X-ray cavities and temperature jumps in the environment of the strong cool core cluster Abell 2390
Abstract We present results based on the systematic analysis of high resolution 95 ks Chandra observations of the strong cool core cluster Abell 2390 at the redshift of $z = 0.228$ that hosts an energetic radio AGN. This analysis has enabled us to investigate five X-ray deficient cavities in the atm...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Sonkamble, S. S. [verfasserIn] Vagshette, N. D. [verfasserIn] Pawar, P. K. [verfasserIn] Patil, M. K. [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2015 |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
Enthalten in: Astrophysics and space science - Dordrecht [u.a.] : Springer Science + Business Media B.V, 1968, 359(2015), 2 vom: 25. Sept. |
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| Übergeordnetes Werk: |
volume:359 ; year:2015 ; number:2 ; day:25 ; month:09 |
| Links: |
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| DOI / URN: |
10.1007/s10509-015-2508-z |
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| Katalog-ID: |
SPR010603867 |
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| 100 | 1 | |a Sonkamble, S. S. |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a X-ray cavities and temperature jumps in the environment of the strong cool core cluster Abell 2390 |
| 264 | 1 | |c 2015 | |
| 336 | |a Text |b txt |2 rdacontent | ||
| 337 | |a Computermedien |b c |2 rdamedia | ||
| 338 | |a Online-Ressource |b cr |2 rdacarrier | ||
| 520 | |a Abstract We present results based on the systematic analysis of high resolution 95 ks Chandra observations of the strong cool core cluster Abell 2390 at the redshift of $z = 0.228$ that hosts an energetic radio AGN. This analysis has enabled us to investigate five X-ray deficient cavities in the atmosphere of Abell 2390 within central $30''$. Presence of these cavities have been confirmed through a variety of image processing techniques like, the surface brightness profiles, unsharp masked image, as well as 2D elliptical model subtracted residual map. Temperature profile as well as 2D temperature map revealed structures in the distribution of ICM, in the sense that ICM in the NW direction is cooler than that on the SE direction. Temperature jump in all directions is evident near $25''$ (90.5 kpc) corresponding to the average Mach number $1.44\pm 0.05$, while another jump from 7.47 keV to 9.10 keV at $68''$ (246 kpc) in the north-west direction, corresponding to Mach number $1.22\pm 0.06$ and these jumps are associated with the cold fronts. Tricolour map as well as hardness ratio map detects cool gas clumps in the central 30 kpc region of temperature $4.45_{-0.10}^{+0.16}~\mbox{keV}$. The entropy profile derived from the X-ray analysis is found to fall systematically inward in a power-law fashion and exhibits a floor near $12.20\pm 2.54~\mbox{keV}\,\mbox{cm}^{2}$ in the central region. This flattening of the entropy profile in the core region confirms the intermittent heating at the centre by AGN. The diffuse radio emission map at 1.4 GHz using VLA L-band data exhibits highly asymmetric morphology with an edge in the north-west direction coinciding with the X-ray edge seen in the unsharp mask image. The mechanical power injected by the AGN in the form of X-ray cavities is found to be $5.94\times 10^{45}~\mbox{erg}\,\mbox{s}^{-1}$ and is roughly an order of magnitude higher than the energy lost by the ICM in the form of X-ray emission, confirming that AGN feedback is capable enough to quench the cooling flow in this cluster. | ||
| 650 | 4 | |a Galaxies: active |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Galaxies: general |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Galaxies: clusters: individual: Abell 2390 |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Intergalactic medium |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a X-rays: galaxies: clusters |7 (dpeaa)DE-He213 | |
| 700 | 1 | |a Vagshette, N. D. |e verfasserin |4 aut | |
| 700 | 1 | |a Pawar, P. K. |e verfasserin |4 aut | |
| 700 | 1 | |a Patil, M. K. |e verfasserin |4 aut | |
| 773 | 0 | 8 | |i Enthalten in |t Astrophysics and space science |d Dordrecht [u.a.] : Springer Science + Business Media B.V, 1968 |g 359(2015), 2 vom: 25. Sept. |w (DE-627)268755868 |w (DE-600)1472548-4 |x 1572-946X |7 nnns |
| 773 | 1 | 8 | |g volume:359 |g year:2015 |g number:2 |g day:25 |g month:09 |
| 856 | 4 | 0 | |u https://dx.doi.org/10.1007/s10509-015-2508-z |z lizenzpflichtig |3 Volltext |
