The Science Case for Building a Band 1 Receiver Suite for ALMA
J. Di Francesco, D. Johnstone, B. Matthews, N. Bartel, L. Bronfman, S. Casassus, S. Chitsazzadeh, M. Cunningham, G. Duchene, A. Hales, M. Houde, D. Iono, P. M. … 展开作者
J. Di Francesco, D. Johnstone, B. Matthews, N. Bartel, L. Bronfman, S. Casassus, S. Chitsazzadeh, M. Cunningham, G. Duchene, A. Hales, M. Houde, D. Iono, P. M. Koch, R. Kothes, S. -P. Lai, S. -Y. Liu, B. Mason, T. Maccarone, G. Schieven, A. M. M. Scaife, D. Scott, H. Shang, S. Takakuwa, J. Wagg, A. Wootten, F. Yusef-Zadeh
We present a set of compelling science cases for the ALMA Band 1 receiver suite. For these cases, we assume in tandem the updated nominal Band 1 frequency range of 35-50 GHz with a likely extension up to 52 GHz; together these frequencies optimize the Band 1 science return. The scope of the science cases ranges from nearby stars to the re-ionization edge of the Universe. Two cases provide additional leverage on the present ALMA Level One Science Goals and are seen as particularly powerful motivations for building the Band 1 Receiver suite: (1) detailing the evolution of grains in protoplanetary disks, as a complement to the gas kinematics, requires continuum observations out to ~35 GHz (~9mm); and (2) detecting CO 3-2 line emission from galaxies like the Milky Way during the epoch of re-ionization, i.e., 6 < z < 10, also requires Band 1 receiver coverage. The range of Band 1 science is wide, however, and includes studies of very small dust grains in the ISM, pulsar wind nebulae, radio supernovae, X-ray binaries, the Galactic Center (i.e., Sgr A*), dense cloud cores, complex carbon-chain molecules, masers, magnetic fields in the dense ISM, jets and outflows from young stars, distant galaxies, and galaxy clusters (i.e., the Sunyaev-Zel'dovich Effect). A comparison of ALMA and the Jansky VLA (JVLA) at the same frequencies of Band 1 finds similar sensitivity performance at 40-50 GHz, with a slight edge for ALMA at higher frequencies (e.g., within a factor of 2 for continuum observations). With its larger number of instantaneous baselines, however, ALMA Band 1data will have greater fidelity than those from the JVLA at similar frequencies.
The Atacama Large Millimeter/submillimeter Array (ALMA) Band-1 Receiver
阿塔卡马大型毫米/亚毫米阵列（ALMA）频段1接收机覆盖35-50 GHz频段。原型接收机，包括关键部件和子系统的开发已经完成，并对两套原型接收机进行了全面测试。我们将提供ALMA Band 1科学目标的概述，以及在ALMA上使用的要求和设计。本文还将讨论接收机的发展现状，并将讨论完全组装的频段1接收机系统的基础设施、集成和评估。最后，将讨论所遇到的技术和管理挑战。
Development Status of Wideband Millimeter-Wave Receivers for LMT-FINER
National Astronomical Observatory of Japan（日本国立天文台）；University of Electro-Communications（电气通信大学）；Nagoya University（名古屋大学）；Kitami Institute of Technology（北见工业大学）
A Wideband Millimeter-wave Receiver at 210-350 GHz for LMT-FINER
National Astronomical Observatory of Japan（日本国立天文台）；The University of Electro-Communications（电气通信大学）；Nagoya University（名古屋大学）；Kitami Institute of Technology（北见工业大学）；Suwa University of Science（诹访科学大学）；National Institute of Information and Communications Technology（信息通信研究机构）；The Graduate University for Advanced Studies (SOKENDAI)（综合研究大学院大学）
FINER: development of the wideband millimeter-wave receiver system and preparations for first light on the Large Millimeter Telescope
Kitami Institute of Technology（北见工业大学）；Nagoya University（名古屋大学）；The University of Electro-Communications（电气通信大学）；University of Tsukuba（筑波大学）；Waseda University（早稻田大学）；National Astronomical Observatory of Japan（日本国立天文台）；The Graduate University for Advanced Studies (SOKENDAI)（综合研究大学院大学）；The University of Tokyo（东京大学）；Suwa University of Science（諏訪精密工科大学）；Keio University（庆应义塾大学）；National Institute of Information and Communications Technology（信息通信研究机构）；Chalmers University of Technology（查尔姆斯理工大学）；Chiba University（千叶大学）；Hokkaido University（北海道大学）；Instituto Nacional de Astrofísica, Óptica y Electrónica（墨西哥国家天体物理学、光学和电子研究所）；University of Yamanashi（山梨大学）；Osaka Metropolitan University（大阪公立大学）；Japan Aerospace Exploration Agency（日本宇宙航空研究开发机构）
