!========================================================================== ! 19-January-1996 ! ! Hi Dustin: ! ! ! ! Here is the revised Phase II for 6066, optimized as best I could ! ! within the various constraints. The new observing strategy is ! ! described in ``Observing_Description'' under the ``Questions'' ! ! section, below. If you have any questions/comments please ! ! contact me. I'll be assembling the Phase II's for my Cyc-6 programs ! ! over the next week, so you'll undoubtedly be hearing from me again! ! ! ! ! best regards, ! ! ! ! Tom ! ! ! !========================================================================== ! ! +====================+ ! | PED OUTPUT PRODUCT | ! +====================+ ! ! /home3/casa/ayres/6066.prop ! Generated by PREPROCESSOR, version 6.0e ! Date: Thu Jan 18 15:25:36 MST 1996 Proposal_Information Title: Distant Futures of Solar Activity Proposal_Category: GO Scientific_Category: Cool Stars Cycle: 5 Investigators PI_Name: Thomas Ayres PI_Institution: University of Colorado CASA CoI_Name: Dainis Dravins CoI_Institution: Lund Observatory Contact: CoI_Name: Philip Judge CoI_Institution: High Altitude Observatory Contact: CoI_Name: Kenneth Carpenter CoI_Institution: NASA/Goddard Space Flight Center Contact: CoI_Name: Richard Robinson CoI_Institution: Computer Sciences Corp. Contact: CoI_Name: Alex Brown CoI_Institution: University of Colorado JILA Contact: CoI_Name: Graham Harper CoI_Institution: University of Colorado JILA Contact: CoI_Name: Philip Bennett CoI_Institution: University of Colorado JILA Contact: CoI_Name: Jeffrey Linsky CoI_Institution: University of Colorado JILA & NIST Contact: Abstract: We will explore possible future fates of solar magnetic activity through high-S/N GHRS spectra of the ancient Sun analog, Arcturus (K1 III). The fundamental mechanisms that drive the hot (T>10^6 K) coronae of cool stars remain elusive. Solving the mystery is a central theme of the ``solar-stellar connection;'' whose importance extends beyond astronomy to areas ranging from basic plasma physics to solar-terrestrial relations. A significant property of the activity is that it subsides with age: G dwarfs in young clusters are intense coronal sources, whereas old low mass K giants are so feable in soft X-rays that most are below current detection limits. For that reason, historical studies of activity have been biased towards the younger stars. Now the HST/GHRS easily can record faint coronal proxies (like Si IV and C IV) in nearby cool subgiants and giants, thereby mitigating the de facto age discrimination. In the solar neighborhood the brightest single star of advanced age (9--11 Gyr) is Alpha Bootis (K1 III). Previous studies have placed the archetype red giant firmly in the ``coronal graveyard.'' Our project focuses on understanding the ``basal'' chromosphere; molecular cooling catastrophes and the structure of the passive ``COmosphere;'' the dynamics and energy balance of the residual subcoronal gas; and mass loss mechanisms. (Secondary target Beta Hydri was eliminated owing to reduced TAC orbit allocation.) Questions Observing_Description: -------------------------------------- !!! NOTE: !!! NEW Phase II (Jan-1996) version: -------------------------------------- (revised owing to A2 ACQ to avoid Digicon saturation) ====================================================== Our observational