Explosive Disintegration of a Massive Young Stellar System in Orion

Zapata, Luis A.; Schmid-Burgk, J.; Ho, Paul T. P.; Rodrı́guez, Luis F.; Menten, K. M.

doi:10.1088/0004-637x/704/1/l45

Cited by 120 publications

(239 citation statements)

References 24 publications

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“…17, which shows the position of the IRc sources from Shuping et al (2004) with respect to the methyl formate emission. On larger scales ( > ∼ 10 or 4500 AU), it seems, as discussed below, that the methyl formate distribution is closely linked to the presence of a few remarkable objects, in particular the "low-velocity" SiO outflow whose origin is attributed to radiosource I by Goddi et al (2009) and Plambeck et al (2009), and linked to the matter (traced in CO and H 2 ) ejected during the recent (∼500 yr) stellar collision or close interaction between the B-type star BN, and the I and n objects (at least) as proposed by, e.g., Zapata et al (2009). Long-range effects of heating, photodissociating photons, or shocks are also possible from BN itself and source n. Our data do not allow us to separate the respective effects of source I from source SMA1, which has recently been identified by Beuther & Nissen (2008) as another candidate source for the high-velocity CO and H 2 outflow.…”

Section: Stars and Ysosmentioning

confidence: 83%

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HCOOCH₃as a probe of temperature and structure in Orion-KL

Favre

Despois

Brouillet

et al. 2011

A&A

100

238

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Context. The Orion Kleinmann-Low nebula (Orion-KL) is a complex region of star formation. Whereas its proximity allows studies on a scale of a few hundred AU, spectral confusion makes it difficult to identify molecules with low abundances. Aims. We studied an important oxygenated molecule, HCOOCH 3 , to characterize the physical conditions, temperature, and density of the different molecular source components. Methyl formate presents strong close rotational transitions covering a wide range of energy, and its emission in Orion-KL is not contaminated by the emission of N-bearing molecules. This study will help in the future 1) to constrain chemical models for the formation of methyl formate in gas phase or on grain mantles and 2) to search for more complex or prebiotic molecules. Methods. We used high-resolution observations from the IRAM Plateau de Bure Interferometer to reduce spectral confusion and to better isolate the molecular emission regions. We used twelve data sets with a spatial resolution down to 1.8 × 0.8 . Continuum emission was subtracted by selecting apparently line-free channels. Results. We identify 28 methyl formate emission peaks throughout the 50 field of observations. The two strongest peaks, named MF1 and MF2, are in the Compact Ridge and in the southwest of the Hot Core, respectively. From a comparison with single-dish observations, we estimate that we miss less than 15% of the flux and that spectral confusion is still prevailing as half of the expected transitions are blended over the region. Assuming that the transitions are thermalized, we derive the temperature at the five main emission peaks. At the MF1 position in the Compact Ridge we find a temperature of 80 K in a 1.8 × 0.8 beam size and 120 K on a larger scale (3.6 × 2.2 ), suggesting an external source of heating, whereas the temperature is about 130 K at the MF2 position on both scales. Transitions of methyl formate in its first torsionally excited state are detected as well, and the good agreement of the positions on the rotational diagrams between the ground state and the v t = 1 transitions suggests a similar temperature. The LSR velocity of the gas is between 7.5 and 8.0 km s −1 depending on the positions and column density peaks vary from 1.6 × 10 16 to 1.6 × 10 17 cm −2 . A second velocity component is observed around 9−10 km s −1 in a north-south structure stretching from the Compact Ridge up to the BN object, and this component is warmer at the MF1 peak. The two other C 2 H 4 O 2 isomers are not detected, and the derived upper limit for the column density is ≤3 × 10 14 cm −2 for glycolaldehyde and ≤2 × 10 15 cm −2 for acetic acid. From the 223 GHz continuum map, we identify several dust clumps with associated gas masses in the range 0.8 to 5.8 M . Assuming that the methyl formate is spatially distributed as the dust is, we find relative abundances of methyl formate in the range ≤0.1 × 10 −8 to 5.2 × 10 −8 . We suggest a relation between the methyl formate distribution and shocks as traced by 2.12 μm H 2 emission.

