A LOFAR-IRAS cross-match study: the far-infrared radio correlation and the 150 MHz luminosity as a star-formation rate tracer
A LOFAR-IRAS cross-match study: the far-infrared radio correlation and the 150 MHz luminosity as a star-formation rate tracer
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LOFAR-IRAS 交叉匹配研究：远红外射电相关性和 150 MHz 光度作为恒星形成率示踪剂
DOI：
10.1051/0004-6361/201935913
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发表时间：
2019
影响因子：
6.5
通讯作者：
Wang L
中科院分区：
文献类型：
--
作者：
Wang L
目的研究局地宇宙150 MHz(红移中值为⟨z⟩∼0.05)的远红外射电相关，并改进利用静止帧150 MHz光度L150作为恒星形成率的示踪剂，它不受尘埃消光的影响。方法我们将60μm选定的IRAS弱源探测红移星表与Hobby-Eberly望远镜暗能量实验(HETDEX)春场中150 MHz选定的LOFAR增值源星表进行交叉匹配。对交叉匹配源的L150进行了估计，并将其与总红外光度、LIR和各种SFR示踪剂进行了比较。结果对于恒星形成星系，我们发现logL150和logLIR之间存在紧密的线性相关，斜率为1.37。我们的主要样本的中值QIR值(定义为LIRto L150比率的对数)及其均方根散布分别为2.14和0.34。我们还发现，logL150与来自三种不同示踪剂的SFRR的对数密切相关，即基于Hα谱线光度的SFRHα、基于静止帧60μm光度的SFR60和基于LIR的SFRIR，其散度为0.3Dex。LogL150(L⊙)=1.35(±0.06)×logSFRHα(M⊙yr−1)+3.2 0(±0.06)；logL150(L⊙)=1.31(±0.05)×logSFr60(M⊙yr−1)+3.14(±0.06)；logL150(L⊙)=1.37(±0.05)×logSFRIR(M⊙yr−1)+3.09(±0.05)。
AimsWe aim to study the far-infrared radio correlation (FIRC) at 150 MHz in the local Universe (at a median redshift ⟨z⟩∼0.05) and improve the use of the rest-frame 150 MHz luminosity,L150, as a star-formation rate (SFR) tracer, which is unaffected by dust extinction.MethodsWe cross-match the 60μm selected Revised IRAS Faint Source Survey Redshift (RIFSCz) catalogue and the 150 MHz selected LOFAR value-added source catalogue in theHobby-EberlyTelescope Dark Energy Experiment (HETDEX) Spring Field. We estimateL150for the cross-matched sources and compare it with the total infrared (IR) luminosity,LIR, and various SFR tracers.ResultsWe find a tight linear correlation between logL150and logLIRfor star-forming galaxies, with a slope of 1.37. The medianqIRvalue (defined as the logarithm of theLIRtoL150ratio) and its rms scatter of our main sample are 2.14 and 0.34, respectively. We also find that logL150correlates tightly with the logarithm of SFR derived from three different tracers, i.e., SFRHαbased on the Hαline luminosity, SFR60based on the rest-frame 60μm luminosity and SFRIRbased onLIR, with a scatter of 0.3 dex. Our best-fit relations betweenL150and these SFR tracers are, logL150(L⊙) = 1.35(±0.06) × log SFRHα(M⊙yr−1) + 3.20(±0.06), logL150(L⊙) = 1.31(±0.05) × log SFR60(M⊙yr−1) + 3.14(±0.06), and logL150(L⊙) = 1.37 (±0.05) × log SFRIR(M⊙yr−1) + 3.09(±0.05), which show excellent agreement with each other.
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