0Assigned ID: 1087
----- Attempting Submission 1 (Fri Apr 07 23:11:31 GMT 2017) -----
HST Phase I Proposal 1087 (hyades.apt) failed submission.
----- Attempting Submission 2 (Fri Apr 07 23:11:52 GMT 2017) -----
HST Phase I Proposal 1087 (hyades.apt) failed submission.
----- Attempting Submission 3 (Fri Apr 07 23:12:28 GMT 2017) -----
HST Phase I Proposal 1087 (hyades.apt) failed submission.
----- Attempting Submission 4 (Fri Apr 07 23:13:00 GMT 2017) -----
HST Phase I Proposal 1087 (hyades.apt) failed submission.
----- Attempting Submission 5 (Fri Apr 07 23:13:54 GMT 2017) -----
HST Phase I Proposal 1087 (hyades.apt) failed submission.
----- Attempting Submission 6 (Fri Apr 07 23:14:53 GMT 2017) -----
HST Phase I Proposal 1087 (hyades.apt) failed submission.
----- Attempting Submission 7 (Fri Apr 07 23:15:56 GMT 2017) -----
HST Phase I Proposal 1087 (hyades.apt) failed submission.
----- Attempting Submission 8 (Fri Apr 07 23:16:35 GMT 2017) -----
HST Phase I Proposal 1087 (hyades.apt) failed submission.
----- Attempting Submission 9 (Fri Apr 07 23:20:36 GMT 2017) -----
HST Phase I Proposal 1087 (hyades.apt) failed submission.
----- Attempting Submission 10 (Fri Apr 07 23:23:45 GMT 2017) -----
HST Phase I Proposal 1087 (hyades.apt) failed submission.
----- Attempting Submission 11 (Fri Apr 07 23:28:13 GMT 2017) -----As instructed, to repeat a failed orbit in visit 2, we have duplicated the visit and numbered it 52. We implemented the same, more efficient ACQ setup for this target as for the other ones, as suggested by John Debes, and adjusted the calculation of the required exposure in consequence. Furthermore, only one orbit is included in this visit, since one orbit of visit 2 was successful.
Positions and proper motions have been updated to reflect Gaia DR2 (with one exception, where Gaia data are not available and we use AllWISE results). In addtion, V magnitudes have been updated in a handful of cases to reflect SIMBAD values (targets 11, 12, 15), and the relevant acquisitions have been updated as well.
We have duplicated visits 1, 8, and 16, numbered as 51, 58, and 66, respectively, to repeat failed visits. Target 8 was duplicated as target 18 so that the proper motions could be updated to the Gaia DR2 values for this star, which were not available previously.-437193557----- Attempting Submission 1 (Fri Jul 21 20:00:28 GMT 2017) -----
HST Phase II Proposal 15090 (phaseII.apt) successfully submitted.
Receipt: # 15090-1
----- Attempting Submission 2 (Tue Oct 17 19:53:29 GMT 2017) -----
HST Phase II Proposal 15090 (go_phaseII_redo.apt) successfully submitted.
Receipt: # 15090-2
----- Attempting Submission 3 (Sun Dec 24 03:52:21 GMT 2017) -----
----- Attempting Submission 5 (Fri Sep 14 15:48:05 GMT 2018) -----
HST Phase II Proposal 15090 (phaseII_planned_obs.apt.2018_09_14_15_45.aptbackup) successfully submitted.
Receipt: # 15090-5
----- Attempting Submission 6 (Fri Sep 21 16:57:08 GMT 2018) -----
HST Phase II Proposal 15090 (phaseII_updated_sep_2018.apt) successfully submitted.
