! File: 3880C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:22:45:05 coverpage: title_1: CIRCUMSTELLAR AND INTERSTELLAR ABSORPTION LINES IN PLANETARY title_2: NEBULA CENTRAL STARS sci_cat: INTERSTELLAR MEDIUM sci_subcat: PLANETARY NEBULAE proposal_for: GO pi_title: DR. pi_fname: HARRIET pi_mi: L. pi_lname: DINERSTEIN pi_inst: UNIVERSITY OF TEXAS pi_country: USA pi_phone: 512-471-3449 hours_pri: 10.00 num_pri: 4 foc: Y hrs: Y funds_amount: 44514 funds_length: 12 pi_position: ASSOCIATE PROFESSOR off_fname: STEPHEN off_mi: A. off_lname: MONTI off_title: VICE PROVOST off_inst: UNIVERSITY OF TEXAS AT AUSTIN off_addr_1: OFFICE OF THE VICE PROVOST off_addr_2: MAIN 201 off_addr_3: UNIVERSITY OF TEXAS off_city: AUSTIN off_state: TX off_zip: 78712 off_country: USA off_phone: 512-471-4363 ! end of coverpage abstract: line_1: We propose to use GHRS observations of planetary nebula central stars to line_2: detect and study massive envelopes of residual neutral material around line_3: the ionized gas. Discovery of these envelopes has major implications for line_4: understanding the process that transforms a star from a red giant into a line_5: white dwarf. Previous radio and infrared work has shown that a signifi- line_6: cant fraction of planetaries (20 - 33%) contain 0.1-1 solar masses of line_7: molecules. Neutral atomic material, although harder to detect from the line_8: ground, may be even more common and contain substantial mass. This con- line_9: clusion is supported by the results of a pilot study by the proposers in line_10: the optical Na I lines. Observations of UV resonance lines of abundant line_11: species offer the most sensitive means for detecting neutral material, line_12: and will provide unique information on the physical and velocity line_13: structure of the nebular envelopes. The far-UV also offers the oppor- line_14: tunity to detect small amounts of vibrationally-excited H2. The GHRS line_15: is the only instrument that can provide sensitive measurements of these line_16: faint stars with high enough spectral resolving power to separate the line_17: nebular from interstellar absorption lines and to optimize detection of line_18: weak lines needed to determine accurate column densities. These obser- line_19: vations will also provide serendipitous information about the central line_20: stars and the ISM along new lines of sight through the galactic halo. ! ! end of abstract general_form_proposers: lname: DINERSTEIN fname: HARRIET title: PI mi: L. inst: UNIVERSITY OF TEXAS country: USA ! lname: SNEDEN fname: CHRISTOPHER inst: UNIVERSITY OF TEXAS country: USA ! lname: DANLY fname: LAURA inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: HEAP fname: SARA mi: R. inst: GODDARD SPACE FLIGHT CENTER country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 0 line_1: ! question: 3 section: 1 line_1: HRS OBSERVATIONS line_2: _ line_3: The primary goal of this proposed project is to study line_4: absorption lines produced by neutral circumnebular material line_5: around planetary nebulae, in order to study the properties line_6: of these neutral envelopes. We will use the UV continuum line_7: of the central star as a backdrop, against which the line_8: absorption lines will appear. All of the four targets line_9: in our modified observing plan have been observed by line_10: two of us at the Na D lines in the optical, and are seen line_11: to have a substantial envelope of such neutral material. line_12: Our plan is to observe them with the HRS at a number of line_13: wavelength settings that cover selected spectral features line_14: of interest. Originally we had hoped to observe the