# The X-ray variability of Seyfert 1.8/1.9 galaxies

## TL;DR

This study investigates the UV and X-ray variability of Seyfert 1.8/1.9 galaxies, revealing distinct variability patterns from Seyfert 2s, and suggests these differences imply they should be treated separately in AGN research.

## Contribution

It provides a homogeneous analysis of UV and X-ray variability in Seyfert 1.8/1.9 galaxies, highlighting their differences from Seyfert 2s in these wavelengths.

## Key findings

- All nuclei show X-ray variability over days to years.
- Intrinsic source changes dominate variability patterns.
- Seyfert 1.8/1.9 differ from Seyfert 2 in UV/X-ray variability.

## Abstract

Seyfert 1.8/1.9 are sources showing weak broad H-alpha components in their optical spectra. We aim at testing whether Seyfert 1.8/1.9 have similar properties at UV and X-ray wavelengths to Seyfert 2. We use the 15 Seyfert 1.8/1.9 in the Veron Cetty and Veron catalogue with public data available from the Chandra and/or XMM-Newton archives at different dates, with timescales between observations ranging from days to years. Our results are homogeneously compared with a previous work using the same methodology applied to a sample of Seyfert 2 (Hernandez-Garcia et al. 2015). X-ray variability is found in all 15 nuclei over the aforementioned ranges of timescales. The main variability pattern is related to intrinsic changes in the sources, which are observed in ten nuclei. Changes in the column density are also frequent, as they are observed in six nuclei, and variations at soft energies, possibly related to scattered nuclear emission, are detected in six sources. X-ray intraday variations are detected in six out of the eight studied sources. Variations at UV frequencies are detected in seven out of nine sources. A comparison between the samples of Seyfert 1.8/1.9 and 2 shows that, even if the main variability pattern is due to intrinsic changes of the sources in the two families, these nuclei exhibit different variability properties in the UV and X-ray domains. In particular, variations in the broad X-ray band on short time-scales (days/weeks), and variations in the soft X-rays and UV on long time-scales (months/years) are detected in Seyfert 1.8/1.9 but not in Seyfert 2. Overall, we suggest that optically classified Seyfert 1.8/1.9 should be kept separated from Seyfert 2 galaxies in UV/X-ray studies of the obscured AGN population because their intrinsic properties might be different.