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Pulkovo compilation of radial velocities for 35495 stars in a common system.
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| The Perkins catalog of revised MK types for the cooler stars
A catalog is presented listing the spectral types of the G, K, M, and Sstars that have been classified at the Perkins Observatory in therevised MK system. Extensive comparisons have been made to ensureconsistency between the MK spectral types of stars in the Northern andSouthern Hemispheres. Different classification spectrograms have beengradually improved in spite of some inherent limitations. In thecatalog, the full subclasses used are the following: G0, G5, G8, K0, K1,K2, K3, K4, K5, M0, M1, M2, M3, M4, M5, M6, M7, and M8. Theirregularities are the price paid for keeping the general scheme of theoriginal Henry Draper classification.
| A list of MK standard stars
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| 1988 Revised MK Spectral Standards for Stars GO and Later
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| Spectral types and their uses
The principles involved in setting up any viable system of spectralclassification are discussed. Their application is illustrated byreviewing the essential features of the original MK system of twodimensions and its extension to additional dimensions, particularattention being paid to the Revised MK System as applied to stars oftypes G0 through M8. The domain of wavelengths within which stars at agiven temperature can be classified on a consistent system is defined.The application of spectral types to the preparation of observingprograms, to statistical studies of the distribution of selected groupsof stars, and to the direct estimation of physical properties of starsis discussed briefly.
| Recognition and classification of strong-CN giants
Fifty of the stars designated as super-metal-rich by Spinrad and Taylor(1969) are classified here on the Revised MK System. Positive CN indicesare assigned in recognition of the characteristic excesses of carbon andnitrogen in their atmospheres, as compared to normal Population I stars.For only a few of the stars, an abnormal strength of the iron lines orof Ca 4226 A is so noticeable that they need to be distinguished bypositive indices for these metals.
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