The JCMT gould belt survey: Evidence for dust grain evolution in Perseus star-forming clumps

Michael Chun Yuan Chen; J. Di Francesco; D. Johnstone; S. Sadavoy; J. Hatchell; J. C. Mottram; H. Kirk; J. Buckle; D. S. Berry; H. Broekhoven-Fiene; M. J. Currie; M. Fich; T. Jenness; D. Nutter; K. Pattle; J. E. Pineda; C. Quinn; C. Salji; S. Tisi; M. R. Hogerheijde; D. Ward-Thompson; P. Bastien; D. Bresnahan; H. Butner; A. Chrysostomou; S. Coude; C. J. Davis; E. Drabek-Maunder; A. Duarte-Cabral; J. Fiege; P. Friberg; R. Friesen; G. A. Fuller; S. Graves; J. Greaves; J. Gregson; W. Holland; G. Joncas; J. M. Kirk; L. B.G. Knee; S. Mairs; K. Marsh; B. C. Matthews; G. Moriarty-Schieven; C. Mowat; S. Pezzuto; J. Rawlings; J. Richer; D. Robertson; E. Rosolowsky; D. Rumble; N. Schneider-Bontemps; H. Thomas; N. Tothill; S. Viti; G. J. White; J. Wouterloot; J. Yates; M. Zhu

doi:10.3847/0004-637X/826/1/95

The JCMT gould belt survey: Evidence for dust grain evolution in Perseus star-forming clumps

Michael Chun Yuan Chen, J. Di Francesco, D. Johnstone, S. Sadavoy, J. Hatchell, J. C. Mottram, H. Kirk, J. Buckle, D. S. Berry, H. Broekhoven-Fiene, M. J. Currie, M. Fich, T. Jenness, D. Nutter, K. Pattle, J. E. Pineda, C. Quinn, C. Salji, S. Tisi, M. R. HogerheijdeD. Ward-Thompson, P. Bastien, D. Bresnahan, H. Butner, A. Chrysostomou, S. Coude, C. J. Davis, E. Drabek-Maunder, A. Duarte-Cabral, J. Fiege, P. Friberg, R. Friesen, G. A. Fuller, S. Graves, J. Greaves, J. Gregson, W. Holland, G. Joncas, J. M. Kirk, L. B.G. Knee, S. Mairs, K. Marsh, B. C. Matthews, G. Moriarty-Schieven, C. Mowat, S. Pezzuto, J. Rawlings, J. Richer, D. Robertson, E. Rosolowsky, D. Rumble, N. Schneider-Bontemps, H. Thomas, N. Tothill, S. Viti, G. J. White, J. Wouterloot, J. Yates, M. Zhu

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Abstract

The dust emissivity spectral index, β, is a critical parameter for deriving the mass and temperature of star-forming structures and, consequently, their gravitational stability. The β value is dependent on various dust grain properties, such as size, porosity, and surface composition, and is expected to vary as dust grains evolve. Here we present β, dust temperature, and optical depth maps of the star-forming clumps in the Perseus Molecular Cloud determined from fitting spectral energy distributions to combined Herschel and JCMT observations in the 160, 250, 350, 500, and 850 μm bands. Most of the derived β and dust temperature values fall within the ranges of 1.0-2.7 and 8-20 K, respectively. In Perseus, we find the β distribution differs significantly from clump to clump, indicative of grain growth. Furthermore, we also see significant localized β variations within individual clumps and find low-β regions correlate with local temperature peaks, hinting at the possible origins of low-β grains. Throughout Perseus, we also see indications of heating from B stars and embedded protostars, as well evidence of outflows shaping the local landscape.

Original language	English
Article number	95
Journal	Astrophysical Journal
Volume	826
Issue number	1
DOIs	https://doi.org/10.3847/0004-637X/826/1/95
Publication status	Published - 2016
Externally published	Yes

Keywords

Dust
Extinction
ISM: clouds
Stars: formation
Stars: low-mass
Stars: protostars

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10.3847/0004-637X/826/1/95

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Chen, M. C. Y., Di Francesco, J., Johnstone, D., Sadavoy, S., Hatchell, J., Mottram, J. C., Kirk, H., Buckle, J., Berry, D. S., Broekhoven-Fiene, H., Currie, M. J., Fich, M., Jenness, T., Nutter, D., Pattle, K., Pineda, J. E., Quinn, C., Salji, C., Tisi, S., ... Zhu, M. (2016). The JCMT gould belt survey: Evidence for dust grain evolution in Perseus star-forming clumps. Astrophysical Journal, 826(1), Article 95. https://doi.org/10.3847/0004-637X/826/1/95

