Silicon Monoxide Observations Reveal a Cluster of Hidden Compact Outflows in the OMC 1 South Region

Zapata, Luis A.; Ho, P. T. P.; Rodrı́guez, Luis F.; O’Dell, C. R.; Zhang, Qizhou; Muench, August

doi:10.1086/508319

Cited by 41 publications

(69 citation statements)

References 45 publications

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“…75.9 ± 3.3 10.7 ± 0.3 2.7 ± 0.3 55.7 ± 2.5 10.6 ± 0.3 2.3 ± 0.3 12 CO J = 7−6 179.9 ± 2.6 10.5 ± 1.1 4.0 ± 1.1 156.2 ± 3.1 10.5 ± 1.1 4.0 ± 1.1 12 CO J = 6−5 180.9 ± 0.9 10.4 ± 1. Orion BN/KL are clearly seen in these images (see Zapata et al 2006Zapata et al , 2009), e.g., V LSR = 0−6 km s −1 for the BN/KL region and V LSR = 12−14 km s −1 for the Orion South region. Besides, no clear north-south velocity gradients across the OMC-1 core region are observed.…”

Section: Molecule/linementioning

confidence: 88%

The APEX-CHAMP⁺view of the Orion Molecular Cloud 1 core

Peng

Wyrowski

Zapata

et al. 2012

A&A

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Aims.A high density portion of the Orion Molecular Cloud 1 (OMC-1) contains the prominent, warm Kleinmann-Low (KL) nebula plus a farther region in which intermediate to high mass stars are forming. Its outside is affected by ultraviolet radiation from the neighboring Orion Nebula Cluster and forms the archetypical photon-dominated region (PDR) with the prominent bar feature. Its nearness makes the OMC-1 core region a touchstone for research on the dense molecular interstellar medium and PDRs. Methods. Using the Atacama Pathfinder Experiment telescope (APEX), we have imaged the line emission from the multiple transitions of several carbon monoxide (CO) isotopologues over the OMC-1 core region. Our observations employed the 2 × 7 pixel submillimeter CHAMP + array to produce maps (∼300 × 350 ) of 12 CO, 13 CO, and C 18 O from mid-J transitions (J = 6−5 to 8−7). We also obtained the 13 CO and C 18 O J = 3−2 images toward this region. Results. The 12 CO line emission shows a well-defined structure which is shaped and excited by a variety of phenomena, including the energetic photons from hot, massive stars in the nearby Orion Nebula's central Trapezium cluster, active high-and intermediate-mass star formation, and a past energetic event that excites the KL nebula. Radiative transfer modeling of the various isotopologic CO lines implies typical H 2 densities in the OMC-1 core region of ∼10 4 −10 6 cm −3 and generally elevated temperatures (∼50−250 K). We estimate a warm gas mass in the OMC-1 core region of 86−285 M .

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Section: Molecule/linementioning

confidence: 88%

The APEX-CHAMP⁺view of the Orion Molecular Cloud 1 core

Peng

Wyrowski

Zapata

et al. 2012

A&A

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“…It has the distinction of being nearly "edge-on," such that the atomic and molecular emission from different stratified layers can be studied (e.g., van der Wiel et al 2009;Nagy et al 2013). OrionS is an embedded starforming region that contains multiple outflows (Schmid-Burgk et al 1990;Ziurys et al 1990;Zapata et al 2005Zapata et al , 2006, shocked gas (Henney et al 2007;Rivilla et al 2013), and a PDR illuminated by the Trapezium stars (Peng et al 2012). In Section 4.2 we show that the CO emission profiles in OrionS can be decomposed into these three components.…”

Section: Introductionmentioning

confidence: 99%

CO Spectral Line Energy Distributions in Galactic Sources: Empirical Interpretation of Extragalactic Observations^∗

