KASHz: No evidence for ionised outflows instantaneously suppressing star formation in moderate luminosity AGN at <i>z</i> ∼ 1.4–2.6

Scholtz, J.; Harrison, C. M.; Rosario, D. J.; Alexander, D. M.; Chen, Chian-Chou; Kakkad, D.; Mainieri, V.; Tiley, Alfred L.; Turner, O. J.; Cirasuolo, M.; Sharples, R. M.; Stach, S. M.

doi:10.1093/mnras/staa030

Cited by 42 publications

(97 citation statements)

References 158 publications

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“…On the other hand, recently a similar study by Scholtz et al (2020) on a sample of eight X-ray selected AGN at z ∼ 2 with strong Hα and [Oiii] lines also found a similar Hα-to-FIR size ratio of 2.3 ± 0.3. This evidence could suggest that somehow AGN is driving the larger Hα sizes, or it could be that this is a general feature of FIR luminous galaxies at z ∼ 2 and the current studies are biased toward galaxies hosting AGN because of their bright-ness of strong optical lines.…”

Section: Size Measurementsmentioning

confidence: 57%

Extended Hα over compact far-infrared continuum in dusty submillimeter galaxies

Chen

Harrison

Smail

et al. 2020

A&A

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Using data from ALMA and near-infrared (NIR) integral field spectrographs including both SINFONI and KMOS on the VLT, we investigate the two-dimensional distributions of Hα and rest-frame far-infrared (FIR) continuum in six submillimeter galaxies at z ∼ 2. At a similar spatial resolution (∼0 . 5 FWHM; ∼4.5 kpc at z = 2), we find that the half-light radius of Hα is significantly larger than that of the FIR continuum in half of the sample, and on average Hα is a median factor of 2.0 ± 0.4 larger. Having explored various ways to correct for the attenuation, we find that the attenuation-corrected Hα-based SFRs are systematically lower than the IR-based SFRs by at least a median factor of 3 ± 1, which cannot be explained by the difference in half-light radius alone. In addition, we find that in 40% of cases the total V-band attenuation (A V ) derived from energy balance modeling of the full ultraviolet(UV)-to-FIR spectral energy distributions (SEDs) is significantly higher than that derived from SED modeling using only the UV-to-NIR part of the SEDs, and the discrepancy appears to increase with increasing total infrared luminosity. Finally, considering all our findings along with the studies in the literature, we postulate that the dust distributions in SMGs, and possibly also in less IR luminous z ∼ 2 massive star-forming galaxies, can be decomposed into three main components; the diffuse dust heated by older stellar populations, the more obscured and extended young star-forming Hii regions, and the heavily obscured central regions that have a low filling factor but dominate the infrared luminosity in which the majority of attenuation cannot be probed via UV-to-NIR emissions.

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Section: Size Measurementsmentioning

confidence: 57%

Extended Hα over compact far-infrared continuum in dusty submillimeter galaxies

Chen

Harrison

Smail

et al. 2020

A&A

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“…The fitting routine then provides posterior probability distributions for various values such as the AGN IR luminosity component, stellar mass, and the integrated luminosity in the IR due to star formation. For further details of the SED modelling, refer to Scholtz et al (2020).…”

Section: Sed Fitting Of the Bat Agn Using Fortesfitmentioning

confidence: 99%

The star formation properties of the observed and simulated AGN Universe: BAT versus EAGLE

Jackson

Rosario

Alexander

et al. 2020

Monthly Notices of the Royal Astronomical Society

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In this paper we present data from 72 low redshift, hard X-ray selected AGN taken from the Swift-BAT 58 month catalogue. We utilise spectral energy distribution fitting to the optical to IR photometry in order to estimate host galaxy properties. We compare this observational sample to a volume and flux matched sample of AGN from the EAGLE hydrodynamical simulations in order to verify how accurately the simulations can reproduce observed AGN host galaxy properties. After correcting for the known +0.2 dex offset in the SFRs between EAGLE and previous observations, we find agreement in the SFR and X-ray luminosity distributions; however we find that the stellar masses in EAGLE are 0.2 − 0.4 dex greater than the observational sample, which consequently leads to lower sSFRs. We compare these results to our previous study at high redshift, finding agreement in both the observations and simulations, whereby the widths of sSFR distributions are similar (∼0.4 − 0.6 dex) and the median of the SFR distributions lie below the star forming main sequence by ∼0.3 − 0.5 dex across all samples. We also use EAGLE to select a sample of AGN host galaxies at high and low redshift and follow their characteristic evolution from z = 8 to z = 0. We find similar behaviour between these two samples, whereby star formation is quenched when the black hole goes through its phase of most rapid growth. Utilising EAGLE we find that 23% of AGN selected at z ∼ 0 are also AGN at high redshift, and that their host galaxies are among the most massive objects in the simulation. Overall we find EAGLE reproduces the observations well, with some minor inconsistencies (∼ 0.2 dex in stellar masses and ∼ 0.4 dex in sSFRs).

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“…203 At the limit of the spatial resolution of our integral field spectroscopic observations (∼few kpc), in combination with high-resolution far-infrared imaging, we have also found no evidence that AGN-driven ionised outflows (traced via high-velocity [O iii] emission) have an instantaneous positive or negative significant impact on the in-situ star-formation in a representative sample of 8 z∼1.4-2.6 AGN (Scholtz et al 2020). This is in qualitative agreement with at least some models that suggest that AGN outflows have no impact upon the in-situ star formation (Gabor & Bournaud 2014).…”

Section: Do Agn Really Suppress Star Formation?mentioning

confidence: 66%

Do AGN really suppress star formation?

Harrison¹,

Alexander

Rosario

et al. 2019

Proc. IAU

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Active galactic nuclei (AGN) are believed to regulate star formation inside their host galaxies through “AGN feedback”. We summarise our on-going study of luminous AGN (z ∼ 0.2−3; LAGN,bol 1043 erg s−1), which is designed to search for observational signatures of feedback by combining observed star-formation rate (SFR) measurements from statistical samples with cosmological model predictions. Using the EAGLE hydrodynamical cosmological simulations, in combination with our Herschel + ALMA surveys, we show that – even in the presence of AGN feedback – we do not necessarily expect to see any relationships between average galaxy-wide SFRs and instantaneous AGN luminosities. We caution that the correlation with stellar mass for both SFR and AGN luminosity can contribute to apparent observed positive trends between these two quantities. On the other hand, the EAGLE simulations, which reproduce our observations, predict that a signature of AGN feedback can be seen in the wide specific SFR distributions of all massive galaxies (not just AGN hosts). Overall, whilst we can not rule out that AGN have an immediate small-scale impact on in-situ star-formation, all of our results are consistent with a feedback model where galaxy-wide in-situ star formation is not rapidly suppressed by AGN, but where the feedback likely acts over a longer timescale than a single AGN episode.

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KASHz: No evidence for ionised outflows instantaneously suppressing star formation in moderate luminosity AGN at z ∼ 1.4–2.6

Cited by 42 publications

References 158 publications

Extended Hα over compact far-infrared continuum in dusty submillimeter galaxies

Extended Hα over compact far-infrared continuum in dusty submillimeter galaxies

The star formation properties of the observed and simulated AGN Universe: BAT versus EAGLE

Do AGN really suppress star formation?

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