Publication

Chasing discs around O-type (proto)stars

Maud, L. T., Cesaroni, R., Kumar, M. S. N., van der Tak, F. F. S., Allen, V., Hoare, M. G., Klaassen, P. D., Harsono, D., Hogerheijde, M. R., Sanchez-Monge, A., Schilke, P., Ahmadi, A., Beltran, M. T., Beuther, H., Csengeri, T., Etoka, S., Fuller, G., Galvan-Madrid, R., Goddi, C., Henning, T., Johnston, K. G., Kuiper, R., Lumsden, S., Moscadelli, L., Mottram, J. C., Peters, T., Rivilla, V. M., Testi, L., Vig, S., de Wit, W. J. & Zinnecker, H., 23-Nov-2018, In : Astronomy & astrophysics. 620, 20 p., 31.

Research output: Contribution to journalArticleAcademicpeer-review

APA

Maud, L. T., Cesaroni, R., Kumar, M. S. N., van der Tak, F. F. S., Allen, V., Hoare, M. G., ... Zinnecker, H. (2018). Chasing discs around O-type (proto)stars. Astronomy & astrophysics, 620, [31]. https://doi.org/10.1051/0004-6361/201833908

Author

Maud, L. T. ; Cesaroni, R. ; Kumar, M. S. N. ; van der Tak, F. F. S. ; Allen, V. ; Hoare, M. G. ; Klaassen, P. D. ; Harsono, D. ; Hogerheijde, M. R. ; Sanchez-Monge, A. ; Schilke, P. ; Ahmadi, A. ; Beltran, M. T. ; Beuther, H. ; Csengeri, T. ; Etoka, S. ; Fuller, G. ; Galvan-Madrid, R. ; Goddi, C. ; Henning, Th. ; Johnston, K. G. ; Kuiper, R. ; Lumsden, S. ; Moscadelli, L. ; Mottram, J. C. ; Peters, T. ; Rivilla, V. M. ; Testi, L. ; Vig, S. ; de Wit, W. J. ; Zinnecker, H. / Chasing discs around O-type (proto)stars. In: Astronomy & astrophysics. 2018 ; Vol. 620.

Harvard

Maud, LT, Cesaroni, R, Kumar, MSN, van der Tak, FFS, Allen, V, Hoare, MG, Klaassen, PD, Harsono, D, Hogerheijde, MR, Sanchez-Monge, A, Schilke, P, Ahmadi, A, Beltran, MT, Beuther, H, Csengeri, T, Etoka, S, Fuller, G, Galvan-Madrid, R, Goddi, C, Henning, T, Johnston, KG, Kuiper, R, Lumsden, S, Moscadelli, L, Mottram, JC, Peters, T, Rivilla, VM, Testi, L, Vig, S, de Wit, WJ & Zinnecker, H 2018, 'Chasing discs around O-type (proto)stars', Astronomy & astrophysics, vol. 620, 31. https://doi.org/10.1051/0004-6361/201833908

Standard

Chasing discs around O-type (proto)stars. / Maud, L. T.; Cesaroni, R.; Kumar, M. S. N.; van der Tak, F. F. S.; Allen, V.; Hoare, M. G.; Klaassen, P. D.; Harsono, D.; Hogerheijde, M. R.; Sanchez-Monge, A.; Schilke, P.; Ahmadi, A.; Beltran, M. T.; Beuther, H.; Csengeri, T.; Etoka, S.; Fuller, G.; Galvan-Madrid, R.; Goddi, C.; Henning, Th.; Johnston, K. G.; Kuiper, R.; Lumsden, S.; Moscadelli, L.; Mottram, J. C.; Peters, T.; Rivilla, V. M.; Testi, L.; Vig, S.; de Wit, W. J.; Zinnecker, H.

In: Astronomy & astrophysics, Vol. 620, 31, 23.11.2018.

Research output: Contribution to journalArticleAcademicpeer-review

Vancouver

Maud LT, Cesaroni R, Kumar MSN, van der Tak FFS, Allen V, Hoare MG et al. Chasing discs around O-type (proto)stars. Astronomy & astrophysics. 2018 Nov 23;620. 31. https://doi.org/10.1051/0004-6361/201833908


