High-resolution spectroscopy of V1853 CYGNI (LS 2 + 34 deg 26): Birth of a planetary nebula?

Details High-resolution spectroscopy of V1853 CYGNI (LS 2 + 34 deg 26): Birth of a planetary nebula? High-resolution spectroscopy of V1853 CYGNI (LS 2 + 34 deg 26): Birth of a planetary nebula?

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...424l.123s&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 424, no. 2, p. L123-L126

Astronomy and Astrophysics

Astronomy

14

Absorption Spectra, Asymptotic Giant Branch Stars, Emission Spectra, Light (Visible Radiation), Planetary Nebulae, Astronomical Observatories, Charge Coupled Devices, Infrared Astronomy Satellite, Optical Thickness, Radial Velocity, Spectrometers

Scientific paper

High-resolution optical spectra are discussed for the high-latitude B-supergiant V1853 Cyg (LS II + 34 deg 26), which has been identified recently as a hot post-asymptotic giant branch (AGB) star with far-infrared Infrared Astronomical Satellite (IRAS) colors similar to those of dusty planetary nebulae. Spectra obtained on eight nights between 1993 August and November reveal strong emission lines of H-alpha, beta, and gamma, as well as a variety of profiles (absorption, emission, P Cygni) for the He I lines. A photospheric spectrum of absorption lines, fairly typical of B1-2 supergiants, is present, but the lines are asymmetric and their shapes and equivalent widths vary significantly on a night-to-night basis. The velocity of the absorption lines varies by approximately 40 km/s. Emission lines from permitted (C II, N II, Si II, and Fe III) and forbidden (N II), (O I), (S II), and (Fe II) transitions are visible at a constant radial velocity over the observing interval. This object may be in the process of becoming a planetary nebula.

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