Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 4492c Report Date: 09-May-96:19:38 Version: ********** Check-in Date: ********** 1.Proposal Title: THE DISTANT FUTURE OF SOLAR ACTIVITY: CYCLE3 MEDIUM ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID COOL STARS GO Sub Category STELLAR ATMOSPHERES ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone Thomas R. Ayres U.COLORADO CASA USA ------------------------------------------------------------------------------------ 7. Abstract Post-main-sequence evolution of the high-excitation chromospheric and coronal activity of cool stars may profitably be studied through detailed comparisons of the current Sun with old sun-like stars of known age, whose parameters can be interpreted in terms of perturbed solar models. Magnetically-inspired activity subsides with age, and in very old solar-mass K-giants might attain the `basal' limit set by residual acoustic heating. In the solar neighborhood, the nearest normal single sun-like star, with an advanced age (~9 Gyr) known from evolutionary tracks, is Beta Hydri (G2 IV). The closest subgiant, it presents a tempting target for detailed scrutiny across the electromagnetic spectrum. We, and our collaborators, have carried out such a study based on optical spectroscopy of traditional chromospheric tracers, and satellite (IUE & EXOSAT) measurements of high -excitation species that form in the subcoronal ``transition zone'', and in the corona itself. The historical data reveal -- through evidence for a `cool' corona (500,000 K) and a low-excitation wind akin to those of the red giants -- that Beta Hyi is a natural link between the ostensibly disparate properties of activity on the MS and in the giant branch. Nevertheless, a number of puzzles remain concerning the future fate of solar activity. The answers lie beyond the limits of the historical missions, but are easily addressed by the HST/GHRS, through high-S/N spectroscopy in its medium resolution and echelle modes. ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 3.75 par: 0 10. Num targs pri: 1 par: 0 ------------------------------------------------------------------------------------ 11. Instruments requested: HRS ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 4492c PI: Thomas R. Ayres Proposal Title: THE DISTANT FUTURE OF SOLAR ACTIVITY: CYCLE3 MEDIUM ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ Pi Thomas R. Ayres U.COLORADO CASA USA Dainis Dravins LUND OBSERVATORY SWEDEN X Peter Linde LUND OBSERVATORY SWEDEN X Page 3 ------------------------------------------------------------------------------------ 2. Scientific Justification. The study of the Sun's ``activity'' -- deriving from its magnetically-inspired chromosphere and corona -- forms the basis for understanding stellar activity and, conversely, studies of activity in sun-like stars promotes the understand- ing of solar phenomena. In particular, correlations of secular changes in act- ivity with changes in the general properties of evolving stars (like convect- ion -zone depth and rotation period) can provide clues to an understanding of the basic mechanisms that underlie the origin and variability of the nonclas- sical high-excitation layers of the stellar outer atmosphere. Besides their astrophysical interest, such changes of solar magnetic activity might have a profound affect on the Earth's climate -- in the past, present, and future. However, the fundamental mechanisms behind the activity remain controversial, despite extensive studies of the Sun over the past three decades, and more re- cent studies of the nearer stars. The major impediment to progress has been the lack of detailed comparisons of the Sun with other solar-type stars of dif- ferent activity levels, evolutionary status, and fundamental properties (esp- ecially metallicity and rotation period). The Sun drowns us in details, that however refer to only a thin -- possibly unrepresentative -- slice of the over- all specimen of stellar activity. On the other hand, while activity indicators routinely are recorded for many bright field stars, it often is difficult or ambigiuous to trace the evolutionary history of such heterogeneous samples, and to determine key subsidiary properties, like rotation period and convection- zone depth. Thus, comparisons with the Sun have been only rough and tentative. The difficulty of studying detailed physical processes in distant stars makes it awkward to identify the precise operational parameters behind the secular evolution of the Sun's activity, even though solar-mass stars display rather dramatic