The nearby dwarf galaxy POX 52 at $z = 0.021$ hosts an active galactic nucleus (AGN) with a black-hole (BH) mass of $M_{\rm BH} \sim 10^{5-6} M_\odot$ and an Eddington ratio of $\sim$ 0.1-1. This object provides the rare opportunity to study both AGN and host-galaxy properties in a low-mass highly accreting system. To do so, we collected its multi-wavelength data from X-ray to radio. First, we construct a spectral energy distribution, and by fitting it with AGN and host-galaxy components, we constrain AGN-disk and dust-torus components. Then, while considering the AGN-disk emission, we decompose optical HST images. As a result, it is found that a classical bulge component is probably present, and its mass ($M_{\rm bulge}$) is consistent with an expected value from a local relation. Lastly, we analyze new quasi-simultaneous X-ray (0.2-30 keV) data obtained by NuSTAR and XMM-Newton. The X-ray spectrum can be reproduced by multi-color blackbody, warm and hot coronae, and disk and torus reflection components. Based on this, the spin is estimated to be $a_{\rm spin} = 0.998_{-0.814}$, which could suggest that most of the current BH mass was achieved by prolonged mass accretion. Given the presence of the bulge, POX 52 would have undergone a galaxy merger, while the $M_{\rm BH}$-$M_{\rm bulge}$ relation and the inferred prolonged accretion could suggest that AGN feedback occurred. Regarding the AGN structure, the spectral slope of the hot corona, its relative strength to the bolometric emission, and the torus structure are found to be consistent with Eddington-ratio dependencies found for nearby AGNs.
The JWST and ALMA view of local dwarf Pox 186: Evidence of stripped binaries driving a hard radiation field and little cold molecular gas resulting in high star-formation efficiency
AURA for European Space Agency (ESA), ESA Office, Space Telescope Science Institute（美国大学研究协会（为欧洲空间局）、欧洲空间局办公室、太空望远镜科学研究所）；Astrophysics Research Institute, Liverpool John Moores University（利物浦约翰摩尔斯大学天体物理研究所）；Space Telescope Science Institute（太空望远镜科学研究所）；Centro de Astrobiología (CAB), CSIC-INTA（天文生物学中心（CAB），西班牙国家科学技术研究委员会-国家航空航天技术研究所）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；AIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris Cité（天体物理学与图像实验室，法国原子能和替代能源委员会，法国国家科学研究中心，巴黎萨克雷大学，巴黎第七大学，索邦巴黎城市大学）；Stockholm University（斯德哥尔摩大学）
Diversity of Ionized Gas Structures in Nearby Metal-poor Dwarf Galaxies
University of Tsukuba（筑波大学）；Tsukuba Institute for Advanced Research (TIAR), University of Tsukuba（筑波大学先进研究院）；Tomonaga Center for the History of the Universe (TCHoU), Faculty of Pure and Applied Sciences, University of Tsukuba（筑波大学理学院朝永振一郎宇宙历史中心）；The University of Tokyo（东京大学）；Stockholm University（斯德哥尔摩大学）；Universidad Nacional Autónoma de México, Instituto de Astronomía（墨西哥国立自治大学天文学研究所）；Nagoya University（名古屋大学）；Waseda University（早稻田大学）
Multi-wavelength morphology and dust emission in low-redshift dwarf galaxies in COSMOS-Web with HST and JWST
University of Hertfordshire（赫特福德大学）；Rochester Institute of Technology（罗切斯特理工学院）；University of Manchester（曼彻斯特大学）；University of Nottingham（诺丁汉大学）；University of Cambridge（剑桥大学）
Chandra and HST Observations of Radio-Selected (Wandering) Massive Black Hole Candidates in Dwarf Galaxies
eXtreme Gravity Institute, Department of Physics, Montana State University（蒙大拿州立大学）；Center for Astrophysics | Harvard & Smithsonian（哈佛-史密森天体物理中心）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado（科罗拉多大学）；Vanderbilt University（范德堡大学）
MaNGA AGN dwarf galaxies (MAD) -- IV. Revealing hidden AGN in dwarf galaxies with radio observations
Donosti International Physics Center (DIPC)（多诺斯蒂亚国际物理中心）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所）；Institut d'Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究学院）
