An analytic expression for the luminosity function for galaxies.

Schechter, Paul L.

doi:10.1086/154079

Cited by 2,750 publications

(2,635 citation statements)

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“…More massive or more luminous galaxies are more strongly clustered because they reside in more massive halos that have higher b h (M ). At low redshift, the large scale bias factor is b g ≤ 1 for galaxies below the characteristic cutoff L * of the Schechter (1976) luminosity function, but it rises sharply at higher luminosities Zehavi et al, 2005Zehavi et al, , 2011.…”

Section: Cmb Anisotropies and Large Scale Structurementioning

confidence: 95%

Observational probes of cosmic acceleration

et al. 2013

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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Section: Cmb Anisotropies and Large Scale Structurementioning

confidence: 95%

Observational probes of cosmic acceleration

et al. 2013

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“…A word of caution is needed as regards the third assumption, however. Larsen (2006) argued for a truncated cluster initial mass function, which can be parametrized well using a Schechter function (Schechter 1976) as demonstrated by Gieles (2009). The tentative current upper-mass limit is ∼ 10 5 M for our Galaxy, well above the mass bin that we use for normalization, so it is likely to have a negligible effect on our estimates.…”

Section: Total Number Of Milky Way Clustersmentioning

confidence: 66%

Infrared surveys of Galactic star clusters

Ivanov¹,

Messineo²,

Zhu³

et al. 2009

Proc. IAU

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Abstract. Many attempts have been made to carry out a complete observational census of Milky Way star clusters based on recent near-and mid-infrared surveys. However, more clusters are still being discovered, indicating that existing catalogs are incomplete. We attempt to estimate the total number of supermassive (SM; M cl 10 4 M ) clusters in the Galaxy, and to improve the yield from the automated cluster searches. Assuming that the 'local' census of SM clusters is complete, and that their surface density accross the disk follows that of the stars, we predict that the Milky Way contains 81 ± 21 SM clusters. We apply a cluster-detection algorithm to the 2mass Point Source Catalog after a preliminary color and/or magnitude selection of the point sources to improves the surface-density cluster-to-field contrast. Our algorithm identified 94 new candidates, and re-identified 34 known clusters. During the visual inspection, we detected an additional 41 new candidates, and re-identified 32 known objects. Preliminary characterization suggests that the new list may contain red-supergiant, open and globular clusters.

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“…The meaning of symbols and lines is the same as in Fig. 1. the bulge component follows a Schechter function (Schechter 1976) with a sharp decrease of the density at faint magnitudes, the LF of the disk component is clearly incomplete below the magnitude limit of the survey. Since the capability to measure the flux in disks is strongly limited by the low surface brightness, this incompleteness is large.…”

Section: Resultsmentioning

confidence: 88%

Where is the Light? Tracing the Evolution of Bulges and Disks since z ~ 0.8

Tasca

Tresse

2010

Proc. IAU

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Abstract. The chronology of galactic bulge and disk formation is studied by analysing the relative contributions of these components to the B band rest-frame luminosity density (LD) at two different cosmological epochs. The luminosity function (LF) of the bulge and disk components at z ∼ 0.8 is computed on a galaxy subsample of the final zCOSMOS "bright" catalogue of roughly 20,000 objects with spectroscopic redshift in the COSMOS field. The comparison is then performed on galaxies in the local universe. Our preliminary results show that the LD in the disk component strongly decreases from ∼ 80% at z ∼ 0.8 to ∼ 50% at z = 0, the bulges having a specular behaviour. The observational constraints provided in this work are aimed to discriminate among competing scenarios of galaxy formation and evolution. An appropriate comparison with hydrodynamical semianalytical models will be considered in a future study to understand further the formation and evolution of galaxies.

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An analytic expression for the luminosity function for galaxies.

Cited by 2,750 publications

References 0 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

Infrared surveys of Galactic star clusters

Where is the Light? Tracing the Evolution of Bulges and Disks since z ~ 0.8

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