INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONSSubmission #4, 25 October 2019. Please contact Kevin France (kevin.france@colorado.edu) with questions or corrections.-285581003----- Attempting Submission 1 (Thu Jul 25 19:29:18 GMT 2019) -----
----- Attempting Submission 2 (Wed Oct 02 20:21:39 GMT 2019) -----
----- Attempting Submission 3 (Fri Oct 25 21:05:04 GMT 2019) -----The evolving magnetic lives of young SunsThis is a coordinated HST+XMM-Newton program to address the conditions that affect habitability on Earth-like planets around Sun-like stars. Both wavelength regimes (far-UV with HST, X-rays with XMM) are needed to constrain models sufficiently to represent realistic conditions. An approved TESS program for our targets will provide additional information on surface inhomogeneities (spots) and their sizes and locations so that that can be taken into account as well. The FUV and X-ray fluxes from young stars are erosive of a planet's atmosphere, particularly for hydrogen, but also for oxygen and nitrogen, both chemically important elements.This program aims to acquire high-S/N FUV spectroscopy of nearby 'solar type' (G and K dwarf) stars so the high energy radiation and particle environments can be estimated as inputs to exoplanet atmopshere models. We use COS over STIS as it is the only way to acheive high-S/N obsrvations in weak, but important, FUV tracers Fe XXI 1354 and O IV] 1401 (required to estimate the X-ray and stellar wind conditions). Other essential travers for estimating the complete EUV environment are C II 1335 and Si IV 1394/1403, and when possible C III 1175 and N V 1240 to complete the FUV temperature coverage and enable estimates of the EUV irradiance.
These observations need to be coordinated with XMM to be contemporaneous, as specified in the approved Phase I proposal.
The HST observing plan is built off the successful MUSCLES Treasury Survey (13650), and acquires targets with a COS ACQ/IMAGE as these stars are all within 50 pc and have high quality Hipparchos or Gaia data available. We observe in G130M lam1291 to cover all of these lines. We restrict observations to FP-POS = 3 and 4 as they are the only two supported modes that access all of these tracers simultaneously. Two targets, kappa1 Cet and epsilon Eri, have stellar LyA profiles that exceed the COS bright limit, so we will observe with segment A only for these targets.
We cleared the fields with the APT BOT tool and created ETC runs for all targets/modes during the Phase II preparation.Kevin France was the PI of the HST MUSCLES Treasury Survey (GO13650) to study the spectral and temporal
properties of red dwarf stars (France et al. 2016; Loyd et al. 2016; Youngblood et al. 2016). He is the co-PI of
the follow-on Mega-MUSCLES Survey (GO15071) that focused on activity in later-type M dwarfs. He was
also a member of the COS instrument and science teams, developing numerous community tools for spectral
and temporal analysis of COS data.
M. Guedel provides expertise in stellar X-ray astronomy and the analysis of XMM-Newton data. He has been
studying high-energy radiation from cool stars, its variability and its long-term evolution with applications to The evolving magnetic lives of young Suns evolving planetary atmospheres. He is leading projects studying effects of space weather on the development of planetary habitability.
V. Airapetian is the overall PI of the international program of which this HST proposal is a part; it includes
observations with TESS, Pic du Midi, Subaru, inter alia. His expertise includes 3-D MHD simulations of solar,
stellar and planetary winds, solar and solar/stellar corona, MHD models of coronal streamers, super-flares from
solar-type stars, physico-chemical models of atmospheric chemistry of early Earth, Mars and exoplanets,
hydrodynamic modeling of ionospheric outflows, optical and soft X-ray spectroscopy, RS CVn stars,
chromospheric heating and wind acceleration from late-type stars, laboratory experiments of prebiotic
chemistry initiated due to energetic particles. He is the author of over 100 publications.
D. Soderblom has long experience with studying stellar activity in the optical and ultraviolet and in using HST.Stellar PhysicsPlanets and Planet Formation6falsefalsefalsefalsefalsefalse32trueSUPPORTEDEXT-STARG V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database, 2018 Gaia coords.
G0V
G130M: COS.sp.1365156 , 16ks to S/N = 10 @ 1401.2. (S/N = 7 in 8000s)
TA: COS.ta.1365369, T_exp = 45s (Castelli & Kurucz G0V)
BOT: only the *OV* target starJ2000J2000EXT-STARG V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
G5V
G130M: COS.sp.1365159 , 1500s to S/N = 10 @ 1401.2. BOP at LyA
TA: COS.ta.1365401 , Kurucz G5V, T_exp = 6s
BOT: cleared, all stars mis-ID'd targetJ2000J2000EXT-STARK V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
K2V
G130M: COS.sp.1365155 , 522s to S/N = 10 @ 1401.2. BOP at LyA
TA: COS.ta.1365403 , Castelli & Kurucz K2V, T_exp = 10s
BOT: cleared. All mis-ID'd target starJ2000J2000EXT-STARG V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database. 2018 Gaia coordinates.
G3V
G130M: COS.sp.1365158 , 6200s to S/N = 10 @ 1401.2.
TA: COS.ta.1365402, Kurucz G2V, T_exp = 22s
BOT: cleared, all mis-ID'd target starJ2000J2000COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG130M1309The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.These observations need to be coordinated with XMM to be contemporaneous, as specified in the approved Phase I proposal.158192585700064.7473903225673(Tic-Visit
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