arXiv 1908.013582019-08-04astro-ph.GA

在$z\sim 2$对大质量活动星系的多波长研究：电离和分子气体运动学的耦合

A multi-wavelength study of a massive, active galaxy at $z\sim 2$: coupling the kinematics of the ionized and molecular gas

Federica Loiacono, Margherita Talia, Filippo Fraternali, Andrea Cimatti, Enrico Maria Di Teodoro, Gabriel Bartosch Caminha

备注：: 18 pages, 12 figures
DOI：: 10.1093/mnras/stz2170

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摘要：

我们报告了对大质量（$M_{\star} \gtrsim 10^{11} \rm{M}_{\odot}$），$z\sim 2$恒星形成星系GMASS 0953的多波长研究，该星系拥有一个模糊的活动星系核。我们结合GNIRS、SINFONI和KMOS光谱仪的近红外观测来研究[O III] $λ5007$和H $α$发射线的运动学。我们的分析表明，GMASS 0953可能拥有一个电离盘，延伸到13 kpc，在最外半径以$V_{\rm{ion}} = 203^{+17}_{-20} {\ \rm kms}^{-1}$的速度旋转。CO（J=6-5）谱线上出现了较小尺度（$R \sim 1$ kpc）旋转的证据。由分子气体追踪到的中心速度$V_{\rm{CO}} = 320^{+ 92}_{-53} {\ \rm kms}^{-1}$高于$V_{\rm{ion}}$，这表明星系拥有一个多相盘，其旋转曲线在非常中心的区域达到峰值。该星系似乎很好地位于$z = 0$重子塔利-费舍尔关系。我们还讨论了[O III] $λ5007$和H $α$速度梯度是由于银河尺度风的可能性。此外，我们还发现了活动星系核驱动的外流的证据，由一个广泛的蓝移机翼影响[O III] $λ5007$线，这提出了一个速度偏移$Δv = -535 \pm 152 {\ \rm kms}^{-1}$从系统速度。由于气体喷射和恒星形成活动消耗气体的时间尺度很短（$τ_{\rm{dep}}\sim 10^8$ yr），GMASS 0953可能会演变成一个被动星系。然而，由于影响流出率的不确定性，活动星系核在耗尽星系气体库中的作用还不清楚。

英文摘要：

We report a multi-wavelength study of the massive ($M_{\star} \gtrsim 10^{11} \rm{M}_{\odot}$), $z\sim 2$ star-forming galaxy GMASS 0953, which hosts an obscured AGN. We combined near-infrared observations of the GNIRS, SINFONI and KMOS spectrographs to study the kinematics of the [O III]$λ5007$ and H$α$ emission lines. Our analysis shows that GMASS 0953 may host an ionized disc extending up to 13 kpc, which rotates at a velocity of $V_{\rm{ion}} = 203^{+17}_{-20} {\ \rm kms}^{-1}$ at the outermost radius. Evidence of rotation on a smaller scale ($R \sim 1$ kpc) arises from the CO(J=6-5) line. The central velocity $V_{\rm{CO}} = 320^{+ 92}_{-53} {\ \rm kms}^{-1}$ traced by the molecular gas is higher than $V_{\rm{ion}}$, suggesting that the galaxy harbors a multi-phase disc with a rotation curve that peaks in the very central regions. The galaxy appears well located on the $z = 0$ baryonic Tully-Fisher relation. We also discuss the possibility that the [O III]$λ5007$ and H$α$ velocity gradients are due to a galactic-scale wind. Besides, we found evidence of an AGN-driven outflow traced by a broad blueshifted wing affecting the [O III]$λ5007$ line, which presents a velocity offset $Δv = -535 \pm 152 {\ \rm kms}^{-1}$ from the systemic velocity. Because of the short depletion timescale ($τ_{\rm{dep}}\sim 10^8$ yr) due to gas ejection and gas consumption by star formation activity, GMASS 0953 may likely evolve into a passive galaxy. However, the role of the AGN in depleting the gas reservoir of the galaxy is quite unclear because of the uncertainties affecting the outflow rate.

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