The Mass of the Classical Cepheid T MON

Details The Mass of the Classical Cepheid T MON The Mass of the Classical Cepheid T MON

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.5868m&link_type=abstract

HST Proposal ID #5868

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Hst Proposal Id #5868 Cool Stars

Scientific paper

This is a proposal to derive the mass of the long period (27^d) binary Cepheid T Mon (=HD 44990). Because it is a high luminosity star, it is particularly relevant to the stars used in extragalactic distance calibration. We will measure the velocity of the companion using a G200M spectrum in a wavelength region uncontaminated by the Cepheid (1800 Angstrom) with an accuracy approaching 1 kms. Since we are continuing to measure the change of the orbital velocity of the Cepheid from the ground, the ratio of the change of the orbital velocities of the Cepheid and the companion at two epochs is the inverse mass ratio. Combining the mass ratio with the mass of the companion from IUE spectral type yields the mass of the Cepheid. The first GHRS velocity will be used to determine the mass ratio using IUE data from 1985. A subsequent HST velocity in 5 to 10 years will bring major improvement to the accuracy of the mass ratio. We stress that from arguments about the observed orbital motion, the current epoch is a window of opportunity to observe the phase of minimum Cepheid orbital velocity which will not recur for at least 100 years. In addition, the fact that the stars are probably near periastron means that the mass ratio can be determined more quickly than at other phases. In the future, the system can be resolved but the mass ratio from this proposal is necessary to interpret these observations.

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