! File: 4492C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:14:38:05 coverpage: title_1: THE DISTANT FUTURE OF SOLAR ACTIVITY: CYCLE3 MEDIUM sci_cat: COOL STARS sci_subcat: STELLAR ATMOSPHERES proposal_for: GO pi_fname: THOMAS pi_mi: R. pi_lname: AYRES pi_inst: U.COLORADO CASA pi_country: USA hours_pri: 3.75 num_pri: 1 hrs: Y funds_length: 12 off_fname: LAURENCE off_mi: D. off_lname: NELSON off_title: DIRECTOR off_inst: 1760 off_addr_1: OFFICE OF CONTRACTS AND GRANTS off_addr_2: CAMPUS BOX 19 off_city: BOULDER off_state: CO off_zip: 80309 off_country: USA off_phone: 303-492-2695 ! end of coverpage abstract: line_1: Post-main-sequence evolution of the high-excitation chromospheric and coronal line_2: activity of cool stars may profitably be studied through detailed comparisons line_3: of the current Sun with old sun-like stars of known age, whose parameters can line_4: be interpreted in terms of perturbed solar models. Magnetically-inspired line_5: activity subsides with age, and in very old solar-mass K-giants might attain line_6: the `basal' limit set by residual acoustic heating. In the solar neighborhood, line_7: the nearest normal single sun-like star, with an advanced age (~9 Gyr) known line_8: from evolutionary tracks, is Beta Hydri (G2 IV). The closest subgiant, it line_9: presents a tempting target for detailed scrutiny across the electromagnetic line_10: spectrum. We, and our collaborators, have carried out such a study based on line_11: optical spectroscopy of traditional chromospheric tracers, and satellite (IUE & line_12: EXOSAT) measurements of high-excitation species that form in the subcoronal line_13: ``transition zone'', and in the corona itself. The historical data reveal -- line_14: through evidence for a `cool' corona (500,000 K) and a low-excitation wind akin line_15: to those of the red giants -- that Beta Hyi is a natural link between the line_16: ostensibly disparate properties of activity on the MS and in the giant branch. line_17: Nevertheless, a number of puzzles remain concerning the future fate of solar line_18: activity. The answers lie beyond the limits of the historical missions, line_19: but are easily addressed by the HST/GHRS, through high-S/N spectroscopy line_20: in its medium resolution and echelle modes. ! ! end of abstract general_form_proposers: lname: AYRES fname: THOMAS title: PI mi: R. inst: U.COLORADO CASA country: USA ! lname: DRAVINS fname: DAINIS inst: LUND OBSERVATORY country: SWEDEN esa: Y ! lname: LINDE fname: PETER inst: LUND OBSERVATORY country: SWEDEN esa: Y ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: The study of the Sun's ``activity'' -- deriving from its magnetically-inspired line_2: chromosphere and corona -- forms the basis for understanding stellar activity line_3: and, conversely, studies of activity in sun-like stars promotes the understand- line_4: ing of solar phenomena. In particular, correlations of secular changes in act- line_5: ivity with changes in the general properties of evolving stars (like convect- line_6: ion-zone depth and rotation period) can provide clues to an understanding of line_7: the basic mechanisms that underlie the origin and variability of the nonclas- line_8: sical high-excitation layers of the stellar outer atmosphere. Besides their line_9: astrophysical interest, such changes of solar magnetic activity might have a line_10: profound affect on the Earth's climate -- in the past, present, and future. line_12: However, the fundamental mechanisms behind the activity remain controversial, line_13: despite extensive studies of the Sun over the past three decades, and more re- line_14: cent studies of the nearer stars. The major impediment to progress has been line_15: the lack of detailed comparisons of the Sun with other solar-type stars of dif- line_16: ferent activity levels, evolutionary status, and fundamental properties (esp- line_17: ecially metallicity and rotation period). The Sun drowns us in details, that line_18: however refer to only a thin -- possibly unrepresentative -- slice of the over- line_19: all specimen of stellar activity. On the other hand, while activity