Arcsecond-Scale Kinematic and Chemical Complexity in Cepheus A East

Brogan, C. L.; Chandler, Claire J.; Hunter, T. R.; Shirley, Yancy L.; Sarma, A. P.

doi:10.1086/518390

Cited by 45 publications

(73 citation statements)

References 24 publications

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“…An opening angle of approximately 20 • (position angle of 90 • ) suffices to excite the individual clumps of the HW 3d complex. This model would be in line with the interpretation of Brogan et al (2007), who detected submillimetre emission towards HW 3c, but not towards HW 3b or 3d. However, the origin of the water maser emission within the HW 3d complex remains unclear in this scenario.…”

Section: Discussionsupporting

confidence: 91%

“…However, there is no consensus about their nature in the literature. In the vicinity of HW 3a, 3b and 3d water maser activity has been found (Cohen et al 1984;Torrelles et al 1998), while HW 3c has an associated submillimetre core (Brogan et al 2007) and a composite spectrum, suggesting the presence of a jet (Hughes 2001). HW 3a breaks up into two time-variable components; one might be associated with an infrared source (GPFW 1a (diamond in Fig.…”

Section: Introductionmentioning

confidence: 98%

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The Chandra X-ray view of the power sources in Cepheus A

Schneider

Günther

Schmitt

2009

A&A

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The central part of the massive star-forming region Cepheus A contains several radio sources which indicates multiple outflow phenomena, yet the driving sources of the individual outflows have not been identified. We present a high-resolution Chandra observation of this region that shows the presence of bright X-ray sources with luminosities of L X 10 30 erg s −1 , consistent with active pre-main sequence stars, while the strong absorption hampers the detection of less luminous objects. A new source has been discovered located on the line connecting H 2 emission regions at the eastern and western parts of Cepheus A. This source could be the driving source of HH 168. We present a scenario relating the observed X-ray and radio emission.

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Section: Discussionsupporting

confidence: 91%

Section: Introductionmentioning

confidence: 98%

The Chandra X-ray view of the power sources in Cepheus A

Schneider

Günther

Schmitt

2009

A&A

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“…the CH 3 CN(12 3 -11 3 )), which is strongly suggestive of external heating. The molecular emission with low excitation temperatures and/or critical densities may have a very erratic behavior for different species, and be unhelpful in pinpointing the true exciting source as already observed in the Orion KL hot core (Wilson et al 2000;Blake et al 1996;Wright et al 1996), and in some other hot cores (Brogan et al 2007;Mookerjea et al 2007). …”

Section: Heating Of the Orion Kl Hot Core By An Explosive Flowmentioning

confidence: 95%

Orion KL: the hot core that is not a “hot core”

Zapata

Schmid-Burgk

Menten

2011

A&A

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We present sensitive high angular resolution submillimeter and millimeter observations of torsionally/vibrationally highly excited lines of the CH 3 OH, HC 3 N, SO 2 , and CH 3 CN molecules and of the continuum emission at 870 and 1300 μm from the Orion KL region, made with the Submillimeter Array (SMA). These observations and SMA CO J = 3−2 and J = 2−1 imaging of the explosive flow originating in this region suggest that the molecular Orion "hot core" is a pre-existing density enhancement heated from the outside by the explosive event. Unlike in other hot cores, we do not find any self-luminous submillimeter, radio, or infrared source embedded in the hot molecular gas, nor observe filamentary CO flow structures or "fingers" in the shadow of the hot core pointing away from the explosion center. The low-excitation CH 3 CN emission shows the typical molecular heart-shaped structure, traditionally named the hot core, and is centered close to the dynamical origin of the explosion. The highest excitation CH 3 CN lines all originate from the northeast lobe of the heart-shaped structure, i.e. from the densest and most highly obscured parts of the extended ridge. The torsionally excited CH 3 OH and vibrationally excited HC 3 N lines appear to form a shell around the strongest submillimeter continuum source. All of these observations suggest that the southeast and southwest sectors of the explosive flow have impinged on a pre-existing very dense part of the extended ridge, thus creating the bright Orion KL hot core. However, additional theoretical and observational studies are required to test this new heating scenario.

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“…Submillimeter wavelength continuum interferometry at 875 μm (Brogan et al 2007) shows strong dust emission from HW2, HW3c, and extended emission to the southwest near HW3a. No submm continuum was detected from HW3d, leading these authors to conclude that HW3c is most likely to harbor the second most luminous and massive YSO in the Cep A core.…”

Section: Overview Of Cep Amentioning

confidence: 98%

A Pulsed, Precessing Jet in Cepheus A

Cunningham

Moeckel

Bally

2009

ApJ

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We present near-infrared H 2 , radio CO, and thermal infrared observations of the nearby massive star-forming region Cepheus A (Cep A). From H 2 bow shocks arranged along four distinct jet axes, we infer that the massive protostellar source HW2 drives a pulsed, precessing jet that has changed its orientation by about 45• in roughly 10 4 years. The current HW2 radio jet represents the most recent event in this time series of eruptions. This scenario is consistent with the recent discovery of a disk around HW2, perpendicular to the current jet orientation, and with the presence of companions at projected distances comparable to the disk radius. We propose that the Cep A system formed by the disk-assisted capture of a sibling star by HW2. We present a numerical model of a 15 M star with a circumstellar disk, orbited by a companion in an inclined, eccentric orbit. Close passages of the companion through or near the disk result in periods of enhanced accretion and mass loss, as well as forced precession of the disk and associated orientation changes in the jet. The observations reveal a second powerful outflow that emerges from radio source HW3c or HW3d. This flow is associated with blueshifted CO emission and a faint H 2 bow shock to the east, and with HH 168 to the west. A collision between the flows from HW2 and HW3c/d may be responsible for X-ray and radio continuum emission in Cep A West.

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Arcsecond-Scale Kinematic and Chemical Complexity in Cepheus A East

Cited by 45 publications

References 24 publications

The Chandra X-ray view of the power sources in Cepheus A

The Chandra X-ray view of the power sources in Cepheus A

Orion KL: the hot core that is not a “hot core”

A Pulsed, Precessing Jet in Cepheus A

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