Receipt: # 15090-6
----- Attempting Submission 7 (Thu Nov 01 15:09:50 GMT 2018) -----
----- Attempting Submission 8 (Wed Dec 19 20:43:26 GMT 2018) -----
----- Attempting Submission 9 (Fri Mar 29 14:11:25 GMT 2019) -----A UV spectroscopic survey of periodic M dwarfs in the HyadesBecause of its proximity, the 650-Myr-old Hyades open cluster is a unique resource for exploring the relationship between magnetic activity, rotation, and age in low-mass stars. While the cluster has been largely ignored in UV studies of the dependence of activity on rotation, we now have an extensive and growing set of complementary rotation period, Halpha, and X-ray measurements with which to examine in detail the rotation-activity relation at 650 Myr and to constrain theories of magnetic heating. We propose to measure Mg II line emission, the strongest NUV activity tracer, in COS spectra of 17 Hyads ranging in spectral type from M0 to M7 with known rotation periods and Halpha and X-ray measurements. These stars form a representative sample of M-dwarf Hyads with known periods and are a significant addition to, and expansion of, the sample of 20 mainly solar-mass rotators with existing (mostly low-resolution) International Ultravioled Explorer (IUE) NUV spectra. The Mg II measurements will contribute significantly to our goal of mapping out the rotation-activity relation star-by-star in this benchmark open cluster. This, in turn, will move us toward an improved understanding of the radiation environment and habitability of the exoplanets we continue to find around low-mass stars.Our focus is on completely characterizing the low-mass Hyads for which we have a measured rotation period and Halpha and X-ray data, a total of 75 <1.1 Msun stars. Twenty of these stars have existing IUE spectra, and we are therefore left with 55 stars for which we require HST NUV spectroscopy.
To compute the exposure times for these targets, we need to select an input spectral energy distribution and magnitude. For G stars, we use the default Bruzual synthetic stellar spectra provided by the COS ETC. For K1 to M5 stars, we input MUSCLES SEDs into the ETC, since these are based in part on HST UV spectra (Loyd et al. 2016), and model spectra for these stars are known to underestimate the chromospheric contribution to the UV.
Twenty-nine of our targets have GALEX NUV magnitudes, and we use these to compute the exposure times for these stars. For the remaining 26 stars, we use the 356 Hyades members with GALEX NUV detections to estimate average absolute NUV magnitudes as a function of spectral type. We then find the NUV magnitude for the spectral type appropriate for each target, and use the distances to each to convert these to apparent NUV magnitudes, thereby accounting for the depth of the cluster. Comparisons between the NUV magnitudes obtained in this way for the 29 targets that have to the GALEX NUV magnitudes indicate that the estimated NUV magnitudes are reasonable. For the solar-mass stars, our estimated magnitudes are systematically too bright by ~0.5 magnitudes, while for the early M dwarfs our estimates are too conservative by roughly the same amount. For the latest-type stars, our estimated NUV magnitudes are again too bright, and to be conservative we therefore add a 0.5 magnitude to the NUV magnitudes we derive to calculate their exposure times.
The results of this procedure warrant a two-pronged approach: for 36 of our targets, the required times are more appropriate for a snapshot program, and we are proposing for those separately. For 19 M0-M7 targets, however, the required exposures correspond to at least one HST orbit, and 17 of those targets are proposed here. Two of the M5 stars in our sample require exposures much greater than four orbits, and we remove those from our sample, which includes five other M5 stars.
To finalize our observing strategy, we followed Instrument Science Report COS 2017-01 to assess the safety of observing our M-dwarf targets. This is a multiple-step process: first, we obtained a spectral type for our targets. For most stars this was done directly from our MDM spectra; for others we converted absolute K magnitudes into spectral types, following the relations laid out in Kraus & Hillenbrand (2007). These spectral types were converted into (U-V) colors using the data presented in Pecaut & Mamajek (2013). We then searched the literature for V magnitudes for our targets; for stars lacking a V in the literature, we computed one from e.g., Sloan Digital Sky Survey (g-r) colors. We combined these V magnitudes with the (U-V) color to obtain the U magnitudes needed to characterize the potential impact of flares on our observations. Our comparisons of these U magnitudes to those in the literature for our targets that have U-band measurements indicate that our derived U magnitudes have uncertainties ~0.3-0.5 magnitudes.
