Sov. Sci. Rev. E Astrophys. Space Phys., Vol. 5, 1986, pp. 39-179

0143 – 0432/86/0005 0179 $30.00/0

© 1986 harwood academic publishers GmhH

Printed in the United Kingdom

EXPERIMENT COLD:

THE FIRST DEEP SKY SURVEY WITH

THE RATAN-600 RADIO TELESCOPE

2 The RATAN-600 Radio Telescope
2.1 Brief History
2.2 Brief Description of the RATAN-600 Radio Telescope

3. Experimental Technique
3.1. Introduction
3.2. Extremely Low-Noise Amplifier
3.3. Radiometer
3.4. "Cooling" the Antenna
3.5. Calibration of the Radiometer in Terms of Antenna Temperature
3.6. Total Noise Temperature and Sensitivity of the System
3.7 Observing Method

4. Limiting Factors and Characteristics of  the RATAN

4.1. Theoretical Sensitivity of the Radio Telescope and the Problem of Attaining it in Practice
4.2. Atmosphere
4.3. Confusion Noise
4.4. Elimination of Discrete Sources
4.5. Sky Surveys Using the RATAN-600
4.6. Brightness Temperature Sensitivity
4.7. Conclusion: The Role of the RA TAN in Modern Radio Astronomy

5  Astrophysical Problems Studied in Experiment Cold
         
5.1. Statement of the Problem
5.2.  A List of the Problems Studied in the Deep-Survey Cycles
5.3.  Other Problems for the "Cold" Program
5.4 The Observer's Goal

6. Data Reduction Methods Used in Experiment Cold
6.1. Point Sources, i.e., on Scales Comparable to the Beam of the Radio Telescope
6.2. Suppressing Anomalous Low-Frequency Noise
6.3. Conclusion
6.4. Protocluster Scales, i.e., on the Order of 10 Arcmin.
6.5. Large Scales – The Background Emission of the Galaxy
6.6. Scales Comparable with the Size of the Horizon at the Recombination Epoch (0.5^o –2^o)
6.7. Conclusions

7. Results of the Discrete Source Observations
 
7.1. General Characteristics of the Region Surveyed
7.2. "Strong" Radio Sources
7.3. "Weak" Radio Sources (13^h < a < 14^h)
7.4. A New Population of Radio Sources?
7.5. Declination and Right Ascension of Some of the Sources
8. The Galaxy

8.1. High-Latitude Background Emission
8.2. Nearby Regions of the Milky Way

9Search for Anisotropy in the 3-Degree Background

9.1. Introduction
9.2. Obtaining the Raw Rata
9.3. Comparison with Other Observations
9.4. Comparison with Theory
9.5. A Search for Polarization in the 3-Degree Background

10. What Next?

10.1. Prospects for the Development of Experiment Cold
10.2. Experiment Cold and the "New-Generation" Radio Astronomy