Development of a new wideband heterodyne receiver system for the Osaka 1.85 m mm–submm telescope: Receiver development and the first light of simultaneous observations in 230 GHz and 345 GHz bands with an SIS-mixer with 4–21 GHz IF output. (12th June 2021)

• Record Type: Journal Article
• Authors: Masui, Sho; Yamasaki, Yasumasa; Ogawa, Hideo; Kondo, Hiroshi; Yokoyama, Koki; Matsumoto, Takeru; Minami, Taisei; Okawa, Masanari; Konishi, Ryotaro; Kawashita, Sana; Konishi, Ayu; Nakao, Yuka; Nishimoto, Shimpei; Yoneyama, Sho; Ueda, Shota; Hasegawa, Yutaka; Fujita, Shinji; Nishimura, Atsushi; Kojima, Takafumi; Uemizu, Kazunori; Kaneko, Keiko; Sakai, Ryo; Gonzalez, Alvaro; Uzawa, Yoshinori; Onishi, Toshikazu
• Is Part Of: Publications of the Astronomical Society of Japan. Volume 73:Number 4(2021)
• Page Start: 1100
• Page End: 1115
• Publication Date: 2021-06-12
• Subjects: instrumentation: detectors -- radio lines: ISM -- telescopes; Astronomy -- Periodicals; 520.5
• DOI: 10.1093/pasj/psab046
• Languages: English
• ISSNs: 0004-6264

Abstract

Abstract: We have developed a wideband receiver system for simultaneous observations in CO lines of J = 2–1 and J = 3–2 transitions using the Osaka 1.85 m mm–submm telescope. As a frequency separation system, we developed multiplexers that connect three types of diplexers, each consisting of branch-line couplers and high-pass filters. The radio frequency (RF) signal is eventually distributed into four frequency bands, each of which is fed to a superconductor–insulator–superconductor (SIS) mixer. The RF signal from the horn is divided into two frequency bands by a wideband diplexer with a fractional bandwidth of $56\%$, and then each frequency band is further divided into two bands by each diplexer. The developed multiplexers were designed, fabricated, and characterized using a vector network analyzer. The measurement results showed good agreement with the simulation. The receiver noise temperature was measured by connecting the SIS-mixers, one of which has a wideband 4–21 GHz intermediate frequency (IF) output. The receiver noise temperatures were measured to be ∼70 K in the 220 GHz band, ∼100 K in the 230 GHz band, 110–175 K in the 330 GHz band, and 150–250 K in the 345 GHz band. This receiver system has been installed on the 1.85 m telescope at the Nobeyama Radio Observatory. We succeeded in simultaneous observations of six CO isotopologue lines with the transitions of J = 2–1 and J = 3–2 toward the Orion KL as well as on-the-fly mappings toward the Orion KL and W 51.