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**Session 19 - Source Surveys, Galaxy Surveys, Distance Scale II.**

*Display session, Wednesday, January 07*

*Exhibit Hall, *

## [19.07] The Radio and Infrared Luminosity Functions

*N. A. Reddy (U. Texas at Austin), M. S. Yun (NRAO)*
The luminosity function (LF) for radio sources was determined at \nu=1.4 GHz and
\lambda=60\mu by correlating infrared sources from the Strauss 1.2 Jy IRAS
Redshift Survey with their radio counterparts in the NRAO VLA Sky Survey (NVSS).
The sample was limited to those galaxies with known redshift and S_60\mu >
2.00 Jy within two regions of the completed NVSS Sky Survey given by the
following coordinates: 4h\leq\alpha<16h, \delta\geq30^\circ and
-40^\circ\leq\delta\leq-10^\circ. The radio-far-infrared correlation was derived and accurate positions for IRAS Redshift Survey sources were obtained through the correlation process. Luminosity distributions for
\nu=1.4 GHz and \lambda=60\mu were then constructed. A determination of the
characteristic volume for a given distance and luminosity interval was used
to construct the luminosity functions corresponding to the distributions.
A \chi^2 analysis of the observed distributions and functions yields
the Schechter parameters corresponding to the analytic distributions and functions.
The analytic distribution at 1.4 GHz is well described by the sum of two Schechter functions with
L_1^*=(3.98\pm0.31)\times 10^22 W Hz^-1 and L_2^*=(24.78\pm3.84)\times
10^22
W Hz^-1, respectively. The analytic distribution at \lambda=60\mu is also
given by two best-fit curves with L_1^*=(14.00\pm1.20)\times 10^9 L_ødot and
L_2^*=(79.75\pm9.78)\times 10^9 L_ødot. The 1.4 GHz luminosity function is
fitted with one curve with L^*=(2.80\pm0.15)\times 10^22 W Hz^-1 and the 60\mu
luminosity function is fitted with two curves with L_1^*=(9.16\pm0.84)\times 10^9
L_ødot and L_2^*=(46.57\pm3.08)\times 10^9 L_ødot, respectively. Two distinct
populations are identified in the radio and far-infrared luminosity functions: 1) normal
late-type galaxies; and 2) starburst/AGN population of galaxies. The former matches the
spiral population of Condon. The latter can be identified with Condon's but is not identical (Note: all calculation use a Hubble constant value of H_o = 75 km s^-1 Mpc^-1).

The author(s) of this abstract have provided an email address for comments about the abstract: naveen@einstein.ph.utexas.edu

**Program
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