goal is the detailed mapping of key intervals in the UV spectrum of Arcturus, as follows: ID mode W0 texp NOTES ======================================================================== * Acquire on Side 2 (Mirror A2) in LSA; then ACQ/Peakup in ssa A0 ECH-B/ssa 2800 5M (similar to orig.) A1 --eliminated-- A2 ECH-B/ssa 2328 7M (similar to orig.) B0 --eliminated B1 G200M/ssa 1900 25M (LSA=>ssa, to stay in ssa) * Side 2 => Side 1 B3 G140M/ssa 1213 13M (G160M=>G140M, shorter exp. than orig. B3) C1 G140M/ssa 1307 11M (similar to orig.) D2 G140L/ssa 1464 18M (single lambda setting replaced with 400 A WSCAN) B2 G140M/LSA 1388 25M (G160M=>G140M, and placed at end of sequence so only one ssa=>LSA ap. maneuver) ------------------------------------------------------------------------ Owing to the change in acquisition strategy---and the attendant increase of 20 minutes in the overhead---we have reorganized the program somewhat, eliminating two exposures; shifting some of the previous Side 2 exposures to the equivalent disperser on Side 1; switching the one remaining medium-res Side 2 observation from LSA to ssa (to avoid having to return to the ssa later); and using a G140L WSCAN to recover some of the lost spectral territory. ---------------------------------------- !!!! NOTE: !!! Original Phase II (pre-1996) version: ---------------------------------------- ID mode W0 texp NOTES ======================================================================== * Acquire on Side 2 (Mirror N2) in LSA; then ACQ/Peakup in ssa A0 ECH-B/ssa 2800 4M (Mg II: same as orig. B3) A1 ECH-B/ssa 2356 4M (Si II]: shorter than orig. B1) A2 ECH-B/ssa 2329 5M (C II]: same as orig. B0) B0 G270M/ssa 2833 4M (Mg I: replaces orig. ECH-B exp. B4) B1 G200M/LSA 1900 16M (Si III], S I: replaces orig. G160M exp. C5) B2 G160M/LSA 1392 22M (Si IV, CO: shorter than orig. C1) B3 G160M/ssa 1222 22M (H I, Si III, O V], N V: replaces orig. ECH-A exp. A0) * Side 2 => Side 1 C1 G140M/ssa 1305 13M (O I, S I: replaces orig. ECH-A exp. A1) D2 G140L/ssa 1469 18M (C II; C IV, CO; etc.: replaces orig. G160H/LSA exps.: C0,C2,C3) ------------------------------------------------------------------------ Owing to the reduction in allocated observing time from that requested (13 orbits => 4 orbits), we dropped our second priority target (Beta Hyi) entirely, and heavily modified our original observing plan. In particular, we replaced two deep ECH-A exposures with shorter integrations using medium resolution gratings and the ssa. Post-COSTAR observations with G160M/ssa have shown that the resolving power is adequate to measure the important ISM deuterium absorption, and narrow wind features; G140M/ssa should produce even higher resolution than G160M. (Specifically for the O I 1305 multiplet where narrow wind/ISM features are evident in the spectrum of Gamma Dra.) In addition, we eliminated 2 ECH-B exposures in the 2000-3000 A region, replacing one with shorter but broader-bandpass integration with G270M/ssa. Finally, we substituted a 287-A G140L/ssa exposure (1325-1612) for several G160M integrations, trading for the broad spectral coverage at high sensitivity against the higher resolution, but longer exposures and narrower coverage of G160M. Our substitutions are geared towards preserving as much of our original scientific program on Arcturus as possible, in the face of the much reduced