A spectral stacking analysis to search for faint outflow signatures in z~6 quasars

TL;DR

This study employs spectral stacking of ALMA data to search for faint high-velocity outflow signatures in z~6 quasars, providing tentative evidence of broad emission components indicative of outflows.

Contribution

It introduces a spectral stacking method tailored for interferometric data to detect faint outflow signals in high-redshift quasars, a novel approach in this context.

Findings

Tentative detection of broad emission line component in stacked spectra.

Broad component characterized by FWHM > 700 km/s.

Sub-sample stacking enhances outflow signal detection.

Abstract

Outflows in quasars during the early epochs of galaxy evolution are an important part of the feedback mechanisms potentially affecting the evolution of the host galaxy. However, systematic observations of outflows are only now becoming possible with the advent of sensitive mm telescopes. In this study we use spectral stacking methods to search for faint high velocity outflow signal in a sample of [C II] detected, z ~ 6 quasars. We search for broad emission line signatures from high-velocity outflows for a sample of 26 z ~ 6 quasars observed with ALMA, with a detection of the [C II] line. The observed emission lines of the sources are dominated by the host galaxy, and outflow emission is not detected for the individual sources. We use a spectral line stacking analysis developed for interferometric data to search for outflow emission. We stack both extracted spectra and the full spectral cubes. We also investigate the possibility that only a sub-set of our sample contributes to the stacked outflow emission. We find only a tentative detection of a broad emission line component in the stacked spectra. When taking a region of about 2 arcsec around the source central position of the stacked cubes, the stacked line shows an excess emission due to a broad component of 1.1-1.5 sigma, but the significance drops to 0.4-0.7 sigma when stacking the extracted spectra from a smaller region. The broad component can be characterised by a line width of full width half max FWHM > 700 km/s. Furthermore, we find a sub-sample of 12 sources the stack of which maximises the broad component emission. The stack of this sub-sample shows an excess emission due to a broad component of 1.2-2.5 sigma. The stacked line of these sources has a broad component of FWHM > 775 km/s. Deeper ALMA observations are necessary to confirm the presence of a broad component in the individual spectra.