1612 MHz Light Curve of V1511 Cyg

Details 1612 MHz Light Curve of V1511 Cyg 1612 MHz Light Curve of V1511 Cyg

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21541716l&link_type=abstract

American Astronomical Society, AAS Meeting #215, #417.16; Bulletin of the American Astronomical Society, Vol. 42, p.273

Astronomy and Astrophysics

Astronomy

Scientific paper

An inventory of circumstellar shells in the Arecibo sky {| b | > 10\deg \& | l | < 90\deg} with MIR colors appropriate for OH/IR stars shows that up to 75\% do not exhibit 1612 MHz masers above the present Arecibo 5 mJy detection threshold: indeed some of these 'mimics' do not exhibit mainline OH or 22 GHz water masers either, whereas more than 90\% of OH/IR stars do. Low-mass OH/IR stars are expected to pass through a proto planetary nebula (PPN) phase once dM/dt \rightarrow 0, while their fossil shells disperse, prior to becoming planetary nebulae. But there is only one PPN candidate without an OH maser to match the sample's 118 mimics, where \sim8 are expected if mimics evolve directly into PPN (ApJ 533, 959: 2000). Inferentially, therefore, most mimics evolve into OH/IR stars before becoming PPN. Thus a mimic is the immediate precursor of every OH/IR star. At least one star has been seen to match this scenario: V1511 Cyg. While 1612 MHz observations at Arecibo and Nan\c{c}ay show that it was a mimic from 1986 to 1992, V1511 Cyg exhibited a classic, double-peaked profile that had an easily detected 332 mJy peak intensity in May 1999. Its light curve, which has since been followed for 10 years, shows substantial changes in the peak intensities of its red \& blue-shifted masers. It is likely that the earlier 'mimic' phase in this case was the result of the masing intensity dropping below the 60 mJy threshold for detection by pre-1999 observations at Arecibo.

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