Molecular tracers of radiative feedback in Orion (OMC-1) Widespread CH+ (J = 1-0), CO (10-9), HCN (6-5), and HCO+ (6-5) emission.

Astronomy and Astrophysics
J R GoicoecheaSara Cuadrado

Abstract

Young massive stars regulate the physical conditions, ionization, and fate of their natal molecular cloud and surroundings. It is important to find tracers that help quantifying the stellar feedback processes that take place at different spatial scales. We present ~85 arcmin2 (~1.3 pc2) velocity-resolved maps of several submillimeter molecular lines, taken with Herschel/HIFI, toward the closest high-mass star-forming region, the Orion molecular cloud 1 core (OMC-1). The observed rotational lines include probes of warm and dense molecular gas that are difficult, if not impossible, to detect from ground-based telescopes: CH+ (J = 1-0), CO (J = 10-9), HCO+ (J = 6-5) and HCN (J = 6-5), and CH (N, J =1, 3/2-1, 1/2). These lines trace an extended but thin layer (A V ≃3-6 mag or ~1016 cm) of molecular gas at high thermal pressure, P th = n H · T k ≈ 107 - 109 cm-3 K, associated with the far ultraviolet (FUV) irradiated surface of OMC-1. The intense FUV radiation field, emerging from massive stars in the Trapezium cluster, heats, compresses and photoevaporates the cloud edge. It also triggers the formation of specific reactive molecules such as CH+. We find that the CH+ (J = 1-0) emission spatially correlates with the flux of FUV photo...Continue Reading

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Nov 17, 2015·The Astrophysical Journal·Javier R GoicoecheaJ Stutzki
Aug 12, 2016·Nature·Javier R GoicoecheaPaolo Pilleri
Dec 23, 2016·Astronomy and Astrophysics·S CuadradoJ Cernicharo
Jul 12, 2017·Astronomy and Astrophysics·Javier R GoicoecheaMaryvonne Gerin
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Oct 11, 2017·Astronomy and Astrophysics·C H M PabstA G G M Tielens
Nov 17, 2017·Astronomy and Astrophysics·S CuadradoB Tercero

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