indicators line_20: routinely are recorded for many bright field stars, it often is difficult or line_21: ambigiuous to trace the evolutionary history of such heterogeneous samples, and line_22: to determine key subsidiary properties, like rotation period and convection- line_23: zone depth. Thus, comparisons with the Sun have been only rough and tentative. ! question: 2 section: 2 line_1: line_2: The difficulty of studying detailed physical processes in distant stars makes line_3: it awkward to identify the precise operational parameters behind the secular line_4: evolution of the Sun's activity, even though solar-mass stars display rather line_5: dramatic aging of their coronal properties. A tantalizing possibility is of- line_6: fered by stars almost identical to the Sun, whose parameters then can be inter- line_7: preted in terms of (perturbed) solar models. A careful selection of such stars line_8: is the key to the probable past and future of solar activity. line_10: On the young side, youthful solar-mass stars normally are sought in undispersed line_11: galactic clusters containing blue MS types. G-type dwarfs in young clusters line_12: (t < 1 Gyr) are characterized by much stronger chromospheric and coronal emis- line_13: sions than the present Sun (t= 5 Gyr). The deline in optical Ca II K activity line_14: with age has been known for several decades and is attributed to the fading of line_16: hydromagetic ``dynamo'' action as the star spins down owing to loss of angular line_17: momentum from its magnetized coronal wind. The fading of high-excitation cor- line_18: onal emission is much faster than that of the lower-temperature chromospheric line_19: layers, based on EINSTEIN studies of young galactic clusters. The behavior of line_20: the key intermediate-temperature layers of the 100,000 K ``transition zone'' line_21: is less-well known, but is the subject of an approved two-year HST program line_22: ``Sleuthing the Dynamo'' (same P.I. as present proposal). ! question: 2 section: 3 line_1: On the old side, the qualitative behavior of activity in aging solar-mass stars line_2: also is known: the chromosphere continues to fade slowly, while the corona line_3: maintains its much more precipitous decline, reaching essentially undetectable line_4: levels (1/10,000-th solar surface flux densities) in old solar-mass red giants. line_5: Complicating matters, however, is the increasing importance of the ``basal'' line_6: chromosphere -- due to residual acoustic heating -- as the magnetic aspect of line_7: the activity subsides, and the appearance of low-excitation winds in the red line_8: giants. The origin of the cool flows of the red giants is at least as contro- line_9: versial as that of the solar coronal wind, while the implications for the en- line_10: ergy balance of the outer atmosphere are more profound (because the gas accel- line_11: eration likely occurs within or close to the high-density chromosphere itself). line_12: Nevertheless, old stars are more difficult to study than young stars because line_13: their activity levels are much reduced, and their ages usually are ambiguous. line_14: Clusters are of little help in that regard, because the globulars that contain line_15: old stars are so distant that solar-quality scrutiny is out of the question. line_17: Happily, however, the immediate galactic neighborhood includes a star -- Beta line_18: Hydri (HD 2151; G2 IV) -- that is virtually identical to the Sun (G2 V) except line_19: for age; and is one of only a handful of stars whose position in the H-R dia- line_20: gram permits its evolutionary history to be accurately deduced differentially line_21: with respect to solar models (Fig. 1, below). At an age of 9 Gyr, Beta Hyi line_22: represents an intermediate step between the present Sun and its far-distant line_23: future: the post-helium-flash K giant Arcturus (Alpha Boo: K2 III). ! question: 2 section: 4 line_1: line_2: By all appearances, Beta Hyi is a fully normal, single star. Its large paral- line_3: lax yields a distance of 6.5 pc; its Teff is similar to the Sun's (5780 K); line_4: while its gravity is 0.5 dex smaller, in