Mapping the ionised gas around the luminous QSO HE 1029-1401: evidence for minor merger events?

Sánchez, S. F.; Wisotzki, L.; Jahnke, K.; Kupko, D.; Nugroho, D.; Schramm, Malte

doi:10.1051/0004-6361/201014559

Cited by 24 publications

(28 citation statements)

References 105 publications

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“…Based on the velocity structure and mass of EELR gas around SSRQs, as well as the correlation between EELRs and radio emission, Fu & Stockton (2009) suggested that EELRs are formed in galaxy minor mergers accompanied by the production of radio jets associated with AGNs. A similar conclusion was reached by Husemann et al (2010) for an RQQ. Villar-Martín et al (2011) found that the majority of the type-2, radio-quiet EELR quasars show the signs of galaxy merger or interaction, while none of the non-EELR counterparts show such signs.…”

Section: Link To Host Galaxiessupporting

confidence: 79%

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Co-Evolution of Galaxies and Central Black Holes: Observational Evidence on the Trigger of Agn Feedback

Matsuoka

2012

ApJ

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A comprehensive analysis of the extended emission-line region (EELR) around quasars is presented. A new Subaru/Suprime-Cam observation is combined with a literature search, resulting in a compilation of 81 EELR measurements for type-1 and type-2 quasars with an associated active galactic nucleus (AGN) and host galaxy properties. It is found that the EELR phenomenon shows clear correlation with the Eddington ratio, which links EELR to the constituents of principal component 1, or eigenvector 1, of the AGN emission correlations. We also find that EELR is preferentially associated with gas-rich, massive blue galaxies. This supports the idea that the primary determinant of EELR creation is gas availability and that the gas may be brought in by galaxy merger, triggering the current star formation as well as AGN activity, and also gives an explanation for the fact that most luminous EELRs are found around radio-loud sources with low Eddington ratio. By combining all the observations, it is suggested that EELR quasars occupy the massive blue corner of the green valley, the AGN realm, on the galaxy color-stellar mass diagram. Once a galaxy is pushed to this corner, an activated AGN would create an EELR by energy injection into the interstellar gas and eventually blow it away, leading to star formation quenching. The results presented here provide a piece of evidence for the presence of such an AGN feedback process, which may play a leading role in the co-evolution of galaxies and central super-massive black holes.

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Section: Link To Host Galaxiessupporting

confidence: 79%

“…We compile the EELR measurements of type-1 quasars from Boroson et al (1985), Stockton & MacKenty (1987), and Husemann et al (2008Husemann et al ( , 2010. The continuum and line luminosities given in Stockton & MacKenty (1987) are converted to the values in the cosmology adopted here.…”

Section: Data Compilationmentioning

confidence: 99%

Co-Evolution of Galaxies and Central Black Holes: Observational Evidence on the Trigger of Agn Feedback

Matsuoka

2012

ApJ

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“…A direct decomposition the stellar continuum of the host galaxy underneath very luminous QSOs with deep optical IFU observations was previously attempted with VIMOS for HE 1029−1401 (Husemann et al 2010). Although HE 1029−1401 is much closer with a redshift of z = 0.086 but has a similar luminosity as PG 1307+085, the achieved S/N in the host spectrum was significantly lower than what we obtained with MUSE for PG 1307+085.…”

Section: The Bh Massσ * Relationcontrasting

confidence: 52%

The MUSE view of QSO PG 1307+085: an elliptical galaxy on theM_BH–σ_*relation interacting with its group environment

Husemann

Bennert

Scharwächter

et al. 2015

Mon. Not. R. Astron. Soc.

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We report deep optical integral-field spectroscopy with the Multi-Unit Spectroscopic Explorer (MUSE) at the Very Large Telescope of the luminous radio-quiet quasi-stellar object (QSO) PG 1307+085 (z = 0.154) obtained during the commissioning of the instrument. Given the high sensitivity and spatial resolution delivered by MUSE, we are able to resolve the compact (r e ∼ 1.3 arcsec) elliptical host galaxy. After careful spectroscopic deblending of the QSO and host galaxy emission, we infer a stellar velocity dispersion of σ * = 155±19 km s −1 . This places PG 1307+085 local M BH − σ * relation within the intrinsic scatter but offset towards a higher black hole mass with respect to the mean relation. The observations with MUSE also reveal a large extended narrow-line region (ENLR) around PG 1307+085 reaching out to ∼30 kpc. In addition, we detect a faint bridge of ionized gas towards the most massive galaxy of the galaxy group being just ∼20 arcsec (50 kpc) away. Previous long-slit spectroscopic observations missed most of these extended features due to a miss-aligned slit. The ionized gas kinematics does not show any evidence for gas outflows on kpc scales despite the high QSO luminosity of L bol > 10 46 erg s −1 . Based on the ionized gas distribution, kinematics and metallicity we discuss the origin of the ENLR with respect to its group environments including minor mergers, ram-pressure stripping or filamentary gas accretion as the most likely scenarios. We conclude that PG 1307+085 is a normal elliptical host in terms of the scaling relations, but that the gas is most likely affected by the environment through gravity or ambient pressure. It is possible that the ongoing interaction with the environment, mainly seen in the ionized gas, is also be responsible for driving sufficient gas to feed the black hole at the centre of the galaxy.

