Detalles de publicación
PP 09056
Intracluster light in the Virgo Cluster: Large scale distribution
(1)Instituto de Astrofísica de Canarias,
(2)European Southern Observatory,
(3)INAF, Osservatorio Astronomico di Pino Torinese
(4)Max-Planck-Institut Institut für Extraterrestrische Physik
(5)Department of Astronomy and Research Center for the Early Universe, School of Science, University of Tokyo
(6)Institute for Cosmic Ray Research, University of Tokyo
(7)Research School of Astronomy and Astrophysics, Mount Stromlo Observatory
Aims. The intracluster light (ICL) is a faint diffuse stellar component of clusters made of stars that are not bound to individual galaxies.
We have carried out a large scale study of this component in the nearby Virgo cluster.
Methods. The diffuse light is traced using planetary nebulae (PNe). The surveyed areas were observed with a narrow-band filter
centered on the [OIII]λ5007 Å emission line redshifted to the Virgo cluster distance (the on-band image), and a broad-band filter (the
off-band image). For some fields, additional narrow band imaging data corresponding to the Hα emission were also obtained. The
PNe are detected in the on-band image due to their strong emission in the [OIII]λ5007 Å line, but disappear in the off-band image.
The contribution of Ly-α emitters at z = 3.14 are corrected statistically using blank field surveys, when the Hα image at the field
position is not available.
Results. We have surveyed a total area of 3.3 square degrees in the Virgo cluster with eleven fields located at different radial distances.
Those fields located at smaller radii than 80 arcmin from the cluster center contain most of the detected diffuse light. In this central
region of the cluster, the ICL has a surface brightness in the range μB = 28.8 − 30 mag arsec−2, it is not uniformly distributed, and
represents about 7% of the total galaxy light in this area. At distances larger than 80 arcmin the ICL is confined to single fields and
individual sub-structures, e.g. in the sub-clump B, the M60/M59 group. For several fields at 2 and 3 degrees from the Virgo cluster
center we set only upper limits.
Conclusions. These results indicate that the ICL is not homogeneously distributed in the Virgo core, and it is concentrated in the high
density regions of the Virgo cluster, e.g. the cluster core and other sub-structures. Outside these regions, the ICL is confined within
areas of ∼ 100 kpc in size, where tidal effects may be at work. These observational results link the formation of the ICL with the
formation history of the most luminous cluster galaxies.
We have carried out a large scale study of this component in the nearby Virgo cluster.
Methods. The diffuse light is traced using planetary nebulae (PNe). The surveyed areas were observed with a narrow-band filter
centered on the [OIII]λ5007 Å emission line redshifted to the Virgo cluster distance (the on-band image), and a broad-band filter (the
off-band image). For some fields, additional narrow band imaging data corresponding to the Hα emission were also obtained. The
PNe are detected in the on-band image due to their strong emission in the [OIII]λ5007 Å line, but disappear in the off-band image.
The contribution of Ly-α emitters at z = 3.14 are corrected statistically using blank field surveys, when the Hα image at the field
position is not available.
Results. We have surveyed a total area of 3.3 square degrees in the Virgo cluster with eleven fields located at different radial distances.
Those fields located at smaller radii than 80 arcmin from the cluster center contain most of the detected diffuse light. In this central
region of the cluster, the ICL has a surface brightness in the range μB = 28.8 − 30 mag arsec−2, it is not uniformly distributed, and
represents about 7% of the total galaxy light in this area. At distances larger than 80 arcmin the ICL is confined to single fields and
individual sub-structures, e.g. in the sub-clump B, the M60/M59 group. For several fields at 2 and 3 degrees from the Virgo cluster
center we set only upper limits.
Conclusions. These results indicate that the ICL is not homogeneously distributed in the Virgo core, and it is concentrated in the high
density regions of the Virgo cluster, e.g. the cluster core and other sub-structures. Outside these regions, the ICL is confined within
areas of ∼ 100 kpc in size, where tidal effects may be at work. These observational results link the formation of the ICL with the
formation history of the most luminous cluster galaxies.