Transiting Exoplanet Observations of GJ 1132b & LHS 1140b with JWST Hannah Diamond-Lowe Harvard-Smithsonian Center for Astrophysics Enabling Transiting Exoplanet Observations with JWST Space Telescope Science Institute 10-12 July 2017 Baltimore, MD
The Stars
The Stars
The Stars GJ 1132 Mass: 0.181 M Radius: 0.211 R Rotation Period: 125 days Type: M4.5V LHS 1140 Mass: 0.146 M Radius: 0.186 R Rotation Period: 131 days Type: M4.5V
The Planets
The Planets
The Planets GJ 1132b
The Planets GJ 1132b LHS 1140b
The Planets GJ 1132b Mass: 1.62 M x4 LHS 1140b Mass: 6.65 M
The Planets GJ 1132b Mass: 1.62 M Radius: 1.13 R x 1.3 LHS 1140b Mass: 6.65 M Radius: 1.43 R
The Planets GJ 1132b Mass: 1.62 M Radius: 1.13 R Period: 1.63 days x 15 LHS 1140b Mass: 6.65 M Radius: 1.43 R Period: 24.7 days
The Planets GJ 1132b Mass: 1.62 M Radius: 1.13 R Period: 1.63 days Scaled distance: 16.54 x6 LHS 1140b Mass: 6.65 M Radius: 1.43 R Period: 24.7 days Scaled distance: 101.0
The Planets GJ 1132b Mass: 1.62 M Radius: 1.13 R Period: 1.63 days Scaled distance: 16.54 Insolation: 19x Earth's LHS 1140b Mass: 6.65 M x.025 Radius: 1.43 R Period: 24.7 days Scaled distance: 101.0 Insolation: 0.46x Earth's
The Planets GJ 1132b Mass: 1.62 M Radius: 1.13 R Period: 1.63 days Scaled distance: 16.54 Insolation: 19x Earth's LHS 1140b Mass: 6.65 M Radius: 1.43 R Period: 24.7 days Scaled distance: 101.0 Insolation: 0.46x Earth's
How do the orbital properties of these planets affect their atmospheres?
To do list (before JWST Launch)
To do list (before JWST Launch) 1) Characterize the UV flux from the host stars 2) Better constrain the mass of LHS 1140b 3) Use current facilities (ground-based, HST, Spitzer) to rule out light atmospheres
UV characterization of GJ 1132 & LHS 1140 Fraction of bolometric luminosity UV line strengths of low-mass M dwarfs are not well-constrained by current MUSCLES stars 0.50 0.45 0.40 0.35 0.30 0.25 Stellar Mass (M ) 0.20 0.15 0.10 0.05 Figure by Zach Berta-Thompson
To do list (before JWST Launch) 1) Characterize the UV flux from the host stars 2) Better constrain the mass of LHS 1140b 3) Use current facilities (ground-based, HST, Spitzer) to rule out light atmospheres
More RV measurements of LHS 1140b LHS 1140b mass: 6.65 M ± 1.82 M Dittmann + (2017)
To do list (before JWST Launch) 1) Characterize the UV flux from the host stars 2) Better constrain the mass of LHS 1140b 3) Use current facilities (ground-based, HST, Spitzer) to rule out light atmospheres
Observations in the works GJ 1132b with Magellan Diamond-Lowe+ (in prep)
Observations in the works GJ 1132b with Magellan Diamond-Lowe+ (in prep)
Observations in the works GJ 1132b with Magellan Diamond-Lowe+ (in prep)
Observations in the works GJ 1132b with Magellan Diamond-Lowe+ (in prep)
Observations in the works GJ 1132b with Magellan Diamond-Lowe+ (in prep)
Observations in the works GJ 1132b with Magellan Diamond-Lowe+ (in prep)
Observations in the works LHS 1140b with Magellan & VLT Four large telescopes will look at LHS 1140b transit on October 26-27, 2017
Observations in the works Scheduled HST/WFC3 programs GJ 1132b: PI Berta-Thompson GJ 1132b: 5 transits H2, μ = 2 LHS 1140b: 2 transits H2, μ = 2 LHS 1140b: PI Dittmann
Observations in the works Scheduled HST/WFC3 programs GJ 1132b: 5 transits H2, μ = 2 All models made using Exo_Transmit (Kempton+ 2016) LHS 1140b: 2 transits GJ 1132b: PI Berta-Thompson H2, μ = 2 LHS 1140b: PI Dittmann
Observations in the works Scheduled HST/WFC3 programs GJ 1132b: 5 transits H2, μ = 2 All models made using Exo_Transmit (Kempton+ 2016) LHS 1140b: 2 transits H2, μ = 2 All data points estimated with PandExo (Batalha+ 2017) GJ 1132b: PI Berta-Thompson LHS 1140b: PI Dittmann
Observations in the works Scheduled HST/WFC3 programs GJ 1132b: PI Berta-Thompson GJ 1132b: 5 transits H2, μ = 2 LHS 1140b: 2 transits H2, μ = 2 LHS 1140b: PI Dittmann
