We found an error in one of our figures in the pdf file. We've fixed the error and are resubmitting.86424739Assigned ID: 792
----- Attempting Submission 1 (Fri Feb 24 22:06:30 GMT 2012) -----
HST Phase I Proposal 792 (HST Cycle 20 dMs.apt) successfully submitted.
----- Attempting Submission 2 (Wed Feb 29 03:36:55 GMT 2012) -----BOT warnings are given fir visits 3, 4 and 7
visit 3 - the dM star itself is being "defaulted" to a O5V star - the coordinates the BOT gives are for the dM star and a B-V of 0.96 is given for the object
visit 4 - the dM star is also defaulted to O5V - again, the coordinates of the dM star are given and a B-V = 1.33 for the object
visit 7 - the dM star is also defaulted to O5V - the coords of the dM star are given and B-V = 1.14
In summary, we have looked into it, and all three BOT warnings are misclassified dM stars. Please let us know if further information is needed.-248985434----- Attempting Submission 1 (Tue Jul 10 16:55:32 GMT 2012) -----
HST Phase II Proposal 13020 (HST_Cycle20_dMs.apt) successfully submitted.
----- Attempting Submission 2 (Tue Jul 10 18:08:53 GMT 2012) -----
----- Attempting Submission 3 (Mon Aug 06 05:21:57 GMT 2012) -----
HST Phase II Proposal 13020 (HST_Cycle20_dMs.apt) successfully submitted.
----- Attempting Submission 4 (Thu Oct 11 20:41:53 GMT 2012) -----
HST Phase II Proposal 13020 (HST_Cycle20_dMs.apt) successfully submitted.
----- Attempting Submission 5 (Wed Oct 24 20:06:45 GMT 2012) -----
----- Attempting Submission 6 (Mon Feb 18 15:47:58 GMT 2013) -----
HST Phase II Proposal 13020 (HST_Cycle20_dMs.apt) successfully submitted.
----- Attempting Submission 7 (Mon Feb 18 17:58:34 GMT 2013) -----
HST Phase II Proposal 13020 (HST_Cycle20_dMs.apt) successfully submitted.
----- Attempting Submission 8 (Sat Feb 23 22:39:52 GMT 2013) -----
HST Phase II Proposal 13020 (HST_Cycle20_dMs_II.apt) successfully submitted.
----- Attempting Submission 9 (Thu Mar 28 20:48:25 GMT 2013) -----All errors have been noted. However, if further clarification is required, just let me know.
scott.engle@villanova.edu
edward.guinan@villanova.eduA Comprehensive COS Study of the Magnetic Dynamos, Rotations, UV Irradiances and Habitability of dM Stars with a Broad Span of AgesWe propose HST/COS FUV spectrophotometry of a carefully selected sample of 9 dM1-5 stars with recently reliably determined ages ranging from ~1-12 Gyr. This program complements our Chandra Cycle 13 program of the same targets to determine their coronal X-ray properties. Ages (of all but one star) have recently been firmly determined from memberships in wide binaries with white dwarf (WD) companions having reliable cooling time+main-sequence evolution ages (Zhao et al. 2012, Garces et al 2011). Until these studies, reliable age determinations for dM stars >2 Gyr were nearly impossible. However, we can now carry out a comprehensive UV study of dM star atmospheres across nearly the full age-range of the current Universe. The primary goals are 1) to study the evolution of their dynamo-generated X-ray and UV (XUV) emissions with age/rotation and to better define the heating and energetics of their atmospheres (via Age-Rotation-Activity-XUV Irradiance relations) and 2) to study the effects of the XUV radiation on planets hosted by red dwarfs. The COS UV spectral region contains numerous important diagnostic emission lines for characterizing the energy transfer and atmospheric structure, while line ratios yield valuable information about the electron density. Further, these data (when combined with our coronal X-ray measures) are also important for gauging dM star XUV emissions - critical for assessing the photochemical & photoionization evolution of planetary atmospheres and ionospheres that in turn strongly affect the possible development of life on hosted extrasolar planets. We are requesting a total of 19 HST orbits to achieve the science goals of the program.We are proposing HST/COS FUV-UV low/medium resolution spectrophotometry of the target stars, all of which are currently being observed by Chandra. The majority of the targets (the stars with d < 20-pc) will be observed from 1150-2830A using G140L and G285M. The most distant target (G 111-72; 37-pc) will be observed from 1150-3150A with the G140L/230L elements. All observations will use the Primary Science Aperture. We are requesting two consecutive HST orbits per target to carry out this program. Taking into account acquisition and overheads this request will result in an average of about 2400-2600 sec of on-target time per HST orbit. We plan to devote the first HST orbit of each visit to the G285M or G230L element (~2400s) and the second orbit (with re-acquire) to G130M (~2600-2800s). The longer exposure is has been chosen for the shorter wavelength region because almost all of the important emission lines are in that region. All exposures will be split to extend wavelength coverage, mitigate cosmics, and to discriminate any observed flare events. Kapteyn's Star is an exceptional target. It has an exceedingly slow rotation period of ~198+/-18 days. Also, it is the nearest of our proposed stars, serves as a proxy for Pop II metal poor stars, and has a large radial velocity of +245 km/sec. At this speed, the Ly-alpha line will be red-shifted by ~1A, moving it off of the ISM and geocoronal features and allowing a "clean" measure of the stellar Ly-alpha flux for a very old (presumably low activity) star. Thus we are proposing for a third orbit on Kapteyn's Star to observe in the G130M element. This will give us the resolution necessary to perform a detailed study of the Ly-alpha feature free of contamination, compare to the deconstructed Ly-alpha fluxes modeled by Wood et al. 2005, and test acoustic heating models for stars with very slow rotations. We are particularly excited by this aspect of the program.COOL STARS12falsefalse0.00.0falsefalsefalseSUPPORTEDSTAREMISSION LINE STARM V-IVJ2000J2000STAREMISSION LINE STARM V-IVJ2000J2000STAREMISSION LINE STARM V-IVJ2000J2000STAREMISSION LINE STARM V-IVJ2000J2000STAREMISSION LINE STARM V-IVJ2000J2000STAREMISSION LINE STARM V-IVJ2000J2000STAREMISSION LINE STARM V-IVJ2000J2000STAREMISSION LINE STARM V-IVJ2000STAREMISSION LINE STARM V-IVJ2000COS/FUVSpectroscopicNoNoG140L1105COS/NUVSpectroscopicNoNoG285M2695COS/FUVSpectroscopicNoNoG140L1105COS/NUVSpectroscopicNoNoG285M2695COS/FUVSpectroscopicNoNoG140L1105COS/NUVSpectroscopicNoNoG285M2695COS/FUVSpectroscopicNoNoG140L1105COS/NUVSpectroscopicNoNoG230L2950COS/FUVSpectroscopicNoNoG140L1105COS/NUVSpectroscopicNoNoG285M2695COS/FUVSpectroscopicNoNoG140L1105COS/NUVSpectroscopicNoNoG285M2695COS/FUVSpectroscopicNoNoG140L1105COS/NUVSpectroscopicNoNoG285M2695COS/FUVSpectroscopicNoNoG140L1105COS/NUVSpectroscopicNoNoG285M2695COS/FUVSpectroscopicNoNoG140L1105COS/NUVSpectroscopicNoNoG285M2695COS/FUVSpectroscopicNoNoG130M1327The scheduling data was generated by CASM 20.2.CASM was run in Phase II mode.C:\Users\Scott\Documents\OP-cache\HST_Cycle20_dMs_II-v01.xml(Tic-Visit
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