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The 2008 Outburst in the Young Stellar System Z Cma III

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The 2008 Outburst in the Young Stellar System Z Cma III A&A 597, A91 (2017) Astronomy DOI: 10.1051/0004-6361/201628693 & c ESO 2017 Astrophysics 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. Bonnefoy1; 2, G. Chauvin1; 2, C. Dougados1; 2, Á. Kóspál3, M. Benisty1; 2, G. Duchêne1; 2; 4, J. Bouvier1; 2, P. J. V. Garcia5, E. Whelan6, S. Antoniucci7, and L. Podio8 1 Univ. Grenoble Alpes, IPAG, 38000 Grenoble, France e-mail: [email protected] 2 CNRS, IPAG, 38000 Grenoble, France 3 Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, PO Box 67, 1525 Budapest, Hungary 4 Astronomy Department, UC Berkeley, 501 Campbell Hall, Berkeley CA 94720-3411, USA 5 Universidade do Porto, Faculdade de Engenharia, Rua Dr. Roberto Frias, s/n, 4200-465 Porto, Portugal 6 Department of Experimental Physics, National University of Ireland Maynooth, Maynooth, Co. Kildare, Ireland 7 INAF–Osservatorio Astronomico di Roma, via Frascati 33, 00078 Monte Porzio Catone, Italy 8 INAF–Osservatorio Astrofisico di Arcetri, L.go E. Fermi 5, 50125 Firenze, Italy Received 11 April 2016 / Accepted 12 June 2016 ABSTRACT Context. Z CMa is a complex pre-main sequence binary with a current separation of 110 mas, known to consist of an FU Orionis star (SE component) and an embedded Herbig Be star (NW component). Although it represents a well-studied and characterized system, the origin of photometric variabilities, the component properties, and the physical configuration of the system remain mostly unknown. Aims. Immediately when the late-2008 outburst of Z CMa was announced to the community, we initiated a high angular resolution imaging campaign aimed at characterizing the outburst state of both components of the system in the near-infrared. Methods. We used the VLT/NACO and the Keck/NIRC2 near-infrared adaptive optics instrument to monitor the astrometric position and the near-infrared photometry of the Z CMa components during the outburst phase and one year after. The VLT/SINFONI and Keck/OSIRIS integral field spectroscrographs were in addition used to characterize for the first time the resolved spectral properties of the FU Orionis and the Herbig Be component during and after the outburst. Results. We confirm that the NW star dominates the system flux in the 1.1−3.8 µm range and is responsible for the photometric outburst. We extract the first medium-resolution (R ∼ 2000−4000) near-infrared (1.1−2.4 µm) spectra of the individual components. The SE component has a spectrum typical of FU Orionis objects. The NW component spectrum is characteristic of embedded out- bursting protostars and EX Or objects. It displays numerous emission lines whose intensity correlates with the system activity. In particular, we find a correlation between the Brγ 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 µm coincidental with the clump or arm seen in broadband polarization differential imaging as well as additional diffuse emission along a PA = 214◦. The origin of these two structures is unclear and deserves further investigation. Key words. techniques: high angular resolution – binaries: general – stars: individual: Z CMa – stars: pre-main sequence 1. Introduction of an optically thick accretion disk surrounding an 1−3 M star −3 −1 with an accretion rate of 10 M yr . The model failed to ex- Z Canis Majoris (Z CMa) is a complex pre-main sequence bi- plain the near-infrared (NIR) part of the Z CMa spectrum, how- nary member of the CMa OB1 association (age < 1 Myr; Herbst ever, as well as a strong increase in brightness in 1987. Dur- et al. 1978), with an estimated distance ranging from 950 pc to ing the 1987 outburst, the optical spectrum was characterized by 1150 pc (Clariá 1974; Humphreys 1978; Kaltcheva & Hilditch a featureless and bluer continuum, a rise of Balmer lines, and 2000). The system is known for its recurring EX Orionis emission lines of Fe II, Cr II, and Ti II (Hessman et al. 1991), (EX Or)-like outbursts with recent events recorded in 1987, which is unconsistent with typical FU Orionis activity. 2000, 2004, 2008, 2011, 2015, and 2016. The problem was partly solved by Koresko et al.(1991) Z CMa was classified by Hartmann et al.