line_15: brighter targets with Echelle A; since this is no longer line_16: available, we will observe all of the targets with line_17: G160M. In order to preserve the best spectral resolving line_18: power, necessary to separate close features and to line_19: separate nebular absorptions from interstellar ones line_20: at nearby velocities, we are forced to use the Small line_21: Science Aperture. Unfortunately, this lengthens the line_22: exposure time needed to achieve good S/N. However, use line_23: of the SSA is also important in order to exclude nebular ! question: 3 section: 2 line_1: emission lines (including, possibly, some of the same line_2: lines that we see in absorption line_3: _ line_4: The observations now planned are summarized in the line_5: following table of integration times (in minutes): line_6: ________________________________________________________ line_7: Table 1. HRS Science Exposures (All SSA, G160M) line_8: ________________________________________________________ line_9: Setting Species BD+30 IC418 NGC40 IC3568 line_10: 1224 HI,H2,NV 60 20 - - line_11: 1274 CI 40 10 - - line_12: 1304 OI, SiII 30 10 30 40 line_13: 1346 CII, OI 30 10 30 40 line_14: 1463 CO 2-0,3-0 30 - - - line_15: 1510 CO 1-0 30 10 - - line_16: 1656 CI 30 16 - - line_17: _ line_18: ________________________________________________________ line_19: S/N anticipated 22 25 12 18 line_20: 1-sigma EW in mA 3 3 3 4 line_21: Total Int Time 250M 70M 60M 60M line_22: ________________________________________________________ line_23: _ ! question: 3 section: 3 line_1: The integration times were determined by choosing a value for line_2: the smallest equivalent width we wished to measure. line_3: We calculated the exposure times from formulae given in the GHRS line_4: Instrument Handbook, version 3.0. Example: line_5: GHRS Observation of BD+30 3639 with G160M at 1304A, 0.25 aperture: line_6: F(l) = 1.7e-12 from Feibelman et al. atlas. S(LSA), the line_7: sensitivity of G160M in the 2.0 aperture, is 6.74e11 (Table 4-13 line_8: in the Handbook). The throughput of the SSA is a factor of 4.5 line_9: smaller (Heap et al 1991, Ap.J. Lett., 377, L29), so line_10: S(SSA) = 1.5e11, and count rate c = F(l) x S(SSA) = 0.255/sec. line_11: Since neither scattered light nor dark count is significant, line_12: (S/N) squared = ct, where t is the integration time in line_13: seconds. In order to achieve a 1sigma error of 3.3 mA, so that an line_14: unresolved line of EW=10 mA is measured with 3sigma, line_15: we require S/N = 22 in a resolution element of .071A. line_16: Therefore, the needed integration time is line_17: t = (22)2/.255 sec = 31.6 min. We round this off to 30 minutes. line_18: _ line_19: FOC OBSERVATIONS FOR EARLY ACQUISITION OF HRS TARGETS line_20: _ line_21: Because of possible difficulties in acquiring two of the line_22: target planetary nebula central stars for spectroscopy, due to line_23: the relatively high surface brightness of the nebulae and low ! question: 3 section: 4 line_1: star/nebula contrast, we have added several FOC observations line_2: to our original program. The two objects in question are line_3: BD+30 3639 and IC 3568. These are both compact nebulae, line_4: BD+30 having a diameter of about 4", and IC 3568 of about line_5: 10". In the case of BD+30, VLA observations by Masson line_6: (Ap.J.346, 243 - 1989) show a ring with two relatively line_7: bright patches, empty in the middle, of about 4" in diameter. line_8: Observations of IC 3568 (Balick et al 1987, Astron.J.94, line_9: 948) show a larger region of emission, with perhaps a line_10: central "hole" or at least shallow depression. The IUE