Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 3880c Report Date: 09-May-96:18:54 Version: ********** Check-in Date: ********** 1.Proposal Title: CIRCUMSTELLAR AND INTERSTELLAR ABSORPTION LINES IN PLANETARY NEBULA CENTRAL STARS ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID INTERSTELLAR MEDIUM GO Sub Category PLANETARY NEBULAE ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone Dr. Harriet L. Dinerstein UNIVERSITY OF TEXAS USA 512-471-3449 ASSOCIATE PROFESSOR ------------------------------------------------------------------------------------ 7. Abstract We propose to use GHRS observations of planetary nebula central stars to detect and study massive envelopes of residual neutral material around the ionized gas. Discovery of these envelopes has major implications for understanding the process that transforms a star from a red giant into a white dwarf. Previous radio and infrared work has shown that a signifi- cant fraction of planetaries (20 - 33%) contain 0.1-1 solar masses of molecules. Neutral atomic material, although harder to detect from the ground, may be even more common and contain substantial mass. This con- clusion is supported by the results of a pilot study by the proposers in the optical Na I lines. Observations of UV resonance lines of abundant species offer the most sensitive means for detecting neutral material, and will provide unique information on the physical and velocity structure of the nebular envelopes. The far -UV also offers the oppor- tunity to detect small amounts of vibrationally-excited H2. The GHRS is the only instrument that can provide sensitive measurements of these faint stars with high enough spectral resolving power to separate the nebular from interstellar absorption lines and to optimize detection of weak lines needed to determine accurate column densities. These obser- vations will also provide serendipitous information about the central stars and the ISM along new lines of sight through the galactic halo. ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 10.00 par: 0 10. Num targs pri: 4 par: 0 ------------------------------------------------------------------------------------ 11. Instruments requested: HRS FOC ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 3880c PI: Dr. Harriet L. Dinerstein Proposal Title: CIRCUMSTELLAR AND INTERSTELLAR ABSORPTION LINES IN PLANETARY NEBULA CENTRAL STARS ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ Pi Harriet L. Dinerstein UNIVERSITY OF TEXAS USA Christopher Sneden UNIVERSITY OF TEXAS USA Laura Danly SPACE TELESCOPE SCIENCE USA INSTITUTE Sara R. Heap GODDARD SPACE FLIGHT CENTER USA ------------------------------------------------------------------------------------ 2. Scientific Justification. Page 3 ------------------------------------------------------------------------------------ 3. Description of proposed observations. HRS OBSERVATIONS _ The primary goal of this proposed project is to study absorption lines produced by neutral circumnebular material around planetary nebulae, in order to study the properties of these neutral envelopes. We will use the UV continuum of the central star as a backdrop, against which the absorption lines will appear. All of the four targets in our modified observing plan have been observed by two of us at the Na D lines in the optical, and are seen to have a substantial envelope of such neutral material. Our plan is to observe them with the HRS at a number of wavelength settings that cover selected spectral features of interest. Originally we had hoped to observe the brighter targets with Echelle A; since this is no longer available, we will observe all of the targets with G160M. In order to preserve the best spectral resolving power, necessary to separate close features and to separate nebular absorptions from interstellar ones at nearby velocities, we are forced to use the Small Science Aperture. Unfortunately, this lengthens the exposure time needed to achieve good