aging of their coronal properties. A tantalizing possibility is of- fered by stars almost identical to the Sun, whose parameters then can be inter- preted in terms of (perturbed) solar models. A careful selection of such stars is the key to the probable past and future of solar activity. On the young side, youthful solar-mass stars normally are sought in undispersed galactic clusters containing blue MS types. G-type dwarfs in young clusters (t < 1 Gyr) are characterized by much stronger chromospheric and coronal emis- sions than the present Sun (t= 5 Gyr). The deline in optical Ca II K activity with age has been known for several decades and is attributed to the fading of hydromagetic ``dynamo'' action as the star spins down owing to loss of angular momentum from its magnetized coronal wind. The fading of high-excitation cor- onal emission is much faster than that of the lower-temperature chromospheric layers, based on EINSTEIN studies of young galactic clusters. The behavior of the key intermediate-temperature layers of the 100,000 K ``transition zone'' is less-well known, but is the subject of an approved two-year HST program ``Sleuthing the Dynamo'' (same P.I. as present proposal). On the old side, the qualitative behavior of activity in aging solar-mass stars also is known: the chromosphere continues to fade slowly, while the corona maintains its much more precipitous decline, reaching essentially undetectable levels (1/10,000-th solar surface flux densities) in old solar-mass red giants. Complicating matters, however, is the increasing importance of the ``basal'' chromosphere -- due to residual acoustic heating -- as the magnetic aspect of the activity subsides, and the appearance of low-excitation winds in the red giants. The origin of the cool flows of the red giants is at least as contro- versial as that of the solar coronal wind, while the implications for the en- ergy balance of the outer atmosphere are more profound (because the gas accel- eration likely occurs within or close to the high-density chromosphere itself). Nevertheless, old stars are more difficult to study than young stars because their activity levels are much reduced, and their ages usually are ambiguous. Clusters are of little help in that regard, because the globulars that contain old stars are so distant that solar-quality scrutiny is out of the question. Happily, however, the immediate galactic neighborhood includes a star -- Beta Hydri (HD 2151; G2 IV) -- that is virtually identical to the Sun (G2 V) except for age; and is one of only a handful of stars whose position in the H-R dia- gram permits its evolutionary history to be accurately deduced differentially with respect to solar models (Fig. 1, below). At an age of 9 Gyr, Beta Hyi represents an intermediate step between the present Sun and its far-distant future: the post-helium-flash K giant Arcturus (Alpha Boo: K2 III). By all appearances, Beta Hyi is a fully normal, single star. Its large paral- lax yields a distance of 6.5 pc; its Teff is similar to the Sun's (5780 K); while its gravity is 0.5 dex smaller, in keeping with its subgiant status. As expected for an old star, Beta Hyi is slightly metal-poor with [Fe/H] 0.2 dex below solar; its rotation period is about 50% longer than the Sun's; and it has a relatively eccentric galactic orbit. Color-magnitude diagrams show Beta Hyi to be comparable in age to the oldest clusters in the galactic halo. Our previous work on Beta Hyi suggests that the nearby subgiant represents, not surprisingly, the ``missing link'' between hot-corona stars like the Sun and the noncoronal red giants like the ancient-Sun analog, Arcturus. In partic- ular, EXOSAT X-ray filter-photometry admits a remarkable ``cool-corona '' sol- ution (1/4 the solar coronal temperature), while IUE spectroscopy has revealed peculiar blue-shifted absorptions in the chromospheric Mg II emission cores which possibly indicate a low-excitation wind like that normally associated with much more luminous, cooler stars. We propose a program with the GHRS of HST to continue our exploration -- beyond the instrumental limits of the historical missions -- of the pivotal role of Beta Hyi in the question of how the MS corona, and its hot high-speed wind, evolves into the ``noncorona'', and its cool low-speed chromospheric wind, of the red-giant branch. Page 4 ------------------------------------------------------------------------------------ 3. Description of proposed observations. The observational objective of the program is to acquire key spectral diagnos- tics of the dynamical and