Imaging of [CLC][ITAL]z[/ITAL][/CLC] ∼ 2 QSO Host Galaxies with the [ITAL]Hubble Space Telescope[/ITAL]

Hutchings, J. B.; Frenette, D.; Hanisch, R. J.; Mo, Jun; Dumont, Philip; Redding, David C.; Neff, Susan G.

doi:10.1086/340472

Cited by 40 publications

(44 citation statements)

References 18 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Although a morphological analysis is beyond the scope of the present study, we note that the morphological mix in the low-L X and high-L X AGNs subsamples may in general be different (e.g. Hutchings et al 2002Hutchings et al , 2009Veilleux et al 2009a;Mainieri et al 2011;Kocevski et al 2012). The same can in principle be true also for the mass-matched control galaxies, even though the mass distribution of low-L X and high-L X AGN host galaxies are very similar, with the latter having an average stellar mass ∼0.14 ± 0.03 dex higher than their lower luminosity counterparts (the comparison has been done in the COSMOS field, where we have the better statistics).…”

Section: Two Modes Of Agn Evolution?mentioning

confidence: 99%

Enhanced star formation rates in AGN hosts with respect to inactive galaxies from PEP-Herschelobservations

Santini

Rosario

Shao

et al. 2012

A&A

211

180

View full text Add to dashboard Cite

We compare the average star formation (SF) activity in X-ray selected AGN hosts with a mass-matched control sample of inactive galaxies, including both star forming and quiescent sources, in the 0.5 < z < 2.5 redshift range. Recent observations carried out by PACS, the 60−210 μm photometric camera on board the Herschel Space Observatory, in GOODS-S, GOODS-N and COSMOS allow us to obtain an unbiased estimate of the far-IR luminosity, and hence of the SF properties, of the two samples. Accurate AGN host stellar mass estimates are obtained by decomposing their total emission into the stellar and the nuclear components. We report evidence of a higher average SF activity in AGN hosts with respect to the control sample of inactive galaxies. The level of SF enhancement is modest (∼0.26 dex at ∼3σ confidence level) at low X-ray luminosities (L X 10 43.5 erg s −1 ) and more pronounced (0.56 dex at >10σ confidence level) in the hosts of luminous AGNs. However, when comparing to star forming galaxies only, AGN hosts are found broadly consistent with the locus of their "main sequence". We investigate the relative far-IR luminosity distributions of active and inactive galaxies, and find a higher fraction of PACS detected, hence normal and highly star forming systems among AGN hosts. Although different interpretations are possible, we explain our findings as a consequence of a twofold AGN growth path: faint AGNs evolve through secular processes, with instantaneous AGN accretion not tightly linked to the current total SF in the host galaxy, while the luminous AGNs co-evolve with their hosts through periods of enhanced AGN activity and star formation, possibly through major mergers. While an increased SF activity with respect to inactive galaxies of similar mass is expected in the latter, we interpret the modest SF offsets measured in low-L X AGN hosts as either a) generated by non-synchronous accretion and SF histories in a merger scenario or b) due to possible connections between instantaneous SF and accretion that can be induced by smaller scale (non-major merger) mechanisms. Far-IR luminosity distributions favour the latter scenario.

show abstract

Section: Two Modes Of Agn Evolution?mentioning

confidence: 99%

Enhanced star formation rates in AGN hosts with respect to inactive galaxies from PEP-Herschelobservations

Santini

Rosario

Shao

et al. 2012

A&A

211

180

View full text Add to dashboard Cite

show abstract

“…Even if the host galaxies at high redshifts are more disturbed, the above law can still be considered appropriate as a description of the main part of the flux (e.g. Hutchings et al 2002), since low surface brightness disk components or tidal features are likely to be missed anyway. Even in the case of a true disk-type host we probably could not distinguish it from an elliptical of similar size and brightness.…”