S/N. However, use of the SSA is also important in order to exclude nebular emission lines (including, possibly, some of the same lines that we see in absorption _ The observations now planned are summarized in the following table of integration times (in minutes): ________________________________________________________ Table 1. HRS Science Exposures (All SSA, G160M) ________________________________________________________ Setting Species BD+30 IC418 NGC40 IC3568 1224 HI,H2,NV 60 20 - - 1274 CI 40 10 - - 1304 OI, SiII 30 10 30 40 1346 CII, OI 30 10 30 40 1463 CO 2-0,3-0 30 - - - 1510 CO 1-0 30 10 - - 1656 CI 30 16 - - _ ________________________________________________________ S/N anticipated 22 25 12 18 1-sigma EW in mA 3 3 3 4 Total Int Time 250M 70M 60M 60M ________________________________________________________ _ The integration times were determined by choosing a value for the smallest equivalent width we wished to measure. We calculated the exposure times from formulae given in the GHRS Instrument Handbook, version 3.0. Example: GHRS Observation of BD+30 3639 with G160M at 1304A, 0.25 aperture: F(l) = 1.7e-12 from Feibelman et al. atlas. S(LSA), the sensitivity of G160M in the 2.0 aperture, is 6.74e11 (Table 4-13 in the Handbook). The throughput of the SSA is a factor of 4.5 smaller (Heap et al 1991, Ap.J. Lett., 377, L29), so S(SSA) = 1.5e11, and count rate c = F(l) x S(SSA) = 0.255/sec. Since neither scattered light nor dark count is significant, (S/N) squared = ct, where t is the integration time in seconds. In order to achieve a 1sigma error of 3.3 mA, so that an unresolved line of EW=10 mA is measured with 3sigma, we require S/N = 22 in a resolution element of .071A. Therefore, the needed integration time is t = (22)2/.255 sec = 31.6 min. We round this off to 30 minutes. _ FOC OBSERVATIONS FOR EARLY ACQUISITION OF HRS TARGETS _ Because of possible difficulties in acquiring two of the target planetary nebula central stars for spectroscopy, due to the relatively high surface brightness of the nebulae and low star/nebula contrast, we have added several FOC observations to our original program. The two objects in question are BD+30 3639 and IC 3568. These are both compact nebulae, BD+30 having a diameter of about 4", and IC 3568 of about 10". In the case of BD+30, VLA observations by Masson (Ap.J.346, 243 - 1989) show a ring with two relatively bright patches, empty in the middle, of about 4" in diameter. Observations of IC 3568 (Balick et al 1987, Astron.J.94, 948) show a larger region of emission, with perhaps a central "hole" or at least shallow depression. The IUE spectra of both of those objects are presented in the IUE Spectral Atlas of Planetary Nebulae, Central Stars, and Related Objects (Feibelman et al 1988, NASA Reference Publication 1203). Each shows continuum throughout the spectral region 1200-3200 A, and several emission lines. Some of the line emission may arise in the central star itself, but other lines, such as C III 1909, may also be present in the nebula. We therefore have decided to obtain FOC images in UV light, mimicking as closely as possible the spectral response of the HRS during acquistion, in order to decide whether there is a significant risk that the brightest point in the HRS search field might be a patch of nebulosity, rather than the central star. _____________________________________________________________ Table 2: FOC Exposures (F/96,512x512 for BD,512x1024 for IC) _____________________________________________________________ Target Filters Exposure Comment BD+30 F152M + F6ND 10M Stellar continuum only BD+30 F195W + F8ND 2M Continuum + Lines IC3568 F140M + F6ND 4M Stellar continnum only IC3568 F165W + F8ND 10M Continuum + Lines _____________________________________________________________ For each nebula, we selected 2 filters: one to isolate the stellar continuum as best as possible, and the other to include all of the strong emission lines seen in the IUE spectra. The optimum