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Topic: Luminosity function

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	Luminosity function - Wikipedia, the free encyclopedia
		The luminosity function is a standard function established by the Commission Internationale de l'Éclairage to account for the variable sensitivity of the human eye to radiation at different wavelengths.
		The standard luminosity function is normalized to a peak value of unity at 555 nm (see luminous coefficient).
		The CIE 1931 color-matching functions, which include the CIE 1924 photopic V(λ) luminosity function as the y function, have long been acknowledged to underestimate the contribution of the blue end of the spectrum to perceived luminance.
	en.wikipedia.org /wiki/Luminosity_function (440 words)

	GOLDMine: The UV luminosity function of ... (Site not responding. Last check: 2007-10-30)
		The UV luminosity function of nearby clusters of galaxies
		We present the UV composite luminosity function for galaxies in the Virgo, Coma and Abell 1367 clusters.
		The luminosity function (LF) is well fitted by a Schechter function with M(UV) - 5 log(h(75)=-20.75 +/- 0.40 and Alpha = -1.50 +/- 0.10 and does not differ significantly from the local UV luminosity function of the field.
	goldmine.mib.infn.it /papers/LF_UV.html (132 words)

	Probing the shape of the Globular Cluster Luminosity Function
		Local calibration of the luminosity function continues to be the main weakness of this distance indicator.
		If the picture of cluster evolution shaping the luminosity function (as first proposed in Fall and Ress 1977) is correct then there should be some variation in the shape of the GCLF when examined at different distances form the center of the host galaxy.
		Panel a) give the luminosity functions for the inner annulus and the background, b) is the inner lf after subtracting the background lf, ie.
	www.cfht.hawaii.edu /Reference/Proceedings/kavelaars/index.html (844 words)

	Local Luminosity Function
		The local stellar luminosity function, the absolute number of stars in the Solar neighbourhood as a function of intrinsic luminosity, is the outcome of the history of star formation, chemical evolution, dynamical evolution, stellar evolution, and any temporal evolution of the stellar initial mass function, throughout the history of the Milky Way.
		The stellar luminosity function is definable only in one way, by completion of an accurate census of all the stars in some volume of space.
		The solid model curve and the lower dotted model curve represent the same mass function: the differences between them are a manifestation of spatial resolution, and the very large Malmquist corrections necessary to convert pencil beam photometric parallax data to a luminosity function (see also Section 1.7.4).
	www.rssd.esa.int /SA-general/Projects/GAIA_files/LATEX2HTML/node61.html (791 words)

	The new X-ray Luminosity Function.
		Secondly the luminosities of the clusters not observed by the PSPC are corrected by the average increase measured (when not including MS0418.3-3844 and MS0353.6-3642).
		All the luminosities we have used to calculate the XLFs in figures 3.7 and 3.8 are based on an integration of the emission to infinity, as is the BCS XLF.
		The same data as in figure 3.8 are plotted, except that all the luminosities were reduced by 8%, to be consistent with the virial radius approximation used by Böhringer et al..
	www.aao.gov.au /local/www/sce/thesis/thesis/node38.html (744 words)

	The luminosity function of compact groups of galaxies (Site not responding. Last check: 2007-10-30)
		The luminosities of compact group galaxies are consistent with their being drawn from a Schechter luminosity function with {alpha} = -2^+0.8^_-0.9_, L* = 1.1 +/- 0.2 x 10^10^ h^-2^ L_Sun_ and PHI* = 1.3^+0.2^_-0.8_ h^3^/Mpc^3^ (99% confidence level).
		In particular, the luminosity function of HCG elliptical galaxies has a mean magnitude which is significantly brighter than the mean magnitude of Virgo cluster elliptical galaxies.
		The mean luminosity density of galaxies in compact groups is estimated to be 1.3^+0.1^_0.8_ x 10^6^ h L_Sun_ Mpc^-3^, which constitutes ~0.8% of the total luminosity density of galaxies in the universe.
	www.cs.wisc.edu /niagara/data/nasa/ApJ_380_30.xml (214 words)

