# Characterization of the continuum and kinematical properties of nearby NLS1

## TL;DR

This study analyzes the spectral and kinematic properties of nearby NLS1 galaxies, revealing their continuum characteristics, black hole masses, and their position relative to the MBH-σ relation, using SDSS data and spectral synthesis techniques.

## Contribution

It provides a detailed spectral analysis of NLS1 galaxies, including continuum modeling and black hole mass estimation, and re-examines their placement on the MBH-σ relation.

## Key findings

- Median non-stellar continuum slope of -1.6
- Black hole masses range from 10^5.6 to 10^7.5 solar masses
- Most NLS1 galaxies lie below the MBH-σ relation

## Abstract

In order to study the slope and strength of the non-stellar continuum, we analyzed a sample of nearby Narrow Line Seyfert 1 (NLS1). Also, we re-examined the location of NLS1 galaxies on the M $-$ $\sigma$ relation using the stellar velocity dispersion and the [OIII]$\lambda$5007 emission line as surrogate of the former. We studied spectra of a sample of 131 NLS1 galaxies taken from the Sloan Digital Sky Survey (SDSS) DR7. We approached determining the non-stellar continuum by employing the spectral synthesis technique, which uses the code {\sc starlight}, and by adopting a power-law base to model the non-stellar continuum. Composite spectra of NLS1 galaxies were also obtained based on the sample.In addition, we obtained the stellar velocity dispersion from the code and by measuring Calcium II Triplet absorption lines and [OIII] emission lines. From Gaussian decomposition of the H$\beta$ profile we calculated the black hole mass. We obtained a median slope of $\beta$ = $-$1.6 with a median fraction of contribution of the non-stellar continuum to the total flux of 0.64. We determined black hole masses in the range of log(M$_{BH}$/M$_{\odot}$) = 5.6 $-$ 7.5 which is in agreement with previous works. We found a correlation between the luminosity of the broad component of H$\beta$ and black hole mass with the fraction of a power-law component. Finally, according to our results, NLS1 galaxies in our sample are located mostly underneath the MBH - $\sigma_{\star}$ relation, both considering the stellar velocity dispersion ($\sigma_{\star}$) and the core component of [OIII]$\lambda$5007.