15304 - collecting the puzzle pieces: completing hst's uv ... · dr. laetitia delrez (coi)...
TRANSCRIPT
![Page 1: 15304 - Collecting the Puzzle Pieces: Completing HST's UV ... · Dr. Laetitia Delrez (CoI) (ESA Member) University of Cambridge lcd44@cam.ac.uk Prof. Brice-Olivier Demory (CoI) (ESA](https://reader033.vdocuments.mx/reader033/viewer/2022060604/60589968f5c5d027dd11c222/html5/thumbnails/1.jpg)
15304 - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the
TRAPPIST-1 System ahead of JWSTCycle: 25, Proposal Category: GO
(UV Initiative, JWST Initative)
(Availability Mode: SUPPORTED)
INVESTIGATORSName Institution E-MailProf. Julien de Wit (PI) (Contact) Massachusetts Institute of Technology [email protected]. Nikole Lewis (CoI) Cornell University [email protected]. Vlada Stamenkovic (CoI) Jet Propulsion Laboratory [email protected]. Michael Gillon (CoI) (ESA Member) Universite de Liege [email protected]. Adam J. Burgasser (CoI) University of California - San Diego [email protected]. Laetitia Delrez (CoI) (ESA Member) Universite de Liege [email protected]. Brice-Olivier Demory (CoI) (ESA Member) University of Bern [email protected]. Emmanuel Jehin (CoI) (ESA Member) Universite de Liege [email protected]. Susan Lederer (CoI) NASA Johnson Space Center [email protected]. Hannah Wakeford (CoI) (ESA Member) University of Bristol [email protected]. Didier Queloz (CoI) (ESA Member) University of Cambridge [email protected]. Amaury Triaud (CoI) (ESA Member) University of Birmingham [email protected]. Valerie Van Grootel (CoI) (ESA Member) Universite de Liege [email protected]. Emeline Bolmont (CoI) (ESA Member) Universite de Namur [email protected]. Franck Selsis (CoI) (ESA Member) Universite de Bordeaux [email protected]. Sean Raymond (CoI) (ESA Member) Universite de Bordeaux [email protected]. Jeremy Leconte (CoI) (ESA Member) Universite de Bordeaux [email protected]. Sara Seager (CoI) Massachusetts Institute of Technology [email protected] Knapp (CoI) Massachusetts Institute of Technology [email protected]
Proposal 15304 (STScI Edit Number: 63, Created: Tuesday, December 8, 2020 at 9:02:12 AM Eastern Standard Time) - Overview
1
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Name Institution E-MailDr. Vincent Bourrier (CoI) (ESA Member) (Contact)
Observatoire de Geneve [email protected]
Prof. David Ehrenreich (CoI) (ESA Member) Observatoire de Geneve [email protected]. Jeff A. Valenti (CoI) Space Telescope Science Institute [email protected]
VISITSVisit Targets used in Visit Configurations used in Visit Orbits Used Last Orbit Planner Run OP Current
with Visit?01 (1) 2MASS-J23062928-0502285 WFC3/IR 4 08-Dec-2020 09:00:41.0 yes
02 (1) 2MASS-J23062928-0502285 WFC3/IR 4 08-Dec-2020 09:00:50.0 yes
03 (1) 2MASS-J23062928-0502285 WFC3/IR 4 08-Dec-2020 09:01:01.0 yes
04 (1) 2MASS-J23062928-0502285 WFC3/IR 4 08-Dec-2020 09:01:09.0 yes
07 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
6 08-Dec-2020 09:01:14.0 yes
31 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
7 08-Dec-2020 09:01:17.0 yes
32 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
7 08-Dec-2020 09:01:21.0 yes
33 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
5 08-Dec-2020 09:01:24.0 yes
16 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:01:27.0 yes
29 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
6 08-Dec-2020 09:01:30.0 yes
30 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
6 08-Dec-2020 09:01:33.0 yes
05 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:01:36.0 yes
Proposal 15304 (STScI Edit Number: 63, Created: Tuesday, December 8, 2020 at 9:02:12 AM Eastern Standard Time) - Overview
2
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Visit Targets used in Visit Configurations used in Visit Orbits Used Last Orbit Planner Run OP Currentwith Visit?
08 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:01:38.0 yes
B1 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:01:40.0 yes
B2 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:01:42.0 yes
C1 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:01:45.0 yes
C2 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:01:47.0 yes
C3 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:01:49.0 yes
D1 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:01:51.0 yes
E1 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:01:53.0 yes
E2 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:01:56.0 yes
F1 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:01:58.0 yes
F2 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:02:00.0 yes
F3 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:02:02.0 yes
G1 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:02:05.0 yes
G2 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:02:07.0 yes
Proposal 15304 (STScI Edit Number: 63, Created: Tuesday, December 8, 2020 at 9:02:12 AM Eastern Standard Time) - Overview
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125 Total Orbits Used
ABSTRACT
Using the Spitzer Space Telescope, our team has discovered 7 Earth-sized planets around the nearby Ultra-cool dwarf star TRAPPIST-1. These
planets are the first to be simultaneously Earth-sized, temperate, and amenable for in-depth atmospheric studies with space-based observatories
(notably, JWST). TRAPPIST-1's system thus provides us with the first opportunity to probe the atmospheres of Earth-sized exoplanets and search for
signs of habitability beyond our solar system, which will require spectral information from the UV to the IR to complete their atmospheric puzzles.
We request 114 HST orbits to complete the UV+NIR survey of the 7 planets in preparation for their in-depth followup with JWST. The suggested
low-density of the planets combined with their complex orbital resonance chain indicate that they migrated inward to their current positions and may
harbor large water rich reservoir or leftover primordial H2 atmospheres. We have already ruled out the presence of clear H2 atmospheres for the 5
innermost planets using WFC3 and are requesting 16 WFC3 orbits to complete the TRAPPIST-1 NIR reconnaissance survey. Our primary request
consists in 98 STIS orbits to complete the survey for extended H-exospheres around each of the planets. H-exospheres are the most accessible
observables for volatile reservoirs, which have not been ruled out by our WFC3 observations. Exosphere detection is only amenable using HST
unique capabilities in the UV and are pivotal to guide JWST's in-depth followup. The combined information from HST's UV and NIR observations
will allow us put the first critical pieces of the atmospheric puzzle in place for these temperate earth-sized worlds.
