Luminosity distributions within rich clusters — I. A ubiquitous dwarf-rich luminosity function?
نویسندگان
چکیده
منابع مشابه
/ 97 04 17 0 v 1 1 7 A pr 1 99 7 Luminosity Distributions within Rich Clusters - I : A Ubiquitous Dwarf - Rich Luminosity Function ?
From deep CCD observations of the cluster Abell 2554 we have recovered the cluster’s luminosity distribution over a wide range of magnitude (−24 < MR < −16). We compare the derived A 2554 cluster luminosity function (at redshift 0.1) with that of the local Coma Cluster (A 1656) and the more distant (z = 0.2) cluster A 963. The distribution is remarkably similar for these three clusters of compa...
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We recover the luminosity distributions over a wide range of absolute magnitude (−24.5 < MR < −16.5) for a sample of seven rich southern galaxy clusters. We find a large variation in the ratio of dwarf to giant galaxies, DGR: 0.8 ≤ DGR ≤ 3.1. This variation is shown to be inconsistent with a ubiquitous cluster luminosity function. The DGR shows a smaller variation from cluster to cluster in the...
متن کاملLuminosity Distributions within Rich Clusters - II: Demonstration and Verification via Simulation
We present detailed simulations of long exposure CCD images. The simulations are used to explore the validity of the statistical method for reconstructing the luminosity distribution of galaxies within a rich cluster i.e. by the subtraction of field number-counts from those of a sight-line through the cluster. In particular we use the simulations to establish the reliability of our observationa...
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We present the K-band (2.2 μ) luminosity functions of the X-ray luminous clusters MS1054−0321 (z = 0.823), MS0451−0305 (z = 0.55), Abell 963 (z = 0.206), Abell 665 (z = 0.182) and Abell 1795 (z = 0.063) down to absolute magnitudes MK = −20. Our measurements probe fainter absolute magnitudes than do any previous studies of the nearinfrared luminosity function of clusters. All the clusters are fo...
متن کاملAxions and the white dwarf luminosity function
The evolution of white dwarfs can be described as a simple cooling process. Recently, it has been possible to determine with an unprecedented precision their luminosity function, that is, the number of stars per unit volume and luminosity interval. Since the shape of the bright branch of this function is only sensitive to the average cooling rate, we use this property to check the possible exis...
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ژورنال
عنوان ژورنال: Monthly Notices of the Royal Astronomical Society
سال: 1997
ISSN: 0035-8711,1365-2966
DOI: 10.1093/mnras/287.2.415