The JCMT Legacy Survey of the Gould Belt : mapping 13CO and C18O in Orion A

J. V. Buckle; C. J. Davis; J. Di Francesco; S. F. Graves; D. Nutter; J. S. Richer; J. F. Roberts; D. Ward-Thompson; G. J. White; C. Brunt; H. M. Butner; B. Cavanagh; A. Chrysostomou; E. I. Curtis; A. Duarte-Cabral; M. Extaluze; M. Fich; P. Friberg; R. Friesen; G. A. Fuller; J. S. Greaves; J. Hatchell; M. R. Hogerheijde; D. Johnstone; B. Matthews; H. Matthews; J. M. C. Rawlings; S. Sadavoy; R. J. Simpson; N. F. H. Tothill; Y. G. Tsamis; S. Viti; J. G. A. Wouterloot; J. Yates

doi:10.1111/j.1365-2966.2012.20628.x

The JCMT Legacy Survey of the Gould Belt : mapping 13CO and C18O in Orion A

J. V. Buckle, C. J. Davis, J. Di Francesco, S. F. Graves, D. Nutter, J. S. Richer, J. F. Roberts, D. Ward-Thompson, G. J. White, C. Brunt, H. M. Butner, B. Cavanagh, A. Chrysostomou, E. I. Curtis, A. Duarte-Cabral, M. Extaluze, M. Fich, P. Friberg, R. Friesen, G. A. FullerJ. S. Greaves, J. Hatchell, M. R. Hogerheijde, D. Johnstone, B. Matthews, H. Matthews, J. M. C. Rawlings, S. Sadavoy, R. J. Simpson, N. F. H. Tothill, Y. G. Tsamis, S. Viti, J. G. A. Wouterloot, J. Yates

Research output: Contribution to journal › Article › peer-review

44 Citations (Scopus)

Abstract

The Gould Belt Legacy Survey will map star-forming regions within 500"ƒpc, using Heterodyne Array Receiver Programme (HARP), Submillimetre Common-User Bolometer Array 2 (SCUBA-2) and Polarimeter 2 (POL-2) on the James Clerk Maxwell Telescope (JCMT). This paper describes HARP observations of the J= 3 â†’ 2 transitions of 13CO and C18O towards Orion A. The 15"ƒarcsec resolution observations cover 5"ƒpc of the Orion filament, including OMC 1 (including BN-KL and Orion bar), OMC 2/3 and OMC 4, and allow a comparative study of the molecular gas properties throughout the star-forming cloud. The filament shows a velocity gradient of âˆ¼1"ƒkm"ƒsâˆ’1"ƒpcâˆ’1 between OMC 1, 2 and 3, and high-velocity emission is detected in both isotopologues. The Orion Nebula and Bar have the largest masses and linewidths, and dominate the mass and energetics of the high-velocity material. Compact, spatially resolved emission from CH3CN, 13CH3OH, SO, HCOOCH3, CH3CHO and CH3OCHO is detected towards the Orion Hot Core. The cloud is warm, with a median excitation temperature of âˆ¼24"ƒK; the Orion Bar has the highest excitation temperature gas, at >80"ƒK. The C18O excitation temperature correlates well with the dust temperature (to within 40 per cent). The C18O emission is optically thin, and the 13CO emission is marginally optically thick; despite its high mass, OMC 1 shows the lowest opacities. A virial analysis indicates that Orion A is too massive for thermal or turbulent support, but is consistent with a model of a filamentary cloud that is threaded by helical magnetic fields. The variation of physical conditions across the cloud is reflected in the physical characteristics of the dust cores. We find similar core properties between starless and protostellar cores, but variations in core properties with position in the filament. The OMC 1 cores have the highest velocity dispersions and masses, followed by OMC 2/3 and OMC 4. The differing fragmentation of these cores may explain why OMC 1 has formed clusters of high-mass stars, whereas OMC 4 produces fewer, predominantly low-mass stars.

