MUSCLES Treasury Survey - Submission #1. Kevin France (kevin.france@colorado.edu), 25 Mar 2014.
-531906070
Assigned ID: 15
----- Attempting Submission 1 (Tue Mar 25 17:44:48 GMT 2014) -----
HST Phase I Proposal 15 (muscles22_kf4.apt) successfully submitted.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
ORBITAL VISIBILITY OVERRUN
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
ORBITAL VISIBILITY OVERRUN
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
Submission 3 - Kevin France (kevin.france@colorado.edu; 303-492-1429). September 4th 2014.
S1: STIS target acq and COS FP-POS strategies modified following discussion with STScI personnel.
S2: STIS observation windows set to keep the geocoronal LyA signal near the ISM absorption trough line-center.
S3: Moved GJ 832 COS TAs from imaging to NUV spectroscopic, per STScI request.
-596326397
----- Attempting Submission 1 (Thu Jul 10 23:50:44 GMT 2014) -----
HST Phase II Proposal 13650 (muscles22_phase2_kf7.apt) successfully submitted.
----- Attempting Submission 2 (Mon Jul 14 20:42:31 GMT 2014) -----
----- Attempting Submission 3 (Fri Sep 05 03:29:01 GMT 2014) -----
The MUSCLES Treasury Survey: Measurements of the Ultraviolet Spectral Characteristics of Low-mass Exoplanetary Systems
It has recently been discovered that 10 - 50% of M dwarfs host Earth-size planets in their habitable zones. Furthermore, the nearest potentially habitable super-Earths orbit M dwarfs, meaning that these systems likely represent our best chance to discover habitable worlds in the coming decade. The ultraviolet (UV) spectrum incident upon Earth-like planets drives the dissociation of water and CO2, the production of O2 and ozone, and may determine their ultimate habitability. At present, we lack the observational and theoretical basis to predict the energetic radiation spectrum (X-ray through UV) of an M dwarf. UV variability of low-mass exoplanet host stars, in particular the possibly sterilizing effect of flare activity, is almost completely unexplored observationally. This proposal aims to acquire the critical UV observations of low-mass host stars now, providing a treasury database for studies of exemplary nearby exoplanetary systems and potentially habitable worlds not yet discovered. Building on our successful pilot program of spectrally and temporally resolved UV radiation fields, we propose the MUSCLES Treasury Survey: a UV survey of nearby low-mass exoplanetary host stars. Using HST-COS and STIS, we will observe the 1150 - 5700A fluxes, reconstruct the important Ly-alpha emission lines, and use these data to estimate the extreme-UV (200 - 912A) irradiances incident upon exoplanetary atmospheres. The UV data will be complemented with contemporaneous X-ray and ground-based observations as well as new M dwarf atmosphere models to constrain atmospheric heating rates and provide a baseline for long-term ground-based studies of these systems.
The target list was chosen to cover a broad range of stellar types (K1V - M6V), exoplanet masses, and semi-major axes; including most of the known M dwarf exoplanet hosts at d < 13pc (7/12), while excluding extreme flare stars (e.g. GJ 674) that require intensive multi-wavelength monitoring to clear HST instrument safety protocols.
Observing Modes: In order to obtain a full census of the UV emission incident on the
habitable zones around low-mass stars, we require spectral coverage from 1150- 3100 Ang:
the G130M, G160M, and G230L modes of COS, and the G/E140M and G230L modes of STIS.
In the FUV (except Ly-alpha) we will use COS G130M and COS G160M. Emission from Ly-alpha, Si IV, C IV,
and He II is particularly interesting because these lines provide constraints on the Lyman
continuum/EUV (200 < lam < 900 Ang) irradiance in these systems. COS is
essential for a moderate spectral resolution line census as the lower effective area and higher
detector background of STIS make observations of all but the very brightest emission line
(H I Ly-alpha) prohibitively time consuming. We will use the medium resolution COS
modes to resolve chromospheric lines and maximize contrast from narrow H2 features.
