TiEMPO: Open-source time-dependent end-to-end model for simulating ground-based submillimeter astronomical observations
Esmee Huijten, Yannick Roelvink, Stefanie A. Brackenhoff, Akio Taniguchi, Tom J. L. C. Bakx, Kaushal B. Marthi, Stan Zaalberg, Jochem J. A. Baselmans, Kah Wuy C… 展开作者
Esmee Huijten, Yannick Roelvink, Stefanie A. Brackenhoff, Akio Taniguchi, Tom J. L. C. Bakx, Kaushal B. Marthi, Stan Zaalberg, Jochem J. A. Baselmans, Kah Wuy Chin, Robert Huiting, Kenichi Karatsu, Alejandro Pascual Laguna, Yoichi Tamura, Tatsuya Takekoshi, Stephen Yates, Maarten van Hoven, Akira Endo
The next technological breakthrough in millimeter-submillimeter astronomy is 3D imaging spectrometry with wide instantaneous spectral bandwidths and wide fields of view. The total optimization of the focal-plane instrument, the telescope, the observing strategy, and the signal-processing software must enable efficient removal of foreground emission from the Earth's atmosphere, which is time-dependent and highly nonlinear in frequency. Here we present TiEMPO: Time-Dependent End-to-End Model for Post-process Optimization of the DESHIMA Spectrometer. TiEMPO utilizes a dynamical model of the atmosphere and parametrized models of the astronomical source, the telescope, the instrument, and the detector. The output of TiEMPO is a time-stream of sky brightness temperature and detected power, which can be analyzed by standard signal-processing software. We first compare TiEMPO simulations with an on-sky measurement by the wideband DESHIMA spectrometer and find good agreement in the noise power spectral density and sensitivity. We then use TiEMPO to simulate the detection of a line emission spectrum of a high-redshift galaxy using the DESHIMA 2.0 spectrometer in development. The TiEMPO model is open source. Its modular and parametrized design enables users to adapt it to design and optimize the end-to-end performance of spectroscopic and photometric instruments on existing and future telescopes.
Thioacetamide (CH3CSNH2) is the sulfur analog to acetamide (CH3CONH2) and it is a viable candidate to search for in astronomical environments specifically toward regions where other S-bearing molecules have been found and, if possible, that also contain a detection of CH3CONH2. If detected, it would not only continue to expand the view of molecular complexity in astronomical environments, but also help to better elucidate the possible formation pathways of these types of species in these environments. The rotational spectrum of CH3CSNH2 was investigated up to 650 GHz. Using the newly refined s…
A substantial amount of important scientific information is contained within astronomical data at the submillimeter and far-infrared (FIR) wavelengths, including information regarding dusty galaxies, galaxy clusters, and star-forming regions; however, these wavelengths are among the least-explored fields in astronomy because of the technological difficulties involved in such research. Over the past 20 years, considerable efforts have been devoted to developing submillimeter- and millimeter-wavelength astronomical instruments and telescopes. The number of detectors is an important property of s…
阿塔卡马大型毫米/亚毫米阵列（英语：Atacama Large Millimeter/Submillimeter Array，简称ALMA）是一个国际射电望远镜，位于智利北部的阿塔卡马沙漠。ALMA位于海拔5000米的干燥场地上，在仪器波长范围为0.3至10毫米的范围内具有良好的大气传输能力。其中一个是多达64个直径为12米的天线，可以在150米到15公里的范围内以多种模式重新配置。第二个阵列由一组四个12米和十二个7米天线组成，在直径约50米的两个紧密排列的配置中的一个中工作。该仪器将提供关于太阳系、银河系和附近高红移宇宙中原子、分子和电离气体和尘埃的干涉和总功率天文信息。在本文中，我们概述了ALMA的科学驱动因素，技术挑战和计划进展。
For submillimeter spectroscopy with ground-based single-dish telescopes, removing noise contribution from the Earth's atmosphere and the instrument is essential. For this purpose, here we propose a new method based on a data-scientific approach. The key technique is statistical matrix decomposition that automatically separates the signals of astronomical emission lines from the drift noise components in the fast-sampled (1--10 Hz) time-series spectra obtained by a position-switching (PSW) observation. Because the proposed method does not apply subtraction between two sets of noisy data (i.e., …
