论文标题
Carla J1103+3449集群Z = 1.44的Carla J1103+3449群集周围的大量分子气体储存
Massive molecular gas reservoir around the central AGN in the CARLA J1103+3449 cluster at z=1.44
论文作者
论文摘要
被动的早期型星系在Z $ \ Lessim $ 1.5的群集核心占主导地位。在较高的红移时，观察到簇核心星系仍在冷分子气体的推动下仍在进行恒星形成。我们测量了与Noema的z = 1.44，在carla j1103+3449群集中的中央区域的分子气体库中。 AGN同步加速器发射在94.48 GHz处主导连续发射，我们在AGN位置和两个无线电飞机的位置测量其通量。将我们的测量结果与在4.71 GHz-94.5 GHz范围内的已发布结果相结合，我们获得了一个平坦的光谱指数$α= 0.14 \ pm 0.03 $，对于AGN核心排放，以及较陡的指数$α= 1.43 \ pm 0.04 $和$ $ $ y = 1.15 = 1.15 \ pm 0.04 $ \ \ pm 0.04 $ closeSters tossesss和Easters和Easters和Easters和Ese and Easty and Easters and Easty and Easty and and Easty and and Easty s。在73.8 MHz-94.5 GHz范围内，总光谱指数为$α= 0.92 \ pm 0.02 $。我们检测到两条CO（2-1）发射线，均相对于AGN进行蓝色转移。它们的排放量对应于AGN西南约17 kpc东南约17 kpc的两个区域，与星系无关。在这两个区域中，我们发现$ M_ {gas} $ = 3.9 $ \ pm $ 0.4 $ 10^{10} m _ {\ odot} $的总体分子气体储量为$ m_ {al} $ = 3.9 $ \ pm $ 0.4 $ 10^{\ odot} $，它以中央总分子气体储量为中心（〜60％）。这些结果可以通过集群中心的大量凉爽气流来解释。 AGN早期型宿主尚未消失。它的恒星形成速率与该场中星形星系的主要序列（SFR〜30-140 $ M _ {\ odot} $/yr）一致，并且预计簇核心分子气体储量有望在静止前喂养AGN和宿主星体。另一个群集确认的成员显示，在类似的红移下，恒星形成速率低于野外主序列的〜2 $σ$，并且没有比该场类似恒星质量的星系大的分子气体质量。
Passive early-type galaxies dominate cluster cores at z $\lesssim$1.5. At higher redshift, cluster core galaxies are observed to have still on-going star-formation, fuelled by cold molecular gas. We measure the molecular gas reservoir of the central region around the radio-loud AGN in the cluster CARLA J1103+3449 at z=1.44 with NOEMA. The AGN synchrotron emission dominates the continuum emission at 94.48 GHz, and we measure its flux at the AGN position and at the position of two radio jets. Combining our measurements with published results over the range 4.71 GHz-94.5 GHz, we obtain a flat spectral index $α= 0.14 \pm 0.03$ for the AGN core emission, and a steeper index $α= 1.43 \pm 0.04$ and $α= 1.15 \pm 0.04$ at positions close to the western and eastern lobe, respectively. The total spectral index is $α= 0.92 \pm 0.02$ over the range 73.8 MHz-94.5 GHz. We detect two CO(2-1) emission lines, both blue-shifted with respect to the AGN. Their emission corresponds to two regions, ~17 kpc south-east and ~14 kpc south-west of the AGN, not associated with galaxies. In these two regions, we find a total massive molecular gas reservoir of $M_{gas}$ = 3.9 $\pm$ 0.4 $10^{10} M_{\odot}$, which dominates (~ 60%) the central total molecular gas reservoir. These results can be explained by massive cool gas flows in the center of the cluster. The AGN early-type host is not yet quenched; its star formation rate is consistent with being on the main sequence of star-forming galaxies in the field (SFR~30-140 $M_{\odot}$/yr), and the cluster core molecular gas reservoir is expected to feed the AGN and the host star-formation before quiescence. The other cluster confirmed members show star formation rates at ~2 $σ$ below the field main sequence at similar redshifts and do not have molecular gas masses larger than galaxies of similar stellar mass in the field.
