Solar system-sized condensations in the Orion Nebula

Churchwell, E.; Wood, D. O. S.; Felli, M.; Massi, M.

doi:10.1086/165648

Cited by 185 publications

(192 citation statements)

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“…Evidence suggests that the proplyds are undergoing mass loss from photoevaporation by the nearby O star q 1 Ori C, so the free-free emission we detect here is likely due to a wind (e.g., Churchwell et al 1987;Henney & Arthur 1998). For emission from a spherically symmetric wind with an arbitrary µ a -n r density profile the expected spectral dependence of free-free emission is (Wright & Barlow 1975).…”

Section: Estimating the Free-free Emission Spectrummentioning

confidence: 68%

“…They were first identified as free-free emission by Garay et al (1987), and suggested to be the ionized material evaporated from protostellar disks by Churchwell et al (1987). Observations of the ONC with the HST firmly established these compact structures as externally ionized protoplanetary disks (e.g., O'Dell et al 1993).…”

Section: Introductionmentioning

confidence: 99%

“…The hot gas ionized by this intense radiation expands freely and flows away at the local sound speed into lower pressure regions (e.g., Henney & Arthur 1998). The ionized winds from the protoplanetary disks emit strong free-free emission at radio wavelengths (e.g., Churchwell et al 1987;Garay et al 1987).…”

Section: Introductionmentioning

confidence: 99%

“…Compact radio sources have long been known in the ONC (e.g., Moran et al 1982;Churchwell et al 1987;Garay et al 1987;Felli et al 1993a;Zapata et al 2004aZapata et al , 2004b. They were first identified as free-free emission by Garay et al (1987), and suggested to be the ionized material evaporated from protostellar disks by Churchwell et al (1987).…”

Section: Introductionmentioning

confidence: 99%

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A Vla Survey for Faint Compact Radio Sources in the Orion Nebula Cluster

Sheehan

Eisner

Mann

et al. 2016

ApJ

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We present Karl G. Jansky Very Large Array 1.3, 3.6, and 6 cm continuum maps of compact radio sources in the Orion Nebular Cluster (ONC). We mosaicked 34 arcmin 2 at 1.3 cm, 70 arcmin 2 at 3.6 cm and 109 arcmin 2 at 6 cm, containing 778 near-infrared detected young stellar objects and 190 Hubble Space Telescope-identified proplyds (with significant overlap between those characterizations). We detected radio emission from 175 compact radio sources in the ONC, including 26 sources that were detected for the first time at these wavelengths. For each detected source, we fitted a simple free-free and dust emission model to characterize the radio emission. We extrapolate the free-free emission spectrum model for each source to ALMA bands to illustrate how these measurements could be used to correctly measure protoplanetary disk dust masses from submillimeter flux measurements. Finally, we compare the fluxes measured in this survey with previously measured fluxes for our targets, as well as four separate epochs of 1.3 cm data, to search for and quantify the variability of our sources.

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Section: Estimating the Free-free Emission Spectrummentioning

confidence: 68%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A Vla Survey for Faint Compact Radio Sources in the Orion Nebula Cluster

Sheehan

Eisner

Mann

et al. 2016

ApJ

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“…Together they cover an area of a few square arcminutes. This area is also one of the most crowded with YSOs emitting at radio frequencies (i.e., Churchwell et al 1987;Garay et al 1987;Zapata et al 2004;Kounkel et al 2014;Forbrich et al 2016). Taking advantage of these characteristics and using multi-epoch observations, the proper motion of several objects were measured by Gómez et al (2005Gómez et al ( , 2008.…”

Section: Introductionmentioning

confidence: 99%

Radio Measurements of the Stellar Proper Motions in the Core of the Orion Nebula Cluster

Dzib

Loinard

Rodrı́guez

et al. 2017

ApJ

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Using multi-epoch Very Large Array observations, covering a time baseline of 29.1 years, we have measured the proper motions of 88 young stars with compact radio emission in the core of the Orion Nebula Cluster (ONC) and the neighboring BN/KL region. Our work increases the number of young stars with measured proper motion at radio frequencies by a factor of 2.5 and enables us to perform a better statistical analysis of the kinematics of the region than was previously possible. 1.27 0.15 mas yr −1 . We looked for organized movements of these stars but found no clear indication of radial expansion/contraction or rotation. The remaining nine stars in our sample show peculiar proper motions that differ from the mean proper motions of the ONC by more than 3σ. One of these stars, V1326 Ori, could have been expelled from the Orion Trapezium 7000 years ago. Two could be related to the multi-stellar disintegration in the BN/KL region, in addition to the previously known sources BN, I and n. The others either have high uncertainties (so their anomalous proper motions are not firmly established) or could be foreground objects.

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Interaction between the Northeastern Boundary of Sgr A East and Giant Molecular Clouds: Excitation Mechanisms of the H Emission

Lee

Pak

Davis

et al. 2003

Proceedings of the Galactic Center Workshop 2002

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We have detected the v = 1 → 0 S(1) (λ = 2.1218µm) and v = 2 → 1 S(1) (λ = 2.2477µm) lines of H 2 in the Galactic centre, in a 90 × 27 arcsec region between the northeastern boundary of the non-thermal source, Sgr A East, and the giant molecular cloud (GMC) M-0.02-0.07. The detected H 2 v = 1 → 0 S(1) emission has an intensity of 1.6 -21 × 10 −18 W m −2 arcsec −2 and is present over most of the region. Along with the high intensity, the broad line widths (FWHM = 40 -70 km s −1 ) and the H 2 v = 2 → 1 S(1) to v = 1 → 0 S(1) line ratios (0.3 -0.5) can be best explained by a combination of C-type shocks and fluorescence. The detection of shocked H 2 is clear evidence that Sgr A East is driving material into the surrounding adjacent cool molecular gas. The H 2 emission lines have two velocity components at ∼ +50 km s −1 and ∼ 0 km s −1 , which are also present in the NH 3 (3,3) emission mapped by McGary, Coil, & Ho (2001). This two-velocity structure can be explained if Sgr A East is driving C-type shocks into both the GMC M-0.02-0.07 and the northern ridge of McGary, Coil, & Ho (2001).

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Solar system-sized condensations in the Orion Nebula

Cited by 185 publications

References 0 publications

A Vla Survey for Faint Compact Radio Sources in the Orion Nebula Cluster

A Vla Survey for Faint Compact Radio Sources in the Orion Nebula Cluster

Radio Measurements of the Stellar Proper Motions in the Core of the Orion Nebula Cluster

Interaction between the Northeastern Boundary of Sgr A East and Giant Molecular Clouds: Excitation Mechanisms of the H Emission

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