2017A&A...597A..91B


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.22CEST06:40:04

2017A&A...597A..91B - Astronomy and Astrophysics, volume 597A, 91-91 (2017/1-1)

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.

BONNEFOY M., CHAUVIN G., DOUGADOS C., KOSPAL A., BENISTY M., DUCHENE G., BOUVIER J., GARCIA P.J.V., WHELAN E., ANTONIUCCI S. and PODIO L.

Abstract (from CDS):

Context. Z CMa is a complex pre-main sequence binary with a current separation of 110mas, 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 1.1-3.8µm range and is responsible for the photometric outburst. We extract the first medium-resolution (R∼2000-4000) near-infrared (1.1-2.4µm) spectra of the individual components. 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 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 [FeII] line emission. We find a point-like structure associated with a peak emission at 2.098µm 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.

Abstract Copyright: © ESO, 2017

Journal keyword(s): techniques: high angular resolution - binaries: general - stars: individual: Z CMa - stars: pre-main sequence

Simbad objects: 27

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Number of rows : 27

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 [CG2010] IRAS 03220+3035(N) Y*O 03 25 09.43 +30 46 21.6           ~ 3 0
2 V* XZ Tau TT* 04 31 40.0868968022 +18 13 56.642439056     10.40 13.12   M2e+M2e 402 1
3 V* VY Tau TT* 04 39 17.4208176970 +22 47 53.361809753     9.00     M0Ve 178 0
4 V* UX Ori Ae* 05 04 29.9881676817 -03 47 14.288047238 10.25 10.93 8.70 9.62 9.43 A4IVe 327 1
5 V* EX Ori LP* 05 24 28.8519295560 -06 08 49.809109129   11.19 9.98     M7III: 32 1
6 V* V1118 Ori TT* 05 34 44.745 -05 33 42.18 15.053 15.378 14.430 15.22 12.701 M1e 115 0
7 V* FU Ori FU* 05 45 22.3650208559 +09 04 12.296285806   10.72 9.60     F0Iab 686 1
8 V* V1647 Ori FU* 05 46 13.1370923766 -00 06 04.876812846     18.1     ~ 220 1
9 HD 53060 * 07 03 14.2033939179 -11 08 14.671149058   8.03 7.99     A0IV/V 11 0
10 V* Z CMa Ae* 07 03 43.1588002461 -11 33 06.230351311 10.51 9.99 8.80     B5/8eq+F5/7 518 3
11 NAME CMa OB1 As* 07 07.0 -10 28           ~ 118 0
12 HD 54335 V* 07 07 59.3656341338 -11 35 47.295061691   8.93 7.38     K4III 4 0
13 HD 67213 * 08 06 17.2824913554 -18 22 23.411333248   7.63 7.60     A0V 8 0
14 HD 97895 * 11 15 21.5289924799 -29 30 57.796919472 8.11 8.66 8.73     B4V 14 0
15 HD 109615 * 12 35 47.3259473253 +39 41 01.314584733   7.246 7.275     A0V 37 0
16 HD 127913 PM* 14 33 51.4909372576 +02 34 32.163440900   9.81 9.14     G6V 16 0
17 V* V836 Cen bC* 14 46 25.7600874450 -37 13 20.072260223 7.04 7.88 8.05     B2 99 0
18 HD 325367 TT* 16 03 05.4914377137 -40 18 25.426543472   11.40 8.50     M0 268 0
19 V* V346 Nor FU* 16 32 32.19 -44 55 30.7           ~ 110 1
20 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2472 0
21 [TS84] IRS 2 Y*O 19 01 41.569 -36 58 31.23           K2 78 0
22 V* V710 CrA Or* 19 01 50.67792 -36 58 09.6132           K7: 114 0
23 V* R CrA Ae* 19 01 53.6850227874 -36 57 08.145519972 12.781 12.651 11.917 11.242 10.412 B5IIIpe 439 1
24 Parsamian 21 FU* 19 29 00.849 +09 38 43.40   15.18 14.07 13.93   F5Iabe 80 1
25 V* PV Cep Or* 20 45 53.9537161790 +67 57 38.678052612   19.27 17.46 15.98 14.60 A5 248 3
26 V* V2492 Cyg Or* 20 51 26.2368444519 +44 05 23.866104173   20.2   18.3   F-GII/MI 61 0
27 V* V1735 Cyg FU* 21 47 20.6624829527 +47 32 03.856911703           ~ 148 0

    Equat.    Gal    SGal    Ecl

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2019.10.22-06:40:04

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