keeping with its subgiant status. As line_5: expected for an old star, Beta Hyi is slightly metal-poor with [Fe/H] 0.2 dex line_6: below solar; its rotation period is about 50% longer than the Sun's; and it has line_7: a relatively eccentric galactic orbit. Color-magnitude diagrams show Beta Hyi line_8: to be comparable in age to the oldest clusters in the galactic halo. line_10: Our previous work on Beta Hyi suggests that the nearby subgiant represents, not line_11: surprisingly, the ``missing link'' between hot-corona stars like the Sun and line_12: the noncoronal red giants like the ancient-Sun analog, Arcturus. In partic- line_13: ular, EXOSAT X-ray filter-photometry admits a remarkable ``cool-corona '' sol- line_14: ution (1/4 the solar coronal temperature), while IUE spectroscopy has revealed line_15: peculiar blue-shifted absorptions in the chromospheric Mg II emission cores line_16: which possibly indicate a low-excitation wind like that normally associated line_17: with much more luminous, cooler stars. We propose a program with the GHRS of line_18: HST to continue our exploration -- beyond the instrumental limits of the line_19: historical missions -- of the pivotal role of Beta Hyi in the question of how line_20: the MS corona, and its hot high-speed wind, evolves into the ``noncorona'', and line_21: its cool low-speed chromospheric wind, of the red-giant branch. ! question: 3 section: 1 line_1: The observational objective of the program is to acquire key spectral diagnos- line_2: tics of the dynamical and structural properties of the chromosphere and sub- line_3: coronal transition zone of Beta Hydri (G2 IV), an analog of the post-MS Sun. line_4: Our observation plan, in order of priority, is as follows: line_6: (1) **70M exposure G160M (LSA) 1386-1420 A**: Moderate-S/N medium-resolution line_7: spectrum of 1400 A region containing O IV] 1401,04,07 multiplet, crucial line_8: density diagnostic in solar-type stars, and the ``emission-measure'' spec- line_9: ies Si IV 1393,1402. Obtain sufficient S/N to record profile shapes and line_10: any systematic Doppler shifts. Line widths indicate the amplitude of non- line_11: thermal Doppler broadening in the 60,000-100,000 K layers of the transition line_12: zone, which plays key role in theories of subcoronal energy balance. Sys- line_13: tematic line shifts could be related to large-scale bulk flows of material, line_14: like redshifts of Si IV-temperature gas routinely observed in coronal stars line_15: of all luminosity classes and thought to be connected with TZ downdrafts line_16: seen in coronal magnetic loops on the Sun. line_18: (1') **25M exposure ECH-B (SSA) 2791-2805 A**: Very-high-S/N spectrum of Mg II line_19: 2800 doublet. Objective is to resolve mysterious blueward absorption fea- line_20: tures in h & k cores into interstellar -- possibly also circumstellar -- line_21: components. If asymmetry is produced by outflowing gas from the star, it line_22: would be crucial ``missing-link'' between hot, fast coronal wind of the Sun line_23: and cool, low-speed flows of solar- mass K giants like Arcturus. ! question: 3 section: 2 line_1: line_2: (2) **45M exposure G160M (LSA) 1538-1572 A**: moderate S/N profile of C IV 1549 line_3: doublet, strongest high-temperature (100,000 K) emission of FUV region. line_5: (3) **60M exposure G160M (LSA) 1209-1245 A**: Moderate S/N profiles of highest line_6: excitation emissions easily accessible in FUV: O V] 1218 (250,000 K) & N V line_7: 1238,42 (200,000 K). line_9: The four G160M settings cover a wide range of ``emission-measure'' species, to line_10: supplement the existing, but poor-quality material from IUE low-dispersion line_11: spectra. These data will be used to construct a detailed physical model of line_12: the outer atmosphere of Beta Hyi, in conjunction with additional diagnostics line_13: of the higher-excitation coronal gas from EXOSAT and, more recently, ROSAT. ! question: 4 section: 1 line_1: The study of Beta Hydri has been pursued vigorously using a wide variety of line_2: historical and recent, ground-based and satellite data sets. The available line_3: data is