Original language	English
Pages (from-to)	521-541
Number of pages	21
Journal	Monthly Notices of the Royal Astronomical Society
Volume	422
DOIs	https://doi.org/10.1111/j.1365-2966.2012.20628.x
Publication status	Published - 2012

Keywords

Gould Belt Legacy Survey
Orion Nebula
data reduction
formation
stars

Access to Document

10.1111/j.1365-2966.2012.20628.x

Cite this

Buckle, J. V., Davis, C. J., Di Francesco, J., Graves, S. F., Nutter, D., Richer, J. S., Roberts, J. F., Ward-Thompson, D., White, G. J., Brunt, C., Butner, H. M., Cavanagh, B., Chrysostomou, A., Curtis, E. I., Duarte-Cabral, A., Extaluze, M., Fich, M., Friberg, P., Friesen, R., ... Yates, J. (2012). The JCMT Legacy Survey of the Gould Belt : mapping 13CO and C18O in Orion A. Monthly Notices of the Royal Astronomical Society, 422, 521-541. https://doi.org/10.1111/j.1365-2966.2012.20628.x

@article{4b56250f133f44d99a6bc0fb0ebbca54,

title = "The JCMT Legacy Survey of the Gould Belt : mapping 13CO and C18O in Orion A",

abstract = "The Gould Belt Legacy Survey will map star-forming regions within 500{"}ƒpc, using Heterodyne Array Receiver Programme (HARP), Submillimetre Common-User Bolometer Array 2 (SCUBA-2) and Polarimeter 2 (POL-2) on the James Clerk Maxwell Telescope (JCMT). This paper describes HARP observations of the J= 3 {\^a}†{\textquoteright} 2 transitions of 13CO and C18O towards Orion A. The 15{"}ƒarcsec resolution observations cover 5{"}ƒpc of the Orion filament, including OMC 1 (including BN-KL and Orion bar), OMC 2/3 and OMC 4, and allow a comparative study of the molecular gas properties throughout the star-forming cloud. The filament shows a velocity gradient of {\^a}ˆ¼1{"}ƒkm{"}ƒs{\^a}ˆ{\textquoteright}1{"}ƒpc{\^a}ˆ{\textquoteright}1 between OMC 1, 2 and 3, and high-velocity emission is detected in both isotopologues. The Orion Nebula and Bar have the largest masses and linewidths, and dominate the mass and energetics of the high-velocity material. Compact, spatially resolved emission from CH3CN, 13CH3OH, SO, HCOOCH3, CH3CHO and CH3OCHO is detected towards the Orion Hot Core. The cloud is warm, with a median excitation temperature of {\^a}ˆ¼24{"}ƒK; the Orion Bar has the highest excitation temperature gas, at >80{"}ƒK. The C18O excitation temperature correlates well with the dust temperature (to within 40 per cent). The C18O emission is optically thin, and the 13CO emission is marginally optically thick; despite its high mass, OMC 1 shows the lowest opacities. A virial analysis indicates that Orion A is too massive for thermal or turbulent support, but is consistent with a model of a filamentary cloud that is threaded by helical magnetic fields. The variation of physical conditions across the cloud is reflected in the physical characteristics of the dust cores. We find similar core properties between starless and protostellar cores, but variations in core properties with position in the filament. The OMC 1 cores have the highest velocity dispersions and masses, followed by OMC 2/3 and OMC 4. The differing fragmentation of these cores may explain why OMC 1 has formed clusters of high-mass stars, whereas OMC 4 produces fewer, predominantly low-mass stars.",

keywords = "Gould Belt Legacy Survey, Orion Nebula, data reduction, formation, stars",

