Astronomy and Astrophysics, volume 559A, 120-120 (2013/11-1)
VLA survey of 22 GHz H2O masers toward ten silicate carbon stars.
OHNAKA K., BOBOLTZ D.A., MULITZ-SCHIMEL G., IZUMIURA H. and WITTKOWSKI M.
Abstract (from CDS):
Despite their carbon-rich photospheres, silicate carbon stars show evidence of oxygen-rich circumstellar material, which is thought to exist in disks. Silicate carbon stars represent interesting cases that allow us to study the possible effects of binarity on stellar evolution and mass loss accompanied by the formation of disks. We present a small survey of 22GHz H2O masers toward ten silicate carbon stars with much better sensitivity than is the case for previous observations. We observed our sample with the Karl G. Jansky Very Large Array (VLA) using the most expanded configuration (A-configuration) with a maximum baseline of 36km. For some of our program stars with noisy Infrared Astronomical Satellite (IRAS) Low Resolution Spectra (LRS), we present new mid-IR spectra obtained with the Very Large Telescope Interferometer and the Spitzer Space Telescope. We detected H2O masers toward five out of ten silicate carbon stars (EU And, V778 Cyg, IRAS06017+1011, V1415 Cyg, and NC83 = V1945 Cyg), with NC83 being a new detection. No H2O masers were detected toward BM Gem, IRAS07221-0431, IRAS08002-3803, IRAS18006-3213, and HD189605. The velocity separation between the most blue- and red-shifted maser features is 10-14km/s. If we assume that the masers originate in circum-companion disks, the measured velocity separations translate into a lower limit of the rotational velocity of 5-7km/s, and the upper limit of the radius of the maser emitting region is estimated to be 10-68 AU for a companion mass of 0.5-1.7M☉. The new mid-IR spectra of NC83, IRAS06017+1011, and HD189605 confirm the 10µm silicate emission. The latter two stars show a bump at ∼11.5µm, which is presumably due to SiC originating in the ongoing mass loss from the carbon-rich primary star, not due to crystalline silicate. We also report on the detection of the UV flux at 2271Å toward HD189605.
radio lines: stars - techniques: interferometric - circumstellar matter - stars: carbon - stars: chemically peculiar - stars: AGB and post-AGB
Paragraph. 2 MC79-11 is probably MC79 2-11 and not MC79 1-11.
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