OBSERVING DESCRIPTION
This program will observe two transits of each TRAPPIST-1 planets with STIS (in LY-a) to search for signs of exospheres while acquiring extra
baseline measurements to monitor the star's activity.
In addition, 16 WFC3 orbits to complete the TRAPPIST-1 NIR reconnaissance survey that has already ruled out the presence of clear H2
atmospheres for the 5 innermost planets.
Visit Targets used in Visit Configurations used in Visit Orbits Used Last Orbit Planner Run OP Currentwith Visit?
H1 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:02:09.0 yes
H2 (1) 2MASS-J23062928-0502285WAVE
STIS/CCDSTIS/FUV-MAMA
4 08-Dec-2020 09:02:12.0 yes
Proposal 15304 (STScI Edit Number: 63, Created: Tuesday, December 8, 2020 at 9:02:12 AM Eastern Standard Time) - Overview
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Vis
itProposal 15304, WFC3 transit of g (3) (01), completed Tue Dec 08 14:02:12 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: WFC3/IR
Special Requirements: SCHED 100%; Period 12.35351378 D AND ZERO-PHASE HJD2457665.257828620
Dia
gn
ost
ics (WFC3 transit of g (3) (01)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(WFC3 transit of g (3) (01)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(WFC3 transit of g (3) (01)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(WFC3 transit of g (3) (01)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 (1) 2MASS-J23062928-0502285
WFC3/IR, MULTIACCUM,GRISM256
F139M NSAMP=10;
SAMP-SEQ=RAPID
PHASE 0 TO 0.0014 2.77815 Secs (2.778 Secs)
[==>]
[1]
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2 (1) 2MASS-J23062928-0502285
WFC3/IR, MULTIACCUM,GRISM256
G141 NSAMP=6;
SAMP-SEQ=SPARS25
SPATIAL SCAN 0.02,90.0 Degrees,Forward
112.00801 Secs X 60 (6720.481 Secs)
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[1]
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[3]
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Orb
it S
tru
ctu
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Vis
itProposal 15304, WFC3 transit of h (1) (02), completed Tue Dec 08 14:02:13 GMT 2020
Diagnostic Status: No Diagnostics
Scientific Instruments: WFC3/IR
Special Requirements: SCHED 100%; Period 18.76745243 D AND ZERO-PHASE HJD2457662.459224910
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 (1) 2MASS-J23062928-0502285
WFC3/IR, MULTIACCUM,GRISM256
F139M NSAMP=10;
SAMP-SEQ=RAPID
PHASE 0 TO 0.0011;
GS ACQ SCENARIO PAIR
Sequence 1-2 Non-Int in WFC3 transit ofh (1) (02)
2.77815 Secs (2.778 Secs)
[==>][1]
2 (1) 2MASS-J23062928-0502285
WFC3/IR, MULTIACCUM,GRISM256
G141 NSAMP=6;
SAMP-SEQ=SPARS25
SPATIAL SCAN 0.02,90.0 Degrees,Forward
Sequence 1-2 Non-Int in WFC3 transit ofh (1) (02)
112.00801 Secs X 12 (1344.096 Secs)
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[1]
3 (1) 2MASS-J23062928-0502285
WFC3/IR, MULTIACCUM,GRISM256
G141 NSAMP=6;
SAMP-SEQ=SPARS25
SPATIAL SCAN 0.02,90.0 Degrees,Forward
Sequence 3-3 Non-Int in WFC3 transit ofh (1) (02)
112.00801 Secs X 13 (1456.104 Secs)
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4 (1) 2MASS-J23062928-0502285
WFC3/IR, MULTIACCUM,GRISM256
G141 NSAMP=6;
SAMP-SEQ=SPARS25
SPATIAL SCAN 0.02,90.0 Degrees,Forward
Sequence 4-4 Non-Int in WFC3 transit ofh (1) (02)
112.00801 Secs X 13 (1456.104 Secs)
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[3]
5 (1) 2MASS-J23062928-0502285
WFC3/IR, MULTIACCUM,GRISM256
G141 NSAMP=6;
SAMP-SEQ=SPARS25
SPATIAL SCAN 0.02,90.0 Degrees,Forward
Sequence 5-5 Non-Int in WFC3 transit ofh (1) (02)
112.00801 Secs X 13 (1456.104 Secs)
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Orb
it S
tru
ctu
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Vis
itProposal 15304, WFC3 transit of h (2) (03), completed Tue Dec 08 14:02:13 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: WFC3/IR
Special Requirements: SCHED 100%; BETWEEN 2018.200:18:00:00 AND 2018.200:19:00:00
Dia
gn
ost
ics (WFC3 transit of h (2) (03)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(WFC3 transit of h (2) (03)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(WFC3 transit of h (2) (03)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(WFC3 transit of h (2) (03)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(WFC3 transit of h (2) (03)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 (1) 2MASS-J23062928-0502285
WFC3/IR, MULTIACCUM,GRISM256
F139M NSAMP=10;
SAMP-SEQ=RAPID
Sequence 1-2 Non-Int in WFC3 transit ofh (2) (03)
2.77815 Secs (2.778 Secs)
[==>] [1]
2 (1) 2MASS-J23062928-0502285
WFC3/IR, MULTIACCUM,GRISM256
G141 NSAMP=6;
SAMP-SEQ=SPARS25
SPATIAL SCAN 0.02,90.0 Degrees,Forward
Sequence 1-2 Non-Int in WFC3 transit ofh (2) (03)
112.00801 Secs X 14 (1568.112 Secs)
[==>(Copy 1)]
[==>(Copy 2)]
[==>(Copy 3)]
[==>(Copy 4)]
[==>(Copy 5)]
[==>(Copy 6)]
[==>(Copy 7)]
[==>(Copy 8)]
[==>(Copy 9)]
[==>(Copy 10)]
[==>(Copy 11)]
[==>(Copy 12)]
[==>(Copy 13)]
[==>(Copy 14)]
[1]
3 (1) 2MASS-J23062928-0502285
WFC3/IR, MULTIACCUM,GRISM256
G141 NSAMP=6;
SAMP-SEQ=SPARS25
SPATIAL SCAN 0.02,90.0 Degrees,Forward
Sequence 3-3 Non-Int in WFC3 transit ofh (2) (03)
112.00801 Secs X 16 (1792.128 Secs)
[==>(Copy 1)]
[==>(Copy 2)]
[==>(Copy 3)]
[==>(Copy 4)]
[==>(Copy 5)]
[==>(Copy 6)]
[==>(Copy 7)]
[==>(Copy 8)]
[==>(Copy 9)]
[==>(Copy 10)]
[==>(Copy 11)]
[==>(Copy 12)]
[==>(Copy 13)]
[==>(Copy 14)]
[==>(Copy 15)]
[==>(Copy 16)]
[2]
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4 (1) 2MASS-J23062928-0502285
WFC3/IR, MULTIACCUM,GRISM256
G141 NSAMP=6;
SAMP-SEQ=SPARS25
SPATIAL SCAN 0.02,90.0 Degrees,Forward
Sequence 4-4 Non-Int in WFC3 transit ofh (2) (03)
112.00801 Secs X 16 (1792.128 Secs)
[==>(Copy 1)]
[==>(Copy 2)]
[==>(Copy 3)]
[==>(Copy 4)]
[==>(Copy 5)]
[==>(Copy 6)]
[==>(Copy 7)]
[==>(Copy 8)]
[==>(Copy 9)]
[==>(Copy 10)]
[==>(Copy 11)]
[==>(Copy 12)]
[==>(Copy 13)]
[==>(Copy 14)]
[==>(Copy 15)]
[==>(Copy 16)]
[3]
5 (1) 2MASS-J23062928-0502285
WFC3/IR, MULTIACCUM,GRISM256
G141 NSAMP=6;
SAMP-SEQ=SPARS25
SPATIAL SCAN 0.02,90.0 Degrees,Forward
Sequence 5-5 Non-Int in WFC3 transit ofh (2) (03)
112.00801 Secs X 15 (1680.12 Secs)
[==>(Copy 1)]
[==>(Copy 2)]
[==>(Copy 3)]
[==>(Copy 4)]
[==>(Copy 5)]
[==>(Copy 6)]
[==>(Copy 7)]
[==>(Copy 8)]
[==>(Copy 9)]
[==>(Copy 10)]
[==>(Copy 11)]
[==>(Copy 12)]
[==>(Copy 13)]
[==>(Copy 14)]
[==>(Copy 15)]
[4]
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Orb
it S
tru
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Vis
itProposal 15304, WFC3 transit of h (3) (04), completed Tue Dec 08 14:02:14 GMT 2020
Diagnostic Status: No Diagnostics
Scientific Instruments: WFC3/IR
Special Requirements: SCHED 100%; Period 18.76745243 D AND ZERO-PHASE HJD2457662.459224910
