0Assigned ID: 91
----- Attempting Submission 1 (Mon Mar 02 22:08:23 GMT 2020) -----
HST Phase I Proposal 91 successfully submitted.
Receipt: # 91-1New submission needed to adjust acquisition strategy for visits 3 and 4 on science target LHS-2021 due to proximity of bright source at mid cycle 28 epoch due to large target proper motions.-1913275999----- Attempting Submission 1 (Tue Jun 30 17:19:21 GMT 2020) -----
----- Attempting Submission 2 (Wed Nov 18 04:34:54 GMT 2020) -----Chromosopheric and Coronal Activity in the Lowest-Mass StarsThe recent discovery of the seven planet TRAPPIST--1 system, including three habitable zone planets, has opened up a new avenue for studying temperate terrrestrial planets, with potentially habitable atmospheres. This system and others like it around the lowest-mass stars will be prime targets for both planet searches and studies to directly characterize the atmospheres of Earth-sized exoplanets. Understanding these atmospheric observations and the potential prospect of such exoplanets to develop and sustain life critically depends on the high-energy stellar radiation environment from X-ray to ultraviolent wavelengths because of the ability of this emission to drive atmospheric mass-loss, and it's strong influence on planetary photochemistry, including its ability to catalyze prebiotic chemical pathways. However, little is known about the X-ray to UV radiation field of stars at the end of the main sequence. We propose a survey of the joint X-ray and UV emission of a sample of M7-M9 dwarfs, to provide the basis for estimating the high-energy stellar radiation environment around these stars across a range of activity levels, and to use these spectral observations as inputs to planetary photochemsitry models. Furthermore, these observations will probe the nature of chromospheric and coronal heating in the coolest stellar atmospheres.This program focuses on the joint FUV and NUV emissions of 6 target very-low mass stars with additional Chandra observations of two of these targets to complete the measurements of the sample's X-ray to NUV emissions. Our program will additionally have ground based support to capture their optical emission features to relate them to these new high-energy measurements. The observations will further form the inputs for modeling of photochemistry in the atmospheres of exoplanets around these very-low mass stars.
The NUV measurements with STIS G230L will capture the entire NUV spectrum, with particular emphasis on the Mg II emission features that will be the most prominent lines. In the FUV, we will use STIS G140M to target the Lyman alpha emission of each target, as the strongest FUV line. Measurements of additional features like Nv at 1239/1243 angstroms will also be possible if strong enough as an additional upper atmosphere diagnostic. The moderatae resultion of the G140M grating enables for the clear reconstruction of the Lyman alpha profile to accounting for the attenuation of the ISM. Because of the importance of the Lyman alpha measurements, the FUV visits need to take place at points along the Earth's orbit that aligns the ISM attenuation with the radial velocity of the Earth's airglow. This coordination provides the necessary overlap in the observed Lyman alpha profiles to facilitate the accurate reconstruction of the intrinsic emission. Using TIME-TAG mode our program will further assess the variabiliy of these targets in the NUV and FUV, including emission line variations in quiescense on short time scales, and the possibility of capturing high-energy flaring behavior.
Using the combined X-ray to NUV emissions of the very-low mass stars we will drive exoplanet atmospheric models to determine the possibility of sustaining prebiotic chemical pathways, and driving the abiotic production of biosignatures. We will then compare these exoplanets around the lowest-mass stellar hosts to similar objects around more massive M-dwarfs.Listed alphabetically by last name:
Dr. Kevin France was the PI of the HST MUSCLES Treasury Survey (GO 13650) 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.
Dr. Alejandro Nunez has extensively studied magnetic activity in low-mas stars and is an expert in X-ray data reduction for such stars (e.g., Nunz et al. 2017). He will lead the X-ray analysis of the proposed observations.
Dr. J. Sebastian Pineda is an expert on magnetic activity from low-mass stars to brown dwarfs (e.g., Pineda et al. 2017), with experience in as PI of UV studies of M-dwarfs (HST GO Programs 14347, 14640), and will lead analyses of the proposed HST spectroscopy.
Dr. Sukrit Ranjan has expertise in evaluating the impact of UV environments on habitability and prebiotic chemistry (Ranjan et al. 2017), and access to and experience with the atmospheric photochemistry model (Hu et al. 2012) that will be used for modelling M-dwarf exoplanet atmospheres in this study.
