Defying jet-gas alignment in two radio galaxies at<i>z</i>~ 2 with extended light profiles: Similarities to brightest cluster galaxies

Collet, C.; Nesvadba, N. P. H.; Breuck, C. De; Lehnert, M. D.; Best, P. N.; Bryant, Julia J.; Dicken, D.; Johnston, Helen M.; Hunstead, R. W.; Wylezalek, Dominika

doi:10.1051/0004-6361/201424544

Cited by 15 publications

(31 citation statements)

References 128 publications

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“…estimate that beam-smearing may lower the measured velocity gradients by about a factor of 2, comparable to inclination (Collet 2014). Overall, the line widths in our galaxies are relatively broad, FWHM = 400−1000 km s −1 , down to the spatial resolution limit of our data.…”

Section: Kinematicssupporting

confidence: 48%

“…The extended emission-line regions in all but one source (discussed further in Collet et al 2015) are aligned with the radio jet axis within 20 • −30 • as would be expected if the jet were inflating an overpressurized bubble of hot gas. Moreover, hydrodynamic models of jet-driven winds do predict that jets with kinetic power of 10 46−47 erg s −1 should accelerate gas to about 500 km s −1 , which is consistent with our findings, in particular if we take seeing (Sect.…”

Section: Outflows or Disk Rotation?mentioning

confidence: 62%

“…This may indicate that the gas is at least partially lit up by photons originating from the AGN in the radio galaxy. The proximity to the radio galaxy may also suggest that this gas is already dominated by the gravitational potential of the radio galaxy itself, either as part of a satellite galaxy that is being accreted (e.g., Ivison et al 2008;Nesvadba et al 2007), or perhaps because it is associated with an extended stellar halo forming around the HzRG, as observed in other cases (Hatch et al 2009; see also Collet et al 2015).…”

Section: Additional Line Emitters and Dynamical Mass Estimates Of Ourmentioning

confidence: 97%

“…The fourth source, NVSS J210626−314003 shows a strong misalignment between the radio source and the extended gas, and no gas along the radio jet axis, which is very different from the other galaxies presented here. This source has already been discussed by Collet et al (2015), so we do not describe its characteristics in detail again, but we do include it in the overall discussion of the properties of our sources. For the CENSORS sources we focus our discussion on the three sources where we detected line emission at the redshifts previously measured in the rest-frame UV.…”

Section: Near-infrared Imaging Spectroscopymentioning

confidence: 99%

“…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%

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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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Section: Kinematicssupporting

confidence: 48%

Section: Outflows or Disk Rotation?mentioning

confidence: 62%

Section: Additional Line Emitters and Dynamical Mass Estimates Of Ourmentioning

confidence: 97%

Section: Near-infrared Imaging Spectroscopymentioning

confidence: 99%

Section: Additional Line Emitters and Dynamical Mass Estimates Of Ourmentioning

confidence: 99%

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

Collet

Nesvadba

Breuck

et al. 2016

A&A

Self Cite

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Identifying protoclusters in distant universe

Costa

Menéndez‐Delmestre

2021

Astron Nachr

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Properties of galaxies, such as color, age, and star formation activity, appear to be associated with the environment in which they are immersed. To investigate how the environment-galaxy relation is established, we study protoclusters, which are numerically dense environments of galaxies in the early Universe, and which give rise to galaxy clusters today. In this work, we use submillimeter galaxies (SMGs)-which are very dusty and distant galaxies, with their copious infrared emission redshifted to the submillimeter wavelengths-as lampposts to trace potential sites of protocluster regions. We undertook deep observations of the environment of SMGs with well-established spectroscopic redshifts in the range of z ≃ 1-5. We made a combination of deep imaging and spectroscopic observations to identify Lyman-alpha emitters (LAEs) as a means to assess the more typical star-forming galaxies in these regions. We identified more than 300 LAE candidates in four potential protocluster regions. Of these, 200 have already been spectroscopically confirmed to be at the SMG redshifts. This is consistent with them being part of the same structure. By probing the redshift range z ≃ 1-5, which corresponds to ≥4 Giga years, we seek insights on the evolution of protoclusters over this time interval.

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The realm of the galaxy protoclusters

Overzier

2016

Astron Astrophys Rev

264

204

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The study of galaxy protoclusters is beginning to fill in unknown details of the important phase of the assembly of clusters and cluster galaxies. This review describes the current status of this field and highlights promising recent findings related to galaxy formation in the densest regions of the early universe. We discuss the main search techniques and the characteristic properties of protoclusters in observations and simulations, and show that protoclusters will have present-day masses similar to galaxy clusters when fully collapsed. We discuss the physical properties of galaxies in protoclusters, including (proto-)brightest cluster galaxies, and the forming red sequence. We highlight the fact that the most massive halos at high redshift are found in protoclusters, making these objects uniquely suited for testing important recent models of galaxy formation. We show that galaxies in protoclusters should be among the first galaxies at high redshift making the transition from a gas cooling regime dominated by cold streams to a regime dominated by hot intracluster gas, which could be tested observationally. We also discuss the possible connections between protoclusters and radio galaxies, quasars, and Ly-alpha blobs. Because of their early formation, large spatial sizes and high total star formation rates, protoclusters have also likely played a crucial role during the epoch of reionization, which can be tested with future experiments that will map the neutral and ionized cosmic web. Last, we review a number of promising observational projects that are expected to make significant impact in this growing, exciting field.Comment: Invited article for The Astronomy and Astrophysics Review (in press

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Defying jet-gas alignment in two radio galaxies atz~ 2 with extended light profiles: Similarities to brightest cluster galaxies

Cited by 15 publications

References 128 publications

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

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

Identifying protoclusters in distant universe

The realm of the galaxy protoclusters

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