At NUV wavelengths, we will use STIS G230L (lam > 2200 Ang NUV continuum, Fe II
2400 and 2600, and Mg II 2800), but we will take advantage of the superior sensitivity
of the COS G230L mode to observe the 1750 - 2200 Ang region that is important to the
photodissociation of O2 and the production of O3. For targets that exceed the G230L
bright-object limit, we will use the higher-resolution E230M mode (CENWAVE1978 + CENWAVE2707 settings).
E230H observations of the Mg II emission lines on the brightest K dwarfs will allow us
to constrain the properties of their astrospheres. In order to calibrate the UV data to
visible/IR photospheric models and the ground-based spectra, we will also acquire short
optical observations with STIS G430L.
We will use the G140M mode of STIS with the 52''x 0.1" slit to measure the Ly-alpha
profile for our M dwarf targets. In our Cycle 19 pilot program, we demonstrated that this
technique can produce high-quality measurements of the local Ly-alpha flux. For the brighter K
dwarfs, we will employ the STIS E140M mode, using the 0.2"
x 0.06" slit. Ly-alpha experiences absorption from the intervening local ISM, and the line must be reconstructed to provide a
reliable measure of the local Ly-alpha radiation field in these exoplanetary systems.
Short duration (minutes-to-hours) flares are the most common on M dwarfs (Loyd &
France 2014; Kowalski et al. 2009), and we will use the most sensitive UV photon-counting mode on HST (COS G130M) to perform 8-hour variability studies (5 contiguous spacecraft orbits) of characteristic chromospheric and transition region lines
(C II, Si III, Si IV, and N V) for each planet host.
This observing strategy naturally splits each target campaign into 3 HST visits: 1) COS G130M, 2) COS G160M+G230L, 3)
STIS G/E140M+G230L+G430L that can be linked within a day of each other.
Exposure Time Calculations: We estimated the expected flux from our target sample
using the observed quiescent spectrum of GJ 876, scaled to the distance of the target star.
For the K-dwarf targets, we used STIS observations of HD 37394 (K1.5V), obtained from
the StarCat database (Ayres 2010). The 5 orbit COS G130M variability observations will
produce deep spectral observations in the 1150 - 1420 Ang range for all targets. For the
remaining UV wavelengths, we estimated exposure times based on the minimum amount of
time required to achieve S/N 10 per resolution element in the characteristic emission lines:
Ly-alpha (STIS E/G140M, lam_meas = 1216.0 Ang), C IV (COS G160M), and Mg II (STIS G230L).
We estimate S/N 5 in the NUV continuum (lam 1900 Ang, COS G230L and lam 2850 Ang, STIS
G230L), and S/N > 20 in the optical (STIS G430L). Using the STScI on-line Exposure
Time Calculator, we have estimated the total exposure time per target given in Table 1
(assuming 2,900 seconds per orbit and incorporating instrument overheads), resulting in a
total observing time allocation request of 125 orbits for the 15 stars in this program.
BOT ran for all target fields, 07/04/14. All cleared. Only safety flags were when APT did not know the spectral type of the target star: epsilon Eri, GJ832, HD40307, HD85512, HD97658.
EXTRA-SOLAR PLANETS
0
Regular
false
true
120.0
20.0
0.0
true
false
false
SUPPORTED
EXT-STAR
EXTRA-SOLAR PLANETARY SYSTEM
K V-IV
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
EXT-STAR
EXTRA-SOLAR PLANETARY SYSTEM
M V-IV
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
(V-IL-AQR)
EXT-STAR
EXTRA-SOLAR PLANETARY SYSTEM
M V-IV
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
(LHS-3685)
EXT-STAR
A4-A9 V-IV
EXTRA-SOLAR PLANETARY SYSTEM
M V-IV
This object was generated by the targetselector and retrieved from the SIMBAD database. but the APT coordinates did not match the coordinates taht I found in Simbad on 06/2/6/14 - kf, and the target confirmation charts show the aperture missing the target. Reverting to successful Cycle 19(12464) coordinates and propoer motions.
