The K-Band Luminosity Function of Galaxies

1998 ◽  
Vol 179 ◽  
pp. 278-280
Author(s):  
J. P. Gardner ◽  
R. M. Sharples ◽  
C. S. Frenk ◽  
B. E. Carrasco
Keyword(s):  
Luminosity Function ◽  
Near Infrared ◽  
Mass Function ◽  
Solar Mass ◽  
The Galaxy ◽  
Statistical Studies ◽  
The Absolute ◽  
Number Counts ◽  
Luminosity Evolution ◽  
K Band

The luminosity function of galaxies is central to many problems in cosmology, including the interpretation of faint number counts. The near-infrared provides several advantages over the optical for statistical studies of galaxies, including smooth and well-understood K-corrections and expected luminosity evolution. The K–band is dominated by near-solar mass stars which make up the bulk of the galaxy. The absolute K magnitude is a measure of the visible mass in a galaxy, and thus the K–band luminosity function is an observational counterpart of the mass function of galaxies.

DARK MATTER IN SPIRAL HALOS AND THE HALO MASS FUNCTION

1994 ◽  
Vol 03 (supp01) ◽  
pp. 87-92
Author(s):  
KEITH M. ASHMAN ◽  
PAOLO SALUCCI ◽  
MASSIMO PERSIC
Keyword(s):  
Dark Matter ◽  
Hierarchical Clustering ◽  
Galaxy Formation ◽  
Luminosity Function ◽  
Mass Function ◽  
Dark Halo ◽  
Constant Mass ◽  
High Luminosity ◽  
The Galaxy ◽  
Galaxy Luminosity Function

Evidence that low-luminosity spirals have a higher dark matter fraction than their high-luminosity counterparts is discussed. The empirical correlation between dark matter fraction and luminosity is used, in conjunction with the galaxy luminosity function of spirals, to derive the dark halo mass function of these galaxies. The mass function is shown to be consistent with hierarchical clustering models of galaxy formation. This contrasts with previous results based on the assumption of a constant mass-to-light ratio for all spirals, which predict too many low-luminosity galaxies.

scholarly journals Virial Halo Mass Function in the Planck Cosmology

2021 ◽  
Vol 922 (1) ◽  
pp. 89
Author(s):  
Masato Shirasaki ◽  
Tomoaki Ishiyama ◽  
Shin’ichiro Ando
Keyword(s):  
Luminosity Function ◽  
Mass Function ◽  
Number Density ◽  
Baseline Model ◽  
Wide Range ◽  
Halo Masses ◽  
Number Counts ◽  
Mass Functions ◽  
Analytic Prediction ◽  
Fitting Parameters

Abstract We study halo mass functions with high-resolution N-body simulations under a ΛCDM cosmology. Our simulations adopt the cosmological model that is consistent with recent measurements of the cosmic microwave backgrounds with the Planck satellite. We calibrate the halo mass functions for 108.5 ≲ M vir/(h −1 M ⊙) ≲ 1015.0–0.45 z , where M vir is the virial spherical-overdensity mass and redshift z ranges from 0 to 7. The halo mass function in our simulations can be fitted by a four-parameter model over a wide range of halo masses and redshifts, while we require some redshift evolution of the fitting parameters. Our new fitting formula of the mass function has a 5%-level precision, except for the highest masses at z ≤ 7. Our model predicts that the analytic prediction in Sheth & Tormen would overestimate the halo abundance at z = 6 with M vir = 108.5–10 h −1 M ⊙ by 20%–30%. Our calibrated halo mass function provides a baseline model to constrain warm dark matter (WDM) by high-z galaxy number counts. We compare a cumulative luminosity function of galaxies at z = 6 with the total halo abundance based on our model and a recently proposed WDM correction. We find that WDM with its mass lighter than 2.71 keV is incompatible with the observed galaxy number density at a 2σ confidence level.

scholarly journals The ALPINE-ALMA [CII] survey

2020 ◽  
Vol 643 ◽  
pp. A8 ◽  
Author(s):  
C. Gruppioni ◽  
M. Béthermin ◽  
F. Loiacono ◽  
O. Le Fèvre ◽  
P. Capak ◽  
...  
Keyword(s):  
Star Formation ◽  
Luminosity Function ◽  
Near Infrared ◽  
Formation Rate ◽  
Ultra Violet ◽  
Far Infrared ◽  
Mass Function ◽  
High Mass ◽  
Near Ir ◽  
Dusty Galaxies

