Speckle masking observations of the young binary Z Canis Majoris

Details Speckle masking observations of the young binary Z Canis Majoris Speckle masking observations of the young binary Z Canis Majoris

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...291..500b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 291, no. 2, p. 500-504

Astronomy and Astrophysics

Astrophysics

25

Binary Stars, H Alpha Line, Pre-Main Sequence Stars, Speckle Interferometry, Visible Spectrum, Accretion Disks, Image Processing, Spectral Energy Distribution

Scientific paper

We present the first speckle masking observations of the pre-main sequence binary system Z canis majoris (Z CMa) at optical wavelengths (narrow-band R filter and edge filter RG 610). The diffraction-limited images confirm that Z CMa is a binary with a separation of 0.100 sec + or - 0.008 sec at position angle 350 deg + or - 2 deg. The intensity ratio of the stars is 7.2 for the narrow-band R filter and 7.7 for the RG610 filter. The south-eastern component is the brighter component (i.e. the FU Ori object), in agreement with the results of Koresko et al. (1991) based on near-infrared speckle data. However, our optical detection of the north-western component (the infrared companion) would not have been expected according to Koresko et al.'s analysis. One possible explanation could be scattered light. This agrees with recent polarimetric evidence from Whitney at a. (1993) that scattering plays a role in seeing the infrared companion. We discuss the possiblity that both components of the Z CMa system may be FU Ori objects.

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