structural properties of the chromosphere and sub- coronal transition zone of Beta Hydri (G2 IV), an analog of the post-MS Sun. Our observation plan, in order of priority, is as follows: (1) **70M exposure G160M (LSA) 1386-1420 A**: Moderate-S/N medium-resolution spectrum of 1400 A region containing O IV] 1401,04,07 multiplet, crucial density diagnostic in solar-type stars, and the ``emission-measure'' spec- ies Si IV 1393,1402. Obtain sufficient S/N to record profile shapes and any systematic Doppler shifts. Line widths indicate the amplitude of non- thermal Doppler broadening in the 60,000-100,000 K layers of the transition zone, which plays key role in theories of subcoronal energy balance. Sys- tematic line shifts could be related to large-scale bulk flows of material, like redshifts of Si IV-temperature gas routinely observed in coronal stars of all luminosity classes and thought to be connected with TZ downdrafts seen in coronal magnetic loops on the Sun. (1') **25M exposure ECH-B (SSA) 2791-2805 A**: Very-high-S/N spectrum of Mg II 2800 doublet. Objective is to resolve mysterious blueward absorption fea- tures in h & k cores into interstellar -- possibly also circumstellar -- components. If asymmetry is produced by outflowing gas from the star, it would be crucial ``missing-link'' between hot, fast coronal wind of the Sun and cool, low-speed flows of solar- mass K giants like Arcturus. (2) **45M exposure G160M (LSA) 1538-1572 A**: moderate S/N profile of C IV 1549 doublet, strongest high-temperature (100,000 K) emission of FUV region. (3) **60M exposure G160M (LSA) 1209-1245 A**: Moderate S/N profiles of highest excitation emissions easily accessible in FUV: O V] 1218 (250,000 K) & N V 1238,42 (200,000 K). The four G160M settings cover a wide range of ``emission-measure'' species, to supplement the existing, but poor-quality material from IUE low-dispersion spectra. These data will be used to construct a detailed physical model of the outer atmosphere of Beta Hyi, in conjunction with additional diagnostics of the higher-excitation coronal gas from EXOSAT and, more recently, ROSAT. Page 5 ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. The study of Beta Hydri has been pursued vigorously using a wide variety of historical and recent, ground-based and satellite data sets. The available data is discussed briefly elsewhere in the proposal, and in great depth in our paper ``The Distant Future of Solar Activity - A Case Study of Beta Hydri'', (Dravins, Linde, Ayres, et al.) which is in press in the Astrophysical Journal (20 Jan 1993 issue). The most remarkable result of our work was the possi- bility, based on filter-photometry with the LE1 X-ray telescope of EXOSAT, that Beta Hyi has a surprisingly cool 500,000 K ``corona''; only 1/4 the temperature of the Sun's. The EXOSAT result is consistent with the detection of Beta Hyi in the ROSAT PSPC survey; and it suggests a profoundly-different sense of cor- onal evolution (in temperature rather than simply emission measure) than has been considered previously. In contrast to the X-ray studies, the previous UV work with the IUE almost immediately reached a number of critical observational limits, leaving key questions unanswered. For example, while the R=10,000 resolution of the IUE LW-HI mode was sufficient to reveal the existence of the surprising blue asymmetries in the Mg II h & k cores of Beta Hyi (Fig. 2, above), it does not permit the origin of the short- ward absorptions to be elucidated. If the features are narrow (at the R= 85,000 resolution of ECH-B), and at precisely the expected ISM velocity, then there would be no need to invoke chromospheric mass loss. On the other hand, if the features are broad, multiple, or appear at velocities inconsistent with the ISM, then a chromospheric-wind origin must be entertained. Another example involves the emission-measure modeling of the high-excitation layers. At present, the only firmly-detected high-excitation emissions in the far-UV spectrum of Beta Hyi are the Si IV 1400 and C IV 1549 doublets (Fig.3, above). These achieve respectable 5-7 sigma status only through the co-addit- ion of a number of optimally-processed SWP-LO spectra representing more than 500M of total exposure. However, the emission-measure models carry little weight without an accurate value for the TZ density (at a known temperature level). The traditional (for IUE) Si III] 1892 + C III] 1909 density diagnos- tic is useless in solar-type stars like Beta Hyi owing to the bright photo- spheric continuum at 1900 A. The IUE is not sensitive enough to