param_1: SEARCH-SIZE=5, param_2: SCAN-STEP=0.2 req_1: ONBOARD ACQ FOR 8; comment_1: TO FULLY CENTER THE comment_2: TARGET FOR SUBSEQUENT comment_3: BLIND OFFSET. ! linenum: 8.000 targname: NGC6402-B config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 20S priority: 1 param_1: SEARCH-SIZE=3, param_2: SCAN-STEP=0.1 req_1: ONBOARD ACQ FOR 9-10; comment_1: TO FULLY CENTER THE comment_2: TARGET FOR SUBSEQUENT comment_3: BLIND OFFSET, USE A comment_4: LONGER EXPOSURE TIME. ! linenum: 9.000 targname: NGC6402-NOVA config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 360S priority: 1 req_1: SEQ 9-10 NO GAP; comment_1: BLIND POINTING FROM comment_2: STAR B TO NOVA. comment_3: CONFIRMATION IMAGE. ! linenum: 10.000 targname: NGC6402-NOVA config: FOS/RD opmode: ACCUM aperture: 0.5 sp_element: PRISM num_exp: 1 time_per_exp: 4500S priority: 1 ! ! end of exposure logsheet ! No scan data records found