XMM-Newton observation of the distant ($\vec{z=0.6}$) galaxy cluster
RX J1120.1+4318

Arnaud, M.; Majerowicz, S.; Lumb, D.; Neumann, D. M.; Aghanim, N.; Blanchard, Alain; Boër, M.; Burke, Douglas; Collins, Chris; Giard, M.; Nevalainen, J.; Nichol, R. C.; Romer, A. K.; Sadat, R.

doi:10.1051/0004-6361:20020669

Cited by 103 publications

(122 citation statements)

References 40 publications

Supporting

Mentioning

119

Contrasting

Order By: Relevance

“…The ratio of the counting rate between 10 and 12 keV (where the sensitivity to X-rays is very low) was computed for the whole field of view in each observation: this ratio was then used to normalise each background spectrum with respect to the corresponding observation spectrum. Another contribution to the background comes from the soft X-ray background which varies from place to place in the sky: a reference X-ray background spectrum was derived outside SN 1006, analysed in the same way as the SN 1006 spectra and added to the instrumental background to obtain the total background to be subtracted to the observation spectrum in a given region (see Arnaud et al 2002, for a complete description of this method). For each region, we extracted at least 2 and up to 6 spectra, since the different observations overlap in the sky.…”

Section: Methodsmentioning

confidence: 99%

Geometry of the non-thermal emission in SN 1006

Rothenflug¹,

Ballet²,

Dubner

et al. 2004

A&A

126

158

View full text Add to dashboard Cite

Abstract. SN 1006 is the prototype of shell supernova remnants, in which non-thermal synchrotron emission dominates the X-ray spectrum. The non-thermal emission is due to the cosmic-ray electrons accelerated behind the blast wave. The X-ray synchrotron emission is due to the highest energy electrons, and is thus a tracer of the maximum energy electrons may reach behind a shock. We have put together all XMM-Newton observations to build a full map of SN 1006. The very low brightness above 2 keV in the interior indicates that the bright non-thermal limbs are polar caps rather than an equator. This implies that the ambient magnetic field runs southwest to northeast, along the Galactic plane. We used a combined VLA/Parkes radio map to anchor the spectrum at low energy, and model the spectra with synchrotron emission from a cut-off power-law electron distribution, plus a thermal component. We present radial and azimuthal profiles of the cut-off frequency. The cut-off frequency decreases steeply with radius towards the center and with position angle away from the maximum emission. The maximum energy reached by accelerated particles, as well as their number, must be higher at the bright limbs than elsewhere. This implies interesting constraints for acceleration at perpendicular shocks. Overall the XMM-Newton data is consistent with the model in which the magnetic field is amplified where acceleration is efficient.

show abstract

Section: Methodsmentioning

confidence: 99%

Geometry of the non-thermal emission in SN 1006

Rothenflug¹,

Ballet²,

Dubner

et al. 2004

A&A

126

158

View full text Add to dashboard Cite

show abstract

“…This indicates that contamination by unresolved point sources of observations made with earlier satellites (e.g., by Fairley et al) was not, on average, a very significant effect. Recent work, assuming a ÃCDM cosmology, has found evidence for positive evolution of the L-T relation (e.g., Arnaud, Aghanim, & Neumann 2002b;Vikhlinin et al 2002); i.e., clusters at high redshift are more luminous for a given temperature (although Holden et al 2002 find no significant evolution in this cosmology). Our data support this general trend of positive evolution, albeit with low statistical significance due to the few points available.…”

Section: Evolution Of Cluster Scaling Relationsmentioning

confidence: 99%

“…The virial radius of a cluster may be estimated using self-similar scaling arguments, normalized to numerical simulations. Here, we adopted the formalism of Arnaud, Aghanim, & Neumann (2002a), which may be applied to a flat…”

Section: Spatial Analysismentioning

confidence: 99%

ChandraX‐Ray Analysis of the Massive High‐Redshift Galaxy Clusters Cl J1113.1−2615 and Cl J0152.7−1357

