6 Fig. 8. The celestial sphere in galactic coordinates with cir- cles of radius 3.1 ◦ centered at the arrival directions of the 27 cosmic rays with highest energy detected by the Pierre Auger Observatory [28]. The positions of the 472 AGN with redshift less than 0.018 (i.e. distance less than 75 Mpc) are in- dicated by red asterisks. The solid line represents the border of the field of view (zenith angles smaller than 60 ◦ ). Darker color indicates larger relative exposure. Each colored band has equal integrated exposure. The dashed line is the su- pergalactic plane. Centaurus A, one of our closest AGN, is marked in white. 9. Plans for Future References 10. Conclusions [14] The Pierre AUGER Collaboration; J. Abraham et al., Submitted to Nuclear Instruments and Meth- ods in Physics Research Section A, arXiv:0907.4282 (2009) [13] T. Suomijarvi, Proceedings of the 31st ICRC, Lodz, Poland (2009), arXiv:0907.2354 [12] J. L. Harton, Proceedings of the 31st ICRC, Lodz, Poland (2009), arXiv:0907.2354 [11] K.-H. Kampert, The 2009 Europhysics Conference on High Energy Physics, Kracow, Poland (2009) [10] The Pierre AUGER Collaboration; J. Abraham et al., Nuclear Instruments and Methods in Physics Research Section A 523, 50 (2004) [9] S. P. Knurenko et al., Nuclear Physics B Proceed- ings Supplements 175, 201 (2008) [8] T. Nonaka et al., Nuclear Physics B Proceedings Supplements 190, 26 (2009) [7] B. Keilhauer, Proceedings of the 31st ICRC, Lodz, Poland (2009), arXiv:0906.2358 [6] L. Valore, Proceedings of the 31st ICRC, Lodz, Poland (2009), arXiv:0906.2358 [5] S. Y. Ben Zvi, Proceedings of the 31st ICRC, Lodz, Poland (2009), arXiv:0906.2358 [4] The Pierre AUGER Collaboration; J. Abraham et al., Physical Review Letters 101, 061101 (2008) [3] T. K. Gaisser and A. M. Hillas, Proceedings of the 15th ICRC, Sofia, Bulgaria (1977) [2] G. T. Zatsepin and V. A. Kuzmin, Journal of Ex- perimental and Theoretical Physics Letters 4, 78 (1966) [1] K. Greisen, Physical Review Letters 16, 748 (1966) spacing on a square grid. The tanks will be observed by a set of fluorescence telescopes arranged in several locations. Research and development works on a small surface detector array, atmospheric monitoring, electron- ics and communication systems have already started and the construction is planned nowadays to start in the year 2011. Assuming the same UHECRs flux in the north sky there will be detected approximately 180 events above the GZK energy per year. Even more ambitious project is planned to take place at the International Space Station. Air shower tracks will be measured from this station in very large volume of the Earth’s atmosphere. The key element of the sensor of JEM-EUSO (Japanese Experiment Module - Extreme Universe Space Observatory) will be a wide-field and fast large-lense telescope [40]. JEM-EUSO is planned to be launched before year of 2015. A significant progress in the study of UHECRs has been achieved by the data measured by the Pierre Auger Observatory. The observatory is routinely measuring now and a release of new results can be expected soon. There will be also results from the Telescope Array dur- ing next years. Moreover, a comparison between the re- sults measured in the southern and northern hemisphere by one experiment may be possible in close future. Up to now the suppression of the cosmic ray flux to- gether with the anisotropy of arrival directions have been observed at the highest energies by the Pierre Auger Observatory. The flux of GZK photons and neutrinos should be reached in few years. Moreover, the cross sec- tion between UHECRs and air can be calculated if the type of primary particle will be found. All these re- sults together with the observed arrival directions will hopefully lead to the finding of the sources of the most energetic particles in the universe. The northern part of the Pierre Auger Observatory is planned to be built in the northern hemisphere. In 2005 the site was chosen in southeast Colorado, USA. It will consist of an array of 4 000 water tanks deployed on an area of 20 000 km $^{2}$, arranged at √$_{2 miles array}$ There are a number of worldwide efforts to develop and establish new detection techniques that promise a cost-effective extension of currently available apertures to even larger dimensions. The detection of radio emis- sion induced by ultra-high-energy cosmic rays hitting the Earth’s atmosphere is possible because of coherent radi- ation from the extensive air shower at radio frequencies. This radiation, which is emitted by secondary particles created in the air shower, can be measured with simple radio antennas. Radio detectors, like LOPES [37] and CODALEMA [38] produce promising results at energies beyond 10 17 eV. The project AERA (Auger Engineering Radio Array) is planned at the Pierre Auger Observatory and it will have a dimension of about 20 km 2 [39]. The progress in next year can be expected also from the laboratory measurements of the fluorescence yield. The absolute measurement of this quantity is expected particularly from the experiment AirFLY [36]. Adopting this result will lead to a significant improvement of the energy reconstruction of all measured data. First of all we can except more data coming from the current experiments. There are also some extensions of current observatories into lower energies, i.e. below 10 18 eV, which are already in progress. The reason for these low energy extensions is making the comparison with the results from experiments (such as KASCADE- Grande [32, 33]), which overlap with the direct measure- ments of cosmic rays. There are already several projects under construction or already in testing phase. At the Pierre Auger Observatory there are three high-elevation fluorescence telescopes (HEAT), which can be tilted and used to observe showers at energies down to 10 17 eV [34]. The other enhancement is AMIGA (Auger Muons and Infill for the Ground Array) which is formed by 85 pairs of a water Cherenkov tank and a buried muon counter arranged at 750 m and 433 m array spacings [35]. In other working experiment the Telescope Array Low En- ergy (TALE) extension is designed to observe cosmic $^{rays down to energies of 3}$× 10 16 eV [8].