Second-epoch JWST/MIRI-MRS mid-IR spectra of SN 1987A show little overall dust evolution but inner equatorial ring fading, rapid ejecta line changes, some ER line fading, first mid-IR H2 from ejecta, and evidence that dense Fe-rich ejecta has reached the reverse shock.
Title resolution pending
5 Pith papers cite this work. Polarity classification is still indexing.
5
Pith papers citing it
years
2026 5representative citing papers
Spatially resolved JWST spectroscopy of M82 reveals an average ortho-to-para H2 ratio half the equilibrium value, attributed to short cloud mixing timescales relative to spin conversion and recent rapid heating.
New NIR diagnostic diagrams using [C I]/Paγ and H2 1-0 O(5)/PAH 3.3μm ratios correlate with radiation field hardness and distinguish star formation, AGN, and shock excitation in galaxy nuclei.
Pulsational mass loss from supermassive stars ejects discrete shells that form the compact dense gas cocoons observed in Little Red Dots.
UV-bright companions to Little Red Dots provide Lyman-Werner fluxes of J21 ~ 10^2.5-10^5 that can suppress H2 cooling and enable direct collapse to massive black holes.
citing papers explorer
-
The evolution of the mid-infrared spectrum of SN 1987A observed with the JWST/MIRI-MRS
Second-epoch JWST/MIRI-MRS mid-IR spectra of SN 1987A show little overall dust evolution but inner equatorial ring fading, rapid ejecta line changes, some ER line fading, first mid-IR H2 from ejecta, and evidence that dense Fe-rich ejecta has reached the reverse shock.
-
JWST Observations of Starbursts: Molecular Hydrogen Excitation and Disequilibrium in M82
Spatially resolved JWST spectroscopy of M82 reveals an average ortho-to-para H2 ratio half the equilibrium value, attributed to short cloud mixing timescales relative to spin conversion and recent rapid heating.
-
Near-infrared diagnostic diagrams of the gas ionization sources in nearby galaxies: a JWST NIRSpec view
New NIR diagnostic diagrams using [C I]/Paγ and H2 1-0 O(5)/PAH 3.3μm ratios correlate with radiation field hardness and distinguish star formation, AGN, and shock excitation in galaxy nuclei.
-
Pulsational mass loss from supermassive stars creates the compact shells of Little Red Dots
Pulsational mass loss from supermassive stars ejects discrete shells that form the compact dense gas cocoons observed in Little Red Dots.
-
Connecting the Dots: UV-Bright Companions of Little Red Dots as Lyman-Werner Sources Enabling Direct Collapse Black Hole Formation
UV-bright companions to Little Red Dots provide Lyman-Werner fluxes of J21 ~ 10^2.5-10^5 that can suppress H2 cooling and enable direct collapse to massive black holes.