WISEPA J182831.08+265037.8 Archives

The top panel shows the synthetic spectrum for a Y dwarf at 10 pc with the atmospheric parameters given in the legend. WISE and JWST filter bandpasses are illustrated as red and yellow lines respectively. The middle and lower panels show the ratio of this spectrum divided by a spectrum where the surface gravity has been reduced, and by a spectrum where the metallicity is reduced, respectively. The total energy emitted by the lower gravity dwarf is greater because the radius is larger (Marley et al. 2021), hence the average value in the middle panel is < 1. Note that all three models have similar flux levels averaged over the λ ≈ 4.5 µm flux peak, for example through an imaging filter, although the strength of the absorption features at these wavelengths (primarily due to CO and CO2) are sensitive to gravity. See Section 3 for further discussion. -- astro-ph.SR

Astronomy & Telescopes, Atmospheres, Climate, Weather, Brown Dwarfs, Exoplanets, -moons, -comets, Imaging & Spectroscopy, Status Report

Redshifting the Study of Cold Brown Dwarfs and Exoplanets: the Mid-Infrared Wavelength Region as an Indicator of Surface Gravity and Mass

by Keith CowingNovember 18, 2024November 18, 2024

JWST is opening many avenues for exploration. For cold brown dwarfs and exoplanets, JWST has opened the door to the mid-infrared wavelength region, where such objects emit significant energy.

WISEPA J182831.08+265037.8

Redshifting the Study of Cold Brown Dwarfs and Exoplanets: the Mid-Infrared Wavelength Region as an Indicator of Surface Gravity and Mass

Roman Space Telescope: Enabling Images Of Distant Worlds

NASA Solar System Exploration Research Virtual Institute (SSERVI) Cooperative Agreement Notice (NNH26ZDA016C) Final Text And Due Dates

Interstellar Aromatic Infrared Bands: IR Absorption Spectroscopy Of The Lowest Triplet State Of Naphthalene

The Highly Unusual Behavior And Chemical Composition Of Interstellar Comet 2I/Borisov

Volatile Depletion In Rocky Planets As A Chemical Fingerprint Of Hybrid Accretion