0 Assigned ID: 666 ----- Attempting Submission 1 (Fri Apr 11 18:37:46 GMT 2014) ----- HST Phase I Proposal 666 (HST22_16Cyg4.pdf.apt) successfully submitted. ------New Comment------ The acquisition strategy now uses the 2676 central wavelengths setting, in accord with the technical review of our proposal. All exposure times and ETC numbers have been updated. ------Old Comment------ It appears that the BOT assumes our two GV stars, Cyg A & B, are O5V types by default, thereby giving erroneously high (worst case) flux warnings. We have checked, and there doesn't appear to be any other objects, other than our program stars, within the field. IUE SWP spectra exist for both objects (SWP05589LS and SWP16477LL), and show no inordinate amounts of FUV flux for either object. -1770654912 ----- Attempting Submission 1 (Wed Jul 23 22:01:55 GMT 2014) ----- HST Phase II Proposal 13861 (HST22_16Cyg4.pdf.apt) successfully submitted. ----- Attempting Submission 2 (Thu Jul 24 18:58:55 GMT 2014) ----- ----- Attempting Submission 3 (Thu Nov 06 20:56:18 GMT 2014) ----- The fortuitous location of the wide G1.5V/G2.5V binary 16 Cyg A&B as the brightest stars in the Kepler Field is a "game changer," permitting the determination of the stars' fundamental properties from asteroseismolgy analyses. Recent studies returned precise determinations of the stars' basic properties including masses and age (6.8+/-0.4 Gyr), along with the rotation periods. Thus, 16 Cyg A&B are now the oldest solar-mass analogs with reliable ages and physical properties. Only the Sun has better determined physical properties. 16 Cyg A&B now serve as old-age anchors for Rotation-Age-Activity-Irradiance relations (and Gyrochronology studies) for solar-type stars. Extensive Ca II HK spectrophotometry reveals low levels of chromospheric emission are below the lowest values for our Sun. These stars serve as critical test beds for studying solar/stellar dynamos for stars less active than the Sun. These advances have catapulted 16 Cyg A&B into a prominent place in solar/stellar astrophysics for studying the evolution, internal structure, magnetic dynamos, angular momentum loss, and FUV irradiances of old solar-mass stars. Although 16 Cyg has been observed from X-ray - IR, there are no observations in the FUV region where most of the crucial diagnostic chromospheric & transition region emissions occur. We request COS FUV medium resolution (G130M, G160M) spectra (six orbits/star). This permits the important FUV (1150-1750A) line emission strengths, profiles and Doppler shifts to be analyzed and compared with the Sun and other solar-analogs. This program is complemented by Ca II HK, high precision uvby observations, and by proposed Chandra X-ray coronal observations. We propose HST/COS FUV 1150-1750A observations of 16 Cyg A&B (six HST orbits per star) to secure good signal/noise (S/N) medium resolution G130M and G160M spectrophotometry. We plan to use the Primary Science Aperture (PSA). Accounting for acquisitions, overheads and utilizing the "re-acquire" between orbits, this request will result in ~5.1 ksec (over 3 orbits) per G130M and G160M elements. We used our previous HST/COS FUV spectra of the solar twin 18 Sco (G2 V; V = 5.50 mag; d = 13.90 pc; age = 3.9 +/- 0.5 Gyr) and archival COS FUV spectra of alpha Cen A (G2 V; V = -0.01; d = 1.34 pc; age = 4.9 +/- 0.7 Gyr) to estimate exposure times and signal-to-noise (S/N) values for the important FUV emissions. We scaled these fluxes (via the inverse square law) to the distance of 16 Cyg A&B (d = 21.10 pc). Also, because 16 Cyg A&B are older, and from lower Ca II H&K emissions, we assumed that their FUV line fluxes could be ~60-75% lower. Our calculations show that 3 consecutive HST orbits with the G130M and G160M elements are required for each star. These exposures will result in S/N (~5-10) for the moderate-to-strong emission lines. The resulting FUV spectra will be suitable for securing reliable integrated emission line fluxes needed to carry out spectral diagnostics from emission line ratios, performing a Volume Emission Measure (VEM) analyses, as well as modeling the line profiles. Importantly, the simulations indicate that the resulting COS/FUV spectra will permit some of the weaker, but important, diagnostic line emissions to be measured and used to determine the physical properties of the stars' chromospheres and transition regions. These spectra will be compared with comparable FUV spectra available for the Sun from solar FUV/UV space missions such as SOLSTICE (SORCE). Also we plan direct differential comparisons with the HST/STIS or COS FUV spectra of alpha Cen A and 18 Sco. COOL STARS Default false true false false false SUPPORTED STAR G V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. HD186408 J2000 J2000 G1.5V STAR G V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. HD186427 J2000 J2000 G3V COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G160M 1577 C:\Users\Scott\AppData\Local\Temp\OPVisit7068457672513331707.xml 1415307108296 The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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