A High-Resolution Map of the Orion Nebula Region at Far-Infrared Wave-Lengths

Fazio, G. G.; Kleinmann, D. E.; Noyes, R. W.; Wright, E. L.; Zeilik, M.; Low, F. J.

doi:10.1086/181580

Cited by 14 publications

(2 citation statements)

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“…The Orion Bar is illuminated by the O7-type star θ 1 Ori C, the most massive member of the Trapezium young stellar cluster, which lies at the heart of the Orion Nebula (about 2′ north west of the Bar, e.g., O'Dell 2001). The intense ionizing radiation and strong winds from θ 1 Ori C power and shape the nebula (Güdel et al 2008;Pabst et al 2019) The Bar (also referred to as the Bright Bar (e.g., Balick et al 1974;Fazio et al 1974;Werner et al 1976) historically refers to the elongated rim near the ionization front (originally detected in the radio continuum and in optical lines) that separates the neutral cloud from the ionized H II gas with an electron temperature T e ≈ 10 4 K and electron density n e of several 1000 cm −3 (e.g., Weilbacher et al 2015, and references therein). The UV radiation field incident on the Orion Bar PDR is G 0 = (1-4) × 10 4 (e.g., Marconi et al 1998).…”

Section: Target: the Orion Barmentioning

confidence: 99%

PDRs4All: A JWST Early Release Science Program on Radiative Feedback from Massive Stars

Berné¹,

Habart²,

Peeters³

et al. 2022

PASP

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Massive stars disrupt their natal molecular cloud material through radiative and mechanical feedback processes. These processes have profound effects on the evolution of interstellar matter in our Galaxy and throughout the universe, from the era of vigorous star formation at redshifts of 1–3 to the present day. The dominant feedback processes can be probed by observations of the Photo-Dissociation Regions (PDRs) where the far-ultraviolet photons of massive stars create warm regions of gas and dust in the neutral atomic and molecular gas. PDR emission provides a unique tool to study in detail the physical and chemical processes that are relevant for most of the mass in inter- and circumstellar media including diffuse clouds, proto-planetary disks, and molecular cloud surfaces, globules, planetary nebulae, and star-forming regions. PDR emission dominates the infrared (IR) spectra of star-forming galaxies. Most of the Galactic and extragalactic observations obtained with the James Webb Space Telescope (JWST) will therefore arise in PDR emission. In this paper we present an Early Release Science program using the MIRI, NIRSpec, and NIRCam instruments dedicated to the observations of an emblematic and nearby PDR: the Orion Bar. These early JWST observations will provide template data sets designed to identify key PDR characteristics in JWST observations. These data will serve to benchmark PDR models and extend them into the JWST era. We also present the Science-Enabling products that we will provide to the community. These template data sets and Science-Enabling products will guide the preparation of future proposals on star-forming regions in our Galaxy and beyond and will facilitate data analysis and interpretation of forthcoming JWST observations.

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Section: Target: the Orion Barmentioning

confidence: 99%

PDRs4All: A JWST Early Release Science Program on Radiative Feedback from Massive Stars

Berné¹,

Habart²,

Peeters³

et al. 2022

PASP

View full text Add to dashboard Cite

show abstract

“…Thermal and Mid-Infrared Data Initial mid-IR scale maps were limited by a combination of the very strong nebular background and the poor angular resolution of early mid-IR cameras. Works by Ney & Allen (1969); Lemke et al (1974); Fazio et al (1974); Gehrz et al (1975), which span the wavelength regime from 20 to 100 µm, tell us little about the overall stellar content or properties of the members of the star cluster although they do reveal many details about the structure of the photodissociation region, e.g. the modern study by Kassis et al (2006).…”

Section: Optical To Infrared Imaging Surveysmentioning

confidence: 99%

Star Formation in the Orion Nebula I: Stellar Content

Muench,

Getman,

Hillenbrand

et al. 2008

Preprint

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The Orion Nebula is one of the most frequently observed nearby (< 1 kiloparsec) star forming regions and, consequently, the subject of a large bibliography of observations and interpretation. The summary in this chapter is bounded spatially by the blister HII region, with sources beyond the central nebula that are part of the same dynamical clustering covered in other chapters in this book. Herein are discussed panchromatic observations of the massive OB stars, the general T Tauri population, the sub-stellar sources and variable stars within the Orion Nebula. First, a brief history of 400 years of observation of the Nebula is presented. As this history is marked clearly by revelations provided in each age of new technology, recent ultra-deep X-ray surveys and high resolution multi-epoch monitoring of massive binary systems and radio stars receive special attention in this review. Topics discussed include the kinematics, multiplicity, mass distribution, rotation, and circumstellar characteristics of the pre-main sequence population. Also treated in depth are historical and current constraints on the distance to the Orion Nebula Cluster; a long standing 10-20% uncertainty has only recently begun to converge on a value near ∼ 400 parsecs. Complementing the current review of the stellar population is a companion chapter reviewing the molecular cloud, ionized HII region and the youngest protostellar sources.

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7.3.4 The individual HII regions

Scheffler¹

Interstellar Matter, Galaxy, Universe

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A High-Resolution Map of the Orion Nebula Region at Far-Infrared Wave-Lengths

Cited by 14 publications

References 0 publications

PDRs4All: A JWST Early Release Science Program on Radiative Feedback from Massive Stars

PDRs4All: A JWST Early Release Science Program on Radiative Feedback from Massive Stars

Star Formation in the Orion Nebula I: Stellar Content

7.3.4 The individual HII regions

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