Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XII, pp. PC1310209

Authors:

  • Kotaro Kohno
  • Akira Endo
  • Yoichi Tamura
  • Akio Taniguchi
  • Tatsuya Takekoshi
  • Shiro Ikeda
  • Naoki Yoshida
  • Kana Moriwaki
  • Kenichi Karatsu
  • Jochem J. A. Baselmans
  • Louis H. Marting
  • Arend Moerman
  • Bruno T. Buijtendorp
  • Shahab Dabironezare
  • Matus Rybak
  • Tom J. L. C. Bakx
  • Leon G. G. Olde Scholtenhuis
  • Fenno Steenvoorde
  • Robert Huiting
  • David J. Thoen
  • Lingyu Wang
  • Aurora Simionescu
  • Stephen J. C. Yates
  • Alessandro Monfardini
  • Martino Calvo
  • Paul P. van der Werf
  • Sten Vollebregt
  • Bernhard R. Brandl
  • Tai Oshima
  • Ryohei Kawabe
  • Kazuyuki Fujita
  • Shunichi Nakatsubo
  • Yuki Kimura
  • Akiyoshi Tsujita
  • Yuki Yoshimura
  • Shinji Fujita
  • Yuri Nishimura
  • Yuka Yamada
  • Sho Fujisawa
  • Kanako Narita
  • Tetsuhiro Minamidani
  • Shun Ishii
  • Fumiya Maeda
  • Adam Lidz
  • Denis Burgarella
  • Bunyo Hatsukade
  • Fumi Egusa
  • Kana Morokuma-Matsui

Keywords:

  • integrated superconducting spectrograph (ISS)
  • submillimeter-wave
  • line-intensity mapping
  • ionized carbon and oxygen lines
  • sparse modeling
  • deep learning

URL:

Abstract:

We present a plan for sub/millimeter-wave line intensity mapping (LIM) using an imaging spectrograph based on the Terahertz Integral Field Units with Universal Nanotechnology (TIFUUN) architecture. We aim to measure the dust-enshrouded cosmic star formation rate density within the first 2 billion years by conducting LIM observations of ionized carbon [C II] 158 µm and oxygen [O III] 88 µm lines, redshifted to sub/millimeter wavelengths. The proposed imaging spectrograph will simultaneously observe two frequency bands: Band-1 (139–179 GHz) and Band-2 (248–301 GHz). Each band will feature up to $\sim$100 imaging pixels (spaxels), with each spaxel having 100 spectral channels, providing a modest spectral resolution (R$\sim$500). The total number of detectors (voxels) will reach $\sim$20,000. This dual-band configuration will allow simultaneous measurement of key spectral lines, e.g., [C II] 158 µm and [O III] 88 µm lines at $z = 10.2 - 12.6$, and CO(4-3), (7-6), C I and (2-1) at $z = 1.9 - 2.2$, enabling cross-correlation analysis. We will develop data-scientific methods to remove atmospheric noise using sparse modeling and to extract signals from the observed data using deep learning.