record the prefered (in solar applications) density-sensitive O IV] 1401,04,07 multiplet, nor does it possess enough resolution in its low-dispersion mode to separate the components from Si IV 1402 (and from each other). Thus, the IUE cannot reach key emission-measure species (like O V] 1218 & N V 1240), and cannot provide a density measurement to pin down the EM distributions for comparison with the EXOSAT (and now also ROSAT) coronal X-ray studies. Further, a heroic 938M NASA/ESA collaborative exposure of Beta Hyi taken by us in 1982 with the IUE SW-HI mode (R= 10,000) failed to record any features shortward of Si II 1808 aside from the red peak of H I 1215 Lyman alpha. How- ever, the latter was faint and seriously corrupted by overexposed geocoronal emission. Thus, IUE cannot provide any information on TZ dynamics -- e.g., Si IV, C IV, & N V profile shapes and Doppler shifts -- in Beta Hyi. Finally, D. Duncan & collaborators have an approved HST program (#3614) to mea- sure UV boron lines in Beta Hyi. Their project in no way conflicts with ours. (b) Exposure Times & S/C Times For the G160M spectrum of the 1400 A region, we would use the high-throughput LSA, because the Si IV and O IV] lines are well- resolved at R= 10,000. The peak flux of Si IV 1393 is about 2.5E-13 ergs/cm^2/s/A for an expected FWHM= 50 km/s (comparable to that of the solar Si IV profile), or about 500 ct/H. Thus, a 1H exposure will yield S/N= 22 at the line peak; a (theoretical) precision in the velocity measurement of 1 km/s; and a precision in the inte- grated flux of 2% (the feature covers about 10 diodes). O IV] 1401 is the stronger component (by a factor of two) of the density-sensitive pair 1401,04; and is about 20% the flux of Si IV 1393 (in HST/GHRS spectra of Capella, an evolved [i.e., low-density] star like Beta Hyi and close in surface tempera- ture). Thus, O IV] 1401 should be recorded at about 100 ct/H (at the line peak), or S/N= 10 in 60M. Similarly, the weaker component of the O IV] pair should achieve S/N= 7 in 1H. The S/N's of the integrated fluxes (total counts over the Gaussian profiles) should be about 20 and 14, respectively, for the two lines, leading to an accurate value for the ratio, and a well- defined electron density: 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 TZ's of evolved stars are thought to lie). The chromospheric Mg II emission of Beta Hyi is quite bright, about 2E-11 ergs/cm^2/s/A in the red peak of the 2795 A k line. Even through the SSA (to achieve maximum purity of the instrumental profile), that corresponds to 7 ct/s with ECH-B, or peak S/N= 80 in 15M. Very-high S/N at the ``k2'' peak ensures S/N> 40 throughout the fainter damping wings, particularly at the im- portant ``k1'' minimum features. Such quality -- typical of solar Mg II pro- files, but unprecedented for stars -- is essential for detailed spectrum-sim - ulation work, particularly in the case of Beta Hyi where resolved structure in the blueward part of the emission core might document outflowing material. For the G160M spectrum of the 1204-1240 A region, we would use the LSA, to obtain the highest throughput, at the expense of some geocoronal contamination at the H I feature. The peak flux of Lyman alpha is about 3E-12, yielding 3,200 ct/H or S/N= 57 in a 1H exposure. The Si III feature should be recorded at a S/N= 30:1 at the line peak. Similarly, a 1H exposure of the O V] + N V inter- val should yield peak S/N> 10:1 at both 1218 and 1238, while a 0.5H exposure of the C IV interval should yield a peak S/N= 20 at the 1548 component. Peak S/N ratios (per diode, smoothed over the substeps) in the range 10-20 are required to provide accuracies in the line centroids compatible with the precision of the wavelength scale assignments. Page 6 ------------------------------------------------------------------------------------ 5. Description of special scheduling requirements. **IMPORTANT NOTE**: If Beta Hyi is observed in the Continuous Viewing Zone, the total S/C time (item 10a, Cover Page) will decrease by about 1.1H, and the pro- gram efficiency (item 10b) will increase from 71% to about 91%. Assurance of the precision of the wavelength scales of the medium-resolution and the 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 spectra. The lamp exposures would be of order 30S, to obtain sub- km/s accuracy in the assigned wavelength scales. ------------------------------------------------------------------------------------ 6. Description of special calibration exposures. OSF Line Number(s) Instrument Mode Special Calibration