0
Assigned ID: 781
----- Attempting Submission 1 (Fri Apr 05 21:21:30 GMT 2019) -----
HST Phase I Proposal 781 (HST_HAZKAT.apt) successfully submitted.
Receipt: # 781-1
Is there any possible way I can add the proper motions for visit 11, BD+16? They are 157.945 -316.326 mas/yr with an epoch of 2000. The parallax is 58.1097 mas.
915916455
----- Attempting Submission 1 (Thu Jul 25 23:40:22 GMT 2019) -----
HST Phase II Proposal 15955 (hst_apt_backup.apt) successfully submitted.
Receipt: # 15955-1
----- Attempting Submission 2 (Thu Aug 15 20:54:22 GMT 2019) -----
HST Phase II Proposal 15955 (hst_apt_v3.apt) successfully submitted.
Receipt: # 15955-2
----- Attempting Submission 3 (Sun Nov 03 20:09:16 GMT 2019) -----
HST Phase II Proposal 15955 (hst_apt_v4.apt) successfully submitted.
Receipt: # 15955-3
----- Attempting Submission 4 (Tue Nov 12 19:47:28 GMT 2019) -----
HST Phase II Proposal 15955 (hst_apt_v5.apt) successfully submitted.
Receipt: # 15955-4
----- Attempting Submission 5 (Wed Nov 27 18:58:37 GMT 2019) -----
HST Phase II Proposal 15955 (hst_apt_v5.apt) successfully submitted.
Receipt: # 15955-5
----- Attempting Submission 6 (Thu Dec 12 23:23:13 GMT 2019) -----
HST Phase II Proposal 15955 (hst_apt_v7.apt) successfully submitted.
Receipt: # 15955-6
----- Attempting Submission 7 (Mon Dec 16 20:21:19 GMT 2019) -----
HST Phase II Proposal 15955 (hst_apt_v8.apt) successfully submitted.
Receipt: # 15955-7
----- Attempting Submission 8 (Thu Dec 19 05:43:00 GMT 2019) -----
HST Phase II Proposal 15955 (hst_apt_v8.apt) successfully submitted.
Receipt: # 15955-8
----- Attempting Submission 9 (Fri Jan 24 20:49:02 GMT 2020) -----
The K Dwarf Advantage: Assessing the Habitability of Planets Orbiting K Stars
Current efforts for finding a potentially habitable planet lie with M stars, yet K stars may offer more habitable conditions due to decreased stellar activity and more distant and wider habitable zones. Knowing the UV environment of a star over a planet's formation and evolution is critical in determining if that planet is potentially habitable and if any biosignatures will be detected, as UV radiation can severely change or destroy a planet's atmosphere. While M star stellar activity evolution has been observed photometrically and spectroscopically, there has been no spectroscopic study of K-star UV evolution. We propose to observe a statistical sample of K stars in the NUV and FUV with COS at three ages representative of UV evolution. By analyzing the full UV spectral range as a function of age, we will be able to provide an empirically-driven grid of model stellar spectra from X-ray to IR, which does not yet exist for K stars. This will include the extreme-UV flux, currently unobservable, which most affects the alteration and erosion of a planet's atmosphere. Both the proposed observations and the subsequent upper-atmosphere stellar models will be vital in determining the potential habitability of planets orbiting K stars.
We have carefully selected 24 K stars (including 5 with archived spectra) with similar masses (0.6 Msol - 0.8 Msol) and varying ages to measure the evolution of these types of stars. For those stars without published masses, we made mass estimates based on the spectral type to effective temperature transformations of Pecaut & Mamajek (2013) and the evolutionary models of Baraffe et al. (2015).
We have drawn the new targets from three representative ages: [1] 7 bona-fide members
of the Tucana-Horologium young moving group (45 Myr, Bell et al. 2015; Kraus et al. 2014); [2] 6 bona-fide members of the Hyades cluster (625 Myr, Perryman et al. 1997; Goldman et al. 2013); and [3] 6 K dwarf field stars within 25 pc, assumed at an age of 5 Gyr. In addition to our new sample, there are three K star members of Tuc-Hor and two field stars that have already been observed in the required modes, for a total of 24 K stars for this evolutionary statistical study. The intermediate age is vital to our understanding of UV evolution, as they provide the shape of the evolutionary curve and would lead to an underestimate of intermediate-activity fluxes for stars of this age if ignored. A similar strategy has proven successful in the spectroscopic evolutionary study of M dwarfs with HST's HAZMAT program (GO-14784, P.I. Shkolnik; Loyd et al. 2018a).
We verified this sample to be single stars and only selected Tuc-Hor members that were confirmed with the addition of youth indicators such as low gravity indices, Halpha emission, and lithium absorption (necessary due to the large spacial dispersion of the group members in the sky) to provide further evidence of true membership. By the age of the Hyades members, these youth indicators are gone and the stars are clustered, therefore, we did not require this step in selecting our targets. The ages of each of our targets are thus well-constrained.
HST observations are fundamental for this analysis as HST provides the only access to UV spectra at the needed spectral resolution. The FUV and NUV emission lines are necessary for building the DEM for estimating the EUV and for completing upper atmosphere models that currently lack information about the chromosphere, transition region, and corona.
