A Sample of Massive Black Holes in Dwarf Galaxies Detected via [Fe X] Coronal Line Emission: Active Galactic Nuclei and/or Tidal Disruption Events

TL;DR

This study identifies 81 dwarf galaxies with coronal [Fe X] emission indicating active massive black holes, revealing a population often missed by traditional optical AGN searches and highlighting coronal lines as effective detection tools.

Contribution

The paper presents a novel method using [Fe X] coronal line emission to detect massive black holes in dwarf galaxies, uncovering many previously unrecognized BHs.

Findings

81 dwarf galaxies with [Fe X] emission indicating BH activity

Most [Fe X] luminosities too high for stellar sources, consistent with BH accretion

Many BH candidates identified only through coronal line emission

Abstract

The massive black hole (BH) population in dwarf galaxies ($M_{\rm BH} \lesssim 10^5~M_\odot$) can provide strong constraints on the origin of BH seeds. However, traditional optical searches for active galactic nuclei (AGNs) only reliably detect high-accretion, relatively high-mass BHs in dwarf galaxies with low amounts of star formation, leaving a large portion of the overall BH population in dwarf galaxies relatively unexplored. Here, we present a sample of 81 dwarf galaxies ($M_\star \le 3 \times 10^9~M_\odot$) with detectable [Fe X]$\lambda$6374 coronal line emission indicative of accretion onto massive BHs, only two of which were previously identified as optical AGNs. We analyze optical spectroscopy from the Sloan Digital Sky Survey and find [Fe X]$\lambda$6374 luminosities in the range $L_{\rm [Fe\,X]}\approx10^{36}$-$10^{39}$ erg s$^{-1}$, with a median value of $1.6 \times 10^{38}$ erg s$^{-1}$. The [Fe X]$\lambda$6374 luminosities are generally much too high to be produced by stellar sources, including luminous Type IIn supernovae (SNe). Moreover, based on known SNe rates, we expect at most 8 Type IIn SNe in our sample. On the other hand, the [Fe X]$\lambda$6374 luminosities are consistent with accretion onto massive BHs from AGNs or tidal disruption events (TDEs). We find additional indicators of BH accretion in some cases using other emission line diagnostics, optical variability, X-ray and radio emission (or some combination of these). However, many of the galaxies in our sample only have evidence for a massive BH based on their [Fe X]$\lambda$6374 luminosities. This work highlights the power of coronal line emission to find BHs in dwarf galaxies missed by other selection techniques and to probe the BH population in bluer, lower mass dwarf galaxies.