ALMA observations of lensed Herschel sources: testing the dark matter halo paradigm
ALMA observations of lensed Herschel sources: testing the dark matter halo paradigm
复制标题
ALMA 对赫歇尔透镜源的观测：测试暗物质晕范式
DOI：
10.1093/mnras/sty138
复制
发表时间：
2018
影响因子：
4.8
通讯作者：
Amvrosiadis A
中科院分区：
文献类型：
--
作者：
Amvrosiadis A
随着广域亚毫米探测的到来，大量高红移、引力透镜状尘埃恒星形成星系被揭示出来。由于在这类调查中确定的候选透镜源的选择标准很简单，如S500 μm>；100 mJy，因此消除了与选择函数建模相关的不确定性。这些属性的结合使得亚毫米测量成为研究强透镜统计的理想选择。我们通过使用阿塔卡马大毫米阵列(ALMA)对从赫歇尔空间天文台进行的调查中挑选的强透镜光源样本进行观测，对亚毫米选定光源的透镜统计进行了初步研究。我们试图使用从包含暗物质和重子的数值模拟中获得的晕质量函数来再现透镜光源的图像分离的分布。我们使用了三种不同的密度分布，一种是基于对Eagle模拟中形成的晕的解析拟合，另一种是以前在透镜研究中使用的两种密度分布[奇异等温球(SIS)和SISSA]。我们发现，只要我们对SIS和SISSA模型施加∼1013M⊙的上质量跃迁，我们就可以用这三种密度分布重现观测到的分布，我们假设密度分布可以用纳瓦罗-弗伦克-怀特分布来表示。我们表明，我们需要一个∼500透镜源的样本来区分密度分布，这在考虑到Herschel调查中预测的透镜源数量的情况下是可行的。
With the advent of wide-area submillimetre surveys, a large number of high-redshift gravitationally lensed dusty star-forming galaxies have been revealed. Because of the simplicity of the selection criteria for candidate lensed sources in such surveys, identified as those withS500 μm> 100 mJy, uncertainties associated with the modelling of the selection function are expunged. The combination of these attributes makes submillimetre surveys ideal for the study of strong lens statistics. We carried out a pilot study of the lensing statistics of submillimetre-selected sources by making observations with the Atacama Large Millimeter Array (ALMA) of a sample of strongly lensed sources selected from surveys carried out with theHerschel Space Observatory. We attempted to reproduce the distribution of image separations for the lensed sources using a halo mass function taken from a numerical simulation that contains both dark matter and baryons. We used three different density distributions, one based on analytical fits to the haloes formed in the EAGLE simulation and two density distributions [Singular Isothermal Sphere (SIS) and SISSA] that have been used before in lensing studies. We found that we could reproduce the observed distribution with all three density distributions, as long as we imposed an upper mass transition of ∼1013M⊙for the SIS and SISSA models, above which we assumed that the density distribution could be represented by a Navarro–Frenk–White profile. We show that we would need a sample of ∼500 lensed sources to distinguish between the density distributions, which is practical given the predicted number of lensed sources in theHerschelsurveys.
登录
查看更多内容
影响因子：
4.8
作者：
S. Dye;M. Negrello;R. Hopwood;J. Nightingale;R. Bussmann;R. Bussmann;S. Amber;N. Bourne;A. Cooray;A. Dariush;L. Dunne;S. Eales;J. González-Nuevo;E. Ibar;R. Ivison;S. Maddox;E. Valiante;Matthew W. L. Smith
通讯作者：
S. Dye;M. Negrello;R. Hopwood;J. Nightingale;R. Bussmann;R. Bussmann;S. Amber;N. Bourne;A. Cooray;A. Dariush;L. Dunne;S. Eales;J. González-Nuevo;E. Ibar;R. Ivison;S. Maddox;E. Valiante;Matthew W. L. Smith
DOI：
10.3847/0004-637x/823/1/17
发表时间：
2016-01
期刊：
The Astrophysical Journal
影响因子：
--
作者：
H. Nayyeri;M. Keele;A. Cooray;D. Riechers;R. Ivison;A. Harris;D. Frayer;A. Baker;S. Chapman;S. Eales;D. Farrah;H. Fu;L. Marchetti;R. Marques-Chaves;P. Mart́ınez-Navajas;S. Oliver;A. Omont;I. Pérez-Fournon;D. Scott;Mattia Vaccari;J. Vieira;M. Viero;L. Wang;J. Wardlow
通讯作者：
H. Nayyeri;M. Keele;A. Cooray;D. Riechers;R. Ivison;A. Harris;D. Frayer;A. Baker;S. Chapman;S. Eales;D. Farrah;H. Fu;L. Marchetti;R. Marques-Chaves;P. Mart́ınez-Navajas;S. Oliver;A. Omont;I. Pérez-Fournon;D. Scott;Mattia Vaccari;J. Vieira;M. Viero;L. Wang;J. Wardlow
影响因子：
3.5
作者：
S. Eales;L. Dunne;D. Clements;A. Cooray;G. Zotti;S. Dye;R. Ivison;M. Jarvis;G. Lagache
通讯作者：
S. Eales;L. Dunne;D. Clements;A. Cooray;G. Zotti;S. Dye;R. Ivison;M. Jarvis;G. Lagache
DOI：
10.1046/j.1365-8711.2001.04029.x
发表时间：
2001-02-21
影响因子：
4.8
作者：
Jenkins, A;Frenk, CS;Yoshida, N
通讯作者：
Yoshida, N
影响因子：
4.8
作者：
Bocquet, Sebastian;Saro, Alex;Mohr, Joseph J.
通讯作者：
Mohr, Joseph J.