Aims. We present the detailed characterisation of a sample of 56 sources serendipitously detected in ALMA band 7 as part of the ALMA Large Program to INvestigate CII at Early Times (ALPINE). These sources, detected in COSMOS and ECDFS, have been used to derive the total infrared luminosity function (LF) and to estimate the cosmic star formation rate density (SFRD) up to z ≃ 6. Methods. We looked for counterparts of the ALMA sources in all the available multi-wavelength (from HST to VLA) and photometric redshift catalogues. We also made use of deeper UltraVISTA and Spitzer source lists and maps to identify optically dark sources with no matches in the public catalogues. We used the sources with estimated redshifts to derive the 250 μm rest-frame and total infrared (8–1000 μm) LFs from z ≃ 0.5 to 6. Results. Our ALMA blind survey (860 μm flux density range: ∼0.3–12.5 mJy) allows us to further push the study of the nature and evolution of dusty galaxies at high-z, identifying luminous and massive sources to redshifts and faint luminosities never probed before by any far-infrared surveys. The ALPINE data are the first ones to sample the faint end of the infrared LF, showing little evolution from z ≃ 2.5 to z ≃ 6, and a “flat” slope up to the highest redshifts (i.e. 4.5 <  z <  6). The SFRD obtained by integrating the luminosity function remains almost constant between z ≃ 2 and z ≃ 6, and significantly higher than the optical or ultra-violet derivations, showing a significant contribution of dusty galaxies and obscured star formation at high-z. About 14% of all the ALPINE serendipitous continuum sources are found to be optically and near-infrared (near-IR) dark (to a depth Ks ∼ 24.9 mag). Six show a counterpart only in the mid-IR and no HST or near-IR identification, while two are detected as [C II] emitters at z ≃ 5. The six HST+near-IR dark galaxies with mid-IR counterparts are found to contribute about 17% of the total SFRD at z ≃ 5 and to dominate the high-mass end of the stellar mass function at z >  3.

scholarly journals Magnification and evolution biases in large-scale structure surveys

2021 ◽  
Vol 2021 (12) ◽  
pp. 009
Author(s):  
Roy Maartens ◽  
José Fonseca ◽  
Stefano Camera ◽  
Sheean Jolicoeur ◽  
Jan-Albert Viljoen ◽  
...  
Keyword(s):  
Luminosity Function ◽  
Large Scale ◽  
Near Infrared ◽  
Physical Change ◽  
Number Density ◽  
Galaxy Surveys ◽  
Intensity Mapping ◽  
The Galaxy ◽  
Infrared Wavelengths ◽  
Derivatives Of

Abstract Measurements of galaxy clustering in upcoming surveys such as those planned for the Euclid and Roman satellites, and the SKA Observatory, will be sensitive to distortions from lensing magnification and Doppler effects, beyond the standard redshift-space distortions. The amplitude of these contributions depends sensitively on magnification bias and evolution bias in the galaxy number density. Magnification bias quantifies the change in the observed number of galaxies gained or lost by lensing magnification, while evolution bias quantifies the physical change in the galaxy number density relative to the conserved case. These biases are given by derivatives of the number density, and consequently are very sensitive to the form of the luminosity function. We give a careful derivation of the magnification and evolution biases, clarifying a number of results in the literature. We then examine the biases for a variety of surveys, encompassing galaxy surveys and line intensity mapping at radio and optical/near-infrared wavelengths.

scholarly journals K Band Galaxy Counts in the South Galactic Pole Region

1999 ◽  
Vol 183 ◽  
pp. 257-257
Author(s):  
T. Minezaki ◽  
Y. Kobayashi ◽  
Y. Yoshii ◽  
B. A. Peterson
Keyword(s):  
Survey Area ◽  
The South ◽  
The Galaxy ◽  
Similar Area ◽  
Large Survey ◽  
Number Counts ◽  
Band Survey ◽  
K Band

We carried out a K′ band survey during August and September, 1994, in the south galactic pole region that covers 180.8 arcmin2 to K = 19 and 2.21 arcmin2 to K = 21 by the ANU 2.3 m telescope at SSO, Australia, equipped with PICNIC, developed at NAOJ. New galaxy number counts from K = 13 to 22 were obtained, which provided the best determination of the galaxy counts from K = 17.5 to 19.0 because of our large survey area. They were very consistent with Gardner, Cowie, & Wainscoat (1993, ApJL, 415, 9) and other observations to K < 19, however, they were larger than the galaxy counts of Saracco et al. (1997, AJ, 114, 887) with similar area and depth of survey around that magnitudes.

scholarly journals The faint-end of galaxy luminosity functions at the Epoch of Reionization

2017 ◽  
Vol 12 (S333) ◽  
pp. 52-55
Author(s):  
B. Yue ◽  
M. Castellano ◽  
A. Ferrara ◽  
A. Fontana ◽  
E. Merlin ◽  
...  
Keyword(s):  
Star Formation ◽  
Formation Process ◽  
Luminosity Function ◽  
Feedback Effects ◽  
Circular Velocity ◽  
Luminosity Functions ◽  
The Galaxy ◽  
Turn Over ◽  
Number Counts ◽  
Galaxy Luminosity Function

AbstractDuring the Epoch of Reionization (EoR), feedback effects reduce the efficiency of star formation process in small halos or even fully quench it. The galaxy luminosity function (LF) may then turn over at the faint-end. We analyze the number counts of z > 5 galaxies observed in the fields of four Frontier Fields (FFs) clusters and obtain constraints on the LF faint-end: for the turn-over magnitude at z ∼ 6, MUVT ≳-13.3; for the circular velocity threshold of quenching star formation process, vc* ≲ 47 km s−1. We have not yet found significant evidence of the presence of feedback effects suppressing the star formation in small galaxies.

