The Physical Properties of the SVS 13 Protobinary System: Two Circumstellar Disks and a Spiraling Circumbinary Disk in the Making. (arXiv:2111.11787v1 [astro-ph.SR])
Ana K. Diaz-Rodriguez (1 and 2), Guillem Anglada (1), Guillermo Blázquez-Calero (1), Mayra Osorio (IAA), José F. Gómez (1), Gary A. Fuller (2, 1 and 3), Robert Estalella (4), José M. Torrelles (5 and 6), Sylvie Cabrit (7 and 8), Luis F. Rodríguez (9), Charlène Lefèvre (10), Enrique Macías (11 and 12), Carlos Carrasco-González (9), Luis A. Zapata (9), Itziar de Gregorio-Monsalvo (12), Paul T. P. Ho (13 and 14) ((1) Instituto de Astrofísica de Andalucía, (2) The UK ALMA Regional Centre Node, Jodrell Bank Centre for Astrophysics, The University of Manchester, (3) I. Physikalisches Institut, University of Cologne, (4) Departament de Física Quàntica i Astrofísica, Institut de Ciències del Cosmos, Universitat de Barcelona, (5) Institut de Ciències de l'Espai (ICE, CSIC), (6) Institut d'Estudis Espacials de Catalunya (IEEC), (7) Univ. Grenoble Alpes, CNRS, IPAG, (8) Observatoire de Paris, PSL University, Sorbonne Université, CNRS, LERMA, (9), Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, (10) Institut de RadioAstronomie Millimétrique (IRAM), (11) Joint ALMA Observatory, (12) European Southern Observatory (ESO), (13) Academia Sinica Institute of Astronomy and Astrophysics, (14) East Asian Observatory)
We present VLA and ALMA observations of the close (0.3" = 90 au separation)
protobinary system SVS 13. We detect two small circumstellar disks (radii
12 and 9 au in dust, and 30 au in gas) with masses of
0.004-0.009 for VLA 4A (the western component) and
0.009-0.030 for VLA 4B (the eastern component). A circumbinary
disk with prominent spiral arms extending 500 au and a mass of
0.052 appears to be in the earliest stages of formation. The
dust emission is more compact and with a very high optical depth toward VLA 4B,
while toward VLA 4A the dust column density is lower, allowing the detection of
stronger molecular transitions. We infer rotational temperatures of 140
K, on scales of 30 au, across the whole source, and a rich chemistry.
Molecular transitions typical of hot corinos are detected toward both
protostars, being stronger toward VLA 4A, with several ethylene glycol
transitions detected only toward this source. There are clear velocity
gradients, that we interpret in terms of infall plus rotation of the
circumbinary disk, and purely rotation of the circumstellar disk of VLA 4A. We
measured orbital proper motions and determined a total stellar mass of 1
. From the molecular kinematics we infer the geometry and orientation
of the system, and stellar masses of 0.26 for VLA 4A and
0.60 for VLA 4B.
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