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 (1) 2MASS-J23062928-0502285
WFC3/IR, MULTIACCUM,GRISM256
F139M NSAMP=10;
SAMP-SEQ=RAPID
PHASE 0 TO 0.0011;
GS ACQ SCENARIO PAIR
Sequence 1-2 Non-Int in WFC3 transit ofh (3) (04)
2.77815 Secs (2.778 Secs)
[==>][1]
2 (1) 2MASS-J23062928-0502285
WFC3/IR, MULTIACCUM,GRISM256
G141 NSAMP=6;
SAMP-SEQ=SPARS25
SPATIAL SCAN 0.02,90.0 Degrees,Forward
Sequence 1-2 Non-Int in WFC3 transit ofh (3) (04)
112.00801 Secs X 12 (1344.096 Secs)
[==>(Copy 1)]
[==>(Copy 2)]
[==>(Copy 3)]
[==>(Copy 4)]
[==>(Copy 5)]
[==>(Copy 6)]
[==>(Copy 7)]
[==>(Copy 8)]
[==>(Copy 9)]
[==>(Copy 10)]
[==>(Copy 11)]
[==>(Copy 12)]
[1]
3 (1) 2MASS-J23062928-0502285
WFC3/IR, MULTIACCUM,GRISM256
G141 NSAMP=6;
SAMP-SEQ=SPARS25
SPATIAL SCAN 0.02,90.0 Degrees,Forward
Sequence 3-3 Non-Int in WFC3 transit ofh (3) (04)
112.00801 Secs X 13 (1456.104 Secs)
[==>(Copy 1)]
[==>(Copy 2)]
[==>(Copy 3)]
[==>(Copy 4)]
[==>(Copy 5)]
[==>(Copy 6)]
[==>(Copy 7)]
[==>(Copy 8)]
[==>(Copy 9)]
[==>(Copy 10)]
[==>(Copy 11)]
[==>(Copy 12)]
[==>(Copy 13)] [2]
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4 (1) 2MASS-J23062928-0502285
WFC3/IR, MULTIACCUM,GRISM256
G141 NSAMP=6;
SAMP-SEQ=SPARS25
SPATIAL SCAN 0.02,90.0 Degrees,Forward
Sequence 4-4 Non-Int in WFC3 transit ofh (3) (04)
112.00801 Secs X 13 (1456.104 Secs)
[==>(Copy 1)]
[==>(Copy 2)]
[==>(Copy 3)]
[==>(Copy 4)]
[==>(Copy 5)]
[==>(Copy 6)]
[==>(Copy 7)]
[==>(Copy 8)]
[==>(Copy 9)]
[==>(Copy 10)]
[==>(Copy 11)]
[==>(Copy 12)]
[==>(Copy 13)]
[3]
5 (1) 2MASS-J23062928-0502285
WFC3/IR, MULTIACCUM,GRISM256
G141 NSAMP=6;
SAMP-SEQ=SPARS25
SPATIAL SCAN 0.02,90.0 Degrees,Forward
Sequence 5-5 Non-Int in WFC3 transit ofh (3) (04)
112.00801 Secs X 13 (1456.104 Secs)
[==>(Copy 1)]
[==>(Copy 2)]
[==>(Copy 3)]
[==>(Copy 4)]
[==>(Copy 5)]
[==>(Copy 6)]
[==>(Copy 7)]
[==>(Copy 8)]
[==>(Copy 9)]
[==>(Copy 10)]
[==>(Copy 11)]
[==>(Copy 12)]
[==>(Copy 13)]
[4]
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Orb
it S
tru
ctu
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Vis
itProposal 15304, STIS Sep 03 (07), completed Tue Dec 08 14:02:14 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: BETWEEN 03-SEP-2017:17:00:00 AND 03-SEP-2017:19:15:00
Dia
gn
ost
ics (STIS Sep 03 (07)) Warning (Orbit Planner): LONG STIS MAMA SU LIKELY TO INTERSECT THE SAA
(STIS Sep 03 (07)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 03 (07)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 03 (07)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 03 (07)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 03 (07)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR Sequence 1-4 Non-Int in STIS Sep 03 (07)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK, 52X0.05 MIRROR Sequence 1-4 Non-Int in STIS Sep 03 (07)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS Sep 03 (07)
1700 Secs (1700 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS Sep 03 (07) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK, 52X0.05 MIRROR Sequence 5-7 Non-Int in STIS Sep 03 (07)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS Sep 03 (07)
2000 Secs (2000 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS Sep 03 (07) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK, 52X0.05 MIRROR Sequence 8-10 Non-Int in STIS Sep 03 (07)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS Sep 03 (07)
2000 Secs (2000 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS Sep 03 (07)
[==>][3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK, 52X0.05 MIRROR Sequence 11-13 Non-Int in STIS Sep 03 (07)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
Proposal 15304 - STIS Sep 03 (07) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS Sep 03 (07)
2000 Secs (2000 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS Sep 03 (07)
[==>][4]
14 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK, 52X0.05 MIRROR Sequence 14-16 Non-Int in STIS Sep 03 (07)
10 Secs (10 Secs)
[==>] [5]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
15 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 14-16 Non-Int in STIS Sep 03 (07)
2000 Secs (2000 Secs)
[==>] [5]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
16 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 14-16 Non-Int in STIS Sep 03 (07)
[==>][5]
17 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK, 52X0.05 MIRROR Sequence 17-19 Non-Int in STIS Sep 03 (07)
10 Secs (10 Secs)
[==>] [6]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
18 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 17-19 Non-Int in STIS Sep 03 (07)
2000 Secs (2000 Secs)
[==>] [6]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
19 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 17-19 Non-Int in STIS Sep 03 (07)
[==>][6]
Proposal 15304 - STIS Sep 03 (07) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
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Proposal 15304 - STIS Sep 03 (07) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
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Vis
itProposal 15304, STIS Sep 22 (31), failed Tue Dec 08 14:02:14 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: BETWEEN 22-SEP-2017:09:00:00 AND 22-SEP-2017:20:30:00
Dia
gn
ost
ics
(STIS Sep 22 (31)) Warning (Orbit Planner): LONG STIS MAMA SU LIKELY TO INTERSECT THE SAA
(STIS Sep 22 (31)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 22 (31)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 22 (31)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 22 (31)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 22 (31)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 22 (31)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
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arg
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# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
Proposal 15304 - STIS Sep 22 (31) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR Sequence 1-4 Non-Int in STIS Sep 22 (31)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS Sep 22 (31)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS Sep 22 (31)
1700 Secs (1700 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS Sep 22 (31) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS Sep 22 (31)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS Sep 22 (31)
2000 Secs (2000 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS Sep 22 (31) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS Sep 22 (31)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS Sep 22 (31)