(1989) as a FU Ori- who discovered that Z CMa consists of a 110 mas binary. onis variable based on its broad, doubled optical line absorp- The SW component of the pair is the FU Orionis star that tions, optical spectral type of F-G, and CO first overtone. The au- dominates the optical flux. The NW component dominates the thors were able to reproduce the UV-optical spectrum by a model NIR (>2 µm) to sub-mm spectrum, and the total luminosity. Article published by EDP Sciences A91, page 1 of 20 A&A 597, A91 (2017) 6 SINFONI P1640 8 OSIRIS NIRSPEC Anto.+09 10 Visual Magnitude AMBER 12 2004 2005 2006 2007 2008 2009 2010 2011 2012 2013 2014 2015 2016 Date (years) Fig. 1. Light curve of Z CMa inferred from AAVSO observations. The spectroscopic observations of the HBe and FUOR are reported in the figure. The dashed zone corresponds to the 2008 outburst of the system. Follow-up observations (Whitney et al. 1993; Garcia et al. 1999; At the Astronomical Unit scale, the FUOR is strongly re- van den Ancker et al. 2004, hereafter VDA04) permitted the solved by the Keck-I interferometer to a level that is difficult conclusion that this component is an Herbig Be star (hereafter to explain with thermal emission of the accretion disk alone HBe). VDA04 obtained a NIR (1.9−4.1 µm) spectrum while the (Millan-Gabet et al. 2006). Hence its close environment appears system was returning to its quiescent state. This spectrum shows to be more complex than expected. The HBe component has Brα, Brγ, and Pfγ in emission and the CO band-head in absorp- also been observed with Keck-I (Monnier et al. 2005) and with tion around 2.3 µm. The authors suggested that the emission AMBER on the VLTI (Li Causi et al. 2008; Benisty et al. 2010). lines are formed into an accreting circumstellar disk surround- Based on the Keck observations, the authors have modelled the ing the HBe, and also in an extended envelope above and below NIR emission as coming from a uniform ring. Nonetheless, they the disk plane. The emission line analysis led VDA04 to infer a have finally concluded that the ring model was doubtful for this B0IIIe spectral type. Luminosity and effective temperature esti- star, considering the large uncertainty of its spectral type. Mo- mates enable the authors to derive a mass of 16−38 M for the rover, the amount of infrared emission coming from this source HBe using various evolutionary model predictions for ages of alone at a given epoch is also poorly known, which adds to the 3 × 105 yr and 4 × 104 yr respectively. difficulty of interpreting the interferometric measurements. From January 2008 to October 2009, the system began At large scales, this system reveals a rich outflow activity. to experience an optical outburst, the largest reported in the A collimated optical outflow (3.9 pc; PA = 240◦) and a bow- past 90 years of available observations (Grankin & Artemenko shock-shaped feature at 6000 have been reported by Poetzel et al. 2009). This outburst triggered additional observations of the sys- (1989). Multiple outflow component profiles traced by optical tem. Hinkley et al.(2013) presented adaptive optics JHKL band forbidden lines are present close to the source. Whelan et al. photometry of the individual components. They concluded (2010) confirmed the existence of a jet driven by the HBe that the embedded HBe component is solely responsible for star (paper II), which is unambiguously the driving source of the outburst. Benisty et al.(2010) obtained spectrally resolved the Z CMa parsec-scale outflow. The HBe star jet is seen os- interferometric observations of the HBe to study the hot gas cillating around a given position angle (jet wiggling), proba- emitting across the Brγ emission line (paper I). They found that bly due to a closer companion to the HBe star. A twin jet the line profile, the astrometric signal, and the visibilities are driven by the FUOR component was also clearly identified. consistent with the emission of a bipolar wind that may be partly Millan-Gabet et al.(2001) also reported a cavity-like structure seen through a disk hole inside the dust sublimation radius at the in adaptive optics J-band imaging, extending to the SW of the au scale. Their multi-epoch observations led them to suggest that system, which they interpreted as light scattered off the wall of a the outburst is related to a period of strong mass-loss and not to a jet-blown cavity aligned with the Z CMa large-scale outflows. change in the extinction along the line of sight. The spectropho- Alonso-Albi et al.(2009) modeled the spectral energy dis- tometric, spectropolarimetric, and polarimetric imaging obser- tribution of the system by contributions from free-free emis- vations of the system (Szeifert et al.
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