The Physical Drivers of the Luminosity-weighted Dust Temperatures in High-redshift Galaxies
The Physical Drivers of the Luminosity-weighted Dust Temperatures in High-redshift Galaxies
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高红移星系中光度加权尘埃温度的物理驱动因素
DOI：
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发表时间：
2021
影响因子：
4.9
通讯作者：
N. Scoville
中科院分区：
文献类型：
--
作者：
A. Burnham;C. Casey;J. Zavala;S. Manning;J. Spilker;S. Chapman;Chian;A. Cooray;D. Sanders;N. Scoville
由于缺乏大型星系样本的远红外/（亚）毫米数据，星系尘埃光谱能量分布（SED）的基本分布（即，由静止框架~3μm到3mm的尘埃再辐射的光谱）仍然相对不受约束。文献中声称，星系的尘埃温度（以尘埃 SED 峰值（λ 峰值）的波长来观察）最密切地可通过其特定的恒星形成率 (sSFR) 或与 SFR-M ⋆ 关系（星系“主序带”）的参数化“距离”来追踪。我们提出了 024 分辨率的 870 μm ALMA 尘埃连续观测数据，对七个 z = 1.4–4.6 尘埃恒星形成星系进行观测，这些星系被选择具有大范围的良好约束的光度加权尘埃温度。我们还利用 Hodge 等人 (2016) 的 ALESS 亚毫米星系样本中类似分辨率的尘埃连续谱图。我们限制灰尘辐射的物理尺度，并将这些测量结果与集成 SED 的特性进行比较。我们确认了 λ 峰值与 L IR（或 SFR）和 ΣIR（∝SFR 表面密度）的显着相关性。我们研究了 log10（λ 峰值）和 log10（ΣIR）之间的相关性，并找到了斯蒂芬-玻尔兹曼定律或等效黑体的有效尺寸所期望的关系。 λ 峰与 sSFR 以及距 SFR-M ⋆ 关系的距离的相关性不如 ΣIR 或 L IR 显着；因此，我们得出的结论是，星系光度加权综合尘埃温度的更基本示踪剂实际上是其恒星形成表面密度，与局部宇宙结果一致，这与星际介质中尘埃的基本几何形状密切相关。
The underlying distribution of galaxies’ dust spectral energy distributions (SEDs) (i.e., their spectra reradiated by dust from rest-frame ∼3 μm to 3 mm) remains relatively unconstrained owing to a dearth of far-IR/(sub)millimeter data for large samples of galaxies. It has been claimed in the literature that a galaxy’s dust temperature—observed as the wavelength where the dust SED peaks (λ peak)—is traced most closely by its specific star formation rate (sSFR) or parameterized “distance” to the SFR–M ⋆ relation (the galaxy “main sequence”). We present 024 resolved 870 μm ALMA dust continuum observations of seven z = 1.4–4.6 dusty star-forming galaxies chosen to have a large range of well-constrained luminosity-weighted dust temperatures. We also draw on similar-resolution dust continuum maps from a sample of ALESS submillimeter galaxies from Hodge et al (2016). We constrain the physical scales over which the dust radiates and compare those measurements to characteristics of the integrated SED. We confirm significant correlations of λ peak with both L IR (or SFR) and ΣIR (∝SFR surface density). We investigate the correlation between log10(λ peak) and log10(ΣIR) and find the relation to hold as would be expected from the Stefan–Boltzmann law, or the effective size of an equivalent blackbody. The correlations of λ peak with sSFR and distance from the SFR–M ⋆ relation are less significant than those for ΣIR or L IR; therefore, we conclude that the more fundamental tracer of galaxies’ luminosity-weighted integrated dust temperatures are indeed their star formation surface densities in line with local universe results, which relate closely to the underlying geometry of dust in the interstellar medium.
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DOI：
10.3847/1538-4357/ab1f77
发表时间：
2019-05
期刊：
The Astrophysical Journal
影响因子：
--
作者：
P. Lang;E. Schinnerer;I. Smail;U. Dudzevivciut.e;A. Swinbank;Daizhong Liu;S. Leslie;O. Almaini;F. An;F. Bertoldi;A. Blain;S. Chapman;Chian-Chou Chen;C. Conselice;E. Cooke;K. Coppin;J. Dunlop;D. Farrah;Y. Fudamoto;J. Geach;B. Gullberg;K. Harrington;J. Hodge;R. Ivison;E. F. Jim'enez-Andrade;B. Magnelli;M. Michałowski;P. Oesch;D. Scott;J. Simpson;V. Smolvci'c;S. Stach;A. Thomson;S. Toft;E. Vardoulaki;J. Wardlow;A. Weiss;P. Werf
通讯作者：
P. Lang;E. Schinnerer;I. Smail;U. Dudzevivciut.e;A. Swinbank;Daizhong Liu;S. Leslie;O. Almaini;F. An;F. Bertoldi;A. Blain;S. Chapman;Chian-Chou Chen;C. Conselice;E. Cooke;K. Coppin;J. Dunlop;D. Farrah;Y. Fudamoto;J. Geach;B. Gullberg;K. Harrington;J. Hodge;R. Ivison;E. F. Jim'enez-Andrade;B. Magnelli;M. Michałowski;P. Oesch;D. Scott;J. Simpson;V. Smolvci'c;S. Stach;A. Thomson;S. Toft;E. Vardoulaki;J. Wardlow;A. Weiss;P. Werf
影响因子：
4.8
作者：
U. Dudzevivciut.e;I. Smail;A. Swinbank;S. Stach;O. Almaini;E. D. Cunha;F. An;V. Arumugam;
通讯作者：
U. Dudzevivciut.e;I. Smail;A. Swinbank;S. Stach;O. Almaini;E. D. Cunha;F. An;V. Arumugam;
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：
10.3847/1538-4357/aba528
发表时间：
2020-07
期刊：
The Astrophysical Journal
影响因子：
--
作者：
C. Casey
通讯作者：
C. Casey