Chandra and XMM-Newton Observations of the Abell 3395/Abell 3391 Intercluster Filament

Alvarez, Gabriella E.; Randall, Scott W.; Bourdin, H.; Jones, C.; Holley‐Bockelmann, Kelly

doi:10.3847/1538-4357/aabad0

Cited by 36 publications

(57 citation statements)

References 76 publications

(111 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Yellow circle represents a 5 arcmin width beam. Both the X-ray and the mm images evidence a blob to the South of A3395, that coincides with galaxy group ESO-161 (see [9] for details about Chandra observations of this system). Bottom-right panel: Wavelet denoised X-ray surface brightness in the energy band 0.5-2.5 keV (see [10] for details about XMM-Newton observations of this system).…”

Section: All-sky Mapping Of the Thermal Sz Signalsupporting

confidence: 57%

See 1 more Smart Citation

Extracting the thermal SZ signal from heterogeneous millimeter data sets

et al. 2020

View full text Add to dashboard Cite

Complementarily to X-ray observations, the thermal SZ effect is a powerful tool to probe the baryonic content of galaxy clusters from their core to their peripheries. While contaminations by astrophysical and instrumental backgrounds require us to scan the thermal SZ signal across various frequencies, the multi-scale nature of cluster morphologies require us to observe such objects at various angular resolutions. We developed component separation algorithms that take advantage of sparse representations to combine these heterogeneous pieces of information, separate the thermal SZ signal from its contaminants, detect and map the thermal SZ signal of galaxy clusters from nearby to more distant clusters of the Planck catalogue. Spatially weighted likelihoods allow us in particular to connect parametric fittings of the component Spectral Energy Distribution with wavelet and curvelet imaging, but also to combine signals registered with beams of various width. Such techniques already allow us to detect sub-structures in the peripheries of nearby clusters with Planck, and could be extended to observations performed at higher angular resolutions.

show abstract

Section: All-sky Mapping Of the Thermal Sz Signalsupporting

confidence: 57%

“…This maps exhibits a blob to the south of A3395, and a sharp bridge that connects A3395 to A3391. The blob might coincide with accreted galaxy group ESO-161 visible in X-ray from a composite Chandra observation (see details in [9]).…”

Section: Cluster Imagingmentioning

confidence: 91%

Extracting the thermal SZ signal from heterogeneous millimeter data sets

et al. 2020

View full text Add to dashboard Cite

show abstract

“…We also estimate the gas temperature at the cores of the filaments and find 0.9 +1.0 −0.6 keV. Our measurement can be compared with other X-ray measurements of individual filaments between cluster pairs or in the outskirts of clusters such as ∼ 0.3 keV by SUZAKU (Hattori et al 2017), ∼ 0.4 keV by Chandra and XMM-Newton (Alvarez et al 2018), and 0.7 -2.0 keV by XMM-Newton (Eckert et al 2015). These measurements are limited to individual, short (∼ a few Mpc), and dense (δ > 200) filaments.…”

Section: Discussionmentioning

confidence: 53%

First detection of stacked X-ray emission from cosmic web filaments

Tanimura

Aghanim

Kolodzig

et al. 2020

A&A

View full text Add to dashboard Cite

We report the first statistical detection of X-ray emission from cosmic web filaments in ROSAT data. We selected 15 165 filaments at 0.2 < z < 0.6 ranging from 30 Mpc to 100 Mpc in length, identified in the Sloan Digital Sky Survey survey. We stacked the X-ray count-rate maps from ROSAT around the filaments, excluding resolved galaxy groups and clusters above the mass of ∼3 × 1013 M⊙ as well as the detected X-ray point sources from the ROSAT, Chandra, and XMM-Newton observations. The stacked signal results in the detection of the X-ray emission from the cosmic filaments at a significance of 4.2σ in the energy band of 0.56−1.21 keV. The signal is interpreted, assuming the Astrophysical Plasma Emission Code model, as an emission from the hot gas in the filament-core regions with an average gas temperature of 0.9−0.6+1.0 keV and a gas overdensity of δ ∼ 30 at the center of the filaments. Furthermore, we show that stacking the SRG/eROSITA data for ∼2000 filaments only would lead to a ≳5σ detection of their X-ray signal, even with an average gas temperature as low as ∼0.3 keV.

