The Multi-Object, Fiber-Fed Spectrographs for SDSS and the Baryon Oscillation Spectroscopic Survey
Stephen Smee, James E. Gunn, Alan Uomoto, Natalie Roe, David Schlegel, Constance M. Rockosi, Michael A. Carr, French Leger, Kyle S. Dawson, Matthew D. Olmstead,… 展开作者
Stephen Smee, James E. Gunn, Alan Uomoto, Natalie Roe, David Schlegel, Constance M. Rockosi, Michael A. Carr, French Leger, Kyle S. Dawson, Matthew D. Olmstead, Jon Brinkmann, Russell Owen, Robert H. Barkhouser, Klaus Honscheid, Paul Harding, Dan Long, Robert H. Lupton, Craig Loomis, Lauren Anderson, James Annis, Mariangela Bernardi, Vaishali Bhardwaj, Dmitry Bizyaev, Adam S. Bolton, Howard Brewington, John W. Briggs, Scott Burles, James G. Burns, Francisco Castander, Andrew Connolly, James R. Davenport, Garrett Ebelke, Harland Epps, Paul D. Feldman, Scott Friedman, Joshua Frieman, Timothy Heckman, Charles L. Hull, Gillian R. Knapp, David M. Lawrence, Jon Loveday, Edward J. Mannery, Elena Malanushenko, Viktor Malanushenko, Aronne Merrelli, Demitri Muna, Peter Newman, Robert C. Nichol, Daniel Oravetz, Kaike Pan, Adrian C. Pope, Paul G. Ricketts, Alaina Shelden, Dale Sandford, Walter Siegmund, Audrey Simmons, D. Smith, Stephanie Snedden, Donald P. Schneider, Michael Strauss, Mark SubbaRao, Christy Tremonti, Patrick Waddell, Donald G. York
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43 pages, 42 figures, revised according to referee report and accepted by AJ. Provides background for the instrument responsible for SDSS and BOSS spectra. 4th in a series of survey technical papers released in Summer 2012, including arXiv:1207.7137 (DR9), arXiv:1207.7326 (Spectral Classification), and arXiv:1208.0022 (BOSS Overview)
We present the design and performance of the multi-object fiber spectrographs for the Sloan Digital Sky Survey (SDSS) and their upgrade for the Baryon Oscillation Spectroscopic Survey (BOSS). Originally commissioned in Fall 1999 on the 2.5-m aperture Sloan Telescope at Apache Point Observatory, the spectrographs produced more than 1.5 million spectra for the SDSS and SDSS-II surveys, enabling a wide variety of Galactic and extra-galactic science including the first observation of baryon acoustic oscillations in 2005. The spectrographs were upgraded in 2009 and are currently in use for BOSS, the flagship survey of the third-generation SDSS-III project. BOSS will measure redshifts of 1.35 million massive galaxies to redshift 0.7 and Lyman-alpha absorption of 160,000 high redshift quasars over 10,000 square degrees of sky, making percent level measurements of the absolute cosmic distance scale of the Universe and placing tight constraints on the equation of state of dark energy.
The twin multi-object fiber spectrographs utilize a simple optical layout with reflective collimators, gratings, all-refractive cameras, and state-of-the-art CCD detectors to produce hundreds of spectra simultaneously in two channels over a bandpass covering the near ultraviolet to the near infrared, with a resolving power R = λ/FWHM ~ 2000. Building on proven heritage, the spectrographs were upgraded for BOSS with volume-phase holographic gratings and modern CCD detectors, improving the peak throughput by nearly a factor of two, extending the bandpass to cover 360 < λ< 1000 nm, and increasing the number of fibers from 640 to 1000 per exposure. In this paper we describe the original SDSS spectrograph design and the upgrades implemented for BOSS, and document the predicted and measured performances.