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“…Large reservoirs of ionized gas on tens to hundreds kpcs scales have been detected around many luminous radio-loud and radio-quiet AGN at low redshifts (Stockton & MacKenty 1983;Danziger et al 1984;van Breugel et al 1985;Stockton & MacKenty 1987;Prieto et al 1993;Shopbell et al 1999;Tadhunter et al 2000;Stockton et al 2002;Villar-Martín et al 2005Husemann et al 2010Husemann et al , 2011Greene et al 2012;Liu et al 2013aLiu et al , 2014Hainline et al 2014;Villar-Martín et al 2017 as well as at high redshifts (e.g. Heckman et al 1991;McCarthy 1993;Christensen et al 2006;North et al 2012;Cantalupo et al 2014;Hennawi et al 2015;Borisova et al 2016;Cai et al 2017;Arrigoni Battaia et al 2018;Husemann et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Jet-driven Galaxy-scale Gas Outflows in the Hyperluminous Quasar 3C 273

Bennert

Jahnke

Davis

et al. 2019

ApJ

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We present an unprecedented view on the morphology and kinematics of the extended narrow-line region (ENLR) and molecular gas around the prototypical hyper-luminous quasar 3C 273 (L bol ∼ 10 47 erg s −1 at z = 0.158) based on VLT-MUSE optical 3D spectroscopy and ALMA observations. We find that: 1) The ENLR size of 12.1 ± 0.2kpc implies a smooth continuation of the size-luminosity relation out to large radii or a much larger break radius as previously proposed. 2) The kinematically disturbed ionized gas with line splits reaching 1000 km s −1 out to 6.1 ± 1.5kpc is aligned along the jet axis. 3) The extreme line broadening on kpc scales is caused by spatial and spectral blending of many distinct gas clouds separated on sub-arcsecond scales with different line-of-sight velocities. The ENLR velocity field combined with the known jet orientation rule out a simple scenario of a radiativelydriven radial expansion of the outflow. Instead we propose that a pressurized expanding hot gas cocoon created by the radio jet is impacting on an inclined gas disk leading to transverse and/or backflow motion with respect to our line-of-sight. The molecular gas morphology may either be explained by a density wave at the front of the outflow expanding along the jet direction as predicted by positive feedback scenario or the cold gas may be trapped in a stellar over-density caused by a recent merger event. Using 3C 273 as a template for observations of high-redshift hyper-luminous AGN reveals that large-scale ENLRs and kpc scale outflows may often be missed due to the brightness of the nuclei and the limited sensitivity of current near-IR instrumentation. nous quasars at low redshift with an absolute brightness of M V = −26.8 mag (e.g. Hamilton et al. 2008) and a radio flux of f 1.4GHz ∼ 45 Jy (Kellermann et al. 1969) corresponding to L 1.4GHz = 2.9 × 10 27 W Hz −1 . 3C 273 is therefore a proto-typical active galactic nucleus (AGN) since only accretion by a super-massive black hole (SMBH) can produce the observed energy (Salpeter 1964).The enormous energy released by luminous AGN like 3C 273 is suspected to significantly affect the evolution

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Mapping the ionised gas around the luminous QSO HE 1029-1401: evidence for minor merger events?

Cited by 24 publications

References 105 publications

Co-Evolution of Galaxies and Central Black Holes: Observational Evidence on the Trigger of Agn Feedback

Co-Evolution of Galaxies and Central Black Holes: Observational Evidence on the Trigger of Agn Feedback

The MUSE view of QSO PG 1307+085: an elliptical galaxy on theM_BH–σ_*relation interacting with its group environment

Jet-driven Galaxy-scale Gas Outflows in the Hyperluminous Quasar 3C 273

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Mapping the ionised gas around the luminous QSO HE 1029-1401: evidence for minor merger events?

Cited by 24 publications

References 105 publications

Co-Evolution of Galaxies and Central Black Holes: Observational Evidence on the Trigger of Agn Feedback

Co-Evolution of Galaxies and Central Black Holes: Observational Evidence on the Trigger of Agn Feedback

The MUSE view of QSO PG 1307+085: an elliptical galaxy on theMBH–σ*relation interacting with its group environment

Jet-driven Galaxy-scale Gas Outflows in the Hyperluminous Quasar 3C 273

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The MUSE view of QSO PG 1307+085: an elliptical galaxy on theM_BH–σ_*relation interacting with its group environment