Physical properties of the molecular cloud, N4, in SS 433: Evidence for an interaction of molecular cloud with the jet from SS 433
Physical properties of the molecular cloud, N4, in SS 433: Evidence for an interaction of molecular cloud with the jet from SS 433
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SS 433 中分子云 N4 的物理特性：分子云与 SS 433 射流相互作用的证据
DOI：
10.1093/pasj/psac012
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发表时间：
2022
期刊：
影响因子：
--
通讯作者：
Kohei Kurahara
中科院分区：
文献类型：
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作者：
Hiroaki Yamamoto;Ryuji Okamoto;Yasuhiro Murata;Hiroyuki Nakanishi;Hiroshi Imai;Kohei Kurahara
在12CO(J=1-0)、12CO(J=3-2)、13CO(J=3-2)和大态OH发射中，我们对位于∼40 PC和射电壳层相同视线的分子云N4进行了观测和分析。N4在北缘、东缘和西缘有12CO(J=1-0，3-2)发射的强积分强度梯度。N4的主体也具有∼0.16 Km S−1(20“)−1的速度梯度。仅在N4的西北部检测到与 49 S−1的系统速度相差3 Km的S −1的速度。用RADEX程序估算了12CO(J=1-0)和13CO(J=3-2)发射的8个局部峰的分子氢气的体积密度和运动温度。计算的N4质量为103 cm−3，Tk范围为∼20~∼56 K，N4的质量估计为∼7300m⊙。N4的热压和湍流压分别为∼105K cm−3和∼107K cm−3。N4中的热压和湍流压的关系趋于类似于银河系平面上分子云的关系。然而，这些值高于银河系平面中典型的分子云中的值。几个代表N4物理性质的间接证据以及与红外和X射线辐射数据的比较表明，N4正在与SS-433的一股喷流相互作用。然而，没有探测到N4的伽马射线辐射。与以往的研究相比，由于目前的伽马射线观测站灵敏度较低，很难探测到宇宙射线质子起源的伽马射线辐射。由于观测的低灵敏度和天线波束的稀释，没有检测到向N4的OH发射。
We conducted observations and analyses of the molecular cloud, N4, which is located at ∼40 pc from SS 433 and the same line of sight as that of the radio shell, in12CO(J= 1–0),12CO(J= 3–2),13CO(J= 3–2), and grand-state OH emissions. N4 has a strong gradient of the integrated intensity of12CO(J= 1–0, 3–2) emission at the northern, eastern, and western edges. The main body of N4 also has a velocity gradient of ∼0.16 km s−1(20″)−1. A velocity shift by up to 3 km s−1from the systemic velocity at ∼49 km s−1is detected at only the northwestern part of N4. The volume density of the molecular hydrogen gas and the kinematic temperature are estimated at eight local peaks of12CO(J= 1–0) and13CO(J= 3–2) emissions by the RADEX code. The calculatedis an order of 103cm−3, andTkranges from ∼20 to ∼56 K. The mass of N4 is estimated to be ∼7300M⊙. The thermal and turbulent pressures in N4 are estimated to be ∼105K cm−3and ∼107K cm−3, respectively. The relation of the thermal and turbulent pressures in N4 tends to be similar to that of the molecular clouds in the Galactic plane. However, these values are higher than those in the typical molecular clouds in the Galactic plane. Several pieces of circumstantial evidence representing the physical properties of N4 and comparison with the data of infrared and X-ray radiation suggest that N4 is interacting with a jet from SS 433. However, no gamma-ray radiation is detected toward N4. Compared to the previous study, it is hard to detect the gamma-ray radiation by cosmic-ray proton origin due to the low sensitivity of the current gamma-ray observatories. No OH emission was detected toward N4 due to the low sensitivity of the observation and antenna beam dilution.