	The evolution of the quasar luminosity function
		The quasar luminosity function is also derived by the redshift range 2.2
		When the data are combined with a new sample of bright quasars, the quasar luminosity functions in all four redshift ranges are consistent with a single power law of index {beta}=0.63.
		Plots of quasar space density as a function of redshift in three luminosity bins are also presented and show strong evolution at low redshift but nearly constant space density beyond a redshift of 2.
	www.cs.wisc.edu /niagara/data/nasa/MNRAS_275_1102.xml (176 words)

	The Luminosity Function Jump (Site not responding. Last check: 2007-10-30)
		The effect of this slowing of the cooling is a contribution to a jump in the luminosity function as the cooling curves pile up on top of one another.
		The resulting luminosity function is shown at left, binned in V.
		The model luminosity functions have been folded through the incompleteness function, as determined by artificial star tests.
	www.astro.ucla.edu /~hansen/choice3.html (294 words)

	QSO luminosity function. (Site not responding. Last check: 2007-10-30)
		The luminosity function gives the space density of QSOs as a function of their luminosity.
		Determination of this evolution has been hampered by the fact that the QSO luminosity function is very close to a power law.
		The best fit of a pure luminosity evolution model would indicate that either: a) Quasars are long lived phenomena and have been dimming systematically since the `quasar epoch' at redshift ~2, or b) Short lived quasars are being produced at the same rate but with progressively lower luminosities.
	www.roe.ac.uk /~jcm/thesis/node31.html (343 words)

	The Local Galaxy Luminosity Function
		Hence, the local luminosity function appeared to be flat.
		, the luminosity function was well-represented by a Schechter function with parameters
		13 exceeded the extrapolation of the Schechter function by a factor of 3
	www.ucolick.org /~simard/phd/root/node7.html (712 words)

	FIR Luminosity Function (Site not responding. Last check: 2007-10-30)
		Adopting the far infrared luminosity as a measure of the massive star formation rate, one finds that the IRAS data reveal a previously unsuspected population of early type (Sa-Sab) spirals with massive star formation rates that rival the most prodisously star forming Sc galaxies.
		The percentage of galaxies with 60 micron luminosities greater than L(lim) is plotted on the y-axis and the value of L(lim) is plotted on the x-axis.
		The luminosity functions are similar for spiral galaxies of types Sa-Scd, whereas the median 60 micron luminosity for the very early, S0-S0/a, and very late, Sd-Sdm, types is about one order of magnitude lower than the other spirals (Sa-Scd).
	earth.ast.smith.edu /shameed/LF.html (279 words)

	White Dwarf Luminosity Function of the Disk
		The luminosity function of white dwarfs at low luminosities, and especially the position of its cut-off, provides important information about the age of the Galactic disk.
		Knox et al.1999]): the distance to the lowest luminosity white dwarfs, the bolometric corrections, and the chemical composition of the outer layers (i.e., DA if hydrogen is present, or non-DA if hydrogen is absent).
		The contribution of the current observational uncertainties to the total error budget of the galactic age is as large as 2 Gyr.
	www.rssd.esa.int /SA-general/Projects/GAIA_files/LATEX2HTML/node77.html (290 words)

	Hickson Group Galaxy Luminosity Function
		Moreover, it is not yet clear whether the slope of the faint end of the luminosity function is dependent on the environment of the galaxies sampled.
		Because each group encompasses a wide range of galaxy luminosities, the shape of the resulting galaxy luminosity function is not sensitive to the details of the weighting procedure.
		The effect on the luminosity function can be significant, as we find that the average pairwise radius of the faint galaxies is about twice that of the bright galaxies.
	ecf.hq.eso.org /~ralbrech/sepdec97apjl/975387.html (3314 words)

	SDSS Luminosity Function
		(2001) published a luminosity function and the relationship of luminosity to other properties for a small amount of commissioning data.
		The points at which these files sample the fit luminosity function are very closely spaced, so there is no way the errors are independent.
		The uncertainties in luminosity for each galaxy are about 0.05 mag, so that is the minimum magnitude difference between independent samples.
	cosmo.nyu.edu /blanton/lf.html (644 words)

