Properties of Interstellar Medium In Infrared Bright QSOs Probed by [O I]63 micron and [C II]158 micron Emission Lines

TL;DR

This study investigates the interstellar medium in QSO host galaxies at low redshift using far-infrared spectroscopy, revealing emission line properties similar to local ULIRGs and suggesting dense, warm ISM conditions near active galactic nuclei.

Contribution

First detailed analysis of [OI]63μm and [CII]158μm emission lines in low-redshift QSOs, linking line ratios to ISM density and radiation fields, and identifying broad emission components.

Findings

[OI] and [CII] emission detected in most sources.

Line ratios comparable to local ULIRGs, higher than high-z QSOs.

Broad [OI] emission in one QSO suggests dense, warm ISM or outflows.

Abstract

We present a study of interstellar medium in the host galaxies of 9 QSOs at 0.1<z<0.2 with blackhole masses of $3\times10^7\,M_\odot$ to $3\times10^9\,M_\odot$ based on the far-IR spectroscopy taken with {\it Herschel Space Observatory}. We detect the [OI]63$\mu$m ([CII]158$\mu$m) emission in 6(8) out of 8(9) sources. Our QSO sample has far-infrared luminosities (LFIR)~several times $10^{11}L_\odot$. The observed line-to-LFIR ratios (LOI/LFIR and LCII/LFIR) are in the ranges of $2.6\times10^{-4}$-$10^{-2}$ and $2.8\times10^{-4}$-$2\times10^{-3}$ respectively (including upper limits). These ratios are comparable to the values found in local ULIRGs, but higher than the average value published so far for $z$$>$1 IR bright QSOs. One target, W0752+19, shows an additional broad velocity component (~720 km/s), and exceptionally strong [OI]63$\mu$m emission with LOI/LFIR of $10^{-2}$, an order of magnitude higher than that of average value found among local (U)LIRGs. Combining with the analyses of the {\it SDSS} optical spectra, we conclude that the [OI]63$\mu$m emission in these QSOs is unlikely excited by shocks. We infer that the broad [OI]63 micron emission in W0752+19 could arise from the warm and dense ISM in the narrow line region of the central AGN. Another possible explanation is the existence of a dense gas outflow with $n_{\rm H}\sim10^4$\,cm$^{-3}$, where the corresponding broad [CII] emission is suppressed. Based on the far-IR [OI] and [CII] line ratios, we estimate the constraints on the ISM density and UV radiation field intensity of $n_{\rm H} \lesssim 10^{3.3}$ cm$^{-3}$ and $10^3<G_0 \lesssim 10^{4.2}$, respectively. These values are consistent with those found in local Seyfert 1 ULIRGs. In contrast, the gas with broad velocity width in W0752+19 has $n_{\rm H} \gtrsim 10^{4.3}$ cm$^{-3}$ and $G_0>10^4$.