J2000
J2000
(V-HO-LIB)
EXT-STAR
EXTRA-SOLAR PLANETARY SYSTEM
M V-IV
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
(LHS-443)
EXT-STAR
EXTRA-SOLAR PLANETARY SYSTEM
M V-IV
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
(LHS-196)
EXT-STAR
EXTRA-SOLAR PLANETARY SYSTEM
M V-IV
This object was generated by the targetselector and retrieved from the SIMBAD database. Coords differ from what Simbad has - 06/26/14 - kf. I reverted to the coordinates used in Cycle 19 (12464) and the target confirmation chart showed better centered agreement between the pink cross and the stellar image.
J2000
J2000
(LHS-310)
EXT-STAR
EXTRA-SOLAR PLANETARY SYSTEM
K V-IV
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
(LHS-2201)
EXT-STAR
EXTRA-SOLAR PLANETARY SYSTEM
M V-IV
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
(LHS-3275)
EXT-STAR
EXTRA-SOLAR PLANETARY SYSTEM
K V-IV
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
EXT-STAR
M V-IV
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
EXT-STAR
M V-IV
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
EXT-STAR
G III-I
M V-IV
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
EXT-STAR
M V-IV
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
EXT-STAR
EXTRA-SOLAR PLANETARY SYSTEM
K V-IV
J2000
J2000
STIS/NUV-MAMA
Spectroscopic
No
No
E230M
1978
STIS/FUV-MAMA
Spectroscopic
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No
E140M
1425
STIS/NUV-MAMA
Spectroscopic
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E230M
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STIS/CCD
Spectroscopic
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No
G430L
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STIS/NUV-MAMA
Spectroscopic
No
No
E230H
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COS/FUV
Spectroscopic
No
No
G130M
1309
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/NUV
Spectroscopic
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No
G230L
2950
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/FUV-MAMA
Spectroscopic
No
No
G140M
1222
STIS/CCD
Spectroscopic
No
No
G430L
4300
COS/FUV
Spectroscopic
No
No
G130M
1309
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/NUV
Spectroscopic
No
No
G230L
2950
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/FUV-MAMA
Spectroscopic
No
No
G140M
1222
STIS/CCD
Spectroscopic
No
No
G430L
4300
COS/FUV
Spectroscopic
No
No
G130M
1309
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/NUV
Spectroscopic
No
No
G230L
2950
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/FUV-MAMA
Spectroscopic
No
No
G140M
1222
STIS/CCD
Spectroscopic
No
No
G430L
4300
COS/FUV
Spectroscopic
No
No
G130M
1309
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/NUV
Spectroscopic
No
No
G230L
2950
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/FUV-MAMA
Spectroscopic
No
No
G140M
1222
STIS/CCD
Spectroscopic
No
No
G430L
4300
COS/FUV
Spectroscopic
No
No
G130M
1309
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/NUV
Spectroscopic
No
No
G230L
2950
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/FUV-MAMA
Spectroscopic
No
No
G140M
1222
STIS/CCD
Spectroscopic
No
No
G430L
4300
COS/FUV
Spectroscopic
No
No
G130M
1309
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/NUV
Spectroscopic
No
No
G230L
2950
STIS/NUV-MAMA
Spectroscopic
No
No
G230L
2376
STIS/FUV-MAMA
Spectroscopic
No
No
G140M
1222
STIS/CCD
Spectroscopic
No
No
G430L
4300
COS/FUV
Spectroscopic
No
No
G130M
1309
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/NUV
Spectroscopic
No
No
G230L
2950
STIS/NUV-MAMA
Spectroscopic
No
No
E230M
1978
STIS/FUV-MAMA
Spectroscopic
No
No
E140M
1425
STIS/NUV-MAMA
Spectroscopic
No
No
E230M
2707
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2713
COS/FUV
Spectroscopic
No
No
G130M
1309
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/NUV
Spectroscopic
No
No
G230L
2950
STIS/NUV-MAMA
Spectroscopic
No
No
E230M
1978
STIS/FUV-MAMA
Spectroscopic
No
No
E140M
1425
STIS/NUV-MAMA
Spectroscopic
No
No
E230M
2707
STIS/CCD
Spectroscopic
No
No
G430L
4300
STIS/NUV-MAMA
Spectroscopic
No
No
E230H
2713
COS/FUV
Spectroscopic
No
No
G130M
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COS/FUV
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G160M
1600
COS/NUV
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No
G230L
2950
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No
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G230L
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STIS/FUV-MAMA
Spectroscopic
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No
G140M
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STIS/CCD
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G430L
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COS/FUV
