Probing Warm-Hot Intergalactic Medium Associated with the Virgo Cluster Using an Oxygen Absorption Line

Fujimoto, R.; Takei, Yoh; Tamura, Takayuki; Mitsuda, Kazuhisa; Yamasaki, Noriko Y.; Shibata, Ryo; Ohashi, T.; Ota, Naomi; Audley, M. D.; Kelley, R. L.; Kilbourne, Caroline A.

doi:10.1093/pasj/56.5.l29

Cited by 33 publications

(31 citation statements)

References 31 publications

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“…Marginal detection of O viii and Ne ix absorption features in XMM-Newton RGS spectra of distant quasars was reported in the vicinity of the Virgo and Coma clusters and interpreted as indication of the presence of dense and hot WHIM concentrations near the clusters (Fujimoto et al 2004;Takei et al 2007). A blind search for WHIM was performed by Nicastro et al (2005), who reported the discovery of two intervening systems at z > 0 in absorption along the line-of-sight to the blazar Mrk 421 in the Chandra Low Energy Transmission Grating Spectrometer (LETGS) spectra.…”

Section: Introductionmentioning

confidence: 92%

Detection of hot gas in the filament connecting the clusters of galaxies Abell 222 and Abell 223

Werner¹,

Finoguenov

Kaastra

et al. 2008

A&A

159

176

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Context. About half of the baryons in the local Universe are invisible and -according to simulations -their dominant fraction resides in filaments connecting clusters of galaxies in the form of low density gas with temperatures in the range of 10 5 < T < 10 7 K. This warm-hot intergalactic medium has never been detected indisputably using X-ray observations. Aims. We aim to probe the low gas densities expected in the large-scale structure filaments by observing a filament connecting the massive clusters of galaxies A 222 and A 223 (z = 0.21), which has a favorable orientation approximately along our line-of-sight. This filament has been previously detected using weak lensing data and as an over-density of colour-selected galaxies. Methods. We analyse X-ray images and spectra obtained from a deep observation (144 ks) of A 222/223 with XMM-Newton. Results. We present observational evidence of X-ray emission from the filament connecting the two clusters. We detect the filament in the wavelet-decomposed soft-band (0.5-2.0 keV) X-ray image with a 5σ significance. Following the emission down to the 3σ significance level, the observed filament is ≈1.2 Mpc wide. The temperature of the gas associated with the filament, determined from the spectra, is k T = 0.91±0.25 keV, and its emission measure corresponds to a baryon density of (3.4±1.3)×10−5 (l/15 Mpc) −1/2 cm −3 , where l is the length of the filament along the line-of-sight. This density corresponds to a baryon over-density of ρ/ ρ C ≈ 150. The properties of the gas in the filament are consistent with results of simulations of the densest and hottest parts of the warm-hot intergalactic medium.

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Section: Introductionmentioning

confidence: 92%

Detection of hot gas in the filament connecting the clusters of galaxies Abell 222 and Abell 223

Werner¹,

Finoguenov

Kaastra

et al. 2008

A&A

159

176

View full text Add to dashboard Cite

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“…The properties of the WHIM in filaments of galaxies have been investigated before. For instance, the density of the WHIM in filaments has been deduced from observations of X-ray absorption lines (Takei et al 2002;Fujimoto et al 2004;Nicastro et al 2005; Kaastra et al 2006;Buote et al 2009;Fang et al 2010;Zappacosta et al 2010;Nicastro et al 2013). Up to now, however, X-ray emission from the WHIM has not been detected yet, due to limited sensitivities of X-ray spectrometers such as CCD cameras, except for reports of angular correlation of the diffuse X-ray background (Galeazzi et al 2009) and emission in a filament linking two clusters of galaxies (Werner et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Properties of the cosmological filament between two clusters: A possible detection of a large-scale accretion shock bySuzaku

Akamatsu

Fujita

Akahori

et al. 2017

A&A

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We report on the results of a Suzaku observation of the plasma in the filament located between the two massive clusters of galaxies Abell 399 and Abell 401. Abell 399 (z=0.0724) and Abell 401 (z=0.0737) are expected to be in the initial phase of a cluster merger. In the region between the two clusters, we find a clear enhancement in the temperature of the filament plasma from 4 keV (expected value from a typical cluster temperature profile) to kT∼6.5 keV. Our analysis also shows that filament plasma is present out to a radial distance of 15 ′ (1.3 Mpc) from a line connecting the two clusters. The temperature profile is characterized by an almost flat radial shape with kT∼6-7 keV within 10 ′ or ∼0.8 Mpc. Across r=8 ′ from the axis, the temperature of the filament plasma shows a drop from 6.3 keV to 5.1 keV, indicating the presence of a shock front. The Mach number based on the temperature drop is estimated to be M ∼1.3. We also successfully determined the abundance profile up to 15 ′ (1.3 Mpc), showing an almost constant value (Z=0.3 solar) at the cluster outskirt. We estimated the Compton y-parameter to be ∼14.5±1.3 × 10 −6 , which is in agreement with Planck's results (14-17×10 −6 on the filament). The line of sight depth of the filament is l∼1.1 Mpc, indicating that the geometry of filament is likely a pancake shape rather than cylindrical. The total mass of the filamentary structure is ∼7.7×10 13 M ⊙ . We discuss a possible interpretation of the drop of X-ray emission at the rim of the filament, which was pushed out by the merging activity and formed by the accretion flow induced by the gravitational force of the filament.

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“…Fujimoto et al (2004) attempted to detect absorption in the quasar LBQS 1228+1116, located behind the Virgo cluster. An XMM-Newton RGS spectrum revealed a marginal feature at the (Virgo) redshifted position of O VIII Lyα, but only at the ∼ 95% confidence level.…”

Section: Intervening Whim Absorbers At Low Redshiftmentioning

confidence: 99%

FUV and X-Ray Absorption in the Warm-Hot Intergalactic Medium

2008

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The Warm-Hot Intergalactic Medium (WHIM) arises from shock-heated gas collapsing in large-scale filaments and probably harbours a substantial fraction of the baryons in the local Universe. Absorption-line measurements in the ultraviolet (UV) and in the Xray band currently represent the best method to study the WHIM at low redshifts. We here describe the physical properties of the WHIM and the concepts behind WHIM absorption line measurements of H I and high ions such as O VI, O VII, and O VIII in the far-ultraviolet and X-ray band. We review results of recent WHIM absorption line studies carried out with UV and X-ray satellites such as FUSE, HST, Chandra, and XMM-Newton and discuss their implications for our knowledge of the WHIM.

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Probing Warm-Hot Intergalactic Medium Associated with the Virgo Cluster Using an Oxygen Absorption Line

Cited by 33 publications

References 31 publications

Detection of hot gas in the filament connecting the clusters of galaxies Abell 222 and Abell 223

Detection of hot gas in the filament connecting the clusters of galaxies Abell 222 and Abell 223

Properties of the cosmological filament between two clusters: A possible detection of a large-scale accretion shock bySuzaku

FUV and X-Ray Absorption in the Warm-Hot Intergalactic Medium

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