Requirement(s) ___________________ __________ _______ __________________________________ 1.0 -- 1.3 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 lines. ------------------------------------------------------------------------------------ 7. Data reduction and analysis plans. The analysis of the GHRS spectra will be conducted both at the P.I.'s institut- ion and at Lund Observatory in Sweden, following an initial visit by the P.I. to the STScI in Baltimore. The preliminary analysis involves the measurement of spectral features using standard fitting routines: the application to the GHRS data sets should be straightforward. We will measure the profile shapes and Doppler shifts of the Si IV and O IV] multiplets from the medium-resolut- ion spectrum; the blueshifts of discrete absorption components in the chromo- spheric cores of the Mg II h and k lines observed at echelle resolution; and the line fluxes of all measurable (i.e., statistically-significant) emissions in the low- resolution spectrum. We then will develop a dynamical picture of the subcoronal transition zone of Beta Hyi from the Doppler widths and shifts of the high- excitation Si III, Si IV, C IV, O IV], N V, & O V] emissions (which span the range 30,000-250,000 K in line-formation temperature); and attempt to connect it to the chromosph- eric layers as diagnosed by the Mg II and Lyman alpha shapes and possible blue- shifted ``wind'' components. We will utilize the line fluxes to construct a physical description of the outer atmosphere, principally through ``emission- measure'' modeling. The program will sample emissions from a wide range of ex- citation and a diversity of optical thicknesses. The available species should very tightly constrain the possible thermal structures, in contrast to the very superficial picture obtainable historically from IUE SWP-LO spectra (a major deficiency of the historical observations is the lack of sufficient spectral resolution or sensitivity to record the key density- sensitive O IV] multiplet). A clear view of the thermal structure then permits a calculation of the excess radiative losses of the gas. Because the distribution of the radiative cooling with height must balance the ``mechanical'' heating, a knowledge of the one can provide valuable insight into the (still elusive) nature of the other. A crucial aspect of the analysis will be to tie together the historical X-ray studies of Beta Hyi by EXOSAT and new results obtained from the ROSAT survey (and possibly also pointed observations). The O IV] density- diagnostic will provide the key to linking the emission measures inferred for the different energy ranges. Furthermore, the gradient of emission measure from C IV temper- atures (100,000 K) through O V] temperatures (250,000 K) should indicate unamb- iguously whether the cool-corona solutions obtained from the EXOSAT LE1/CMA de- tections are viable. ------------------------------------------------------------------------------------ 8. Additional comments or special requests. N/A Page 7 ------------------------------------------------------------------------------------ 9. Description of previous HST work. (a) HST program numbers and titles: 2485: ``Sleuthing the Dynamo: Cycle 1 Observations'' [peripherly related to present project: see text] 3908: ``Sleuthing the Dynamo: Cycle 2 Observations'' [peripherly related to present project: see text] (b) Summary of main results: no observations obtained to date in these programs (c) HST-related publications: ``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, to appear 10 Jan 1993. ``The hydrogen Lyman alpha emission of Capella'', Ayres, T. R., Brown, A., Gayley, K. G., & Linsky, J. L., Astrophysical Journal, to appear 10 Jan 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). ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). At the University of Colorado a version of the reduction software written by the GHRS team is available on a VAXstation. A recent version of IRAF/SDAS is hosted on a DECstation and a SUN-4. We, and our students at Colorado and Lund, will conduct theoretical studies of the UV emissions from the outer atmosphere and wind of Beta Hyi using fast numerical simulation codes recently implemented on a variety of workstation platforms. ------------------------------------------------------------------------------------ 11. Address Information Name: THOMAS R. AYRES Category: PI Institution: U.Colorado CASA 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): ------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 4492c [ 