The Orion fingers: Near-IR adaptive optics imaging of an explosive protostellar outflow

Bally, John; Ginsburg, Adam; Silvia, Devin W.; Youngblood, Allison

doi:10.1051/0004-6361/201425073

Cited by 59 publications

(140 citation statements)

References 63 publications

(103 reference statements)

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“…The dynamical decay model also provides an explanation for the system of high velocity (up to 300 km s −1 ) "bullets," bow shocks and "fingers" that are visible in lines of H 2 , Fe II, and CO, and that appear to emerge from a common center a few arcseconds NW of SrcI (Allen & Burton 1993;Zapata et al 2009;Bally et al 2011Bally et al , 2015. At one time the finger system was assumed to be a high velocity outflow from SrcI, but now it is recognized as the signpost of an explosive event 500-1000 years ago (Doi et al 2002;Bally et al 2011).…”

Section: Rethinking the Paradigmmentioning

confidence: 95%

“…At one time the finger system was assumed to be a high velocity outflow from SrcI, but now it is recognized as the signpost of an explosive event 500-1000 years ago (Doi et al 2002;Bally et al 2011). The bullets are interpreted as dense fragments of circumstellar disks that were torn apart in a stellar encounter and launched into the surrounding cloud (Bally et al 2015).…”

Section: Rethinking the Paradigmmentioning

confidence: 99%

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ALMA OBSERVATIONS OF ORION SOURCE I AT 350 AND 660 GHz

Plambeck¹,

Wright

2016

ApJ

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Orion Source I ("SrcI") is the protostar at the center of the Kleinmann-Low Nebula. ALMA observations of SrcI with 0.2 angular resolution were made at 350 and 660 GHz to search for the H26α and H21α hydrogen recombination lines and to measure the continuum flux densities. The recombination lines were not detected, ruling out the possibility that SrcI is a hypercompact HII region. The deconvolved size of the continuum source is approximately 0. 23 × 0. 07 (∼ 100 × 30 AU); it is interpreted as a disk viewed almost edge-on. Optically thick thermal emission from ∼500 K dust is the most plausible source of the continuum, even at frequencies as low as 43 GHz; the disk mass is most likely in the range 0.02-0.2 M . A rich spectrum of molecular lines is detected, mostly from sulfur-and silicon-rich molecules like SO, SO 2 , and SiS, but also including vibrationally excited CO and several unidentified transitions. Lines with upper energy levels E U > 500 K appear in emission and are symmetric about the source's LSR velocity of 5 km s −1 , while lines with E U < 500 K appear as blueshifted absorption features against the continuum, indicating that they originate in outflowing gas. The emission lines exhibit a velocity gradient along the major axis of the disk that is consistent with rotation around a 5-7 M central object. The relatively low mass of SrcI and the existence of a 100 AU disk around it are difficult to reconcile with the model in which SrcI and the nearby Becklin-Neugebauer Object were ejected from a multiple system 500 years ago.

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Section: Rethinking the Paradigmmentioning

confidence: 95%

Section: Rethinking the Paradigmmentioning

confidence: 99%

ALMA OBSERVATIONS OF ORION SOURCE I AT 350 AND 660 GHz

Plambeck¹,

Wright

2016

ApJ

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“…These "upside-down V-shaped" features may trace very low-velocity CO swept-up from the ambient medium. Figure 9 shows a high-resolution image of the outflow from Bally et al (2015). Figure 10 shows a cartoon illustrating the various features discussed above.…”

Section: Low Radial-velocity Structurementioning

confidence: 99%

“…The momentum and kinetic energy in the motion of BN could be balanced by slower and lower-mass Source I plus the momentum and energy of Source n. Source n has a luminosity of ∼2000 L e , an estimated mass of 3-6 M e , and is surrounded by a 340 by 230 au diameter disk detected at 8 and 11.7 μm Bally et al (2015) in the region containing the north and northwest fingers. (Greenhill et al 2004).…”

Section: The Potential Role Of Source Nmentioning

confidence: 99%

“…Short-lived, powerful explosions, accompanied by luminous infrared flares can be powered by gravitational interactions of three or more stars in dense star clusters that can lead to the formation of binaries by capture and stellar mergers (Bally & Zinnecker 2005;Soker & Tylenda 2006;Moeckel & Bally 2007a, 2007bPortegies Zwart & van den Heuvel 2016). Such an explosion occurred behind the Orion Nebula ∼500 years ago (Zapata et al 2009;Bally et al 2011Bally et al , 2015.…”

Section: Introductionmentioning

confidence: 99%

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The ALMA View of the OMC1 Explosion in Orion

Bally¹,

Ginsburg²,

Arce

et al. 2017

ApJ

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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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Scientific Goals of the Kunlun Infrared Sky Survey (KISS)

Burton

Zheng²,

Mould

et al. 2016

Publ. Astron. Soc. Aust.

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The high Antarctic plateau provides exceptional conditions for conducting infrared observations of the cosmos on account of the cold, dry and stable atmosphere above the ice surface. This paper describes the scientific goals behind the first program to examine the time-varying universe in the infrared from Antarctica -the Kunlun Infrared Sky Survey (KISS). This will employ a small (50 cm aperture) telescope to monitor the southern skies in the 2.4µm K dark window from China's Kunlun station at Dome A, on the summit of the Antarctic plateau, through the uninterrupted 4-month period of winter darkness. An earlier paper discussed optimisation of the K dark filter for the best sensitivity (Li et al. 2016). This paper examines the scientific program for KISS. We calculate the sensitivity of the camera for the extrema of observing conditions that will be encountered. We present the parameters for sample surveys that could then be carried out for a range of cadences and sensitivities. We then discuss several science programs that could be conducted with these capabilities, involving star formation, brown dwarfs and hot Jupiters, exoplanets around M dwarfs, the terminal phases of stellar evolution, discovering fast transients as part of multi-wavelength campaigns, embedded supernova searches, reverberation mapping of active galactic nuclei, gamma ray bursts and the detection of the cosmic infrared background.

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The Orion fingers: Near-IR adaptive optics imaging of an explosive protostellar outflow

Cited by 59 publications

References 63 publications

ALMA OBSERVATIONS OF ORION SOURCE I AT 350 AND 660 GHz

ALMA OBSERVATIONS OF ORION SOURCE I AT 350 AND 660 GHz

The ALMA View of the OMC1 Explosion in Orion

Scientific Goals of the Kunlun Infrared Sky Survey (KISS)

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