论文标题
CFHTLEN：星系偏置作为尺度，恒星质量和颜色的函数。半分析模型的预测冲突
CFHTLenS: Galaxy bias as function of scale, stellar mass, and colour. Conflicts with predictions by semi-analytic models
论文作者
论文摘要
星系模型预测了星系聚类与宇宙学量表上的暗物质之间存在紧密的关系，但是细节的预测显着差异。我们利用了这个机会，并通过慕尼黑和达勒姆集团的两个半分析模型进行了加拿大 - 法兰西 - 弗朗西·霍瓦伊望远镜镜头调查（CFHTLENS）的数据。在测试中，我们测量了与规模相关的星系偏差因子$ b（k）$和相关因子$ r（k）$从线性到非线性尺度的$ k \ of10 \，h \，h \，\ rm mpc^{ - 1} $在两个红色shifts $ \ bar {z} = 0.355,5,5,5,5,5,5,5,5,5,5,5,5,5,5,5,5,5,5,5,5,5,5,5,5,5,5,5,5,5,5,5,51 $中， $ 3 \ times10^{11} \，h _ {\ rm 70}^{ - 2} \，{\ rm m} _ \ odot $。我们改进的重力镜头技术解释了源的固有比对和晶状体星系的放大，以更好地限制星系 - 膜相关性$ r（k）$。 Cfhtlens的星系偏见随着$ K $和出色的质量而增加，它依赖于颜色，揭示了星系类型的单个足迹。尽管与规模和星系属性的相对变化达成了合理的模型协议，但对于$ b（k）$，没有模型偏好存在明显的冲突：模型星系太弱了。这可能会标记所有恒星群众的$ z \ gtrsim0.3 $的模型问题。但是，与模型一样，所有尺度上物质和星系密度之间都有高相关性$ r（k）$，而星系偏置通常与线性尺度上的确定性偏差一致。只有我们的蓝色和低质量星系约为$ 7 \ times10^9 \，h _ {\ rm 70}^{ - 2} \，{\ rm m} _ \ odot $ at $ \ bar {z} = 0.51 $ at $ \ bar {z} = 0.51 $显示，与型号相反，a s linear s linseal scales in $ s linear s linear s linear s linear s linear s linear calme in cy cy in uias in cy rias in cy。 ls} = 0.75 \ pm0.14 \，{\ rm（stat。）} \ pm0.06 \，{\ rm（sys。）} $。此结果是依赖确定性星系偏置的宇宙学探针感兴趣的，例如$ e _ {\ rm g} $。
Galaxy models predict a tight relation between the clustering of galaxies and dark matter on cosmological scales, but predictions differ notably in the details. We used this opportunity and tested two semi-analytic models by the Munich and Durham groups with data from the Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS). For the test we measured the scale-dependent galaxy bias factor $b(k)$ and correlation factor $r(k)$ from linear to non-linear scales of $k\approx10\,h\,\rm Mpc^{-1}$ at two redshifts $\bar{z}=0.35,0.51$ for galaxies with stellar mass between $5\times10^9$ and $3\times10^{11}\,h_{\rm 70}^{-2}\,{\rm M}_\odot$. Our improved gravitational lensing technique accounts for the intrinsic alignment of sources and the magnification of lens galaxies for better constraints for the galaxy-matter correlation $r(k)$. Galaxy bias in CFHTLenS increases with $k$ and stellar mass, it is colour-dependent, revealing the individual footprints of galaxy types. Despite a reasonable model agreement for the relative change with both scale and galaxy properties, there is a clear conflict for $b(k)$ with no model preference: the model galaxies are too weakly clustered. This may flag a model problem at $z\gtrsim0.3$ for all stellar masses. As in the models, however, there is a high correlation $r(k)$ between matter and galaxy density on all scales, and galaxy bias is typically consistent with a deterministic bias on linear scales. Only our blue and low-mass galaxies of about $7\times10^9\,h_{\rm 70}^{-2}\,{\rm M}_\odot$ at $\bar{z}=0.51$ show, contrary to the models, a weak tendency towards a stochastic bias on linear scales where $r_{\rm ls}=0.75\pm0.14\,{\rm(stat.)}\pm0.06\,{\rm(sys.)}$. This result is of interest for cosmological probes, such as $E_{\rm G}$, that rely on a deterministic galaxy bias.
