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arXiv 2301.02822astro-ph.GA
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$z$ = 5.2射电星系PDKEEPAAAAD PDKEEPAAAAE $-$ 2201的VLA CO（1-0）观测发现的大量分子气体伴星

Massive molecular gas companions uncovered by VLA CO(1-0) observations of the $z$ = 5.2 radio galaxy TN J0924$-$2201

Kianhong Lee, Kotaro Kohno, Bunyo Hatsukade, Fumi Egusa, Takuji Yamashita, Malte Schramm, Kohei Ichikawa, Masatoshi Imanishi, Takuma Izumi, Tohru Nagao, Yoshiki… 展开作者

Kianhong Lee, Kotaro Kohno, Bunyo Hatsukade, Fumi Egusa, Takuji Yamashita, Malte Schramm, Kohei Ichikawa, Masatoshi Imanishi, Takuma Izumi, Tohru Nagao, Yoshiki Toba, Hideki Umehata

备注：
14 pages, 9 figures. Accepted for publication in ApJ
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摘要：

我们介绍卡尔G。Jansky甚大阵列（VLA）K波段（19 GHz）观测到的朝向$z=5.2$射电星系TN J 0924 $-$ 2201的红移CO（1-0）线发射，这是最遥远的CO探测到的射电星系之一。在$\sim2''$的角分辨下，CO（1-0）谱线辐射被分解成三个团簇，在$\pm500$ km_1，s范围内，相对于其红移，由Ly $α$决定。我们发现，他们位于偏离中心和12-33 kpc的主机星系的中心，其中有对应的$HST$ $i$波段，$Spitzer$ /IRAC和ALMA波段-6（230 GHz; 1.3 mm）。通过ALMA探测，我们估计宿主星系的$L_{\rm IR}$和SFR分别为$(9.3\pm1.7)\times10^{11} L_{\odot}$和$110\pm20$ $M_{\odot}\,\rm yr^{-1}$。我们还导出了宿主星系中$M_{\rm H_{2}}<1.3\times10^{10}$ $M_{\odot}$的$3σ$上限。三个团块的CO（1-0）线光度检测值，$L'_{\rm CO(1-0)}$ =（3.2-4.7）$\times10^{10}$ $\rm\,K\,km\,s^{-1}pc^{2}$，表明存在三个块状分子气藏，$M_{\rm H_{2}}$ =（2.5-3.7）$\times10^{10}$ $M_{\odot}$，通过假定CO至H的$_{2}$转换因子$α_{\rm CO} = 0.8$ $M_{\rm \odot}\rm\,(K\,km\,s^{-1}pc^{2})^{-1}$，虽然恒星形成率（SFR）没有提高，因为没有检测到ALMA 1.3 mm连续体（SFR $<$ 40 $M_\odot$ yr $^{-1}$）。距离主星系最近的分子气体团标记为团A，显然与射电喷流轴对齐，显示射电CO对齐。TN J 0924 $-$ 2201周围这三个团块的可能起源可以解释为合并，射流诱导的金属富集和流出。

英文摘要：

We present Karl G. Jansky Very Large Array (VLA) K-band (19 GHz) observations of the redshifted CO(1-0) line emission toward the radio galaxy TN J0924$-$2201 at $z=5.2$, which is one of the most distant CO-detected radio galaxies. With the angular resolution of $\sim2''$, the CO(1-0) line emission is resolved into three clumps, within $\pm500$ km\,s$^{-1}$ relative to its redshift, where is determined by Ly$α$. We find that they locate off-center and 12-33 kpc away from the center of the host galaxy, which has counterparts in $HST$ $i$-band, $Spitzer$/IRAC and ALMA Band-6 (230 GHz; 1.3 mm). With the ALMA detection, we estimate $L_{\rm IR}$ and SFR of the host galaxy to be $(9.3\pm1.7)\times10^{11} L_{\odot}$ and $110\pm20$ $M_{\odot}\,\rm yr^{-1}$, respectively. We also derive the $3σ$ upper limit of $M_{\rm H_{2}}<1.3\times10^{10}$ $M_{\odot}$ at the host galaxy. The detected CO(1-0) line luminosities of three clumps, $L'_{\rm CO(1-0)}$ = (3.2-4.7)$\times10^{10}$ $\rm\,K\,km\,s^{-1}pc^{2}$, indicate the presence of three massive molecular gas reservoirs with $M_{\rm H_{2}}$ = (2.5-3.7)$\times10^{10}$ $M_{\odot}$, by assuming the CO-to-H$_{2}$ conversion factor $α_{\rm CO} = 0.8$ $M_{\rm \odot}\rm\,(K\,km\,s^{-1}pc^{2})^{-1}$, although the star formation rate (SFR) is not elevated because of the non-detection of ALMA 1.3 mm continuum (SFR $<$ 40 $M_\odot$ yr$^{-1}$). From the host galaxy, the nearest molecular gas clump labeled as clump A, is apparently aligning with the radio jet axis, showing the radio-CO alignment. The possible origin of these three clumps around TN J0924$-$2201 can be interpreted as merger, jet-induced metal enrichment and outflow.

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