The Eggen uvby photometric system
Basic Reference
Eggen O.J. 1976, Publ. Astron. Soc. Pacific 88, 732
Abstract
In four-color, intermediate-band photometry of late-type stars, difficulty
has been experienced in reproducing the Strömgren system defined by
standard stars by Crawford and Barnes. The difficulty is believed to be
connected with the fact that an international bulk of order for filters
has produced a considerably narrower v filter than that used in
the original observations of standard stars. Because of this difficulty
a new system has been defined which is characterized by
(b-y) = (b-y)Strömgren, M1 = m1(Strömgren) for (b-y) < 0.30
and C1 = c1(Strömgren) for (b-y) < 0.20.
The use of M1 as a metal-abundance parameter is demonstrated with
Hyades-cluster and group stars and members of the Arcturus group, as well
as some very metal-weak subdwarfs.
Content
Access to the data and references
Asiago Database on Photometric System (ADPS)
Indices and Parameters
Ve, b-y, M1, C1
Filters
Photomultiplier
Problems
In the course of a systematic comparison of photometric data, a
number of problems have been found, but could not
be solved. Generally the data associated with a star identification are not
in agreement with those from other systems, usually the UBV, uvby and Geneva
systems.
Errata
A number of printing errors have been found in
tables.
Please, send your
commentsto epaunzen@physics.muni.cz
epaunzen@physics.muni.cz
Last update: 13 September 2002