GALAXY CLUSTERS AROUND RADIO-LOUD ACTIVE GALACTIC NUCLEI AT 1.3 &lt;<i>z</i>&lt; 3.2 AS SEEN BY<i>SPITZER</i>

Wylezalek, Dominika; Galametz, A.; Stern, Daniel; Vernet, J.; Breuck, C. De; Seymour, N.; Brodwin, M.; Eisenhardt, Peter; Gonzalez, Anthony H.; Hatch, N. A.; Jarvis, Matt J.; Rettura, Alessandro; Stanford, S. A.; Stevens, J. A.

doi:10.1088/0004-637x/769/1/79

Cited by 208 publications

(360 citation statements)

References 73 publications

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“…Current literature will often forego the first requirement, particularly for distant clusters, due to the challenges of acquiring such data-and this is particularly problematic for our RLAGN targets due to Inverse Compton scattering of the cosmic microwave background by the hot plasma associated with AGN radio lobes into the X-ray regime. Nonetheless, we show that some CARLA systems have clear overdensities of passive galaxy candidates (see also Cooke et al 2015;Cooke et al 2016, in preparation), and Wylezalek et al (2013) show that the CARLA cluster member candidates are, on average, centrally concentrated around the target RLAGN.…”

Section: Introductionsupporting

confidence: 66%

“…In particular, as discussed in Section 1, other hallmarks of a bona fide cluster include a significant population of evolved massive galaxies and a centrally concentrated distribution of galaxies. We show in Section 5.2.1 that CARLA J2039−2514 contains an overdensity of (spectroscopically unconfirmed) red galaxies with properties consistent with being passive galaxies at the redshift of the structure, and prior work by our team has demonstrated that the color-selected (i.e., red) candidate cluster members are centrally concentrated around the target RLAGN (Wylezalek et al 2013). The overdensities reach s 9.0 and s 7.8 above the field value for the fields around MRC 2036−254 and B30756+406, respectively.…”

Section: Cluster Membershipmentioning

confidence: 68%

“…The galaxy density of these cluster candidates strongly peaks toward the position of the targeted RLAGN, suggesting thatthe clusters are reliable and that the RLAGN reside at the cluster cores. Detailed descriptions of the sample and initial scientific results are presented in Wylezalek et al (2013Wylezalek et al ( , 2014.…”

Section: The Carla Samplementioning

confidence: 99%

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HST GRISM CONFIRMATION OF TWO z ∼ 2 STRUCTURES FROM THE CLUSTERS AROUND RADIO-LOUD AGN (CARLA) SURVEY

Noirot

Vernet

Breuck

et al. 2016

ApJ

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Using Hubble Space Telescope slitless grism data, we report the spectroscopic confirmation of two distant structures atz 2 associated with powerful high-redshift radio-loud active galactic nuclei(AGNs). These rich structures, likely (forming) clusters, are among the most distant structures currently known, and were identified on the basis of Spitzer/IRAC [3.6]-[4.5] color. We spectroscopically confirm nine members in the field of MRC2036 −254, comprising eight star-forming galaxies and the targeted radio galaxy. The median redshift is z=2.000. We spectroscopically confirm 10 members in the field of B30756+406, comprising 8 star-forming galaxies and 2 AGNs, including the targeted radio-loud quasar. The median redshift is z=1.986. All confirmed members are within 500 kpc (1 arcmin) of the targeted AGNs. We derive median (mean) star-formation rates of based on mid-infrared fluxes and spectral energy distribution modeling. Most of our confirmed members are located above the star-forming mainsequence toward starburst galaxies, consistent with clusters at these early epochs being the sites of significant levels of star formation. The structure around MRC2036−254 shows an overdensity of IRAC-selected candidate galaxy cluster members consistent with being quiescent galaxies, while the structure around B30756+406 shows field values, albeit with many lower limits to colors that could allow an overdensity of faint red quiescent galaxies. The structure around MRC2036−254 shows a red sequence of passive galaxy candidates.

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Section: Introductionsupporting

confidence: 66%

Section: Cluster Membershipmentioning

confidence: 68%

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HST GRISM CONFIRMATION OF TWO z ∼ 2 STRUCTURES FROM THE CLUSTERS AROUND RADIO-LOUD AGN (CARLA) SURVEY

Noirot

Vernet

Breuck

et al. 2016

ApJ

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“…Additionally, their radio-loud sample shows a larger clustering amplitude than their radio-quiet sources. Previous observations at low and intermediate redshift of the environments of radio galaxies and radio-loud AGNs suggest that these reside in denser regions compared with control fields (e.g., Miley et al 2006;Wylezalek et al 2013). At z 1.5, Mpc-sized dense regions have not yet virialized within a single cluster-sized DMH and are consider to be the progenitors of present day galaxy clusters (Kurk et al 2004;Miley & De Breuck 2008).…”

