Publication

Substructures in the Keplerian disc around the O-type (proto-)star G17.64+0.16

Maud, L. T., Cesaroni, R., Kumar, M. S. N., Rivilla, V. M., Ginsburg, A., Klaassen, P. D., Harsono, D., Sánchez-Monge, Á., Ahmadi, A., Allen, V., Beltrán, M. T., Beuther, H., Galván-Madrid, R., Goddi, C., Hoare, M. G., Hogerheijde, M. R., Johnston, K. G., Kuiper, R., Moscadelli, L., Peters, T., Testi, L., van der Tak, F. F. S. & de Wit, W. J., 1-Jul-2019, In : Astronomy and astrophysics. 627, July 2019, 7 p., L6.

Research output: Contribution to journalArticleAcademicpeer-review

APA

Maud, L. T., Cesaroni, R., Kumar, M. S. N., Rivilla, V. M., Ginsburg, A., Klaassen, P. D., ... de Wit, W. J. (2019). Substructures in the Keplerian disc around the O-type (proto-)star G17.64+0.16. Astronomy and astrophysics, 627(July 2019), [L6]. https://doi.org/10.1051/0004-6361/201935633

Author

Maud, L. T. ; Cesaroni, R. ; Kumar, M. S. N. ; Rivilla, V. M. ; Ginsburg, A. ; Klaassen, P. D. ; Harsono, D. ; Sánchez-Monge, Á. ; Ahmadi, A. ; Allen, V. ; Beltrán, M. T. ; Beuther, H. ; Galván-Madrid, R. ; Goddi, C. ; Hoare, M. G. ; Hogerheijde, M. R. ; Johnston, K. G. ; Kuiper, R. ; Moscadelli, L. ; Peters, T. ; Testi, L. ; van der Tak, F. F. S. ; de Wit, W. J. / Substructures in the Keplerian disc around the O-type (proto-)star G17.64+0.16. In: Astronomy and astrophysics. 2019 ; Vol. 627, No. July 2019.

Harvard

Maud, LT, Cesaroni, R, Kumar, MSN, Rivilla, VM, Ginsburg, A, Klaassen, PD, Harsono, D, Sánchez-Monge, Á, Ahmadi, A, Allen, V, Beltrán, MT, Beuther, H, Galván-Madrid, R, Goddi, C, Hoare, MG, Hogerheijde, MR, Johnston, KG, Kuiper, R, Moscadelli, L, Peters, T, Testi, L, van der Tak, FFS & de Wit, WJ 2019, 'Substructures in the Keplerian disc around the O-type (proto-)star G17.64+0.16', Astronomy and astrophysics, vol. 627, no. July 2019, L6. https://doi.org/10.1051/0004-6361/201935633

Standard

Substructures in the Keplerian disc around the O-type (proto-)star G17.64+0.16. / Maud, L. T.; Cesaroni, R.; Kumar, M. S. N.; Rivilla, V. M.; Ginsburg, A.; Klaassen, P. D.; Harsono, D.; Sánchez-Monge, Á.; Ahmadi, A.; Allen, V.; Beltrán, M. T.; Beuther, H.; Galván-Madrid, R.; Goddi, C.; Hoare, M. G.; Hogerheijde, M. R.; Johnston, K. G.; Kuiper, R.; Moscadelli, L.; Peters, T.; Testi, L.; van der Tak, F. F. S.; de Wit, W. J.

In: Astronomy and astrophysics, Vol. 627, No. July 2019, L6, 01.07.2019.

Research output: Contribution to journalArticleAcademicpeer-review

Vancouver

Maud LT, Cesaroni R, Kumar MSN, Rivilla VM, Ginsburg A, Klaassen PD et al. Substructures in the Keplerian disc around the O-type (proto-)star G17.64+0.16. Astronomy and astrophysics. 2019 Jul 1;627(July 2019). L6. https://doi.org/10.1051/0004-6361/201935633


