发表机构
Kavli Institute for Astronomy and Astrophysics, Peking University; Department of Astronomy, School of Physics, Peking University; Department of Astronomy, University of Massachusetts, Amherst; Department of Astronomy, University of Science and Technology of China; School of Astronomy and Space Science, University of Science and Technology of China（北京大学科维理天文与天体物理研究所; 北京大学物理学院天文学系; 马萨诸塞大学阿默斯特分校天文学系; 中国科学技术大学天文学系; 中国科学技术大学天文与空间科学学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
利用与弱引力透镜约束一致的晕质量估计，在SDSS样本中未发现单暗晕星系一致性信号，表明先前基于丰度匹配的强信号主要源于晕质量估计偏差。
AI 中文摘要
单暗晕星系一致性是指在固定晕质量下，中心星系被熄灭的暗晕中的卫星星系，其恒星形成活动低于中心星系仍在形成恒星的暗晕中的卫星星系的趋势。它是探究星系-暗晕连接以及可能耦合中心星系和卫星星系演化的整个暗晕熄灭过程的重要探针。然而，其存在性仍存争议，因为一致性必须在固定晕质量下测量，而晕质量难以准确估计。在本快报中，我们利用五个恒星质量完备样本和三种晕质量估计方法测量了SDSS中的单暗晕一致性：一种最大似然（ML）估计，其恒星形成和熄灭的恒星质量-晕质量关系（SHMR）与独立的弱引力透镜约束一致，以及两种传统的丰度匹配（AM）估计。我们将一致性量化为恒星形成和熄灭中心星系的卫星星系之间中值$\log({\rm sSFR})$的差异，同时使用卫星级和晕级统计量。两种AM估计产生了强的正一致性信号，与先前基于AM的测量一致，但这些信号无法用ML晕质量重现。对于晕级统计量，代表性的基于AM的信号对于光度排序和质量排序的AM晕质量分别为$+0.38\pm0.04$ dex和$+0.23\pm0.04$ dex，相对于无一致性分别以约$10\sigma$和$6\sigma$检测到。相比之下，ML结果与无一致性一致，为$+0.00\pm0.03$ dex；卫星级统计量给出类似结果。因此，在晕质量估计与弱引力透镜约束一致的情况下，我们在当前的SDSS样本中未发现可探测的单暗晕一致性信号，这表明强的基于AM的信号在很大程度上是由晕质量估计偏差驱动的。
英文摘要
One-halo galactic conformity is the tendency for satellites in halos with quenched centrals to have lower star-formation activity than those in halos with star-forming centrals at fixed halo mass. It is an important probe of the galaxy--halo connection and halo-wide quenching processes that may couple central and satellite evolution. However, its existence remains controversial, because conformity must be measured at fixed halo mass, while halo masses are difficult to estimate accurately. In this Letter, we measure one-halo conformity in SDSS using five stellar-mass-complete samples and three halo-mass estimates: an ML estimate whose star-forming and quenched stellar mass--halo mass relations (SHMRs) agree with independent weak-lensing constraints, and two conventional abundance-matching (AM) estimates. We quantify conformity as the difference in median $\log({\rm sSFR})$ between satellites of star-forming and quenched centrals, using both satellite-level and halo-level statistics. The two AM estimates produce strong positive conformity signals, consistent with previous AM-based measurements, but these signals are not reproduced with the ML halo masses. For the halo-level statistic, the representative AM-based signals are $+0.38\pm0.04$ dex and $+0.23\pm0.04$ dex for the luminosity-ranking and mass-ranking AM halo masses, detected relative to no conformity at about $10σ$ and $6σ$, respectively. In contrast, the ML result is consistent with no conformity, $+0.00\pm0.03$ dex; the satellite-level statistic gives a similar result. Thus, with halo-mass estimates consistent with weak-lensing constraints, we find no detectable one-halo conformity signal in the present SDSS sample, suggesting that the strong AM-based signal is largely driven by halo-mass estimation biases.
Comments9 pages, 4 figures, 1 table; Accepted for publication in the ApJL; This is the seventeenth paper in the "From Halos to Galaxies" series
