Diffuse Extreme-Ultraviolet Emission from the Coma Cluster: Evidence for Rapidly Cooling Gases at Submegakelvin Temperatures

Lieu, Richard; Mittaz, Jonathan P. D.; Bowyer, Stuart; Breen, J.; Lockman, Felix J.; Murphy, E. M.; Hwang, Chorng-Yuan

doi:10.1126/science.274.5291.1335

Cited by 139 publications

(143 citation statements)

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“…It is evident that clusters like Sér-sic 159-03 (Bonamente et al 2001c), where the soft excess reaches a prominence of 50%-100% in PSPC C band, are exceptional. A few cases where comparison with EUVE/ Deep Survey data in the $65-190 eV band are available (Coma, Virgo, A2199, A1795; Lieu et al 1996aLieu et al , 1996bMittaz et al 1998;Lieu et al 1999a) suggest that the soft excess phenomenon may be intrinsically very soft, e.g., more suitably revealed with large in the extreme-ultraviolet band.…”

Section: Resultsmentioning

confidence: 99%

“…The excess emission of Coma (Lieu et al 1996a), Virgo (Lieu et al 1996b;Bonamente et al 2001b), A2199 (Lieu et al 1999), A1795 (Bonamente et al 2001b), A3558 and A3571 (Bonamente et al 2001d), and of Sérsic 159-03 (Bonamente et al 2001c, not included in this sample) indicate that the emission may be due to either a second phase of the ICM at lower temperature (T $ 10 6 K, . Dotted diamonds are regions where C-band emission is below 25% of the C-band background; where no dotted diamonds are reported, either the PSPC boresight position did not allow extending the analysis to larger radii (A1367, Coma, and Virgo) or the peculiar cluster morphology impeded it (Hercules).…”

Section: Discussionmentioning

confidence: 99%

“…The initial discovery of soft X-ray and extreme-ultraviolet (EUV) excess emission in a few nearby galaxy clusters with the Extreme Ultraviolet Explorer and ROSAT missions (Coma, Virgo, A2199, and A1795; Lieu et al 1996aLieu et al , 1996bMittaz, Lieu, & Lockman 1998;Lieu, Bonamente, & Mittaz 1999a) was soon followed by many reobservations and reanalyses of the same objects, plus a few more clusters, with the aid of complementary data from BeppoSAX, Far Ultraviolet Spectroscopic Explorer, Rossi X-Ray Timing Explorer, and the Hopkins Ultraviolet Telescope (Fabian 1996;Bonamente, Lieu, & Mittaz 2001b;Bonamente et al 2001d;Lieu et al 1999bLieu et al , 1999cBerghoefer, Bowyer, & Korpela 2000a, 2000bBowyer & Berghoefer 1998, Bowyer, Korpela, & Berghoefer 2001Bowyer, Berghoefer, & Korpela 1999;Arabadjis & Bregman 1999;Reynolds et al 1999;Kaastra et al 1999;Dixon et al 2001;Dixon, Hurwitz, & Ferguson 1996;Valinia et al 2000;Fusco-Femiano et al 2000;Buote 2000aBuote , 2000bBuote , 2001Arnaud et al 2001). The present analysis of a very large sample of X-ray-selected clusters has the primary aim of assessing the cosmological importance of this '' soft excess '' emission.…”

Section: Introductionmentioning

confidence: 99%

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The Soft X‐Ray Emission in a Large Sample of Galaxy Clusters with theROSATPosition Sensitive Proportional Counter

Bonamente

Lieu

Joy

et al. 2002

ApJ

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148

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The study of soft X-ray emission of 38 X-ray-selected galaxy clusters observed by the ROSAT Position Sensitive Proportional Counter indicates that the '' soft excess '' phenomenon may be a common occurrence in galaxy clusters. Excess soft X-ray radiation, above the contribution from the hot intracluster medium, is evident in a large fraction of sources and is clearly detected with large statistical significance in the deepest observations. The investigation relies on new, high-resolution 21 cm H i observations. The sample selection also features analysis of infrared images to further ensure reliability of results with respect to the characteristics of Galactic absorption. The possibility of background or calibration effects as cause of the excess emission is likewise investigated; a detailed analysis of the distribution of the excess emission with respect to detector position and Galactic H i column density shows that the excess emission is a genuine celestial phenomenon. We find evidence for a preferential distribution of the soft excess emission at distances larger than $150-200 kpc from the centers of clusters; this behavior may be naturally explained in the context of a nonthermal inverse Compton scenario. Alternatively, we propose that the phenomenon may be caused by thermal emission of very large scale '' warm '' filaments seen in recent hydrodynamic simulations. This new interpretation relieves the very demanding requirements of either the traditional intracluster '' warm '' gas and the nonthermal scenarios. We also investigate the possibility of the soft excess originating from unresolved, X-ray-faint cluster galaxies.

