SDSS-V local volume mapper instrument: overview and status
SDSS-V local volume mapper instrument: overview and status
复制标题
SDSS-V 局部体积映射仪：概述和状态
DOI：
10.1117/12.2557565
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发表时间：
2020
期刊：
影响因子：
--
通讯作者：
R. Yan
中科院分区：
文献类型：
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作者：
N. Konidaris;N. Drory;C. Froning;Anthony Hebert;P. Bilgi;G. Blanc;A. Lanz;C. Hull;J. Kollmeier;S. Ramírez;S. Wachter;K. Kreckel;S. Pak;E. Pellegrini;Andr'es Almeida;S. Case;R. Zhelem;T. Feger;J. Lawrence;M. Lesser;T. Herbst;J. Sánchez;M. Bershady;Sabyasachi Chattopadhyay;A. Hauser;Michael P. Smith;M. Wolf;R. Yan
斯隆数字巡天V(SDSS-V)是对600万个天体的全天光谱观测，旨在破译银河系的历史，揭示恒星的内部运作，调查太阳系的起源，并跟踪整个宇宙中超大质量黑洞的增长。当地体积测绘仪(LVM)是一种设备，旨在从智利的拉斯坎帕纳斯天文台提供连续的2,500°2积分野外调查，为期3.5年。在这篇文章中，我们提供了LVM仪器(下称LVM-I)的概述和状态更新。每个积分场单位的象素探测亚帕秒(银河系)到∼10 pC(麦哲伦云)的线性尺度，角直径为36.900。LVM的光谱分辨率为R=λ/∆λ∼4000，探测从365 nm到950 nm的33千米−1(1σ)的速度。LVM使用四个16厘米的望远镜为三个光谱仪提供食物。其中一个望远镜承载了大部分科学负载，∼1,800根光纤通过一对小透镜阵列耦合到场上，两个望远镜用于测量科学场两侧田野的夜空光谱，第四个望远镜同时监测明亮的标准恒星，以确定大气消光。我们希望LVM-I能够在重要的线比上提供百分比级别的精度，低至几个瑞利。这三台光谱仪是由法国Winlight公司在暗能量光谱仪(DESI)的基础上建造的。本文介绍了LVM-I的高层次系统设计，包括微透镜耦合光纤IFU、望远镜、制导+捕获系统、定标系统、外壳和光谱仪。
The Sloan Digital Sky Survey V (SDSS-V) is an all-sky spectroscopic survey of <6 million objects, designed to decode the history of the Milky Way, reveal the inner workings of stars, investigate the origin of solar systems, and track the growth of supermassive black holes across the Universe. The Local Volume Mapper (LVM) is a facility designed to provide a contiguous 2,500 deg2 integral-field survey over a 3.5 year period from Las Campanas Observatory in Chile. In this paper we provide an overview and status update for the LVM instrument (hereafter LVM-I). Each integral-field unit’s spaxel probes linear scales that are sub-parsec (Milky Way) to ∼10 pc (Magellanic Clouds) which is accomplished with an angular diameter of 36.900. LVM’s spectral resolution is R = λ/∆λ ∼ 4, 000 which probes velocities of 33 kms−1 (1 σ) from 365 nm to 950 nm. LVM uses four 16-cm telescopes feeding three spectrographs. One telescope carries the bulk of the science load with ∼1,800 fibers coupled to the field via a pair of lenslet arrays, two telescopes are used to measure the night sky spectra in fields that flank the science field, and a fourth telescope contemporaneously monitors bright standard stars to determine atmospheric extinction. We expect LVM-I to deliver percent-level precision on important line ratios down to a few Rayleigh. The three spectrographs are being built by Winlight corporation in France based on those for the Dark Energy Spectroscopic Instrument (DESI). In this paper we present the high-level system design of LVM-I including the lenslet-coupled fiber IFUs, telescopes, guiding+acquisition system, calibration systems, enclosures, and spectrographs.
DOI：
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发表时间：
2016-10
期刊：
arXiv: Instrumentation and Methods for Astrophysics
影响因子：
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作者：
Desi Collaboration Amir Aghamousa;J. Aguilar;S. Ahlen;S. Alam;L. Allen;C. Prieto;J. Annis;S. Bailey-S
通讯作者：
Desi Collaboration Amir Aghamousa;J. Aguilar;S. Ahlen;S. Alam;L. Allen;C. Prieto;J. Annis;S. Bailey-S