2000 Secs (2000 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS Sep 22 (31)
[==>][3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS Sep 22 (31)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
Proposal 15304 - STIS Sep 22 (31) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS Sep 22 (31)
2000 Secs (2000 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS Sep 22 (31)
[==>][4]
14 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 14-16 Non-Int in STIS Sep 22 (31)
10 Secs (10 Secs)
[==>] [5]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
15 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 14-16 Non-Int in STIS Sep 22 (31)
2000 Secs (2000 Secs)
[==>] [5]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
16 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 14-16 Non-Int in STIS Sep 22 (31)
[==>][5]
17 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 17-19 Non-Int in STIS Sep 22 (31)
10 Secs (10 Secs)
[==>] [6]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
18 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 17-19 Non-Int in STIS Sep 22 (31)
2000 Secs (2000 Secs)
[==>] [6]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
19 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 17-19 Non-Int in STIS Sep 22 (31)
[==>][6]
20 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 20-22 Non-Int in STIS Sep 22 (31)
10 Secs (10 Secs)
[==>] [7]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
21 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 20-22 Non-Int in STIS Sep 22 (31)
2000 Secs (2000 Secs)
[==>] [7]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
22 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 20-22 Non-Int in STIS Sep 22 (31)
[==>][7]
Proposal 15304 - STIS Sep 22 (31) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
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Orb
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Proposal 15304 - STIS Sep 22 (31) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
44
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Proposal 15304 - STIS Sep 22 (31) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
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Vis
itProposal 15304, STIS Sep 28 (32), completed Tue Dec 08 14:02:14 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: BETWEEN 28-SEP-2017:06:30:00 AND 28-SEP-2017:18:30:00
Dia
gn
ost
ics
(STIS Sep 28 (32)) Warning (Orbit Planner): LONG STIS MAMA SU LIKELY TO INTERSECT THE SAA
(STIS Sep 28 (32)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 28 (32)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 28 (32)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 28 (32)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 28 (32)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 28 (32)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 28 (32)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
Proposal 15304 - STIS Sep 28 (32) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
47
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR Sequence 1-4 Non-Int in STIS Sep 28 (32)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS Sep 28 (32)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS Sep 28 (32)
1900 Secs (1900 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS Sep 28 (32) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS Sep 28 (32)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS Sep 28 (32)
2200 Secs (2200 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS Sep 28 (32) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS Sep 28 (32)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS Sep 28 (32)
2200 Secs (2200 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS Sep 28 (32)
[==>][3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS Sep 28 (32)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
Proposal 15304 - STIS Sep 28 (32) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS Sep 28 (32)
2200 Secs (2200 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS Sep 28 (32)
[==>][4]
14 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 14-16 Non-Int in STIS Sep 28 (32)
10 Secs (10 Secs)
[==>] [5]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
15 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 14-16 Non-Int in STIS Sep 28 (32)
2200 Secs (2200 Secs)
[==>] [5]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
16 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 14-16 Non-Int in STIS Sep 28 (32)
[==>][5]
17 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 17-19 Non-Int in STIS Sep 28 (32)
10 Secs (10 Secs)
[==>] [6]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
18 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 17-19 Non-Int in STIS Sep 28 (32)
2200 Secs (2200 Secs)
[==>] [6]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
19 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 17-19 Non-Int in STIS Sep 28 (32)
[==>][6]
20 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 20-22 Non-Int in STIS Sep 28 (32)
10 Secs (10 Secs)
[==>] [7]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
21 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 20-22 Non-Int in STIS Sep 28 (32)
2200 Secs (2200 Secs)
[==>] [7]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
22 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 20-22 Non-Int in STIS Sep 28 (32)
[==>][7]
Proposal 15304 - STIS Sep 28 (32) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
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Orb
it S
tru
ctu
reProposal 15304 - STIS Sep 28 (32) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
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Proposal 15304 - STIS Sep 28 (32) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
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Proposal 15304 - STIS Sep 28 (32) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
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Vis
itProposal 15304, STIS Oct 13 (33), failed Tue Dec 08 14:02:14 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: BETWEEN 12-OCT-2017:23:20:00 AND 13-OCT-2017:00:30:00
Dia
gn
ost
ics (STIS Oct 13 (33)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Oct 13 (33)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Oct 13 (33)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Oct 13 (33)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Oct 13 (33)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
Proposal 15304 - STIS Oct 13 (33) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ahe...
