The e-MERGE Survey (e-MERLIN Galaxy Evolution Survey): overview and survey description
The e-MERGE Survey (e-MERLIN Galaxy Evolution Survey): overview and survey description
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e-MERGE 调查（e-MERLIN 星系演化调查）：概述和调查说明
DOI：
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发表时间：
2020
影响因子：
4.8
通讯作者：
T. Venturi
中科院分区：
文献类型：
--
作者：
T. Muxlow;A. Thomson;J. Radcliffe;N. Wrigley;R. Beswick;I. Smail;I. McHardy;S. Garrington;R. Ivison;M. Jarvis;I. Prandoni;M. Bondi;D. Guidetti;M. Argo;D. Bacon;P. Best;A. Biggs;S. Chapman;K. Coppin;H. Chen;T. Garratt;M. Garrett;E. Ibar;J. Kneib;K. Knudsen;L. Koopmans;L. Morabito;E. Murphy;A. Njeri;C. Pearson;M. Pérez;A. Richards;H. Röttgering;M. Sargent;S. Serjeant;C. Simpson;J. Simpson;A. M. Swinbank;E. Varenius;T. Venturi
我们提出了一个概述和描述的e-MERGE调查（e-MERLIN银河系演化调查）数据发布1（DR 1），一个大型计划的高分辨率1.5 GHz的无线电观测的GOODS-N字段包括140小时的观测与增强多元素远程链接干涉仪网络（e-MERLIN）和140小时的超大型阵列（VLA）。我们联合收割机结合了e-MERLIN的长基线（提供高角度分辨率）与VLA的相对紧密包装的天线（提供出色的表面亮度灵敏度）进行深度1.5 GHz无线电测量，灵敏度（${\sim}1.5\，\mu$ Jy beam−1），角分辨率（0.2-0.7弧秒）和视场（15 × 15弧分2），以探测和空间分辨恒星形成星系和活动星系核（AGN）。e-MERGE的目标是对SKA 1-mid将调查的深亚弧秒无线电天空提供新的限制。在这份最初的出版物中，我们讨论了我们的数据分析技术，包括采取步骤来模拟在20年的基线和新的点扩散函数/初级光束模型的发展，无缝地合并e-MERLIN和VLA数据在紫外线平面上的光束源的变化。我们提出了早期的科学成果，包括测量的光度和/或线性大小的1.5 GHz的10000个星系选择。结合哈勃太空望远镜的观测，我们测量到的平均射电-光学尺寸比为re-MERGE/rHST = 1.02 ± 0.03，这表明在大多数高红移星系中，1.0GHz的连续辐射跟踪光学成像中看到的恒星光。这是一系列论文中的第一篇，这些论文将探索e-MERGE DR 1观测到的GOODS-N场中恒星形成星系和活动星系核的射电性质。
We present an overview and description of the e-MERGE Survey (e-MERLIN Galaxy Evolution Survey) Data Release 1 (DR1), a large program of high-resolution 1.5-GHz radio observations of the GOODS-N field comprising ∼140 h of observations with enhanced-Multi-Element Remotely Linked Interferometer Network (e-MERLIN) and ∼40 h with the Very Large Array (VLA). We combine the long baselines of e-MERLIN (providing high angular resolution) with the relatively closely packed antennas of the VLA (providing excellent surface brightness sensitivity) to produce a deep 1.5-GHz radio survey with the sensitivity (${\sim}1.5\, \mu$ Jy beam−1), angular resolution (0.2–0.7 arcsec) and field-of-view (∼15 × 15 arcmin2) to detect and spatially resolve star-forming galaxies and active galactic nucleus (AGN) at $z$ ≳ 1. The goal of e-MERGE is to provide new constraints on the deep, sub-arcsecond radio sky which will be surveyed by SKA1-mid. In this initial publication, we discuss our data analysis techniques, including steps taken to model in-beam source variability over an ∼20-yr baseline and the development of new point spread function/primary beam models to seamlessly merge e-MERLIN and VLA data in the uv plane. We present early science results, including measurements of the luminosities and/or linear sizes of ∼500 galaxies selected at 1.5 GHz. In combination with deep Hubble Space Telescope observations, we measure a mean radio-to-optical size ratio of re-MERGE/rHST ∼ 1.02 ± 0.03, suggesting that in most high-redshift galaxies, the ∼GHz continuum emission traces the stellar light seen in optical imaging. This is the first in a series of papers that will explore the ∼kpc-scale radio properties of star-forming galaxies and AGN in the GOODS-N field observed by e-MERGE DR1.