BibTeX

@article{2fa922f15f0640f08b75461ef7ee94cf,
title = "Chasing discs around O-type (proto)stars",
abstract = "We present high angular resolution (similar to 0.2 '') continuum and molecular emission line Atacama Large Millimeter/sub-millimeter Array (ALMA) observations of G17.64+0.16 in Band 6 (220-230 GHz) taken as part of a campaign in search of circumstellar discs around (proto)-O-stars. At a resolution of similar to 400 au the main continuum core is essentially unresolved and isolated from other strong and compact emission peaks. We detect SiO (5-4) emission that is marginally resolved and elongated in a direction perpendicular to the large-scale outflow seen in the (CO)-C-13 (2-1) line using the main ALMA array in conjunction with the Atacama Compact Array (ACA). Morphologically, the SiO appears to represent a disc-like structure. Using parametric models we show that the position-velocity profile of the SiO is consistent with the Keplerian rotation of a disc around an object between 10 and 30M(circle dot) in mass, only if there is also radial expansion from a separate structure. The radial motion component can be interpreted as a disc wind from the disc surface. Models with a central stellar object mass between 20 and 30 M-circle dot are the most consistent with the stellar luminosity (1 x 10(5) L-circle dot) and indicative of an O-type star. The H30 alpha millimetre recombination line (231.9 GHz) is also detected, but spatially unresolved, and is indicative of a very compact, hot, ionised region co-spatial with the dust continuum core. The broad line-width of the H30 alpha emission (full-width-half-maximum = 81.9 km s(-1)) is not dominated by pressure-broadening but is consistent with underlying bulk motions. These velocities match those required for shocks to release silicon from dust grains into the gas phase. CH3CN and CH3OH thermal emission also shows two arc shaped plumes that curve away from the disc plane. Their coincidence with OH maser emission suggests that they could trace the inner working surfaces of a wide-angle wind driven by G17.64 which impacts the diffuse remnant natal cloud before being redirected into the large-scale outflow direction. Accounting for all observables, we suggest that G17.64 is consistent with a O-type young stellar object in the final stages of protostellar assembly, driving a wind, but that has not yet developed into a compact HII region. The existance and detection of the disc in G17.64 is likely related to its isolated and possibly more evolved nature, traits which may underpin discs in similar sources.",
keywords = "stars: formation, stars: protostars, stars: massive, stars: winds, outflows, stars: pre-main sequence, submillimeter: stars, SUBMILLIMETER ARRAY OBSERVATIONS, INFRARED REFLECTION NEBULA, DISTANCE-LIMITED SAMPLE, MASSIVE STAR-FORMATION, LINE-DRIVEN ABLATION, IMAGING POLARIMETRY, CIRCUMSTELLAR DISCS, RADIATION PRESSURE, EARLY EVOLUTION, RADIO-EMISSION",
author = "Maud, {L. T.} and R. Cesaroni and Kumar, {M. S. N.} and {van der Tak}, {F. F. S.} and V. Allen and Hoare, {M. G.} and Klaassen, {P. D.} and D. Harsono and Hogerheijde, {M. R.} and A. Sanchez-Monge and P. Schilke and A. Ahmadi and Beltran, {M. T.} and H. Beuther and T. Csengeri and S. Etoka and G. Fuller and R. Galvan-Madrid and C. Goddi and Th. Henning and Johnston, {K. G.} and R. Kuiper and S. Lumsden and L. Moscadelli and Mottram, {J. C.} and T. Peters and Rivilla, {V. M.} and L. Testi and S. Vig and {de Wit}, {W. J.} and H. Zinnecker",
year = "2018",
month = "11",
day = "23",
doi = "10.1051/0004-6361/201833908",
language = "English",
volume = "620",
journal = "Astronomy & astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",

}

RIS

TY - JOUR

T1 - Chasing discs around O-type (proto)stars

AU - Maud, L. T.

AU - Cesaroni, R.

AU - Kumar, M. S. N.

AU - van der Tak, F. F. S.

AU - Allen, V.

AU - Hoare, M. G.

AU - Klaassen, P. D.

AU - Harsono, D.

AU - Hogerheijde, M. R.

AU - Sanchez-Monge, A.

AU - Schilke, P.

AU - Ahmadi, A.

AU - Beltran, M. T.

AU - Beuther, H.

AU - Csengeri, T.

AU - Etoka, S.

AU - Fuller, G.

AU - Galvan-Madrid, R.

AU - Goddi, C.

AU - Henning, Th.

AU - Johnston, K. G.

AU - Kuiper, R.

AU - Lumsden, S.

AU - Moscadelli, L.

AU - Mottram, J. C.

AU - Peters, T.

AU - Rivilla, V. M.

AU - Testi, L.

AU - Vig, S.

AU - de Wit, W. J.

AU - Zinnecker, H.