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G130M
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COS/FUV
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G160M
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COS/NUV
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No
G230L
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STIS/NUV-MAMA
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E230M
1978
STIS/FUV-MAMA
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G140M
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No
No
E230M
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STIS/CCD
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No
G430L
4300
COS/FUV
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No
G130M
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COS/FUV
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No
No
G160M
1600
COS/NUV
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G230L
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No
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COS/FUV
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No
G160M
1600
COS/FUV
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No
G160M
1600
COS/FUV
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No
G160M
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true
5
0
Duplicate of visit 15 which failed during a HST safing event.
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false
5
0
Timing link suitability includes constraints ([17 After 16 by at most 1.0 days])
The scheduling data was generated by CASM 22.2.
CASM was run in Phase II mode.
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false
2
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Timing link suitability includes constraints ([17 After 16 by at most 1.0 days] [18 After 17 by at most 1.0 days])
The scheduling data was generated by CASM 22.2.
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true
3
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Timing link suitability includes constraints ([18 After 17 by at most 1.0 days])
The scheduling data was generated by CASM 22.2.
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true
5
1
Timing link suitability includes constraints ([20 After 19 by at most 1.0 days])
The scheduling data was generated by CASM 22.2.
CASM was run in Phase II mode.
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true
3
0
Timing link suitability includes constraints ([20 After 19 by at most 1.0 days] [21 After 20 by at most 1.0 days])
The scheduling data was generated by CASM 22.2.
CASM was run in Phase II mode.
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true
3
0
Timing link suitability includes constraints ([21 After 20 by at most 1.0 days])
The scheduling data was generated by CASM 22.2.
CASM was run in Phase II mode.
(Tic-Visit
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true
5
0
Timing link suitability includes constraints ([23 After 22 by at most 1.0 days])
The scheduling data was generated by CASM 22.2.
CASM was run in Phase II mode.
(Tic-Visit
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true
3
0
Timing link suitability includes constraints ([23 After 22 by at most 1.0 days] [24 After 23 by at most 1.0 days])
The scheduling data was generated by CASM 22.2.
CASM was run in Phase II mode.
(Tic-Visit
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(Tic-Orbit
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)
true
3
0
Timing link suitability includes constraints ([24 After 23 by at most 1.0 days])
The scheduling data was generated by CASM 22.2.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 13650
:visit-id "24"
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:trans-version "20140605"
:date "08-Jul-2014 14:22:08.0"
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(Tic-Obset
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(Tic-Orbit
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)
(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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:low-sky "N"
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)
true
5
0
Timing link suitability includes constraints ([26 After 25 by at most 1.0 days])
The scheduling data was generated by CASM 22.2.
CASM was run in Phase II mode.
This needs to go as closely as possible to visits 26 & 27. 062.01:20:57 - 08:37:45 is a tested spot.
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82.4534999540906
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)
(Tic-Obset
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(Tic-Orbit
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