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AKARI and IRAS: From beam corrections to SEDs

机译：Akari和Iras：从梁校正到SED

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There is significant scientific value to be gained from combining AKARI fluxes with data at other far-infrared (IR) wavelengths from the Infrared Astronomical Satellite (IRAS) and Herschel missions. To be able to do this we must ensure that there are no systematic differences between the data sets that need to be corrected before the fluxes are compatible with each other. One such systematic effect identified in the Bright Source Catalog version 1 (BSCv1) data is the issue of beam corrections. We determine these for the BSC version 2 (BSCv2) data by correlating ratios of appropriate IRAS and AKARI bands with the difference in 2 Micron All Sky Survey (2MASS) J-band extended and point source magnitudes for sources cross-matched between the IRAS Faint Source Catalog (FSC), AKARI BSCv2 and 2MASS catalogs. We find significant correlations (p 10(-13)) indicating that beam corrections are necessary in the 65 and 90 mu m bands. We then use these corrected fluxes to supplement existing data in spectral energy distribution (SED) fits for ultraluminous infrared galaxies (ULIRGs) in the Herschel ULIRG Survey (HERUS). The addition of AKARI fluxes makes little difference to the results of simple (T, beta) fits to the SEDs of these sources, though there is a general decrease in reduced chi(2) values. The utility of the extra AKARI data, however, is in allowing physically more realistic SED models with more parameters to be fitted to the data. We also extend our analysis of beam correction issues in the AKARI data by examining the Herschel Reference Sample (HRS) galaxies, which have Herschel photometry from 100 to 500 mu m and which are more spatially extended than the HERUS ULIRGs. 34 of the HRS sources have good Herschel SEDs and matching data from AKARI. This investigation finds that our simple 2MASS-based beam correction scheme is inadequate for these larger and more complex sources. There are also indications that additional beam corrections at 140 and 160 mu m are needed for these sources, extended on scales >1'.
机译：将Akari通量与来自红外天文卫星（IRA）和Herschel任务的其他远红外（IR）波长的数据相结合的科学价值与其他远红外（IR）波长的数据相结合。为了能够这样做，我们必须确保在助势彼此兼容之前需要纠正的数据集之间没有系统差异。在明亮的源目录版本1（BSCV1）数据中识别的一种这样的系统效果是波束校正的问题。我们通过将适当的IRA和Akari频段的比率与2微米的差异相互作用来确定这些用于BSC版本2（BSCV2）数据的数据（2mass）J频段延伸和点源大小，用于在IRA之间交叉匹配源目录（FSC），Akari BSCv2和2mass目录。我们发现了显着的相关性（P 10（-13）），指示在65和90 mu m频带中需要光束校正。然后，我们使用这些校正的助量来补充诸如Herschel Ulirg调查（赫鲁）的超易用红外星系（ULIRGS）的光谱能量分布（SED）中的现有数据。 Akari助焊剂的添加对符合这些来源的SED的简单（T，BETA）的结果几乎没有差异，尽管CHI（2）值的一般性降低。然而，额外的Akari数据的效用是允许物理上更具现实的SED模型，具有更多参数来安装到数据。我们还通过检查Herschel参考样品（HRS）星系，从100至500μm的Herschel光​​度测定，延伸到Akari数据中的光束校正问题的分析。 HRS来源的34个Herschel Seds和Akari的匹配数据。本研究发现，对于这些较大和更复杂的来源，我们的简单2Mass的光束校正方案是不充分的。还有迹象表明，对于这些来源，需要在140和160μm处进行额外的光束校正，在尺度> 1'上延伸。

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