	[130.05] The Kuiper Belt Luminosity Function (Site not responding. Last check: 2007-10-30)
		The luminosity function of Kuiper Belt Objects (the number of KBOs brighter than R per square degree) reflects their underlying size and distance distributions.
		The size distribution is important for understanding accretion and collisional processes at work on these remnant planetesimals, and the radial distance distribution provides clues to the extent and density of the primordial solar nebula.
		We test the compatibility of the present data with a "broken" luminosity function, where the value of \alpha changes at faint magnitudes.
	www.aas.org /publications/baas/v34n4/aas201/898.htm (179 words)

	Luminosity Function for L > L* Galaxies
		Model and observed SEDs were reddened as a function of band and redshift to account for intervening absorption (only), as prescribed by Madau (1995).
		The luminosity functions of GH (in the range 3
		However, it is critical to discriminate between the SLY suggestion of a rising faint end of the luminosity function and the flatter faint end hinted at by the S96 data.
	ecf.hq.eso.org /~ralbrech/novdec97apjl/965819.html (3340 words)

	The X-ray Luminosity Function.
		The X-ray luminosity is much easier to measure than the X-ray temperature.
		Schechter (1976), originally proposed for the optical luminosity function of galaxies,
		The exact degree of evolution (if any) is unclear largely due to the small numbers of high redshift, high luminosity clusters in the surveys.
	www.aao.gov.au /local/www/sce/thesis/thesis/node25.html (276 words)

	Faint end Luminosity Function
		In a typical Luminosity Function (LF), the number of bright stars is not as large as the number of faint stars.
		The luminosity function is determined by (a.o.) the Initial Mass Function (IMF), the age, and the star formation history of the field of stars in question.
		In uncorrected magnitudes the raw luminosity function is as shown in the figure below.
	www.astro.lu.se /~ralph/lumfunc (1791 words)

	[24.01] Similarities and Differences in the Luminosity and Mass Functions of the Young Stellar Clusters NGC 2362 and IC ... (Site not responding. Last check: 2007-10-30)
		Using deep infrared surveys, we have constructed the Infrared Luminosity Functions of two young stellar clusters, IC 348 and NGC 2362.
		For both clusters, the derived luminosity function is complete from stars as massive as B type stars (10 M
		By comparing the two cluster luminosity functions and by using a suite of model luminosity functions, we show that the underlying stellar Mass Functions of these two clusters are quite similar despite the difference in their apparent star formation rates and the more significant O and B star content of NGC 2362.
	www.aas.org /publications/baas/v32n4/aas197/998.htm (155 words)

	Search and Luminosity Function of high-z (z>5) QSOs
		Over the past years, much observational effort has gone into the construction of complete samples of quasars in order to determine the luminosity function and its evolution with redshift.
		The form of the evolution at these redshifts is less clear than at lower redshifts, and it appears that a combination of luminosity evolution and density evolution is taking place.
		quasars and the estimate of their luminosity function is essentially a technical one: at
	www.mporzio.astro.it /WFI-LBT/biocamlbt/node34.html (470 words)

	UvA DARE (Site not responding. Last check: 2007-10-30)
		We examine the width of the gamma-ray burst (GRB) luminosity function through the distribution of GRB peak count rates, Cpeak, as detected by Burst and Transient Source Experiment (BATSE) (1993).
		In the context of Galactic corona spatial distribution models, we attempt to place constaints on the characteristic width of the luminosity function by comparing the observed intensity distribution with those produced by a range of density and luminosity functions.
		However, the distribution of intrinsic luminosities of detected bursts can be limited: we find that most observed bursts have luminosities that are in a range of one to two decades, but a significant population of undetected less luminous bursts cannot be excluded.
	dare.uva.nl /record/135242 (224 words)

	The Luminosity Function of Individually Undetectable Stars - Snel (ResearchIndex) (Site not responding. Last check: 2007-10-30)
		A method is presented to derive the faint end of the stellar luminosity function in crowded fields.
		A simulated image with known luminosity function is compared with an observed image, and the luminosity function is adjusted until the images look sufficiently similar.
		Snel, R., (1997), The luminosity function of individually undetectable stars, in prep.
	citeseer.ist.psu.edu /193111.html (276 words)