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR Sequence 1-4 Non-Int in STIS Oct 13 (33)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS Oct 13 (33)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS Oct 13 (33)
1900 Secs (1900 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS Oct 13 (33) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS Oct 13 (33)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS Oct 13 (33)
2200 Secs (2200 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS Oct 13 (33) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS Oct 13 (33)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS Oct 13 (33)
2200 Secs (2200 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS Oct 13 (33)
[==>][3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS Oct 13 (33)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
Proposal 15304 - STIS Oct 13 (33) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ahe...
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS Oct 13 (33)
2200 Secs (2200 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS Oct 13 (33)
[==>][4]
14 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 14-16 Non-Int in STIS Oct 13 (33)
10 Secs (10 Secs)
[==>] [5]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
15 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 14-16 Non-Int in STIS Oct 13 (33)
2200 Secs (2200 Secs)
[==>] [5]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
16 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 14-16 Non-Int in STIS Oct 13 (33)
[==>][5]
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Vis
itProposal 15304, STIS Oct 17 (16), completed Tue Dec 08 14:02:14 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: BETWEEN 17-OCT-2017:23:00:00 AND 18-OCT-2017:05:00:00
Dia
gn
ost
ics (STIS Oct 17 (16)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Oct 17 (16)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Oct 17 (16)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Oct 17 (16)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR GS ACQ SCENARIO BASE1B3
Sequence 1-4 Non-Int in STIS Oct 17 (16)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS Oct 17 (16)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS Oct 17 (16)
1900 Secs (1900 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS Oct 17 (16) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS Oct 17 (16)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS Oct 17 (16)
2200 Secs (2200 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS Oct 17 (16) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS Oct 17 (16)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS Oct 17 (16)
2200 Secs (2200 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS Oct 17 (16)
[==>][3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS Oct 17 (16)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS Oct 17 (16)
2200 Secs (2200 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS Oct 17 (16)
[==>][4]
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Vis
itProposal 15304, STIS Sep 14 (29), completed Tue Dec 08 14:02:14 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: BETWEEN 14-SEP-2017:12:00:00 AND 14-SEP-2017:13:00:00
Dia
gn
ost
ics (STIS Sep 14 (29)) Warning (Orbit Planner): LONG STIS MAMA SU LIKELY TO INTERSECT THE SAA
(STIS Sep 14 (29)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 14 (29)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 14 (29)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 14 (29)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 14 (29)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR Sequence 1-4 Non-Int in STIS Sep 14 (29)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS Sep 14 (29)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS Sep 14 (29)
1700 Secs (1700 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS Sep 14 (29) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS Sep 14 (29)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS Sep 14 (29)
2000 Secs (2000 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS Sep 14 (29) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS Sep 14 (29)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS Sep 14 (29)
2000 Secs (2000 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS Sep 14 (29)
[==>][3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS Sep 14 (29)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS Sep 14 (29)
2000 Secs (2000 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS Sep 14 (29)
[==>][4]
14 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 14-16 Non-Int in STIS Sep 14 (29)
10 Secs (10 Secs)
[==>] [5]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
15 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 14-16 Non-Int in STIS Sep 14 (29)
2000 Secs (2000 Secs)
[==>] [5]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
16 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 14-16 Non-Int in STIS Sep 14 (29)
[==>][5]
17 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 17-19 Non-Int in STIS Sep 14 (29)
10 Secs (10 Secs)
[==>] [6]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
18 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 17-19 Non-Int in STIS Sep 14 (29)
2000 Secs (2000 Secs)
[==>] [6]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
19 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 17-19 Non-Int in STIS Sep 14 (29)
[==>][6]
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Vis
itProposal 15304, STIS Sep 17 (30), completed Tue Dec 08 14:02:15 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: BETWEEN 17-SEP-2017:11:30:00 AND 17-SEP-2017:12:30:00
Dia
gn
ost
ics (STIS Sep 17 (30)) Warning (Orbit Planner): LONG STIS MAMA SU LIKELY TO INTERSECT THE SAA
(STIS Sep 17 (30)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 17 (30)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 17 (30)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 17 (30)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Sep 17 (30)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR Sequence 1-4 Non-Int in STIS Sep 17 (30)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS Sep 17 (30)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS Sep 17 (30)
1700 Secs (1700 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS Sep 17 (30) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS Sep 17 (30)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS Sep 17 (30)
2000 Secs (2000 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS Sep 17 (30) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS Sep 17 (30)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS Sep 17 (30)
2000 Secs (2000 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS Sep 17 (30)
[==>][3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS Sep 17 (30)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS Sep 17 (30)
2000 Secs (2000 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS Sep 17 (30)
[==>][4]
14 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 14-16 Non-Int in STIS Sep 17 (30)
10 Secs (10 Secs)
[==>] [5]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
15 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 14-16 Non-Int in STIS Sep 17 (30)
2000 Secs (2000 Secs)
[==>] [5]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
16 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 14-16 Non-Int in STIS Sep 17 (30)
[==>][5]
17 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 17-19 Non-Int in STIS Sep 17 (30)
10 Secs (10 Secs)
[==>] [6]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
18 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 17-19 Non-Int in STIS Sep 17 (30)
2000 Secs (2000 Secs)
[==>] [6]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
19 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 17-19 Non-Int in STIS Sep 17 (30)
[==>][6]
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Vis
itProposal 15304, STIS Nov 09 (05), completed Tue Dec 08 14:02:15 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: BETWEEN 09-NOV-2017:09:50:00 AND 09-NOV-2017:16:00:00
Dia
gn
ost
ics (STIS Nov 09 (05)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Nov 09 (05)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Nov 09 (05)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR Sequence 1-4 Non-Int in STIS Nov 09 (05)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS Nov 09 (05)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS Nov 09 (05)
1800 Secs (1800 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS Nov 09 (05)
[==>][1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS Nov 09 (05)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS Nov 09 (05)
2100 Secs (2100 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS Nov 09 (05)
[==>][2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS Nov 09 (05)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS Nov 09 (05)
2100 Secs (2100 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS Nov 09 (05)
[==>][3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS Nov 09 (05)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
Proposal 15304 - STIS Nov 09 (05) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS Nov 09 (05)
2100 Secs (2100 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS Nov 09 (05)
[==>][4]
Proposal 15304 - STIS Nov 09 (05) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
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Proposal 15304 - STIS Nov 09 (05) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
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Vis
itProposal 15304, STIS Nov 13 (08), completed Tue Dec 08 14:02:15 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: BETWEEN 13-NOV-2017:10:30:00 AND 13-NOV-2017:17:00:00
Dia
gn
ost
ics (STIS Nov 13 (08)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Nov 13 (08)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS Nov 13 (08)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR Sequence 1-4 Non-Int in STIS Nov 13 (08)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS Nov 13 (08)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS Nov 13 (08)
1700 Secs (1700 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS Nov 13 (08)
[==>][1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS Nov 13 (08)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS Nov 13 (08)
2000 Secs (2000 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS Nov 13 (08)
[==>][2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS Nov 13 (08)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS Nov 13 (08)
2000 Secs (2000 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS Nov 13 (08)
[==>][3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS Nov 13 (08)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS Nov 13 (08)
2000 Secs (2000 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS Nov 13 (08)
[==>][4]
Proposal 15304 - STIS Nov 13 (08) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ah...
