论文标题
在早期型Galaxy NGC \ 4472的超大质量黑洞二进制上迈向天体限制。
Toward Astrometric Constraints on a Supermassive Black Hole Binary in the Early-Type Galaxy NGC\,4472
论文作者
论文摘要
两个星系的合并，每个星系托管一个质量$ 10^6 $ \，m $ _ {\ odot} $或更多的超级质量黑洞（SMBH）可能会产生绑定的SMBH二进制文件。对于早期类型的星系NGC \，4472，我们研究如何使用下一代非常大的阵列（NGVLA）来监视质量$ M _ {\ rm Pri} $的主要SMBH的反射运动，因为它是由中学Smbh tugy tauge of Mass $ m _ _ _ _ _ _ _ _ {根据其期间$ p $，半轴轴$ a _ {\ rm bin} $铸造推定的SMBH二进制的轨道，质量比$ q = m _ {\ rm sec} / m _ {\ rm pri} \ rm pri} \ le 1 $，我们找到以下的$ 1 $，我们会找到以下时期： 40 \，您可以在空间上解决和监测。 （2）对于95 \％的准确度，根据监视时期，可以在概念概念上的一系列质量比范围内访问$ a _ {\ rm bin} $的sub-parsec值（$ a {\ rm bin} $（$ q>> \ q> \ frac {1}} {1} {4} {4} {4} {4} {4} {4} {4} {4} $ q <\ freac} yg freac {1} {1} {1} {1} （3）如果未检测到1（10）\，yr监测后的$ m _ {\ rm pri} $，则可以排除$ p = 4（40）$ \，yr和质量比$ q> 0.01（0.003）$的SMBH二进制。这将没有表明过去的主要合并的当今证据，例如最近模拟的，在$ q \ sim 1 $ smbh二进制的搜索中，二进制形成了具有运动特征的恒星核心，例如NGC \，4472。 （4）从搜索NGC \，4472的连续重力波中搜索$ Q $的上限可以独立检查上限。
The merger of two galaxies, each hosting a supermassive black hole (SMBH) of mass $10^6$\,M$_{\odot}$ or more, could yield a bound SMBH binary. For the early-type galaxy NGC\,4472, we study how astrometry with a next-generation Very Large Array (ngVLA) could be used to monitor the reflex motion of the primary SMBH of mass $M_{\rm pri}$, as it is tugged on by the secondary SMBH of mass $M_{\rm sec}$. Casting the orbit of the putative SMBH binary in terms of its period $P$, semimajor axis $a_{\rm bin}$, and mass ratio $q = M_{\rm sec} / M_{\rm pri} \le 1$, we find the following: (1) Orbits with fiducial periods of $P = 4$\,yr and 40\,yr could be spatially resolved and monitored. (2) For a 95\% accuracy of $2\,μ$as per monitoring epoch, sub-parsec values of $a_{\rm bin}$ could be accessed over a range of mass ratios notionally encompassing major ($q > \frac{1}{4}$) and minor ($q < \frac{1}{4}$) galaxy mergers. (3) If no reflex motion is detected for $M_{\rm pri}$ after 1(10)\,yr of monitoring, a SMBH binary with period $P = 4(40)$\,yr and mass ratio $q > 0.01(0.003)$ could be excluded. This would suggest no present-day evidence for a past major merger like that recently simulated, where scouring by a $q \sim 1$ SMBH binary formed a stellar core with kinematic traits like those of NGC\,4472. (4) Astrometric monitoring could independently check the upper limits on $q$ from searches for continuous gravitational waves from NGC\,4472.
