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Lookup NU author(s): Dr Chris HarrisonORCiD, Dr David RosarioORCiD
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© 2020 The Author(s). As part of our KMOS AGN Survey at High-redshift (KASHz), we present spatially resolved VLT/KMOS and VLT/SINFONI spectroscopic data and ALMA 870 μm continuum imaging of eight z = 1.4-2.6 moderate AGN (L2-10 kev = 1042-1045 ergs s-1).We map [OIII], Hα and rest-frame FIR emission to search for any spatial anticorrelation between ionised outflows (traced by the [O III] line) and star formation (SF; traced by Hα and FIR), that has previously been claimed for some high-z AGN and used as evidence for negative and/or positive AGN feedback. First, we conclude that Hα is unreliable to map SF inside our AGN host galaxies based on: (i) SF rates inferred from attenuation-corrected Hα can lie below those inferred from FIR; (ii) the FIR continuum is more compact than the Hα emission by a factor of ≈2 on average; (iii) in half of our sample, we observe significant spatial offsets between the FIR and Hα emission, with an average offset of 1.4 ± 0.6 kpc. Secondly, for the five targets with outflows we find no evidence for a spatial anticorrelation between outflows and SF using either Hα or FIR as a tracer. This holds for our re-analysis of a famous z = 1.6 X-ray AGN ('XID 2028') where positive and negative feedback has been previously claimed. Based on our results, any impact on SF by ionised outflows must be subtle, either occurring on scales below our resolution, or on long time-scales.
Author(s): Scholtz J, Harrison CM, Rosario DJ, Alexander DM, Chen C-C, Kakkad D, Mainieri V, Tiley AL, Turner O, Cirasuolo M, Sharples RM, Stach S
Publication type: Article
Publication status: Published
Journal: Monthly Notices of the Royal Astronomical Society
Year: 2020
Volume: 492
Issue: 3
Pages: 3194-3216
Print publication date: 01/03/2020
Online publication date: 10/01/2020
Acceptance date: 19/12/2019
ISSN (print): 0035-8711
ISSN (electronic): 1365-2966
Publisher: Oxford University Press
URL: https://doi.org/10.1093/mnras/staa030
DOI: 10.1093/mnras/staa030
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