discussed briefly elsewhere in the proposal, and in great depth in our line_4: paper ``The Distant Future of Solar Activity - A Case Study of Beta Hydri'', line_5: (Dravins, Linde, Ayres, et al.) which is in press in the Astrophysical Journal line_6: (20 Jan 1993 issue). The most remarkable result of our work was the possi- line_7: bility, based on filter-photometry with the LE1 X-ray telescope of EXOSAT, that line_8: Beta Hyi has a surprisingly cool 500,000 K ``corona''; only 1/4 the temperature line_9: of the Sun's. The EXOSAT result is consistent with the detection of Beta Hyi line_10: in the ROSAT PSPC survey; and it suggests a profoundly-different sense of cor- line_11: onal evolution (in temperature rather than simply emission measure) than has line_12: been considered previously. In contrast to the X-ray studies, the previous UV line_13: work with the IUE almost immediately reached a number of critical observational line_14: limits, leaving key questions unanswered. line_16: For example, while the R=10,000 resolution of the IUE LW-HI mode was sufficient line_17: to reveal the existence of the surprising blue asymmetries in the Mg II h & k line_18: cores of Beta Hyi (Fig. 2, above), it does not permit the origin of the short- line_19: ward absorptions to be elucidated. If the features are narrow (at the R= line_20: 85,000 resolution of ECH-B), and at precisely the expected ISM velocity, then line_21: there would be no need to invoke chromospheric mass loss. On the other hand, line_22: if the features are broad, multiple, or appear at velocities inconsistent with line_23: the ISM, then a chromospheric-wind origin must be entertained. ! question: 4 section: 2 line_1: line_2: Another example involves the emission-measure modeling of the high-excitation line_3: layers. At present, the only firmly-detected high-excitation emissions in the line_4: far-UV spectrum of Beta Hyi are the Si IV 1400 and C IV 1549 doublets (Fig.3, line_5: above). These achieve respectable 5-7 sigma status only through the co-addit- line_6: ion of a number of optimally-processed SWP-LO spectra representing more than line_7: 500M of total exposure. However, the emission-measure models carry little line_8: weight without an accurate value for the TZ density (at a known temperature line_9: level). The traditional (for IUE) Si III] 1892 + C III] 1909 density diagnos- line_10: tic is useless in solar-type stars like Beta Hyi owing to the bright photo- line_11: spheric continuum at 1900 A. The IUE is not sensitive enough to record the line_12: prefered (in solar applications) density-sensitive O IV] 1401,04,07 multiplet, line_13: nor does it possess enough resolution in its low-dispersion mode to separate line_14: the components from Si IV 1402 (and from each other). Thus, the IUE cannot line_15: reach key emission-measure species (like O V] 1218 & N V 1240), and cannot line_16: provide a density measurement to pin down the EM distributions for comparison line_17: with the EXOSAT (and now also ROSAT) coronal X-ray studies. line_19: Further, a heroic 938M NASA/ESA collaborative exposure of Beta Hyi taken by us line_20: in 1982 with the IUE SW-HI mode (R= 10,000) failed to record any features line_21: shortward of Si II 1808 aside from the red peak of H I 1215 Lyman alpha. How- line_22: ever, the latter was faint and seriously corrupted by overexposed geocoronal line_23: emission. Thus, IUE cannot provide any information on TZ dynamics -- e.g., ! question: 4 section: 3 line_1: Si IV, C IV, & N V profile shapes and Doppler shifts -- in Beta Hyi. line_3: Finally, D. Duncan & collaborators have an approved HST program (#3614) to mea- line_4: sure UV boron lines in Beta Hyi. Their project in no way conflicts with ours. line_6: (b) Exposure Times & S/C Times line_8: For the G160M spectrum of the 1400 A region, we would use the high-throughput line_9: LSA, because the Si IV and O IV] lines are well-resolved at R= 10,000. The line_10: peak flux of Si IV 1393 is about 2.5E-13 ergs/cm^2/s/A for an expected line_11: FWHM= 50 km/s (comparable to that of the solar Si IV profile), or about 500 line_12: ct/H. Thus, a 1H exposure