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The Lamost Survey of Background Quasars in the Vicinity of the Andromeda and Triangulum Galaxies

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The Lamost Survey of Background Quasars in the Vicinity of the Andromeda and Triangulum Galaxies The Astronomical Journal, 145:159 (8pp), 2013 June doi:10.1088/0004-6256/145/6/159 C 2013. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE LAMOST SURVEY OF BACKGROUND QUASARS IN THE VICINITY OF THE ANDROMEDA AND TRIANGULUM GALAXIES. II. RESULTS FROM THE COMMISSIONING OBSERVATIONS AND THE PILOT SURVEYS Zhi-Ying Huo1,Xiao-WeiLiu2,3, Mao-Sheng Xiang3,Hai-BoYuan2,8, Yang Huang3, Hui-Hua Zhang3,LinYan4, Zhong-Rui Bai1, Jian-Jun Chen1, Xiao-Yan Chen1, Jia-Ru Chu5, Yao-Quan Chu5, Xiang-Qun Cui6,BingDu1, Yong-Hui Hou6, Hong-Zhuan Hu5, Zhong-Wen Hu6,LeiJia1, Fang-Hua Jiang6, Ya-Juan Lei1,Ai-HuaLi6, Guang-Wei Li1,Guo-PingLi6,JianLi1,Xin-NanLi6,YanLi7, Ye-Ping Li6, Gen-Rong Liu6, Zhi-Gang Liu5,Qi-ShuaiLu6, A-Li Luo1, Yu Luo1,LiMen1, Ji-Jun Ni6, Yong-Jun Qi6, Zhao-Xiang Qi7, Jian-Rong Shi1, Huo-Ming Shi1, Shi-Wei Sun1, Zheng-Hong Tang7,YuanTian1, Liang-Ping Tu1,DanWang1, Feng-Fei Wang1, Gang Wang1, Jia-Ning Wang6, Lei Wang6, Shu-Qing Wang1,YouWang6, Yue-Fei Wang6, Ming-Zhi Wei1,YueWu1, Xiang-Xiang Xue1, Zheng-Qiu Yao6,YongYu7,HuiYuan1, Chao Zhai5, En-Peng Zhang1, Hao-Tong Zhang1, Jian-Nan Zhang1, Wei Zhang1, Yan-Xia Zhang1, Yong Zhang6, Zhen-Chao Zhang6, Gang Zhao1, Ming Zhao7, Yong-Heng Zhao1, Fang Zhou6, Xin-Lin Zhou1, Yong-Tian Zhu6, and Si-Cheng Zou1 1 Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, P. R. China; [email protected] 2 Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, P. R. China 3 Department of Astronomy, Peking University, Beijing 100871, P. R. China 4 Infrared Processing and Analysis Center, California Institute of Technology, MS 100-22, Pasadena, CA 91125, USA 5 University of Science and Technology of China, Hefei 230026, P. R. China 6 Nanjing Institute of Astronomical Optics & Technology, National Astronomical Observatories, Chinese Academy of Sciences, Nanjing 210042, P. R. China 7 Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, P. R. China Received 2012 November 5; accepted 2013 April 7; published 2013 May 10 ABSTRACT We present new quasars discovered in the vicinity of the Andromeda and Triangulum galaxies with the Large Sky Area Multi-Object Fiber Spectroscopic Telescope, also named the Guoshoujing Telescope, during the 2010 and 2011 observational seasons. Quasar candidates are selected based on the available Sloan Digital Sky Survey, Kitt Peak National Observatory 4 m telescope, Xuyi Schmidt Telescope Photometric Survey optical, and Wide-field Infrared Survey Explorer near-infrared photometric data. We present 509 new quasars discovered in a stripe of ∼135 deg2 from M31 to M33 along the Giant Stellar Stream in the 2011 pilot survey data sets, and also 17 new quasars discovered in an area of ∼100 deg2 that covers the central region and the southeastern halo of M31 in the 2010 commissioning data sets. These 526 new quasars have i magnitudes ranging from 15.5 to 20.0, redshifts from 0.1 to 3.2. They represent a significant increase of the number of identified quasars in the vicinity of M31 and M33. There are now 26, 62, and 139 known quasars in this region of the sky with i magnitudes brighter than 17.0, 17.5, and 18.0, respectively, of which 5, 20, and 75 are newly discovered. These bright quasars provide an invaluable collection with which to probe the kinematics and chemistry of the interstellar/intergalactic medium in the Local Group of galaxies. A total of 93 quasars are now known with locations within 2◦.5 of M31, of which 73 are newly discovered. Tens of quasars are now known to be located behind the Giant Stellar Stream, and hundreds are behind the extended halo and its associated substructures of M31. The much enlarged sample of known quasars in the vicinity of M31 and M33 can potentially be utilized to construct a perfect astrometric reference frame to measure the minute proper motions (PMs) of M31 and M33, along with the PMs of substructures associated with the Local Group of galaxies. Those PMs are some of the most fundamental properties of the Local Group. Key words: galaxies: individual (M31, M33) – quasars: emission lines – quasars: general Online-only material: color figures, machine-readable and VO tables 1. INTRODUCTION associated substructures are vital for our understanding of M31, and also for the theory of galaxy formation and evolution in Being the most luminous member of the Local Group and general. the nearest archetypical spiral galaxy, M31 serves as the best Finding background quasars in the vicinity of M31 have the astrophysical laboratory for the studies of the physical and two following potential important applications. First, the back- astrophysical processes that govern the structure, kinematics ground quasars can serve as an ideal