论文标题
普兰克PSZ1源在金丝雀群岛观测台上的光学验证和表征。 ii。 ITP13观察的第二年
Optical validation and characterisation of Planck PSZ1 sources at the Canary Islands observatories. II. Second year of ITP13 observations
论文作者
论文摘要
我们报告了PSZ1目录中以前未知的新星系簇。这里提出的结果是在一项为期两年的观察计划的第二年中实现的，即在罗克·德洛斯·莫·曼乔（Roque de los Muchachos）天文台（西班牙拉帕尔马）开发的ITP13。我们通过执行深度光学成像和光谱范围来表征75个具有较低SZ显着性的SZ源，SZ S/N $ <5.32 $，以将实际的Galaxy簇与SZ Planck源相关联。我们基于2D空间分布，丰富度和速度分散剂来确认最高$ z <0.85 $的实际光学对应物。在ITP13观察计划的末尾，我们使用$ dec \ geq -15^{\ circ} $（其中212个完全未知）研究256 sz源，找到了152 sz源的光学对应物。 ITP13验证程序使我们能够更新PSZ1纯度，该PSZ1纯度现在更加精致，在低SZ S/N制度中从72 \％增加到83 \％。我们的结果与完整的PSZ1目录的预测纯度曲线以及前景信号的非高斯噪声引起的预期纯度曲线一致。实际上，我们发现未确认的来源的数量与857 GHz处的弥漫性银河粉尘的热发射之间存在很强的相关性，从而增加了低银河纬度下的假planck SZ检测的比例。
We report new galaxy clusters previously unknown included in the PSZ1 catalogue. The results here presented have been achieved during the second year of a 2-year observational programme, the ITP13, developed at the Roque de los Muchachos Observatory (La Palma, Spain). We characterise 75 SZ sources with low SZ significance, SZ S/N$<5.32$ by performing deep optical imaging and spectroscopy in order to associate actual galaxy clusters to the SZ Planck source. We adopt robust criteria, based on the 2D-spatial distribution, richness and velocity dispersions to confirm actual optical counterparts up to $z<0.85$. At the end of the ITP13 observational programme, we study 256 SZ sources with $Dec \geq -15^{\circ}$ (212 of them completely unknown), finding optical counterparts for 152 SZ sources. The ITP13 validation programme has allowed us to update the PSZ1 purity, which is now more refined, increasing from 72\% to 83\% in the low SZ S/N regime. Our results are consistent with the predicted purity curve for the full PSZ1 catalogue and with the expected fraction of false detections caused by the non-Gaussian noise of foreground signals. Indeed, we find a strong correlation between the number of unconfirmed sources and the thermal emission of diffuse galactic dust at 857 GHz, thus increasing the fraction of false Planck SZ detections at low galactic latitudes.
