scholarly journals X-ray study of the merging galaxy cluster Abell 3411-3412 with XMM-Newton and Suzaku

2020 ◽  
Vol 642 ◽  
pp. A89
Author(s):  
X. Zhang ◽  
A. Simionescu ◽  
H. Akamatsu ◽  
J. S. Kaastra ◽  
J. de Plaa ◽  
...  
Keyword(s):  
Temperature Profile ◽  
Surface Brightness ◽  
Galaxy Cluster ◽  
Low Density ◽  
X Ray ◽  
Temperature Jumps ◽  
Cluster Temperature ◽  
X Ray Background ◽  
Edge Temperature ◽  
Complex Scenario

Context. Previous Chandra observations of the Abell 3411-3412 merging galaxy cluster system revealed an outbound bullet-like sub-cluster in the northern part and many surface brightness edges at the southern periphery, where multiple diffuse sources are also reported from radio observations. Notably, a southeastern radio relic associated with fossil plasma from a radio galaxy and with a detected X-ray edge provides direct evidence of shock re-acceleration. The properties of the reported surface brightness features have yet to be constrained from a thermodynamic viewpoint. Aims. We use the XMM-Newton and Suzaku observations of Abell 3411-3412 to reveal the thermodynamical nature of the previously reported re-acceleration site and other X-ray surface brightness edges. We also aim to investigate the temperature profile in the low-density outskirts with Suzaku data. Methods. We performed both imaging and spectral analysis to measure the density jump and the temperature jump across multiple known X-ray surface brightness discontinuities. We present a new method to calibrate the vignetting function and spectral model of the XMM-Newton soft proton background. Archival Chandra, Suzaku, and ROSAT data are used to estimate the cosmic X-ray background and Galactic foreground levels with improved accuracy compared to standard blank sky spectra. Results. At the southeastern edge, temperature jumps revealed by both XMM-Newton and Suzaku point to a ℳ ∼ 1.2 shock, which agrees with the previous result from surface brightness fits with Chandra. The low Mach number supports the re-acceleration scenario at this shock front. The southern edge shows a more complex scenario, where a shock and the presence of stripped cold material may coincide. There is no evidence for a bow shock in front of the northwestern “bullet” sub-cluster. The Suzaku temperature profiles in the southern low-density regions are marginally higher than the typical relaxed cluster temperature profile. The measured value kT500 = 4.84 ± 0.04 ± 0.19 keV with XMM-Newton and kT500 = 5.17 ± 0.07 ± 0.13 keV with Suzaku are significantly lower than previously inferred from Chandra.

scholarly journals An improved deprojection and PSF-deconvolution technique for galaxy-cluster X-ray surface-brightness profiles

2006 ◽  
Vol 459 (3) ◽  
pp. 1007-1019 ◽  
Author(s):  
J. H. Croston ◽  
M. Arnaud ◽  
E. Pointecouteau ◽  
G. W. Pratt
Keyword(s):  
Surface Brightness ◽  
Galaxy Cluster ◽  
X Ray ◽  
Deconvolution Technique

scholarly journals Figuring Out Gas & Galaxies In Enzo (FOGGIE). V. The Virial Temperature Does Not Describe Gas in a Virialized Galaxy Halo

2021 ◽  
Vol 922 (2) ◽  
pp. 121
Author(s):  
Cassandra Lochhaas ◽  
Jason Tumlinson ◽  
Brian W. O’Shea ◽  
Molly S. Peeples ◽  
Britton D. Smith ◽  
...  
Keyword(s):  
Kinetic Energy ◽  
Surface Brightness ◽  
Radiative Cooling ◽  
Low Density ◽  
Energy Partition ◽  
X Ray ◽  
Stellar Feedback ◽  
Galaxy Halo ◽  
Definition Of ◽  
Halo Gas

Abstract The classical definition of the virial temperature of a galaxy halo excludes a fundamental contribution to the energy partition of the halo: the kinetic energy of nonthermal gas motions. Using simulations of low-redshift, ∼L* galaxies from the Figuring Out Gas & Galaxies In Enzo (FOGGIE) project that are optimized to resolve low-density gas, we show that the kinetic energy of nonthermal motions is roughly equal to the energy of thermal motions. The simulated FOGGIE halos have ∼2× lower bulk temperatures than expected from a classical virial equilibrium, owing to significant nonthermal kinetic energy that is formally excluded from the definition of T vir. We explicitly derive a modified virial temperature including nonthermal gas motions that provides a more accurate description of gas temperatures for simulated halos in virial equilibrium. Strong bursts of stellar feedback drive the simulated FOGGIE halos out of virial equilibrium, but the halo gas cannot be accurately described by the standard virial temperature even when in virial equilibrium. Compared to the standard virial temperature, the cooler modified virial temperature implies other effects on halo gas: (i) the thermal gas pressure is lower, (ii) radiative cooling is more efficient, (iii) O vi absorbing gas that traces the virial temperature may be prevalent in halos of a higher mass than expected, (iv) gas mass estimates from X-ray surface brightness profiles may be incorrect, and (v) turbulent motions make an important contribution to the energy balance of a galaxy halo.

