The 2008 Outburst in the Young Stellar System Z CMa: The First Detection of Twin Jets

• Type: Article in International Scientific Journal
• Date: 2010

Authors

E. T. Whelan (Author) Other; C. Dougados (Author) Other; M. D. Perrin (Author) Other; M. Bonnefoy (Author) Other; I. Bains (Author) Other; M. P. Redman (Author) Other; T. P. Ray (Author) Other; H. Bouy (Author) Other; M. Benisty (Author) Other; J. Bouvier (Author) Other; G. Chauvin (Author) Other; P. J. V. Garcia (Author) FEUP; K. Grankvin (Author) Other; F. Malbet (Author) Other

Journal

Title: Astrophysical Journal Letters

Vol. 720 No. 1

Pages: L119-L124

ISSN: 2041-8205

Publisher: American Astronomical Society

Indexing

ISI Web of Knowledge - 21 Citations

ISI Web of Science

Scopus - 26 Citations

INSPEC

Scientific classification

FOS: Natural sciences > Physical sciences

Other information

Authenticus ID: P-003-344

DOI: 10.1088/2041-8205/720/1/L119

Abstract (EN): The Z CMa binary is understood to undergo both FU Orionis (FUOR) and EX Orionis (EXOR) type outbursts. While the SE component has been spectroscopically classified as an FUOR, the NW component, a Herbig Be star, is the source of the EXOR outbursts. The system has been identified as the source of a large outflow; however, previous studies have failed to identify the driver. Here, we present adaptive optics assisted [Fe II] spectro-images which reveal for the first time the presence of two small-scale jets. Observations made using OSIRIS at the Keck Observatory show the Herbig Be star to be the source of the parsec-scale outflow, which within 2'' of the source shows signs of wiggling and the FUOR to be driving a ~0farcs4 jet. The wiggling of the Herbig Be star's jet is evidence for an additional companion which could in fact be generating the EXOR outbursts, the last of which began in 2008. Indeed, the dynamical scale of the wiggling corresponds to a timescale of 4-8 years which is in agreement with the timescale of these outbursts. The spectro-images also show a bow-shock-shaped feature and possible associated knots. The origin of this structure is as of yet unclear. Finally, interesting low velocity structure is also observed. One possibility is that it originates in a wide-angle outflow launched from a circumbinary disk.

Language: English

Type (Professor's evaluation): Scientific