Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 5323 Report Date: 18-Jul-95:17:09 Version: ********** Check-in Date: ********** 1.Proposal Title: ATMOSPHERIC DYNAMICS AND MASS LOSS IN GAPPERS, CLUMPERS, AND HYBRIDS CYC4 - MEDIUM ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID COOL STARS GO Sub Category ATMOSPHERES & WINDS ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone Thomas R. Ayres 1762 USA 303-492-4051 RESEARCH PROFESSOR ------------------------------------------------------------------------------------ 7. Abstract The giant branch evolution of moderate-mass stars provides a vital test of our understanding of magnetic dynamo action, coronal energization, and winds. The blatant``X-ray deficiency'' of the Hertzsprung-gap giants appears to be genuine, while that of many ``hybrid-chromosphere'' supergiants appears to be due to absorption by a previously unrecognized warm or hot component of their winds; not apparent in the Mg II circumstellar features but quite evident in the H I Lyman- alpha profile (of at least one case). There also is new evidence for a warm wind on the G0 secondary of Capella -- a ``gap'' star. The mass-loss rate is low, but dynamically quite significant in braking the fast stellar rotation. Outflows of some kind probably exist on post-helium-flash Clump giants, as well, although ``antiwinds'' are the hallmark of the archetype, Beta Ceti. I propose to clarify the subcoronal properties of the Hertzsprung-gap, active Clump, and Hybrid stars through a spectral dissection of one representative of each class. My strategy is to use the HST/GHRS to record key FUV emissions -- spanning the broad temperature range 10,000-250,000 K -- with high S/N to measure line widths, profile asymmetries, circumstellar absorptions, systematic Doppler shifts, and density-sensitive line ratios. Such diagnostics will be used to constrain existing physical models, and develop new ones. The HST spectra will strongly complement ongoing X-ray work with ROSAT and recent EUVE spectroscopy. ------------------------------------------------------------------------------------ 8. Scientific Key Words: STAR, G III-I, K III-I, CORONA, WIND ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 10.48 par: 0 10. Num targs pri: 3 par: 0 ------------------------------------------------------------------------------------ 11. Instruments requested: HRS ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 5323 PI: Thomas R. Ayres Proposal Title: ATMOSPHERIC DYNAMICS AND MASS LOSS IN GAPPERS, CLUMPERS, AND HYBRIDS CYC4 - MEDIUM ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ Dr. Thomas Ayres COLORADO, UNIVERSITY OF USA ------------------------------------------------------------------------------------ 3. Description of proposed observations. The observational objective is to acquire selected important spectral diagnostics of the dynamical and structural properties of the sub- coronal layers and winds of three pivotal giants either in or near the Hertzsprung gap, or in the post-helium-flash Clump. As a side benefit, the chromospheric H I & Mg II emissions contain ISM components that probe local sightlines. The observation plan, in order of priority, is as follows: ========================================================================== setting/aper wavelengths purpose ------------------------------- ------------------------------------------- (1) G160M/LSA 1205-1240 moderate S/N profiles of key emission-measure (1') -- /SSA -- species O V] 1218 (250,000 K) and N V 1238 (200,000 K); high S/N profiles of strong chromo- spheric feature H I 1215 (<20,000 K) and Si III 1206 (30,000 K). Use short exposure with SSA to suppress geocoronal H I in extreme core of stellar H I emission profile; use deeper exp- osure through LSA to obtain moderate (>20:1 at peak) S/N profiles of fainter emissions. (2) G160M/LSA 1386-1420 high S/N profiles of Si IV 1393,1402; detections of density-sensitive O IV] 1401,04,07 multiplet (3) G160M/LSA 1538-1572 high S/N profiles of key emission-measure spec- ies C IV 1548,50 (100,000 K); detect possible warm wind absorption features. (4)ECH- B20/SSA 2791-2805 very high S/N profiles of key chromospheric emissions Mg II 2795,802. SSA for best resol- ution of LISM and/or circumstellar components. --- ---------------------------------------------------------------------- I intend to obtain sufficient S/N to record not only