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

  • 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
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.
Original languageEnglish
Article numberL6
Number of pages7
JournalAstronomy and astrophysics
Volume627
Issue numberJuly 2019
Publication statusPublished - 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
Related Publications
  1. 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., Testi, L., van der Tak, F. F. S. & de Wit, W. J., 1-Aug-2019, In : Astronomy and astrophysics. 628, August 2019, 1 p., C1.

    Research output: Contribution to journalComment/Letter to the editorAcademicpeer-review

View all (1) »

Download statistics

No data available

ID: 118169380