BibTeX

@article{4593cb1bb5354513ad2441d66e290fe0,
title = "Substructures in the Keplerian disc around the O-type (proto-)star G17.64+0.16",
abstract = "We present the highest angular resolution (̃20 × 15 mas-44 × 33 au) Atacama Large Millimeter/sub-millimeter Array (ALMA) observations that are currently possible of the proto-O-star G17.64+0.16 in Band 6. The Cycle 5 observations with baselines out to 16 km probe scales < 50 au and reveal the rotating disc around G17.64+0.16, a massive forming O-type star. The disc has a ring-like enhancement in the dust emission that is especially visible as arc structures to the north and south. The Keplerian kinematics are most prominently seen in the vibrationally excited water line, H2O 55, 0-64, 3 ν2 = 1 (Eu = 3461.9 K). The mass of the central source found by modelling the Keplerian rotation is consistent with 45 ± 10 M☉. The H30α (231.9 GHz) radio-recombination line and the SiO (5-4) molecular line were detected at up to the ̃10σ level. The estimated disc mass is 0.6 - 2.6 M☉ under the optically thin assumption. Analysis of the Toomre Q parameter in the optically thin regime indicates that the disc stability is highly dependent on temperature. The disc currently appears stable for temperatures > 150 K; this does not preclude that the substructures formed earlier through disc fragmentation. Data cubes of the source are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/627/L6.",
keywords = "stars: formation, stars: protostars, stars: massive, stars: winds, outflows, stars: pre-main sequence, submillimeter: stars, Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies",
author = "Maud, {L. T.} and R. Cesaroni and Kumar, {M. S. N.} and Rivilla, {V. M.} and A. Ginsburg and Klaassen, {P. D.} and D. Harsono and {\'A}. S{\'a}nchez-Monge and A. Ahmadi and V. Allen and Beltr{\'a}n, {M. T.} and H. Beuther and R. Galv{\'a}n-Madrid and C. Goddi and Hoare, {M. G.} and Hogerheijde, {M. R.} and Johnston, {K. G.} and R. Kuiper and L. Moscadelli and T. Peters and L. Testi and {van der Tak}, {F. F. S.} and {de Wit}, {W. J.}",
year = "2019",
month = "7",
day = "1",
doi = "10.1051/0004-6361/201935633",
language = "English",
volume = "627",
journal = "Astronomy & astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",
number = "July 2019",

}

RIS

TY - JOUR

T1 - Substructures in the Keplerian disc around the O-type (proto-)star G17.64+0.16

AU - Maud, L. T.

AU - Cesaroni, R.

AU - Kumar, M. S. N.

AU - Rivilla, V. M.

AU - Ginsburg, A.

AU - Klaassen, P. D.

AU - Harsono, D.

AU - Sánchez-Monge, Á.

AU - Ahmadi, A.

AU - Allen, V.

AU - Beltrán, M. T.

AU - Beuther, H.

AU - Galván-Madrid, R.

AU - Goddi, C.

AU - Hoare, M. G.

AU - Hogerheijde, M. R.

AU - Johnston, K. G.

AU - Kuiper, R.

AU - Moscadelli, L.

AU - Peters, T.

AU - Testi, L.

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

AU - de Wit, W. J.

PY - 2019/7/1

Y1 - 2019/7/1

N2 - We present the highest angular resolution (̃20 × 15 mas-44 × 33 au) Atacama Large Millimeter/sub-millimeter Array (ALMA) observations that are currently possible of the proto-O-star G17.64+0.16 in Band 6. The Cycle 5 observations with baselines out to 16 km probe scales < 50 au and reveal the rotating disc around G17.64+0.16, a massive forming O-type star. The disc has a ring-like enhancement in the dust emission that is especially visible as arc structures to the north and south. The Keplerian kinematics are most prominently seen in the vibrationally excited water line, H2O 55, 0-64, 3 ν2 = 1 (Eu = 3461.9 K). The mass of the central source found by modelling the Keplerian rotation is consistent with 45 ± 10 M☉. The H30α (231.9 GHz) radio-recombination line and the SiO (5-4) molecular line were detected at up to the ̃10σ level. The estimated disc mass is 0.6 - 2.6 M☉ under the optically thin assumption. Analysis of the Toomre Q parameter in the optically thin regime indicates that the disc stability is highly dependent on temperature. The disc currently appears stable for temperatures > 150 K; this does not preclude that the substructures formed earlier through disc fragmentation. Data cubes of the source are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/627/L6.

AB - We present the highest angular resolution (̃20 × 15 mas-44 × 33 au) Atacama Large Millimeter/sub-millimeter Array (ALMA) observations that are currently possible of the proto-O-star G17.64+0.16 in Band 6. The Cycle 5 observations with baselines out to 16 km probe scales < 50 au and reveal the rotating disc around G17.64+0.16, a massive forming O-type star. The disc has a ring-like enhancement in the dust emission that is especially visible as arc structures to the north and south. The Keplerian kinematics are most prominently seen in the vibrationally excited water line, H2O 55, 0-64, 3 ν2 = 1 (Eu = 3461.9 K). The mass of the central source found by modelling the Keplerian rotation is consistent with 45 ± 10 M☉. The H30α (231.9 GHz) radio-recombination line and the SiO (5-4) molecular line were detected at up to the ̃10σ level. The estimated disc mass is 0.6 - 2.6 M☉ under the optically thin assumption. Analysis of the Toomre Q parameter in the optically thin regime indicates that the disc stability is highly dependent on temperature. The disc currently appears stable for temperatures > 150 K; this does not preclude that the substructures formed earlier through disc fragmentation. Data cubes of the source are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/627/L6.

KW - stars: formation

KW - stars: protostars

KW - stars: massive

KW - stars: winds

KW - outflows

KW - stars: pre-main sequence

KW - submillimeter: stars

KW - Astrophysics - Solar and Stellar Astrophysics

KW - Astrophysics - Astrophysics of Galaxies

U2 - 10.1051/0004-6361/201935633

DO - 10.1051/0004-6361/201935633

M3 - Article

VL - 627

JO - Astronomy & astrophysics

JF - Astronomy & astrophysics

SN - 0004-6361

IS - July 2019

M1 - L6

ER -

ID: 118169380