The BLAST Observatory: A Sensitivity Study for Far-IR Balloon-borne Polarimeters

IF 3.3 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS Publications of the Astronomical Society of the Pacific Pub Date : 2024-03-27 DOI:10.1088/1538-3873/ad2e11
Gabriele Coppi, Simon Dicker, James E. Aguirre, Jason E. Austermann, James A. Beall, Susan E. Clark, Erin G. Cox, Mark J. Devlin, Laura M. Fissel, Nicholas Galitzki, Brandon S. Hensley, Johannes Hubmayr, Sergio Molinari, Federico Nati, Giles Novak, Eugenio Schisano, Juan D. Soler, Carole E. Tucker, Joel N. Ullom, Anna Vaskuri, Michael R. Vissers, Jordan D. Wheeler, Mario Zannoni, (The BLAST Observatory Collaboration)
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Abstract

Sensitive wide-field observations of polarized thermal emission from interstellar dust grains will allow astronomers to address key outstanding questions about the life cycle of matter and energy driving the formation of stars and the evolution of galaxies. Stratospheric balloon-borne telescopes can map this polarized emission at far-infrared wavelengths near the peak of the dust thermal spectrum—wavelengths that are inaccessible from the ground. In this paper we address the sensitivity achievable by a Super Pressure Balloon polarimetry mission, using as an example the Balloon-borne Large Aperture Submillimeter Telescope (BLAST) Observatory. By launching from Wanaka, New Zealand, the BLAST Observatory can obtain a 30 days flight with excellent sky coverage—overcoming limitations of past experiments that suffered from short flight duration and/or launch sites with poor coverage of nearby star-forming regions. This proposed polarimetry mission will map large regions of the sky at sub-arcminute resolution, with simultaneous observations at 175, 250, and 350 μm, using a total of 8274 microwave kinetic inductance detectors. Here, we describe the scientific motivation for the BLAST Observatory, the proposed implementation, and the forecasting methods used to predict its sensitivity. We also compare our forecasted experiment sensitivity with other facilities.
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BLAST 天文台:远红外气球载极地测量仪灵敏度研究
对星际尘粒的偏振热辐射进行灵敏的宽视场观测,将使天文学家能够解决有关物质和能量生命周期驱动恒星形成和星系演化的关键未决问题。平流层气球载望远镜可以在尘埃热光谱峰值附近的远红外波段绘制这种偏振发射图--这些波段是地面无法到达的。本文以气球载大孔径亚毫米波望远镜(BLAST)天文台为例,探讨了超压气球偏振测量任务所能达到的灵敏度。BLAST 观测站从新西兰的瓦纳卡发射,可以获得 30 天的飞行时间和极好的天空覆盖范围--克服了以往实验因飞行时间短和/或发射地点对附近恒星形成区覆盖范围小而受到的限制。这项拟议中的偏振测量任务将利用总共 8274 个微波动感探测器,以亚arcminute 分辨率绘制大面积天空,同时在 175、250 和 350 μm 波段进行观测。在此,我们将介绍 BLAST 天文台的科学动机、拟议的实施方案以及用于预测其灵敏度的预测方法。我们还将我们预测的实验灵敏度与其他设施进行了比较。
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来源期刊
Publications of the Astronomical Society of the Pacific
Publications of the Astronomical Society of the Pacific 地学天文-天文与天体物理
CiteScore
6.70
自引率
5.70%
发文量
103
审稿时长
4-8 weeks
期刊介绍: The Publications of the Astronomical Society of the Pacific (PASP), the technical journal of the Astronomical Society of the Pacific (ASP), has been published regularly since 1889, and is an integral part of the ASP''s mission to advance the science of astronomy and disseminate astronomical information. The journal provides an outlet for astronomical results of a scientific nature and serves to keep readers in touch with current astronomical research. It contains refereed research and instrumentation articles, invited and contributed reviews, tutorials, and dissertation summaries.
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