论文标题
用阿尔玛检测到的亚毫米级星系的聚类
The clustering of submillimeter galaxies detected with ALMA
论文作者
论文摘要
先前测量亚毫米星系聚类（SMG）的研究基于单次检测到的来源的测量，从而找到了强烈聚类的证据。但是，阿尔玛（Alma）透露，由于这些仪器的粗角度分辨率粗糙，单次源可以由多种来源组成。这意味着可以高估了从单次调查推断出的聚类。在这里，我们根据Aless调查（ALMA调查）测量SMG的聚类，这是对Laboca ECDFS亚毫米列表（LIME）中先前确定的来源的ALMA随访。我们提出了一种基于单次望远镜鉴定的ALMA源聚类的方法，该方法基于向前建模单dish和Alma观测值。我们限制了halos托管SMG的中位数的上限，以$ 1 <z <3 $，找到$ M _ {\ rm {halo}} \ leq2.4 \ leq2.4 \ times10^{12} {12} \，\ rm \，m _ {\ odot} $ $ s_ {870} \ geq4.0 \，$ mjy，它至少是$ 3.8^{+3.8} _ { - 2.6} $次，比基于较少来源的群集所推论的质量低。这表明，基于单次观测值的SMG聚类的强度被高估了，因此SMG可能是通过暗物质光环托管的，而不是以前估计的巨大。通过将我们的型号推算为$ s_ {870} \ geq1.2 \，\ rm \，$ mjy的通量密度，我们发现这样的SMG居住在中位数质量$ m _ {\ rm {halo}} \ leq3.2 \ times10^{11} \，\ rm \，m _ {\ odot} $。我们得出的结论是，只有最亮的（$ s_ {870} \ gtrsim5-6 \，\ rm \，$ mjy）SMGS会以$ z \ sim2 $和$ s_ {870} \ gtrsim6 \ gtrsim6 \ rm rm falmages callaties to callassies to callassies controve，$ s \ sim2 $和$ s_ {870}中间红移和高红移星形星系，而Fainter SMG不太可能与这些人群联系起来。
Previous studies measuring the clustering of submillimeter galaxies (SMGs) have based their measurements on single-dish detected sources, finding evidence for strong clustering. However, ALMA has revealed that, due to the coarse angular resolution of these instruments, single-dish sources can be comprised of multiple sources. This implies that the clustering inferred from single-dish surveys may be overestimated. Here, we measure the clustering of SMGs based on the ALESS survey, an ALMA follow-up of sources previously identified in the LABOCA ECDFS Submillimeter Survey (LESS). We present a method to measure the clustering of ALMA sources that have been previously identified using single-dish telescopes, based on forward modeling both the single-dish and the ALMA observations. We constrain upper limits for the median mass of halos hosting SMGs at $1<z<3$, finding $M_{\rm{halo}}\leq2.4\times10^{12}\,\rm\,M_{\odot}$ for SMGs with flux densities $S_{870}\geq4.0\,$mJy, which is at least $3.8^{+3.8}_{-2.6}$ times lower than the mass inferred based on the clustering of the LESS sources alone. This suggests that the strength of SMG clustering based on single-dish observations was overestimated and therefore SMGs might be hosted by dark matter halos less massive than has previously been estimated. By extrapolating our models down to flux densities of $S_{870}\geq1.2\,\rm\,$mJy, we find that such SMGs inhabit halos with median mass $M_{\rm{halo}}\leq3.2\times10^{11}\,\rm\,M_{\odot}$. We conclude that only the brightest ($S_{870}\gtrsim5-6\,\rm\,$mJy) SMGs would trace massive structures at $z\sim2$ and only SMGs with $S_{870}\gtrsim6\,\rm\,$mJy may be connected to massive local elliptical galaxies, quasars at intermediate redshifts and high-redshift star-forming galaxies, whereas fainter SMGs are unlikely linked to these populations.
