KAOSS：z~1.3-2.6尘埃遮蔽恒星形成星系中湍动但呈盘状的运动学特征
KAOSS: turbulent, but disc-like kinematics in dust-obscured star-forming galaxies at $z\sim$1.3-2.6
AI总结：
基于KAOSS项目对27个z~1.3-2.6尘埃遮蔽恒星形成星系的Hα积分场光谱观测，发现其中24个呈盘状运动学特征，兼具较快旋转与较高速度弥散，并证实其恒星质量Tully-Fisher关系自z~2以来无演化，支持其演化为大质量早型星系。
摘要：
我们展示了27个ALMA证认的尘埃遮蔽恒星形成星系（DSFGs）在z~1.3-2.6处的空间分辨运动学，这些星系通过VLT/KMOS近红外积分场光谱观测的Hα发射线进行追踪，数据来自“KMOS-ALMA亚毫米源观测”（KAOSS）大型项目。我们推导了这些DSFGs的Hα旋转曲线和速度弥散剖面，发现在27个具有明亮、空间延展Hα发射的源中，有24个显示出盘状运动学证据。对于这些盘状源，我们测得在2.2Rd处的倾角校正速度中值为vrot=190±40 km/s，内禀速度弥散为σ0=87±6 km/s。运动学给出的中值圆周速度为vcirc=230±20 km/s，在2Re（半径约7 kpc）内的动力学质量为Mdyn=(1.1±0.2)×10^11 M⊙。与恒星形成活动较弱的星系相比，KAOSS DSFGs旋转更快且具有更高的内禀速度弥散，但具有相似的vrot/σ0比值，中值v/σ0=2.5±0.5。我们认为这些DSFGs的运动学以旋转支撑为主，但存在不可忽略的压力支撑贡献，这可能由恒星形成或并合/相互作用驱动。我们估算了盘状DSFGs的恒星质量Tully-Fisher关系（sTFR）的归一化，并与本地研究进行比较，发现在固定斜率下z~2与z~0之间没有演化。最后，我们表明DSFG群体的运动学性质与它们演化为大质量早型星系一致，后者是在这些质量处z~0时期的主导群体。
英文摘要：
We present spatially resolved kinematics of 27 ALMA-identified dust-obscured star-forming galaxies (DSFGs) at $z\sim$1.3-2.6, as traced by H$α$ emission using VLT/KMOS near-infrared integral field spectroscopy from the "KMOS-ALMA Observations of Submillimetre Sources" (KAOSS) Large Programme. We derive H$α$ rotation curves and velocity dispersion profiles for the DSFGs, and find that among the 27 sources with bright, spatially extended H$α$ emission, 24 display evidence for disc-like kinematics. We measure a median inclination-corrected velocity at 2.2$R_{\rm d}$ of $v_{\rm rot}=$190$\pm$40kms$^{-1}$ and intrinsic velocity dispersion of $σ_0=$87$\pm$6kms$^{-1}$ for these disc-like sources. The kinematics yield median circular velocities of $v_{\rm circ}=$230$\pm$20kms$^{-1}$ and dynamical masses within 2$R_{\rm e}$ ($\sim$7kpc radius) of $M_{\rm dyn}=$(1.1$\pm$0.2)$\times$10$^{11}$M$_\odot$. Compared to less actively star-forming galaxies, KAOSS DSFGs are both faster rotating with higher intrinsic velocity dispersions, but have similar $v_{\rm rot}/σ_0$ ratios, median $v/σ_0=$2.5$\pm$0.5. We suggest that the kinematics of the DSFGs are primarily rotation supported but with a non-negligible contribution from pressure support, which may be driven by star formation or mergers/interactions. We estimate the normalisation of the stellar mass Tully-Fisher relation (sTFR) for the disc-like DSFGs and compare it with local studies, finding no evolution at fixed slope between $z\sim$2 and $z\sim$0. Finally, we show that the kinematic properties of the DSFG population are consistent with them evolving into massive early-type galaxies, the dominant $z\sim$0 population at these masses.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