line_11: spectra of both of those objects are presented in the IUE line_12: Spectral Atlas of Planetary Nebulae, Central Stars, and line_13: Related Objects (Feibelman et al 1988, NASA Reference line_14: Publication 1203). Each shows continuum throughout the line_15: spectral region 1200-3200 A, and several emission lines. line_16: Some of the line emission may arise in the central star line_17: itself, but other lines, such as C III 1909, may also line_18: be present in the nebula. We therefore have decided to line_19: obtain FOC images in UV light, mimicking as closely as line_20: possible the spectral response of the HRS during acquistion, line_21: in order to decide whether there is a significant risk line_22: that the brightest point in the HRS search field might line_23: be a patch of nebulosity, rather than the central star. ! question: 3 section: 5 line_1: _____________________________________________________________ line_2: Table 2: FOC Exposures (F/96,512x512 for BD,512x1024 for IC) line_3: _____________________________________________________________ line_4: Target Filters Exposure Comment line_5: BD+30 F152M + F6ND 10M Stellar continuum only line_6: BD+30 F195W + F8ND 2M Continuum + Lines line_7: IC3568 F140M + F6ND 4M Stellar continnum only line_8: IC3568 F165W + F8ND 10M Continuum + Lines line_9: _____________________________________________________________ line_10: For each nebula, we selected 2 filters: one to isolate the line_11: stellar continuum as best as possible, and the other to line_12: include all of the strong emission lines seen in the IUE line_13: spectra. The optimum choices are different for the two line_14: cases. Also, because these are bright objects, it is line_15: necessary to insert neutral density filters, in order to line_16: keep the count rate below 5 counts/sec and avoid problems line_17: with non-linearity of response. The exposure times were line_18: chosen to yield a peak S/N ratio of about 25. ! question: 4 section: 1 line_1: The HRS on HST is needed to make further progress on this line_2: project because of its unique ability to obtain high- line_3: dispersion, high S/N ultraviolet spectra of faint stars. line_4: The PI and co-I Sneden have observed the target nebulae line_5: from the ground at Na I, 5889,95A, and detected nebular line_6: absorption features in all four of them. The strengths line_7: of these features range from weak (EW 20-40 mA) in IC3568 line_8: to very strong (EW=300 mA) in BD+30 3639, corresponding line_9: to equivalent H I column densities of 1e19 cm-2 for IC3568 line_10: to 1e21 cm-2 for BD+30. The optical spectral region contains line_11: few other useful absorption lines for studying the line_12: neutral material. Long integrations (>90min) have line_13: yielded detections of the Ca II 3933,63 lines and line_14: K I near 7600A for BD+30 only. The prime spectral line_15: region for resonance lines of abundant ions is the UV. line_16: _ line_17: In view of this, the PI carried out an archival study line_18: of the IUE high-dispersion spectra of these and other line_19: planetary nebula central stars, in hopes of detecting line_20: nebular absorption lines. One of the target nebulae, line_21: BD+30 3639, had already been studied by Pwa, Pottasch, line_22: and Mo (1986, Astr.Ap.164,184), who noted the nebular line_23: features. Most of the features they reported could ! question: 4 section: 2 line_1: arise either in the ionized or in the neutral region. line_2: Our proposed observations will provide higher S/N line_3: measurements, enabling us to decide, for example, line_4: whether certain weaker features such as OI 1304,1306, line_5: