arXiv 1206.60792012-06-26astro-ph.CO

亚毫米波半导体的测光红移

Photometric Redshifts of Submillimeter Galaxies

Sukanya Chakrabarti, Benjamin Magnelli, Christopher F. McKee, Dieter Lutz, Stefano Berta, Paola Popesso, Francesca Pozzi

备注：: 7 pages, 2 figures, submitted to ApJ
DOI：: 10.1088/0004-637X/773/2/113

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摘要：

我们使用Chakrabarti & McKee（2008）的光度红移方法，利用PACS演化探测器（PEP）计划获得的远红外（FIR）$\it{Herschel}$数据推断亚毫米星系的光度红移。对于光谱红移的样品，我们证明了这种方法的有效性在大范围的红移（$ 4 \ga z \ga 0.3$）和光度，发现在$(1+z_{\rm phot})/(1+z_{\rm spec})$的平均精度为10%。因此，该方法比其他FIR光度红移方法更精确。这种方法不同于典型的远红外测光方法，它是从远红外光谱能量分布（SED）推断的红外亮星系的光气质量（$L/M$）比而不是尘埃温度来推导红移。一旦得到红移，我们就可以确定红外亮星系的物理性质，包括尘埃包层内的温度变化、光度、质量和表面密度。我们使用GOODS-S场的数据来计算AzTEC和PACS探测到的亚毫米亮源的恒星形成率密度（SFRD）。具有阈值$850 \micron$通量$\ga 5 \rm mJy$的AzTEC-PACS源贡献了来自所有ULIRG（$L_{\rm IR} \ga 10^{12} L_{\odot}$）的SFRD的15%，以及在$z \sim 2$的总SFRD的3%。

英文摘要：

We use the photometric redshift method of Chakrabarti & McKee (2008) to infer photometric redshifts of submillimeter galaxies with far-IR (FIR) $\it{Herschel}$ data obtained as part of the PACS Evolutionary Probe (PEP) program. For the sample with spectroscopic redshifts, we demonstrate the validity of this method over a large range of redshifts ($ 4 \ga z \ga 0.3$) and luminosities, finding an average accuracy in $(1+z_{\rm phot})/(1+z_{\rm spec})$ of 10%. Thus, this method is more accurate than other FIR photometric redshift methods. This method is different from typical FIR photometric methods in deriving redshifts from the light-to-gas mass ($L/M$) ratio of infrared-bright galaxies inferred from the FIR spectral energy distribution (SED), rather than dust temperatures. Once the redshift is derived, we can determine physical properties of infrared bright galaxies, including the temperature variation within the dust envelope, luminosity, mass, and surface density. We use data from the GOODS-S field to calculate the star formation rate density (SFRD) of sub-mm bright sources detected by AzTEC and PACS. The AzTEC-PACS sources, which have a threshold $850 \micron$ flux $\ga 5 \rm mJy$, contribute 15% of the SFRD from all ULIRGs ($L_{\rm IR} \ga 10^{12} L_{\odot}$), and 3% of the total SFRD at $z \sim 2$.

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