scholarly journals Heating of the Interstellar Medium by Supernova Remnants

1983 ◽  
Vol 101 ◽  
pp. 385-392
Author(s):  
Donald P. Cox
Keyword(s):  
Interstellar Medium ◽  
Supernova Remnants ◽  
Supernova Remnant ◽  
Low Density ◽  
The Sun ◽  
X Ray ◽  
Interstellar Material ◽  
X Ray Background

We observe the heating of interstellar material in young supernova remnants (SNR). In addition, when analyzing the soft X-ray background we find evidence for large isolated regions of apparently hot, low density material. These, we infer, may have been heated by supernovae. One such region seems to surround the Sun. This has been modeled as a supernova remnant viewed from within. The most reasonable parameters are ambient density no ~ 0.004 cm−3, radius of about 100 pc, age just over 105 years (Cox and Anderson 1982).

scholarly journals ClG 0217+70: A massive merging galaxy cluster with a large radio halo and relics

2020 ◽  
Vol 642 ◽  
pp. L3
Author(s):  
X. Zhang ◽  
A. Simionescu ◽  
J. S. Kaastra ◽  
H. Akamatsu ◽  
D. N. Hoang ◽  
...  
Keyword(s):  
Surface Brightness ◽  
Galaxy Cluster ◽  
Precise Determination ◽  
Optical Data ◽  
Scaling Relations ◽  
Thermal Pressure ◽  
X Ray ◽  
Radio Halo ◽  
Physical Scale

We present an analysis of archival Chandra data of the merging galaxy cluster ClG 0217+70. The Fe XXV Heα X-ray emission line is clearly visible in the 25 ks observation, allowing a precise determination of the redshift of the cluster as z = 0.180 ± 0.006. We measure kT500 = 8.3  ±  0.4 keV and estimate M500 = (1.06 ± 0.11) × 1015 M⊙ based on existing scaling relations. Correcting both the radio and X-ray luminosities with the revised redshift reported here, which is much larger than previously inferred based on sparse optical data, this object is no longer an X-ray underluminous outlier in the LX − Pradio scaling relation. The new redshift also means that, in terms of physical scale, ClG 0217+70 hosts one of the largest radio halos and one of the largest radio relics known to date. Most of the relic candidates lie in projection beyond r200. The X-ray morphological parameters suggest that the intracluster medium is still dynamically disturbed. Two X-ray surface brightness discontinuities are confirmed in the northern and southern parts of the cluster, with density jumps of 1.40 ± 0.16 and 3.0 ± 0.6, respectively. We also find a 700 × 200 kpc X-ray faint channel in the western part of the cluster, which may correspond to compressed heated gas or increased non-thermal pressure due to turbulence or magnetic fields.

scholarly journals A radio halo surrounding the Brightest Cluster Galaxy in RXCJ0232.2–4420: a mini-halo in transition?

2019 ◽  
Vol 486 (1) ◽  
pp. L80-L84 ◽  
Author(s):  
Ruta Kale ◽  
Krishna M Shende ◽  
Viral Parekh
Keyword(s):  
Radio Source ◽  
Surface Brightness ◽  
Galaxy Cluster ◽  
Cosmic Ray ◽  
Radio Sources ◽  
Cluster Galaxy ◽  
X Ray ◽  
Radio Halo ◽  
The Galaxy ◽  
Radio Power

ABSTRACT Diffuse radio sources associated with the intra-cluster medium are direct probes of the cosmic ray electrons and magnetic fields. We report the discovery of a diffuse radio source in the galaxy cluster RXCJ0232.2–4420 (SPT-CL J0232–4421, z = 0.2836) using 606 MHz observations with the Giant Metrewave Radio Telescope. The diffuse radio source surrounds the Brightest Cluster Galaxy in the cluster-like typical radio mini-haloes. However the total extent of it is 550 × 800 kpc2, which is larger than mini-haloes and similar to that of radio haloes. The BCG itself is also a radio source with a marginally resolved core at 7 arcsec (30 kpc) resolution. We measure the 606 MHz flux density of the RH to be 52 ± 5 mJy. Assuming a spectral index of 1.3, the 1.4 GHz radio power is 4.5 × 1024 W Hz−1. The dynamical state of the cluster has been inferred to be 'relaxed’ and also as 'complex’, depending on the classification methods based on the morphology of the X-ray surface brightness. This system thus seems to be in the transition phase from a mini-halo to a radio halo.