reference frame which and the formation and evolution of distant galaxies. Recent would allow highly accurate astrometric measurement of the deep optical surveys have revealed complex substructures within minute proper motion (PM) of M31 and also the PMs of its as- hundreds of kiloparsecs (kpc) of M31, with some of them sociated coherent substructures. Second, absorption-line spec- stretching from M31 all the way to M33, which is about 200 kpc troscopy of bright background quasars can be used to probe from M31, suggesting a possible recent close encounter of the the distribution, chemical composition, and kinematics of the two galaxies (Ibata et al. 2007; McConnachie et al. 2009). interstellar medium (ISM) of M31, the Milky Way, and the Detailed chemical and kinematic investigations of M31 and intergalactic medium (IGM) of the Local Group of galaxies. This technique can be used to probe structures further out from 8 LAMOST Fellow the center of the galaxy than would be possible with traditional 1 The Astronomical Journal, 145:159 (8pp), 2013 June Huo et al. stellar spectroscopy, or using H i 21 cm observations. In addi- et al. (1997) presented several quasar candidates. Until recently, tion, M31 has always been a focus of interest for astronomical Sloan Digital Sky Survey (SDSS; York et al. 2000) obtained 75 observations. Extensive photometric data spanning tens of years low-redshift quasars in three spectroscopic plates in two fields exist. Therefore, identifying background quasars in the vicinity in the outer halo of M31 (cf. Adelman-McCarthy et al. 2006, of M31 should also enable the construction of a valuable sample 2007). As far as we are aware, since 2007 no further observations for studying quasar variability. targeting quasars around M31 have been made by SDSS. The PM of M31 represents one of the most fundamental In the first of this series of papers we presented 14 new quantities of the Local Group, and its accurate measurement is quasars discovered with the Large Sky Area Multi-Object vital to the study of the formation, evolution, and dynamics Fiber Spectroscopic Telescope (LAMOST) during its early of the Local Group, in particular for quantifying the dark commissioning phase (see Huo et al. 2010, hereafter Paper I). matter content. M31 is known to be located at a distance of LAMOST is a quasi-meridian reflecting Schmidt telescope ∼785 kpc (McConnachie et al. 2005), and is moving toward the with an effective aperture of about 4 m and a field of view Milky Way with a velocity of 117 km s−1 (Binney & Tremaine of 5◦ in diameter (Wang et al. 1996;Suetal.1998;Xing 1987, p. 605). However, its transverse velocity has remained et al. 1998; Zhao 2000; Cui et al. 2004, 2010, 2012;Zhu unknown for a long time. The Very Long Baseline Array, with et al. 2006,seehttp://www.lamost.org/website/en/). Recording a PM measurement uncertainty of the order of 1 microarcsec, 4000 celestial object spectra simultaneously with a parallel fully has measured the distance and PM of M33 by water maser controllable fiber positioning system, LAMOST is the telescope observations (Brunthaler et al. 2005). However, water maser with the highest rate of spectral acquisition at the present sources in M31 have been discovered only recently (Darling time. After a period of two years of commissioning for the 2011); thus we do not yet have a long enough time baseline for a purpose of technical fine-tuning, performance characterization meaningful PM measurement. Based on kinematic information and optimization, as well as scientific capability demonstration, about M31’s satellite galaxies, M33 and IC10, Loeb et al. (2005) the LAMOST pilot surveys were initiated in 2011 October and and van der Marel & Guhathakurta (2008) deduced theoretical completed in spring the following year (see Zhao et al. 2012). In estimates for the PM of M31 of about 80 km s−1 (20 μas yr−1). this paper, we report newly discovered background quasars in Sohn et al. (2012) presented the first direct PM measurements the vicinity of M31 and M33, based on LAMOST data obtained for three M31 fields (∼2.7 × 2.7 arcmin2 for each field) using during the commissioning phase of 2010 as well as during the Hubble Space Telescope observations that span a time baseline pilot surveys from autumn 2011 to spring 2012. of 5–7 yr. Due to the sparseness of known background quasars, their analysis had to resort to using compact background 2. CANDIDATE SELECTION galaxies as reference sources, even though it was hard to obtain With the aim of searching for background quasars in the highly accurate positions for those galaxies given their nature vicinity of M31 and M33, we selected quasar candidates based as extended sources. Being essentially point sources with zero on the available optical, near-infrared (IR) photometric data in PMs, background quasars can serve as perfect reference sources the extended area of M31 and M33.
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