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Vis
itProposal 15304, STIS b1 (B1), completed Tue Dec 08 14:02:15 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: Period 1.510887062 D AND ZERO-PHASE HJD2457322.410224490
Dia
gn
ost
ics (STIS b1 (B1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS b1 (B1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS b1 (B1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
Proposal 15304 - STIS b1 (B1) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ahead ...
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR PHASE 0 TO 0.013 Sequence 1-4 Non-Int in STIS b1 (B1)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS b1 (B1)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS b1 (B1)
1800 Secs (1800 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS b1 (B1) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS b1 (B1)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS b1 (B1)
2100 Secs (2100 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS b1 (B1) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS b1 (B1)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS b1 (B1)
2100 Secs (2100 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS b1 (B1) [==>] [3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS b1 (B1)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS b1 (B1)
2100 Secs (2100 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS b1 (B1) [==>] [4]
Proposal 15304 - STIS b1 (B1) - Collecting the Puzzle Pieces: Completing HST's UV+NIR Survey of the TRAPPIST-1 System ahead ...
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Vis
itProposal 15304, STIS b2 (B2), completed Tue Dec 08 14:02:15 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: Period 1.510887062 D AND ZERO-PHASE HJD2457322.410224490
Dia
gn
ost
ics (STIS b2 (B2)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS b2 (B2)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS b2 (B2)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR PHASE 0 TO 0.013 Sequence 1-4 Non-Int in STIS b2 (B2)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS b2 (B2)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS b2 (B2)
1800 Secs (1800 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS b2 (B2) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS b2 (B2)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS b2 (B2)
2100 Secs (2100 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS b2 (B2) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS b2 (B2)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS b2 (B2)
2100 Secs (2100 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS b2 (B2) [==>] [3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS b2 (B2)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS b2 (B2)
2100 Secs (2100 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS b2 (B2) [==>] [4]
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Vis
itProposal 15304, STIS c1 (C1), completed Tue Dec 08 14:02:15 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: BETWEEN 2018.253:22:00:00 AND 2018.253:23:00:00
Dia
gn
ost
ics (STIS c1 (C1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS c1 (C1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS c1 (C1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR Sequence 1-4 Non-Int in STIS c1 (C1)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS c1 (C1)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS c1 (C1)
1800 Secs (1800 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS c1 (C1) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS c1 (C1)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS c1 (C1)
2100 Secs (2100 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS c1 (C1) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS c1 (C1)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS c1 (C1)
2100 Secs (2100 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS c1 (C1) [==>] [3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS c1 (C1)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS c1 (C1)
2100 Secs (2100 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS c1 (C1) [==>] [4]
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Vis
itProposal 15304, STIS c2 (C2), completed Tue Dec 08 14:02:15 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: Period 2.421787216 D AND ZERO-PHASE HJD2457282.706940840
Dia
gn
ost
ics (STIS c2 (C2)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS c2 (C2)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS c2 (C2)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR PHASE 0 TO 0.009 Sequence 1-4 Non-Int in STIS c2 (C2)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS c2 (C2)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS c2 (C2)
1800 Secs (1800 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS c2 (C2) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS c2 (C2)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS c2 (C2)
2100 Secs (2100 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS c2 (C2) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS c2 (C2)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS c2 (C2)
2100 Secs (2100 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS c2 (C2) [==>] [3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS c2 (C2)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS c2 (C2)
2100 Secs (2100 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS c2 (C2) [==>] [4]
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Vis
itProposal 15304, STIS c3 (C3), completed Tue Dec 08 14:02:15 GMT 2020
Diagnostic Status: No Diagnostics
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: SCHED 100%; Period 2.421787216 D AND ZERO-PHASE HJD2457282.706940840
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR PHASE 0 TO 0.009 Sequence 1-4 Non-Int in STIS c3 (C3)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS c3 (C3)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS c3 (C3)
1800 Secs (1594 Secs)
[==>1594.0 Secs ] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS c3 (C3) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS c3 (C3)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS c3 (C3)
2080 Secs (1773 Secs)
[==>1773.0 Secs ] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS c3 (C3) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS c3 (C3)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS c3 (C3)
2080 Secs (1773 Secs)
[==>1773.0 Secs ] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS c3 (C3) [==>] [3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS c3 (C3)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS c3 (C3)
2080 Secs (1773 Secs)
[==>1773.0 Secs ] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS c3 (C3) [==>] [4]
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Vis
itProposal 15304, STIS d1 (D1), completed Tue Dec 08 14:02:15 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: Period 4.049643595 D AND ZERO-PHASE HJD2457670.055702060; VISIBILITY INTERVAL 52.8 M
Dia
gn
ost
ics (STIS d1 (D1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS d1 (D1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS d1 (D1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR PHASE 0 TO 0.005 Sequence 1-4 Non-Int in STIS d1 (D1)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS d1 (D1)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS d1 (D1)
1800 Secs (1800 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS d1 (D1) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS d1 (D1)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS d1 (D1)
2100 Secs (2100 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS d1 (D1) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS d1 (D1)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS d1 (D1)