author = "Buckle, {J. V.} and Davis, {C. J.} and {Di Francesco}, J. and Graves, {S. F.} and D. Nutter and Richer, {J. S.} and Roberts, {J. F.} and D. Ward-Thompson and White, {G. J.} and C. Brunt and Butner, {H. M.} and B. Cavanagh and A. Chrysostomou and Curtis, {E. I.} and A. Duarte-Cabral and M. Extaluze and M. Fich and P. Friberg and R. Friesen and Fuller, {G. A.} and Greaves, {J. S.} and J. Hatchell and Hogerheijde, {M. R.} and D. Johnstone and B. Matthews and H. Matthews and Rawlings, {J. M. C.} and S. Sadavoy and Simpson, {R. J.} and Tothill, {N. F. H.} and Tsamis, {Y. G.} and S. Viti and Wouterloot, {J. G. A.} and J. Yates",

year = "2012",

doi = "10.1111/j.1365-2966.2012.20628.x",

language = "English",

volume = "422",

pages = "521--541",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

}

Buckle, JV, Davis, CJ, Di Francesco, J, Graves, SF, Nutter, D, Richer, JS, Roberts, JF, Ward-Thompson, D, White, GJ, Brunt, C, Butner, HM, Cavanagh, B, Chrysostomou, A, Curtis, EI, Duarte-Cabral, A, Extaluze, M, Fich, M, Friberg, P, Friesen, R, Fuller, GA, Greaves, JS, Hatchell, J, Hogerheijde, MR, Johnstone, D, Matthews, B, Matthews, H, Rawlings, JMC, Sadavoy, S, Simpson, RJ, Tothill, NFH, Tsamis, YG, Viti, S, Wouterloot, JGA & Yates, J 2012, 'The JCMT Legacy Survey of the Gould Belt : mapping 13CO and C18O in Orion A', Monthly Notices of the Royal Astronomical Society, vol. 422, pp. 521-541. https://doi.org/10.1111/j.1365-2966.2012.20628.x

TY - JOUR

T1 - The JCMT Legacy Survey of the Gould Belt : mapping 13CO and C18O in Orion A

AU - Buckle, J. V.

AU - Davis, C. J.

AU - Di Francesco, J.

AU - Graves, S. F.

AU - Nutter, D.

AU - Richer, J. S.

AU - Roberts, J. F.

AU - Ward-Thompson, D.

AU - White, G. J.

AU - Brunt, C.

AU - Butner, H. M.

AU - Cavanagh, B.

AU - Chrysostomou, A.

AU - Curtis, E. I.

AU - Duarte-Cabral, A.

AU - Extaluze, M.

AU - Fich, M.

AU - Friberg, P.

AU - Friesen, R.

AU - Fuller, G. A.

AU - Greaves, J. S.

AU - Hatchell, J.

AU - Hogerheijde, M. R.

AU - Johnstone, D.

AU - Matthews, B.

AU - Matthews, H.

AU - Rawlings, J. M. C.

AU - Sadavoy, S.

AU - Simpson, R. J.

AU - Tothill, N. F. H.

AU - Tsamis, Y. G.

AU - Viti, S.

AU - Wouterloot, J. G. A.

AU - Yates, J.

