Dust and star formation properties of a complete sample of local galaxies drawn from the Planck Early Release Compact Source Catalogue
Dust and star formation properties of a complete sample of local galaxies drawn from the Planck Early Release Compact Source Catalogue
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DOI：
10.1093/mnras/stt760
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发表时间：
2013-05
影响因子：
4.8
通讯作者：
M. Clemens;M. Negrello;G. Zotti;J. González-Nuevo;L. Bonavera;G. Cosco;G. Guarese;L. Boaretto;P. Salucci;C. Baccigalupi;D. Clements;L. Danese;A. Lapi;N. Mandolesi;N. Mandolesi;R. B. Partridge;F. Perrotta;S. Serjeant;D. Scott;L. Toffolatti
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文献类型：
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作者：
M. Clemens;M. Negrello;G. Zotti;J. González-Nuevo;L. Bonavera;G. Cosco;G. Guarese;L. Boaretto;P. Salucci;C. Baccigalupi;D. Clements;L. Danese;A. Lapi;N. Mandolesi;N. Mandolesi;R. B. Partridge;F. Perrotta;S. Serjeant;D. Scott;L. Toffolatti
我们将 857、545、353 和 217 GHz 的普朗克高频仪器数据与来自广域红外巡天探测器 (WISE)、斯皮策、IRAS 和赫歇尔的数据相结合，以研究本地恒星形成星系的明确定义的通量限制样本的属性。选择 545 GHz 通量密度限制，以便样本在此频率下完成 80%，所得样本总共包含 234 个本地恒星形成星系。我们通过各种模型研究了样本的尘埃排放和恒星形成特性，并计算了局部尘埃质量函数。尽管单分量修改黑体非常适合 80 μm 长距离的尘埃发射，中值 β = 1.83，但尘埃温度和 β 之间已知的简并性也意味着，尘埃发射率指数固定为 β = 2、温度范围为 10-25 K 的尘埃分量可以很好地描述光谱能量分布。尽管需要第二个较温暖的尘埃分量来拟合较短波长数据，并且贡献了总红外光的大约三分之一。发射，其质量可以忽略不计。没有发现极冷（6-10 K）尘埃成分的证据。冷尘埃成分的温度很大程度上受到恒星形成率与尘埃总质量之比的影响。这意味着，与通常的假设相反，~20 K 尘埃的发射有很大一部分是由正在进行的恒星形成提供动力的，无论尘埃本身是否与恒星形成云或“卷云”有关。有统计证据表明，免费对免费对 217 GHz 通量密度的贡献为 ≲20%。我们发现尘埃与恒星的质量比中值为 0.0046；并且这个比率与星系质量反相关。尘埃质量和原子气体质量之间存在良好的相关性（中值Md/MHI=0.022），这表明具有更多尘埃（Md/M*值较高）的星系通常具有更多的星际介质。我们推导出的尘埃质量函数意味着当地宇宙（对于星系内的尘埃）的平均尘埃质量密度为 7.0 ± 1.4 × 105 M⊙ Mpc−3，明显大于使用赫歇尔数据的最新估计中发现的值。
We combine Planck High Frequency Instrument data at 857, 545, 353 and 217 GHz with data from Wide-field Infrared Survey Explorer (WISE), Spitzer, IRAS and Herschel to investigate the properties of a well-defined, flux-limited sample of local star-forming galaxies. A 545 GHz flux density limit was chosen so that the sample is 80 per cent complete at this frequency, and the resulting sample contains a total of 234 local, star-forming galaxies. We investigate the dust emission and star formation properties of the sample via various models and calculate the local dust mass function. Although single-component-modified blackbodies fit the dust emission longward of 80 μm very well, with a median β = 1.83, the known degeneracy between dust temperature and β also means that the spectral energy distributions are very well described by a dust component with dust emissivity index fixed at β = 2 and temperature in the range 10–25 K. Although a second, warmer dust component is required to fit shorter wavelength data, and contributes approximately a third of the total infrared emission, its mass is negligible. No evidence is found for a very cold (6–10 K) dust component. The temperature of the cold dust component is strongly influenced by the ratio of the star formation rate to the total dust mass. This implies, contrary to what is often assumed, that a significant fraction of even the emission from ∼20 K dust is powered by ongoing star formation, whether or not the dust itself is associated with star-forming clouds or ‘cirrus’. There is statistical evidence of a free–free contribution to the 217 GHz flux densities of ≲20 per cent. We find a median dust-to-stellar mass ratio of 0.0046; and that this ratio is anticorrelated with galaxy mass. There is good correlation between dust mass and atomic gas mass (median Md/MHI=0.022), suggesting that galaxies that have more dust (higher values of Md/M*) have more interstellar medium in general. Our derived dust mass function implies a mean dust mass density of the local Universe (for dust within galaxies), of 7.0 ± 1.4 × 105 M⊙ Mpc−3, significantly greater than that found in the most recent estimate using Herschel data.