2100 Secs (2100 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS d1 (D1) [==>] [3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS d1 (D1)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS d1 (D1)
2100 Secs (2100 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS d1 (D1) [==>] [4]
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Vis
itProposal 15304, STIS e1 (E1), completed Tue Dec 08 14:02:15 GMT 2020
Diagnostic Status: No Diagnostics
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: SCHED 30%; Period 6.099483074 D AND ZERO-PHASE HJD2457660.265088220
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR PHASE 0 TO 0.0035 Sequence 1-4 Non-Int in STIS e1 (E1)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS e1 (E1)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS e1 (E1)
1800 Secs (1817 Secs)
[==>1817.0 Secs ] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS e1 (E1) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS e1 (E1)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS e1 (E1)
2100 Secs (1996 Secs)
[==>1996.0 Secs ] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS e1 (E1) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS e1 (E1)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS e1 (E1)
2100 Secs (1996 Secs)
[==>1996.0 Secs ] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS e1 (E1) [==>] [3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS e1 (E1)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS e1 (E1)
2100 Secs (1996 Secs)
[==>1996.0 Secs ] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS e1 (E1) [==>] [4]
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Vis
itProposal 15304, STIS e2 (E2), implementation Tue Dec 08 14:02:15 GMT 2020
Diagnostic Status: No Diagnostics
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: SCHED 100%; Period 6.099483074 D AND ZERO-PHASE HJD2457660.265088220
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR PHASE 0 TO 0.0035 Sequence 1-4 Non-Int in STIS e2 (E2)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS e2 (E2)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS e2 (E2)
1594 Secs (1594 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS e2 (E2) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS e2 (E2)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS e2 (E2)
1773 Secs (1773 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS e2 (E2) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS e2 (E2)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS e2 (E2)
1773 Secs (1773 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS e2 (E2) [==>] [3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS e2 (E2)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS e2 (E2)
1773 Secs (1773 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS e2 (E2) [==>] [4]
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Vis
itProposal 15304, STIS f1 (F1), completed Tue Dec 08 14:02:16 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: Period 9.206318826 D AND ZERO-PHASE HJD2457671.276243970
Dia
gn
ost
ics (STIS f1 (F1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS f1 (F1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS f1 (F1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR PHASE 0 TO 0.0022 Sequence 1-4 Non-Int in STIS f1 (F1)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS f1 (F1)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS f1 (F1)
1800 Secs (1800 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS f1 (F1) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS f1 (F1)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS f1 (F1)
2100 Secs (2100 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS f1 (F1) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS f1 (F1)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS f1 (F1)
2100 Secs (2100 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS f1 (F1) [==>] [3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS f1 (F1)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS f1 (F1)
2100 Secs (2100 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS f1 (F1) [==>] [4]
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Vis
itProposal 15304, STIS f2 (F2), completed Tue Dec 08 14:02:16 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: Period 9.206318826 D AND ZERO-PHASE HJD2457671.276243970
Dia
gn
ost
ics (STIS f2 (F2)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS f2 (F2)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS f2 (F2)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR PHASE 0 TO 0.0022 Sequence 1-4 Non-Int in STIS f2 (F2)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS f2 (F2)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS f2 (F2)
1800 Secs (1800 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS f2 (F2) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS f2 (F2)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS f2 (F2)
2100 Secs (2100 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS f2 (F2) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS f2 (F2)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS f2 (F2)
2100 Secs (2100 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS f2 (F2) [==>] [3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS f2 (F2)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS f2 (F2)
2100 Secs (2100 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS f2 (F2) [==>] [4]
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Vis
itProposal 15304, STIS f3 (F3), implementation Tue Dec 08 14:02:16 GMT 2020
Diagnostic Status: No Diagnostics
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: SCHED 100%; Period 9.206318826 D AND ZERO-PHASE HJD2457671.276243970
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR PHASE 0 TO 0.0022 Sequence 1-4 Non-Int in STIS f3 (F3)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS f3 (F3)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS f3 (F3)
1594 Secs (1594 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS f3 (F3) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS f3 (F3)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS f3 (F3)
1773 Secs (1773 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS f3 (F3) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS f3 (F3)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS f3 (F3)
1773 Secs (1773 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS f3 (F3) [==>] [3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS f3 (F3)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS f3 (F3)
1773 Secs (1773 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS f3 (F3) [==>] [4]
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Vis
itProposal 15304, STIS g1 (G1), completed Tue Dec 08 14:02:16 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: Period 12.35351378 D AND ZERO-PHASE HJD2457665.257828620
Dia
gn
ost
ics (STIS g1 (G1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS g1 (G1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS g1 (G1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR PHASE 0 TO 0.0016 Sequence 1-4 Non-Int in STIS g1 (G1)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS g1 (G1)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS g1 (G1)
1800 Secs (1800 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS g1 (G1) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS g1 (G1)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS g1 (G1)
2100 Secs (2100 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS g1 (G1) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS g1 (G1)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS g1 (G1)
2100 Secs (2100 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS g1 (G1) [==>] [3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS g1 (G1)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS g1 (G1)
