The rare, galaxy cluster environment of the short GRB161104A and a comparison to the short GRB host population

2020 ◽  
Author(s):  
Anya Elizabeth Nugent
Keyword(s):  
Galaxy Cluster ◽  
Host Population ◽  
Cluster Environment

scholarly journals The Distant, Galaxy Cluster Environment of the Short GRB 161104A at z ∼ 0.8 and a Comparison to the Short GRB Host Population

2020 ◽  
Vol 904 (1) ◽  
pp. 52
Author(s):  
A. E. Nugent ◽  
W. Fong ◽  
Y. Dong ◽  
A. Palmese ◽  
J. Leja ◽  
...  
Keyword(s):  
Galaxy Cluster ◽  
Host Population ◽  
Distant Galaxy ◽  
Cluster Environment

scholarly journals Quasar Activity in Rich Galaxy Clusters

1992 ◽  
Vol 9 ◽  
pp. 695-696
Author(s):  
H. K. C. Yee ◽  
E. Ellingson
Keyword(s):  
Spatial Distribution ◽  
Galaxy Clusters ◽  
Galaxy Cluster ◽  
Clusters Of Galaxies ◽  
Spatial Covariance ◽  
Class 1 ◽  
The Galaxy ◽  
Cluster Environment

We have carried out a number of imaging surveys of fields around quasars to study their global environments (e.g. Yee and Green 1987, Ellingson, Yee and Green 1991). The richness of the galaxy cluster environment of each quasar was determined using the galaxy-quasar spatial covariance amplitude, a quantity which is normalized for the expected luminosity and spatial distribution of galaxies (Longair and Seldner 1978, Yee and Green 1987). We find that ~40% of the brightest radio-loud quasars inhabit rich clusters of galaxies (Abell class 1 or higher) at z≳0.5 whereas only fainter AGN inhabit clusters at more recent epochs (Figure 1). This can be understood if quasars in rich clusters evolve much faster than those in poor environments.

scholarly journals AGN jet feedback on a moving mesh: lobe energetics and X-ray properties in a realistic cluster environment

2019 ◽  
Vol 490 (1) ◽  
pp. 343-349 ◽  
Author(s):  
Martin A Bourne ◽  
Debora Sijacki ◽  
Ewald Puchwein
Keyword(s):  
Active Galactic Nuclei ◽  
Galaxy Cluster ◽  
Galactic Nuclei ◽  
Moving Mesh ◽  
X Ray ◽  
Cluster Galaxies ◽  
Hot Gas ◽  
Brightest Cluster Galaxies ◽  
Cluster Environment ◽  
Very High

ABSTRACT Jet feedback from active galactic nuclei (AGN) harboured by brightest cluster galaxies is expected to play a fundamental role in regulating cooling in the intracluster medium (ICM). While observations and theory suggest energy within jet lobes balances ICM radiative losses, the modus operandi of energy communication with the ICM remains unclear. We present simulations of very high resolution AGN-driven jets launching in a live, cosmological galaxy cluster, within the moving mesh code arepo. As the jet propagates through the ICM the majority of its energy, which is initially in the kinetic form, thermalizes quickly through internal shocks and inflates lobes of very hot gas. The jets effectively heat the cluster core, with PdV work and weather-aided mixing being the main channels of energy transfer from the lobes to the ICM, while strong shocks and turbulence are subdominant. We additionally present detailed mock X-ray maps at different stages of evolution, revealing clear cavities surrounded by X-ray bright rims, with lobes being detectable for up to ∼108 yr even when magnetic draping is ineffective. We find bulk motions in the cluster can significantly affect lobe propagation, offsetting them from the jet direction and imparting bulk velocities that can dominate over the buoyantly rising motion.

scholarly journals Molecular gas in two companion cluster galaxies at z = 1.2

2018 ◽  
Vol 617 ◽  
pp. A103 ◽  
Author(s):  
G. Castignani ◽  
F. Combes ◽  
P. Salomé ◽  
S. Andreon ◽  
M. Pannella ◽  
...  
Keyword(s):  
Star Formation ◽  
Line Emission ◽  
Galaxy Cluster ◽  
Star Formation History ◽  
Molecular Gas ◽  
Density Peak ◽  
Distant Cluster ◽  
Cluster Galaxies ◽  
Star Forming ◽  
Cluster Environment