scholarly journals The Luminosity Function of Galaxies in Some Nearby Clusters

2021 ◽  
Vol 5 (2) ◽  
pp. 1-10
Author(s):  
Mariwan Ahmed Rasheed ◽  
Khalid K. Mohammad
Keyword(s):  
Luminosity Function ◽  
Velocity Dispersion ◽  
Absolute Magnitude ◽  
Normalization Constant ◽  
Minimization Method ◽  
Redshift Range ◽  
Magnitude Distribution ◽  
The Galaxy ◽  
The Absolute ◽  
Galaxy Luminosity Function

In the present work, the galaxy luminosity function (LF) has been studied for a sample of seven clusters in the redshift range (0.0 ≲ z ≲ 0.1), within Abell radius (1.5 h−1 Mpc), in the five SDSS passbands ugriz. In each case, the absolute magnitude distribution is found and then fitted with a Schechter function. The fitting is done, using the χ2 – minimization method to find the best values of Schechter parameters Ф* (normalization constant), M* (characteristic absolute magnitude), and α (faint-end slope). No remarkable changes are found in the values of M* and α, for any cluster, in any passband. Furthermore, the LF does not seem to vary with such cluster parameters as richness, velocity dispersion, and Bautz–Morgan morphology. Finally, it is found that M* becomes brighter toward redder bands, whereas almost no variation is seen in the value of α with passband, being around (−1.00).

scholarly journals GAMA: a new galaxy survey

2007 ◽  
Vol 3 (S245) ◽  
pp. 83-84 ◽  
Author(s):  
I. Baldry ◽  
J. Liske ◽  
S. P. Driver ◽  
Keyword(s):  
Cold Dark Matter ◽  
Mass Function ◽  
Cold Dark Matter Model ◽  
The Galaxy ◽  
Low Mass ◽  
Statistical Studies ◽  
Resolution Imaging ◽  
Merger Rate ◽  
The Relationship ◽  
Dark Matter Model

AbstractThe case is outlined for a new galaxy survey, including spectroscopy with AAOmega and sub-arcsecond multi-band imaging, that bridges a crucial gap between the SDSS and VVDS surveys. The science focus is to study structure and the relationship between matter and light on kpc-to-Mpc scales. The range of scales probed will enable direct constraints on the Cold Dark Matter model by: (1) measuring the halo mass function down to $10^{12}{\cal M}_{\odot}$ and its evolution to z ~ 0.4; (2) measuring the galaxy stellar mass function to very low mass limits of $10^{7}{\cal M}_{\odot}$ constraining baryonic feedback processes; and (3) quantifying the environment-dependent merger rate since z ~ 0.4. Here, we highlight the fact that the high-resolution imaging will enable the bulge-disk decomposition of ~200000 galaxies in u–K, providing a valuable resource for statistical studies of bulge properties.

scholarly journals Securing the Faint End of the Galaxy Luminosity Function

2004 ◽  
Vol 21 (4) ◽  
pp. 356-359 ◽  
Author(s):  
Helmut Jerjen ◽  
Brent Tully ◽  
Neil Trentham
Keyword(s):  
Surface Brightness ◽  
Luminosity Function ◽  
Dwarf Galaxy ◽  
Full Range ◽  
Mass Function ◽  
Wide Field ◽  
Distance Information ◽  
The Galaxy ◽  
Brightness Fluctuation ◽  
Galaxy Luminosity Function

AbstractThe history of the formation of galaxies must leave an imprint in the properties of the mass function of collapsed objects and in its observational manifestation, the galaxy luminosity function. At present the faint end of the luminosity function is poorly known. Accurate knowledge of the luminosity function over the full range of galaxy clustering scales would provide serious constraints on both initial cosmological conditions and modulating astrophysical processes.Wide field imaging surveys with large ground-based telescopes now provide the capability to identify dwarf galaxy candidates to very faint levels (μR ≈ 26 mag arcsec–2), too low in surface brightness for spectroscopy (measuring redshifts) even with telescopes like Keck. Other means have to be explored to get distance information for these candidates in order to separate cluster members from back/foreground systems beyond doubt. On the quest to establish the properties (slope and possible turning point) of the the faint end of the galaxy luminosity function we are employing the surface brightness fluctuation (SBF) method to determine adequate distances, potentially resulting in the best definition ever of the luminosity function to MR ≈ –11 in the cluster and group environments.

scholarly journals Merging galaxies in compact groups: analytical theory

2000 ◽  
Vol 174 ◽  
pp. 423-427
Author(s):  
Victor M. Kontorovich
Keyword(s):  
Luminosity Function ◽  
Mass Function ◽  
Compact Groups ◽  
Merging Galaxies ◽  
Massive Galaxies ◽  
The Galaxy ◽  
Minor Mergers ◽  
Power Law Index ◽  
Galaxy Luminosity Function ◽  
Non Locality

AbstractThe predominance of minor mergers, i.e. the non-locality of mergings, results in a mass function slope (“Shechter” index) intermediate between a power-law index of a spectrum with constant mass flux and that of constant flux of the number of massive galaxies. The index proves to be close to that of the faint end of the galaxy luminosity function.

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