@article{6eeca8a03602418bbd2501e6c7df6808,

title = "The JCMT gould belt survey: Evidence for dust grain evolution in Perseus star-forming clumps",

abstract = "The dust emissivity spectral index, β, is a critical parameter for deriving the mass and temperature of star-forming structures and, consequently, their gravitational stability. The β value is dependent on various dust grain properties, such as size, porosity, and surface composition, and is expected to vary as dust grains evolve. Here we present β, dust temperature, and optical depth maps of the star-forming clumps in the Perseus Molecular Cloud determined from fitting spectral energy distributions to combined Herschel and JCMT observations in the 160, 250, 350, 500, and 850 μm bands. Most of the derived β and dust temperature values fall within the ranges of 1.0-2.7 and 8-20 K, respectively. In Perseus, we find the β distribution differs significantly from clump to clump, indicative of grain growth. Furthermore, we also see significant localized β variations within individual clumps and find low-β regions correlate with local temperature peaks, hinting at the possible origins of low-β grains. Throughout Perseus, we also see indications of heating from B stars and embedded protostars, as well evidence of outflows shaping the local landscape.",

keywords = "Dust, Extinction, ISM: clouds, Stars: formation, Stars: low-mass, Stars: protostars",

author = "Chen, {Michael Chun Yuan} and {Di Francesco}, J. and D. Johnstone and S. Sadavoy and J. Hatchell and Mottram, {J. C.} and H. Kirk and J. Buckle and Berry, {D. S.} and H. Broekhoven-Fiene and Currie, {M. J.} and M. Fich and T. Jenness and D. Nutter and K. Pattle and Pineda, {J. E.} and C. Quinn and C. Salji and S. Tisi and Hogerheijde, {M. R.} and D. Ward-Thompson and P. Bastien and D. Bresnahan and H. Butner and A. Chrysostomou and S. Coude and Davis, {C. J.} and E. Drabek-Maunder and A. Duarte-Cabral and J. Fiege and P. Friberg and R. Friesen and Fuller, {G. A.} and S. Graves and J. Greaves and J. Gregson and W. Holland and G. Joncas and Kirk, {J. M.} and Knee, {L. B.G.} and S. Mairs and K. Marsh and Matthews, {B. C.} and G. Moriarty-Schieven and C. Mowat and S. Pezzuto and J. Rawlings and J. Richer and D. Robertson and E. Rosolowsky and D. Rumble and N. Schneider-Bontemps and H. Thomas and N. Tothill and S. Viti and White, {G. J.} and J. Wouterloot and J. Yates and M. Zhu",

note = "Publisher Copyright: {\textcopyright} 2016. The American Astronomical Society.",

year = "2016",

doi = "10.3847/0004-637X/826/1/95",

language = "English",

volume = "826",

journal = "Astrophysical Journal",

issn = "0004-637X",

number = "1",

}

Chen, MCY, Di Francesco, J, Johnstone, D, Sadavoy, S, Hatchell, J, Mottram, JC, Kirk, H, Buckle, J, Berry, DS, Broekhoven-Fiene, H, Currie, MJ, Fich, M, Jenness, T, Nutter, D, Pattle, K, Pineda, JE, Quinn, C, Salji, C, Tisi, S, Hogerheijde, MR, Ward-Thompson, D, Bastien, P, Bresnahan, D, Butner, H, Chrysostomou, A, Coude, S, Davis, CJ, Drabek-Maunder, E, Duarte-Cabral, A, Fiege, J, Friberg, P, Friesen, R, Fuller, GA, Graves, S, Greaves, J, Gregson, J, Holland, W, Joncas, G, Kirk, JM, Knee, LBG, Mairs, S, Marsh, K, Matthews, BC, Moriarty-Schieven, G, Mowat, C, Pezzuto, S, Rawlings, J, Richer, J, Robertson, D, Rosolowsky, E, Rumble, D, Schneider-Bontemps, N, Thomas, H, Tothill, N, Viti, S, White, GJ, Wouterloot, J, Yates, J & Zhu, M 2016, 'The JCMT gould belt survey: Evidence for dust grain evolution in Perseus star-forming clumps', Astrophysical Journal, vol. 826, no. 1, 95. https://doi.org/10.3847/0004-637X/826/1/95

TY - JOUR

T1 - The JCMT gould belt survey

T2 - Evidence for dust grain evolution in Perseus star-forming clumps

AU - Chen, Michael Chun Yuan

AU - Di Francesco, J.

