JWST NIRSpec observations of LTT 1445 A b yield a featureless 3-5μm transmission spectrum, limiting atmospheric metallicity to ≳350× solar under grey-cloud models.
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GJ 3929 b's full four-eclipse JWST/MIRI data set yields an eclipse depth of 118±22 ppm, consistent with a bare rocky surface and ruling out thick CO2 atmospheres at >3σ.
TRAPPIST-1 flares follow a single power law N(≥E_TESS) ∝ E_TESS^{-0.753} from 10^{29} to 10^{33} erg after sensitivity corrections and bandpass conversion.
Accounting for stellar and orbital uncertainties shows that predicted eclipse depths for bare-rock models of rocky exoplanets carry substantial uncertainty comparable to measurements, establishing a fundamental precision limit for atmospheric and compositional inferences.
Reference differential imaging of archival MIRI F1500W TSO data reaches 5σ contrasts of ~10^{-3} at 1" and ~2×10^{-4} beyond 3", enabling sensitivity to ~4–10 MJup planets at tens of AU around old M-dwarfs.
citing papers explorer
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JWST COMPASS Program: The 3--5$\mu$m transmission spectrum of LTT 1445 A b
JWST NIRSpec observations of LTT 1445 A b yield a featureless 3-5μm transmission spectrum, limiting atmospheric metallicity to ≳350× solar under grey-cloud models.
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GJ 3929 b as the First Complete Rocky Worlds DDT Data Set
GJ 3929 b's full four-eclipse JWST/MIRI data set yields an eclipse depth of 118±22 ppm, consistent with a bare rocky surface and ruling out thick CO2 atmospheres at >3σ.
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A single power law for the TRAPPIST-1 flare distribution across four orders of magnitude in energy
TRAPPIST-1 flares follow a single power law N(≥E_TESS) ∝ E_TESS^{-0.753} from 10^{29} to 10^{33} erg after sensitivity corrections and bandpass conversion.
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Uniform Reinterpretation of Rocky Exoplanet Secondary Eclipse Observations and the Impact of Stellar and Orbital Uncertainties
Accounting for stellar and orbital uncertainties shows that predicted eclipse depths for bare-rock models of rocky exoplanets carry substantial uncertainty comparable to measurements, establishing a fundamental precision limit for atmospheric and compositional inferences.
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A Search for Wide-orbit Planets Around M-dwarfs using Deep MIRI 15-micron Images
Reference differential imaging of archival MIRI F1500W TSO data reaches 5σ contrasts of ~10^{-3} at 1" and ~2×10^{-4} beyond 3", enabling sensitivity to ~4–10 MJup planets at tens of AU around old M-dwarfs.