Context. Probing both star formation history and evolution of distant cluster galaxies is essential to evaluate the effect of dense environment on shaping the galaxy properties we observe today. Aims. We investigate the effect of cluster environment on the processing of the molecular gas in distant cluster galaxies. We study the molecular gas properties of two star-forming galaxies separated by 6 kpc in the projected space and belonging to a galaxy cluster selected from the Irac Shallow Cluster Survey, at a redshift z = 1.2, that is, ~ 2 Gyr after the cosmic star formation density peak. This work describes the first CO detection from 1 < z < 1.4 star-forming cluster galaxies with no clear reported evidence of active galactic nuclei. Methods. We exploit observations taken with the NOEMA interferometer at ~3 mm to detect CO(2−1) line emission from the two selected galaxies, unresolved by our observations. Results. Based on the CO(2−1) spectrum, we estimate a total molecular gas mass M(H2) = (2.2+0.50.4) × 1010 M⊙, where fully excited gas is assumed, and a dust mass Mdust < 4.2 × 108 M⊙ for the two blended sources. The two galaxies have similar stellar masses and Hα-based star formation rates (SFRs) found in previous work, as well as a large relative velocity of ~400 km s−1 estimated from the CO(2−1) line width. These findings tend to privilege a scenario where both sources contribute to the observed CO(2−1). Using the archival Spitzer MIPS flux at 24 μm we estimate an SFR (24μm) = (28+12−8) M⊙/yr for each of the two galaxies. Assuming that the two sources contribute equally to the observed CO(2−1), our analysis yields a depletion timescale of τdep = (3.9+1.4−1.8) × 108 yr, and a molecular gas to stellar mass ratio of 0.17 ± 0.13 for each of two sources, separately. We also provide a new, more precise measurement of an unknown weighted mean of the redshifts of the two galaxies, z = 1.163 ± 0.001. Conclusions. Our results are in overall agreement with those of other distant cluster galaxies and with model predictions for main sequence (MS) field galaxies at similar redshifts. The two target galaxies have molecular gas mass and depletion times that are marginally compatible with, but smaller than those of MS field galaxies, suggesting that the molecular gas has not been sufficiently refueled. We speculate that the cluster environment might have played a role in preventing the refueling via environmental mechanisms such as galaxy harassment, strangulation, ram-pressure, or tidal stripping. Higher-resolution and higher-frequency observations will enable us to spatially resolve the two sources and possibly distinguish between different gas processing mechanisms.

scholarly journals Magnetic field transport from AGN cores to jets, lobes, and the IGM

2008 ◽  
Vol 4 (S259) ◽  
pp. 499-508 ◽  
Author(s):  
Philipp P. Kronberg
Keyword(s):  
Energy Flow ◽  
Energy Transport ◽  
Magnetic Energy ◽  
Galaxy Cluster ◽  
Particle Beam ◽  
X Rays ◽  
Plasma Properties ◽  
Flow Paths ◽  
Poynting Flux ◽  
Cluster Environment

AbstractI describe various stages of energy flow along an extragalactic jet, which subsequently evolves into an extended lobe which is visible in radio and X-rays. The sizes of the lobes vary from kpc scales to several megaparsec, so that the largest lobes are clearly injecting back hole energy into the IGM on scales comparable with a galaxy-galaxy separation. This is sometimes loosely referred to as Black hole-IGM “feedback”. My talk begins with a well-formed jet, and avoids the complex and unclarified physics at less than a few Schwarzschild radii that cause the initial launching the jet.This presentation focuses on recent thinking and supercomputer simulations that appear to clarify the fundamental nature of these remarkable jets and lobes. The energy transport process appears to be electrodynamic, rather than particle beam–driven. A new observational verification of a 1018 Ampère current in an actual jet is concordant with the predictions and simulations of poynting flux-dominated electromagnetic jets. In this model the current is tightly related to the BH mass and angular energy.The magneto-plasma properties of the lobes must obviously match to the jets which feed them. The “energy sink” phase is when BH energy is ultimately deposited on supra-galactic scales. The process from the BH to the lobe production happens with remarkable efficiency. The presence or absence of a galaxy cluster environment creates laboratory conditions that help to calibrate the energy flow paths, and the magnetic rigidity of these jet-lobe systems.I conclude by describing recent, sensitive radio observations on supra-cluster scales that test for final magnetic energy deposition - the “sink” phase - into the intergalactic medium.

scholarly journals AlFoCS  + F3D – II. Unexpectedly low gas-to-dust ratios in the Fornax galaxy cluster

2021 ◽  
Vol 502 (4) ◽  
pp. 4723-4742
Author(s):  
Nikki Zabel ◽  
Timothy A Davis ◽  
Matthew W L Smith ◽  
Marc Sarzi ◽  
Alessandro Loni ◽  
...  
Keyword(s):  
Gas Phase ◽  
Large Fraction ◽  
Galaxy Cluster ◽  
Mass Range ◽  
Stellar Mass ◽  
Virgo Cluster ◽  
Cluster Galaxies ◽  
Cluster Environment ◽  
Fornax Cluster ◽  
Compact Array

