1970
DOI: 10.1017/s0074180900000553
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Galactic clusters and H II regions

Abstract: The galactic clusters and the exciting stars of H II regions are powerful indicators of the spiral structure since these objects lie on or very close to the zero age main sequence (ZAMS). For clusters this behaviour can be confirmed by direct photometric observation. The exciting stars of H II regions are probably so young as not to have evolved from the ZAMS. The coincidence of these objects with the ZAMS indicates that there is little scattering in the absolute magnitudes and, as a consequence, little uncert… Show more

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Cited by 17 publications
(5 citation statements)
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“…The fact that young open clusters are tracers of the spiral structure has been known for several decades (eg. Becker & Fenkart, 1970). The distribution of open clusters in the Galactic disk is shown in Figure 1, for clusters younger than 7 Myr, and in Figure 2, for clusters older than 30 Myr .…”
Section: Basic Assumptionsmentioning
confidence: 99%
“…The fact that young open clusters are tracers of the spiral structure has been known for several decades (eg. Becker & Fenkart, 1970). The distribution of open clusters in the Galactic disk is shown in Figure 1, for clusters younger than 7 Myr, and in Figure 2, for clusters older than 30 Myr .…”
Section: Basic Assumptionsmentioning
confidence: 99%
“…Young open clusters have long been recognised as privileged spiral tracers (Becker & Fenkart 1970). Their distances can be better determined than those of individual stars and their youth keeps them close to the spiral arms where they were born.…”
Section: Introductionmentioning
confidence: 99%
“…s (1978) compilation: Radial velocity, distance, colour excess, total apparent magnitude, total absolute magnitude, linear diameter, age, mass Basel data (Becker and Fenkart 1971;Fenkart and Binggeli 1979): Photometric system, colour excess, interstellar extinction, distance, spectral type of hottest star, colour type of bluest star, linear diameter, type of observation van den Bergh-Hagen (1975) data: Angular diameter, richness Lynga (1979) compilation: Selected angular diameter, references (various other parameters with references will be included later).…”
mentioning
confidence: 99%