2016A&A...596A..88L


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.06CEST20:04:42

2016A&A...596A..88L - Astronomy and Astrophysics, volume 596A, 88-88 (2016/12-1)

ALMA observations of the Th 28 protostellar disk. A new example of counter-rotation between disk and optical jet.

LOUVET F., DOUGADOS C., CABRIT S., HALES A., PINTE C., MENARD F., BACCIOTTI F., COFFEY D., MARDONES D., BRONFMAN L. and GUETH F.

Abstract (from CDS):

Aims. Recently, differences in Doppler shifts across the base of four close classical T Tauri star jets have been detected with the HST in optical and near-ultraviolet (NUV) emission lines, and these Doppler shifts were interpreted as rotation signatures under the assumption of steady state flow. To support this interpretation, it is necessary that the underlying disks rotate in the same sense. Agreement between disk rotation and jet rotation determined from optical lines has been verified in two cases and rejected in one case. Meanwhile, the near-ultraviolet lines, which may trace faster and more collimated inner spines of the jet than optical lines, either agree or show no clear indication. We propose to perform this test on the fourth system, Th 28.
Methods. We present ALMA high angular resolution Band 7 continuum, 12CO(3-2) and 13CO(2-1) observations of the circumstellar disk around the T Tauri star Th 28.
Results. The sub-arcsecond angular resolution (0.46''x0.37'') and high sensitivity reached enable us to detect, in CO and continuum, clear signatures of a disk in Keplerian rotation around Th 28. The 12CO emission is clearly resolved, allowing us to derive estimates of disk position angle and inclination. The large velocity separation of the peaks in 12CO, combined with the resolved extent of the emission, indicate a central stellar mass in the range 1-2M. The rotation sense of the disk is well detected in both 13CO and 12CO emission lines, and this direction is opposite to that implied by the transverse Doppler shifts measured in the optical lines of the jet.
Conclusions. The Th 28 system is now the second system, among the four investigated so far, where counter-rotation between the disk and the optical jet is detected. These findings imply either that optical transverse velocity gradients detected with HST do not trace jet rotation or that modeling the flow with the steady assumption is not valid. In both cases jet rotation studies that rely solely on optical lines are not suitable to derive the launching radius of the jet.

Abstract Copyright: © ESO, 2016

Journal keyword(s): stars: individual: Th 28 - ISM: jets and outflows - techniques: interferometric - submillimeter: ISM - stars: formation - circumstellar matter

Simbad objects: 11

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Number of rows : 11

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 V* CW Tau Or* 04 14 17.0041128798 +28 10 57.765657757 13.92 13.64 12.36 12.86   K0Ve 315 0
2 V* RY Tau Or* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 648 1
3 V* DG Tau Or* 04 27 04.6913654419 +26 06 16.041555299 13.57 13.97 10.50 12.28   K6Ve 923 1
4 V* RW Aur TT* 05 07 49.5662483 +30 24 05.177426   10.86 9.60 9.95   K1/5e+K5e 708 0
5 QSO B1514-24 BLL 15 17 41.8135246339 -24 22 19.482167214   15.13 14.00 13.95   ~ 643 3
6 ICRF J153454.6-352623 QSO 15 34 54.68760070 -35 26 23.4970592   20.25   18.72   ~ 23 1
7 WRAY 16-203 Or* 16 08 29.7086692265 -39 03 10.994386198   16.26 15.91 15.38 15.69 K0: 152 1
8 NAME Lupus III SFR 16 09.6 -39 03           ~ 271 0
9 QSO B1730-130 QSO 17 33 02.70578476 -13 04 49.5481484   18 18.5 18.78 17.39 ~ 983 1
10 HH 228E1 HH ~ ~           ~ 4 0
11 HH 228W HH ~ ~           ~ 4 0

    Equat.    Gal    SGal    Ecl

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2020.07.06-20:04:42

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