Galaxy luminosity function: a new analytic expression

Alcaniz, J. S.; Lima, J. A. S.

doi:10.1590/s0103-97332004000300026

Cited by 8 publications

(11 citation statements)

References 17 publications

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“…Alcaniz & Lima 2004) collapses when ξ = 0 Luminosity functions of the {L i } i=20 i=1 groups ordered by increasing arc-length (blue triangles with a dashed line fit from…”

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confidence: 99%

Single Parameter Galaxy Classification: The Principal Curve Through the Multi-Dimensional Space of Galaxy Properties

Taghizadeh-Popp

Heinis

Szalay

2012

ApJ

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We propose to describe the variety of galaxies from the Sloan Digital Sky Survey (SDSS) by using only one affine parameter. To this aim, we construct the Principal Curve (P-curve) passing through the spine of the data point cloud, considering the eigenspace derived from Principal Component Analysis (PCA) of morphological, physical and photometric galaxy properties. Thus, galaxies can be labeled, ranked and classified by a single arc length value of the curve, measured at the unique closest projection of the data points on the P-curve. We find that the P-curve has a "W" letter shape with 3 turning points, defining 4 branches that represent distinct galaxy populations. This behavior is controlled mainly by two properties, namely u − r and SF R (from blue young at low arc length to red old at high arc length), while most of other properties correlate well with these two. We further present the variations of several important galaxy properties as a function of arc length. Luminosity functions variate from steep Schechter fits at low arc length, to double power law and ending in Log-normal fits at high arc length. Galaxy clustering shows increasing autocorrelation power at large scales as arc length increases. Cross correlation of galaxies with different arc lengths shows that the probability of 2 galaxies belonging to the same halo decreases as their distance in arc length increases.PCA analysis allowed to find peculiar galaxy populations located apart from the main cloud of data points, such as small red galaxies dominated by a disk, of relatively high stellar mass-to-light ratio and surface mass density. On the other hand, the P-curve helped understanding the average trends, encoding 75% of the available information in the data.The P-curve allows not only dimensionality reduction, but also provides supporting evidence for relevant physical models and scenarios in extragalactic astronomy: 1) Evidence for the hierarchical merging scenario in the formation of a selected group of red massive galaxies. These galaxies present a log-normal r-band luminosity function, which might arise from multiplicative processes involved in this scenario.2) Connection between the onset of AGN activity and star formation quenching as mentioned in Martin et al. (2007), which appears in green galaxies when transitioning from blue to red populations.

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“…Alcaniz & Lima 2004) collapses when ξ = 0 Luminosity functions of the {L i } i=20 i=1 groups ordered by increasing arc-length (blue triangles with a dashed line fit from…”

mentioning

confidence: 99%

Single Parameter Galaxy Classification: The Principal Curve Through the Multi-Dimensional Space of Galaxy Properties

Taghizadeh-Popp

Heinis

Szalay

2012

ApJ

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“…The numerical exploration of a new LF for galaxies requires that the χ 2 red is smaller or approximately equal to that of the Schechter LF. As an example, the LF given by the generalized gamma distribution with four parameters gives χ 2 red smaller than that of the Schechter LF in the five bands of the Sloan Digital Sky Survey (SDSS) galaxies, see equation (21) an Table II in [42]…”

Section: The Schechter Functionmentioning

confidence: 99%

“…Over the years, other LFs for galaxies have been suggested, such as a two-component Schechter-like LF, see [18], the hybrid Schechter+power-law LF to fit the faint end of the K-band, see [19], and the double Schechter LF, see [20]. To improve the flexibility at the bright end, a new parameter η was introduced in the Schechter LF, see [21]. A third astrophysical application is in the photometric maximum visible in the number of cluster of galaxies as function of the redshift; for example, see Figure 7 in [22] where the number of galaxies as function of the redshift is plotted and Figure 2 in [23] where the number of clusters for three catalogs are reported as function of the redshift.…”

Section: Introductionmentioning

confidence: 99%

The Truncated Lindley Distribution with Applications in Astrophysics

Zaninetti¹

2019

Galaxies

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This paper reviews the Lindley distribution and then introduces the scale and the double truncation. The unknown parameters of the truncated Lindley distribution are evaluated with the maximum likelihood estimators. An application of the Lindley distribution with scale is done to the initial mass function for stars. The magnitude version of the Lindley distribution with scale is applied to the luminosity function for the Sloan Digital Sky Survey (SDSS) galaxies and to the photometric maximum of the 2MASS Redshift Survey (2MRS) galaxies. The truncated Lindley luminosity function allows us to model the Malquist bias of the 2MRS galaxies.

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“…The χ 2 and χ 2 red are smaller in five bands over five in respect to those of the Schechter LF. This goodness of fit is due to the flexibility introduced by the fourth parameter η as outlined in [27].…”

Section: Goodness Of Fit Testsmentioning

confidence: 99%

The Luminosity Function of Galaxies as Modeled by a Left Truncated Beta Distribution

Zaninetti¹

2014

IJAA

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A first new luminosity functions of galaxies can be built starting from a left truncated beta probability density function , which is characterized by four parameters. In the astrophysical conversion, the number of parameters increases by one, due to the addition of the overall density of galaxies. A second new galaxy luminosity function is built starting from a left truncated beta probability for the mass of galaxies once a simple nonlinear relationship between mass and luminosity is assumed; in this case the number of parameters is six because the overall density of galaxies and a parameter that regulates mass and luminosity are added. The two new galaxy luminosity functions with finite boundaries were tested on the Sloan Digital Sky Survey (SDSS) in five different bands; the results produce a "better fit" than the Schechter luminosity function in two of the five bands considered. A modified Schechter luminosity function with four parameters has been also analyzed.

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Galaxy luminosity function: a new analytic expression

Cited by 8 publications

References 17 publications

Single Parameter Galaxy Classification: The Principal Curve Through the Multi-Dimensional Space of Galaxy Properties

Single Parameter Galaxy Classification: The Principal Curve Through the Multi-Dimensional Space of Galaxy Properties

The Truncated Lindley Distribution with Applications in Astrophysics

The Luminosity Function of Galaxies as Modeled by a Left Truncated Beta Distribution

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