Finally, we used our MDM spectra to determine whether, based on their measured Halpha EqWs, our targets are magnetically active. This sets the maximum U-band magnitude increases (Delta U) of the brightest flare that would occur with a probability of 10^-4. We then computed U_{flare} = U_{quiescent} + Delta U and determined global and local count rates for a flare of this magnitude using COS ETC calculations for the NUV. All of our targets are well below the count-rate limits for the COS photon-counting detectors.
Our instrumental set-up is as follows: we wish to observe our targets using COS in low-resolution mode with the G230L grating. Centered at 2950 A, the resulting spectra will cover the Mg II h and k lines, which are the strongest NUV tracers of magnetic activity. We set up the exposure in ACQ/IMAGE mode, requesting S/N = 40 in the COST ETC. We use TIME-TAG mode for the actual observation of each target and set FP-POS = 4. We note that four of the visits we arrange have durations of four orbits each, beyond the suggested two-three orbit maximum. These objects are very faint; spliting four orbits into two visits would reduce the exposure time (and thus the maximum S/N) we can reach. Therefore, we request to observe each of our targets in single visit. The exposure times we calculate insure that we have a S/N > 10 in the Mg II lines, which based on the IUE spectra is what is requred to measure these lines confidently, and a S/N ~ 3-8 for the nearby continuum, based on the MUSCLES SEDs.Stellar Physics6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTARM V-IVNOPositions and proper motions updated to Gaia DR2 values.LP416-570J2000J200020.950(GALEX)STARM V-IVNOGJ3278J2000J200020.990(GALEX)STARM V-IVNOPositions and proper motions updated to Gaia DR2 values.LP415-794J2000J200020.708(Derived)STARM V-IVNOPositions and proper motions updated to Gaia DR2 values.LP415-543J2000J200021.411386311STARM V-IVNOSIMBAD gives V=14.47EPIC210470484J2000J200021.388(Derived)STARM V-IVNOPositions and proper motions updated to Gaia DR2 values.LP246-31J2000J200021.478(GALEX)STARM V-IVNOSIMBAD has V=17.70EPIC210894955J2000J200021.097(Derived)STARM V-IVNOEPIC210704853J2000J200021.323(Derived)STARM V-IVNOUpdated proper motions to Gaia DR2 valuesEPIC210704853J2000J200021.323(Derived)STARM V-IVNOPositions and proper motions updated to Gaia DR2 values.LP474-28J2000J200022.127(Derived)STARM V-IVNOPositions and proper motions updated to Gaia DR2 values.LP474-54J2000J200022.189(Derived)STARM V-IVNOPositions and proper motions updated to Gaia DR2 values. V magnitude changed to SIMBAD value of 16.13.LP414-1100J2000J200021.549(GALEX)STARM V-IVNOPositions and proper motions updated to Gaia DR2 values. V magnitude changed to SIMBAD value of 16.09.LP414-158J2000J200022.705(GALEX)STARM V-IVNOPositions and proper motions updated to Gaia DR2 values.LP415-875J2000J200022.381(Derived)STARM V-IVNOClassified as BY Dra in SIMBAD. Positions and proper motions updated to Gaia DR2 values.V1104TAUJ2000J200021.437(Derived)STARM V-IVNOPositions and proper motions updated to Gaia DR2 values. V magnitude updated to SIMBAD value of 19.23.LP415-20J2000J200021.924(Derived)STARM V-IVNOListed as BD in SIMBAD. No V magnitude available. Proper motions updated to AllWISE survey values.EPIC210371851J2000J200021.196(Derived)STARM V-IVNOEPIC210743724J200021.24COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950COS/NUVSpectroscopicNoNoG230L2950The scheduling data was generated by CASM 27.0.CASM was run in Phase II mode./tmp/OPVisit4247788199273374900.xml154821051300071.0(Tic-Visit
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:data-volume 174416
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(Tic-Obset
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(Tic-Orbit
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