Tentative evidence for a super-Jupiter at 15-100 AU or brown dwarf at 20-170 AU in 51 Pegasi from RV curvature, but the signal is likely driven by Lick/Hamilton instrument drift.
year = 2024, month = sep, volume =
4 Pith papers cite this work. Polarity classification is still indexing.
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JWST/MIRI imaging of Eps Ind A b prefers a double-PSF model likely due to systematics but demonstrates sensitivity to exomoons down to 1.3 M_Jup at separations >2 AU and 2.5 M_Jup at 0.52 AU.
Archival MIRI imaging reaches contrasts of 10^-3 to 10^-4 at 1-3 arcseconds, enabling detection of ~170 K Jupiter-sized planets at separations >35 AU around M-dwarfs at 12.5 pc, with no new planets found but useful sensitivity maps produced.
The disk instability model remains viable for explaining giant planets that form early, at large orbital distances, and around M-dwarf stars, supported by updated simulations and observations.
citing papers explorer
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An Outer Giant Planet or Brown Dwarf in the 51 Pegasi System?
Tentative evidence for a super-Jupiter at 15-100 AU or brown dwarf at 20-170 AU in 51 Pegasi from RV curvature, but the signal is likely driven by Lick/Hamilton instrument drift.
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Direct Imaging Constraints on Binary Planets and Exomoons around Epsilon Indi A b
JWST/MIRI imaging of Eps Ind A b prefers a double-PSF model likely due to systematics but demonstrates sensitivity to exomoons down to 1.3 M_Jup at separations >2 AU and 2.5 M_Jup at 0.52 AU.
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A Search for Wide-orbit Planets Around M-dwarfs using Deep MIRI 15-micron Images
Archival MIRI imaging reaches contrasts of 10^-3 to 10^-4 at 1-3 arcseconds, enabling detection of ~170 K Jupiter-sized planets at separations >35 AU around M-dwarfs at 12.5 pc, with no new planets found but useful sensitivity maps produced.
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Giant Planet Formation by Disk Instability
The disk instability model remains viable for explaining giant planets that form early, at large orbital distances, and around M-dwarf stars, supported by updated simulations and observations.