please direct issues with the DDT proposal or APT submission to Dr. Kevin France, kevin.france@colorado.edu. - v2, 03/29/231306432382Assigned ID: 3903
----- Attempting Submission 1 (Tue Mar 28 20:12:59 GMT 2023) -----
HST Phase I Proposal 3903 successfully submitted.
Receipt: # 3903-1
----- Attempting Submission 2 (Wed Mar 29 17:39:26 GMT 2023) -----
HST Phase I Proposal 3903 successfully submitted.
Receipt: # 3903-2The number of orbits used exceeds the number allocated
Unsupported characters were found in Observing Description and replaced with |*|
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONS
INEFFICIENT ORDERING OF FP-POS POSITIONSKevin France, 17305, version 3, following the discussions with Amber Armstrong. 09/15/23-174457042----- Attempting Submission 3 (Fri Sep 15 18:45:05 GMT 2023) -----An X-ray through Radio Exo-Space Weather Campaign to Study the Infant Sun DS TucWe propose to obtain COS spectra in support of an approved, international, multi-wavelength campaign to constrain the space weather conditions of the early proto-solar system. The focus of the proposed study is the magnetic activity of the young (45 Myr) Sun-like star, DS Tuc A. This nearby star thought to be an ideal proxy of the infant Sun at a near-zero-age main-sequence epoch, when the Earth's atmosphere transitioned from the primary to the secondary nitrogen and carbon dioxide rich atmosphere. Thus, the knowledge of the stellar ionizing radiation in the form of quiescent and flare X-ray and EUV emission, stellar wind and CME pressure that can affect the atmospheric escape and its chemistry is of critical importance for the study of early Venus, Earth and Mars environments. DS Tuc A, which is also exemplary for very young stars in its hosting of a transiting planet, is the subject of an approved ground-based, TESS, and NICER campaign that will occur in August 2023. We request director's discretionary time observations with COS to obtain simultaneous FUV spectra of this exemplar system to provide a physically consistent picture of the drivers and outputs of the magnetically driven stellar coronal and wind structures of infant suns. We will use these observations as inputs to a fully thermodynamic model of the corona-wind system of DS Tuc using the AWSoM code. AWSoM will output the missing EUV and stellar wind parameters that are required to predict the atmospheric evolution of terrestrial planets orbiting young suns.FUV Spectroscopy with COS:
The HST data will use COS with G130M, CENWAVE=1291 to record the emission lines
of C III (117.5 nm), Si III (120.6 nm), N V (123.8nm), C I (132.9nm), C II (133.5 nm), Fe
XXI (135.4nm), O V (137.1nm), O IV] (140.1nm), and Si IV (139.4, 140.3 nm). To resolve
the physical processes relevant to chromospheric and coronal heating, we require R |*|
15,000. To constrain the stellar wind density of DS Tuc A, we require signal-to-noise ~8
per resolution element at the peak of the O IV] 140 nm line. We used archival spectra of
the young G-type stars EK Dra and |*| Boo A [19,20] to compute S/N estimates for DS Tuc
A. We assumed the flux of EK Dra, scaled by the distance to DS Tuc, and then divided by
a factor of two to add margin for the slight stellar mass difference between the two stars.
Using the on-line STScI ETC, we estimate that 7,700 seconds (~three orbits) per visit will
be sufficient for detection of S/N |*| 8 per resolution element in the peak of the densitysensitive
O IV] features (COS.sp.1841043). This 3-orbit exposure time ensures high S/N
in all of the other lines of interest: S/N between 10 and 20 in the peak of several C I lines
and Fe XXI (COS.sp.1841045), S/N between 20 and 30 in N V (COS.sp.1841047) and S/N
> 35 in Si III, C II, and Si IV (COS.sp.1841044). This high-fidelity spectrum will allow us to identify temporal variability and will provide robust line-fit measurements of thermal
and non-thermal widths and line kinematics (Figure 2 below illustrates the line-profile
measurements that will be conducted on these data; this example was constructed from
archival observations of EK Dra, [20]).
The approved ground-based, TESS, and NICER programs will follow DS Tuc A over
several rotation periods (DS Tuc A|*|s rotation period is 2.85 days) in August 2023. To
explore the connection between time-variable phenomena (flares, CMEs) with magnetic
surface topology and X-ray output, we request four epochs spread over two rotation
periods; the four visits covering a stellar rotation period is a simplified version of the
observing cadence adopted for the ULLYSES monitoring stars [21]. Breaking the total
observing period into four visits also maximizes the chance of successful coordination with
the ground-based observations; multi-wavelength observations of transient stellar
phenomena is the crux of this proposal and the requested HST observing cadence has been
tailored accordingly. Therefore, the total time request for this GO proposal is 3 orbits x
4 visits = 12 orbits.
Target Acquisition: We did a quantitative ETC target acquisition calculation using the
STScI online tools, we scaled a Kurucz G8 V atmosphere model to V-magnitude of V =
8.23, and we find that an exposure time of approximately 7.4s are required
(COS.ta.1841052), using an imaging target acquisition in BOA+MIRRORA.
Instrument Safety: The same ETC calculations presented above (COS.sp.1841051) find no
bright object violations using the COS G130M 1291 mode, therefore these observations
present no risk to the instrument and are consistent with the COS 2025 observing
guidelines.PI: K. France - University of Colorado
Kevin France is the PI of the HST MUSCLES Treasury Survey (GO13650) and MEATS (GO16166) Survey to study the spectral and temporal properties of exoplanet host stars (France et al. 2016, 2018, 2020; Loyd et al. 2016; Youngblood et al. 2016). He is the co-PI of the follow-on Mega-MUSCLES (GO15071) and Mega-MEATS (16701) Surveys that focused on activity in stars optimal for planetary characterization with JWST. He was a member of the COS instrument and science teams; he is intimately familiar with HST-COS and -STIS instrument, data, and analysis procedures. His research group has developed numerous community tools for spectral and temporal analysis of COS and STIS data. Dr France has authored over 70 refereed publications on exoplanets, cool stars, and planet-forming disks using UV spectra from HST.
Vladimir Airapetian is Senior Astrophysicist at Heliophysics Science Division, NASA Goddard Space Flight Center and Research Professor at American University, DC. He is an internationally known expert in theoretical modeling of the Sun and young solar analogs including solar-stellar magnetic fields, flare physics, and impacts on planetary atmospheres. He leads several NASA projects relating to exoplanet habitability and astrobiology. He is responsible for MHD modeling of the corona-wind system as well as flare and CMEs from EK Dra.Stellar Physics and Stellar TypesExoplanets and Exoplanet Formation0falseSUPPORTEDEXT-STAREXTRA-SOLAR PLANETARY SYSTEMG V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.HD-222259AJ2000J2000COS/FUVSpectroscopicNoNoG130M1291/private/var/folders/bl/s7q0tqnn5gbcbyvcfnrhj2rh0004nc/T/OPVisit6585743935544581187.xmlTiming link suitability includes constraints ([02 After 01 by 0.5 to 2.5 days])The scheduling data was generated by CASM 31.1.CASM was run in Phase II mode.170000477900051.12909913997359(Tic-Visit
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