From our sample of 108 pulsars (with an expected flux density
mJy at this frequency)
we detected 87 pulsars and obtained good quality pulse profiles
for most of them.
Eight pulsars (B1541+09, B1737+23, B1738-08, B1831-04, B1841-05,
B1914+13, B1915+13 and B2111+46) were detected by Seiradakis et al. (1995)
but with poor signal-to-noise ratio (S/N) and pulse shapes were not presented.
These pulsars were re-observed in the present survey and we obtained
good quality profiles in a short integration time. For four
other pulsars from our sample (B1900+01, B2016+28, B2045-16, B2310+42),
profiles were published by Seiradakis et al. (1995) with poor S/N and are now
presented with much better S/N. Eight pulsars
which are presented here
(B0450-18, B0611+22, B0626-28, B0809+74, B0818-13, B0834+06,
B1604-00 and B1818-04), have been observed previously
(see Sect. 1) using the old less sensitive system.
We observed but did not detect 21 pulsars which
are listed in Table 2 (click here). From the 33 pulsars not detected by Seiradakis
et al. (1995) we attempted to observe 16 pulsars and detected 14 of them.
Only two pulsars (B0320+39, B0531+21) were not
detected.
It is notable that PSR B0320+39 was observed by Kuzmin et al. (1986)
at 4.6 GHz but during the last survey (Seiradakis et al. 1995)
and in our observations this pulsar
was not detected even after 30 min integration time.
| PSR B | N | Time |  | PSR B | N | Time | |
| [min] | [mJy] | [min] | [mJy] | ||||
| 0320+39 | 1 | 30 | 0.03 | 1732-07 | 1 | 10 | 0.04 |
| 0353+52 | 1 | 15 | 0.06 | 1754-24 | 2 | 31 | 0.04 |
| 0410+69 | 2 | 30 | 0.02 | 1811+40 | 1 | 30 | 0.04 |
| 0531+21 | 3 | 40 | 0.02 | 1820-14 | 2 | 20 | 0.02 |
| 0613-02 | 1 | 10 | 1834-04 | 1 | 15 | 0.04 | |
| 0621-04 | 3 | 41 | 0.01 | 1848+04 | 1 | 10 | |
| 0751+18 | 1 | 35 | 1848+12 | 1 | 10 | 0.04 | |
| 0841+80 | 1 | 10 | 1859+01 | 1 | 25 | 0.03 | |
| 1322+83 | 2 | 30 | 0.05 | 2044+15 | 3 | 50 | 0.03 |
| 1534+12 | 3 | 31 | 2229+26 | 1 | 15 | ||
| 1700-18 | 1 | 20 | 0.03 |
for
the flux density are listed
The detection limit at 1.4 GHz for the survey by Seiradakis et al. (1995)
lies around 
mJy.
The 4.85 GHz survey has yielded a lower limit of 
0.05 mJy, as is
visible from Table 1 (click here) and the upper limits for
not detected pulsars (see Table 2 (click here)).
Scatter broadening makes it difficult to detect pulsars with high dispersion
measure at low frequencies, and
only 11 pulsars with dispersion measures DM> 600 cm-3pc are known.
All of them were discovered at 1.4 GHz (Clifton et al. 1992) or at 1.5 GHz
(Johnston et al. 1992). However, scattering is still a limiting factor even at
these frequencies. Using the new receiver at 6 cm we detected 9 pulsars
with DM> 500
cm-3pc. We easily measured, for instance, B1758-23, which has presently
the largest known DM of 1074 cm-3pc (see Fig. 1 (click here) and Table 1 (click here)).
B1750-24 (
cm-3pc) shows a double (more likely complex)
component profile at 4.85 GHz, whereas the components are completely
smeared out at 1.4 GHz due to scatter broadening (Clifton et al. 1992).
Finally, we observed four millisecond pulsars at this frequency (for
more detailes see Kijak et al. 1997).
Figure 1: Pulse shapes for 87 pulsars at 4.85 GHz
In Fig. 1 (click here) we present all pulse shapes obtained as result of
our observations.
The errors in flux density
and pulse width were estimated by taking into account
the calibration
results, the signal-to-noise ratio and the resolution of the profiles.
The error of the pulse width after smoothing is indicated by
the width of the error box at the lower, right corner of each figure.
The results are given in Table 1 (click here). For each pulsar, Col. (5) and (6) contain
the pulse widths W50 and W10.
The flux densities S and their
errors are listed in Col. (7) and (8), respectively.
The spectral index 
for flux densities between 1.4 and 4.85 GHz is given in Col. (9)
with errors in Col. (10).
We assumed that the pulsar flux spectra are well
described by a power law of the form 
.
An index was obtained between 1.4 and 4.85 GHz
using data from Lorimer et al. (1995) at 1.4
and 1.6 GHz, Sieber (1973) at 2.7 GHz, Seiradakis et al. (1995) at
1.4 and 4.75 GHz
and this paper.