choices are different for the two cases. Also, because these are bright objects, it is necessary to insert neutral density filters, in order to keep the count rate below 5 counts/sec and avoid problems with non- linearity of response. The exposure times were chosen to yield a peak S/N ratio of about 25. Page 4 ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. The HRS on HST is needed to make further progress on this project because of its unique ability to obtain high- dispersion, high S/N ultraviolet spectra of faint stars. The PI and co-I Sneden have observed the target nebulae from the ground at Na I, 5889,95A, and detected nebular absorption features in all four of them. The strengths of these features range from weak (EW 20-40 mA) in IC3568 to very strong (EW=300 mA) in BD+30 3639, corresponding to equivalent H I column densities of 1e19 cm-2 for IC3568 to 1e21 cm-2 for BD+30. The optical spectral region contains few other useful absorption lines for studying the neutral material. Long integrations (>90min) have yielded detections of the Ca II 3933,63 lines and K I near 7600A for BD+30 only. The prime spectral region for resonance lines of abundant ions is the UV. _ In view of this, the PI carried out an archival study of the IUE high-dispersion spectra of these and other planetary nebula central stars, in hopes of detecting nebular absorption lines. One of the target nebulae, BD+30 3639, had already been studied by Pwa, Pottasch, and Mo (1986, Astr.Ap.164,184), who noted the nebular features. Most of the features they reported could arise either in the ionized or in the neutral region. Our proposed observations will provide higher S/N measurements, enabling us to decide, for example, whether certain weaker features such as OI 1304,1306, absorptions from excited fine-structure levels, and OI 1358 (an intercombination line), are present. We also hope to see CO in absorption (never reported before for BD+30, which has been detected in the CO millimeter emission lines). In general, the archival IUE spectra did not prove tremendously useful. They are limited by a relatively poor spectral resolution (25-30 km/sec) and limited dynamic range, which prevents high S/N measurements from being possible. ------------------------------------------------------------------------------------ 5. Description of special scheduling requirements. In our Phase 1 proposal, we pointed out the potential difficulties in acquiring the central stars of several of our targets, given that they are located on a a bright background, the UV emission of the nebulae. In particular, during HRS acquistion, the signal which is used to peak up on is the total brightness seen with the N2 mirror, therefore the total UV bandpass of 1200-3200 A. This bandpass contains a number of potentially bright emission lines. Using available information about the targets, their spatial structure as seen in the optical or radio maps, and their 1200-3200 A spectra as seen by IUE, we have attempted to estimate a worst-case scenario, where all of the line emission is concentrated into a small angular region. In that case, the HRS acquisition algorithm might possibly become confused and center on a patch of the nebula rather than on the central star. In order to avoid this awful occurrence, we are requesting permission to obtain UV images with the FOC for early acquistion purposes. We will examine these images in order to determine whether such confusion might occur. _ As described in question 3 above, we took the two targets for which this might be an issue, and selected two bandpasses for each. One bandpass is chosen to most closely mimic the way the nebula would look in "white" UV light, the other to best isolate the stellar continuum. The choices are different for each object because there IS no FOC filter covering 1200-3200 A; instead we try to include all substantial emission lines in the "star + nebula" filter, and to exclude them in the "star