Site Quality Analysis for an Indian Submillimeter Telescope: A Reanalysis-Based Approach
Raman Research Institute（拉曼研究所）；School of Earth and Space Exploration, Arizona State University（亚利桑那州立大学地球与空间探索学院）；Department of Physics, California Institute of Technology（加州理工学院物理系）；Jet Propulsion Laboratory（喷气推进实验室）
The proposed next generation Event Horizon Telescope (ngEHT) concept envisions the imaging of various astronomical sources on scales of microarcseconds in unprecedented detail with at least two orders of magnitude improvement in the image dynamic ranges by extending the Event Horizon Telescope (EHT). A key technical component of ngEHT is the utilization of large aperture telescopes to anchor the entire array, allowing the connection of less sensitive stations through highly sensitive fringe detections to form a dense network across the planet. Here, we introduce two projects for planned next g…
The BLAST Observatory is a proposed superpressure balloon-borne polarimeter designed for a future ultra-long duration balloon campaign from Wanaka, New Zealand. To maximize scientific output while staying within the stringent superpressure weight envelope, BLAST will feature new 1.8m off-axis optical system contained within a lightweight monocoque structure gondola. The payload will incorporate a 300L $^4$He cryogenic receiver which will cool 8,274 microwave kinetic inductance detectors (MKIDs) to 100mK through the use of an adiabatic demagnetization refrigerator (ADR) in combination with a $^…
Recent spectroscopic observations by sensitive radio telescopes require accurate molecular spectral line frequencies to identify molecular species in a forest of lines detected. To measure rest frequencies of molecular spectral lines in the laboratory, an emission-type millimeter and submillimeter-wave spectrometer utilizing state-of-the-art radio-astronomical technologies is developed. The spectrometer is equipped with a 200 cm glass cylinder cell, a two sideband (2SB) Superconductor-Insulator-Superconductor (SIS) receiver in the 230 GHz band, and wide-band auto-correlation digital spectromet…
Development of a planar cable-driven parallel robot for submillimeter and terahertz beam mapping measurements
University of Arizona（亚利桑那大学）；California Institute of Technology（加州理工学院）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Cornell University（康奈尔大学）
CASA, the Common Astronomy Software Applications, is the primary data processing software for the Atacama Large Millimeter/submillimeter Array (ALMA) and the Karl G. Jansky Very Large Array (VLA), and is frequently used also for other radio telescopes. The CASA software can handle data from single-dish, aperture-synthesis, and Very Long Baseline Interferometery (VLBI) telescopes. One of its core functionalities is to support the calibration and imaging pipelines for ALMA, VLA, VLA Sky Survey (VLASS), and the Nobeyama 45m telescope. This paper presents a high-level overview of the basic structu…
The Atacama Large Aperture Submillimeter Telescope (AtLAST): enabling large-scale sub-mm science beyond 2030
Institute of Theoretical Astrophysics, University of Oslo（奥斯陆大学理论天体物理研究所）；Institute of Space Sciences (ICE-CSIC)（空间科学研究所（ICE-CSIC））；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究学院（IEEC））；Instituto de Astrofísica de Canarias (IAC)（加那利群岛天体物理研究所（IAC））；Departamento de Astrofísica, Universidad de La Laguna（拉古纳大学天体物理学系）；European Southern Observatory (ESO)（欧洲南方天文台（ESO））；OHB Digital Connect（OHB数字连接公司）；Department of Technology Systems, University of Oslo（奥斯陆大学技术系统系）；MPIfR（马克斯·普朗克射电天文研究所）；UK Astronomy Technology Centre, Royal Observatory Edinburgh（英国天体技术中心，爱丁堡皇家天文台）；IPARCOS-UCM, Universidad Complutense de Madrid（马德里康普顿斯大学IPARCOS研究中心）；Department of EEC Engineering, University of Pretoria（比勒陀利亚大学电气工程与电子工程系）；University of Tokyo（东京大学）；INAF Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）；Nagoya University（名古屋大学）；Rosseland Centre for Solar Physics, University of Oslo（奥斯陆大学罗斯兰太阳物理中心）；ESO（欧洲南方天文台）；ICREA（加泰罗尼亚卓越研究奖计划）；Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM（巴黎萨克雷大学、巴黎西岱大学、法国原子能和替代能源委员会、法国国家科学研究中心、AIM）；TU Delft（代尔夫特理工大学）
