IRAS Point Source Identifications (MacConnell, 1993; rev. 2009)

Details IRAS Point Source Identifications (MacConnell, 1993; rev. 2009) IRAS Point Source Identifications (MacConnell, 1993; rev. 2009)

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ycat.3170....0m&link_type=abstract

VizieR On-line Data Catalog: III/170A. Originally published in: (unpublished, 1993; revised 2009)

Physics

Infrared Sources, Stars: Late-Type, Cross Identifications

Scientific paper

Most of the sources are south of the celestial equator and have been classified in increasing galactic longitude over the period Sept. 1985 to May 1992. They have been classified on Kodak I-N objective-prism plates taken primarily with the Curtis Schmidt telescope at Cerro Tololo, but some northern plates taken with the Burrell Schmidt at Kitt Peak were also used for classification. The spectra cover the range 680-880nm at a dispersion of 340nm/mm at the A-band, and the plate scale is 96.6"/mm. They are ideal for classifying M stars of type M3 and cooler (increasing strength of TiO and VO bands) and carbon stars (CN bands), but stars warmer than M2 and most S stars cannot be classified or identified as such. The M stars M3 and cooler can be separated into about five groups. The limiting mag of the deepest plates is I about 13.5.
The IRAS PS were identified on transparent overlays made to the plate scale for each plate center, and the association of a spectrum with a given PS is usually unambiguous. In cases of doubt or offset, a comment is made. Note that there are some cases where the PSC gives an incorrect association on the basis of position, and the correct association is with a faint, uncatalogued M star.
(4 data files).

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