ABSTRACT We combine observations from Atacama Large Millimeter/submillimeter Array (ALMA), Australia Telescope Compact Array, Multi Unit Spectroscopic Explorer (MUSE), and Herschel to study gas-to-dust ratios in 15 Fornax cluster galaxies detected in the FIR/sub-mm by Herschel and observed by ALMA as part of the ALMA Fornax Cluster Survey. The sample spans a stellar mass range of 8.3 ≤  log(M⋆/M⊙) ≤ 11.16, and a variety of morphological types. We use gas-phase metallicities derived from MUSE observations (from the Fornax3D survey) to study these ratios as a function of metallicity, and to study dust-to-metal ratios, in a sub-sample of nine galaxies. We find that gas-to-dust ratios in Fornax galaxies are systematically lower than those in field galaxies at fixed stellar mass/metallicity. This implies that a relatively large fraction of the metals in these Fornax systems is locked up in dust, which is possibly due to altered chemical evolution as a result of the dense environment. The low ratios are not only driven by H i deficiencies, but H2-to-dust ratios are also significantly decreased. This is different in the Virgo cluster, where low gas-to-dust ratios inside the virial radius are driven by low H i-to-dust ratios, while H2-to-dust ratios are increased. Resolved observations of NGC 1436 show a radial increase in H2-to-dust ratio, and show that low ratios are present throughout the disc. We propose various explanations for the low H2-to-dust ratios in the Fornax cluster, including the more efficient stripping of H2 compared to dust, more efficient enrichment of dust in the star formation process, and altered interstellar medium physics in the cluster environment.

scholarly journals Feedback from reorienting AGN jets

2018 ◽  
Vol 617 ◽  
pp. A58 ◽  
Author(s):  
S. Cielo ◽  
A. Babul ◽  
V. Antonuccio-Delogu ◽  
J. Silk ◽  
M. Volonteri
Keyword(s):  
Orientation Angle ◽  
Galaxy Cluster ◽  
Cluster Core ◽  
Opening Angle ◽  
Intracluster Medium ◽  
X Ray ◽  
The Core ◽  
Cluster Environment ◽  
Jet Energy ◽  
Jet Power

Aims. We test the effects of re-orienting jets from an active galactic nucleus (AGN) on the intracluster medium in a galaxy cluster environment with short central cooling time. We investigate both the appearance and the properties of the resulting cavities, and the efficiency of the jets in providing near-isotropic heating to the cooling cluster core. Methods. We use numerical simulations to explore four models of AGN jets over several active/inactive cycles. We keep the jet power and duration fixed across the models, varying only the jet re-orientation angle prescription. We track the total energy of the intracluster medium (ICM) in the cluster core over time, and the fraction of the jet energy transferred to the ICM. We pay particular attention to where the energy is deposited. We also generate synthetic X-ray images of the simulated cluster and compare them qualitatively to actual observations. Results. Jets whose re-orientation is minimal (≲20°) typically produce conical structures of interconnected cavities, with the opening angle of the cones being ~15–20°, extending to ~300 kpc from the cluster centre. Such jets transfer about 60% of their energy to the ICM, yet they are not very efficient at heating the cluster core, and even less efficient at heating it isotropically, because the jet energy is deposited further out. Jets that re-orientate by ≳20° generally produce multiple pairs of detached cavities. Although smaller, these cavities are inflated within the central 50 kpc and are more isotropically distributed, resulting in more effective heating of the core. Such jets, over hundreds of millions of years, can deposit up to 80% of their energy precisely where it is required. Consequently, these models come the closest in terms of approaching a heating/cooling balance and mitigating runaway cooling of the cluster core even though all models have identical jet power/duration profiles. Additionally, the corresponding synthetic X-ray images exhibit structures and features closely resembling those seen in real cool-core clusters.

scholarly journals INTERACTIONS OF GALAXIES IN THE GALAXY CLUSTER ENVIRONMENT

2009 ◽  
Vol 699 (2) ◽  
pp. 1595-1609 ◽  
Author(s):  
Changbom Park ◽  
Ho Seong Hwang
Keyword(s):  
Galaxy Cluster ◽  
The Galaxy ◽  
Cluster Environment

scholarly journals Ram pressure stripping candidates in the coma cluster: evidence for enhanced star formation

2020 ◽  
Vol 495 (1) ◽  
pp. 554-569 ◽  
Author(s):  
Ian D Roberts ◽  
Laura C Parker
Keyword(s):  
Star Formation ◽  
Galaxy Cluster ◽  
Coma Cluster ◽  
Star Forming ◽  
Normal Star ◽  
Isolated Galaxies ◽  
Ram Pressure ◽  
The Galaxy ◽  
Cluster Environment ◽  
Concentration Asymmetry

ABSTRACT The Coma cluster is the nearest massive ($M \gtrsim 10^{15}\, \mathrm{M_\odot }$) galaxy cluster, making it an excellent laboratory to probe the influence of the cluster environment on galaxy star formation. Here, we present a sample of 41 galaxies with disturbed morphologies consistent with ram pressure stripping. These galaxies are identified visually using high-quality, multiband imaging from the Canada–France–Hawaii telescope covering ${\sim}9\, \mathrm{deg^2}$ of the Coma cluster. These ‘stripping candidates’ are clear outliers in common quantitative morphological measures, such as concentration-asymmetry and Gini-M20, confirming their disturbed nature. Based on the orientations of observed asymmetries, as well as the galaxy positions in projected phase space, these candidates are consistent with galaxies being stripped shortly after infall on to the Coma cluster. Finally, the stripping candidates show enhanced star formation rates, both relative to ‘normal’ star-forming Coma galaxies and isolated galaxies in the field. Ram pressure is likely driving an enhancement in star formation during the stripping phase, prior to quenching. On the whole, ram pressure stripping appears to be ubiquitous across all regions of the Coma cluster.

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