PY - 2018/11/23

Y1 - 2018/11/23

N2 - We present high angular resolution (similar to 0.2 '') continuum and molecular emission line Atacama Large Millimeter/sub-millimeter Array (ALMA) observations of G17.64+0.16 in Band 6 (220-230 GHz) taken as part of a campaign in search of circumstellar discs around (proto)-O-stars. At a resolution of similar to 400 au the main continuum core is essentially unresolved and isolated from other strong and compact emission peaks. We detect SiO (5-4) emission that is marginally resolved and elongated in a direction perpendicular to the large-scale outflow seen in the (CO)-C-13 (2-1) line using the main ALMA array in conjunction with the Atacama Compact Array (ACA). Morphologically, the SiO appears to represent a disc-like structure. Using parametric models we show that the position-velocity profile of the SiO is consistent with the Keplerian rotation of a disc around an object between 10 and 30M(circle dot) in mass, only if there is also radial expansion from a separate structure. The radial motion component can be interpreted as a disc wind from the disc surface. Models with a central stellar object mass between 20 and 30 M-circle dot are the most consistent with the stellar luminosity (1 x 10(5) L-circle dot) and indicative of an O-type star. The H30 alpha millimetre recombination line (231.9 GHz) is also detected, but spatially unresolved, and is indicative of a very compact, hot, ionised region co-spatial with the dust continuum core. The broad line-width of the H30 alpha emission (full-width-half-maximum = 81.9 km s(-1)) is not dominated by pressure-broadening but is consistent with underlying bulk motions. These velocities match those required for shocks to release silicon from dust grains into the gas phase. CH3CN and CH3OH thermal emission also shows two arc shaped plumes that curve away from the disc plane. Their coincidence with OH maser emission suggests that they could trace the inner working surfaces of a wide-angle wind driven by G17.64 which impacts the diffuse remnant natal cloud before being redirected into the large-scale outflow direction. Accounting for all observables, we suggest that G17.64 is consistent with a O-type young stellar object in the final stages of protostellar assembly, driving a wind, but that has not yet developed into a compact HII region. The existance and detection of the disc in G17.64 is likely related to its isolated and possibly more evolved nature, traits which may underpin discs in similar sources.

AB - We present high angular resolution (similar to 0.2 '') continuum and molecular emission line Atacama Large Millimeter/sub-millimeter Array (ALMA) observations of G17.64+0.16 in Band 6 (220-230 GHz) taken as part of a campaign in search of circumstellar discs around (proto)-O-stars. At a resolution of similar to 400 au the main continuum core is essentially unresolved and isolated from other strong and compact emission peaks. We detect SiO (5-4) emission that is marginally resolved and elongated in a direction perpendicular to the large-scale outflow seen in the (CO)-C-13 (2-1) line using the main ALMA array in conjunction with the Atacama Compact Array (ACA). Morphologically, the SiO appears to represent a disc-like structure. Using parametric models we show that the position-velocity profile of the SiO is consistent with the Keplerian rotation of a disc around an object between 10 and 30M(circle dot) in mass, only if there is also radial expansion from a separate structure. The radial motion component can be interpreted as a disc wind from the disc surface. Models with a central stellar object mass between 20 and 30 M-circle dot are the most consistent with the stellar luminosity (1 x 10(5) L-circle dot) and indicative of an O-type star. The H30 alpha millimetre recombination line (231.9 GHz) is also detected, but spatially unresolved, and is indicative of a very compact, hot, ionised region co-spatial with the dust continuum core. The broad line-width of the H30 alpha emission (full-width-half-maximum = 81.9 km s(-1)) is not dominated by pressure-broadening but is consistent with underlying bulk motions. These velocities match those required for shocks to release silicon from dust grains into the gas phase. CH3CN and CH3OH thermal emission also shows two arc shaped plumes that curve away from the disc plane. Their coincidence with OH maser emission suggests that they could trace the inner working surfaces of a wide-angle wind driven by G17.64 which impacts the diffuse remnant natal cloud before being redirected into the large-scale outflow direction. Accounting for all observables, we suggest that G17.64 is consistent with a O-type young stellar object in the final stages of protostellar assembly, driving a wind, but that has not yet developed into a compact HII region. The existance and detection of the disc in G17.64 is likely related to its isolated and possibly more evolved nature, traits which may underpin discs in similar sources.

KW - stars: formation

KW - stars: protostars

KW - stars: massive

KW - stars: winds, outflows

KW - stars: pre-main sequence

KW - submillimeter: stars

KW - SUBMILLIMETER ARRAY OBSERVATIONS

KW - INFRARED REFLECTION NEBULA

KW - DISTANCE-LIMITED SAMPLE

KW - MASSIVE STAR-FORMATION

KW - LINE-DRIVEN ABLATION

KW - IMAGING POLARIMETRY

KW - CIRCUMSTELLAR DISCS

KW - RADIATION PRESSURE

KW - EARLY EVOLUTION

KW - RADIO-EMISSION

U2 - 10.1051/0004-6361/201833908

DO - 10.1051/0004-6361/201833908

M3 - Article

VL - 620

JO - Astronomy & astrophysics

JF - Astronomy & astrophysics

SN - 0004-6361

M1 - 31

ER -

ID: 76702487