Maughan

Jones

Ebeling³

et al. 2003

ApJ

119

View full text Add to dashboard Cite

We present an analysis of Chandra observations of two high-redshift clusters of galaxies, Cl J1113.1À2615 at z ¼ 0:725 and Cl J0152.7À1357 at z ¼ 0:833. We find Cl J1113.1À2615 to be morphologically relaxed with a temperature of kT ¼ 4:3 þ0:5 À0:4 keV and a mass (within the virial radius) of 4:3 þ0:8 À0:7 Â 10 14 M . Cl J0152.7À1357, by contrast, is resolved into a northern and southern subcluster, each massive and X-rayluminous, in the process of merging. The temperatures of the subclusters are found to be 5:5 þ0:9 À0:8 and 5:2 þ1:1 À0:9keV, respectively, and we estimate their respective masses to be 6:1 þ1:7 À1:5 Â 10 14 and 5:2 þ1:8 À1:4 Â 10 14 M within the virial radii. A dynamical analysis of the system shows that the subclusters are likely to be gravitationally bound. If the subclusters merge, they will form a system with a mass similar to that of the Coma Cluster. Two-dimensional modeling of the X-ray surface brightness reveals excess emission between the subclusters, suggestive, but not conclusive, evidence of a shock front. We make a first attempt at measuring the cluster M-T relation at z % 0:8 and find no evolution in its normalization, supporting the previous assumption of an unevolving M-T relation when constraining cosmological parameters from cluster evolution studies. A comparison of the cluster properties with those of nearby systems also finds little or no evolution in the L-T relation, the gas fraction-T relation, the -T relation, or the metallicity. These results suggest that, in at least some massive clusters, the hot gas was in place, and containing its metals, at z % 0:8 and thus that the clusters were assembled at redshifts significantly higher than z ¼ 0:8, as predicted in low-M models. We also highlight the need to correct for the degradation of the Chandra ACIS low-energy quantum efficiency in high-redshift cluster studies when the low-energy absorption is often assumed to be the Galactic value, rather than measured.

show abstract

“…In addition, we transformed the coordinates of the background file such that they were the same as for the associated cluster data set. The background subtraction was performed using the double subtraction process described in full detail in Arnaud et al (2002). It involves subtraction of the normalised blank field data, and subsequent subtraction of the cosmic X-ray background component estimated in the area of the field of view that does not show cluster emission.…”

Section: X-ray Analysismentioning

confidence: 99%

Metallicity map of the galaxy cluster A3667

Lovisari¹,

Kapferer²,

Schindler³

et al. 2009

A&A

View full text Add to dashboard Cite

We use XMM-Newtondata of the merging cluster Abell 3667 to analyze its metallicity distribution. A detailed abundance map of the central 1.1 × 1.1 Mpc region indicates that metals are inhomogeneously distributed in the cluster showing a non-uniform and very complex metal pattern. The highest peak in the map corresponds to a cold region, slightly offset South of the X-ray center. This could be interpreted as stripped gas due to a merger between a group moving from NW towards the SE and the main cluster. We note several clumps of high metallicity also in the opposite direction with respect to the X-ray peak. Furthermore we determined abundances for 5 elements (O, Si, S, Ar, Fe) in four different regions of the cluster. Comparisons between these observed abundances and theoretical supernovae yields allow to get constraints on the relative number of SN Ia and II contributing to the enrichment of the intra-cluster medium. To reproduce the observed abundances of the best determined elements (Fe, O and Si) in a region of 7 around the X-ray center, 65-80% of SN II are needed. The comparison between the metal map, a galaxy density map obtained using 550 spectroscopically confirmed cluster members and, our simulations suggest a recent merger between the main cluster and the group in the SE.

show abstract

XMM-Newton observation of the distant ($\vec{z=0.6}$) galaxy cluster RX J1120.1+4318

Cited by 103 publications

References 40 publications

Geometry of the non-thermal emission in SN 1006

Geometry of the non-thermal emission in SN 1006

ChandraX‐Ray Analysis of the Massive High‐Redshift Galaxy Clusters Cl J1113.1−2615 and Cl J0152.7−1357

Metallicity map of the galaxy cluster A3667

Contact Info

Product

Resources

About