only" filter. ------------------------------------------------------------------------------------ 6. Description of special calibration exposures. Page 5 ------------------------------------------------------------------------------------ 7. Data reduction and analysis plans. Pipeline processing of the data by STScI will yield calibrated spectra in FITS format, that can be read into various data-analysis packages. The important quantities for this project, such as equivalent widths, do not require accurate absolute flux calibration, which would be difficult to achieve in any case with the SSA. We will determine EW's and wavelengths using IRAS/STDAS or a custom-made line-fitting program used at Texas (Fitzpatrick and Sneden 1987, BAAS, 19, 1129). Derivation of column densities from the measured equivalent widths is straightforward for weak, linear-regime and curve-of-growth techniques can be used for some stronger lines. In some cases, it may be useful to undertake multiple-component modelling of the line profiles. For example, data from Na I observations taken at higher dispersion on the ground, could be used to generate input velocities and column densities for fits to lower-resolution observations with G160M. Danly and Sneden have experience in these techniques. It also will be important to be aware of the roles of nebular emission lines and stellar spectral features. Dinerstein is an expert in emission line studies of planetary nebulae, and Heap is an expert in the study of the ultraviolet spectra of planetary nebulae and the properties of their central stars. ------------------------------------------------------------------------------------ 8. Additional comments or special requests. The targets are all listed as sources in the GSC. However, it will probably be possible to obtain more accurate coordinates, from Lick Observatory astrographic plate material. Therefore, although the GSC coordinates are expected to be adequate for acquiring the objects (apart from the considerations discussed in question 5), we hope to obtain improved coordinates early in the planning process (before May 1), with the kind assistance of colleagues at UC Santa Cruz. ------------------------------------------------------------------------------------ 9. Description of previous HST work. Dinerstein, Sneden: None. Danly: Program 2644, "The Environments of Starburst Galaxies," PI: Norman; Co-Is: Blades, Danly, and Heckman. Unrelated project. Heap: Program 1212: "Highly Evolved Stars of Low Mass". Somewhat, but not closely related; involves imagery and spectroscopy of 3 PN central stars, in NGC 7027, NGC 2440, and K648. These nebulae have very hot, faint central stars. There is no overlap with our target list. _ Heap: Images of NGC 2440 in several filters have been obtained. The central star is visible in all of them. Additional processing should yield a value for the temperature of the central star. ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). Most of the analysis will be carried out at UT Austin, which provides office space but not salaries for graduate research assistants. We will use computers and workstations shared by the astronomy department or by research subgroups of McDonald Observatory. We request funding for the following items which the University does not directly support for large projects: partial summer salary, research assistant salary, travel, publication expenses, long- distance telephone calls, data storage tapes, etc. ------------------------------------------------------------------------------------ 11. Address Information Name: HARRIET L. DINERSTEIN Category: PI Institution: UNIVERSITY OF TEXAS Address: ASTRONOMY DEPARTMENT RLM 15.308 UNIVERSITY OF TEXAS City: AUSTIN State: TX Zip Code: 78712 Country: USA Telephone: 512-471-3449 Telex (or e-mail): 910-874-1351 ------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 3880c [ 6] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial |Acqui|FLX| Flux data No | Name | Description | Position |Eqnx | Vel. |Prblm|REF| | | | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 1 BD+30D3639 A, 184, G, 502 RA = 19H 34M 45.326S +/- J2000 V = -68 BKG 1 V=9.9+/-0.2, TYPE=WC9 PK64+05D1 0.025S, 2 F-CONT(1200)=10+/-2E-13 HD184738 DEC = +30D 30' 58.59" +/- 3 F-CONT(1300)=17+/-2E-13 0.32" 4 F-CONT(1400)=22+/-2E-13 5 F-CONT(1600)=22+/-2E-13 6 F-CONT(1800)=22+/-2E-13 7 F-CONT(2500)=8+/-2E-13 8 F-LINE(1909)=6+/-1E-11 8 W-LINE(1909)=15+/-5 Comments: THE CENTRAL STAR IS A WOLF-RAYET STAR, 9 F-LINE(2300)=4+/-1E-11 WITH STRONG EMISSION LINES. SOME OF THE UV EMISSION LINES SEEN WITH IUE MAY ARISE IN THE STAR, BUT SOME, E.G. CIII 1909, PROBABLY ARISE IN THE NEBULA. ------------------------------------------------------------------------------------------------------------------------------------ 2 IC418 PK215- A, 184, G, 502 RA = 05H 27M 28.180S +/- 2000 V=+47 1 V=9.4 +/- 0.2, TYPE=O7F 24D1 HD35914 .014S, 2 F-CONT(1200)=60+/-10E-13 DEC = -12D 41' 50.12" +/- 3 F-CONT(1300)=105 +/- 15 E-13 0.2" 4 F-CONT(1400)=90 +/- 10 E-13 5 F-CONT(1600)=70 +/- 10 E-13 6 F-CONT(1800)=55 +/- 5 E-13 7 F-CONT(2200)=25 +/- 5 E-13 8 F-CONT(2800)=25 +/- 5 E-13 9 F-LINE(2320)=9 +/- 1 E-11 Comments: THE SPECTRUM RISES STRONGLY TOWARDS 9 W-LINE(2320)=20 +/- 5 SHORTER WAVELENGTHS. THE LYMAN ALPHA REGION HAS A DEEP ABSORPTION WHICH MAY BE PARTLY NEBULAR AND PARTLY INTERSTELLAR. AT LAMBDA > 2000 A, THE SPECTRUM IS FLAT EXCEPT FOR PROMINENT EMISSION LINES AT 2320 A (BLEND OF OIII, CII, AND SI II), AND 2800 A (MG II). ------------------------------------------------------------------------------------------------------------------------------------ 3 NGC40 A, 184, G, 502 RA = 00H 13M 00.907S +/- 2000 V = -55 1 V=11.8 +/- 0.2, TYPE=WC8 PK120+09D1 .066S, 2 F-CONT(1200)=5 +/- 1 E-13 HD826 DEC = +72D 31' 19.99" +/- 3 F-CONT(1400)=8 +/- 2 E-13 0.3" 4 F-CONT(1600)=5 +/- 2 E-13 5 F-CONT(2000)=20 +/- 5 E-14 6 F-CONT(2800)=20 +/- 5 E-14 7 F-LINE(1560)=24 +/- 4 E-12 7 W-LINE(1560)=15 +/- 5 8 F-LINE(2320)=9 +/- 1 E-11 Comments: THE UV SPECTRUM OF NGC 40 IS DOMINATED 8 W-LINE(2320)=20 +/- 5 BY THE LATE WC-TYPE CENTRAL STAR, WHICH HAS NUMEROUS STRONG EMISSION LINES. WE BELIEVE THAT MOST OF THE LINE EMISSION AS WELL AS CONTINUUM BELOW 2000 A IS DUE TO THE CENTRAL STAR. ------------------------------------------------------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 3880c [ 7] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial |Acqui|FLX| Flux data No | Name | Description | Position |Eqnx | Vel. |Prblm|REF| | | | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 4 IC3568 A, 184, G, 502 RA = 12H 33M 06.912S +/- 2000 V = -46 BKG 1 V=12.0 +/- 0.4, TYPE=O5 PK123+34 .15S, 2 F-CONT(1300)=11 +/- 1 E-13 HD109540 DEC = +82D 33' 50.22" +/- 3 F-CONT(1400)=10 +/- 1 E-13 0.3" 4 F-CONT(1600)=7 +/- 1 E-13 5 F-CONT(2000)=4 +/- 1 E-13 6 F-CONT(2500)=25 +/- 5 E-14 7 F-LINE(1240)=12 +/- 2 E-12 7 W-LINE(1240)=10 +/- 3 8 F-LINE(1550)=6 +/- 1 E-12 Comments: AGAIN, THIS OBJECT HAS A CENTRAL STAR 9 F-LINE(1909)=9 +/- 2 E-12 WITH A STRONG WIND. THE NV 1240A AND CIV 1550 LINES PROBABLY COME FROM THE CENTRAL STAR, IN VIEW OF THEIR P CYGNI PROFILES, BUT [C III] 1909, WHICH DOES NOT HAVE A P CYGNI PROFILE, PROBABLY ARISES IN THE NEBULA. ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 3880c [ 8] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 1 BD+30D3639 FOC/96 IMAGE 512X512 F152M, 1 10M 25 4 1 CYCLE 2 F6ND 5 EARLY ACQ FOR 5-14 GROUP 1-2 NON-INT Comments: TO INSURE ACCURATE SPATIAL REGISTRATION OF LINE AND CONTINUUM IMAGES ------------------------------------------------------------------------------------------------------------------------------------ 2 BD+30D3639 FOC/96 IMAGE 512X512 F195W, 1 2M 25 5 1 CYCLE 2 F8ND 7 EARLY ACQ FOR 5-14 8 9 ------------------------------------------------------------------------------------------------------------------------------------ 3 IC3568 FOC/96 IMAGE 512X102 F140M, PIXEL=50X25 1 4M 25 2 2 CYCLE 2 4 F6ND 3 EARLY