For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.0Assigned ID: 3906
----- Attempting Submission 1 (Thu Mar 30 13:30:09 GMT 2023) -----
HST Phase I Proposal 3906 successfully submitted.
Receipt: # 3906-1
----- Attempting Submission 2 (Thu Apr 06 13:23:32 GMT 2023) -----
HST Phase I Proposal 3906 successfully submitted.
Receipt: # 3906-2
----- Attempting Submission 3 (Tue May 09 02:43:55 GMT 2023) -----
HST Phase I Proposal 3906 successfully submitted.
Receipt: # 3906-3
----- Attempting Submission 4 (Thu May 11 18:43:41 GMT 2023) -----
HST Phase I Proposal 3906 successfully submitted.
Receipt: # 3906-4
----- Attempting Submission 5 (Tue May 23 22:18:50 GMT 2023) -----
HST Phase I Proposal 3906 successfully submitted.
Receipt: # 3906-5The warnings concern use of COS G160M. The proposal discusses the approved use of G160M at
LP4, instead of high-overhead LP6, because each visit is only one orbit in duration.For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.G160M exposure times revised according to APT2023.5.1
More detail added to NUV-ACQ exposure Comments
Visit 14 NUV-ACQ changed to MirrA+BOA
COS.ta number added to Visit 14505988986----- Attempting Submission 1 (Mon Aug 21 21:31:57 GMT 2023) -----
HST Phase II Proposal 17453 successfully submitted.
Receipt: # 17453-1
----- Attempting Submission 2 (Fri Aug 25 17:12:32 GMT 2023) -----
HST Phase II Proposal 17453 successfully submitted.
Receipt: # 17453-2
----- Attempting Submission 3 (Sat Aug 26 16:55:17 GMT 2023) -----
----- Attempting Submission 4 (Tue Jan 23 04:35:18 GMT 2024) -----
----- Attempting Submission 5 (Tue Jan 23 14:46:27 GMT 2024) -----The warnings are for the use of 2 FP-POS splits for each exposure instead of the default 4.
This is justified because the target FUV spectra are faint, and would not benefit from the
fixed-pattern mitigation delivered by the 4 FP-POS steps; but would benefit from the extra 25%
exposure time achived with the 2-split sequence.Activity at the EdgeA central goal of cool-star astronomy is to link the high-energy FUV+X-ray ("XUV") luminosity -- which among other things can affect the local stellar environs, especially orbiting exoplanets -- to properties of the "dynamo" that controls the generation of magnetic flux deep inside spinning, convective stars. In the 1980s it was discovered that the ratio of the stellar rotation period to a convective turnover time could unify the behavior of Ca II HK chromospheric fluxes broadly over the FGK spectral types. This "Rossby number" plays a fundamental role in terrestrial and stellar dynamo theories, so the unification was promising. A more recent attempt to achieve a similar synthesis at high energies, more closely connected to concentrated surface magnetic activity, met with some success for the early- to mid-G types, but theoretical convective turnover times showed a sharper drop in the early-F types than empirical estimates. That "edge" occurs where stellar convection zones are rapidly thinning toward the warmer spectral types, a challenge to theory. Unfortunately, the existing sample of empirical turnover times has a conspicuous gap in the F types, so the intermediate behavior is unknown. This gap can be filled by new HST/COS FUV (and Chandra X-ray) observations of 17 carefully selected F5-G1 dwarfs in the nearby Pleiades cluster; which have accurate photometric rotation periods, common age and similar composition. Validation of the Rossby framework with this unique stellar cohort not only could strengthen the theory; but also ultimately allow "one-stop shopping" to estimate XUV luminosities of cool stars beyond the range of current high-energy space observatories.To test whether the Rossby formalism can successfully bridge the F/G break illustrated in the original proposal, one needs a collection of single dwarf stars that have similar fundamental properties, such as age and chemical composition; and differ mainly in surface temperature, which controls the convective properties and thus the turnover time. (The restriction to dwarfs aligns with the better developed state of solar dynamo theories.) The stars should have well determined rotation periods, ideally photometric (avoiding the orientation ambiguity of spectroscopic velocities); and be accessible in both the FUV and X-rays, to construct the crucial XUV metric. Such homogenous stellar samples can be found in galactic clusters. The Pleiades, in particular, is close enough (136 pc) to have F and G dwarfs that can be captured by HST in the FUV and Chandra (or XMM-Newton) at X-ray energies. (The Hyades cluster would be another option, but there are too few suitable F to early-G candidates. The Hyades, nevertheless, is a better for the fainter, cool K dwarfs, the subject of a related joint Chandra/HST Rossby project.) Further, uniformly measured photometric rotational periods, from the ground and space, are available for many of the Pleiades dwarfs; while Gaia DR3 provides accurate distances, colors, broad-band visual magnitudes, and radial velocities (RV). Variances of the Gaia RVs over the numerous sky scans can reveal spectroscopic binaries. After careful consideration of potential candidates from a recent Pleiades survey catalog, 17 were found suitable. These late-type dwarfs have PROT= 1.8-3.8 d, and appear to be single by virtue of H-R diagram position and small Gaia RV dispersions.
As alluded previously, the principal stellar activity metric to compare to the Rossby number is the "XUV hybrid flux," intended to document the main radiative losses of the magnetically energized outer atmosphere; a proxy related to the delivery rate of concentrated magnetic flux into the stellar surface layers (ultimately connected to the dynamo itself). The FUV not only contributes specific bright emission lines -- from species like C III, Si III, N V, Si IV, and C IV -- but also provides surrogates for contributions by the important, but unseen, EUV features, such as He II 30 nm (scales with C IV 155 nm) and C III 97 nm (scales with C III 117 nm). Consequently, FUV spectra are a crucial piece of the combined XUV flux.