will yield S/N= 22 at the line peak; a (theoretical) line_13: precision in the velocity measurement of 1 km/s; and a precision in the inte- line_14: grated flux of 2% (the feature covers about 10 diodes). O IV] 1401 is the line_15: stronger component (by a factor of two) of the density-sensitive pair 1401,04; line_16: and is about 20% the flux of Si IV 1393 (in HST/GHRS spectra of Capella, an line_17: evolved [i.e., low-density] star like Beta Hyi and close in surface tempera- line_18: ture). Thus, O IV] 1401 should be recorded at about 100 ct/H (at the line line_19: peak), or S/N= 10 in 60M. Similarly, the weaker component of the O IV] line_20: pair should achieve S/N= 7 in 1H. The S/N's of the integrated fluxes (total line_21: counts over the Gaussian profiles) should be about 20 and 14, respectively, line_22: for the two lines, leading to an accurate value for the ratio, and a well- line_23: defined electron density: a 5% uncertainty in the flux ratio translates into ! question: 4 section: 4 line_1: a (very small) 15% uncertainty in the electron density over the range log N= line_2: 8.5-10.5 where the O IV] diagnostic is useful (and where the densities of the line_3: TZ's of evolved stars are thought to lie). line_5: The chromospheric Mg II emission of Beta Hyi is quite bright, about 2E-11 line_6: ergs/cm^2/s/A in the red peak of the 2795 A k line. Even through the SSA (to line_7: achieve maximum purity of the instrumental profile), that corresponds to 7 line_8: ct/s with ECH-B, or peak S/N= 80 in 15M. Very-high S/N at the ``k2'' peak line_9: ensures S/N> 40 throughout the fainter damping wings, particularly at the im- line_10: portant ``k1'' minimum features. Such quality -- typical of solar Mg II pro- line_11: files, but unprecedented for stars -- is essential for detailed spectrum-sim- line_12: ulation work, particularly in the case of Beta Hyi where resolved structure in line_13: the blueward part of the emission core might document outflowing material. line_14: For the G160M spectrum of the 1204-1240 A region, we would use the LSA, to line_15: obtain the highest throughput, at the expense of some geocoronal contamination line_16: at the H I feature. The peak flux of Lyman alpha is about 3E-12, yielding 3,200 line_17: ct/H or S/N= 57 in a 1H exposure. The Si III feature should be recorded at a line_18: S/N= 30:1 at the line peak. Similarly, a 1H exposure of the O V] + N V inter- line_19: val should yield peak S/N> 10:1 at both 1218 and 1238, while a 0.5H exposure of line_20: the C IV interval should yield a peak S/N= 20 at the 1548 component. Peak S/N line_21: ratios (per diode, smoothed over the substeps) in the range 10-20 are required line_22: to provide accuracies in the line centroids compatible with the precision of line_23: the wavelength scale assignments. ! question: 5 section: 1 line_1: **IMPORTANT NOTE**: If Beta Hyi is observed in the Continuous Viewing Zone, the line_2: total S/C time (item 10a, Cover Page) will decrease by about 1.1H, and the pro- line_3: gram efficiency (item 10b) will increase from 71% to about 91%. line_5: Assurance of the precision of the wavelength scales of the medium-resolution line_6: and the high-resolution spectra is essential to the scientific objectives of line_7: our program. Thus we propose to obtain wavelength calibrations for the G160M line_8: and ECH-B20 spectra. The lamp exposures would be of order 30S, to obtain sub- line_9: km/s accuracy in the assigned wavelength scales. ! question: 6 section: 1 line_1: OSF Line Number(s) Instrument Mode Special Calibration Requirement(s) line_2: ___________________ __________ _______ __________________________________ line_4: 1.0 -- 1.3 GHRS ACCUM Lamp exposures to ensure precis- line_5: ion of wavelength scales for line_6: G160M & ECH-B20 spectra. Should line_7: achieve S/N= 10, or better, in line_8: moderate-strength Pt II lines. ! question: 7 section: 1 line_1: The analysis of the GHRS spectra will be conducted both at the P.I.'s institut- line_2: ion and at Lund Observatory in Sweden, following an initial visit by the P.I. line_3: to the STScI in Baltimore. The preliminary analysis involves