标题： 红外和亚毫米巡天中ULIRGs的选择 显示英文标题

标题： Selection of ULIRGs in Infrared and Submm Surveys

摘要： 我们检查了IRAS、斯皮策、BLAST、赫歇尔和SCUBA的红外和亚毫米波巡天的选择特性，并确定这些巡天对处于ULIRG光度范围（12<log(LIR)<13）的星系所敏感的尘埃温度范围，在z=0到z=4之间。 我们发现，巡天在无偏见的红移范围内覆盖的程度是选择波长、通量密度限制和ULIRG光度的函数。 短波长（<200{\mu }m）的巡天，如IRAS、斯皮策/MIPS和赫歇尔/PACS，在其可访问的红移范围的相当大一部分内，对所有SED类型在较大的温度区间（17-87K）都是敏感的。 另一方面，长波长（>200{\mu }m）的巡天，如BLAST、赫歇尔/SPIRE和SCUBA，对冷的ULIRG更为敏感，在低红移时甚至会偏向于排除较暖的SED。 我们在巡天选择效应的背景下评估观测结果，发现本地（z<0.1）宇宙中缺乏冷的ULIRG并不是选择效应的结果，而且本地看到的ULIRG温度范围只是高红移时存在的一大更广范围的一部分。 我们证明，本地的光度-温度（L-T）关系表明更明亮的源也更热，当将其外推到ULIRG领域时，在遥远的宇宙中并不适用，因为观测到的温度的离散性太大。 最后，我们表明本地和高红移处ULIRG温度分布之间的差异不是由于星系因L-T关系随红移演化而变冷的结果。 相反，它们与红外光度函数的演化依赖于温度的图景一致，即冷星系的演化速度比温暖星系更快。 显示英文摘要

摘要： We examine the selection characteristics of infrared and sub-mm surveys with IRAS, Spitzer, BLAST, Herschel and SCUBA and identify the range of dust temperatures these surveys are sensitive to, for galaxies in the ULIRG luminosity range (12<log(LIR)<13), between z=0 and z=4. We find that the extent of the redshift range over which surveys are unbiased is a function of the wavelength of selection, flux density limit and ULIRG luminosity. Short wavelength (<200{\mu}m) surveys with IRAS, Spitzer/MIPS and Herschel/PACS are sensitive to all SED types in a large temperature interval (17-87K), over a substantial fraction of their accessible redshift range. On the other hand, long wavelength (>200{\mu}m) surveys with BLAST, Herschel/ SPIRE and SCUBA are significantly more sensitive to cold ULIRGs, disfavouring warmer SEDs even at low redshifts. We evaluate observations in the context of survey selection effects, finding that the lack of cold ULIRGs in the local (z<0.1) Universe is not a consequence of selection and that the range of ULIRG temperatures seen locally is only a subset of a much larger range which exists at high redshift. We demonstrate that the local luminosity-temperature (L-T) relation, which indicates that more luminous sources are also hotter, is not applicable in the distant Universe when extrapolated to the ULIRG regime, because the scatter in observed temperatures is too large. Finally, we show that the difference between the ULIRG temperature distributions locally and at high redshift is not the result of galaxies becoming colder due to an L-T relation which evolves as a function of redshift. Instead, they are consistent with a picture where the evolution of the infrared luminosity function is temperature dependent, i.e. cold galaxies evolve at a faster rate than their warm counterparts.