The Tartu Observatory Fiber-fed Echelle Spectrograph (TOFES) Data Reduction Pipeline
Tartu Observatory, University of Tartu（塔尔图大学塔尔图天文台）；Space Research Institute, Austrian Academy of Sciences（奥地利科学院空间研究所）；Institute for Theoretical and Computation Physics, Graz University of Technology（格拉茨工业大学理论与计算物理研究所）；Department of Physics and Astronomy, Uppsala University（乌普萨拉大学物理与天文学系）；Department of Physics and Astronomy, University College London（伦敦大学学院物理与天文学系）；European Southern Observatory（欧洲南方天文台）
Studying focal ratio degradation of optical fibers for Subaru Prime Focus Spectrograph
聚焦比退化（FRD）是由纤维光学引起的光角分布的变化。FRD对于光纤馈电的光谱天文系统很重要，因为它会导致信号丢失、光谱分辨率下降或光谱仪设计复杂性增加。Nacional de Astrofísica（LNA）开发了一种系统，可以准确和精确地测量FRD，使用绝对方法，也可以测量光纤吞吐量。本文介绍了计量系统，并显示了Polymicro纤维FBP129168190，FBP127165190和藤仓纤维128170190的测量。虽然这两种光纤的FRD很低，并且彼此相似，但了解这些光纤的确切特性非常重要，因为它们都将用于建造FOCCoS（光纤电缆和连接器系统），用于安装在斯巴鲁望远镜上的PFS（主焦点光谱仪）。
精确的多普勒径向速度（RV）仪器将继续在推进我们对系外行星系统的全面理解方面发挥重要作用。从过境调查和后续RV测量的轨道参数的组合是至关重要的解锁质量和密度估计检测到的行星，让我们深入了解他们的环境和结构。然而，系外行星领域正处于一个关键时刻：现有径向速度仪器的测量灵敏度正在成为进一步增加我们知识的限制因素。如果不提高RV测量精度，我们将无法为新的凌日任务（包括凌日系外行星勘测卫星（TESS））预期的一些最令人兴奋（因此也是最具挑战性）的发现提供动态质量和密度估计（Plavchan et al. 2015，Ricker et al. 2014）。RV的精度需要达到10厘米/秒的水平，以充分确认类似地球的类似物，提供质量并测量这些任务的密度到1-5%的水平。此外，这种RV能力对于詹姆斯韦伯太空望远镜（JWST）等设施的有效目标选择也很重要。实现这一目标的一个有希望的方法是使用单模光纤将光注入光谱仪。这减轻了当前一代视见受限RV仪器面临的许多误差项，同时在较小的光学足迹内提供了高分辨率光谱的能力（Schwab等人，2012年; Crepp 2014年; Jovanovic等人，2016年a）。我们讨论了这种技术的好处，它的挑战，以及目前的发展状况。
ANDES, the high-resolution spectrograph for the ELT: design and performance analysis of the YJH spectrograph
UK Astronomy Technology Centre, Royal Observatory Edinburgh（英国天文学技术中心，爱丁堡皇家天文台）；Université de Montréal（蒙特利尔大学）；Université Laval（拉瓦尔大学）；Cavendish Laboratory, University of Cambridge（剑桥大学卡文迪许实验室）；Uppsala University（乌普萨拉大学）；INAF – Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；INAF - Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）
Design and development of a near-IR integral field spectrograph for the HWO Coronagraph Instrument
UKATC, Royal Observatory Edinburgh（英国天文技术中心，爱丁堡皇家天文台）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天体物理研究所）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）
Commissioning and on-sky performance of FiberPol: a fiber-fed spectropolarimetric system for the SAAO 1.9 m telescope
South African Astronomical Observatory（南非天文台）；Sub-department of Astrophysics, University of Oxford（牛津大学天体物理子系）；Department of Astronomy, University of Cape Town（开普敦大学天文学系）；Space Science and Engineering Initiative, College of Engineering, University of Hawaii at Manoa（夏威夷大学马诺阿分校工程学院空间科学与工程倡议）；Centre for Space Research, North-West University（西北大学空间研究中心）；University of Wisconsin–Madison（威斯康星大学麦迪逊分校）
