English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT

Released

Journal Article

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

MPS-Authors

Maud,  L. T.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Cesaroni,  R.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Kumar,  M. S. N.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Rivilla,  V. M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Ginsburg,  A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Klaassen,  P. D.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Harsono,  D.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Sánchez-Monge,  Á.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Ahmadi,  A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Allen,  V.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Beltrán,  M. T.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Beuther,  H.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Galván-Madrid,  R.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Goddi,  C.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Hoare,  M. G.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Hogerheijde,  M. R.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Johnston,  K. G.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Kuiper,  R.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Moscadelli,  L.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Peters,  T.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Testi,  L.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

van der Tak,  F. F. S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

de Wit,  W. J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Fulltext (restricted access)
There are currently no full texts shared for your IP range.
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available
Citation

Maud, L. T., Cesaroni, R., Kumar, M. S. N., Rivilla, V. M., Ginsburg, A., Klaassen, P. D., et al. (2019). Substructures in the Keplerian disc around the O-type (proto-)star G17.64+0.16. Astronomy and Astrophysics, 627.


Cite as: https://hdl.handle.net/21.11116/0000-0005-D2F1-D
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 &lt; 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 &gt; 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 <A href="http://cdsarc.u-strasbg.fr/">http://cdsarc.u-strasbg.fr</A> (ftp://130.79.128.5) or via <A href="http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/627/L6">http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/627/L6</A>.