HERUS: The far-IR/submm spectral energy distributions of local ULIRGs and photometric atlas
HERUS: The far-IR/submm spectral energy distributions of local ULIRGs and photometric atlas
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DOI：
10.1093/mnras/stx3227
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发表时间：
2017-12
影响因子：
4.8
通讯作者：
D. Clements;C. Pearson;C. Pearson;C. Pearson;D. Farrah;J. Greenslade;J. Bernard-Salas;E. González-Alfonso;J. Afonso;A. Efstathiou;D. Rigopoulou;D. Rigopoulou;V. Lebouteiller;V. Lebouteiller;P. Hurley;H. Spoon
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作者：
D. Clements;C. Pearson;C. Pearson;C. Pearson;D. Farrah;J. Greenslade;J. Bernard-Salas;E. González-Alfonso;J. Afonso;A. Efstathiou;D. Rigopoulou;D. Rigopoulou;V. Lebouteiller;V. Lebouteiller;P. Hurley;H. Spoon
本文介绍了作为赫歇尔超亮红外星系巡天（HERUS）的一部分，由IRAS在60 μm处选取的43个局部超亮红外星系（ULIRGs）的完整通量限制样本的赫歇尔-SPIRE光度图集。使用SPIRE仪器在250、350和500 μm处获得光度测定观察结果。我们描述了这些观测结果，提出的结果，并结合联合收割机的新的观测数据从IRAS检查远红外光谱能量分布（SED）的这些来源。我们用一个简单的参数化的修正黑体模型拟合了观测到的HERUS天体的SED，其中温度和发射率β是自由参数。我们将拟合值与非ULIRG本星系的拟合值进行了比较，发现与早期结果一致，HERUS ULIRG具有更温暖的尘埃（中值温度T = 37.9 ± 4.7 K，而不是21.3 ± 3.4 K），但与Herschel参考样本（HRS，Cortese et al. 2014）星系相似的β分布（中值β = 1.7，而不是1.8）。尘埃质量的范围为107.5-109 Mpa，明显高于HRS源。我们比较了我们的结果与本地ULIRGs的红移较高的样品选择在250和850 μm。后者通常比我们选择的60 μ m ULIRG具有更冷的尘埃和/或更红的100至250 μm颜色。我们发现，这种差异可能部分是由于在不同的波长选择的源，而不是一个简单的指示人口的属性的快速演变。
We present the Herschel-SPIRE photometric atlas for a complete flux limited sample of 43 local ultraluminous infrared galaxies (ULIRGs), selected at 60 μm by IRAS, as part of the HERschel ULIRG Survey (HERUS). Photometry observations were obtained using the SPIRE instrument at 250, 350, and 500 μm. We describe these observations, present the results, and combine the new observations with data from IRAS to examine the far-infrared spectral energy distributions (SEDs) of these sources. We fit the observed SEDs of HERUS objects with a simple parametrized modified blackbody model, where temperature and emissivity β are free parameters. We compare the fitted values to those of non-ULIRG local galaxies, and find, in agreement with earlier results, that HERUS ULIRGs have warmer dust (median temperature T = 37.9 ± 4.7 K compared to 21.3 ± 3.4 K) but a similar β distribution (median β = 1.7 compared to 1.8) to the Herschel reference sample (HRS, Cortese et al. 2014) galaxies. Dust masses are found to be in the range of 107.5–109 M⊙, significantly higher than that of HRS sources. We compare our results for local ULIRGs with higher redshift samples selected at 250 and 850 μm. These latter sources generally have cooler dust and/or redder 100-to-250 μm colours than our 60 μm-selected ULIRGs. We show that this difference may in part be the result of the sources being selected at different wavelengths rather than being a simple indication of rapid evolution in the properties of the population.