scholarly journals Radio Emission from Extended Shell-Like SNRs

1998 ◽  
Vol 188 ◽  
pp. 249-250
Author(s):  
A.I. Asvarov
Keyword(s):  
Radio Emission ◽  
Thin Shell ◽  
Large Fraction ◽  
Radiative Cooling ◽  
Interstellar Space ◽  
Low Density ◽  
Shell Formation ◽  
X Ray ◽  
Cooling Effects ◽  
X Ray Background

Observations of the soft X-Ray background and interstellar UV absorption lines have indicated that a large fraction of interstellar space is filled with a high temperature low density “coronal” gas. In such low density environments SNRs will expand up to 200 pc in radius without thin shell formation which occurs due to radiative cooling effects. Such SNRs can occupy a large fraction of volume of Galaxy and can be the main source of background emissions. In the present work we examine the evolution of the radio emission of shell-like SNR evolving in the hot ISM.

scholarly journals Investigating the Relationship Between the Hot Gas and the Dark Matter Components of Galaxy Clusters.

2007 ◽  
Vol 3 (S244) ◽  
pp. 374-375
Author(s):  
Leila C. Powell ◽  
Scott T. Kay ◽  
Arif Babul ◽  
Andisheh Mahdavi
Keyword(s):  
Dark Matter ◽  
Total Mass ◽  
Surface Brightness ◽  
Galaxy Cluster ◽  
Weak Lensing ◽  
X Ray ◽  
Hot Gas ◽  
Cluster Properties ◽  
The Impact ◽  
The Relationship

AbstractVarious differences in galaxy cluster properties derived from X-ray and weak lensing observations have been highlighted in the literature. One such difference is the observation of mass concentrations in lensing maps which have no X-ray counterparts (e.g. Jee, White, Ford et al. 2005). We investigate this issue by identifying substructures in maps of projected total mass (analogous to weak lensing mass reconstructions) and maps of projected X-ray surface brightness for three simulated clusters. We then compare the 2D mass substructures with both 3D subhalo data and the 2D X-ray substructures. Here we present preliminary results from the first comparison, where we have assessed the impact of projecting the data on subhalo identification.

scholarly journals The Evaporation of Nearby Clouds and the Soft X-ray Background

1997 ◽  
Vol 166 ◽  
pp. 169-172
Author(s):  
Jonathan D. Slavin
Keyword(s):  
Solar System ◽  
Thermal Conduction ◽  
Low Density ◽  
Local Bubble ◽  
X Ray ◽  
Hot Gas ◽  
Single Temperature ◽  
Temperature Equilibrium ◽  
X Ray Background ◽  
The One

AbstractIn recent years the nature of the low density clouds within the Local Bubble has been increasingly well characterized. These clouds, including the one which surrounds the solar system, are embedded in the hot gas and therefore should be evaporating via thermal conduction. If several evaporation fronts exist within the Local Bubble, the emissivity and spectrum of the hot gas is significantly different from a single temperature, equilibrium ionization plasma. We explore models in which the the temperature, density and ionization in the hot gas are influenced by cloud evaporation and compare the results with the observed Soft X-ray Background.

scholarly journals SuperModel predictions in the outskirts of the galaxy cluster Zwicky 3146

2020 ◽  
Vol 494 (1) ◽  
pp. 1250-1256
Author(s):  
Roberto Fusco-Femiano
Keyword(s):  
Temperature Profile ◽  
Density Profile ◽  
Previous Analysis ◽  
Galaxy Cluster ◽  
Temperature Profiles ◽  
Pressure Data ◽  
Thermal Pressure ◽  
Gas Density ◽  
X Ray ◽  
The Galaxy

ABSTRACT The relaxed galaxy cluster Zwicky 3146 is analysed via the SuperModel, a tool already tested on many clusters since 2009. In particular, this analysis is focused on the intracluster medium X-ray temperature data measured by XMM–Newton up to r500. A previous analysis was based on the temperature profile derived from the Sunyaev-Zeld′ovich effect pressure data. The gas mass fraction fgas is obtained from the resulting SuperModel temperature profile extrapolated up to the virial radius R, which turns out in agreement with the steep temperature profiles observed by Suzaku, and from the gas density profile observed by XMM–Newton. The comparison between fgas with the universal value indicates a non-thermal pressure component, pnth, in the cluster outskirts. The SuperModel analysis shows a ratio α(R) (${\simeq}50{{\ \rm per\ cent}}$) of pnth to the total pressure greater than the values found by simulations, highlighting the possible presence of accreting substructures and inhomogeneities in the gas density profile. Once that this profile is corrected for clumpiness, the level of pnth is considerably reduced. However, a significant turbulence ($\alpha (R)\simeq 20{{\ \rm per\ cent}}$) and entropy flattening are still present in the outskirts of the galaxy cluster Zwicky 3146.

Sign in / Sign up

Export Citation Format

Share Document