OMEGA - OSIRIS Mapping of Emission-line Galaxies in A901/2 - I. Survey description, data analysis, and star formation and AGN activity in the highest density regions
OMEGA - OSIRIS Mapping of Emission-line Galaxies in A901/2 - I. Survey description, data analysis, and star formation and AGN activity in the highest density regions
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OMEGA - A901/2 中发射线星系的 OSIRIS 测绘 - I. 勘测描述、数据分析以及最高密度区域中的恒星形成和 AGN 活动
DOI：
10.1093/mnras/stv779
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发表时间：
2015
影响因子：
4.8
通讯作者：
Chies-Santos A
中科院分区：
文献类型：
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作者：
Chies-Santos A
我们介绍了OMEGA（OSIRIS Mapping of Emission-line Galerkin in the multicluster system A901/2）巡天的概况和初步结果。这个项目的最终目标是研究星星的形成和活动星系核（AGN）的活动在一个单一的红移范围广泛的环境。利用Gran Telescopio Canarias上的成像光学系统和低中分辨率集成光谱仪（OSIRIS）的可调谐滤波器模式，我们在包含z = 0.167多集群系统A901/2的0.5 × 0.5 deg 2区域内对H α和$[N}\，\small {II}]$发射线进行了目标定位。在本文中，我们描述了设计的调查，观察和数据分析技术的发展。然后，我们提出了早期的结果，从两个OSIRIS点集中在核心的A901 a和A902集群。活动星系核和恒星形成（SF）天体是用$[N}\，\small {II}]\，/\，\mathrm{H}\，\alpha$ versusWH α诊断图来识别的。活动星系核的宿主比SF星系更亮、更大质量，并且具有更早的类型形态。这两个种群都倾向于位于我们研究的高密度地区的郊区。这些源的典型H α光度明显低于红移相似的场星系，但大于A1689，一个Z = 0.2的富星系团。我们的天体的H α光度转换为星星形成率（SFR）在0.02到6兆年之间。比较恒星质量和H α导出的SFR之间的关系与在野外发现的结果表明，在星团的核心中，星星的形成受到抑制。这些发现与以前基于其他星星形成指标对这种多星团结构的研究一致，并证明了可调滤波器在这种研究中的作用。
We present an overview of and first results from the OMEGA (OSIRIS Mapping of Emission-line Galaxies in the multicluster system A901/2) survey. The ultimate goal of this project is to study star formation and active galactic nucleus (AGN) activity across a broad range of environments at a single redshift. Using the tuneable-filter mode of the Optical System for Imaging and low-Intermediate-Resolution Integrated Spectroscopy (OSIRIS) instrument on Gran Telescopio Canarias, we target H α and $[\mathrm{N}\,\small {II}]$ emission lines over an ∼0.5 × 0.5 deg2region containing thez∼ 0.167 multicluster system A901/2. In this paper, we describe the design of the survey, the observations and the data analysis techniques developed. We then present early results from two OSIRIS pointings centred on the cores of the A901a and A902 clusters. AGN and star-forming (SF) objects are identified using the $[\mathrm{N}\,\small {II}]\,/\,\mathrm{H}\,\alpha$ versusWH αdiagnostic diagram. The AGN hosts are brighter, more massive, and possess earlier type morphologies than SF galaxies. Both populations tend to be located towards the outskirts of the high-density regions we study. The typical H α luminosity of these sources is significantly lower than that of field galaxies at similar redshifts, but greater than that found for A1689, a rich cluster atz∼ 0.2. The H α luminosities of our objects translate into star formation rates (SFRs) between ∼0.02 and 6 M⊙yr−1. Comparing the relationship between stellar mass and H α-derived SFR with that found in the field indicates a suppression of star formation in the cores of the clusters. These findings agree with previous investigations of this multicluster structure, based on other star formation indicators, and demonstrate the power of tuneable filters for this kind of study.