FINER: Far-Infrared Nebular Emission Receiver for the Large Millimeter Telescope
Paper i proceeding, 2024
Unveiling the emergence and prevalence of massive/bright galaxies during the epoch of reionization and beyond, within the first 600 million years of the Universe, stands as a pivotal pursuit in astronomy. Remarkable progress has been made by JWST in identifying an immense population of bright galaxies, which hints at exceptionally efficient galaxy assembly processes. However, the underlying physical mechanisms propelling their rapid growth remain unclear. With this in mind, millimeter and submillimeter-wave spectroscopic observations of redshifted far-infrared spectral lines, particularly the [O iii] 88 µm and [C ii] 158 µm lines, offers a crucial pathway to address this fundamental query. To this end, we develop a dual-polarization sideband-separating superconductor-insulator-superconductor (SIS) mixer receiver, FINER, for the Large Millimeter Telescope (LMT) situated in Mexico. Harnessing advancements from ALMA's wideband sensitivity upgrade (WSU) technology, FINER covers radio frequencies spanning 120-360 GHz, delivering an instantaneous intermediate frequency (IF) of 3-21 GHz per sideband per polarization, which is followed by a set of 10.24 GHz-wide digital spectrometers. At 40% of ALMA's light-collecting area, the LMT's similar atmospheric transmittance and FINER's 5 times wider bandwidth compared to ALMA culminate in an unparalleled spectral scanning capability in the northern hemisphere, paving the way for finer spectral-resolution detection of distant galaxies.
SIS receiver
Millimeter and submillimeter instrumentation
Heterodyne receiver
LMT
High-redshift universe
Interstellar medium
Galaxy formation
ALMA
Författare
Y. Tamura
Nagoya University
T. Sakai
University of Electro-Communications
Ryohei Kawabe
National Astronomical Observatory of Japan
Takafumi Kojima
National Astronomical Observatory of Japan
Akio Taniguchi
Nagoya University
Tatsuya Takekoshi
Kitami Institute of Technology
Haoran Kang
National Astronomical Observatory of Japan
Wenlei Shan
National Astronomical Observatory of Japan
Masato Hagimoto
Nagoya University
Norika Okauchi
Nagoya University
Airi Tetsuka
University of Electro-Communications
Akio K. Inoue
Waseda University
Kotaro Kohno
University of Tokyo
Kunihiko Tanaka
Keio University
Tom Bakx
Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik
Yoshinobu Fudamoto
Chiba University
Kazuyuki Fujita
Hokkaido University
Yuichi Harikane
University of Tokyo
Takuya Hashimoto
University of Tsukuba
B. Hatsukade
National Astronomical Observatory of Japan
D. Hughes
Instituto Nacional de Astrofísica, Óptica y Electrońica
Takahiro Iino
University of Tokyo
Yuki Kimura
Hokkaido University
Hiroyuki Maezawa
Osaka Metropolitan University
Y. Matsuda
National Astronomical Observatory of Japan
Ken Mawatari
Waseda University
T. Nakajima
Nagoya University
Shunichi Nakatsubo
JAXA Institute of Space and Astronautical Science
Tai Oshima
National Astronomical Observatory of Japan
H. Sagawa
Kyoto Sangyo University
T. Savolainen
University of Massachusetts
Shigeru Takahashi
University of Tokyo
Kotomi Taniguchi
National Astronomical Observatory of Japan
Akiyoshi Tsujita
University of Tokyo
H. Umehata
Nagoya University
Teppei Yonetsu
Osaka Metropolitan University
Min S. Yun
University of Massachusetts
Proceedings of SPIE - The International Society for Optical Engineering
0277786X (ISSN) 1996756X (eISSN)
Vol. 13102 131020G9781510675278 (ISBN)
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XII 2024
Yokohama, Japan,
Yokohama, Japan,
Ämneskategorier
Astronomi, astrofysik och kosmologi
DOI
10.1117/12.3017788