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Section: Resultsmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Soft X‐Ray Emission in a Large Sample of Galaxy Clusters with theROSATPosition Sensitive Proportional Counter

Bonamente

Lieu

Joy

et al. 2002

ApJ

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148

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“…The Coma cluster also features a large-scale halo of warm gas at sub-virial temperatures that was discovered from ROSAT and EUVE (Lieu et al 1996;Bonamente et al 2003Bonamente et al , 2009). Pointed ROSAT observations that cover the entire Coma cluster measured a temperature of kT 1 /4 keV for the warm gas, in addition to the well-known hot intra-cluster medium.…”

Section: The Sightline Towards X Comae and The Coma Clustermentioning

confidence: 99%

Characterization of the warm–hot intergalactic medium near the Coma cluster through high-resolution spectroscopy of X Comae

Bonamente

Ahoranta

Tilton

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We have analyzed all available archival XMM-Newton observations of X Comae, a bright X-ray quasar behind the Coma cluster, to study the properties of the warm-hot intergalactic medium in the vicinity of the nearest massive galaxy cluster. The RGS observations confirm the possible presence of a Ne IX Kα absorption line at the redshift of Coma, although with a limited statistical significance. This analysis is therefore in line with the earlier analysis by Takei et al. (2007) based on a sub-set of these data. Its large column density and optical depth, however, point to implausible conditions for the absorbing medium, thereby casting serious doubts to its reality. Chandra has never observed X Comae and therefore cannot provide additional information on this source. We combine upper limits to the presence of other X-ray absorption lines (notably from O VII and O VIII) at the redshift of Coma with positive measurements of the soft excess emission from Coma measured by ROSAT (Bonamente et al. 2003). The combination of emission from warm-hot gas at kT ∼ 1 /4 keV and upper limits from absorption lines provide useful constraints on the density and the sightline length of the putative WHIM towards Coma. We conclude that the putative warm-hot medium towards Coma is consistent with expected properties, with a baryon overdensity δ b ≥ 10 and a sightline extent of order of tens of Mpc.Subject headings: quasars: individual: X Comae, large-scale structure of Universe, intergalactic medium, quasars: absorption lines, X-rays: galaxies The search for missing baryonsThe diffuse intergalatic medium contains the majority of the universe's baryons at all redshifts , and references therein). At high redshift, the bulk of this mass is in the pho-

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“…The first interpretation proposed was that the soft excess emission was thermal, with a single component of ICM gas at a temperature between 5 × 10 5 K and 10 6 K for Virgo (Lieu et al 1996a) and two components at 8 × 10 5 K and 2 × 10 6 K for Coma (Lieu et al 1996b). The immediate implication of this hypothesis was that such warm gas would cool very rapidly, implying a very high mass accretion rate of several hundred Solar masses per year, and therefore the production of a large amount of gas in the cool phase (of the order of 10 14 M , Lieu et al 1996aLieu et al , 1996b). …”

Section: The Firstmentioning

confidence: 99%

Soft X-Ray and Extreme Ultraviolet Excess Emission from Clusters of Galaxies

Durret

Kaastra

Nevalainen

et al.

Clusters of Galaxies

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An excess over the extrapolation to the extreme ultraviolet and soft X-ray ranges of the thermal emission from the hot intracluster medium has been detected in a number of clusters of galaxies. We briefly present each of the satellites (EUVE, ROSAT PSPC and BeppoSAX, and presently XMM-Newton, Chandra and Suzaku) and their corresponding instrumental issues, which are responsible for the fact that this soft excess remains controversial in a number of cases. We then review the evidence for this soft X-ray excess and discuss the possible mechanisms (thermal and non-thermal) which could be responsible for this emission.

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Diffuse Extreme-Ultraviolet Emission from the Coma Cluster: Evidence for Rapidly Cooling Gases at Submegakelvin Temperatures

Cited by 139 publications

References 14 publications

The Soft X‐Ray Emission in a Large Sample of Galaxy Clusters with theROSATPosition Sensitive Proportional Counter

The Soft X‐Ray Emission in a Large Sample of Galaxy Clusters with theROSATPosition Sensitive Proportional Counter

Characterization of the warm–hot intergalactic medium near the Coma cluster through high-resolution spectroscopy of X Comae

Soft X-Ray and Extreme Ultraviolet Excess Emission from Clusters of Galaxies

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