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Universe
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High Energy Emission from Clusters, Groups, and Filaments: Current Observations...
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High Energy Emission from Clusters, Groups, and Filaments: Current Observations and Future Prospects

A special issue of Universe (ISSN 2218-1997). This special issue belongs to the section "Galaxies and Clusters".

Deadline for manuscript submissions: closed (31 December 2023) | Viewed by 4382

Special Issue Editor

Prof. Dr. Mark Henriksen

E-Mail Website
Guest Editor
Physics Department, University of Maryland, Baltimore County, Baltimore, MD 21250, USA
Interests: high energy emission from clusters, groups, and filaments; galaxy evolution; astrobiology

Special Issue Information

Dear Colleagues,

From the HEAO satellites nearly 50 years ago to the present cadre of active observatories— Chandra, XMM, Suzaku, NuStar, and eRosita—our view of the physics of structure formation has changed enormously. X-ray observations of superclusters, clusters, groups, and filaments have provided unprecedented insight into structure formation. Given the huge increase in spectral and spatial resolution, as well as sensitivity that has been achieved during this time, it is especially timely to present new results with an eye toward the most important issues in structure formation that should be addressed by future missions and the telescope–detector requirements needed to carry them out. In this Special Issue, we solicit contributions that address high energy emission from clusters, groups, and filaments: current observations and future prospects.

Topics include (but are not limited to):

  • The physics of mergers and accretions including thermodynamic quantities (T,P,S) based on X-ray observations;
  • Shock physics in the intracluster medium;
  • The central region of clusters, in particular the AGN-ICM connection seen in X-ray cavities;
  • Searches for the non-thermal signature in structure formation;
  • Studies of the outskirts of the intracluster medium, including non-hydrostatic gas, accretion shocks, cool baryons;
  • Studies related to uniformity of the average abundance in clusters and spatial deviations from solar abundance;
  • Filamentary baryons;
  • Structure in supercluster/filament systems;
  • High redshift clusters of galaxies;
  • The requirements for future X-ray missions (e.g., AXIS, Athena) to address the most compelling issues for galaxy clusters.

Prof. Dr. Mark Henriksen
Guest Editor

Manuscript Submission Information

Manuscripts should be submitted online at www.mdpi.com by registering and logging in to this website. Once you are registered, click here to go to the submission form. Manuscripts can be submitted until the deadline. All submissions that pass pre-check are peer-reviewed. Accepted papers will be published continuously in the journal (as soon as accepted) and will be listed together on the special issue website. Research articles, review articles as well as short communications are invited. For planned papers, a title and short abstract (about 100 words) can be sent to the Editorial Office for announcement on this website.

Submitted manuscripts should not have been published previously, nor be under consideration for publication elsewhere (except conference proceedings papers). All manuscripts are thoroughly refereed through a single-blind peer-review process. A guide for authors and other relevant information for submission of manuscripts is available on the Instructions for Authors page. Universe is an international peer-reviewed open access monthly journal published by MDPI.

Please visit the Instructions for Authors page before submitting a manuscript. Submitted papers should be well formatted and use good English. Authors may use MDPI's English editing service prior to publication or during author revisions.

Keywords

  • clusters of galaxies
  • X-ray emission
  • superclusters
  • filaments
  • non-thermal emission
  • structure formation
  • future missions
  • intracluster medium
  • X-ray cavities
  • cluster atmosphere

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Published Papers (4 papers)