AU - Johnstone, D.

AU - Sadavoy, S.

AU - Hatchell, J.

AU - Mottram, J. C.

AU - Kirk, H.

AU - Buckle, J.

AU - Berry, D. S.

AU - Broekhoven-Fiene, H.

AU - Currie, M. J.

AU - Fich, M.

AU - Jenness, T.

AU - Nutter, D.

AU - Pattle, K.

AU - Pineda, J. E.

AU - Quinn, C.

AU - Salji, C.

AU - Tisi, S.

AU - Hogerheijde, M. R.

AU - Ward-Thompson, D.

AU - Bastien, P.

AU - Bresnahan, D.

AU - Butner, H.

AU - Chrysostomou, A.

AU - Coude, S.

AU - Davis, C. J.

AU - Drabek-Maunder, E.

AU - Duarte-Cabral, A.

AU - Fiege, J.

AU - Friberg, P.

AU - Friesen, R.

AU - Fuller, G. A.

AU - Graves, S.

AU - Greaves, J.

AU - Gregson, J.

AU - Holland, W.

AU - Joncas, G.

AU - Kirk, J. M.

AU - Knee, L. B.G.

AU - Mairs, S.

AU - Marsh, K.

AU - Matthews, B. C.

AU - Moriarty-Schieven, G.

AU - Mowat, C.

AU - Pezzuto, S.

AU - Rawlings, J.

AU - Richer, J.

AU - Robertson, D.

AU - Rosolowsky, E.

AU - Rumble, D.

AU - Schneider-Bontemps, N.

AU - Thomas, H.

AU - Tothill, N.

AU - Viti, S.

AU - White, G. J.

AU - Wouterloot, J.

AU - Yates, J.

AU - Zhu, M.

PY - 2016

Y1 - 2016

N2 - The dust emissivity spectral index, β, is a critical parameter for deriving the mass and temperature of star-forming structures and, consequently, their gravitational stability. The β value is dependent on various dust grain properties, such as size, porosity, and surface composition, and is expected to vary as dust grains evolve. Here we present β, dust temperature, and optical depth maps of the star-forming clumps in the Perseus Molecular Cloud determined from fitting spectral energy distributions to combined Herschel and JCMT observations in the 160, 250, 350, 500, and 850 μm bands. Most of the derived β and dust temperature values fall within the ranges of 1.0-2.7 and 8-20 K, respectively. In Perseus, we find the β distribution differs significantly from clump to clump, indicative of grain growth. Furthermore, we also see significant localized β variations within individual clumps and find low-β regions correlate with local temperature peaks, hinting at the possible origins of low-β grains. Throughout Perseus, we also see indications of heating from B stars and embedded protostars, as well evidence of outflows shaping the local landscape.

AB - The dust emissivity spectral index, β, is a critical parameter for deriving the mass and temperature of star-forming structures and, consequently, their gravitational stability. The β value is dependent on various dust grain properties, such as size, porosity, and surface composition, and is expected to vary as dust grains evolve. Here we present β, dust temperature, and optical depth maps of the star-forming clumps in the Perseus Molecular Cloud determined from fitting spectral energy distributions to combined Herschel and JCMT observations in the 160, 250, 350, 500, and 850 μm bands. Most of the derived β and dust temperature values fall within the ranges of 1.0-2.7 and 8-20 K, respectively. In Perseus, we find the β distribution differs significantly from clump to clump, indicative of grain growth. Furthermore, we also see significant localized β variations within individual clumps and find low-β regions correlate with local temperature peaks, hinting at the possible origins of low-β grains. Throughout Perseus, we also see indications of heating from B stars and embedded protostars, as well evidence of outflows shaping the local landscape.

KW - Dust

KW - Extinction

KW - ISM: clouds

KW - Stars: formation

KW - Stars: low-mass

KW - Stars: protostars

UR - http://www.scopus.com/inward/record.url?scp=84994361281&partnerID=8YFLogxK

U2 - 10.3847/0004-637X/826/1/95

DO - 10.3847/0004-637X/826/1/95

M3 - Article

AN - SCOPUS:84994361281

SN - 0004-637X

VL - 826

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

M1 - 95

ER -

The JCMT gould belt survey: Evidence for dust grain evolution in Perseus star-forming clumps

Abstract

Keywords

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