Evolution of the blue and far-infrared galaxy luminosity functions

1993 ◽  
Vol 105 ◽  
pp. 1333 ◽  
Author(s):  
Carol J. Lonsdale ◽  
Arati Chokshi
Keyword(s):  
Far Infrared ◽  
Infrared Galaxy ◽  
Luminosity Functions

scholarly journals A surprising consistency between the far-infrared galaxy luminosity functions of the field and Coma

2014 ◽  
Vol 442 (2) ◽  
pp. 1286-1293 ◽  
Author(s):  
S. Hickinbottom ◽  
C. J. Simpson ◽  
P. A. James ◽  
E. Ibar ◽  
D. Carter ◽  
...  
Keyword(s):  
Far Infrared ◽  
Infrared Galaxy ◽  
Luminosity Functions

scholarly journals From rest-frame luminosity functions to observer-frame colour distributions: tackling the next challenge in cosmological simulations

2020 ◽  
Vol 497 (3) ◽  
pp. 3026-3046 ◽  
Author(s):  
Matías Bravo ◽  
Claudia del P Lagos ◽  
Aaron S G Robotham ◽  
Sabine Bellstedt ◽  
Danail Obreschkow
Keyword(s):  
Survey Design ◽  
Target Selection ◽  
Broad Band ◽  
Complex Mixture ◽  
Far Infrared ◽  
Bimodal Distribution ◽  
Spectral Energy ◽  
Recent Success ◽  
Luminosity Functions ◽  
Radiation Output

ABSTRACT Galaxy spectral energy distributions (SEDs) remain among the most challenging yet informative quantities to reproduce in simulations due to the large and complex mixture of physical processes that shape the radiation output of a galaxy. With the increasing number of surveys utilizing broad-band colours as part of their target selection criteria, the production of realistic SEDs in simulations is necessary for assisting in survey design and interpretation of observations. The recent success in reproducing the observed luminosity functions (LFs) from far-ultraviolet (UV) to far-infrared (IR), using the state-of-the-art semi-analytic model shark and the SED generator ProSpect, represents a critical step towards better galaxy colour predictions. We show that with shark and ProSpect we can closely reproduce the optical colour distributions observed in the panchromatic Galaxy And Mass Assembly (GAMA) survey. The treatment of feedback, star formation, central–satellite interactions, and radiation reprocessing by dust are critical for this achievement. The first three processes create a bimodal distribution, while dust attenuation defines the location and shape of the blue and red populations. While a naive comparison between observation and simulations displays the known issue of overquenching of satellite galaxies, the introduction of empirically motivated observational errors and classification from the same group finder used in GAMA greatly reduces this tension. The introduction of random reassignment of ${\sim} 15{{\ \rm per\ cent}}$ of centrals/satellites as satellites/centrals on the simulation classification closely resembles the outcome of the group finder, providing a computationally less intensive method to compare simulations with observations.

scholarly journals Identifications of Faint IRAS Sources

1996 ◽  
Vol 171 ◽  
pp. 402-402
Author(s):  
M.W. Kümmel ◽  
S.J. Wagner
Keyword(s):  
Broad Band ◽  
Far Infrared ◽  
Power Laws ◽  
Point Sources ◽  
Spectral Energy ◽  
Energy Distributions ◽  
The North ◽  
Luminosity Functions ◽  
Error Circle ◽  
Radio Band

From overlapping scans in the IRAS all-sky survey and additional pointed observations the deepest far infrared survey before ISO exists in the region around the North Ecliptic Pole (NEP) (Hacking P. and Houck J.R., ApJS 63 p. 311). This survey contains detections up to 10 and fluxes up to 100 times fainter than the IRAS survey. In the central square degree around the NEP we combine the far IR-survey with deep radio data at 151 MHz and 1.5 GHz (Visser, A.E. et al., A&AS 110 p. 419, Kollgaard, R.I. et al., ApJS 93 p. 145) and own observation at 2.2μm (K′) and 435nm (B). The error circle around the IRAS source was chosen to include the true source with 85% probability (1.4 sigma). For 29 of the 32 IRAS sources we found at least one possible counterpart. Ten of the objects have multiple (up to four) counterparts in K′. Four of the IRAS sources have counterparts in the 1.5 GHz survey. The higher accuracy of the radio position (∼ 1″) allowed an unambiguous identification of the K′ counterpart. None of the IRAS sources could be found in the 151 MHz survey. The broad band spectra of the three galaxies with measured radio flux exhibit maximum emission between the radio band and 100μm which corresponds to emission by cool dust (< 50 K). Contrary to the infrared luminosity functions at 12μm and 60μm which show power laws, the K′ luminosity function is bimodal. The brightest K′ objects are all point sources. Due to the small number statistics the power law indices of the luminosity functions can not be distinguished. We find a linear relationship between the K′ flux and the flux at 60μm and 12μm over at least one decade. The large deviations by individual sources make an identification of the correct counterpart through this relation impossible. The spectral energy distributions of unambiguously identified sources span only one decade in energy (vSv), i.e. they have flat energy distributions. This suggests an identification of K′ objects with flat energy distribution in case of multiple counterparts.

scholarly journals Far-infrared luminosity functions of normal galaxies

1992 ◽  
Vol 79 ◽  
pp. 197 ◽  
Author(s):  
Takashi Isobe ◽  
Eric D. Feigelson
Keyword(s):  
Far Infrared ◽  
Normal Galaxies ◽  
Luminosity Functions
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