absorptions from excited fine-structure levels, and line_6: OI 1358 (an intercombination line), are present. We line_7: also hope to see CO in absorption (never reported line_8: before for BD+30, which has been detected in the line_9: CO millimeter emission lines). line_10: In general, the archival IUE spectra did not line_11: prove tremendously useful. They are limited by line_12: a relatively poor spectral resolution (25-30 km/sec) line_13: and limited dynamic range, which prevents high line_14: S/N measurements from being possible. ! question: 5 section: 1 line_1: In our Phase 1 proposal, we pointed out the potential line_2: difficulties in acquiring the central stars of several line_3: of our targets, given that they are located on a line_4: a bright background, the UV emission of the nebulae. line_5: In particular, during HRS acquistion, the signal line_6: which is used to peak up on is the total brightness line_7: seen with the N2 mirror, therefore the total UV line_8: bandpass of 1200-3200 A. This bandpass contains line_9: a number of potentially bright emission lines. line_10: Using available information about the targets, line_11: their spatial structure as seen in the optical or line_12: radio maps, and their 1200-3200 A spectra as seen line_13: by IUE, we have attempted to estimate a worst-case line_14: scenario, where all of the line emission is concentrated line_15: into a small angular region. In that case, the HRS line_16: acquisition algorithm might possibly become confused line_17: and center on a patch of the nebula rather than on line_18: the central star. In order to avoid this awful line_19: occurrence, we are requesting permission to obtain line_20: UV images with the FOC for early acquistion purposes. line_21: We will examine these images in order to determine line_22: whether such confusion might occur. line_23: _ ! question: 5 section: 2 line_1: As described in question 3 above, we took the two line_2: targets for which this might be an issue, and selected line_3: two bandpasses for each. One bandpass is chosen to line_4: most closely mimic the way the nebula would look in line_5: "white" UV light, the other to best isolate the stellar line_6: continuum. The choices are different for each object line_7: because there IS no FOC filter covering 1200-3200 A; line_8: instead we try to include all substantial emission line_9: lines in the "star + nebula" filter, and to exclude line_10: them in the "star only" filter. ! question: 6 section: 0 line_1: ! question: 7 section: 1 line_1: Pipeline processing of the data by STScI will yield calibrated line_2: spectra in FITS format, that can be read into various data-analysis line_3: packages. The important quantities for this project, such as line_4: equivalent widths, do not require accurate absolute flux calibration, line_5: which would be difficult to achieve in any case with the SSA. line_6: We will determine EW's and wavelengths using IRAS/STDAS or a line_7: custom-made line-fitting program used at Texas (Fitzpatrick and Sneden line_8: 1987, BAAS, 19, 1129). Derivation of column densities from the line_9: measured equivalent widths is straightforward for weak, linear-regime line_10: and curve-of-growth techniques can be used for some stronger lines. line_11: In some cases, it may be useful to undertake multiple-component line_12: modelling of the line profiles. For example, data from Na I line_13: observations taken at higher dispersion on the ground, could be used line_14: to generate input velocities and column densities for fits to line_15: lower-resolution observations with G160M. Danly and Sneden have line_16: experience in these