show abstract

“…According to our expectations from detailed simulations, the best places to search for LSS activity such as infalling substructures and the hot dense fraction of the WHIM is close to nearby galaxy clusters, in their outskirts, and in the presumed warm filaments connecting them. Therefore, searching in the direction of superclusters, between galaxy clusters, or within large-scale galaxy structures or galaxy pairs using X-ray and and Sunyaev-Zeldovich (SZ) observations seems to be the currently most promising way forward (e.g., Fujita et al 2008;Werner et al 2008;Fang et al 2010;Dietrich et al 2012;Planck Collaboration et al 2013;Nevalainen et al 2015;Eckert et al 2015;Bulbul et al 2016;Parekh et al 2017;Akamatsu et al 2017;Alvarez et al 2018;Tanimura et al 2019;de Graaff et al 2019;Parekh et al 2020;Tanimura et al 2020;Ghirardini et al, subm.). (Jarrett et al 2000).…”

Section: Introductionmentioning

confidence: 99%

The Abell 3391/95 galaxy cluster system

Reiprich

Veronica

Pacaud

et al. 2021

A&A

View full text Add to dashboard Cite

Context. Inferences about dark matter, dark energy, and the missing baryons all depend on the accuracy of our model of large-scale structure evolution. In particular, with cosmological simulations in our model of the Universe, we trace the growth of structure, and visualize the build-up of bigger structures from smaller ones and of gaseous filaments connecting galaxy clusters. Aims. Here we aim to reveal the complexity of the large-scale structure assembly process in great detail and on scales from tens of kiloparsecs up to more than 10 Mpc with new sensitive large-scale observations from the latest generation of instruments. We also aim to compare our findings with expectations from our cosmological model. Methods. We used dedicated SRG/eROSITA performance verification (PV) X-ray, ASKAP/EMU Early Science radio, and DECam optical observations of a ~15 deg2 region around the nearby interacting galaxy cluster system A3391/95 to study the warm-hot gas in cluster outskirts and filaments, the surrounding large-scale structure and its formation process, the morphological complexity in the inner parts of the clusters, and the (re-)acceleration of plasma. We also used complementary Sunyaev-Zeldovich (SZ) effect data from the Planck survey and custom-made Galactic total (neutral plus molecular) hydrogen column density maps based on the HI4PI and IRAS surveys. We relate the observations to expectations from cosmological hydrodynamic simulations from the Magneticum suite. Results. We trace the irregular morphology of warm and hot gas of the main clusters from their centers out to well beyond their characteristic radii, r200. Between the two main cluster systems, we observe an emission bridge on large scale and with good spatial resolution. This bridge includes a known galaxy group but this can only partially explain the emission. Most gas in the bridge appears hot, but thanks to eROSITA’s unique soft response and large field of view, we discover some tantalizing hints for warm, truly primordial filamentary gas connecting the clusters. Several matter clumps physically surrounding the system are detected. For the “Northern Clump,” we provide evidence that it is falling towards A3391 from the X-ray hot gas morphology and radio lobe structure of its central AGN. Moreover, the shapes of these X-ray and radio structures appear to be formed by gas well beyond the virial radius, r100, of A3391, thereby providing an indirect way of probing the gas in this elusive environment. Many of the extended sources in the field detected by eROSITA are also known clusters or new clusters in the background, including a known SZ cluster at redshift z = 1. We find roughly an order of magnitude more cluster candidates than the SPT and ACT surveys together in the same area. We discover an emission filament north of the virial radius of A3391 connecting to the Northern Clump. Furthermore, the absorption-corrected eROSITA surface brightness map shows that this emission filament extends south of A3395 and beyond an extended X-ray-emitting object (the “Little Southern Clump”) towards another galaxy cluster, all at the same redshift. The total projected length of this continuous warm-hot emission filament is 15 Mpc, running almost 4 degrees across the entire eROSITA PV observation field. The Northern and Southern Filament are each detected at >4σ. The Planck SZ map additionally appears to support the presence of both new filaments. Furthermore, the DECam galaxy density map shows galaxy overdensities in the same regions. Overall, the new datasets provide impressive confirmation of the theoretically expected structure formation processes on the individual system level, including the surrounding warm-hot intergalactic medium distribution; the similarities of features found in a similar system in the Magneticum simulation are striking. Our spatially resolved findings show that baryons indeed reside in large-scale warm-hot gas filaments with a clumpy structure.

show abstract

Chandra and XMM-Newton Observations of the Abell 3395/Abell 3391 Intercluster Filament

Cited by 36 publications

References 76 publications

Extracting the thermal SZ signal from heterogeneous millimeter data sets

Extracting the thermal SZ signal from heterogeneous millimeter data sets

First detection of stacked X-ray emission from cosmic web filaments

The Abell 3391/95 galaxy cluster system

Contact Info

Product

Resources

About