the measurement line_4: of spectral features using standard fitting routines: the application to the line_5: GHRS data sets should be straightforward. We will measure the profile shapes line_6: and Doppler shifts of the Si IV and O IV] multiplets from the medium-resolut- line_7: ion spectrum; the blueshifts of discrete absorption components in the chromo- line_8: spheric cores of the Mg II h and k lines observed at echelle resolution; and line_9: the line fluxes of all measurable (i.e., statistically-significant) emissions line_10: in the low-resolution spectrum. line_12: We then will develop a dynamical picture of the subcoronal transition zone of line_13: Beta Hyi from the Doppler widths and shifts of the high-excitation Si III, line_14: Si IV, C IV, O IV], N V, & O V] emissions (which span the range 30,000-250,000 line_15: K in line-formation temperature); and attempt to connect it to the chromosph- line_16: eric layers as diagnosed by the Mg II and Lyman alpha shapes and possible blue- line_17: shifted ``wind'' components. We will utilize the line fluxes to construct a line_18: physical description of the outer atmosphere, principally through ``emission- line_19: measure'' modeling. The program will sample emissions from a wide range of ex- line_20: citation and a diversity of optical thicknesses. The available species should line_21: very tightly constrain the possible thermal structures, in contrast to the very line_22: superficial picture obtainable historically from IUE SWP-LO spectra (a major line_23: deficiency of the historical observations is the lack of sufficient spectral ! question: 7 section: 2 line_1: resolution or sensitivity to record the key density-sensitive O IV] multiplet). line_2: A clear view of the thermal structure then permits a calculation of the excess line_3: radiative losses of the gas. Because the distribution of the radiative cooling line_4: with height must balance the ``mechanical'' heating, a knowledge of the one can line_5: provide valuable insight into the (still elusive) nature of the other. line_7: A crucial aspect of the analysis will be to tie together the historical X-ray line_8: studies of Beta Hyi by EXOSAT and new results obtained from the ROSAT survey line_9: (and possibly also pointed observations). The O IV] density-diagnostic will line_10: provide the key to linking the emission measures inferred for the different line_11: energy ranges. Furthermore, the gradient of emission measure from C IV temper- line_12: atures (100,000 K) through O V] temperatures (250,000 K) should indicate unamb- line_13: iguously whether the cool-corona solutions obtained from the EXOSAT LE1/CMA de- line_14: tections are viable. ! question: 8 section: 1 line_1: N/A ! question: 9 section: 1 line_1: (a) HST program numbers and titles: line_3: 2485: ``Sleuthing the Dynamo: Cycle 1 Observations'' line_4: [peripherly related to present project: see text] line_6: 3908: ``Sleuthing the Dynamo: Cycle 2 Observations'' line_7: [peripherly related to present project: see text] line_9: (b) Summary of main results: line_11: no observations obtained to date in these programs line_13: (c) HST-related publications: line_15: ``GHRS observations of the local interstellar medium and the deuterium/hydrogen line_16: ratio along the line of sight towards Capella,'' Linsky, J. L., Brown, A., line_17: Gayley, K. G., Diplas, A., Savage, B. D., Ayres, T. R., Landsman, W., Shore, line_18: S., & Heap, S. R., Astrophysical Journal, to appear 10 Jan 1993. line_20: ``The hydrogen Lyman alpha emission of Capella'', Ayres, T. R., Brown, A., line_21: Gayley, K. G., & Linsky, J. L., Astrophysical Journal, to appear 10 Jan 1993. line_23: ``IUE far-ultraviolet spectra of Capella and Gamma Draconis for comparison to ! question: 9 section: 2 line_1: HST/GHRS GTO observations'', Ayres, T. R., in The First Year of HST Observat- line_2: ions, ed. A. L. Kinney and J. C. Blades (Baltimore: Space Telescope Science line_3: Institute), p. 216 (1991). ! question: 10 section: 1 line_1: At the University of Colorado a version of the reduction software written by line_2: the GHRS team is available on a VAXstation. A