orbit allocation. Real_Time_Justification: Calibration_Justification: Additional_Comments: Fixed_Targets Target_Number: 1 Target_Name: HD124897 Alternate_Names: ALPHA-BOO,ARCTURUS Description: STAR, K III-I, Corona, Wind Position: RA=14H 15M 39.68S +/- 0.05S,DEC=19D 10' 56.7" +/- 1" Equinox: 2000 RV_or_Z: V = -5 RA_PM: -0.0772 Dec_PM: -1.998 Epoch: 2000 Annual_Parallax: 0.097 Flux: V = -0.04+/-0.1 B-V = +1.23+/-0.1 TYPE=K1III Comments: Solar_System_Targets Generic_Targets Scan_Data Visits Visit_Number: 01 Visit_Requirements: On_Hold_Comments: Visit_Comments: Exposure_Number: 1 Target_Name: HD124897 Config: HRS Opmode: ACQ Aperture: 2.0 Sp_Element: MIRROR-A2 Wavelength: Optional_Parameters: BRIGHT=RETURN,SEARCH-SIZE=3 Number_of_Iterations: 1 Time_Per_Exposure: 9.0S Special_Requirements: ONBOARD ACQ FOR 2 Comments: STEP-TIME = 1.0 SEC (Approx. 5000 cts in STEP-TIME) Exposure_Number: 2 Target_Name: HD124897 Config: HRS Opmode: ACQ/PEAKUP Aperture: 0.25 Sp_Element: MIRROR-A2 Wavelength: Optional_Parameters: SEARCH-SIZE=5 Number_of_Iterations: 1 Time_Per_Exposure: 45S Special_Requirements: ONBOARD ACQ FOR 11-90 Comments: STEP-TIME = 1.8 SEC (Approx. 5000 cts in STEP-TIME) Exposure_Number: 11 Target_Name: HD124897 Config: HRS Opmode: ACCUM Aperture: 0.25 Sp_Element: ECH-B20 Wavelength: 2799 Optional_Parameters: COMB=FOUR,STEP-PATT=DEF,DOPPLER=DEF,FP-SPLIT=STD Number_of_Iterations: 1 Time_Per_Exposure: 326.4S Special_Requirements: Comments: Exposure_Number: 12 Target_Name: HD124897 Config: HRS Opmode: ACCUM Aperture: 0.25 Sp_Element: ECH-B24 Wavelength: 2328 Optional_Parameters: COMB=FOUR,STEP-PATT=DEF,DOPPLER=DEF,FP-SPLIT=STD Number_of_Iterations: 1 Time_Per_Exposure: 435.2S Special_Requirements: Comments: Exposure_Number: 41 Target_Name: HD124897 Config: HRS Opmode: ACCUM Aperture: 0.25 Sp_Element: G200M Wavelength: 1900 Optional_Parameters: COMB=FOUR,STEP-PATT=DEF,DOPPLER=DEF,FP-SPLIT=STD Number_of_Iterations: 1 Time_Per_Exposure: 1523.2S Special_Requirements: Comments: Exposure_Number: 61 Target_Name: HD124897 Config: HRS Opmode: ACCUM Aperture: 0.25 Sp_Element: G140M Wavelength: 1213 Optional_Parameters: COMB=FOUR,STEP-PATT=DEF,DOPPLER=DEF,FP-SPLIT=STD Number_of_Iterations: 1 Time_Per_Exposure: 761.6S Special_Requirements: Comments: Exposure_Number: 71 Target_Name: HD124897 Config: HRS Opmode: ACCUM Aperture: 0.25 Sp_Element: G140M Wavelength: 1307 Optional_Parameters: COMB=FOUR,STEP-PATT=DEF,DOPPLER=DEF,FP-SPLIT=STD Number_of_Iterations: 1 Time_Per_Exposure: 652.8S Special_Requirements: Comments: Exposure_Number: 80 Target_Name: HD124897 Config: HRS Opmode: WSCAN Aperture: 0.25 Sp_Element: G140L Wavelength: 1256-1672 Optional_Parameters: COMB=FOUR,STEP-PATT=DEF,DOPPLER=DEF,FP-SPLIT=NO, WAVE-STEP=104 Number_of_Iterations: 1 Time_Per_Exposure: 1088.0S Special_Requirements: Comments: Exposure_Number: 90 Target_Name: HD124897 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140M Wavelength: 1388 Optional_Parameters: COMB=FOUR,STEP-PATT=DEF,DOPPLER=DEF,FP-SPLIT=STD Number_of_Iterations: 1 Time_Per_Exposure: 1523.2S Special_Requirements: Comments: Data_Distribution ! Defaults indicated; change if desired Medium: 8MM Blocking_Factor: 10 Ship_To: PI_Address Ship_Via: UPS Recipient_Email: ! Let us know what you think of this template and software! ! Please send a list of your likes and dislikes to your Program Coordinator