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

L. T. Maud; R. Cesaroni; M. S. N. Kumar; V. M. Rivilla; A. Ginsburg; P. D. Klaassen; D. Harsono; Á. Sánchez-Monge; A. Ahmadi; V. Allen; M. T. Beltrán; H. Beuther; R. Galván-Madrid; C. Goddi; M. G. Hoare; M. R. Hogerheijde; K. G. Johnston; R. Kuiper; L. Moscadelli; T. Peters; L. Testi; F. F. S. van der Tak; W. J. de Wit

doi:10.1051/0004-6361/201935633

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

L. T. Maud, R. Cesaroni, M. S. N. Kumar, V. M. Rivilla, A. Ginsburg, P. D. Klaassen, D. Harsono, Á. Sánchez-Monge, A. Ahmadi, V. Allen, M. T. Beltrán, H. Beuther, R. Galván-Madrid, C. Goddi, M. G. Hoare, M. R. Hogerheijde, K. G. Johnston, R. Kuiper, L. Moscadelli, T. PetersL. Testi, F. F. S. van der Tak, W. J. de Wit

Astronomy

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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 5_{5, 0}-6_{4, 3} ν₂ = 1 (E_u = 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.

Original language	English
Article number	L6
Number of pages	7
Journal	Astronomy & Astrophysics
Volume	627
Issue number	July 2019
DOIs	https://doi.org/10.1051/0004-6361/201935633
Publication status	Published - 1-Jul-2019

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

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Substructures in the Keplerian disc around the O-type (proto-)starG17.64+0.16Final publisher's version, 4.11 MBLicence: Unspecified

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Erratum: 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. & 3 others, Testi, L., van der Tak, F. F. S. & de Wit, W. J., 1-Aug-2019, In: Astronomy & Astrophysics. 628, August 2019, 1 p., C1.
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ALMA Long Baseline maps of G17.64+0.16
Maud, L. T. (Contributor), Cesaroni, R. (Contributor), Kumar, M. S. N. (Contributor), Rivilla, V. M. (Contributor), Ginsburg, A. (Contributor), Klaassen, P. D. (Contributor), Harsono, D. (Contributor), Sánchez-Monge, A. (Contributor), Ahmadi, A. (Contributor), Allen, V. (Contributor), Beltrán, M. T. (Contributor), Beuther, H. (Contributor), Galván-Madrid, R. (Contributor), Goddi, C. (Contributor), Hoare, M. G. (Contributor), Hogerheijde, M. R. (Contributor), Johnston, K. G. (Contributor), Kuiper, R. (Contributor), Moscadelli, L. (Contributor), Peters, T. (Contributor), Testi, L. (Contributor), van der Tak, F. (Contributor) & De Wit, W. J. (Contributor), University of Groningen, 9-Jul-2019
DOI: 10.26093/cds/vizier.36279006
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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., ... de Wit, W. J. (2019). Substructures in the Keplerian disc around the O-type (proto-)star G17.64+0.16. Astronomy & Astrophysics, 627(July 2019), Article L6. https://doi.org/10.1051/0004-6361/201935633

@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 = jul,

day = "1",

doi = "10.1051/0004-6361/201935633",

language = "English",

volume = "627",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = " EDP Sciences",

number = "July 2019",

}

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 & Astrophysics, vol. 627, no. July 2019, L6. https://doi.org/10.1051/0004-6361/201935633

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

SN - 0004-6361

VL - 627

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

IS - July 2019

M1 - L6

ER -

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

Abstract

Keywords

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

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ALMA Long Baseline maps of G17.64+0.16

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