For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.
For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present.dm_FUVCont_cy31_sub1, kevin.france@colorado.edu-176810347Assigned ID: 3962
----- Attempting Submission 1 (Fri May 19 04:04:15 GMT 2023) -----
HST Phase I Proposal 3962 successfully submitted.
Receipt: # 3962-1For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
GS Acq Scenario may not be specified in Supported mode.
GS Acq Scenario may not be specified in Supported mode.
GS Acq Scenario may not be specified in Supported mode.
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
GS Acq Scenario may not be specified in Supported mode.
GS Acq Scenario may not be specified in Supported mode.
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
For the best data quality, it is generally required to use all four FP-POS positions when observing at a given COS cenwave.
GS Acq Scenario may not be specified in Supported mode.
GS Acq Scenario may not be specified in Supported mode.
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.Submission number 5. Moved STIS G140M lam1518 to slit position 52x0.2D1 to avoid detector glow associated with 3 orbit program.
Thanks, Kevin France - University of Colorado-139944180----- Attempting Submission 1 (Wed Aug 30 22:56:40 GMT 2023) -----
HST Phase II Proposal 17428 successfully submitted.
Receipt: # 17428-1
----- Attempting Submission 2 (Sat Sep 09 01:00:08 GMT 2023) -----
----- Attempting Submission 3 (Tue Dec 19 14:32:36 GMT 2023) -----
HST Phase II Proposal 17428 successfully submitted.
Receipt: # 17428-3
----- Attempting Submission 4 (Tue Dec 26 12:11:57 GMT 2023) -----
----- Attempting Submission 5 (Thu Feb 01 20:09:04 GMT 2024) -----The M dwarf FUV Continuum: A Missing Driver of Atmospheric Hazes in Exoplanet AtmospheresPhotochemical hazes are common in exoplanetary systems, serving as important reservoirs for atmospheric molecules while influencing our ability to measure the local physical conditions in a planet's atmosphere. Characterization and modeling of aerosol and hazes have taken on added importance as JWST examines exoplanet atmospheres in exquisite detail. Understanding the formation and composition of atmospheric hazes on all types of exoplanets requires knowledge of both the atmospheric spectra and the driving stellar ultraviolet radiation. A key area of uncertainty in modeling haze formation on planets around M dwarfs is the spectral shape and absolute flux level of the stellar far-ultraviolet (FUV) continuum. The quiescent FUV continuum flux is below the instrumental background level for essentially all of HST's previous M dwarf characterization programs, and resultant uncertainty in input conditions changes the predicted haze abundances by an order-of-magnitude on temperate exoplanets.
We propose a novel set of FUV spectroscopic observations with HST-COS to directly measure the quiescent FUV continuum flux in a small sample of benchmark M dwarfs for the first time. We will use a combination of COS G130M, G160M, and G185M settings to measure high-fidelity FUV continuum spectra in both quiescent and flare states, while avoiding the chromospheric emission lines that set the bright object avoidance levels for COS. We will release fully reduced FUV continuum spectra to support atmospheric models of haze formation, photochemistry, and simulated transmission spectra for a range of exoplanets observed with both HST and JWST.The target list includes three well-studied M dwarfs (Table 1); these are the brightest nearby
M dwarfs and are the only stars for which sufficient archival data exists to ensure the feasibility
of the observing program. By choosing historically well-studied M dwarfs, the proposed
data set holds important legacy value as benchmark objects for the physics of low-mass
stars and how those stars influence orbiting planets. These three targets have been safely
observed by HST-COS or -STIS previously and satisfy bright-object protection restrictions
when accounting for 'M dwarf flare safety margins' outlined by Osten et al (2017) in COS
ISR 2017-01(v3).
We will employ three COS spectroscopic observing modes for each star, and augment
those with FUV/NUV photometry from WFC3/UVIS. The COS spectroscopic modes are
chosen to access hundreds of Angstroms of FUV continuum spectra while avoiding the brightest
emission lines that are of concern for bright object protection (e.g., Ly-alpha, Si IV, C IV;
these bright emission lines are well studied by previous authors, see, e.g., Pagano et al. 2000;
Hawley et al. 2003; Melbourne et al. 2020 and references therein).
COS G130M CENWAVE 1222 is used to acquire spectra in the 1065-1207 Ang and
1224 -1365 range. This configuration has resulted in the only high-S/N measurement
of the quiescent FUV continuum on M dwarfs to date (GO16164; Feinstein et al. 2022)
and provides the empirical flux scaling used to estimate exposure times for this program
(Figure 2).
COS G160M CENWAVE 1577, Segment A only, is used to acquire spectra in the
1565 - 1755 Ang range. We turn the FUV MCP Segment B high-voltage to LOW for
these observations to mitigate bright object concerns from the C IV emission line.
COS G185M CENWAVE 1900 is used to acquire spectra in the 1782 - 1818 Ang, 1882 -1918 Ang, and 1982 - 2018 Ang regions in the three spectroscopic stripes on the COS
NUV MAMA detector.
All COS observations will be acquired in photon-counting time-tag mode (TTAG) to
facilitate lightcurve creation on arbitrary timescales depending on the frequency and amplitude
of any observed flares. This temporal separation will allow us to measure the spectrum
of the FUV continuum from these objects in both flare and quiescent states. The COS
M-mode gratings were selected because the high-S/N of these bright M dwarfs will allow
us to confidently identify the emission line and continuum regions in the spectra (see, e.g.,
Feinstein et al. 2022). The COS M modes provide the optimal combination of sensitivity (to
detect the faint FUV continuum) and spectral resolution to separate the line and continuum
regions.