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Research

26 pages, 11389 KiB  
Article
UHECR Clustering: Lightest Nuclei from Local Sheet Galaxies
by Daniele Fargion, Pier Giorgio De Sanctis Lucentini and Maxim Yu. Khlopov
Universe 2024, 10(8), 323; https://doi.org/10.3390/universe10080323 - 9 Aug 2024
Viewed by 495
Abstract
The ultra-high-energy cosmic ray (UHECR) puzzle is reviewed under the hints of a few basic results: clustering, anisotropy, asymmetry, bending, and composition changes with energies. We show how the lightest UHECR nuclei from the nearest AGN or Star-Burst sources, located inside a few [...] Read more.
The ultra-high-energy cosmic ray (UHECR) puzzle is reviewed under the hints of a few basic results: clustering, anisotropy, asymmetry, bending, and composition changes with energies. We show how the lightest UHECR nuclei from the nearest AGN or Star-Burst sources, located inside a few Mpc Local Sheets, may explain, at best, the observed clustering of Hot Spots at tens EeV energy. Among the possible local extragalactic candidate sources, we derived the main contribution of very few galactic sources. These are located in the Local Sheet plane within a distance of a few Mpc, ejecting UHECR at a few tens of EeV energy. UHECR also shine at lower energies of several EeV, partially feeding the Auger dipole by LMC and possibly a few nearer galactic sources. For the very recent highest energy UHECR event, if a nucleon, it may be explained by a model based on the scattering of UHE ZeV neutrinos on low-mass relic neutrinos. Such scatterings are capable of correlating, via Z boson resonance, the most distant cosmic sources above the GZK bound with such an enigmatic UHECR event. Otherwise, these extreme events, if made by the heaviest composition, could originate from the largest bending trajectory of heaviest nuclei or from nearby sources, even galactic ones. In summary, the present lightest to heavy nuclei model UHECR from the Local Sheet could successfully correlate UHECR clustering with the nearest galaxies and AGN. Heavy UHECR may shine by being widely deflected from the Local Sheet or from past galactic, GRB, or SGR explosive ejection. Full article
(This article belongs to the Special Issue High Energy Emission from Clusters, Groups, and Filaments: Current Observations and Future Prospects)
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31 pages, 1771 KiB  
Article
Energetic Particles and High-Energy Processes in Cosmological Filaments and Their Astronomical Implications
by Kinwah Wu, Ellis R. Owen, Qin Han, Yoshiyuki Inoue and Lilian Luo
Universe 2024, 10(7), 287; https://doi.org/10.3390/universe10070287 - 1 Jul 2024
Viewed by 801
Abstract
Large-scale cosmic filaments connect galaxies, clusters, and voids. They are permeated by magnetic fields with a variety of topologies. Cosmic rays with energies up to 1020eV can be produced in astrophysical environments associated with star-formation and AGN activities. The fate of [...] Read more.
Large-scale cosmic filaments connect galaxies, clusters, and voids. They are permeated by magnetic fields with a variety of topologies. Cosmic rays with energies up to 1020eV can be produced in astrophysical environments associated with star-formation and AGN activities. The fate of these cosmic rays in filaments, which cannot be directly observed on Earth, are rarely studied. We investigate the high-energy processes associated with energetic particles (cosmic rays) in filaments, adopting an ecological approach that includes galaxies, clusters/superclusters, and voids as key cosmological structures in the filament ecosystem. We derive the phenomenology for modelling interfaces between filaments and these structures, and investigate how the transfer and fate of energetic cosmic ray protons are affected by the magnetism of the interfaces. We consider different magnetic field configurations in filaments and assess the implications for cosmic ray confinement and survival against hadronic pion-producing and photo-pair interactions. Our analysis shows that the fate of the particles depends on the location of their origin within a filament ecosystem, and that filaments act as ‘highways’, channelling cosmic rays between galaxies, galaxy clusters, and superclusters. Filaments can also operate as cosmic ‘fly paper’, capturing cosmic ray protons with energies up to 1018eV from cosmic voids. Our analysis predicts the presence of a population of ∼1012–1016eV cosmic ray protons in filaments and voids accumulated continually over cosmic time. These protons do not suffer significant energy losses through photo-pair or pion production, nor can they be cooled efficiently. Instead, they form a cosmic ray fossil record of the power generation history of the Universe. Full article
(This article belongs to the Special Issue High Energy Emission from Clusters, Groups, and Filaments: Current Observations and Future Prospects)
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14 pages, 709 KiB  
Article
Tracking Dusty Cloud Crushed by a Hot Flow
by Svyatoslav Dedikov and Evgenii Vasiliev
Universe 2024, 10(4), 155; https://doi.org/10.3390/universe10040155 - 26 Mar 2024
Viewed by 944
Abstract
The destructionof clouds by strong shocks and hot winds is the key process responsible for the transporting of metals and dust from the ISM to the ICM/IGM, and establishing the multiphase structure in and around galaxies. In this work, we perform a detailed [...] Read more.
The destructionof clouds by strong shocks and hot winds is the key process responsible for the transporting of metals and dust from the ISM to the ICM/IGM, and establishing the multiphase structure in and around galaxies. In this work, we perform a detailed analysis of this process using two different approaches for tracking the cloud material (gas and dust): the so-called ‘colored’ fluid, and the Lagrangian (trace) particles. We find that for the clouds in the hot phase (T>105 K), the two methods produce significantly different mass fractions and velocities of the cloud material. In contrast, the two methods produce similar results for the clouds that are in the warm/cold phases (T<105 K). We find that the Kelvin–Helmholtz instability is suppressed in the warm clouds of size ∼100 pc and metallicity Z> 0.1Zduetoeffectivegascooling.ThiscausesadelayinthedestructionofsuchcloudsthatareinteractingwiththehotICMflow.Wedemonstratethatthedustparticlesthatareevacuatedfromtheir‘parent’cloudstothehotmediumshowdifferentdynamicswhencomparedtothatoftheLagrangian(trace)particles.Ourresultsindicatethatthedustgrainssweptouttothehotgasaredestroyed. Full article
(This article belongs to the Special Issue High Energy Emission from Clusters, Groups, and Filaments: Current Observations and Future Prospects)
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20 pages, 1010 KiB  
Article
VLBI Analysis of a Potential High-Energy Neutrino Emitter Blazar
by Janka Kőmíves, Krisztina Éva Gabányi, Sándor Frey and Emma Kun
Universe 2024, 10(2), 78; https://doi.org/10.3390/universe10020078 - 6 Feb 2024
Viewed by 1340
Abstract
Recent studies suggest that high-energy neutrinos can be produced in the jets of blazars, radio-loud active galactic nuclei (AGN) with jets pointing close to the line of sight. Due to the relatively poor angular resolution of current neutrino detectors, several sources can be [...] Read more.
Recent studies suggest that high-energy neutrinos can be produced in the jets of blazars, radio-loud active galactic nuclei (AGN) with jets pointing close to the line of sight. Due to the relatively poor angular resolution of current neutrino detectors, several sources can be regarded as the possible counterpart of a given neutrino event. Therefore, follow-up observations of counterpart candidates in the electromagnetic regime are essential. Since the Very Long Baseline Interferometry (VLBI) technique provides the highest angular resolution to study the radio jets of blazars, a growing number of investigations are being conducted to connect individual blazars to given high-energy neutrino events. We analyzed more than 20 years of available archival VLBI data of the blazar CTD 74, which has been listed as a possible counterpart of a neutrino event. Using cm-wavelength data, we investigated the jet structure, determined the apparent speed of jet components, and the core flux density before and after the neutrino event. Our results indicate stationary jet features and a significant brightening of the core after the neutrino event. Full article
(This article belongs to the Special Issue High Energy Emission from Clusters, Groups, and Filaments: Current Observations and Future Prospects)
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