8] ------------------------------------------------------------------------------------------------------------------------------------ 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 HD2151 BETA- A, 137, 901, 905 RA = 0H 23M 9.374S +/- 1950 V=+23 1 V = 2.80 +/- 0.10, TYPE = G2IV HYI 0.03S, 2 B-V = +0.62 +/- 0.01 DEC = -77D 32' 8.50" +/- 3 F-LINE(1215)= 3 +/- 1 E-12 0.1" 4 W-LINE(1216)= 1 +/- 0.2 5 F-LINE(2795)= 20 +/- 5 E-12 6 W-LINE(2795)= 1 +/- 0.2 7 F-LINE(1393)= 2.0 +/- 0.5 E-13 8 W-LINE(1393)= 0.25 +/- 0.05 9 F-LINE(1548)= 4.0 +/- 0.5 E-13 10 W-LINE(1548)= 0.25 +/- 0.05 Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec) B 1950.00 0.6885 +/- 0.0000 0.3270 +/- 0.0000 0.1590 +/- 0.0070 ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 4492c [ 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 ------------------------------------------------------------------------------------------------------------------------------------ 1 HD2151 HRS ACQ 2.0 MIRROR-A2 SEARCH-SIZE=5 1 12.5S 35 1 1 ONBOARD ACQ FOR BRIGHT=RETURN 0.5S 2 1.1 CYCLE 3 / 1-5.1 GROUP 1-5.1 NO GAP Comments: STEP TIME = 0.5 SEC ------------------------------------------------------------------------------------------------------------------------------------ 1.1 HD2151 HRS ACQ/ 0.25 MIRROR-A2 1 40.0S 63 1 1 ONBOARD ACQ FOR PEAKUP 1.6S 2 2.0-5.1 Comments: STEP-TIME=1.6 SEC ------------------------------------------------------------------------------------------------------------------------------------ 2 WAVE HRS ACCUM SC2 ECH-B20 2798 STEP-PATT=7 1 27.2S 30 1 CALIB FOR 2.1 30S SEQ 2-2.1 NO GAP ------------------------------------------------------------------------------------------------------------------------------------ 2.1 HD2151 ^ ^ 0.25 ^ ^ STEP-PATT=7 1 1524S 40 5 ^ FP-SPLIT=STD 5M 6 ------------------------------------------------------------------------------------------------------------------------------------ 3 HD2151 HRS IMAGE 2.0 MIRROR-A2 1 128S 35 1 2 0.5S 2 Comments: TAKE MAP AFTER CENTERING 0.5 SEC INTEGRATIONS ------------------------------------------------------------------------------------------------------------------------------------ 3.1 WAVE HRS ACCUM SC2 G160M 1403 STEP-PATT=5 1 27.2S 30 1 CALIB FOR 3.2 30S SEQ 3-3.2 NO GAP ------------------------------------------------------------------------------------------------------------------------------------ 3.2 HD2151 ^ ^ 2.0 ^ ^ STEP-PATT=5 3 1415S 20 7 ^ FP-SPLIT=STD 1H 8 ------------------------------------------------------------------------------------------------------------------------------------ 4 WAVE HRS ACCUM SC2 G160M 1555 STEP-PATT=5 1 27.2S 30 2 CALIB FOR 4.1 30S SEQ 4-4.1 NO GAP ------------------------------------------------------------------------------------------------------------------------------------ 4.1 HD2151 ^ ^ 2.0 ^ ^ STEP-PATT=5 2 1306S 25 9 ^ FP-SPLIT=STD 1H 10 ------------------------------------------------------------------------------------------------------------------------------------ 5 WAVE HRS ACCUM SC2 G160M 1223 STEP-PATT=5 1 27.2S 30 3 CALIB FOR 5.1 30S SEQ 5-5.1 NO GAP ------------------------------------------------------------------------------------------------------------------------------------ 5.1 HD2151 HRS ACCUM 2.0 G160M 1223 STEP-PATT=5 2 1850S 57 3 ^ FP-SPLIT=STD 1H 4 ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 4492c [ 10] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations HRS ^ ------------------------------------------------------------------------------------------------------------------------------------ Opmodes ACQ ACQ/PEAKUP ACCUM ^ IMAGE ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters SEARCH-SIZE=5 BRIGHT=RETURN STEP-PATT=7 FP-SPLIT=STD STEP-PATT=5 ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 3.75 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category COOL STARS ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category STELLAR ATMOSPHERES ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements ONBOARD ACQ FOR 1.1; CYCLE 3 / 1-5.1; GROUP 1-5.1 NO GAP; ONBOARD ACQ FOR 2.0-5.1 CALIB FOR 2.1; SEQ 2-2.1 NO GAP CALIB FOR 3.2; SEQ 3-3.2 NO GAP CALIB FOR 4.1; SEQ 4-4.1 NO GAP CALIB FOR 5.1; SEQ 5-5.1 NO GAP ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements MIRROR-A2 ECH-B20 ^ G160M ------------------------------------------------------------------------------------------------------------------------------------ Target Names HD2151 BETA-HYI ------------------------------------------------------------------------------------------------------------------------------------