Herbig Haro Objects in the Orion Nebula.

O’Dell, C. R.; Hartigan, Patrick; Lane, W. M.; Wong, S. K.; Burton, M. G.; Raymond, John R.; Axon, D. J.

doi:10.1086/118507

Cited by 48 publications

(50 citation statements)

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“…At the bar, HH 203 and HH 204 (at 120 00 , À160 00 and 130 00 , À180 00 , respectively) are detected at mid-infrared wavelengths. Both HH 203 and HH 204 are bow shocks propagating to the southeast (O'Dell et al 1997). Flows HH 202 and HH 529 are propagating north and east, respectively, from OMC1-S.…”

Section: Source Identification and Optical Counterpartsmentioning

confidence: 98%

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Mid‐Infrared Emission at Photodissociation Regions in the Orion Nebula

Kassis

Adams

Campbell

et al. 2006

ApJ

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The mid-infrared emission from a photodissociation region (PDR) viewed edge-on in the Orion Nebula is examined through 8.7-20.6 m images and 8-13 m spectra. The polycyclic aromatic hydrocarbon (PAH ) emission is located between the edges of H ii regions and layers of [C i] emission, agreeing with PDR theory. Using a simple model, the spatial variations in the emission from PAHs detected at 8.6, 11.2, and 12.7 m are demonstrated to be directly proportional to the material column density and the intensity of the UV field. For a homogeneous, neutral cloud illuminated by a bright OB star, PDR theory predicts that the ultraviolet (UV ) radiation is attenuated exponentially (e À1:8 A v ). The predicted UV attenuation is confirmed by observations of broad PAH emission features found at 8.6, 11.2, and 12.7 m. The PAH emission is found in cool regions having greater optical depths relative to regions where mid-infrared emission from ionized gas is observed. Through modeling we determine a gas density of 9:7 ; 10 4 cm À3 . On large and small size scales, the relative strengths of the 8.6, 11.2, and 12.7 m PAH features at the bar of the Orion Nebula indicate that there is not a simple transition from ionized to neutral PAHs across the PDR.

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Section: Source Identification and Optical Counterpartsmentioning

confidence: 98%

“…Shocks and jets are common in the Orion Nebula (O'Dell et al 1997;Bally et al 2000), and a handful of mid-infrared features are coincident with Herbig-Haro (HH) flows. At the bar, HH 203 and HH 204 (at 120 00 , À160 00 and 130 00 , À180 00 , respectively) are detected at mid-infrared wavelengths.…”

Section: Source Identification and Optical Counterpartsmentioning

confidence: 99%

Mid‐Infrared Emission at Photodissociation Regions in the Orion Nebula

Kassis

Adams

Campbell

et al. 2006

ApJ

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“…Over a dozen shocks protrude into the Orion Nebula as Herbig-Haro (HH) objects (Axon & Taylor 1984;O'dell et al 1997a, 1997bKaifu et al 2000;Doi et al 2002;Graham et al 2003;Doi et al 2004) demonstrating that the outflow is located within ∼0.1 pc of the ionization front at the rear of the Nebula. The HH objects and [Fe II] knots north and northwest of OMC1, located at the largest projected distance from this core, exhibit proper motions of over 400 km s −1 , indicating an∼500 year age of the outflow, similar to the time since the ejection of the stars (Jones & Walker 1985;Lee & Burton 2000;Doi et al 2002;Bally et al 2011Bally et al , 2015.…”

Section: The Omc1 Outflowmentioning

confidence: 99%

The ALMA View of the OMC1 Explosion in Orion

Bally¹,

Ginsburg²,

Arce

et al. 2017

ApJ

105

157

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Most massive stars form in dense clusters where gravitational interactions with otherstars may be common. The two nearest forming massive stars, the BN object and Source I, located behind the Orion Nebula, were ejected with velocities of ∼29 and ∼13 km s −1 about 500 years ago by such interactions. This event generated an explosion in the gas. New ALMA observations show in unprecedented detail, a roughly spherically symmetric distribution of over a hundred 12 CO J=2−1 streamers with velocities extending from V LSR =−150 to +145 km s −1 . The streamer radial velocities increase (or decrease) linearly with projected distance from the explosion center, forming a "Hubble Flow" confined to within 50″ of the explosion center. They point toward the high proper-motion, shockexcited H 2 and [Fe II] "fingertips" and lower-velocity CO in the H 2 wakes comprising Orionʼs "fingers." In some directions, the H 2 "fingers" extend more than a factor of two farther from the ejection center than the CO streamers. Such deviations from spherical symmetry may be caused by ejecta running into dense gas or the dynamics of the N-body interaction that ejected the stars and produced the explosion. This ∼10 48 erg event may have been powered by the release of gravitational potential energy associated with the formation of a compact binary or a protostellar merger. Orion may be the prototype for a new class of stellar explosiozn responsible for luminous infrared transients in nearby galaxies.

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“…As discussed in detail in G2003, our procedures thus reject weaker objects and are ill-suited to the detection of relatively faint bullets in the field. We are aware of two cases of such faint objects superposed on brigher, slower moving features: HH208 (Axon & Taylor 1984;O'Dell et al 1997), and that mentioned in G2003. In fact we detect a low velocity component of HH208, object B-42, Table A.3.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Observations of spatial and velocity structure in the Orion molecular cloud

Nissen¹,

Gustafsson²,

Lemaire

et al. 2007

A&A

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Observations are reported of H 2 IR emission in the S(1) v = 1−0 line at 2.121 µm in the Orion Molecular Cloud, OMC1, using the GriF instrument on the Canada-France-Hawaii Telescope. GriF uses a combination of adaptive optics and Fabry-Perot interferometry, yielding a spatial resolution of 0.15 to 0.18 and velocity discrimination as high as 1 km s −1 . 193 bright H 2 emission regions can be identified in OMC1. The general characteristics of these features are described in terms of radial velocities, brightness and spatial displacement of maxima of velocity and brightness, the latter to yield the orientation of flows in the plane of the sky. Strong spatial correlation between velocity and bright H 2 emission is found and serves to identify many features as shocks. Important results are: (i) velocities of the excited gas illustrate the presence of a zone to the south of BN-IRc2 and Peak 1, and the west of Peak 2, where there is a powerful blue-shifted outflow with an average velocity of −18 km s −1 . This is shown to be the NIR counterpart of an outflow previously identified in the radio, originating from either source I or source n. (ii) There is a band of weak radial velocity features (<5 km s −1 ) in Peak 1. (iii) A small proportion of the flows may represent sites of low mass star formation and one region shows evidence of multiple flows which may indicate multiple low mass star formation within OMC1.

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Herbig Haro Objects in the Orion Nebula.

Cited by 48 publications

References 0 publications

Mid‐Infrared Emission at Photodissociation Regions in the Orion Nebula

Mid‐Infrared Emission at Photodissociation Regions in the Orion Nebula

The ALMA View of the OMC1 Explosion in Orion

Observations of spatial and velocity structure in the Orion molecular cloud

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