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The Pierre Auger Observatory is the world’s largest operating detection system for the observation of ultra high energy cosmic rays (UHECRs), with energies above <inline-formula> <math display="inline"> <semantics> <msup> <mn>10</mn> <mn>17</mn> </msup> </semantics> </math> </inline-formula> eV. The detector allows detailed measurements of the energy spectrum, mass composition and arrival directions of primary cosmic rays in the energy range above <inline-formula> <math display="inline"> <semantics> <msup> <mn>10</mn> <mn>17</mn> </msup> </semantics> </math> </inline-formula> eV. The data collected at the Auger Observatory over the last decade show the suppression of the cosmic ray flux at energies above <inline-formula> <math display="inline"> <semantics> <mrow> <mn>4</mn> <mo>×</mo> <msup> <mn>10</mn> <mn>19</mn> </msup> </mrow> </semantics> </math> </inline-formula> eV. However, it is still unclear if this suppression is caused by the energy limitation of their sources or by the Greisen–Zatsepin–Kuzmin (GZK) cut-off. In such a case, UHECRs would interact with the microwave background (CMB), so that particles traveling long intergalactic distances could not have energies greater than <inline-formula> <math display="inline"> <semantics> <mrow> <mn>5</mn> <mo>×</mo> <msup> <mn>10</mn> <mn>19</mn> </msup> </mrow> </semantics> </math> </inline-formula> eV. The other puzzle is the origin of UHECRs. Some clues can be drawn from studying the distribution of their arrival directions. The recently observed dipole anisotropy has an orientation that indicates an extragalactic origin of UHECRs. The Auger surface detector array is also sensitive to showers due to ultra high energy neutrinos of all flavors and photons, and recent neutrino and photon limits provided by the Auger Observatory can constrain models of the cosmogenic neutrino production and exotic scenarios of the UHECRs origin, such as the decays of super heavy, non-standard-model particles. In this paper, the recent results on measurements of the energy spectrum, mass composition and arrival directions of cosmic rays, as well as future prospects are presented.