Observational evidence of quasar feedback quenching star formation at high redshift

Cano-Díaz, M.; Maiolino, R.; Marconi, A.; Netzer, H.; Shemmer, Ohad; Cresci, G.

doi:10.1051/0004-6361/201118358

Cited by 342 publications

(472 citation statements)

References 25 publications

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“…IFU spectroscopy may also be critical to map the spatial distribution of the SFR (as traced by the narrow component of Hα) and verify if SF is heavily suppressed in the region with the strongest velocity component (as done in, e.g., Cano-Díaz et al 2012). This can provide a direct observational proof of quasar feedback quenching SF at high-z, measured for the first time on radio-quiet, Xray selected obscured QSOs, more representative of the full AGN population than radio-loud and/or very luminous unobscured QSOs.…”

Section: Perspectivesmentioning

confidence: 99%

X-shooter reveals powerful outflows in z ∼ 1.5 X-ray selected obscured quasi-stellar objects

Brusa

Bongiorno

Cresci

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present X-shooter@VLT observations of a sample of 10 luminous, X-ray obscured QSOs at z∼ 1.5 from the XMM-COSMOS survey, expected to be caught in the transitioning phase from starburst to AGN dominated systems. The main selection criterion is X-ray detection at bright fluxes (L X > ∼ 10 44 erg s −1 ) coupled to red optical-to-NIR-to-MIR colors. Thanks to its large wavelength coverage, X-shooter allowed us to determine accurate redshifts from the presence of multiple emission lines for five out of six targets for which we had only a photometric redshift estimate, with a 80% success rate, significantly larger than what is observed in similar programs of spectroscopic follow-up of red QSOs. We report the detection of broad and shifted components in the [OIII]λλ5007,4959 complexes for 6 out of 8 sources with these lines observable in regions free from strong atmospheric absorptions. The FWHM associated with the broad components are in the range FWHM∼ 900 − 1600 km s −1 , larger than the average value observed in SDSS Type 2 AGN samples at similar observed [OIII] luminosity, but comparable to those observed for QSO/ULIRGs systems for which the presence of kpc scale outflows have been revealed through IFU spectroscopy. Although the total outflow energetics (inferred under reasonable assumptions) may be consistent with winds accelerated by stellar processes, we favour an AGN origin for the outflows given the high outflow velocities oberved (v> 1000 km s −1 ) and the presence of strong winds also in objects undetected in the far infrared.

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Section: Perspectivesmentioning

confidence: 99%

X-shooter reveals powerful outflows in z ∼ 1.5 X-ray selected obscured quasi-stellar objects

Brusa

Bongiorno

Cresci

et al. 2014

Monthly Notices of the Royal Astronomical Society

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160

218

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“…A second estimate of the mass outflow rate can be obtained by using the [OIII] λ5007Å emission line (Cano-Díaz et al 2012, see appendix A there), with similar assumptions about the gas properties. In this case:…”

Section: Agn Feedback and Sf Quenchingmentioning

confidence: 99%

Evidence of ongoing AGN-driven feedback in a quiescent post-starburst E+A galaxy

Baron

Netzer

Poznanski

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Post starburst E+A galaxies are thought to have experienced a significant starburst that was quenched abruptly. Their disturbed, bulge-dominated morphologies suggest that they are merger remnants. We present ESI/Keck observations of SDSS J132401.63+454620.6, a post starburst galaxy at redshift z = 0.125, with a starburst that started 400 Myr ago, and other properties, like star formation rate (SFR) consistent with what is measured in ultra luminous infrared galaxies (ULRIGs). The galaxy shows both zero velocity narrow lines, and blueshifted broader Balmer and forbidden emission lines (FWHM=1350 ± 240 km s −1 ). The narrow component is consistent with LINER-like emission, and the broader component with Seyfert-like emission, both photoionized by an active galactic nucleus (AGN) whose properties we measure and model. The velocity dispersion of the broad component exceeds the escape velocity, and we estimate the mass outflow rate to be in the range 4-120 M /yr. This is the first reported case of AGN-driven outflows, traced by ionized gas, in post starburst E+A galaxies. We show, by ways of a simple model, that the observed AGN-driven winds can consistently evolve a ULIRG into the observed galaxy. Our findings reinforce the evolutionary scenario where the more massive ULIRGs are quenched by negative AGN feedback, evolve first to post starburst galaxies, and later become typical red and dead ellipticals.

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“…However, studies of X-ray luminous AGN do not show any evidence for this (e.g. Harrison et al 2012, but see Cano-Díaz et al 2012, Barger et al 2014and Brusa et al 2015.…”

Section: Introductionmentioning

confidence: 99%

Herschel-ATLAS: the connection between star formation and AGN activity in radio-loud and radio-quiet active galaxies

Gürkan¹,

Hardcastle²,

Jarvis³

et al. 2015

Mon. Not. R. Astron. Soc.

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We examine the relationship between star formation and AGN activity by constructing matched samples of local (0 < z < 0.6) radio-loud and radio-quiet AGN in the Herschel-ATLAS fields. Radio-loud AGN are classified as high-excitation and low-excitation radio galaxies (HERGs, LERGs) using their emission lines and WISE 22-µm luminosity. AGN accretion and jet powers in these active galaxies are traced by [OIII] emission-line and radio luminosity, respectively. Star formation rates (SFRs) and specific star formation rates (SSFRs) were derived using Herschel 250-µm luminosity and stellar mass measurements from the SDSS−MPA-JHU catalogue. In the past, star formation studies of AGN have mostly focused on high-redshift sources to observe the thermal dust emission that peaks in the far-infrared, which limited the samples to powerful objects. However, with Herschel we can expand this to low redshifts. Our stacking analyses show that SFRs and SSFRs of both radio-loud and radioquiet AGN increase with increasing AGN power but that radio-loud AGN tend to have lower SFR. Additionally, radio-quiet AGN are found to have approximately an order of magnitude higher SSFRs than radio-loud AGN for a given level of AGN power. The difference between the star formation properties of radio-loud and -quiet AGN is also seen in samples matched in stellar mass.

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Observational evidence of quasar feedback quenching star formation at high redshift

Cited by 342 publications

References 25 publications

X-shooter reveals powerful outflows in z ∼ 1.5 X-ray selected obscured quasi-stellar objects

X-shooter reveals powerful outflows in z ∼ 1.5 X-ray selected obscured quasi-stellar objects

Evidence of ongoing AGN-driven feedback in a quiescent post-starburst E+A galaxy

Herschel-ATLAS: the connection between star formation and AGN activity in radio-loud and radio-quiet active galaxies

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