 |
Figure 1:
Differential counts,
 ,
of
different source populations at 30 and 150 GHz, based on the De Zotti et al. (2005)
evolution model. Solid lines: canonical flat- plus steep-spectrum
sources; dot-dashed lines: starburst galaxies; short-dashed
lines: dusty proto-spheroidal galaxies with (upper curve) and
without the mm excess (see text). In the left-hand panel only
the estimated counts of GPS sources (dotted line) and of
ADAF/ADIOS sources (long-dashed line) are also shown. |
| Open with DEXTER | |
In the text
 |
Figure 2:
Angular power spectrum (
 )
measured at 30 GHz by CBI ( left-hand panel;
data points from Readhead et al. 2004) and by BIMA (right-hand
panel; data points from Dawson et al. 2002). In each panel, we
have plotted the primordial CMB angular power spectrum
(dot-dashed-line), the estimated range of contributions of
unsubtracted canonical radio sources (dotted lines; see text), and
of Poisson distributed (short-dashed line) and clustered
(long-dashed line) proto-spheroidal galaxies. In the BIMA case,
the upper pair of long- and short-dashed lines refers to
proto-spheroidal galaxies with the submillimeter excess mentioned
in Sect. 2 (not shown in the other panel). The contributions of
the latter sources are insensitive to the adopted flux limit
because of the very steep counts. The shaded areas show the ranges
spanned by the quadratic sum of the different contributions. |
| Open with DEXTER | |
In the text
 |
Figure 3:
Angular power spectrum (
)
measured by ACBAR at 150 GHz (data
points are from Kuo et al. 2004). The dotted, long- and short-dashed,
and dot-dashed curves have the same meaning as in Fig. 2; the solid
lines are the quadratic sum of all the contributions. The contribution given by
undetected Poisson distributed and clustered proto-spheroidal
galaxies has been calculated without ( left-hand panel) and with
( right-hand panel) the excess mm-wave emission discussed in the text.
In this case we adopted
 mJy ( left-hand panel)
and
 mJy ( right-hand panel) for source detection.
These limits correspond to the 
source detection threshold
estimated as in Negrello et al. (2004) for a 5
FWHM.
|
| Open with DEXTER | |
In the text