Photometric Redshift Using the Far-infrared Spectral Energy Distribution
Photometric Redshift Using the Far-infrared Spectral Energy Distribution
复制标题
利用远红外光谱能量分布进行光度红移
DOI：
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发表时间：
2003
期刊：
影响因子：
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通讯作者：
T. Wiklind
中科院分区：
文献类型：
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作者：
T. Wiklind
提出了一种利用亚毫米波段测定发光、高z、尘埃星系光度红移的方法。这是基于观测到的局部超红外星系（ulrgs）在波长λ bbb50 μm处具有非常小的色散的平均光谱能量分布（SED）。长波部分的形状与本地ulrg是否拥有活动星系核无关。一个本地模板来源于2001年Klaas等人提供的ulrg数据样本。利用该模板及其形状的内色散，证明了在450和850 μm两个固定的亚毫米波波段观测，可以确定红移范围为1 < z < 5的星系的光度红移。模板SED引起的红移不确定度为Δz/z ~ 0.3，在较高的红移范围内有所改善。讨论了利用该方法和阿塔卡马大型毫米波阵列（ALMA）的大瞬时带宽利用CO发射导出光谱红移的意义。
A method for using the submillimeter band to determine photometric redshifts of luminous, high-z, dusty galaxies is presented. It is based on the observation that local ultraluminous infrared galaxies (ULIRGs) show an average spectral energy distribution (SED) that has a remarkably small dispersion for wavelengths λ > 50 μm. The shape of the long-wavelength part is independent of whether the local ULIRG possesses an active galactic nucleus or not. A local template is derived from a sample of ULIRG data presented by Klaas et al. in 2001. Using this template and the internal dispersion in its shape, it is shown that observations at two fixed submillimeter wavelengths, e.g., 450 and 850 μm, can be used to determine the photometric redshift of galaxies in the redshift range 1 < z < 5. The uncertainty in the redshift arising from the template SED amounts to Δz/z ~ 0.3, with an improvement at the higher redshift range. Implications for using this method together with the large instantaneous bandwidth of the Atacama Large Millimeter Array (ALMA) for deriving spectroscopic redshifts using CO emission is discussed.