techniques. It also will be important to be line_17: aware of the roles of nebular emission lines and stellar spectral line_18: features. Dinerstein is an expert in emission line studies of line_19: planetary nebulae, and Heap is an expert in the study of the line_20: ultraviolet spectra of planetary nebulae and the properties of line_21: their central stars. ! question: 8 section: 1 line_1: The targets are all listed as sources in the GSC. However, line_2: it will probably be possible to obtain more accurate coordinates, line_3: from Lick Observatory astrographic plate material. Therefore, line_4: although the GSC coordinates are expected to be adequate for line_5: acquiring the objects (apart from the considerations discussed line_6: in question 5), we hope to obtain improved coordinates early line_7: in the planning process (before May 1), with the kind line_8: assistance of colleagues at UC Santa Cruz. ! question: 9 section: 1 line_1: Dinerstein, Sneden: None. line_2: Danly: Program 2644, "The Environments of Starburst Galaxies," PI: line_3: Norman; Co-Is: Blades, Danly, and Heckman. Unrelated project. line_4: Heap: Program 1212: "Highly Evolved Stars of Low Mass". Somewhat, line_5: but not closely related; involves imagery and spectroscopy of 3 line_6: PN central stars, in NGC 7027, NGC 2440, and K648. These line_7: nebulae have very hot, faint central stars. There is no overlap line_8: with our target list. line_9: _ line_10: Heap: Images of NGC 2440 in several filters have been obtained. line_11: The central star is visible in all of them. Additional processing line_12: should yield a value for the temperature of the central star. ! question: 10 section: 1 line_1: Most of the analysis will be carried out at UT Austin, which provides line_2: office space but not salaries for graduate research assistants. We line_3: will use computers and workstations shared by the astronomy line_4: department or by research subgroups of McDonald Observatory. line_5: We request funding for the following items which the University line_6: does not directly support for large projects: partial summer salary, line_7: research assistant salary, travel, publication expenses, long- line_8: distance telephone calls, data storage tapes, etc. ! !end of general form text general_form_address: lname: DINERSTEIN fname: HARRIET mi: L. category: PI inst: UNIVERSITY OF TEXAS addr_1: ASTRONOMY DEPARTMENT addr_2: RLM 15.308 addr_3: UNIVERSITY OF TEXAS city: AUSTIN state: TX zip: 78712 country: USA phone: 512-471-3449 telex: 910-874-1351 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: BD+30D3639 name_2: PK64+05D1 name_3: HD184738 descr_1: A, 184, G, 502 pos_1: RA = 19H 34M 45.326S +/- 0.025S, pos_2: DEC = +30D 30' 58.59" +/- 0.32" equinox: J2000 rv_or_z: V = -68 acqpr_1: BKG comment_1: THE CENTRAL STAR IS A WOLF-RAYET comment_2: STAR, WITH STRONG EMISSION LINES. comment_3: SOME OF THE UV EMISSION LINES comment_4: SEEN WITH IUE MAY ARISE IN THE comment_5: STAR, BUT SOME, E.G. CIII 1909, comment_6: PROBABLY ARISE IN THE NEBULA. fluxnum_1: 1 fluxval_1: V=9.9+/-0.2, TYPE=WC9 fluxnum_2: 2 fluxval_2: F-CONT(1200)=10+/-2E-13 fluxnum_3: 3 fluxval_3: F-CONT(1300)=17+/-2E-13 fluxnum_4: 4 fluxval_4: F-CONT(1400)=22+/-2E-13 fluxnum_5: 5 fluxval_5: F-CONT(1600)=22+/-2E-13 fluxnum_6: 6 fluxval_6: F-CONT(1800)=22+/-2E-13 fluxnum_7: 7 fluxval_7: F-CONT(2500)=8+/-2E-13 fluxnum_8: 8 fluxval_8: F-LINE(1909)=6+/-1E-11 fluxnum_9: 8 fluxval_9: W-LINE(1909)=15+/-5 fluxnum_10: 9 fluxval_10: F-LINE(2300)=4+/-1E-11 ! targnum: 2 name_1: IC418 name_2: PK215-24D1 name_3: HD35914 descr_1: A, 184, G, 502 pos_1: RA = 05H 27M 28.180S +/- .014S, pos_2: DEC = -12D 41' 50.12" +/- 0.2" equinox: 2000 rv_or_z: V=+47 comment_1: THE SPECTRUM RISES STRONGLY comment_2: TOWARDS SHORTER WAVELENGTHS. comment_3: THE LYMAN ALPHA REGION HAS A comment_4: DEEP ABSORPTION WHICH MAY BE PARTLY comment_5: NEBULAR AND PARTLY INTERSTELLAR. comment_6: AT LAMBDA > 2000 A, THE SPECTRUM comment_7: IS FLAT EXCEPT FOR PROMINENT comment_8: EMISSION LINES AT 2320 A comment_9: (BLEND OF OIII, CII, AND comment_10: SI II), AND 2800 A (MG II). fluxnum_1: 1 fluxval_1: V=9.4 +/- 0.2, TYPE=O7F fluxnum_2: 2 fluxval_2: F-CONT(1200)=60+/-10E-13 fluxnum_3: 3 fluxval_3: F-CONT(1300)=105 +/- 15 E-13 fluxnum_4: 4 fluxval_4: F-CONT(1400)=90 +/- 10 E-13 fluxnum_5: 5 fluxval_5: F-CONT(1600)=70 +/- 10 E-13 fluxnum_6: 6 fluxval_6: F-CONT(1800)=55 +/- 5 E-13 fluxnum_7: 7 fluxval_7: F-CONT(2200)=25 +/- 5 E-13 fluxnum_8: 8 fluxval_8: F-CONT(2800)=25 +/- 5 E-13 fluxnum_9: 9 fluxval_9: F-LINE(2320)=9 +/- 1 E-11 fluxnum_10: 9 fluxval_10: W-LINE(2320)=20 +/- 5 ! targnum: 3 name_1: NGC40 name_2: PK120+09D1 name_3: HD826 descr_1: A, 184, G, 502 pos_1: RA = 00H 13M 00.907S +/- .066S, pos_2: DEC = +72D 31' 19.99" +/- 0.3" equinox: 2000 rv_or_z: V = -55 comment_1: THE UV SPECTRUM OF NGC 40 IS comment_2: DOMINATED BY THE LATE WC-TYPE comment_3: CENTRAL STAR, WHICH HAS comment_4: NUMEROUS STRONG EMISSION comment_5: LINES. WE BELIEVE THAT MOST comment_6: OF THE LINE EMISSION AS WELL AS comment_7: CONTINUUM BELOW 2000 A IS DUE comment_8: TO THE CENTRAL STAR. fluxnum_1: 1 fluxval_1: V=11.8 +/- 0.2, TYPE=WC8 fluxnum_2: 2 fluxval_2: F-CONT(1200)=5 +/- 1 E-13 fluxnum_3: 3 fluxval_3: F-CONT(1400)=8 +/- 2 E-13 fluxnum_4: 4 fluxval_4: F-CONT(1600)=5 +/- 2 E-13 fluxnum_5: 5 fluxval_5: F-CONT(2000)=20 +/- 5 E-14 fluxnum_6: 6 fluxval_6: F-CONT(2800)=20 +/- 5 E-14 fluxnum_7: 7 fluxval_7: F-LINE(1560)=24 +/- 4 E-12 fluxnum_8: 7 fluxval_8: W-LINE(1560)=15 +/- 5 fluxnum_9: 8 fluxval_9: F-LINE(2320)=9 +/- 1 E-11 fluxnum_10: 8 fluxval_10: W-LINE(2320)=20 +/- 5 ! targnum: 4 name_1: IC3568 name_2: PK123+34 name_3: HD109540 descr_1: A, 184, G, 502 pos_1: RA = 12H 33M 06.912S +/- .15S, pos_2: DEC = +82D 33' 50.22" +/- 0.3" equinox: 2000 rv_or_z: V = -46 acqpr_1: BKG comment_1: AGAIN, THIS OBJECT HAS A comment_2: CENTRAL STAR WITH A STRONG comment_3: WIND. THE NV 1240A AND CIV comment_4: 1550 LINES PROBABLY COME FROM comment_5: THE CENTRAL STAR, IN VIEW OF comment_6: THEIR P CYGNI PROFILES, BUT comment_7: [C III] 1909, WHICH DOES NOT comment_8: HAVE A P CYGNI PROFILE, comment_9: PROBABLY ARISES IN THE NEBULA. fluxnum_1: 1 fluxval_1: V=12.0 +/- 0.4, TYPE=O5 fluxnum_2: 2 fluxval_2: F-CONT(1300)=11 +/- 1 E-13 fluxnum_3: 3 fluxval_3: F-CONT(1400)=10 +/- 1 E-13 fluxnum_4: 4 fluxval_4: F-CONT(1600)=7 +/- 1 E-13 fluxnum_5: 5 fluxval_5: F-CONT(2000)=4 +/- 1 E-13 fluxnum_6: 6 fluxval_6: F-CONT(2500)=25 +/- 5 E-14 fluxnum_7: 7 fluxval_7: F-LINE(1240)=12 +/- 2 E-12 fluxnum_8: 7 fluxval_8: W-LINE(1240)=10 +/- 3 fluxnum_9: 8 fluxval_9: F-LINE(1550)=6 +/- 1 E-12 fluxnum_10: 9 fluxval_10: F-LINE(1909)=9 +/- 2 E-12 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: BD+30D3639 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F152M, F6ND num_exp: 1 time_per_exp: 10M s_to_n: 25 fluxnum_1: 4 fluxnum_2: 5 priority: 1 req_1: CYCLE 2; req_2: EARLY ACQ FOR 5-14; req_3: GROUP 1-2 NON-INT comment_1: TO INSURE ACCURATE SPATIAL comment_2: REGISTRATION OF LINE AND comment_3: CONTINUUM IMAGES ! linenum: 2.000 targname: BD+30D3639 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F195W, F8ND num_exp: 1 time_per_exp: 2M s_to_n: 25 fluxnum_1: 5 fluxnum_2: 7 fluxnum_3: 8 fluxnum_4: 9 priority: 1 req_1: CYCLE 2; req_2: EARLY ACQ FOR 5-14 ! linenum: 3.000 targname: IC3568 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F140M, F6ND num_exp: 1 time_per_exp: 4M s_to_n: 25 fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 2 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: EARLY ACQ FOR 26-29; req_3: GROUP 3-4 NON-INT comment_1: TO INSURE REGISTRATION ! linenum: 4.000 targname: IC3568 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F165W, F8ND num_exp: 1 time_per_exp: 10M s_to_n: 25 fluxnum_1: 2 fluxnum_2: 5 fluxnum_3: 8 fluxnum_4: 9 priority: 2 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: EARLY ACQ FOR 26-29 ! linenum: 5.000 targname: BD+30D3639 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S s_to_n: 60 fluxnum_1: 3 fluxnum_2: 6 fluxnum_3: 7 fluxnum_4: 8 priority: 1 param_1: BRIGHT=RETURN, param_2: LOCATE=YES req_1: CYCLE 2; req_2: ONBOARD ACQ FOR 6-14 comment_1: THIS STRATEGY ASSUMES THAT comment_2: THE EARLY ACQ IMAGES (LINES comment_3: 1-2) PROVED THAT THE CENTRAL comment_4: IS INDEED THE BRIGHTEST comment_5: IN THE SEARCH REGION. ! linenum: 6.000 targname: BD+30D3639 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 20.4S s_to_n: 60 fluxnum_1: 3 fluxnum_2: 6 fluxnum_3: 7 fluxnum_4: 8 priority: 1 req_1: CYCLE 2 ! linenum: 8.000 targname: BD+30D3639 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1224 num_exp: 3 time_per_exp: 20M s_to_n: 19 fluxnum_1: 2 priority: 1 param_1: FP-SPLIT=STD, param_2: STEP-PATT=DEF, param_3: COMB=FOUR req_1: CYCLE 2 comment_1: SPECTRAL FEATURES: comment_2: LY ALPHA, H2*, N V ! linenum: 9.000 targname: BD+30D3639 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1274 num_exp: 2 time_per_exp: 20M s_to_n: 22 fluxnum_1: 3 priority: 1 param_1: FP-SPLIT=STD, param_2: STEP-PATT=DEF, param_3: COMB=FOUR req_1: CYCLE 2 comment_1: SPECTRAL FEATURES: comment_2: C I, C I* ! linenum: 10.000 targname: BD+30D3639 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1304 num_exp: 1 time_per_exp: 30M s_to_n: 22 fluxnum_1: 3 priority: 1 param_1: FP-SPLIT=STD, param_2: STEP-PATT=DEF, param_3: COMB=FOUR req_1: CYCLE 2 comment_1: SPECTRAL FEATURES: comment_2: O I, O I*, SI II ! linenum: 11.000 targname: BD+30D3639 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1346 num_exp: 1 time_per_exp: 30M s_to_n: 22 fluxnum_1: 3 fluxnum_2: 4 priority: 1 param_1: FP-SPLIT=STD, param_2: STEP-PATT=DEF, param_3: COMB=FOUR req_1: CYCLE 2 comment_1: SPECTRAL FEATURES: comment_2: C II, O I INTERCOMB. ! linenum: 12.000 targname: BD+30D3639 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1463 num_exp: 1 time_per_exp: 30M s_to_n: 22 fluxnum_1: 4 fluxnum_2: 5 priority: 1 param_1: FP-SPLIT=STD, param_2: STEP-PATT=DEF, param_3: COMB=FOUR req_1: CYCLE 2 comment_1: SPECTRAL FEATURES: comment_2: CO 2-0, 3-0 ! linenum: 13.000 targname: BD+30D3639 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1510 num_exp: 1 time_per_exp: 30M s_to_n: 22 fluxnum_1: 4 fluxnum_2: 5 priority: 1 param_1: FP-SPLIT=STD, param_2: STEP-PATT=DEF, param_3: COMB=FOUR req_1: CYCLE 2 comment_1: SPECTRAL FEATURES: comment_2: CO 1-0 ! linenum: 14.000 targname: BD+30D3639 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1656 num_exp: 1 time_per_exp: 30M s_to_n: 22 fluxnum_1: 5 priority: 1 param_1: FP-SPLIT=STD, param_2: STEP-PATT=DEF, param_3: COMB=FOUR req_1: CYCLE 2 comment_1: SPECTRAL FEATURES: comment_2: C I, C I* ! linenum: 15.000 targname: IC418 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S s_to_n: 100 fluxnum_1: 3 fluxnum_2: 6 fluxnum_3: 8 fluxnum_4: 9 priority: 2 param_1: BRIGHT=RETURN, param_2: LOCATE=YES req_1: CYCLE 2; req_2: ONBOARD ACQ FOR 16-24 ! linenum: 16.000 targname: IC418 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 