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Section: Stars and Ysosmentioning

confidence: 83%

“…Most of the H 2 emission can be traced to a common center whose coordinates are given in Table 9 (e.g. Zapata et al 2009, and refs. therein).…”

Section: Hcooch 3 and Ir 11 μM Mapmentioning

confidence: 99%

HCOOCH₃as a probe of temperature and structure in Orion-KL

Favre

Despois

Brouillet

et al. 2011

A&A

100

238

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“…Menten & Reid (1995) detected the radio continuum emission of the IR source n and the very embedded radio source I (located a few arcseconds to the south of the young and massive star IRc2), which could be a binary system with a total mass of ∼20 M , according to measurements of the proper motions of this source and the object BN (Goddi et al 2011). Source I has been proposed as a possible driver of the two outflows observed in Orion KL: a high-velocity (30−100 km s −1 ), wide-angle (∼1 rad) outflow A&A 559, A51 (2013) that extends northwest-southeast over 0.3 pc, and a low-velocity (∼18 km s −1 ) elongated northeast-southwest outflow (Genzel & Stutzki 1989;Greenhill et al 1998;Zapata et al 2009). …”

Section: Introductionmentioning

confidence: 99%

Combined IRAM andHerschel/HIFI study of cyano(di)acetylene in Orion KL: tentative detection of DC₃N

Esplugues

Cernicharo

Viti

et al. 2013

A&A

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Context. We present a study of cyanoacetylene (HC 3 N) and cyanodiacetylene (HC 5 N) in Orion KL using observations from two line surveys performed with the IRAM 30-m telescope and the HIFI instrument onboard the Herschel telescope. The frequency ranges covered are 80−280 GHz and 480−1906 GHz. Aims. This study (divided by families of molecules) is part of a global analysis of the physical conditions of Orion KL and the molecular abundances in the different components of this cloud. Methods. We modeled the observed lines of HC 3 N, HC 5 N, their isotopologues (including DC 3 N), and vibrational modes using a non-local thermodynamic equilibrium (non-LTE) radiative transfer code. In addition, to investigate the chemical origin of HC 3 N and DC 3 N in Orion KL, we used a time-dependent chemical model. Results. We detect 40 lines of the ground vibrational state of HC 3 N and 68 lines of its 13 C isotopologues. We also detect 297 lines of six vibrational modes of this molecule (ν 7 , 2ν 7 , 3ν 7 , ν 6 , ν 5 , and ν 6 +ν 7 ) and 35 rotational lines of the ground vibrational state of HC 5 N. We report the first tentative detection of DC 3 N in a giant molecular cloud. We have obtained a DC 3 N/HC 3 N abundance ratio of 0.015 ± 0.009, similar to typical D/H ratios of cold dark clouds. We provide column densities for all species and derived isotopic and molecular abundances. We also made a 2 × 2 map around Orion IRc2 and present maps of the HC 3 N lines with energies from 34 to 154 K and of the HC 3 N vibrational modes ν 6 and ν 7 with energies between 354 and 872 K. In addition, a comparison of our results for HC 3 N with those in other clouds has allowed us to derive correlations between the column density, the FWHM, the mass, and the luminosity of the clouds. Conclusions. The high column densities of HC 3 N obtained in the hot core, in particular of the ground vibrational state and the vibrational mode ν 7 , make this molecule an excellent tracer of hot and dense gas. In addition, the wide frequency range covered reveals the need to consider a temperature and density gradient in the hot core to obtain better line fits. The high D/H ratio (similar to that obtained in cold clouds) that we derive suggests a deuterium enrichment. Our chemical models indicate that the possible deuterated HC 3 N in Orion KL is formed during the gas-phase. This fact provides new hints concerning the processes leading to deuteration.

