The stellar content of OMC 2/3

Nielbock, M.; Chini, R.; Muller, S.

doi:10.1051/0004-6361:20030961

Cited by 49 publications

(106 citation statements)

References 28 publications

Supporting

Mentioning

103

Contrasting

Unclassified

Order By: Relevance

“…The Class 0 object MMS 4 along with the molecular cores are located more to the East followed by the cold and dense MMS 6 at the most eastern end of Sa 188. A similar trend was found in the FDC of OMC 1 to 3 (Nielbock et al 2003). 4.…”

Section: Discussionsupporting

confidence: 84%

See 1 more Smart Citation

Star formation in Sandqvist 187 and 188

Nielbock¹,

Chini²

2005

A&A

Self Cite

View full text Add to dashboard Cite

Abstract. We present 1.2 mm continuum data of the filamentary dark cloud Sandqvist 187/188 -also known as the Norma cloud -taken with SIMBA (SEST Imaging Bolometer Array). The data are complemented by measurements from the 2MASS, MSX and IRAS surveys. The extended 1.2 mm emission traces the optical dark cloud down to a visual extinction of A V = 3.7 mag. We derive a mean column density of N(H 2 ) = 1.4 × 10 22 cm −2 , equivalent to a visual extinction of A V = 7.6 mag and a total mass of the cloud of 340 M . We also find six compact millimetre sources, labelled MMS 1 to 6, five of which coincide with known stellar objects. MMS 6, however, only has a very weak MSX counterpart at 14.56 µm and an absorption feature at 8.28 µm consistent with a visual extinction of A V > 145 mag. Dust temperatures, luminosities and gas masses for all compact millimetre sources are given. In an effort to further constrain the uncertain distance to Sandqvist 187/188, we analyse its stellar content based on 2MASS colours and find an improved lower limit of 440 ± 50 pc.

show abstract

Section: Discussionsupporting

confidence: 84%

“…Finally, there is the most evolved, well studied region around MMS 1 and 2 including V386 Nor. A similar trend of an age sequence along a filamentary cloud was found for OMC 1-3 in Orion A (Nielbock et al 2003).…”

Section: The Protostellar Content Of Sa 187/188supporting

confidence: 78%

Star formation in Sandqvist 187 and 188

Nielbock¹,

Chini²

2005

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…Column 1 indicates the molecular cloud core, Col. 2 the right ascension, Col. 3 gives the declination, Col. 4 the core mass, Col. 5 the distance, Col. 6 the infrared luminosity, Col. 7 the line width of the transition J = 10-9 of HC 3 N, Col. 8 the HC 3 N column density, and Col. 9 the references. (a) Result obtained from data shown in Table A (2003); (13) Ridge et al (2003); (14) Wang et al (1993); (15) Lada et al (1976); (16) Bergin et al (1997); (17) Morris et al (1976); (18) Tatematsu et al (1993); (19) Peng et al (2012); (20) Chung et al (1991); (21) Gezari et al (1998); (22) Gezari (1982); (23) Sandell (2000); (24) Liu et al (2011); (25) Nielbock et al (2003); (26) Thronson (1978); (27) Bujarrabal et al (1981) found N(HC 5 N) = (5 ± 2) × 10 12 cm −2 for the ridge component, consistent with our values.…”

Section: Hc 5 Nmentioning

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

View full text Add to dashboard Cite

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.

show abstract

“…These include continuum observations at several wavelengths (e.g. Chini et al 1997;Johnstone & Bally 1999;Nielbock et al 2003) and various molecular line studies (e.g. Tatematsu 1993;Cesaroni & Wilson 1994;Takahashi et al 2008;Tatematsu et al 2008;Liu et al 2011;Li et al 2012).…”

Section: Parametermentioning

confidence: 99%

High-angular resolution observations towards OMC-2 FIR 4: Dissecting an intermediate-mass protocluster

López-Sepulcre

Taquet

Sánchez-Monge

et al. 2013

A&A

View full text Add to dashboard Cite

Context. Intermediate-mass stars are an important ingredient of our Galaxy and a key to understanding how high-and low-mass stars form in clusters. One of the closest known young intermediate-mass protoclusters is OMC-2 FIR 4, which is located at a distance of 420 pc in Orion. This region is one of the few where the complete 500-2000 GHz spectrum has been observed with the heterodyne spectrometer HIFI on board the Herschel satellite, and unbiased spectral surveys at 0.8, 1, 2, and 3 mm have been obtained with the JCMT and IRAM 30-m telescopes. Aims. We aim to disentangle the core multiplicity, to investigate the morphology of this region in order to study the formation of a low-and intermediate-mass protostar cluster, and to aid in interpretation of the single-dish line profiles already in our hands. Methods. We used the IRAM Plateau de Bure Interferometer to image OMC-2 FIR 4 in the 2-mm continuum emission, as well as in DCO + (2-1), DCN(2-1), C 34 S(3-2), and several CH 3 OH lines. In addition, we analysed observations of the NH 3 (1, 1) and (2, 2) inversion transitions that used the Very Large Array of the NRAO. The resulting maps have an angular resolution that allows us to resolve structures of 5 , which is equivalent to ∼2000 AU. Results. Our observations reveal three spatially resolved sources within OMC-2 FIR 4, of one or several solar masses each, with hints of further unresolved substructure within them. Two of these sources have elongated shapes and are associated with dust continuum emission peaks, thus likely containing at least one molecular core each. One of them also displays radio continuum emission, which may be attributed to a young B3-B4 star that dominates the overall luminosity output of the region. The third identified source displays a DCO + (2-1) emission peak and weak dust continuum emission. Its higher abundance of DCO + relative to the other two regions suggests a lower temperature, hence its possible association with either a younger low-mass protostar or a starless core. It may alternatively be part of the colder envelope of OMC-2 FIR 4. Conclusions. Our interferometric observations show the complexity of the intermediate-mass protocluster OMC-2 FIR 4, where multiple cores, chemical differentiation, and an ionised region all coexist within an area of only 10 000 AU.

show abstract

The stellar content of OMC 2/3

Cited by 49 publications

References 28 publications

Star formation in Sandqvist 187 and 188

Star formation in Sandqvist 187 and 188

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

High-angular resolution observations towards OMC-2 FIR 4: Dissecting an intermediate-mass protocluster

Contact Info

Product

Resources

About

The stellar content of OMC 2/3

Cited by 49 publications

References 28 publications

Star formation in Sandqvist 187 and 188

Star formation in Sandqvist 187 and 188

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

High-angular resolution observations towards OMC-2 FIR 4: Dissecting an intermediate-mass protocluster

Contact Info

Product

Resources

About

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