Discovery of an Ionized F[CLC]e[/CLC] K Edge in the [ITAL][CLC]z[/CLC][/ITAL] = 3.91 Broad Absorption Line Quasar APM 08279+5255 with [ITAL]XMM-Newton[/ITAL]

Hasinger, G.; Schartel, N.; Komossa, Stefanie

doi:10.1086/342191

Cited by 129 publications

(182 citation statements)

References 14 publications

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“…By comparing photometric data acquired from the Beijing-Arizona-TaiwanConnecticut system with up-to-date theoretical synthesis models, Ma et al [467] obtained the ages of 139 globular clusters (GCs) in the M31 galaxy, in which 9 extremely old GCs are older than the present cosmic age predicted by the 7-year WMAP observations [468]. In addition, the existence of high-z quasar APM 08279+5255 at z = 3.91 [469] is also a mystery [470,471,472]. Using the maximum likelihood values of the 7-year WMAP observations Ω m = 0.272 and h = 0.704, the ΛCDM model can only give a cosmic age t = 1.63 Gyr at redshift z = 3.91, while the lower limit of this quasar's age is 1.8 Gyr.…”

Section: Cosmic Age Testsmentioning

confidence: 99%

Dark Energy

Li¹,

Li²,

Wang³

et al. 2011

Commun. Theor. Phys.

772

560

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Section: Cosmic Age Testsmentioning

confidence: 99%

Dark Energy

Li¹,

Li²,

Wang³

et al. 2011

Commun. Theor. Phys.

772

560

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“…We prefer to use as background the long observation (100 ks) of the quasar APM 08279+5255 (Hasinger et al 2002) performed with the medium filter, which has also a Galactic N H of 4 × 10 20 cm −2 more similar to the one in the direction of A3528 (6.1 × 10 20 cm −2 ). We performed the same selection criteria for the background as the source, we removed all the bright sources and after rejection of soft proton flares we got an effective exposure time of 73 ks for MOS and 62 ks for PN.…”

Section: Observation and Data Preparationmentioning

confidence: 99%

XMM-Newtonobservation of the interacting cluster Abell 3528

Gastaldello

Ettori

Molendi

et al. 2003

A&A

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Abstract.We analyze the XMM-Newton dataset of the interacting cluster of galaxies Abell 3528 located westward in the core of the Shapley Supercluster, the largest concentration of mass in the nearby Universe. A3528 is formed by two interacting clumps (A3528-N at North and A3528-S at South) separated by 0.9 h −1 70 Mpc at redshift 0.053. XMM-Newton data describe these clumps as a relaxed structure with an overall temperature of 4.14 ± 0.09 and 4.29 ± 0.07 keV in A3528-N and A3528-S, respectively, and a core cooler by a factor 1.4-1.5 and super-solar metal abundance in the inner 30 arcsec. These clumps are connected by a X-ray soft, bridge-like emission and present an asymmetric surface brightness with significant excess in the North-West region of A3528-N and in the North-East area of A3528-S. However, we do not observe any evidence of shock heated gas, both in the surface brightness and in the temperature map. Considering also that the optical light distribution is more concentrated around A3528-N and makes A3528-S barely detectable, we do not find support for the originally suggested head-on pre-merging scenario and conclude that A3528 is in an off-axis post-merging phase, where the closest core encounter happened about 1-2 Gyrs ago.

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“…Several processes have been proposed to explain the observed enrichment in the ICM: ram-pressure stripping (Gunn & Gott 1972), galactic winds (De Young 1978), galaxy-galaxy interactions (Gnedin 1998), AGN outflows (De Young 1986;Hasinger et al 2002), intracluster supernovae (Gerhard et al 2002), and others. Simulations show an inhomogeneous distribution of the metals independent of the enrichment processes (Kapferer et al 2006;Schindler & Diaferio 2008).…”

Section: Introductionmentioning

confidence: 99%

Inhomogeneous metal distribution in the intracluster medium

Lovisari

Schindler

Kapferer

2011

A&A

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Context. The hot gas that fills the space between galaxies in clusters is rich in metals. In their large potential wells, galaxy clusters accumulate metals over the whole cluster history and hence retain important information on cluster formation and evolution. Aims. We use a sample of five cool core clusters to study the distribution of metals in the ICM. We investigate whether the X-ray observations yield good estimates for the metal mass and whether the heavy elements abundances are consistent with a certain relative fraction of SN Ia to SNCC. Methods. We derived detailed metallicity maps of the clusters from XMM-Newton observations and used them as a measure for the metal mass in the ICM. We determined radial profiles for several elements, and using population synthesis and chemical enrichment models, we studied the agreement between the measured abundances and the theoretical yields. Results. We show that the distribution of metals show a lot of inhomogeneities even in relaxed clusters. Using metal maps usually gives a metal mass 10-30% higher than the metal mass computed using a single extraction region, so it is expected that most previous metal mass determination have underestimated metal mass. The abundance ratio of α-elements to Fe, even in the central parts of clusters, are consistent with an enrichment thanks to the combination of SN Ia and SNCC.

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Discovery of an Ionized F[CLC]e[/CLC] K Edge in the [ITAL][CLC]z[/CLC][/ITAL] = 3.91 Broad Absorption Line Quasar APM 08279+5255 with [ITAL]XMM-Newton[/ITAL]

Cited by 129 publications

References 14 publications

Dark Energy

Dark Energy

XMM-Newtonobservation of the interacting cluster Abell 3528

Inhomogeneous metal distribution in the intracluster medium

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