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“…This is consistent with the measured high proper motions of that object (e.g., Plambeck et al 1995). Whether the BN object is expelled from the Trapezium system or during a disintegration of a bound system once containing source I, source n and the BN object itself is still a matter of debate (e.g., Tan 2004;Gómez et al 2005;Zapata et al 2009). …”

Section: Introductionmentioning

confidence: 99%

Disk and outflow signatures in Orion-KL: the power of high-resolution thermal infrared spectroscopy

Beuther¹,

Linz²,

Bik³

et al. 2010

A&A

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Context. The Orion-KL region contains the closest examples of high-mass accretion disk candidates. Studying their properties is an essential step in studying high-mass star formation. Aims. Resolving the molecular line emission at high spatial and spectral resolution in the immediate environment of the exciting sources to infer the physical properties of the associated gas. Methods. We used the CRIRES high-resolution spectrograph mounted on the VLT to study the ro-vibrational 12 CO, 13 CO, the Pfund β, and H 2 emission between 4.59 and 4.72 μm wavelengths toward the BN object, the disk candidate source n, and a proposed dust density enhancement IRC3. Results. We detected CO absorption and emission features toward all three targets. Toward the BN object, the data partly confirm the results obtained more than 25 years ago; however, we also identify several new features. While the blue-shifted absorption is likely caused by outflowing gas, toward the BN object we detect CO in emission extending in diameter to ∼3300 AU with a velocity structure close to the v lsr . Although at the observational spectral resolution limit, the 13 CO line width of that feature increases with energy levels, consistent with a disk origin. If one also attributes the extended CO emission to a disk origin, its extent is consistent with other massive disk candidates in the literature. For source n, we also find the blueshifted CO absorption likely from an outflow. However, it also exhibits a narrower range of redshifted CO absorption and adjacent weak CO emission, consistent with infalling motions. We do not spatially resolve the emission for source n. For both sources we conduct a Boltzmann analysis of the 13 CO absorption features and find temperatures between 100 and 160 K, and H 2 column densities of a few times 10 23 cm −2 . The observational signatures from IRC3 are very different with only weak absorption against a much weaker continuum source. However, the CO emission is extended and shows wedge-like position velocity signatures consistent with jet-entrainment of molecular gas, potentially associated with the Orion-KL outflow system. We also present and discuss the Pfund β and H 2 emission in the region. Conclusions. This analysis toward the closest high-mass disk candidates outlines the power of high spectral and spatial resolution mid-infrared spectroscopy for studying the gas properties close to young massive stars. We will extend qualitatively similar studies to larger samples of high-mass young stellar objects to constrain the physical properties of the dense innermost gas structures in more detail and in a statistical sense.

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Explosive Disintegration of a Massive Young Stellar System in Orion

Cited by 120 publications

References 24 publications

HCOOCH₃as a probe of temperature and structure in Orion-KL

HCOOCH₃as a probe of temperature and structure in Orion-KL

Combined IRAM andHerschel/HIFI study of cyano(di)acetylene in Orion KL: tentative detection of DC₃N

Disk and outflow signatures in Orion-KL: the power of high-resolution thermal infrared spectroscopy

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Explosive Disintegration of a Massive Young Stellar System in Orion

Cited by 120 publications

References 24 publications

HCOOCH3as a probe of temperature and structure in Orion-KL

HCOOCH3as a probe of temperature and structure in Orion-KL

Combined IRAM andHerschel/HIFI study of cyano(di)acetylene in Orion KL: tentative detection of DC3N

Disk and outflow signatures in Orion-KL: the power of high-resolution thermal infrared spectroscopy

Contact Info

Product

Resources

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HCOOCH₃as a probe of temperature and structure in Orion-KL

HCOOCH₃as a probe of temperature and structure in Orion-KL

Combined IRAM andHerschel/HIFI study of cyano(di)acetylene in Orion KL: tentative detection of DC₃N