Removing sky emission is essential to extract astronomical signals for submillimeter spectroscopy with ground-based single-dish telescopes, however, conventional switching methods not only cause baseline instability but result in low observing efficiency of on-source. Here we present two statistical approaches to efficient sky removal. For a heterodyne receiver, we develop an off-point-less observing method by a frequency-modulating local oscillator (FMLO; Taniguchi et al., PASJ, in press), which is three times more efficient than the conventional method. For an ultra-wideband spectrometer (DESHIMA; Endo et al. 2019a, 2019b), we develop a sky removal method applicable to continuum observations by using an atmospheric model.
We present an archive system named "Adria", which have been developed and maintained by ALMA project team of National Astronomical Observatory of Japan (NAOJ). Adria aims to store and open to the public various science data. Adria is composed of an object storage to store the observation data, the access control by "ticket", JSON format metadata, JavaScript APIs and html documents. The combination has the advantages of flexibility and solidity, which are important to store various telescope data in the same platform and to be maintained with small cost for a long time. Firstly, we have applied Adria to the observation data (since July 2013) of Nobeyama Radio Observatory (NRO) 45m, and then we have added the data (since June 2019) of Atacama Submillimeter Telescope Experiment (ASTE) to the same platform.
We are promoting the Hybrid Installation Project in Nobeyama, Triple-band Oriented (HINOTORI), a project aiming at triple-band simultaneous single-dish and VLBI observation in the 22-, 43- and 86-GHz bands using the Nobeyama 45-m Telescope. The triple-band simultaneous observation becomes possible by developing two perforated plates and mounting them in the Nobeyama 45-m Telescope optics. One is a 22/43-GHz-band perforated plate, which transmits the higher frequency (43-GHz) band and reflects the lower frequency (22-GHz) band, and the other is a 43/86-GHz-band perforated plate, which transmits the 86-GHz band and reflects the 43-GHz band or lower. Both plates are designed to be installed in the large telescope optics with a beam diameter as large as 50 cm and insertion/reflection losses are both 0.22 dB (5%) or less in the design. The receivers used in triple-band simultaneous observation system are the H22 and H40 receivers, which are already installed in the Nobeyama 45-m Telescope, and the TZ receiver, which is a 100-GHz-band receiver including the 86-GHz band and reinstalled in the Nobeyama 45-m Telescope. A system of simultaneous observations in the 22- and 43-GHz bands of the Nobeyama 45-m Telescope with the 22/43- GHz-band perforated plate has been completed and commissioned for scientific observations. Also VLBI fringes between the Nobeyama 45-m telescope with the dual-band observation system and the VERA 20-m telescopes at 22 and 43 GHz was detected successfully.
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