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VLA-COSMOS 3 GHz 大型项目：高度恒星形成星系的平均射电频谱能量分布
影响因子：
6.5
作者：
Tisanić;Smolčić;Delhaize
通讯作者：
Delhaize
影响因子：
6.5
作者：
E. F. Jim'enez-Andrade;B. Magnelli;A. Karim;G. Zamorani;M. Bondi;E. Schinnerer;M. Sargent;E. Romano-D'iaz;M. Novak;P. Lang;F. Bertoldi;E. Vardoulaki;S. Toft;V. Smolčić;K. Harrington;S. Leslie;J. Delhaize;Daizhong Liu;C. Karoumpis;J. Kartaltepe;A. Koekemoer
通讯作者：
E. F. Jim'enez-Andrade;B. Magnelli;A. Karim;G. Zamorani;M. Bondi;E. Schinnerer;M. Sargent;E. Romano-D'iaz;M. Novak;P. Lang;F. Bertoldi;E. Vardoulaki;S. Toft;V. Smolčić;K. Harrington;S. Leslie;J. Delhaize;Daizhong Liu;C. Karoumpis;J. Kartaltepe;A. Koekemoer
影响因子：
4.8
作者：
M. Swinbank;J. Simpson;I. Smail;C. Harrison;J. Hodge;A. Karim;F. Walter;D. Alexander;N. Brandt;C. Breuck;E. D. Cunha;S. Chapman;K. Coppin;A. Danielson;H. Dannerbauer;Roberto Decarli Thomas Greve;R. Ivison;K. Knudsen;C. Lagos;E. Schinnerer;A. Thomson;J. Wardlow;A. Weiss;Paul van der Werf Icc;Durham;Heidelberg;Bonn;Penn State;Eső;Dalhousie;Hertfordshire;Vienna;Ucl;Ifa;Edinburgh;Chalmers;UC Irvine;Leiden
通讯作者：
M. Swinbank;J. Simpson;I. Smail;C. Harrison;J. Hodge;A. Karim;F. Walter;D. Alexander;N. Brandt;C. Breuck;E. D. Cunha;S. Chapman;K. Coppin;A. Danielson;H. Dannerbauer;Roberto Decarli Thomas Greve;R. Ivison;K. Knudsen;C. Lagos;E. Schinnerer;A. Thomson;J. Wardlow;A. Weiss;Paul van der Werf Icc;Durham;Heidelberg;Bonn;Penn State;Eső;Dalhousie;Hertfordshire;Vienna;Ucl;Ifa;Edinburgh;Chalmers;UC Irvine;Leiden
DOI：
10.1088/0004-637x/769/1/80
发表时间：
2013-05
期刊：
The Astrophysical Journal
影响因子：
--
作者：
M. Ashby;S. Willner;G. Fazio;J.-S. Huang;R. Arendt;P. Barmby;G. Barro;E. Bell;R. Bouwens
通讯作者：
M. Ashby;S. Willner;G. Fazio;J.-S. Huang;R. Arendt;P. Barmby;G. Barro;E. Bell;R. Bouwens
影响因子：
4.8
作者：
S. Stach;U. Dudzevivciut.e;I. Smail;A. Swinbank;J. Geach;J. Simpson;F. An;O. Almaini;V. Arumugam;A. Blain;S. Chapman;C. C. Chen-C.;C. Conselice;E. Cooke;K. Coppin;E. D. Cunha;J. Dunlop;D. Farrah;B. Gullberg;J. Hodge;R. Ivison;D. Kocevski;M. Michałowski;T. Miyaji;D. Scott;A. Thomson;J. Wardlow;A. Weiss;P. University;U. Hertfordshire;Asiaa;Purple Mountain Observatory;U. Nottingham;Eső;U. Edinburgh;U. Leicester;D. University;A. N. University;U. Hawaii;Leiden University;Colby College;Adam Mickiewicz University;Unam;U. Columbia;U. Manchester;L. University;Max-Planck Institut
通讯作者：
S. Stach;U. Dudzevivciut.e;I. Smail;A. Swinbank;J. Geach;J. Simpson;F. An;O. Almaini;V. Arumugam;A. Blain;S. Chapman;C. C. Chen-C.;C. Conselice;E. Cooke;K. Coppin;E. D. Cunha;J. Dunlop;D. Farrah;B. Gullberg;J. Hodge;R. Ivison;D. Kocevski;M. Michałowski;T. Miyaji;D. Scott;A. Thomson;J. Wardlow;A. Weiss;P. University;U. Hertfordshire;Asiaa;Purple Mountain Observatory;U. Nottingham;Eső;U. Edinburgh;U. Leicester;D. University;A. N. University;U. Hawaii;Leiden University;Colby College;Adam Mickiewicz University;Unam;U. Columbia;U. Manchester;L. University;Max-Planck Institut