the line fluxes but also the profile shapes and any systematic Doppler shifts of the high- excitation species. The profile widths indicate the amplitudes of non- thermal Doppler motions in the 30,000-250,000 K layers of the transition zone, which play a crucial role in theories of the subcoronal energy balance. Any systematic line shifts could be related to large-scale bulk flows of material, like the redshifts (antiwinds) of Si IV-C IV tempera- ture gas routinely observed in coronal stars of all luminosity classes, and thought to be connected with the TZ downdrafts seen in coronal mag- netic loops on the Sun. Finally, the high resolution (20,000) and high S/N (>30) obtainable on the Si IV 1393 and C IV 1548 features might permit the detection of blue-shifted absorptions due to warm winds. Page 3 ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. The object of the program is to study the subcoronal properties of pivotal stars selected from X-ray/C IV correlation diagrams. The appropriate diagnostics (of 30,000-200,000 K gas) are high-excitation emissions of the FUV region: the dramatic differences between the various groups seen in their behavior of C IV vis-a-vis X-rays is not mirrored in the Ca II or H-alpha lines, for example. All three of the target stars have been studied extensively with the IUE in its low- resolution (5 A) mode. Thirty-one Comae has been attempted once, Beta Ceti twice, and Alpha TrA several times in the R=10,000 FUV echelle mode of IUE. However, the resulting spectra -- the deepest pos- sible with IUE -- are of marginal value (C IV faint; Lyman alpha severely contaminated by overexposed geocoronal emission; O IV] well below sensi- tivity threshholds). Indeed, the key O IV] features have been seen by IUE (faintly) in only two `normal' late-type stars: Alpha Aurigae Ab (G0 III) and Beta Draconis (G2 Ib), both of which are significantly brighter FUV sources than the three giants proposed here. (Incident- ally, Capella itself is not a suitable target for the present purpose because the FUV emissions from the two stars -- one an active Clump giant, the other a Hertzsprung-gap giant -- are blended at all orbital phases, and difficult to unambiguously separate.) By virtue of the RIASS program, the three targets have been studied in detail based on ROSAT survey material: 31 Com and Beta Cet were strong detections by the PSPC, both having sufficient counts for a crude det - ermination of the coronal temperature; and both class-III giants were seen by the WFC in its S2 filter. Indeed, I am PI of an EUVE spectro- scopy program to record both giants: observations of 31 Com already were obtained in February 1993. Alpha TrA was a relatively weak PSPC detect- ion in the RASS, but was the subject of a deep ROSAT pointing by R. Ros- ner and collaborators. Unfortunately, Alpha TrA is too absorbed in the 100-300 A region to provide a useable EUVE spectrum. My colleague J. Linsky (JILA) has obtained GHRS/GTO observations of selected FUV emissions, and the Mg II h & k lines, in Alpha TrA very recently. However, owing to lack of observing time, he dropped ob- servations of the 1205-1240 A region because -- at the time the Phase II plan was prepared -- Lyman-alpha was believed to be uninteresting. However, the very recent recognition of anomalous blueward absorption in IUE profiles of Lyman- alpha has elevated that interval to one of crucial importance. Thus I propose here to obtain a spectrum of the vital 1205-1240 A region, but will not duplicate the other FUV set- tings already acquired by Linsky. A brief exposure of Mg II h & k at echelle resolution is warranted, however, because the profiles are known to be variable. Thus, the proposed HST investigation builds upon a strong base of pre- vious and current work, which however has reached the limitations of the historical FUV instrumentation. Only the HST/GHRS can provide the new high S/N, high spectral resolution material required to make further progress in understanding the wide diversity in the coronal/subcoronal properties of stars in the moderate-mass sector of the giant branch. I obtained FUV emission fluxes for the three proposed targets from coadded IUE SWP-LO spectra, and additional values for H I Lyman-alpha from a recent survey of high-resolution profiles by myself and collaborators. I estimated line widths by reference to existing (weak) SWP- HI spectra of the the C IV emissions of the program stars. The table below provides a summary of the typical peak flux values, proposed exposure times, and expected S/N ratios. ===================================================================== prio.