The Night-sky at the Calar Alto Observatory Ii: the Sky at the near Infrared

We present the characterization of additional properties of the night-sky at the Calar Alto observatory, following the study started in Sánchez et al. (2007), hereafter Paper I. We focus here on the night sky-brightness at the near-infrared, the telescope seeing, and the fraction of useful time at the observatory. For this study we have collected a large dataset comprising 7311 near-infrared images taken regularly along the last four years for the ALHAMBRA survey (J , H and Ks-bands), together with a more reduced dataset of additional near-infrared images taken for the current study. In addition we collected the information derived by the meteorological station at the observatory during the last 10 years, together with the results from the cloud sensor for the last ∼2 years. We analyze the dependency of the near-infrared night sky-brightness with the airmass and the seasons, studying its origins and proposing a zenithal correction. A strong correlation is found between the night sky-brightness in the Ks-band and the air temperature, with a gradient of ∼ −0.08 mag per 1 ◦ C. The typical (darkest) night sky-brightness in the J , H and Ks-band are 15.95 mag (16.95 mag), 13.99 mag (14.98 mag) and 12.39 mag (13.55 mag), respectively. These values have been derived for the first time for this observatory, showing that Calar Alto is as dark in the near-infrared as most of the other astronomical astronomical sites in the world that we could compare with. Only Mauna Kea is clearly darker in the Ks-band, but not only compared to Calar Alto but to any other observatory in the world. The typical telescope seeing and its distribution was derived on the basis of the FWHM of the stars detected in the considered near-infrared images. This value, ∼1.0 when converted to the V-band, is only slightly larger than the atmospheric seeing measured at the same time by the seeing monitor, ∼0.9. Therefore, the effects different than the atmosphere produce a reduced degradation on the telescope seeing, of the order of ∼10%. Finally we estimate the fraction of useful time based on the relative humidity, gust wind speed and presence of clouds. This fraction, ∼72%, is very similar to the one derived in Paper I, based on the fraction of time when the extinction monitor is working. Subject headings: Astronomical Phenomena and Seeing