One-milliarsecond precision parallax studies in the regions of Delta Cephei and EV Lacertae

Details One-milliarsecond precision parallax studies in the regions of Delta Cephei and EV Lacertae One-milliarsecond precision parallax studies in the regions of Delta Cephei and EV Lacertae

Oct 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993pasp..105.1101g&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 105, no. 692, p. 1101-1106

Astronomy and Astrophysics

Astronomy

6

Astronomy, Stellar Magnitude, Stellar Parallax, Variable Stars, Stellar Luminosity, Stellar Spectrophotometry

Scientific paper

Trigonometric parallaxes for stars in the regions of the variable stars delta Cephei and EV Lacertae are derived from data collected with the Multichannel Astrometric Photometer (MAP) and the Thaw Refractor of the University of Pittsburgh's Allegheny Observatory. The weighted mean parallax of all trigonometric studies of delta Cephei is now + 0.0030 sec + or - 0.00093 sec, corresponding to a distance modulus of 7.61 + or - 0.67 mag. This indicates that this luminosity standard star is approximately one standard deviation more distance than has been generally accepted. The weighted mean trigonometric parallax of all studies of the variable star EV Lacertae (BD + 43 deg 4305) is + 0.1993 sec + or - 0.00093 sec, implying a distance modulus of - 1.498 + or - 0.0010 mag. The calculated absolute magnitude of this star is almost exactly that predicted by its (R-I)Kron magnitude and by the Gliese (R-I) main-sequence value for stars in the solar neighborhood. We also find a parallax of 0.0189 sec + or - 0.0008 sec for the FO IVn star, HR 8666 (BD + 43 sec 4300). The derived luminosity of this star is midway between that expected for luminosity class IV and V stars at the indicated temperature.

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