PY - 2012

Y1 - 2012

N2 - The Gould Belt Legacy Survey will map star-forming regions within 500"ƒpc, using Heterodyne Array Receiver Programme (HARP), Submillimetre Common-User Bolometer Array 2 (SCUBA-2) and Polarimeter 2 (POL-2) on the James Clerk Maxwell Telescope (JCMT). This paper describes HARP observations of the J= 3 â†’ 2 transitions of 13CO and C18O towards Orion A. The 15"ƒarcsec resolution observations cover 5"ƒpc of the Orion filament, including OMC 1 (including BN-KL and Orion bar), OMC 2/3 and OMC 4, and allow a comparative study of the molecular gas properties throughout the star-forming cloud. The filament shows a velocity gradient of âˆ¼1"ƒkm"ƒsâˆ’1"ƒpcâˆ’1 between OMC 1, 2 and 3, and high-velocity emission is detected in both isotopologues. The Orion Nebula and Bar have the largest masses and linewidths, and dominate the mass and energetics of the high-velocity material. Compact, spatially resolved emission from CH3CN, 13CH3OH, SO, HCOOCH3, CH3CHO and CH3OCHO is detected towards the Orion Hot Core. The cloud is warm, with a median excitation temperature of âˆ¼24"ƒK; the Orion Bar has the highest excitation temperature gas, at >80"ƒK. The C18O excitation temperature correlates well with the dust temperature (to within 40 per cent). The C18O emission is optically thin, and the 13CO emission is marginally optically thick; despite its high mass, OMC 1 shows the lowest opacities. A virial analysis indicates that Orion A is too massive for thermal or turbulent support, but is consistent with a model of a filamentary cloud that is threaded by helical magnetic fields. The variation of physical conditions across the cloud is reflected in the physical characteristics of the dust cores. We find similar core properties between starless and protostellar cores, but variations in core properties with position in the filament. The OMC 1 cores have the highest velocity dispersions and masses, followed by OMC 2/3 and OMC 4. The differing fragmentation of these cores may explain why OMC 1 has formed clusters of high-mass stars, whereas OMC 4 produces fewer, predominantly low-mass stars.

AB - The Gould Belt Legacy Survey will map star-forming regions within 500"ƒpc, using Heterodyne Array Receiver Programme (HARP), Submillimetre Common-User Bolometer Array 2 (SCUBA-2) and Polarimeter 2 (POL-2) on the James Clerk Maxwell Telescope (JCMT). This paper describes HARP observations of the J= 3 â†’ 2 transitions of 13CO and C18O towards Orion A. The 15"ƒarcsec resolution observations cover 5"ƒpc of the Orion filament, including OMC 1 (including BN-KL and Orion bar), OMC 2/3 and OMC 4, and allow a comparative study of the molecular gas properties throughout the star-forming cloud. The filament shows a velocity gradient of âˆ¼1"ƒkm"ƒsâˆ’1"ƒpcâˆ’1 between OMC 1, 2 and 3, and high-velocity emission is detected in both isotopologues. The Orion Nebula and Bar have the largest masses and linewidths, and dominate the mass and energetics of the high-velocity material. Compact, spatially resolved emission from CH3CN, 13CH3OH, SO, HCOOCH3, CH3CHO and CH3OCHO is detected towards the Orion Hot Core. The cloud is warm, with a median excitation temperature of âˆ¼24"ƒK; the Orion Bar has the highest excitation temperature gas, at >80"ƒK. The C18O excitation temperature correlates well with the dust temperature (to within 40 per cent). The C18O emission is optically thin, and the 13CO emission is marginally optically thick; despite its high mass, OMC 1 shows the lowest opacities. A virial analysis indicates that Orion A is too massive for thermal or turbulent support, but is consistent with a model of a filamentary cloud that is threaded by helical magnetic fields. The variation of physical conditions across the cloud is reflected in the physical characteristics of the dust cores. We find similar core properties between starless and protostellar cores, but variations in core properties with position in the filament. The OMC 1 cores have the highest velocity dispersions and masses, followed by OMC 2/3 and OMC 4. The differing fragmentation of these cores may explain why OMC 1 has formed clusters of high-mass stars, whereas OMC 4 produces fewer, predominantly low-mass stars.

KW - Gould Belt Legacy Survey

KW - Orion Nebula

KW - data reduction

KW - formation

KW - stars

UR - http://handle.uws.edu.au:8081/1959.7/519514

U2 - 10.1111/j.1365-2966.2012.20628.x

DO - 10.1111/j.1365-2966.2012.20628.x

M3 - Article

SN - 0035-8711

VL - 422

SP - 521

EP - 541

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

ER -

The JCMT Legacy Survey of the Gould Belt : mapping 13CO and C18O in Orion A

Abstract

Keywords

Access to Document

Other files and links

Fingerprint

Cite this