14 citations · 15 across the 2 of their papers we have counts for
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PDRs4All XVII: Formation and excitation of HD in photodissociation regions. Application to the Orion Bar
Marion Zannese, Jacques Le Bourlot, Evelyne Roueff +12
The James Webb Space Telescope enabled the first detection of several rovibrational emission lines of HD in the Orion Bar, a prototypical photodissociation region. This provides an…
JWST observations of photodissociation regions: II. Warm molecular Hydrogen spectroscopy in the Horsehead nebula
M. Zannese, P. Guillard, A. Abergel +16
H2 is the most abundant molecule in the interstellar medium and is a useful tool to study photodissociation regions, where radiative feedback from massive stars on molecular clouds…
PDRs4All XIX. The 6 to 9 m region as a probe of PAH charge and size in the Orion Bar
Baria Khan, Samuel A. Daza Rodriguez, Els Peeters +24
Infrared emission from polycyclic aromatic hydrocarbons (PAHs) play a major role in determining the charge balance of their host environments that include photo-dissociation region…
JWST Observations of Photo-dissociation Regions. II. Aliphatic/Aromatic Carbonaceous Dust, Ices, and Gas Phase Spectral Line Inventory
K. Misselt, A. N. Witt, K. D. Gordon +10
This paper provides an overview of the spectroscopic data obtained by the JWST Guaranteed Time Observations (GTO) program 1192, "The Physics and Chemistry of PDR Fronts", including…
PDRs4All XI. Detection of infrared CH and CH rovibrational emission in the Orion Bar and disk d203-506: evidence of chemical pumping
Marion Zannese, Benoît Tabone, Emilie Habart +20
The methylidyne cation (CH) and the methyl cation (CH) are building blocks of organic molecules, yet their coupled formation and excitation mechanisms remain mainly unpro…
Evidence of dust grain evolution from extinction mapping in the IC 63 photodissociation region
Dries Van De Putte, Karl D. Gordon, Julia Roman-Duval +5
Photodissociation regions (PDRs) are parts of the ISM consisting of predominantly neutral gas, located at the interface between H II regions and molecular clouds. The physical cond…