Dr. Allison Youngblood is the PI of several proposals utilizing HST's unique UV capabilities to study topics like Lyman alpha emission and NUV flaring from cool dwarf stars. She performed the Lyman alpha reconstructions for the MUSCLES Treasury Survey (Youngblood et al. 2016), and is also completing the Lyman alpha reconstructions for the Mega-MUSCLES Treasury Survey and the FUMES survey. She will lead the Lyman alpha work in this study.Stellar Physics and Stellar TypesExoplanets and Exoplanet Formation6falsefalsetruefalsefalsefalsefalse30trueSUPPORTEDSTARM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000J = 11.38, sloan i = 14.165, gaia dr2 G=15.77, gaia dr2 G_BP = 19.3267STARM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARK V-IVNOGaia DR2 source: 599891555546067200 ; Bp - Rp = 1.8 , V-mag is from APASS Henden '16; Teff~4000J2000G = 14.2STIS/FUV-MAMASpectroscopicNoNoG140M1222STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140M1222STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140M1222STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140M1222STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140M1222STIS/NUV-MAMASpectroscopicNoNoG230L2376STIS/FUV-MAMASpectroscopicNoNoG140M1222STIS/NUV-MAMASpectroscopicNoNoG230L2376Timing link suitability includes constraints ([Group (01 02) Within 21.0 days])The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.2 Orbits of FUV. To ensure that the Lyman alpha airglow emission coincides spectrally with the ISM absorption trough, Hubble must not observe this target between Nov 25 and May 9 (any year).162851296100094.57039907961831(Tic-Visit
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)true40V=18.881; Phoenix M dwarf Models M7.5 2600. 5., S/N=78; U =19.58 flare STIS.ta.1452276Phoenix M dwarf Models M7.5 2600. 5., V=18.881, S/N = 53; U=19.58 flare STIS.ta.1452280Sci - User Spectrum ETC; U = 19.58 flare LyA - 9.47E-14 erg/s/cm2; STIS.sp.1452609Sci - User Spectrum ETC; U = 19.58 flare LyA - 9.47E-14 erg/s/cm2; STIS.sp.1452609Sci - User Spectrum ETC; U = 19.58 flare LyA - 9.47E-14 erg/s/cm2; STIS.sp.1452609Sci - User Spectrum ETC; U = 19.58 flare LyA - 9.47E-14 erg/s/cm2; STIS.sp.1452609Timing link suitability includes constraints ([Group (05 06) Within 21.0 days])The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.3 Orbits of LP412-31 in NUV. No requirement included but if possible, preference for NUV visit to coincide with FUV visit.1628098138000255.33929178888047(Tic-Visit
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)true20V=17.3, Phoenix M dwarf Models M8 2500. 5, S/N = 86; U=18 flare STIS.ta.1452288Phoenix M dwarf Models M8 2500. 5., V=17.3, S/N =86; U=18 flare STIS.ta.1452299Sci - User Spectrum ETC; U=18 flare LyA - 3.62E-13 erg/s/cm2 -- STIS.sp.1452649Sci - User Spectrum ETC; U=18 flare LyA - 3.62E-13 erg/s/cm2 -- STIS.sp.1452649Timing link suitability includes constraints ([Group (07 08) Within 21.0 days])The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.2 Orbits of NUV. No requirement included but if possible, preference for NUV visit to coincide with FUV visit.163503852600077.42842931535199(Tic-Visit
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)true20V=17.3, Phoenix M dwarf Models M8 2500. 5, S/N = 86; U=18 flare STIS.ta.1452288Phoenix M dwarf Models M8 2500. 5., V=17.3, S/N =86; U=18 flare STIS.ta.1452299Sci - User Spectrum ETC; U=18 flare -- STIS.sp.1452658Sci - User Spectrum ETC; U=18 flare -- STIS.sp.14526582 Orbits of NUV. No requirement included but if possible, preference for NUV visit to coincide with FUV visit.(Tic-Visit
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:si-bright-earth-limb-angle 20.0
:data-volume 522304
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16197
:visit-id "08"
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)
(Tic-Orbit
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(Tic-Orbit
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)false20V=17.3, Phoenix M dwarf Models M8 2500. 5, S/N = 86; U=18 flare STIS.ta.1452288Phoenix M dwarf Models M8 2500. 5., V=17.3, S/N =86; U=18 flare STIS.ta.1452299Sci - User Spectrum ETC; U=18 flare -- STIS.sp.1452658Sci - User Spectrum ETC; U=18 flare -- STIS.sp.1452658Timing link suitability includes constraints ([Group (09 10) Within 21.0 days])The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.3 Orbits of FUV.1622358086000104.13723688397289(Tic-Visit
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:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 3