	Revised luminosity function parameters
		are the normalisation of the number of galaxies per unit volume, the index of the faint-end slope, and the characteristic luminosity, respectively.
		Of particular interest to the LF are elliptical and lenticular (E/S0) galaxies, which dominate the contribution to lensing statistics (Maoz and Rix 1993).
		The lensing probability can then be computed as a function of the LF parameters.
	www.stanford.edu /~dorris/research/paper1/node18.html (318 words)

	Planetary Nebula Luminosity Functions (Site not responding. Last check: 2007-10-30)
		Planetary Nebulae have very repeatable luminosity distributions, and this uniformity is the key to the technique.
		The luminosity function for planetary nebulae in the nearby Andromeda Galaxy (M31).
		Notice that the function drops to zero very sharply at the bright (left) end of the distribution.
	www.noao.edu /jacoby/pnlf/pnlf.html (137 words)

	Luminosity Function
		The luminosity function of the Kuiper belt has, until recently, not been well constrained near
		Using the data from this survey and previous work, new constraints were determined on the luminosity function of the Kuiper belt near
		(1998) indicate that a break in the luminosity of the Kuiper Belt is not required unless the photographic survey by Kowal (1989) had a high detection efficiency to the limiting magnitude stated by Kowal or Irwin et al.
	www.atnf.csiro.au /pasa/15_2/brown/paper/node3.html (312 words)

	Photopic luminosity function (Site not responding. Last check: 2007-10-30)
		The standard photopic luminosity function is based on a curious combination of luminosity data from several sources and obtained by several methods (Gibson and Tyndall, 1923; CIE, 1926).
		The uncertainty surrounding it is illustrated by the fact that the values from the different studies that were averaged to define it diverged by as much as a factor of ten in the violet (CIE, 1926; Le Grand, 1968).
		The function seriously underestimates sensitivity at short wavelengths.
	cvision.ucsd.edu /database/text/lum/vl.htm (117 words)

	The HI Luminosity Function from ``Blind'' Surveys
		Recent neutral hydrogen (HI) surveys are detecting enough sources to make initial predictions of the extragalactic HI luminosity function.
		I suggest several procedures for determining the effective sensitivity of HI surveys.
		Applied to two recent Arecibo surveys, these suggest that the HI luminosity function may be much steeper than its optical counterpart, and that the Parkes surveys may detect a large number of low-mass sources.
	www.atnf.csiro.au /pasa/14_1/schneider/paper (136 words)

	The luminosity function of ultracool dwarfs (Site not responding. Last check: 2007-10-30)
		With this dataset, we present the first robust measurement of the luminosity function of objects that span the stellar/brown dwarf boundary.
		In addition, we have doubled the number of ultracool dwarfs known within 20 pc.
		I will describe these results, summarize its implications on the mass function, and discuss the prospects for the future.
	www.hs.uni-hamburg.de /cs13/abstract16.html (84 words)

	The K-Band Galaxy Luminosity Function (ResearchIndex) (Site not responding. Last check: 2007-10-30)
		If your firewall is blocking outgoing connections to port 3125, you can use these links to download local copies.
		Abstract: We measured the K-band luminosity function using a complete sample of 4192 morphologically-typed 2MASS galaxies with Ks = 20 mag/arcsec 2 isophotal magnitudes 7 !
		\Gamma0:5) galaxies have similarly shaped luminosity functions, ff e = \Gamma0:92 \Sigma 0:10 and ff l = \Gamma0:87 \Sigma 0:09.
	citeseer.ist.psu.edu /422801.html (195 words)

	Find in a Library: The nearby stars and the stellar luminosity function
		The nearby stars and the stellar luminosity function
		To find this item in a library, enter a postal code, state, province, or country in the field above.
		WorldCat is provided by OCLC Online Computer Library Center, Inc. on behalf of its member libraries.
	worldcatlibraries.org /wcpa/ow/13a6f4e9e932692da19afeb4da09e526.html (74 words)

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