We calculated the exposure times using the COS/ETC and spectra from the K dwarfs observed by the MUSCLES program (France et al. 2016; Cycle 22, GO-13650, PI: France) scaled to the GALEX NUV and FUV magnitudes. We require an integrated S/N of 20 in the strong emission lines with formation temperatures ranging from 1E4 to 1E7 K to trace the evolution of stellar activity in the chromosphere, transition region, and corona. The Acquisition Image exposure times for each of the targets is between 1 second and 2 minutes. We require measurements of the slope of the NUV spectrum and the emission lines in the FUV to reconstruct the DEM for the EUV; therefore, we need exposures using COS G230L (2950 A), COS G160M (1577 A), and COS G130M (1309 A). High-level science products will be contributed to MAST.
Dr. Travis Barman (University of Arizona) is a lead developer of the PHOENIX model atmosphere code. His work has been used to predict and interpret the atmospheric properties of exoplanets. Dr. Barman will head the modeling component of this program.
Dr. R. O. Parke Loyd (Arizona State University) has expertise in UV emission of stars and the impacts of flares on planetary atmospheres. He is proficient in the reduction and analysis of HST COS data, being a PI for proposal #15174 in Cycle 25 and a Co-I for eight other successful programs. Dr. Loyd will assist in the data reduction and analysis for this program.
Prof. Victoria Meadows (University of Washington) is the PI for the NASA Astrobiology Institute's Virtual Planetary Laboratory Lead Team. She is an expert in observing and modeling terrestrial planet environments.
Tyler Richey-Yowell (Arizona State University) is a graduate student working with Dr. Evgenya Shkolnik, researching the UV environments of K stars and their implications on exoplanet formation and habitability. She will assist in the data reduction, data analysis, and publication efforts.
Dr. Adam Schneider (Arizona State University) has expertise in the formation and evolution of low-mass stars and exoplanets. He is the PI of two successful Hubble programs from Cycle 23 (#14233) and Cycle 25 (#15286). Dr. Schneider will assist in the data reduction and analysis for this program.
Dr. Evgenya Shkolnik (Arizona State University) is an expert in the evolution of high-energy stellar radiation of low-mass stars and its planetary impacts. She is the PI of the Cycle 24 HST proposal #14784, which studied the UV evolution of early M stars. Dr. Shkolnik will assist in the data reduction, data analysis, and publication efforts.
Stellar Physics
Planets and Planet Formation
6
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false
true
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SUPPORTED
STAR
K V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
K V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
K V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
K V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
K V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
K V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
K V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
K V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
K V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
K V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
K V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
K V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
K V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
K V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
K V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
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J2000
STAR
M V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
M V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
K V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
STAR
K V-IV
NO
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
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COS/FUV
Spectroscopic
No
No
G130M
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COS/FUV
Spectroscopic
No
No
G160M
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COS/NUV
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No
No
G230L
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COS/FUV
Spectroscopic
No
No
G130M
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COS/FUV
Spectroscopic
No
No
G160M
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COS/NUV
Spectroscopic
No
No
G230L
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COS/FUV
Spectroscopic
No
No
G130M
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COS/FUV
Spectroscopic
No
No
G160M
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COS/NUV
Spectroscopic
No
No
G230L
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COS/FUV
Spectroscopic
No
No
G130M
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COS/FUV
Spectroscopic
No
No
G160M
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COS/NUV
Spectroscopic
No
No
G230L
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COS/FUV
Spectroscopic
No
No
G130M
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COS/FUV
Spectroscopic
No
No
G160M
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COS/NUV
Spectroscopic
No
No
G230L
2950
COS/FUV
Spectroscopic
No
No
G130M
1309
COS/FUV
Spectroscopic
No
No
G160M
1577
COS/NUV
Spectroscopic
No
No
G230L
2950
COS/FUV
Spectroscopic
No
No
G130M
1309
COS/FUV
Spectroscopic
No
No
G160M
1577
COS/NUV
Spectroscopic
No
No
G230L
2950
COS/FUV
Spectroscopic
No
No
G130M
1309
COS/FUV
Spectroscopic
No
No
G160M
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COS/NUV
Spectroscopic
No
No
G230L
2950
COS/FUV
Spectroscopic
No
No
G130M
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COS/FUV
Spectroscopic
No
No
G160M
1577
COS/NUV
Spectroscopic
No
No
G230L
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COS/FUV
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COS/FUV
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No
G160M
1577
COS/NUV
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No
No
G230L
2950
COS/FUV
Spectroscopic
No
No
G130M
1309
COS/FUV
Spectroscopic
No
No
G160M
1577
COS/NUV
Spectroscopic
No
No
G230L
2950
COS/FUV
Spectroscopic
No
No
G130M
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COS/FUV
Spectroscopic
No
No
G160M
1577
COS/NUV
Spectroscopic
No
No
G230L
2950
COS/FUV
Spectroscopic
No
No
G130M
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COS/FUV
Spectroscopic
No
No
G160M
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COS/NUV
Spectroscopic
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No
G230L
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No
G130M
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COS/FUV
Spectroscopic
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No
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No
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No
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COS/FUV
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G160M
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COS/NUV
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No
No
G230L
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No
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COS/FUV
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No
G160M
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COS/NUV
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COS/FUV
Spectroscopic
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No
G160M
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COS/NUV
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G230L
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COS/FUV
Spectroscopic
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No
G130M
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COS/FUV
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G160M
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No
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COS/FUV
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No
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Copy of original visit 11 but with corrected target #22.
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The scheduling data was generated by CASM 27.2.
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