Section: Individual Imagesmentioning

confidence: 99%

High-redshift quasar host galaxies with adaptive optics

Kuhlbrodt

Örndahl

Wisotzki

et al. 2005

A&A

View full text Add to dashboard Cite

Abstract. We present K band adaptive optics observations of three high-redshift (z ∼ 2.2) high-luminosity quasars, all of which were studied for the first time. We also observed several point spread function (PSF) calibrators, non-simultaneously because of the small field of view. The significant temporal PSF variations on timescales of minutes inhibited a straightforward scaled PSF removal from the quasar images. Characterising the degree of PSF concentration by the radii encircling 20% and 80% of the total flux, respectively, we found that even under very different observing conditions the r 20 vs. r 80 relation varied coherently between individual short exposure images, delineating a well-defined relation for point sources. Placing the quasar images on this relation, we see indications that all three objects were resolved. We designed a procedure to estimate the significance of this result, and to estimate host galaxy parameters, by reproducing the statistical distribution of the individual short exposure images. We find in all three cases evidence for a luminous host galaxy, with a mean absolute magnitude of M R = −27.0 and scale lengths around ∼4-12 kpc. Together with a rough estimate of the central black hole masses obtained from C line widths, the location of the objects on the bulge luminosity vs. black hole mass relation is not significantly different from the low-redshift regime, assuming only passive evolution of the host galaxy. Corresponding Eddington luminosities are L nuc /L Edd ∼ 0.1-0.6.

show abstract

“…Quasars outshine their host galaxies by an order of magnitude or more, making it observationally challenging to detect and study their faint underlying galaxies (Lehnert et al 1999;Hutchings et al 2002;Jahnke et al 2004;Falomo et al 2005;Floyd et al 2013;Glikman et al 2015). The sizes of distant (z>1; look-back time of 9.25 Gyr) galaxies are small (∼1″), roughly the same angular size as ground-based "seeing" and space-based instrument resolution and contrast sensitivity.…”

Section: Introductionmentioning

confidence: 99%

Galactic-scale Feedback Observed in the 3C 298 Quasar Host Galaxy

Vayner

Wright

Murray

et al. 2017

ApJ

View full text Add to dashboard Cite

We present high angular resolution multiwavelength data of the 3C 298 radio-loud quasar host galaxy (z = 1.439) taken using the W.M. Keck Observatory OSIRIS integral field spectrograph (IFS) with adaptive optics, the Atacama Large Millimeter/submillimeter Array (ALMA), the Hubble Space Telescope (HST) WFC3, and the Very Large Array (VLA). Extended emission is detected in the rest-frame optical nebular emission lines Hβ, [O III], Hα, [N II], and [S II], as well as in the molecular lines CO (J = 3−2) and (J = 5−4). Along the path of the relativistic jets of 3C 298, we detect conical outflows in ionized gas emission with velocities of up to 1700 km s 1 -and an outflow rate of 450-1500 M yr 1 - extended over 12 kpc. Near the spatial center of the conical outflow, CO (J = 3−2) emission shows a molecular gas disk with a rotational velocity of±150 km s 1 -and total molecular mass (M H 2 ) of M 6.6 0.36 10 9 ´. On the blueshifted side of the molecular disk, we observe broad extended emission that is due to a molecular outflow with a rate of 2300 M yr 1 - and depletion timescale of 3 Myr. We detect no narrow Hαemission in the outflow regions, suggesting a limit on star formation of 0.3 M yr kpc. Quasardriven winds are evacuating the molecular gas reservoir, thereby directly impacting star formation in the host galaxy. The observed mass of the supermassive black hole is M 10 9.37 9.56  -,and we determine a dynamical bulge mass of M M 1 1.7 10 R bulge 10 1.6 kpc =´ -. The bulge mass of 3C 298 lies 2-2.5 orders of magnitude below the expected value from the local galactic bulge-supermassive black hole mass (M M bulge BH -) relationship. A second galactic disk observed in nebular emission is offset from the quasar by 9 kpc, suggesting that the system is an intermediate-stage merger. These results show that galactic-scale negative feedback is occurring early in the merger phase of 3C 298, well before the coalescence of the galactic nuclei and assembly on the local M M bulge BH -relationship.

show abstract

Imaging of [CLC][ITAL]z[/ITAL][/CLC] ∼ 2 QSO Host Galaxies with the [ITAL]Hubble Space Telescope[/ITAL]

Cited by 40 publications

References 18 publications

Enhanced star formation rates in AGN hosts with respect to inactive galaxies from PEP-Herschelobservations

Enhanced star formation rates in AGN hosts with respect to inactive galaxies from PEP-Herschelobservations

High-redshift quasar host galaxies with adaptive optics

Galactic-scale Feedback Observed in the 3C 298 Quasar Host Galaxy

Contact Info

Product

Resources

About