To connect the new COS spectroscopy of the FUV continuum with the better characterized,
lambda > 2200 Ang NUV continuum and emission line spectra of M dwarfs (see, e.g., Loyd
et al. 2016; Tilipman et al. 2021, Figure 2), we will acquire photometric observations with
the WFC3 UVIS F218W (lambda1950 - 2450 Ang), FQ232N (lambda 2300 - 2350 Ang), and FQ243N (lambda 2400 - 2450 Ang) filters. S/N = 40 photometric
precision in all three filters can be achieved in approximately one orbit per star.
FUV Continuum Extraction: We will extract the FUV continuum from our observed
spectra following the general procedures outlined by France et al. (2014). Because every
high-S/N UV M dwarf spectrum reveals a wealth of strong and weak emission lines, we will
create a spectral mask of the FUV continuum by hand, isolating 0.5- 0.7 Ang (approximately 7
spectral resolution elements) spectral regions that are free of observed emission line features.
We will cross-reference these regions against M dwarf UV line lists (e.g., Pagano et al.
2000). We refer to these as "binned FUV continuum spectra". Each individual binned FUV
continuum point is taken as the median of the flux in the 0.5 - 0.7Ang spectral window, and the
error on each individual binned FUV continuum point is taken to be the standard deviation
about the mean flux in the bin. This process yields 30 - 50 binned data points per 100 Ang
of spectral coverage (Froning et al. 2019), demonstrating that there will be ample empirical
samples of the FUV continuum emission across the FUV band. Finally, we will take two
approaches to determining the overall FUV continuum spectrum for our targets: 1) we will
scale M dwarf atmosphere models (such as Peacock et al. 2019, Figure 2 and Tilipman et
al. 2021) to the measured, binned FUV continuum spectra to explore whether or not these
models accurately reproduce the shape of the observed continuum, and 2) we will fit a simple
polynomial function to the binned FUV continuum spectra (France et al. 2014) to provide
an empirical flux level across the FUV band without introducing the biases of any particular
spectral synthesis model.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.
Co-I Youngblood is the PI of multiple HST programs to study the UV emission from M dwarfs, including serving as co-PI of the Mega_MEATS (16701) survey. She is a member of the MUSCLES and Mega-MUSCLES teams, and has experience analyzing M dwarf flares.
Co-I Pineda has extensive experience in the study of magnetic activity in low-mass stars. He leads several HST programs targeting M-dwarfs (HST-14640, 16197) in the UV, measuring their spectra and flare behavior.
Co-I Dr. Froning is the PI of the HST Mega-MUSCLES Treasury Survey, a large program using HST, Chandra, XMM, Swift, and several ground-based telescopes to obtain pan-chromatic spectroscopy of a broad survey of M stars to evaluate their high energy irradiance environment, exoplanet atmospheric parameters and biomarker production, and the potential for habitabilty. Dr. Froning is an experienced observer and instrument developer with expertise in stellar astrophysics and the design and development of UV/OIR imagers and spectrographs for ground and space facilities. She was the Project Scientist for the Cosmic Origins Spectrograph and an expert on UV spectroscopy.
Eliza Kempton is an expert in the theoretical modeling of exoplanet atmospheres, specifically focusing on
photochemistry, radiative transfer, and spectroscopic observables. She and her team at UMD (Matej Malik and
DJ Teal) will provide guidance to the team on how to best incorporate the UV data products into exoplanet
atmosphere models and will lead an effort to perform photochemical calculations with VULCAN and Atmos for
planets orbiting the observed host stars. She has been a theorist co-I on 13 HST programs totaling over 300
orbits, and she serves as PI or co-PI on two selected JWST Cycle 1 observing programs.
David Wilson is a member of the Mega-MUSCLES team and PI of three previous HST programs (13719, 15189, 16449) obtaining ultraviolet spectroscopy of stars using both COS and STIS, and has published multiple first-author papers based on HST data. He has extensive experience using the HST calibration tools to perform the non-standard reductions necessary for studying late-type stars.Exoplanets and Exoplanet FormationStellar Physics and Stellar Types0falsetruefalsefalsefalsefalseSUPPORTEDEXT-STARM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000EXT-STARM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000EXT-STARM V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG185M1900COS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG185M1900WFC3/UVISImagingNoNoF218WWFC3/UVISImagingNoNoFQ232NWFC3/UVISImagingNoNoFQ243NCOS/FUVSpectroscopicNoNoG130M1222COS/FUVSpectroscopicNoNoG160M1577COS/NUVSpectroscopicNoNoG185M1900WFC3/UVISImagingNoNoF218WWFC3/UVISImagingNoNoFQ232NWFC3/UVISImagingNoNoFQ243NWFC3/UVISImagingNoNoF218WWFC3/UVISImagingNoNoFQ232NWFC3/UVISImagingNoNoFQ243NPOS-TARGDITHER0.145LINEfalsefalse446.86SPIRAL2falseThe scheduling data was generated by CASM 32.0.CASM was run in Phase II mode.1711146955000246.2683050803845(Tic-Visit
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