Observations in the works Scheduled HST/WFC3 programs GJ 1132b: 5 transits LHS 1140b: 2 transits GJ 1132b: PI Berta-Thompson H2, μ = 2 H2, μ = 2 H2, μ = 2, massive LHS 1140b: PI Dittmann
Observations in the works Scheduled HST/WFC3 programs GJ 1132b: PI Berta-Thompson GJ 1132b: 5 transits H2, μ = 2 LHS 1140b: 2 transits H2, μ = 2 LHS 1140b: PI Dittmann
Observations in the works Scheduled HST/WFC3 programs GJ 1132b: 5 transits LHS 1140b: 2 transits GJ 1132b: PI Berta-Thompson H2, μ = 2 H2O, μ = 18 H2, μ = 2 H2O, μ = 18 LHS 1140b: PI Dittmann
What will JWST do? GTO programs GJ 1132b NIRISS SOSS: 4 transits Wavelengths: 0.83-2.81μm Disperser: GR700 R: ~700 at 1.25μm (1st order) and 0.63μm (2nd order) Total time: 17.2 hours LHS 1140b NIRISS SOSS: 2 transits Wavelengths: 0.83-2.81μm Disperser: GR700 R: ~700 at 1.25μm (1st order) and 0.63μm (2nd order) Total time: 13.7 hours NIRSpec Fixed Slit: 1 transit Wavelengths: 2.87-5.18μm Grating/Filter: G396H/F290LP R: ~2700 at 3.95μm Total time: 4.45 hours NIRISS: PI Doyon NIRSpec: PI Ferruit
JWST on GJ 1132b Image credit: ESO/L. Calçada
JWST on GJ 1132b HST/WFC3: 5 transits H2O, μ = 18
JWST on GJ 1132b HST/WFC3: 5 transits, JWST/NIRISS: 4 transits H2O, μ = 18
JWST on GJ 1132b NIRISS: 4 transits, NIRSpec: 4 transits, MIRI: 4 transits H2O, μ = 18
JWST on GJ 1132b NIRISS: 10 transits, NIRSpec: 10 transits, MIRI: 10 transits CO2, μ = 44
JWST on GJ 1132b NIRISS: 10 transits, NIRSpec: 10 transits, MIRI: 10 transits 29% H2O, 70% O2, 1% O3, μ 28
JWST on GJ 1132b NIRISS: 10 transits, NIRSpec: 10 transits, MIRI: 10 transits 29% H2O, 70% O2, 1% O3, μ 28 100% H2O, μ = 18
JWST on GJ 1132b NIRISS: 10 transits, NIRSpec: 10 transits, MIRI: 10 transits 29% H2O, 70% O2, 1% O3, μ 28 100% H2O, μ = 18 The most common outcome for GJ 1132b from our simulations is a tenuous atmosphere dominated by O2 Schaefer+ (2016)
JWST on GJ 1132b NIRISS: 10 transits, NIRSpec: 10 transits, MIRI: 10 transits 29% H2O, 70% O2, 1% O3, μ 28 100% H2O, μ = 18
JWST on GJ 1132b NIRISS: 15 transits, NIRSpec: 15 transits, MIRI: 15 transits 30% H2O, 70% O2, 0% O3, μ 28
JWST on GJ 1132b NIRISS: 15 transits, NIRSpec: 15 transits, MIRI: 15 transits 30% H2O, 70% O2, 0% O3, μ 28 100% H2O, μ = 18
JWST on GJ 1132b NIRISS: 500 transits, NIRSpec: 500 transits, MIRI: 500 transits O2, μ = 32
JWST on GJ 1132b NIRISS: 500 transits O2, μ = 32
JWST on LHS 1140b Image credit: CfA/M. Weiss
JWST on LHS 1140b HST/WFC3: 2 transits H2O, μ = 18
JWST on LHS 1140b HST/WFC3: 2 transits, JWST/NIRISS: 2 transits, JWST/NIRSpec: 1 transit H2O, μ = 18
JWST on LHS 1140b NIRISS: 3 transits, NIRSpec: 3 transits, MIRI: 3 transits H2O, μ = 18
JWST on LHS 1140b NIRISS: 11 transits, NIRSpec: 11 transits, MIRI: 11 transits CO2, μ = 44
JWST on LHS 1140b NIRISS: 11 transits, NIRSpec: 11 transits, MIRI: 11 transits 29% H2O, 70% O2, 1% O3, μ 28
JWST on LHS 1140b NIRISS: 11 transits, NIRSpec: 11 transits, MIRI: 11 transits 29% H2O, 70% O2, 1% O3, μ 28 100% H2O, μ = 18
JWST on LHS 1140b NIRISS: 25 transits, NIRSpec: 25 transits, MIRI: 25 transits 30% H2O, 70% O2, 0% O3, μ 28
JWST on LHS 1140b NIRISS: 25 transits, NIRSpec: 25 transits, MIRI: 25 transits 30% H2O, 70% O2, 0% O3, μ 28 100% H2O, μ = 18
JWST on LHS 1140b NIRISS: 900 transits, NIRSpec: 900 transits, MIRI: 900 transits O2, μ = 32
JWST on LHS 1140b NIRISS: 900 transits O2, μ = 32
Conclusions Pre-JWST to-do list: understand UV emission from host stars constrain the mass of LHS 1140b complete analysis of ground-based, HST, and Spitzer data Post-JWST: JWST data will work with optical data from the GMT & ELTs if we find more terrestrial targets, this will be a pathway for atmospheric characterization
Number of JWST transits needed for atmospheres on GJ 1132b & LHS 1140b Atmosphere Composition GJ 1132b LHS 1140b 100% H2 1 1 100% H2O 4 3 100% CO2 10 11 29%H2O, 70%O2, 1%O3 10 11 30%H2O, 70%O2, 0%O3 15 25 100% O2 500 (too many) 900 (too many)