Very long baseline interferometric observations of the hydroxyl masers in VY Canis Majoris

Details Very long baseline interferometric observations of the hydroxyl masers in VY Canis Majoris Very long baseline interferometric observations of the hydroxyl masers in VY Canis Majoris

Feb 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...220..229r&link_type=abstract

Astrophysical Journal, Part 1, vol. 220, Feb. 15, 1978, p. 229-238.

Astronomy and Astrophysics

Astrophysics

38

Hydroxyl Emission, Interstellar Masers, Stellar Envelopes, Variable Stars, Very Long Base Interferometry, Data Processing, Infrared Radiation, Line Spectra, Radial Flow, Water Masers

Scientific paper

Results are presented for spectral-line VLBI observations of the OH emission from VY CMa. The main-line (1665 and 1667 MHz) emission was mapped with an angular resolution of 0.02 arcsec by analyzing interferometer phase data. The main-line emission comes from many maser components of apparent size less than 0.03 arcsec which are separated by up to 0.5 arcsec. New maser features near the center of the OH spectra were detected and found to lie within the region encompassed by the low-velocity OH emission. The 1612-MHz emission was mapped by Fourier inversion of the VLBI data from two baselines. All spatially isolated maser components appeared smaller than 0.15 arcsec; however, the maser emission is very complex at most velocities. Maser components within a velocity range of 1.3 km/s are often separated by more than 1 arcsec, while components more than 10 km/s apart in each emission complex are often coincident to 0.2 arcsec.

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