DYNAMICAL STRUCTURE OF THE MOLECULAR INTERSTELLAR MEDIUM IN AN EXTREMELY BRIGHT, MULTIPLY LENSED z ≃ 3 SUBMILLIMETER GALAXY DISCOVERED WITH HERSCHEL
DYNAMICAL STRUCTURE OF THE MOLECULAR INTERSTELLAR MEDIUM IN AN EXTREMELY BRIGHT, MULTIPLY LENSED z ≃ 3 SUBMILLIMETER GALAXY DISCOVERED WITH HERSCHEL
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赫歇尔发现的极亮多重透镜 z ≃ 3 亚毫米星系中分子星际介质的动态结构
DOI：
10.1088/2041-8205/733/1/l12
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发表时间：
2011
期刊：
影响因子：
--
通讯作者：
G. Wright
中科院分区：
文献类型：
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作者：
D. Riechers;A. Cooray;A. Omont;R. Neri;A. Harris;A. Baker;P. Cox;D. Frayer;J. Carpenter;R. Auld;H. Aussel;A. Beelen;R. Blundell;J. Bock;D. Brisbin;D. Burgarella;P. Chanial;S. Chapman;D. Clements;A. Conley;C. Dowell;S. Eales;D. Farrah;A. Franceschini;R. Gavazzi;J. Glenn;M. Griffin;M. Gurwell;R. Ivison;S. Kim;M. Krips;A. Mortier;S. Oliver;M. Page;A. Papageorgiou;C. Pearson;I. Pérez;M. Pohlen;J. Rawlings;G. Raymond;G. Rodighiero;I. Roseboom;M. Rowan‐Robinson;K. Scott;N. Seymour;A. Smith;M. Symeonidis;K. Tugwell;Mattia Vaccari;J. Vieira;L. Vigroux;L. Wang;J. Wardlow;G. Wright
报道了用高原德布雷干涉仪、毫米波天文研究组合阵列和绿岸望远镜在强透镜、赫歇尔/尖顶选择的亚毫米级星系Hermes J105751.1+573027中探测到的CO(J=5→4)、CO(J=3→2)和CO(J=1→0)发射，z=2.9574±0.0001。这些观测在空间上将分子气体分解成四个透镜图像，最大分离度为∼9“，并揭示了该系统中的内部气体动力学。得到了经透镜校正后的L钴(1-0)=(4.17±0.41)，L钴(3-2)=(3.96±0.20)，L钴(5-4)=(3.45±0.20)×10~(10) (μL/10.9−1K km S−_1PC_2的CO谱线发光度，对应的发光度比分别为R31=0.95±0.10，R53=0.87±0.06，R51=0.83±0.09。由此推算出MGA的总分子气质量为3.3×10 10(αCO/0.8)(μL/10.9)−1 M☉。气体质量、气体质量分数、气体耗尽时间尺度、恒星形成效率和比恒星形成率是SMG的典型特征。气藏的速度结构表明，最亮的两个透镜图像是银河系中同一尘埃遮挡区域的动态分辨率投影，它们在运动学上偏离了未分辨率较暗的图像。解析的运动学似乎与在主要的“湿”(即，富气)合并中观察到的复杂的速度结构一致。大型合并在SMG中很常见，很可能是在高耗气率下助长其强烈星暴的原因。这项研究表明，通过利用引力透镜提供的有效空间分辨率和灵敏度的增加，可以研究早期宇宙中的星系的详细程度。
We report the detection of CO(J = 5 → 4), CO(J = 3 → 2), and CO(J = 1 → 0) emission in the strongly lensed, Herschel/SPIRE-selected submillimeter galaxy (SMG) HERMES J105751.1+573027 at z = 2.9574 ± 0.0001, using the Plateau de Bure Interferometer, the Combined Array for Research in Millimeter-wave Astronomy, and the Green Bank Telescope. The observations spatially resolve the molecular gas into four lensed images with a maximum separation of ∼9″ and reveal the internal gas dynamics in this system. We derive lensing-corrected CO line luminosities of L′CO(1–0) = (4.17 ± 0.41), L′CO(3–2) = (3.96 ± 0.20), and L′CO(5–4) = (3.45 ± 0.20) × 1010 (μL/10.9)−1 K km s−1 pc2, corresponding to luminosity ratios of r31 = 0.95 ± 0.10, r53 = 0.87 ± 0.06, and r51 = 0.83 ± 0.09. This suggests a total molecular gas mass of Mgas = 3.3×1010 (αCO/0.8) (μL/10.9)−1 M☉. The gas mass, gas mass fraction, gas depletion timescale, star formation efficiency, and specific star formation rate are typical for an SMG. The velocity structure of the gas reservoir suggests that the brightest two lensed images are dynamically resolved projections of the same dust-obscured region in the galaxy that are kinematically offset from the unresolved fainter images. The resolved kinematics appear consistent with the complex velocity structure observed in major, “wet” (i.e., gas-rich) mergers. Major mergers are commonly observed in SMGs and are likely to be responsible for fueling their intense starbursts at high gas consumption rates. This study demonstrates the level of detail to which galaxies in the early universe can be studied by utilizing the increase in effective spatial resolution and sensitivity provided by gravitational lensing.
DOI：
10.1088/2041-8205/720/2/l131
发表时间：
2010-08
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
D. Riechers;P. Capak;C. Carilli;P. Cox;R. Neri;N. Scoville;E. Schinnerer;F. Bertoldi;Lin Yan
通讯作者：
D. Riechers;P. Capak;C. Carilli;P. Cox;R. Neri;N. Scoville;E. Schinnerer;F. Bertoldi;Lin Yan