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:data-volume 470096
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:coron NIL
)
(Tic-Obset
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(Tic-Orbit
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(Tic-Orbit
:proposal-id 16197
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(Tic-Orbit
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)true30V=17.532; Phoenix M dwarf Models M9.5 2300. 5, S/N = 95.4; U flare = 18.23 STIS.ta.1452310Phoenix M dwarf Models M9.5 2300. 5., V=17.532, S/N = 100; U=18.23 flare STIS.ta.1452315Sci - User Spectrum ETC; U = 18.23 flare, LyA 2.97E-13 erg/s/cm2 -- STIS.sp.1452684Sci - User Spectrum ETC; U = 18.23 flare, LyA 2.97E-13 erg/s/cm2 -- STIS.sp.1452684Sci - User Spectrum ETC; U = 18.23 flare, LyA 2.97E-13 erg/s/cm2 -- STIS.sp.1452684Timing link suitability includes constraints ([Group (09 10) Within 21.0 days])The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.2 Orbits of NUV. No requirement included but if possible, preference for NUV visit to coincide with FUV visit.1621935032000111.5(Tic-Visit
:proposal-id 16197
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:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 591888
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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)
(Tic-Orbit
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)
(Tic-Orbit
:proposal-id 16197
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)true20V=17.532; Phoenix M dwarf Models M9.5 2300. 5, S/N = 95.4; U flare = 18.23 STIS.ta.1452310Phoenix M dwarf Models M9.5 2300. 5., V=17.532, S/N = 100; U=18.23 flare STIS.ta.1452315Sci - User Spectrum ETC; U = 18.23 flare -- STIS.sp.1452691Sci - User Spectrum ETC; U = 18.23 flare -- STIS.sp.1452691Timing link suitability includes constraints ([Group (11 12) Within 21.0 days])The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.5 Orbits of FUV. To ensure that the Lyman alpha airglow emission coincides spectrally with the ISM absorption trough, Hubble must not observe this target between Mar 12 and July 6 (any year).161471733900080.0(Tic-Visit
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:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 5
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:si-bright-earth-limb-angle 20.0
:data-volume 783184
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:coron NIL
)
(Tic-Obset
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)
(Tic-Orbit
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:pcs-gap 0
)
(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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)true50V=18.959, Phoenix M dwarf Models M9.5 2300. 5., S/N = 111; U = 19.66 flare STIS.ta.1452320V=18.959, S/N=90, Phoenix M dwarf Models M9.5 2300. 5.; U = 19.66 STIS.ta.1452329Sci User Spectrum ETC; U=19.66 flare LyA - 8.87E-14 erg/s/cm2 --STIS.sp.1452699Sci User Spectrum ETC; U=19.66 flare LyA - 8.87E-14 erg/s/cm2 --STIS.sp.1452699Sci User Spectrum ETC; U=19.66 flare LyA - 8.87E-14 erg/s/cm2 --STIS.sp.1452699Sci User Spectrum ETC; U=19.66 flare LyA - 8.87E-14 erg/s/cm2 --STIS.sp.1452699Sci User Spectrum ETC; U=19.66 flare LyA - 8.87E-14 erg/s/cm2 --STIS.sp.1452699Timing link suitability includes constraints ([Group (11 12) Within 21.0 days])The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.4 Orbits of NUV. No requirement included but if possible, preference for NUV visit to coincide with FUV visit.161480886400080.0(Tic-Visit
:proposal-id 16197
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:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 4
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:si-bright-earth-limb-angle 20.0
:data-volume 1113728
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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)
(Tic-Orbit
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)
(Tic-Orbit
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)
(Tic-Orbit
:proposal-id 16197
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)
(Tic-Orbit
:proposal-id 16197
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)true40V=18.959, Phoenix M dwarf Models M9.5 2300. 5., S/N = 111; U = 19.66 flare STIS.ta.1452320V=18.959, S/N=90, Phoenix M dwarf Models M9.5 2300. 5.; U = 19.66 STIS.ta.1452329Sci - User Spectrum ETC; U=19.66 flare -- STIS.sp.1452701Sci - User Spectrum ETC; U=19.66 flare -- STIS.sp.1452701Sci - User Spectrum ETC; U=19.66 flare -- STIS.sp.1452701Sci - User Spectrum ETC; U=19.66 flare -- STIS.sp.1452701