The Galaxian Luminosity Function

Kiang, T.

doi:10.1093/mnras/122.3.263

Cited by 44 publications

(16 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Some values of R are now reported: R 20 by Kiang (1961) and Persic & Salucci (1992), R = 20 by Padmanabhan (1996), R = 5.93 by van der Marel (1991). Later, Bell & de Jong (2001) (amongst others) demonstrated that M/L varies as a function of galaxy color, and therefore type.…”

Section: The Case Of Galaxiesmentioning

confidence: 93%

“…This function was suggested by Schechter (1976) in order to substitute other analytical expressions, see for example Formula (3) in Kiang (1961). Over the years this function has also been applied to describe physical quantities related to the optical luminosity, such as the CO luminosity for galaxies (Keres et al 2003) and the baryonic mass function of galaxies (Bell et al 2003a).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

A New Luminosity Function for Galaxies as Given by the Mass-Luminosity Relationship

Zaninetti¹

2008

The Astronomical Journal

View full text Add to dashboard Cite

The search for a luminosity function for galaxies both alternative or companion to a Schechter function is a key problem in the reduction of data from catalogs of galaxies. Two luminosity functions for galaxies can be built starting from two distributions of mass as given by the fragmentation. A first overall distribution function is the Kiang function, which represents a useful description of the area and volume distribution of the Poisson Voronoi diagrams. The second distribution, which covers the case of low-mass galaxies, is the truncated Pareto distribution: in this model we have a natural bound due to the minimum mass/luminosity observed and an upper bound (function of the considered environment) represented by the boundary with the observed mass/luminosity overall behavior. The mass distribution is then converted into a luminosity distribution through a standard mass-luminosity relationship. The mathematical rules to convert the probability density function are used and the two new functions are normalized to the total number of galaxies per unit volume. The test of the two new luminosity functions for galaxies that cover different ranges in magnitude was made on the Sloan Digital Sky Survey (SDSS) in five different bands; the results are comparable to those of the Schechter function. A new parameter, which indicates the stellar content, is derived. The joint distribution in redshift and flux, the mean redshift and the number density connected with the first luminosity function for galaxies are obtained by analogy with the Schechter function. A new formula, which allows us to express the mass as a function of the absolute magnitude, is derived.

show abstract

Section: The Case Of Galaxiesmentioning

confidence: 93%

Section: Introductionmentioning

confidence: 99%

A New Luminosity Function for Galaxies as Given by the Mass-Luminosity Relationship

Zaninetti¹

2008

The Astronomical Journal

View full text Add to dashboard Cite

show abstract

“…The local density of ordinary galaxies in space is ~3x 10" 2 Mpc" 3 if # 0 = 75 Mpc" 3 (Sandage, 1965;cf. van den Bergh, 1961;Kiang, 1961). * Using %R H as the effective 'cosmological' superposition radius, we find that the 1-10 keV integrated intensity due to ordinary galaxies should be /(erg cm" 2 s" 1 sr" 1 ) ~ ~ 2.4 x 10" 9 .…”

Section: Mainstream X-rays: Isotropic Componentmentioning

confidence: 91%

‘Local’ Theories of the X-Ray Background

Felten

1973

Symp. - Int. Astron. Union

View full text Add to dashboard Cite

Abstract. Recent theories of the origins of diffuse-background X-rays are reviewed, with emphasis on theories of the soft flux in the galactic plane and at the poles. This is probably partly galactic and partly extragalactic in origin. Failure to observe absorption by the Small Magellanic Cloud and by galactic gas in neighboring directions may be due to sources in the Cloud and to statistical fluctua tions in galactic emission and absorption. Several models for numerous low-luminosity sources in the Galaxy are available. True 'diffuse' emission seems unnecessary. Absorption by Galactic gas seems to agree roughly with theory. The soft extragalactic component may arise in a hot intergalac tic medium.The existence of a 'diffuse' galactic-plane excess in 1-100 keV is in some doubt. Low-luminosity sources may contribute to this as well.For isotropic X-rays in 1 keV -1 MeV, superposition theories involving clusters of galaxies, Seyfert galaxies, etc. over a cosmological path length are now roughly viable. Simple 'metagalactic' Compton theories seem excluded if the break at 40 keV is sharp, but this is now in doubt. A very hot intergalactic medium at x 10 8 K would give the possibility of a sharp break. A recent upper limit on the line source strength of 100-MeV photons in the galactic plane may create some difficulties for cosmic-ray theory. The spectral shape of n-y photons has become a matter of theoretical dispute.

show abstract

“…Over the years, many attempts have been done for determining the shape of the GLF (Zwicky 1957;Kiang 1961;Abell 1965;Arakelyan & Kalloglyan 1975). Such studies culminated with an elegant analytic form proposed by Schechter (1976) which nowadays is usually referred to as the general Schechter luminosity function.…”

mentioning

confidence: 99%

Galaxy luminosity function: a new analytic expression

Alcaniz

Lima

2004

Braz. J. Phys.

View full text Add to dashboard Cite

We propose a new analytic approximation for the luminosity function of galaxies. The suggested expression behaves like the Schechter function at the faint end (φ ∼ L α ) but departs considerably at the bright end (L >> L * ). We argue here that such a behavior may provide a better fit for the current observational data than does the Schechter function. Its practical interest is stressed by considering roughly the data set provided by the Stromlo-APM redshift survey. Implications on the estimates of the matter density parameter from mass-to-light ratio are also briefly discussed.The galaxy luminosity function (GLF) is a key quantity for any study of galaxy evolution and one of the most important astrophysical tools in practical cosmology. It describes the distribution of galaxies with different intrinsic luminosities L (or magnitudes M ), and since the main source of data coming from the distant past is provided by the light emitted (or scattered) by ordinary matter, the GLF also supplies the primary information about the baryonic content of the Universe.Over the years, many attempts have been done for determining the shape of the GLF (Zwicky

show abstract

The Galaxian Luminosity Function

Cited by 44 publications

References 0 publications

A New Luminosity Function for Galaxies as Given by the Mass-Luminosity Relationship

A New Luminosity Function for Galaxies as Given by the Mass-Luminosity Relationship

‘Local’ Theories of the X-Ray Background

Galaxy luminosity function: a new analytic expression

Contact Info

Product

Resources

About