Section: Introductionmentioning

confidence: 93%

Probing the radio loud/quiet AGN dichotomy with quasar clustering

Retana-Montenegro

Röttgering

2017

A&A

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We investigate the clustering properties of 45441 radio-quiet quasars (RQQs) and 3493 radio-loud quasars (RLQs) drawn from a joint use of the Sloan Digital Sky Survey (SDSS) and Faint Images of the Radio Sky at 20 cm (FIRST) surveys in the range 0.3 < z < 2.3. This large spectroscopic quasar sample allow us to investigate the clustering signal dependence on radio-loudness and black hole (BH) virial mass. We find that RLQs are clustered more strongly than RQQs in all the redshift bins considered. We find a real-space correlation length of r 0 = 6.59 +0.33 −0.24 h −1 Mpc and r 0 = 10.95 +1.22 −1.58 h −1 Mpc for RQQs and RLQs, respectively, for the full redshift range. This implies that RLQs are found in more massive host haloes than RQQs in our samples, with mean host halo masses of ∼ 4.9 × 10 13 h −1 M and ∼ 1.9 × 10 12 h −1 M , respectively. Comparison with clustering studies of different radio source samples indicates that this mass scale of 1 × 10 13 h −1 M is characteristic for the bright radio-population, which corresponds to the typical mass of galaxy groups and galaxy clusters. The similarity we find in correlation lengths and host halo masses for RLQs, radio galaxies and flat-spectrum radio quasars agrees with orientation-driven unification models. Additionally, the clustering signal shows a dependence on black hole (BH) mass, with the quasars powered by the most massive BHs clustering more strongly than quasars having less massive BHs. We suggest that the current virial BH mass estimates may be a valid BH proxies for studying quasar clustering. We compare our results to a previous theoretical model that assumes that quasar activity is driven by cold accretion via mergers of gas-rich galaxies. While the model can explain the bias and halo masses for RQQs, it cannot reproduce the higher bias and host halo masses for RLQs. We argue that other BH properties such as BH spin, environment, magnetic field configuration, and accretion physics must be considered to fully understand the origin of radio-emission in quasars and its relation to the higher clustering.

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“…A large number of imaging and spectroscopic studies have demonstrated conclusively that many massive radio galaxies at z ≥ 2 are surrounded by galaxy overdensities at the same redshift, as well as significant reservoirs of molecular, atomic, and ionized gas, including diffuse intra-halo gas (Le Fèvre et al 1996;Venemans et al 2007;Hayashi et al 2012;Galametz et al 2012;van Ojik et al 1997;Villar-Martín et al 2003;De Breuck et al 2003;Nesvadba et al 2009;Wylezalek et al 2013;Collet et al 2015). With the small field of view of only 8 × 8 , SINFONI can only constrain the very nearby environment of HzRGs out to a few tens of kpc (8 correspond to 64 kpc at z ∼ 2); however, this small-scale environment is particularly interesting, e.g., to study how accretion and merging may affect the evolutionary state of the radio galaxy.…”

Section: Additional Line Emitters and Dynamical Mass Estimates Of Ourmentioning

confidence: 99%

Kinematic signatures of AGN feedback in moderately powerful radio galaxies atz~ 2 observed with SINFONI

Collet

Nesvadba

Breuck

et al. 2016

A&A

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Most successful galaxy formation scenarios now postulate that the intense star formation in massive, high-redshift galaxies during their major growth period was truncated when powerful AGNs launched galaxy-wide outflows of gas that removed large parts of the interstellar medium. SINFONI imaging spectroscopy of the most powerful radio galaxies at z ∼ 2 show clear signatures of such winds, but are too rare to be good representatives of a generic phase in the evolution of all massive galaxies at high redshift. Here we present SINFONI imaging spectroscopy of the rest-frame optical emission-line gas in 12 radio galaxies at redshifts ∼2. Our sample spans a range in radio power that is intermediate between the most powerful radio galaxies with known wind signatures at these redshifts and vigorous starburst galaxies, and are about two orders of magnitude more common than the most powerful radio galaxies. Thus, if AGN feedback is a generic phase of massive galaxy evolution for reasonable values of the AGN duty cycle, these are just the sources where AGN feedback should be most important. Our sources show a diverse set of gas kinematics ranging from regular velocity gradients with amplitudes of Δv = 200−400 km s −1 consistent with rotating disks to very irregular kinematics with multiple velocity jumps of a few 100 km s −1 . Line widths are generally high, typically around FWHM = 800 km s −1 , more similar to the more powerful high-z radio galaxies than mass-selected samples of massive high-z galaxies without bright AGNs, and consistent with the velocity range expected from recent hydrodynamic models. A broad Hα line in one target implies a black hole mass of a few 10 9 M . Velocity offsets of putative satellite galaxies near a few targets suggest dynamical masses of a few 10 11 M for our sources, akin to the most powerful high-z radio galaxies. Ionized gas masses are 1−2 orders of magnitude lower than in the most powerful radio galaxies, and the extinction in the gas is relatively low, up to A V ∼ 2 mag. The ratio of line widths, σ, to bulk velocity, v, is so large that even the gas in galaxies with regular velocity fields is unlikely to be gravitationally bound. It is unclear, however, whether the large line widths are due to turbulence or unresolved, local outflows as are sometimes observed at low redshifts. We compare our sources with sets of radio galaxies at low and high redshift, finding that they may have more in common with gas-rich nearby radio galaxies with similar jet power than with the most powerful high-z radio galaxies. Comparison of the kinetic energy with the energy supply from the AGNs through jet and radiation pressure suggests that the radio source still plays a dominant role for feedback, consistent with low-redshift radio-loud quasars.

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GALAXY CLUSTERS AROUND RADIO-LOUD ACTIVE GALACTIC NUCLEI AT 1.3 <z< 3.2 AS SEEN BYSPITZER

Cited by 208 publications

References 73 publications

HST GRISM CONFIRMATION OF TWO z ∼ 2 STRUCTURES FROM THE CLUSTERS AROUND RADIO-LOUD AGN (CARLA) SURVEY

HST GRISM CONFIRMATION OF TWO z ∼ 2 STRUCTURES FROM THE CLUSTERS AROUND RADIO-LOUD AGN (CARLA) SURVEY

Probing the radio loud/quiet AGN dichotomy with quasar clustering

Kinematic signatures of AGN feedback in moderately powerful radio galaxies atz~ 2 observed with SINFONI

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