20.4S s_to_n: 100 fluxnum_1: 3 fluxnum_2: 6 fluxnum_3: 8 fluxnum_4: 9 priority: 2 req_1: CYCLE 2 ! linenum: 18.000 targname: IC418 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1224 num_exp: 1 time_per_exp: 20M s_to_n: 25 fluxnum_1: 2 priority: 2 param_1: FP-SPLIT=STD, param_2: STEP-PATT=DEF, param_3: COMB=FOUR req_1: CYCLE 2 ! linenum: 19.000 targname: IC418 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1274 num_exp: 1 time_per_exp: 10M s_to_n: 25 fluxnum_1: 3 priority: 2 param_1: FP-SPLIT=STD, param_2: STEP-PATT=DEF, param_3: COMB=FOUR req_1: CYCLE 2 ! linenum: 20.000 targname: IC418 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1304 num_exp: 1 time_per_exp: 10M s_to_n: 25 fluxnum_1: 3 priority: 2 param_1: FP-SPLIT=STD, param_2: STEP-PATT=DEF, param_3: COMB=FOUR req_1: CYCLE 2 ! linenum: 21.000 targname: IC418 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1346 num_exp: 1 time_per_exp: 10M s_to_n: 25 fluxnum_1: 4 priority: 2 param_1: FP-SPLIT=STD, param_2: STEP-PATT=DEF, param_3: COMB=FOUR req_1: CYCLE 2 ! linenum: 23.000 targname: IC418 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1510 num_exp: 1 time_per_exp: 10M s_to_n: 25 fluxnum_1: 4 fluxnum_2: 5 priority: 2 param_1: FP-SPLIT=STD, param_2: STEP-PATT=DEF, param_3: COMB=FOUR req_1: CYCLE 2 ! linenum: 24.000 targname: IC418 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1656 num_exp: 1 time_per_exp: 16M s_to_n: 25 fluxnum_1: 5 priority: 2 param_1: FP-SPLIT=STD, param_2: STEP-PATT=DEF, param_3: COMB=FOUR req_1: CYCLE 2 comment_5: POSITION IN THE SEARCH REGION. ! linenum: 25.000 targname: IC3568 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S s_to_n: 55 fluxnum_1: 3 fluxnum_2: 6 fluxnum_3: 7 fluxnum_4: 9 priority: 3 param_1: BRIGHT=RETURN, param_2: LOCATE=YES req_1: CYCLE 2; req_2: ONBOARD ACQ FOR 26-29 comment_1: THIS STRATEGY ASSUMES THAT comment_2: THE EARLY ACQ IMAGES (LINES comment_3: 3-4) PROVED THAT THE CENTRAL comment_4: IS INDEED THE BRIGHTEST ! linenum: 26.000 targname: IC3568 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 20.4S s_to_n: 55 fluxnum_1: 3 fluxnum_2: 6 fluxnum_3: 7 fluxnum_4: 9 priority: 3 req_1: CYCLE 2 ! linenum: 28.000 targname: IC3568 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1304 num_exp: 2 time_per_exp: 20M s_to_n: 18 fluxnum_1: 2 priority: 3 param_1: FP-SPLIT=STD, param_2: STEP-PATT=DEF, param_3: COMB=FOUR req_1: CYCLE 2 ! linenum: 29.000 targname: IC3568 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1346 num_exp: 2 time_per_exp: 20M s_to_n: 20 fluxnum_1: 2 fluxnum_2: 3 priority: 3 param_1: FP-SPLIT=STD, param_2: STEP-PATT=DEF, param_3: COMB=FOUR req_1: CYCLE 2 ! linenum: 30.000 targname: NGC40 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S s_to_n: 28 fluxnum_1: 3 fluxnum_2: 6 fluxnum_3: 7 fluxnum_4: 8 priority: 4 param_1: BRIGHT=RETURN, param_2: LOCATE=YES req_1: CYCLE 2; req_2: ONBOARD ACQ FOR 31-34 ! linenum: 31.000 targname: NGC40 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 20.4S s_to_n: 28 fluxnum_1: 3 fluxnum_2: 6 fluxnum_3: 7 fluxnum_4: 8 priority: 4 req_1: CYCLE 2 ! linenum: 33.000 targname: NGC40 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1304 num_exp: 1 time_per_exp: 30M s_to_n: 12 fluxnum_1: 2 fluxnum_2: 3 priority: 4 param_1: FP-SPLIT=STD, param_2: STEP-PATT=DEF, param_3: COMB=FOUR req_1: CYCLE 2 ! linenum: 34.000 targname: NGC40 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1346 num_exp: 1 time_per_exp: 30M s_to_n: 12 fluxnum_1: 2 fluxnum_2: 3 priority: 4 param_1: FP-SPLIT=STD, param_2: STEP-PATT=DEF, param_3: COMB=FOUR req_1: CYCLE 2 ! ! end of exposure logsheet ! No scan data records found