Cosmic Origins Spectrograph was specifically designed for FUV spectroscopy of faint objects. COS can achieve full-coverage FUV spectra of late-type stars (i.e., C III 117 nm to He II 164 nm) by combining two medium-resolution settings, G130M-1222 and G160M-1533 (low-resolution grating COS G140L misses important Si III 120 nm and N V 123+124 nm). The G130M-1222 detector gap excludes H I 121 nm Ly-alpha, so there are no safety concerns. This simple combination is optimum for the faint Pleiades dwarfs. The two COS CENWAVEs can be accommodated in a single orbit per star. The NUV imaging target acquisition is appropriate for the Pleiades V-magnitude range. Time-Tag is the default exposure mode, and is helpful to identify any transient flare events (expected to be rare).
The NUV imaging target acquisition can be done with Mirror-A and the BOA for targets 1-12, with exposures of 13-24 s. The fainter, cooler targets 13-17 can be done with Mirror-B and the PSA, with an exposure of 2 s.
In one orbit, accounting for overheads, about 1 ks of exposure is available for each CENWAVE (2 ks total in the overlap between them).
These targets are faint in the FUV, so it is advantageous to utilize only 2 of the 4 FP-POS splits for each setting. FP-POS 1+2 are used with M-1222 to capture Si III 120 nm; FP-POS 3+4 are used with M-1533 to fully capture the Fe II 134 nm + Fe XXI 135 nm region. Restricting the FP-POSs yields 25% more exposure time: the S/N will not be high enough to make best use of the fixed-pattern mitigation delivered by the full complement of FP-POS splits.
The M-1533 exposures can be done at Lifetime Position 4 (instead of LP6 with its high-overhead lamp-flash calibrations) because the duration of each visit is a single orbit.PI Ayres has extensive experience with HST, especially the UV spectrographs, dating back to the launch of Hubble. He has carried out many HST programs, mostly concerning high-energy stellar phenomena, and has published numerous papers on HST data.Stellar Physics and Stellar Types6falsefalsetruefalsefalsefalsefalsetruePRIMARY104trueAVAILABLESTARF3-F9NOJ2000J2000F5V (from Teff=6415), (BP-RP)=0.679, G=9.53, RV=5.5+/-0.5 kps, Prot=1.9 dSTARF3-F9NOJ2000J2000F5V (from Teff=6400), (BP-RP)=0.684, G=9.57, RV=6.5+/-0.6 kps, Prot=1.8 d, fX=1.0e-13STARF3-F9NOJ2000J2000F6V (from Teff=6335), (BP-RP)=0.701, G=9.73, RV=5.3+/-0.4 kps, Prot=2.8 dSTARF3-F9NOJ2000J2000F6V (from Teff=6325), (BP-RP)=0.706, G=9.72, RV=4.3+/-0.7 kps, Prot=1.9 d, fX=1.7e-13STARF3-F9NOJ2000J2000F6V (from Teff=6325), (BP-RP)=0.708, G=9.76, RV=5.6+/-0.3 kps, Prot=2.8 d, fX=0.8e-13STARF3-F9NOJ2000J2000F6V (from Teff=6310), (BP-RP)=0.711, G=9.71, RV=7.0+/-0.5 kps, Prot=2.4 dSTARF3-F9NOJ2000J2000F7V (from Teff=6230), (BP-RP)=0.734, G=9.90, RV=4.8+/-0.4 kps, Prot=2.5 dSTARF3-F9NOJ2000J2000F8V (from Teff=6220), (BP-RP)=0.740, G=9.99, RV=6.5+/-0.4 kps, Prot=2.5 d, fX=0.6e-13STARF3-F9NOJ2000J2000F8V (from Teff=6205), (BP-RP)=0.744, G=9.94, RV=6.8+/-0.8 kps, Prot=2.1 d, fX=1.5e-13STARF3-F9NOJ2000J2000F8V (from Teff=6200), (BP-RP)=0.748, G=9.85, RV=7.3+/-0.3 kps, Prot=2.9 dSTARF3-F9NOJ2000J2000F9V (from Teff=6090 ), (BP-RP)=0.779, G=10.14, RV=6.6+/-0.6 kps, Prot=2.2 dSTARF3-F9NOV mag from Gaia G: V= G + 0.2J2000J2000F9V (from Teff=6090), (BP-RP)=0.780, G=10.16, RV=4.6+/-0.6 kps, Prot=2.2 d, fX=0.7e-13STARG V-IVNOV mag from Gaia G: V= G + 0.2J2000J2000G0V (from Teff=6060), (BP-RP)=0.790, G=10.21, RV=6.5+/-0.5 kps, Prot=2.9 d, fX=1.1e-13STARG V-IVNOJ2000J2000G0V (from Teff=6030), (BP-RP)=0.796, G=10.00, RV=5.8+/-0.4 kps, Prot=2.9 d, fX=1.5e-13STARG V-IVNOV mag from Gaia G: V= G + 0.2 (SIMBAD V=12.1 apparently in error)J2000J2000G0V (from Teff=6030), (BP-RP)=0.798, G=10.25, RV=5.7+/-0.4 kps, Prot=3.8 d, fX=0.6e-13STARG V-IVNOJ2000J2000G1V (from Teff=5980), (BP-RP)=0.815, G=10.39, RV=5.7+/-0.3 kps, Prot=3.6 d, fX=0.6e-13STARG V-IVNOV mag from Gaia G: V= G + 0.2J2000J2000G1V (from Teff=5960), (BP-RP)=0.821, G=10.30, RV=6.6+/-0.5 kps, Prot=3.2 d, fX=0.9e-13COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1533The scheduling data was generated by CASM 32.0.CASM was run in Phase II mode.170911621900076.91124456077182(Tic-Visit
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