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The 2008 outburst in the Young Stellar System Z CMa. III - Multi-epoch high-angular resolution images and spectra of the components in near-infrared | | M. Bonnefoy
; G. Chauvin
; C. Dougados
; A. Kospal
; M. Benisty
; G. Duchene
; J. Bouvier
; P. J. V. Garcia
; E. Whelan
; S. Antoniucci
; L. Podio
; | | Date: |
29 Aug 2016 | | Abstract: | Z CMa is a complex pre-main sequence binary with a current separation of 100
mas, known to consist of an FU Orionis star (SE component) and an embedded
Herbig Be star (NW component). Immediately when the late-2008 outburst of Z CMa
was announced to the community, we initiated a high angular resolution imaging
campaign with VLT/NaCo, Keck/NIRC2, VLT/SINFONI, and Keck/OSIRIS which aimed at
characterizing the outburst of both components of the system in the
near-infrared. We confirm that the NW star dominates the system flux in the
1.1-3.8 microns range and is responsible for the photometric outburst. We
extract the first medium-resolution (R=2000-4000) near-infrared (1.1-2.4
microns) spectra of the individual components during and after the outburst.
The SE component has a spectrum typical of FU Orionis objects. The NW component
spectrum is characteristic of embedded outbursting protostars and EX Or
objects. It displays numerous emission lines during the outburst whose
intensity correlates with the system activity. In particular, we find a
correlation between the Brackett gamma equivalent width and the system
brightness. The bluing of the continuum of the NW component along with the
absolute flux and color-variation of the system during the outburst suggests
that the outburst was caused by a complex interplay between a variation of the
extinction in the line of sight of the NW component on one hand, and the
emission of shocked regions close to the NW component on the other. We confirm
the recently reported wiggling of the SE component jet from [Fe II] line
emission. We find a point-like structure associated with a peak emission at
2.098 microns coincidental with the clump or arm seen in broadband polarization
differential imaging as well as additional diffuse emission along a PA=214
degrees. The origin of these two structures is unclear and deserves further
investigation. | | Source: | arXiv, 1608.8035 | | Services: | Forum | Review | PDF | Favorites | |
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