| exp. 1 & 1' | exp. 2 | exp. 3 | exp. 4 | ---------------------- ----------------------------------------------- | Si III H I N V | Si IV O IV] | C IV | Mg II | | 1206 1215 1238 | 1393 1401 | 1548 | 2795 | ===================================================================== -- 31 Comae (G0 III) -- --------------------------------------------------------------------- Flux | 8: 60 3 | 7 0.5: | 16 | 90 | ---------- ----------------------------------------------------------- texp | 65M LSA + 10M SSA | 70M LSA | 30M LSA | 25M SSA | -------------------------------- ------------------------------------- S/N | 30 40/ssb 20 | 40 10: | 35 | 50/ssb | ===================================================================== -- Beta Ceti (K0 III) -- ---------------------------------------------------------------- ----- Flux | 15: 120 11 | 12 1: | 8 | 500 | ---- ----------------------------------------------------------------- texp | 30M LSA + 5M SSA | 45M LSA | 40M LSA | 5M SSA | ------------------------ --------------------------------------------- S/N | 30 40/ssb 25 | 40 10: | 30 | 50/ssb | ===================================================================== -- Alpha Trianguli Australis (K2 II-III) -- ---------------------------------------------- ----------------------- Flux | 8: 80 5 | -- | -- | 700 | ------------------------------------------------------------------- -- texp | 65M LSA + 10M SSA | -- | -- | 5M SSA | ------- -------------------------------------------------------------- S/N | 30 50/ssb 25 | -- | -- | 60/ssb | ===================================================================== Notes: Fluxes in units of 1E-13 ergs/cm^2/s/A at Earth at line peak; S/N is either per resolution element (i.e., 1 diode), after smoothing over substep pattern, or per substep bin (ssb). For a well-resolved line (FWHM >> 1 diode), the S/N of the integrated flux is about twice the peak S/N (per diode), thus a peak S/N of 10 ensures an accuracy in the line flux of about 5%. For the density-sensitive O IV] lines, a 5% uncertainty in the flux ratio translates into a (very small) 15% uncertainty in the electron density over the range log N= 8.5-10.5 where the O IV] diagnostic is useful (and where the densities of the sub- coronal layers of evolved stars are thought to lie). In addition, a peak S/N of 10 or more will yield an accuracy in the emission centroid of about a tenth of a diode or better, or about 1.5 km/s for G160M. This is compar- able to the precision of the GHRS wavelength scales that can be achieved for a well-centered image in the LSA, with an accompanying lamp spectrum. Page 4 ------------------------------------------------------------------------------------ 5. Description of special scheduling requirements. Assurance of the precision of the wavelength scales of the medium-resolution and high-resolution spectra is essential to the scientific objectives of our program. Thus we propose to obtain wavelength calibrations for the G160M and ECH-B20 settings. The lamp exposures should be of order 60S or longer, to obtain the requisite accuracy in the assigned wavelength scales. ------------------------------------------------------------------------------------ 6. Description of special calibration exposures. OSF Line Number(s) Instrument Mode Special Calibration Requirement(s) ___________________ __________ _______ __________________________________ 1.0 -- 3.3 GHRS ACCUM Lamp exposures to ensure precis- ion of wavelength scales for G160M & ECH-B20 spectra. Should achieve S/N= 10, or better, in moderate-strength Pt II emissions ------------------------------------------------------------------------------------ 9. Description of previous HST work. P2485: ``Sleuthing the Dynamo: Cycle 1 Observations'' [peripherly related to present project] P3908: ``Sleuthing the Dynamo: Cycle 2 Observations'' [peripherly related to present project] P4492: ``The Distant Future of Solar Activity: Cycle 3 Observations'' [peripherly related to present project] P2485: all five targets observed fall `92; P3908: four of five targets observed fall `92. Spectra currently are being reduced and analyzed. P2485 targets were weaker than expected at C IV 1549; but P3908 