Volume 586, February 2016
|Number of page(s)||6|
|Section||Interstellar and circumstellar matter|
|Published online||27 January 2016|
The radio continuum spectrum of Mira A and Mira B up to submillimeter wavelengths
Observatorio Astronómico Nacional (OAN-IGN), Alfonso XII 3, 28014 Madrid, Spain
Received: 25 November 2015
Accepted: 20 December 2015
Aims. We present new measurements of the flux densities at submillimeter wavelengths based on ALMA band 7 (338 GHz, λ0.89 mm) and band 9 (679 GHz, λ0.44 mm) observations to better constrain the origin of the continuum emission of the Mira AB binary system and to check its orbit.
Methods. We have measured the Mira A and Mira B continuum in ALMA band 7, with a resolution of ~0.̋31, and for the first time in ALMA band 9, with a resolution of ~0.̋18. We have resolved the binary system at both bands, and derived the continuum spectral index of the stars and their relative position. We also analyzed ALMA Science Verification data obtained in bands 6 and 3. Measurements at centimeter wavelengths obtained by other authors have been included in our study of the spectral energy distribution of the Mira components.
Results. The Mira A continuum emission has a spectral index of 1.98 ± 0.04 extending from submillimeter down to centimeter wavelengths. The spectral index of the Mira B continuum emission is 1.93 ± 0.06 at wavelengths ranging from submillimeter to ~3.1 mm, and a shallower spectral index of 1.22 ± 0.09 at longer wavelengths. The high precision relative positions of the A and B components are shown to significantly depart from the current (preliminary) orbit by ~14 mas.
Conclusions. The Mira A continuum emission up to submillimeter wavelengths is consistent with that of a radio photosphere surrounding the evolved star for which models predict a spectral index close to 2. The Mira B continuum emission cannot be described with a single ionized component. An extremely compact and dense region around the star can produce the nearly thermal continuum measured in the range λ0.4−3.1 mm, and an inhomogeneous, less dense, and slightly larger ionized envelope could be responsible for the emission at longer wavelengths. Our results illustrate the potential of ALMA for high precision astrometry of binary systems. We have found a significant discrepancy between the ALMA measurements and the predicted orbit positions.
Key words: binaries: general / stars: AGB and post-AGB / stars: atmospheres / stars: individual: Mira A / stars: individual: Mira B
© ESO, 2016
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