EMISSION-LINE GALAXIES FROM THE PEARS HUBBLE ULTRA DEEP FIELD: A 2D DETECTION METHOD AND FIRST RESULTS
EMISSION-LINE GALAXIES FROM THE PEARS HUBBLE ULTRA DEEP FIELD: A 2D DETECTION METHOD AND FIRST RESULTS
复制标题
来自梨哈勃超深场的发射线星系：二维探测方法和初步结果
DOI：
10.1088/0004-6256/135/4/1624
复制
发表时间：
2008
期刊：
影响因子：
--
通讯作者：
S. D. Alighieri
中科院分区：
文献类型：
--
作者：
A. Straughn;G. Meurer;N. Pirzkal;S. Cohen;S. Malhotra;J. Rhoads;R. Windhorst;J. Gardner;N. Hathi;Chun Xu;C. Gronwall;A. Koekemoer;J. Walsh;S. D. Alighieri
哈勃空间望远镜高级巡天照相机的棱镜探测演化和再电离光谱（PEARS）巡天提供了一个大型数据集，其中包含来自GOODS南北场数千个星系的低分辨率光谱。这些数据中的一个重要的对象子集是发射线星系（ELG），我们已经研究了几种不同的方法，旨在系统地选择这些星系。在这里，我们提出了一种新的方法和结果的搜索这些ELG在PEARS观测的哈勃超深场（HUDF）使用的2D检测方法，利用观测，许多发射线起源于星系内的clueroscles结。这种二维线发现的方法被证明是有用的，在检测发射线从星系内的紧凑的结，否则可能无法检测到使用更传统的一维线发现技术。我们发现在HUDF中共有96条发射线，来自63个星系内的81个不同的“结”。我们发现，一般来说，[O iii]发射体是最常见的，占样品的44%，平均具有高等效宽度（70%的[O iii]发射体具有静止帧EW>100 μ m）。有12个星系有多个发射结，不同的发射结表现出不同的通量值，这表明在一个星系中不同的恒星形成特性通常可以在红移0.2-0.4的范围内进行探测。最普遍的形态是大的面对螺旋和cluerous相互作用的系统，许多是独特的检测，由于这里描述的2D方法，从而突出了这种技术的优势。
The Hubble Space Telescope Advanced Camera for Surveys grism Probing Evolution And Reionization Spectroscopically (PEARS) survey provides a large dataset of low-resolution spectra from thousands of galaxies in the GOODS north and south fields. One important subset of objects in these data is emission-line galaxies (ELGs), and we have investigated several different methods aimed at systematically selecting these galaxies. Here, we present a new methodology and results of a search for these ELGs in the PEARS observations of the Hubble Ultra Deep Field (HUDF) using a 2D detection method that utilizes the observation that many emission lines originate from clumpy knots within galaxies. This 2D line-finding method proves to be useful in detecting emission lines from compact knots within galaxies that might not otherwise be detected using more traditional 1D line-finding techniques. We find in total 96 emission lines in the HUDF, originating from 81 distinct “knots” within 63 individual galaxies. We find in general that [O iii] emitters are the most common, comprising 44% of the sample, and on average have high equivalent widths (70% of [O iii] emitters having rest-frame EW>100 Å). There are 12 galaxies with multiple emitting knots—with different knots exhibiting varying flux values, suggesting that the differing star-formation properties across a single galaxy can in general be probed at redshifts ≳0.2–0.4. The most prevalent morphologies are large face-on spirals and clumpy interacting systems, many being unique detections owing to the 2D method described here, thus highlighting the strength of this technique.