35øN, 137øE, 70 m above sea level). In the present article we report diurnal and seasonal variations of 0 3 mixing ratios observed at Nagoya University.
Instrument and Data ReductionsThe instrument consists of an offset paraboloidal reflector, a heterodyne receiver, acoustooptical spectrometers, and a system computer. The offset paraboloidal reflector with a diameter of 10 cm couples to the waveguide input of the heterodyne mixer via a feed horn. The optical configuration is shown in the block diagram of the instrument (Figure 1). By rotation of the reflector we can point the beam on the sky at an arbitrary zenith angle, the hot load at the ambient temperature, and the cold load by computer control. The central part of the cold load is kept at 20 K by a cryogenic cooler and the outer part is kept at the ambient temperature. When we observe the spectral line by the load switching mode, the input to the receiver from the cold load is adjusted to the sky temperature by slight rotation of the reflector with a stepping motor at the beginning of the integration cycle.The heterodyne mixer is a Nb SIS mixer [Ogawa et al., 1990;Ogawa, 1991]. The heterodyne mixer is the same type as the one used in the Nagoya 4-m millimeter-wave telescope for radio astronomical observations since 1989. The SIS array is composed of eight SIS junctions connected in series in order to 1371