recent version of IRAF/SDAS is line_3: hosted on a DECstation and a SUN-4. We, and our students at Colorado and Lund, line_4: will conduct theoretical studies of the UV emissions from the outer atmosphere line_5: and wind of Beta Hyi using fast numerical simulation codes recently implemented line_6: on a variety of workstation platforms. ! !end of general form text general_form_address: lname: AYRES fname: THOMAS mi: R. category: PI inst: U.Colorado CASA addr_1: CNTR. ASTROPHYS. & SPACE ASTRON. addr_2: CAMPUS BOX 389 (CASA) city: BOULDER state: CO zip: 80309 country: USA phone: 303-492-4051 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD2151 name_2: BETA-HYI descr_1: A, 137, 901, 905 pos_1: RA = 0H 23M 9.374S +/- 0.03S, pos_2: DEC = -77D 32' 8.50" +/- 0.1" equinox: 1950 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 1950.00 ra_pm_val: 0.688501 dec_pm_val: 0.3270 an_prlx_val: 0.1590 an_prlx_unct: 0.0070 rv_or_z: V=+23 fluxnum_1: 1 fluxval_1: V = 2.80 +/- 0.10, TYPE = G2IV fluxnum_2: 2 fluxval_2: B-V = +0.62 +/- 0.01 fluxnum_3: 3 fluxval_3: F-LINE(1215)= 3 +/- 1 E-12 fluxnum_4: 4 fluxval_4: W-LINE(1216)= 1 +/- 0.2 fluxnum_5: 5 fluxval_5: F-LINE(2795)= 20 +/- 5 E-12 fluxnum_6: 6 fluxval_6: W-LINE(2795)= 1 +/- 0.2 fluxnum_7: 7 fluxval_7: F-LINE(1393)= 2.0 +/- 0.5 E-13 fluxnum_8: 8 fluxval_8: W-LINE(1393)= 0.25 +/- 0.05 fluxnum_9: 9 fluxval_9: F-LINE(1548)= 4.0 +/- 0.5 E-13 fluxnum_10: 10 fluxval_10: W-LINE(1548)= 0.25 +/- 0.05 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: HD2151 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 12.5S s_to_n: 35 s_to_n_time: 0.5S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: SEARCH-SIZE=5, param_2: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 1.1; req_2: CYCLE 3 / 1-5.1; req_3: GROUP 1-5.1 NO GAP; comment_1: STEP TIME = 0.5 SEC ! linenum: 1.100 targname: HD2151 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 40.0S s_to_n: 63 s_to_n_time: 1.6S fluxnum_1: 1 fluxnum_2: 2 priority: 1 req_1: ONBOARD ACQ FOR 2.0-5.1 comment_1: STEP-TIME=1.6 SEC ! linenum: 2.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B20 wavelength: 2798 num_exp: 1 time_per_exp: 27.2S s_to_n: 30 s_to_n_time: 30S priority: 1 param_1: STEP-PATT=7 req_1: CALIB FOR 2.1; req_2: SEQ 2-2.1 NO GAP ! linenum: 2.100 targname: HD2151 config: ^ opmode: ^ aperture: 0.25 sp_element: ^ wavelength: ^ num_exp: 1 time_per_exp: 1524S s_to_n: 40 s_to_n_time: 5M fluxnum_1: 5 fluxnum_2: 6 priority: ^ param_1: STEP-PATT=7 param_2: FP-SPLIT=STD ! linenum: 3.000 targname: HD2151 config: HRS opmode: IMAGE aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 128S s_to_n: 35 s_to_n_time: 0.5S fluxnum_1: 1 fluxnum_2: 2 priority: 2 comment_1: TAKE MAP AFTER CENTERING comment_2: 0.5 SEC INTEGRATIONS ! linenum: 3.100 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1403 num_exp: 1 time_per_exp: 27.2S s_to_n: 30 s_to_n_time: 30S priority: 1 param_1: STEP-PATT=5 req_1: CALIB FOR 3.2; req_2: SEQ 3-3.2 NO GAP ! linenum: 3.200 targname: HD2151 config: ^ opmode: ^ aperture: 2.0 sp_element: ^ wavelength: ^ num_exp: 3 time_per_exp: 1415S s_to_n: 20 s_to_n_time: 1H fluxnum_1: 7 fluxnum_2: 8 priority: ^ param_1: STEP-PATT=5 param_2: FP-SPLIT=STD ! linenum: 4.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1555 num_exp: 1 time_per_exp: 27.2S s_to_n: 30 s_to_n_time: 30S priority: 2 param_1: STEP-PATT=5 req_1: CALIB FOR 4.1; req_2: SEQ 4-4.1 NO GAP ! linenum: 4.100 targname: HD2151 config: ^ opmode: ^ aperture: 2.0 sp_element: ^ wavelength: ^ num_exp: 2 time_per_exp: 1306S s_to_n: 25 s_to_n_time: 1H fluxnum_1: 9 fluxnum_2: 10 priority: ^ param_1: STEP-PATT=5 param_2: FP-SPLIT=STD ! linenum: 5.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1223 num_exp: 1 time_per_exp: 27.2S s_to_n: 30 s_to_n_time: 30S priority: 3 param_1: STEP-PATT=5 req_1: CALIB FOR 5.1; req_2: SEQ 5-5.1 NO GAP ! linenum: 5.100 targname: HD2151 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1223 num_exp: 2 time_per_exp: 1850S s_to_n: 57 s_to_n_time: 1H fluxnum_1: 3 fluxnum_2: 4 priority: ^ param_1: STEP-PATT=5 param_2: FP-SPLIT=STD ! ! end of exposure logsheet ! No scan data records found