# An energetic high-velocity compact cloud: CO$-$0.31+0.11

## TL;DR

The paper reports the discovery of a high-velocity compact cloud near the Galactic center with properties suggesting it may host an intermediate-mass black hole, based on its kinematics, compactness, and energetic features.

## Contribution

It presents the identification and analysis of CO$-$0.31+0.11, proposing it as a potential signature of an intermediate-mass black hole in the Galactic center region.

## Key findings

- The cloud exhibits broad velocity width and high CO intensity ratio.
- Kinematic modeling suggests a massive object of 2x10^5 solar masses within 0.1 pc.
- The cloud's features imply interaction with a possible intermediate-mass black hole.

## Abstract

We have discovered an energetic high-velocity compact cloud CO$-$0.31+0.11 in the central molecular zone of our Galaxy. CO$-$0.31+0.11 is located at a projected distance of $\sim 45$ pc from the Galactic nucleus Sgr A$^*$. It is characterized by its compact spatial appearance ($d\simeq4$ pc), extremely broad velocity width ($\Delta V > 100$ km s$^{-1}$), and high CO $J$=3$-$2/$J$=1$-$0 intensity ratio. The total gas mass and kinetic energy are estimated as approximately $10^4$ $M_\odot$ and $10^{51}$ erg, respectively. Two expanding bubble-like structures are found in our HCN $J$=1$-$0 map obtained with the Nobeyama Radio Observatory 45 m telescope. In the longitude--velocity maps, CO$-$0.31+0.11 exhibits an asymmetric V-shape. This kinematical structure can be well fitted by Keplerian motion on an eccentric orbit around a point mass of $2\times 10^5$ $M_\odot$. The enhanced CO $J$=3$-$2/$J$=1$-$0 ratio is possibly attributed to the tidal compression during the pericenter passage. The model suggests that a huge mass is packed within a radius of $r < 0.1$ pc. The huge mass, compactness and absence of luminous stellar counterparts may correspond to a signature of an intermediate-mass black hole (IMBH) inside. We propose a formation scenario of CO$-$0.31+0.11 in which a compact cloud has gravitationally interacted with an IMBH and a bipolar molecular outflow was driven by the past activity of the putative IMBH.