Indriolo

Bergin

Goicoechea

et al. 2017

ApJ

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The relative populations in rotational transitions of CO can be useful for inferring gas conditions and excitation mechanisms at work in the interstellar medium. We present CO emission lines from rotational transitions observed with Herschel/HIFI in the star-forming cores OrionS, OrionKL, SgrB2(M), and W49N. Integrated line fluxes from these observations are combined with those from Herschel/PACS observations of the same sources to construct CO spectral line energy distributions (SLEDs) from 5J u 48. These CO SLEDs are compared to those reported in other galaxies, with the intention of empirically determining which mechanisms dominate excitation in such systems. We find that CO SLEDs in Galactic star-forming cores cannot be used to reproduce those observed in other galaxies, although the discrepancies arise primarily as a result of beam filling factors. The much larger regions sampled by the Herschel beams at distances of several megaparsecs contain significant amounts of cooler gas, which dominate the extragalactic CO SLEDs, in contrast to observations of Galactic starforming regions, which are focused specifically on cores containing primarily hot molecular gas.

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“…In contrast, the densities of the interclump medium fall between a few 10 4 cm −3 (Young Owl et al 2000) and 2 × 10 5 cm −3 (Simon et al 1997). Orion S is an active star-forming region, located 1 southwest of the Trapezium, as indicated by the number of outflows and Herbig-Haro flows (Zapata et al 2006). The mass of Orion S is ∼100 M , and the size of this region is similar to that of Orion BN/KL, but its bolometric luminosity of 10 4 L is an order of magnitude lower (Mezger et al 1990), which may indicate that Orion S is less evolved (McMullin et al 1993).…”

Section: Introductionmentioning

confidence: 99%

A non-equilibrium ortho-to-para ratio of water in the Orion PDR

Choi

Tak

Bergin

et al. 2014

A&A

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Context. The ortho-to-para ratio (OPR) of H 2 O is thought to be sensitive to the temperature of water formation. The OPR of H 2 O is thus useful for studying the formation mechanism of water. Aims. We investigate the OPR of water in the Orion PDR (photon-dominated region), at the Orion Bar and Orion S positions, using data from Herschel/HIFI. Methods. We detect the ground-state lines of ortho-and para-H 18 2 O in the Orion Bar and Orion S and estimate the column densities using local thermodynamical equilibrium (LTE) and non-LTE methods. Results. Based on our calculations, the OPR in the Orion Bar is 0.1−0.5, which is unexpectedly low given the gas temperature of ∼85 K, and also lower than the values measured for other interstellar clouds and protoplanetary disks. Toward Orion S, our OPR estimate is below 2. Conclusions. This low OPR at 2 positions in the Orion PDR is inconsistent with gas phase formation and with thermal evaporation from dust grains, but it may be explained by photodesorption.

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Silicon Monoxide Observations Reveal a Cluster of Hidden Compact Outflows in the OMC 1 South Region

Cited by 41 publications

References 45 publications

The APEX-CHAMP⁺view of the Orion Molecular Cloud 1 core

The APEX-CHAMP⁺view of the Orion Molecular Cloud 1 core

CO Spectral Line Energy Distributions in Galactic Sources: Empirical Interpretation of Extragalactic Observations^∗

A non-equilibrium ortho-to-para ratio of water in the Orion PDR

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Silicon Monoxide Observations Reveal a Cluster of Hidden Compact Outflows in the OMC 1 South Region

Cited by 41 publications

References 45 publications

The APEX-CHAMP+view of the Orion Molecular Cloud 1 core

The APEX-CHAMP+view of the Orion Molecular Cloud 1 core

CO Spectral Line Energy Distributions in Galactic Sources: Empirical Interpretation of Extragalactic Observations∗

A non-equilibrium ortho-to-para ratio of water in the Orion PDR

Contact Info

Product

Resources

About

The APEX-CHAMP⁺view of the Orion Molecular Cloud 1 core

The APEX-CHAMP⁺view of the Orion Molecular Cloud 1 core

CO Spectral Line Energy Distributions in Galactic Sources: Empirical Interpretation of Extragalactic Observations^∗