ACQ FOR 26- 4 29 GROUP 3-4 NON-INT Comments: TO INSURE REGISTRATION ------------------------------------------------------------------------------------------------------------------------------------ 4 IC3568 FOC/96 IMAGE 512X102 F165W, PIXEL=50X25 1 10M 25 2 2 CYCLE 2 4 F8ND 5 EARLY ACQ FOR 26- 8 29 9 ------------------------------------------------------------------------------------------------------------------------------------ 5 BD+30D3639 HRS ACQ 2.0 MIRROR-N2 BRIGHT=RETURN 1 1.8S 60 3 1 CYCLE 2 LOCATE=YES 6 ONBOARD ACQ FOR 6- 7 14 8 Comments: THIS STRATEGY ASSUMES THAT THE EARLY ACQ IMAGES (LINES 1-2) PROVED THAT THE CENTRAL IS INDEED THE BRIGHTEST IN THE SEARCH REGION. ------------------------------------------------------------------------------------------------------------------------------------ 6 BD+30D3639 HRS ACQ/ 2.0 MIRROR-N2 1 20.4S 60 3 1 CYCLE 2 PEAKUP 6 7 8 ------------------------------------------------------------------------------------------------------------------------------------ 8 BD+30D3639 HRS ACCUM 0.25 G160M 1224 FP-SPLIT=STD 3 20M 19 2 1 CYCLE 2 STEP-PATT=DEF COMB=FOUR Comments: SPECTRAL FEATURES: LY ALPHA, H2*, N V ------------------------------------------------------------------------------------------------------------------------------------ 9 BD+30D3639 HRS ACCUM 0.25 G160M 1274 FP-SPLIT=STD 2 20M 22 3 1 CYCLE 2 STEP-PATT=DEF COMB=FOUR Comments: SPECTRAL FEATURES: C I, C I* ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 3880c [ 9] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 10 BD+30D3639 HRS ACCUM 0.25 G160M 1304 FP-SPLIT=STD 1 30M 22 3 1 CYCLE 2 STEP-PATT=DEF COMB=FOUR Comments: SPECTRAL FEATURES: O I, O I*, SI II ------------------------------------------------------------------------------------------------------------------------------------ 11 BD+30D3639 HRS ACCUM 0.25 G160M 1346 FP-SPLIT=STD 1 30M 22 3 1 CYCLE 2 STEP-PATT=DEF 4 COMB=FOUR Comments: SPECTRAL FEATURES: C II, O I INTERCOMB. ------------------------------------------------------------------------------------------------------------------------------------ 12 BD+30D3639 HRS ACCUM 0.25 G160M 1463 FP-SPLIT=STD 1 30M 22 4 1 CYCLE 2 STEP-PATT=DEF 5 COMB=FOUR Comments: SPECTRAL FEATURES: CO 2-0, 3-0 ------------------------------------------------------------------------------------------------------------------------------------ 13 BD+30D3639 HRS ACCUM 0.25 G160M 1510 FP-SPLIT=STD 1 30M 22 4 1 CYCLE 2 STEP-PATT=DEF 5 COMB=FOUR Comments: SPECTRAL FEATURES: CO 1-0 ------------------------------------------------------------------------------------------------------------------------------------ 14 BD+30D3639 HRS ACCUM 0.25 G160M 1656 FP-SPLIT=STD 1 30M 22 5 1 CYCLE 2 STEP-PATT=DEF COMB=FOUR Comments: SPECTRAL FEATURES: C I, C I* ------------------------------------------------------------------------------------------------------------------------------------ 15 IC418 HRS ACQ 2.0 MIRROR-N2 BRIGHT=RETURN 1 1.8S 100 3 2 CYCLE 2 LOCATE=YES 6 ONBOARD ACQ FOR 16 8 -24 9 ------------------------------------------------------------------------------------------------------------------------------------ 16 IC418 HRS ACQ/ 2.0 MIRROR-N2 1 20.4S 100 3 2 CYCLE 2 PEAKUP 6 8 9 ------------------------------------------------------------------------------------------------------------------------------------ 18 IC418 HRS ACCUM 0.25 G160M 1224 FP-SPLIT=STD 1 20M 25 2 2 CYCLE 2 STEP-PATT=DEF COMB=FOUR ------------------------------------------------------------------------------------------------------------------------------------ 19 IC418 HRS ACCUM 0.25 G160M 1274 FP-SPLIT=STD 1 10M 25 3 2 CYCLE 2 STEP-PATT=DEF COMB=FOUR ------------------------------------------------------------------------------------------------------------------------------------ 20 IC418 HRS ACCUM 0.25 G160M 1304 FP-SPLIT=STD 1 10M 25 3 2 CYCLE 2 STEP-PATT=DEF COMB=FOUR ------------------------------------------------------------------------------------------------------------------------------------ 