The globular cluster system of NGC 4374

M. Gómez, T. Richtler

Resultado de la investigación: Article

22 Citas (Scopus)

Resumen

We study the globular cluster system (GCS) of the giant elliptical NGC 4374 (M 84) in the Virgo cluster using B and R photometry. The colour distribution is bimodal with peaks at B - R = 1.11 and B - R = 1.36, fitting well to those found in other early-type galaxies. The radial profile of the cluster number density is flatter than the galaxy light. Using the luminosity function we derive a distance modulus of μ = 31.61 ± 0.2, which within the uncertainty agrees with the distance from surface brightness fluctuations. Blue and red clusters show similar radial concentrations and azimuthal distributions. The total number of clusters is N = 1775 ± 150, which together with our distance modulus leads to a specific frequency of SN = 1.6 ± 0.3. This value is surprisingly low for a giant elliptical, but resembles the case of merger remnants like NGC 1316, where the low specific frequency is probably caused by the luminosity contribution of an intermediate-age population. A further common property is the high rate of type Ia supernovae which also may indicate the existence of a younger population. However, unlike in the case of NGC 1316, one cannot find any further evidence that NGC 4374 indeed hosts younger populations. The low specific frequency would also fit to a SO galaxy seen face-on.

Idioma originalEnglish
Páginas (desde-hasta)499-508
Número de páginas10
PublicaciónAstronomy and Astrophysics
Volumen415
N.º2
DOI
EstadoPublished - feb 2004

Huella dactilar

young population
globular clusters
common property resource
galaxies
merger
luminosity
photometry
supernovae
brightness
color
distribution
profiles
rate

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Citar esto

Gómez, M. ; Richtler, T. / The globular cluster system of NGC 4374. En: Astronomy and Astrophysics. 2004 ; Vol. 415, N.º 2. pp. 499-508.
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The globular cluster system of NGC 4374. / Gómez, M.; Richtler, T.

En: Astronomy and Astrophysics, Vol. 415, N.º 2, 02.2004, p. 499-508.

Resultado de la investigación: Article

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AU - Richtler, T.

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AB - We study the globular cluster system (GCS) of the giant elliptical NGC 4374 (M 84) in the Virgo cluster using B and R photometry. The colour distribution is bimodal with peaks at B - R = 1.11 and B - R = 1.36, fitting well to those found in other early-type galaxies. The radial profile of the cluster number density is flatter than the galaxy light. Using the luminosity function we derive a distance modulus of μ = 31.61 ± 0.2, which within the uncertainty agrees with the distance from surface brightness fluctuations. Blue and red clusters show similar radial concentrations and azimuthal distributions. The total number of clusters is N = 1775 ± 150, which together with our distance modulus leads to a specific frequency of SN = 1.6 ± 0.3. This value is surprisingly low for a giant elliptical, but resembles the case of merger remnants like NGC 1316, where the low specific frequency is probably caused by the luminosity contribution of an intermediate-age population. A further common property is the high rate of type Ia supernovae which also may indicate the existence of a younger population. However, unlike in the case of NGC 1316, one cannot find any further evidence that NGC 4374 indeed hosts younger populations. The low specific frequency would also fit to a SO galaxy seen face-on.

KW - Galaxies: distances and redshifts

KW - Galaxies: elliptical and lenticular, cD

KW - Galaxies: individual: NGC 4374

KW - Galaxies: interactions

KW - Galaxies: star clusters

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