Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26as...67..423m&link_type=abstract
Astronomy and Astrophysics Supplement Series (ISSN 0365-0138), vol. 67, no. 3, Feb. 1987, p. 423-445. Research supported by the
Astronomy and Astrophysics
Astrophysics
23
Galactic Structure, Magellanic Clouds, Star Distribution, Stellar Motions, F Stars, Hot Stars, K Stars, M Stars, Radial Velocity, Supergiant Stars
Scientific paper
We present high accuracy radial velocity measurements for 233 stars of spectral types F0 and later in the direction of the Small Magellanic Cloud and between the two Magellanic Clouds. 33 of them are considered as galactic stars. With the previously known data from spectrographic observations, mainly of OBA-type stars, we now possess radial velocities of 274 SMC stars (plus the 33 galactic stars). The new observations presented here were made with the photoelectric scanner CORAVEL attached to the 1.54 m Danish telescope at La Silla, ESO, in Chile. The standard errors for a single measurement are 2.0 km/s for F-type stars and 1.3 km/s for M-type stars. The comparison with the previous spectrographic radial velocities for OBA supergiants in the SMC shows that these must be corrected by -3 km/s to be on the IAU (and CORAVEL) system. The surface distribution of supergiants shows a tendency for the radial velocities to cluster in groups of different values, of low dispersion (approximately 5 km/s) and of typical size of the order of 0.8 kpc at the distance of the SMC. The global histogramme of the radial velocity distribution does not show the two peaks possibly indicated by the OBA supergiants. The overall mean radial velocity is, after correction for the solar motion, RVGSR = - 1 ± 1 km/s, and the dispersion (approximately 18 km/s) is the same for OBA and F0 to M-type supergiants. All these considerations confirm the probable existence of several stellar groups of different radial velocities at different distances along the line of sight in the Small Magellanic Cloud. On the basis of these considerations and of the radial velocity criterion, we discuss the membership of individual stars. We consider that three of these stars belong to the Junction between the Large and the Small Magellanic Cloud and that 15 are high radial velocity residual stars, probably Magellanic. The 256 remaining stars are probable normal members of the Small Magellanic System.
Andersen Jeppe J.
Ardeberg Arne
Bardin Cl.
Imbert M.
Lindgren Harri
No associations
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