2100 Secs (2100 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS g1 (G1) [==>] [4]
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Vis
itProposal 15304, STIS g2 (G2), completed Tue Dec 08 14:02:16 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: Period 12.35351378 D AND ZERO-PHASE HJD2457665.257828620
Dia
gn
ost
ics (STIS g2 (G2)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS g2 (G2)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS g2 (G2)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR PHASE 0 TO 0.0016 Sequence 1-4 Non-Int in STIS g2 (G2)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS g2 (G2)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS g2 (G2)
1800 Secs (1800 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS g2 (G2) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS g2 (G2)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS g2 (G2)
2100 Secs (2100 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS g2 (G2) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS g2 (G2)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS g2 (G2)
2100 Secs (2100 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS g2 (G2) [==>] [3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS g2 (G2)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS g2 (G2)
2100 Secs (2100 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS g2 (G2) [==>] [4]
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Vis
itProposal 15304, STIS h1 (H1), completed Tue Dec 08 14:02:16 GMT 2020
Diagnostic Status: Warning
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: Period 18.76745243 D AND ZERO-PHASE HJD2457662.459224910
Dia
gn
ost
ics (STIS h1 (H1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS h1 (H1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
(STIS h1 (H1)) Warning (Orbit Planner): ORBITAL VISIBILITY OVERRUN
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR PHASE 0 TO 0.0011 Sequence 1-4 Non-Int in STIS h1 (H1)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS h1 (H1)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS h1 (H1)
1800 Secs (1800 Secs)
[==>] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS h1 (H1) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS h1 (H1)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS h1 (H1)
2100 Secs (2100 Secs)
[==>] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS h1 (H1) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS h1 (H1)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS h1 (H1)
2100 Secs (2100 Secs)
[==>] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS h1 (H1) [==>] [3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS h1 (H1)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS h1 (H1)
2100 Secs (2100 Secs)
[==>] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS h1 (H1) [==>] [4]
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Vis
itProposal 15304, STIS h2 (H2), implementation Tue Dec 08 14:02:16 GMT 2020
Diagnostic Status: No Diagnostics
Scientific Instruments: STIS/CCD, STIS/FUV-MAMA
Special Requirements: SCHED 100%; Period 18.76745243 D AND ZERO-PHASE HJD2457662.459224910
Fix
ed T
arg
ets
# Name Target Coordinates Targ. Coord. Corrections Fluxes Miscellaneous
(1) 2MASS-J23062928-0502285
Alt Name1: TRAPPIST-1
RA: 23 06 30.3400 (346.6264167d)
Dec: -05 02 36.44 (-5.04346d)
Equinox: J2000
Proper Motion RA: 922.1 mas/yr
Proper Motion Dec: -471.9 mas/yr
Parallax: 0.08258"
Epoch of Position: 2015.86
Radial Velocity: -51.688 km/sec
V=18.798+/-0.082
V=18.80+-0.08,
R=16.47+-0.07,
I=14.0+-0.1,
J=11.35+-0.02,
K=10.30+-0.02
Reference Frame: ICRS
Comments: We measured the J2000 equatorial coordinates of TRAPPIST-1 in the 2015 TRAPPIST images, using 29 stars from the UCAC2 catalog and the Pulkovo Observatory Izmccd astrometric software (we usethe mean epoch of these observations secured between September and December 2015). We adopt uncertainties on RA and Dec as those for 2MASS for this object.We checked that the input coordinates and those given in SIMBAD at Epoch 2000 yield the same position in the APT target confirmation chart at Epoch 1991.68. We also checked independently that these coordinatesand proper motion match with the position of the star in POSS image (1953) and 2MASS image (1998).Radial velocity comes from Barnes et al. 2014Category=STARDescription=[EXTRA-SOLAR PLANETARY SYSTEM]
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Exp
osu
res
# Label(ETC Run)
Target Config,Mode,Aperture Spectral Els. Opt. Params. Special Reqs. Groups Exp. Time (Total)/[Actual Dur.] Orbit
1 ACQ(STIS.ta.781643)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ, F28X50LP MIRROR PHASE 0 TO 0.0011 Sequence 1-4 Non-Int in STIS h2 (H2)
5 Secs (5 Secs)
[==>] [1]
Comments: We use the F28X50LP filter for this ACQ image, as recommended for this star with V magnitude of 18.8. It also ensures the brightness is weighted most strongly toward red wavelengths, where the target star is brightest. We estimated the exposure time for several stellar models close to the target star (STIS.ta.781640, STIS.ta.781641, STIS.ta.781643). Exposure times to reach a SNR of 40 range from 1.5 to 3.6s, and minimum saturation time is 290s. We thus choose an exposure time of 5s.We used Aladin to check that the closest star is at a distance of more than 220 arcsec. There is thus no chance that STIS acquires another object in the 5x5 arcsec search area.
2 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 1-4 Non-Int in STIS h2 (H2)
10 Secs (10 Secs)
[==>] [1]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
3 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 1-4 Non-Int in STIS h2 (H2)
1800 Secs (1594 Secs)
[==>1594.0 Secs ] [1]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
4 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 1-4 Non-Int in STIS h2 (H2) [==>] [1]
5 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 5-7 Non-Int in STIS h2 (H2)
10 Secs (10 Secs)
[==>] [2]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
6 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 5-7 Non-Int in STIS h2 (H2)
2100 Secs (1773 Secs)
[==>1773.0 Secs ] [2]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
7 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 5-7 Non-Int in STIS h2 (H2) [==>] [2]
8 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 8-10 Non-Int in STIS h2 (H2)
10 Secs (10 Secs)
[==>] [3]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
9 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 8-10 Non-Int in STIS h2 (H2)
2100 Secs (1773 Secs)
[==>1773.0 Secs ] [3]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
10 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 8-10 Non-Int in STIS h2 (H2) [==>] [3]
11 ACQ/PEAK(STIS.ta.783365)
(1) 2MASS-J23062928-0502285
STIS/CCD, ACQ/PEAK,52X0.05D1
MIRROR Sequence 11-13 Non-Int in STIS h2 (H2)
10 Secs (10 Secs)
[==>] [4]
Comments: The ETC lists a time to saturation through the 52X0.05 slit of 1086s (for a black body model with the same temperature as the star). With our 10s exposure, we should reach 5600 source electrons, above the 5000 required for peak-up with the mirror element.
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12 SCIENCE(STIS.sp.415432)
(1) 2MASS-J23062928-0502285
STIS/FUV-MAMA, TIME-TAG,52X0.05D1
G140M
1222 A
BUFFER-TIME=900;
WAVECAL=NO
Sequence 11-13 Non-Int in STIS h2 (H2)
2100 Secs (1773 Secs)
[==>1773.0 Secs ] [4]
Comments: The target star is a M8 ultracool dwarf from which we expect a much lower emission at Lyman-alpha than from GJ436 targeted in program GO#12965 (in the GJ140M spectral range, the stellar emission from these stars will arise from the Lyman-alpha line alone). We can thus use safely the same settings as program GO#12965.
13 GO-WAVECAL
WAVE STIS/FUV-MAMA, ACCUM,52X0.05
G140M
1222 A
Sequence 11-13 Non-Int in STIS h2 (H2) [==>] [4]
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161