21 IC418 HRS ACCUM 0.25 G160M 1346 FP-SPLIT=STD 1 10M 25 4 2 CYCLE 2 STEP-PATT=DEF COMB=FOUR ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 3880c [ 10] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 23 IC418 HRS ACCUM 0.25 G160M 1510 FP-SPLIT=STD 1 10M 25 4 2 CYCLE 2 STEP-PATT=DEF 5 COMB=FOUR ------------------------------------------------------------------------------------------------------------------------------------ 24 IC418 HRS ACCUM 0.25 G160M 1656 FP-SPLIT=STD 1 16M 25 5 2 CYCLE 2 STEP-PATT=DEF COMB=FOUR Comments: POSITION IN THE SEARCH REGION. ------------------------------------------------------------------------------------------------------------------------------------ 25 IC3568 HRS ACQ 2.0 MIRROR-N2 BRIGHT=RETURN 1 1.8S 55 3 3 CYCLE 2 LOCATE=YES 6 ONBOARD ACQ FOR 26 7 -29 9 Comments: THIS STRATEGY ASSUMES THAT THE EARLY ACQ IMAGES (LINES 3-4) PROVED THAT THE CENTRAL IS INDEED THE BRIGHTEST ------------------------------------------------------------------------------------------------------------------------------------ 26 IC3568 HRS ACQ/ 2.0 MIRROR-N2 1 20.4S 55 3 3 CYCLE 2 PEAKUP 6 7 9 ------------------------------------------------------------------------------------------------------------------------------------ 28 IC3568 HRS ACCUM 0.25 G160M 1304 FP-SPLIT=STD 2 20M 18 2 3 CYCLE 2 STEP-PATT=DEF COMB=FOUR ------------------------------------------------------------------------------------------------------------------------------------ 29 IC3568 HRS ACCUM 0.25 G160M 1346 FP-SPLIT=STD 2 20M 20 2 3 CYCLE 2 STEP-PATT=DEF 3 COMB=FOUR ------------------------------------------------------------------------------------------------------------------------------------ 30 NGC40 HRS ACQ 2.0 MIRROR-N2 BRIGHT=RETURN 1 1.8S 28 3 4 CYCLE 2 LOCATE=YES 6 ONBOARD ACQ FOR 31 7 -34 8 ------------------------------------------------------------------------------------------------------------------------------------ 31 NGC40 HRS ACQ/ 2.0 MIRROR-N2 1 20.4S 28 3 4 CYCLE 2 PEAKUP 6 7 8 ------------------------------------------------------------------------------------------------------------------------------------ 33 NGC40 HRS ACCUM 0.25 G160M 1304 FP-SPLIT=STD 1 30M 12 2 4 CYCLE 2 STEP-PATT=DEF 3 COMB=FOUR ------------------------------------------------------------------------------------------------------------------------------------ 34 NGC40 HRS ACCUM 0.25 G160M 1346 FP-SPLIT=STD 1 30M 12 2 4 CYCLE 2 STEP-PATT=DEF 3 COMB=FOUR ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 3880c [ 11] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations FOC/96 HRS ------------------------------------------------------------------------------------------------------------------------------------ Opmodes IMAGE ACQ ACQ/PEAKUP ACCUM ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters PIXEL=50X25 BRIGHT=RETURN LOCATE=YES FP-SPLIT=STD STEP-PATT=DEF COMB=FOUR ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 10.00 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category INTERSTELLAR MEDIUM ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category PLANETARY NEBULAE ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements CYCLE 2; EARLY ACQ FOR 5-14; GROUP 1-2 NON-INT EARLY ACQ FOR 5-14 EARLY ACQ FOR 26-29; GROUP 3-4 NON-INT EARLY ACQ FOR 26-29 ONBOARD ACQ FOR 6-14 CYCLE 2 ONBOARD ACQ FOR 16-24 ONBOARD ACQ FOR 26-29 ONBOARD ACQ FOR 31-34 ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements F152M, F6ND F195W, F8ND F140M, F6ND F165W, F8ND MIRROR-N2 G160M ------------------------------------------------------------------------------------------------------------------------------------ Target Names BD+30D3639 PK64+05D1 HD184738 IC418 PK215-24D1 HD35914 NGC40 PK120+09D1 HD826 IC3568 PK123+34 HD109540 ------------------------------------------------------------------------------------------------------------------------------------