targets were brighter, and one of the Pleiades G stars flared during one of the three orbits of observation with the FOS. The main results of the program will be presented at the summer `93 meeting of the AAS in Berkeley, and at the 8th Cambridge Workshop in the fall. P4492: No observations to date. ``GHRS observations of the local interstellar medium and the deuterium/hydrogen ratio along the line of sight towards Capella,'' Linsky, J. L., Brown, A., Gayley, K. G., Diplas, A., Savage, B. D., Ayres, T. R., Landsman, W., Shore, S., & Heap, S. R., Astrophysical Journal, 402, 694, (1993). ``The hydrogen Lyman alpha emission of Capella'', Ayres, T. R., Brown, A., Gayley, K. G., & Linsky, J. L., Astrophysical Journal, 402, 710, (1993). ``IUE far-ultraviolet spectra of Capella and Gamma Draconis for comparison to HST/GHRS GTO observations'', Ayres, T. R., in The First Year of HST Observat- ions, ed. A. L. Kinney and J. C. Blades (Baltimore: Space Telescope Science Institute), p. 216 (1991). ``A Remarkable FUV Flare on the Pleiades G Dwarf HZ 314'', Ayres,T., Basri, G., Simon, T., Stauffer, J., Stern, R., Antiochos, S., Bookbinder, J., Brown, A., Doschek, G., Linsky, J., Ramsey, L., & Walter, F., in Bull. Am. Astron. Soc. (in press, 1993). ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). At the University of Colorado a version of the reduction software writ- ten by the GHRS team is available on a variety of platforms; as is IRAF/SDAS. We expect to conduct theoretical studies of the UV and X-ray emissions from stellar atmospheres using fast numerical simulat- ion codes recently implemented on high- performance workstations. These codes were developed originally for use with IUE and ROSAT/WFC data, and modified more recently for EUVE spectroscopy. Their appli- cation to the HST data is straightforward. There are a number of un- dergraduate and graduate students working on HST data, who potentially could contribute significantly to (and benefit intellectually from) the Sleuthing continuation. The University provides substantial help in the form of matching funds for hardware purchases and FTE funding for some of the computer system support staff and other essential administrative positions. ------------------------------------------------------------------------------------ 11. Address Information Page 5 Name: THOMAS R. AYRES Category: PI Institution: 1762 Address: CNTR. ASTROPHYS. & SPACE ASTRON. CAMPUS BOX 389 (CASA) City: BOULDER State: CO Zip Code: 80309 Country: USA Telephone: 303-492-4051 Telex (or e-mail): (SPAN) HYADES::AYRES ------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 5323 [ 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 HD111812 31- A, 138, 901, 905 RA = 12H 51M 41.84S +/- 2000 V=-1 1 V = 4.94 +/- 0.10, TYPE = G0III COM 0.03S, 2 B-V = +0.67 +/- 0.01 DEC = +27D 32' 26.3" +/- 3 F-LINE(1215)= 60 +/- 10 E-13 0.1" 4 W-LINE(1215)= 3 +/- 1 5 F-LINE(2795)= 90 +/- 10 E-13 6 W-LINE(2795)= 3 +/- 1 7 F-LINE(1393)= 7 +/- 1 E-13 8 W-LINE(1393)= 1 +/- 0.3 9 F-LINE(1548)= 16 +/- 3 E-13 10 W-LINE(1548)= 1 +/- 0.3 Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec) J 2000.00 -0.0010 +/- 0.0000 -0.0130 +/- 0.0000 0.0110 +/- 0.0070 ------------------------------------------------------------------------------------------------------------------------------------ 2 HD4128 BETA- A, 140, 901, 905 RA = 0H 43M 35.30S +/- 2000 V=+13 1 V = 2.04 +/- 0.10, TYPE = K0III CET 0.03S, 2 B-V = +1.02 +/- 0.01 DEC = -17D 59' 12.0" +/- 3 F-LINE(1215)= 120 +/- 20 E-13 0.1" 4 W-LINE(1215)= 2 +/- 1 5 F-LINE(2795)= 500 +/- 100 E-13 6 W-LINE(2795)= 2 +/- 1 7 F-LINE(1393)= 12 +/- 3 E-13 8 W-LINE(1393)= 1 +/- 0.3 9 F-LINE(1548)= 8 +/- 2 E-13 10 W-LINE(1548)= 1 +/- 0.3 Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec) J 2000.00 0.0163 +/- 0.0000 0.0360 +/- 0.0000 0.0610 +/- 0.0070 ------------------------------------------------------------------------------------------------------------------------------------ 3 HD150798 A, 140, 901, 905 RA = 16H 48M 39.89S +/- 2000 V=-3 1 V = 1.92 +/- 0.10, TYPE = K2II ALPHA-TRA 0.03S, 2 B-V = +1.44 +/- 0.01 DEC = -69D 1' 39.5" +/- 0.1" 3 F-LINE(1215)= 80 +/- 10 E-13 4 W-LINE(1215)= 3 +/- 1 5 F-LINE(2795)= 700 +/- 100 E-13 6 W-LINE(2795)= 3 +/- 1 Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec) J 2000.00 0.0052 +/- 0.0000 -0.0340 +/- 0.0000 0.0310 +/- 0.0070 ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5323 [ 7] ------------------------------------------------------------------------------------------------------------------------------------ 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 ------------------------------------------------------------------------------------------------------------------------------------ 2 DEFINE WAVE HRS ACCUM SC2 ECH-B20 2798 STEP-PATT=3 1 32S 30 1 CALIB FOR 2.1 MAG DOPPLER=OFF 30S SEQ 2-2.1 NO GAP ------------------------------------------------------------------------------------------------------------------------------------ 2.1 DEFINE # ^ ^ 0.25 ^ ^ STEP-PATT=7 1 326.4S # 5 ^ MAG FP-SPLIT=STD # 6 DOPPLER=ON ------------------------------------------------------------------------------------------------------------------------------------ 2.5 DEFINE WAVE HRS ACCUM SC2 ECH-B20 2798 STEP-PATT=3 1 32S 30 1 CALIB FOR 2.6 MAG1 DOPPLER=OFF 30S SEQ 2.5-2.6 NO GAP ------------------------------------------------------------------------------------------------------------------------------------ 2.6 DEFINE # ^ ^ 0.25 ^ ^ STEP-PATT=7 1 1305.6S # 5 ^ MAG1 FP-SPLIT=STD # 6 DOPPLER=ON ------------------------------------------------------------------------------------------------------------------------------------ 3 DEFINE WAVE HRS ACCUM SC2 G160M 1223 STEP-PATT=3 1 64S 30 1 CALIB FOR 3.1 LYA1 DOPPLER=OFF 30S SEQ 3-3.1 NO GAP ------------------------------------------------------------------------------------------------------------------------------------ 3.1 DEFINE # HRS ACCUM 0.25 G160M 1223 STEP-PATT=5 1 326.4S # 3 3 LYA1 FP-SPLIT=STD # 4 DOPPLER=ON ------------------------------------------------------------------------------------------------------------------------------------ 3.5 DEFINE WAVE HRS ACCUM SC2 G160M 1223 STEP-PATT=3 1 64S 30 1 CALIB FOR 3.6 LYA11 DOPPLER=OFF 30S SEQ 3.5-3.6 NO GAP ------------------------------------------------------------------------------------------------------------------------------------ 3.6 DEFINE # HRS ACCUM 0.25 G160M 1223 STEP-PATT=5 1 652.8S # 3 3 LYA11 FP-SPLIT=STD # 4 DOPPLER=ON ------------------------------------------------------------------------------------------------------------------------------------ 3.8 DEFINE # HRS ACCUM 2.0 G160M 1223 STEP-PATT=5 # 1523.2S # 3 1 LYA2 FP-SPLIT=STD # 4 DOPPLER=ON ------------------------------------------------------------------------------------------------------------------------------------ 4 DEFINE WAVE HRS ACCUM SC2 G160M 1403 STEP-PATT=3 1 64S 30 1 CALIB FOR 4.1 SILI DOPPLER=OFF 30S SEQ 4-4.1 NO GAP ------------------------------------------------------------------------------------------------------------------------------------ 4.1 DEFINE # ^ ^ 2.0 ^ ^ STEP-PATT=5 # 1305.6S # 7 ^ SILI FP-SPLIT=STD # 8 DOPPLER=ON ------------------------------------------------------------------------------------------------------------------------------------ 5 DEFINE WAVE HRS ACCUM SC2 G160M 1555 STEP-PATT=3 1 64S 30 2 CALIB FOR 5.1 CARB DOPPLER=OFF 30S SEQ 5-5.1 NO GAP ------------------------------------------------------------------------------------------------------------------------------------ 5.1 DEFINE # ^ ^ 2.0 ^ ^ STEP-PATT=5 1 1305.6S # 9 ^ CARB FP-SPLIT=STD # 10 DOPPLER=ON ------------------------------------------------------------------------------------------------------------------------------------ 10 HD111812 HRS ACQ 2.0 MIRROR-A2 SEARCH-SIZE=3 1 45S 70 1 1 ONBOARD ACQ FOR BRIGHT=RETURN 6S 2 10.1 CYCLE 4 / 10-10.7 SEQ 10-10.7 NO GAP Comments: STEP TIME = 5 SEC ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5323 [ 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 ------------------------------------------------------------------------------------------------------------------------------------ 10.1 ^ HRS ACQ/ 0.25 MIRROR-A2 SEARCH-SIZE=5 1 125S 70 1 1 ONBOARD ACQ FOR PEAKUP 6S 2 10.2-10.7 Comments: STEP-TIME=5 SEC ------------------------------------------------------------------------------------------------------------------------------------ 10.2 USE ^ 50 MAG1 25M ------------------------------------------------------------------------------------------------------------------------------------ 10.3 USE ^ 40 LYA11 70M ------------------------------------------------------------------------------------------------------------------------------------ 10.5 USE ^ 2 40 LYA2 70M ------------------------------------------------------------------------------------------------------------------------------------ 10.6 USE ^ 3 40 SILI 70M ------------------------------------------------------------------------------------------------------------------------------------ 10.7 USE HD111812 30 CARB 30M ------------------------------------------------------------------------------------------------------------------------------------ 11 HD4128 HRS ACQ 2.0 MIRROR-A2 SEARCH-SIZE=3 1 22.5S 70 1 1 ONBOARD ACQ FOR BRIGHT=RETURN 2.5S 2 11.1 CYCLE 4 / 11-11.7 SEQ 11-11.7 NO GAP Comments: STEP TIME = 2.5 SEC ------------------------------------------------------------------------------------------------------------------------------------ 11.1 ^ HRS ACQ/ 0.25 MIRROR-A2 SEARCH-SIZE=5 1 62.5S 70 1 1 ONBOARD ACQ FOR PEAKUP 2.5S 2 11.2-11.7 Comments: STEP-TIME=2.5 SEC ------------------------------------------------------------------------------------------------------------------------------------ 11.2 USE MAG ^ 50 5M ------------------------------------------------------------------------------------------------------------------------------------ 11.3 USE ^ 40 LYA1 35M ------------------------------------------------------------------------------------------------------------------------------------ 11.5 USE ^ 1 40 LYA2 35M ------------------------------------------------------------------------------------------------------------------------------------ 11.6 USE ^ 2 40 SILI 45M ------------------------------------------------------------------------------------------------------------------------------------ 11.7 USE ^ 30 CARB 40M ------------------------------------------------------------------------------------------------------------------------------------ 12 HD150798 HRS ACQ 2.0 MIRROR-A2 SEARCH-SIZE=3 1 90S 70 1 1 ONBOARD ACQ FOR BRIGHT=RETURN 12.5S 2 12.1 CYCLE 4 / 12-12.5 SEQ 12-12.5 NO GAP Comments: STEP TIME = 10 SEC ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5323 [ 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 ------------------------------------------------------------------------------------------------------------------------------------ 12.1 ^ HRS ACQ/ 0.25 MIRROR-A2 SEARCH-SIZE=5 1 250S 70 1 1 ONBOARD ACQ FOR PEAKUP 12.5S 2 12.2-12.5 Comments: STEP-TIME=10 SEC ------------------------------------------------------------------------------------------------------------------------------------ 12.2 USE MAG HD150798 50 5M ------------------------------------------------------------------------------------------------------------------------------------ 12.3 USE ^ 40 LYA11 70M ------------------------------------------------------------------------------------------------------------------------------------ 12.5 USE ^ 2 40 LYA2 70M ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 5323 [ 10] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations HRS ^ ------------------------------------------------------------------------------------------------------------------------------------ Opmodes ACCUM ^ ACQ ACQ/PEAKUP ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters STEP-PATT=3 DOPPLER=OFF STEP-PATT=7 FP-SPLIT=STD DOPPLER=ON STEP-PATT=5 SEARCH-SIZE=3 BRIGHT=RETURN SEARCH-SIZE=5 ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 10.48 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category COOL STARS ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category ATMOSPHERES & WINDS ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements CALIB FOR 2.1; SEQ 2-2.1 NO GAP CALIB FOR 2.6; SEQ 2.5-2.6 NO GAP CALIB FOR 3.1; SEQ 3-3.1 NO GAP CALIB FOR 3.6; SEQ 3.5-3.6 NO GAP CALIB FOR 4.1; SEQ 4-4.1 NO GAP CALIB FOR 5.1; SEQ 5-5.1 NO GAP ONBOARD ACQ FOR 10.1; CYCLE 4 / 10-10.7; SEQ 10-10.7 NO GAP; ONBOARD ACQ FOR 10.2-10.7 ONBOARD ACQ FOR 11.1; CYCLE 4 / 11-11.7; SEQ 11-11.7 NO GAP; ONBOARD ACQ FOR 11.2-11.7 ONBOARD ACQ FOR 12.1; CYCLE 4 / 12-12.5; SEQ 12-12.5 NO GAP; ONBOARD ACQ FOR 12.2-12.5 ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements ECH-B20 ^ G160M MIRROR-A2 ------------------------------------------------------------------------------------------------------------------------------------ Target Names HD111812 31-COM HD4128 BETA-CET HD150798 ALPHA-TRA ------------------------------------------------------------------------------------------------------------------------------------