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10.1007/s10509-015-2508-z doi (DE-627)SPR010603867 (SPR)s10509-015-2508-z-e DE-627 ger DE-627 rakwb eng 520 530 620 ASE 39.00 bkl 39.22 bkl Sonkamble, S. S. verfasserin aut X-ray cavities and temperature jumps in the environment of the strong cool core cluster Abell 2390 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We present results based on the systematic analysis of high resolution 95 ks Chandra observations of the strong cool core cluster Abell 2390 at the redshift of $z = 0.228$ that hosts an energetic radio AGN. This analysis has enabled us to investigate five X-ray deficient cavities in the atmosphere of Abell 2390 within central $30''$. Presence of these cavities have been confirmed through a variety of image processing techniques like, the surface brightness profiles, unsharp masked image, as well as 2D elliptical model subtracted residual map. Temperature profile as well as 2D temperature map revealed structures in the distribution of ICM, in the sense that ICM in the NW direction is cooler than that on the SE direction. Temperature jump in all directions is evident near $25''$ (90.5 kpc) corresponding to the average Mach number $1.44\pm 0.05$, while another jump from 7.47 keV to 9.10 keV at $68''$ (246 kpc) in the north-west direction, corresponding to Mach number $1.22\pm 0.06$ and these jumps are associated with the cold fronts. Tricolour map as well as hardness ratio map detects cool gas clumps in the central 30 kpc region of temperature $4.45_{-0.10}^{+0.16}~\mbox{keV}$. The entropy profile derived from the X-ray analysis is found to fall systematically inward in a power-law fashion and exhibits a floor near $12.20\pm 2.54~\mbox{keV}\,\mbox{cm}^{2}$ in the central region. This flattening of the entropy profile in the core region confirms the intermittent heating at the centre by AGN. The diffuse radio emission map at 1.4 GHz using VLA L-band data exhibits highly asymmetric morphology with an edge in the north-west direction coinciding with the X-ray edge seen in the unsharp mask image. The mechanical power injected by the AGN in the form of X-ray cavities is found to be $5.94\times 10^{45}~\mbox{erg}\,\mbox{s}^{-1}$ and is roughly an order of magnitude higher than the energy lost by the ICM in the form of X-ray emission, confirming that AGN feedback is capable enough to quench the cooling flow in this cluster. Galaxies: active (dpeaa)DE-He213 Galaxies: general (dpeaa)DE-He213 Galaxies: clusters: individual: Abell 2390 (dpeaa)DE-He213 Intergalactic medium (dpeaa)DE-He213 X-rays: galaxies: clusters (dpeaa)DE-He213 Vagshette, N. D. verfasserin aut Pawar, P. K. verfasserin aut Patil, M. K. verfasserin aut Enthalten in Astrophysics and space science Dordrecht [u.a.] : Springer Science + Business Media B.V, 1968 359(2015), 2 vom: 25. Sept. (DE-627)268755868 (DE-600)1472548-4 1572-946X nnns volume:359 year:2015 number:2 day:25 month:09 https://dx.doi.org/10.1007/s10509-015-2508-z lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE 39.22 ASE AR 359 2015 2 25 09 |
| spelling |
10.1007/s10509-015-2508-z doi (DE-627)SPR010603867 (SPR)s10509-015-2508-z-e DE-627 ger DE-627 rakwb eng 520 530 620 ASE 39.00 bkl 39.22 bkl Sonkamble, S. S. verfasserin aut X-ray cavities and temperature jumps in the environment of the strong cool core cluster Abell 2390 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We present results based on the systematic analysis of high resolution 95 ks Chandra observations of the strong cool core cluster Abell 2390 at the redshift of $z = 0.228$ that hosts an energetic radio AGN. This analysis has enabled us to investigate five X-ray deficient cavities in the atmosphere of Abell 2390 within central $30''$. Presence of these cavities have been confirmed through a variety of image processing techniques like, the surface brightness profiles, unsharp masked image, as well as 2D elliptical model subtracted residual map. Temperature profile as well as 2D temperature map revealed structures in the distribution of ICM, in the sense that ICM in the NW direction is cooler than that on the SE direction. Temperature jump in all directions is evident near $25''$ (90.5 kpc) corresponding to the average Mach number $1.44\pm 0.05$, while another jump from 7.47 keV to 9.10 keV at $68''$ (246 kpc) in the north-west direction, corresponding to Mach number $1.22\pm 0.06$ and these jumps are associated with the cold fronts. Tricolour map as well as hardness ratio map detects cool gas clumps in the central 30 kpc region of temperature $4.45_{-0.10}^{+0.16}~\mbox{keV}$. The entropy profile derived from the X-ray analysis is found to fall systematically inward in a power-law fashion and exhibits a floor near $12.20\pm 2.54~\mbox{keV}\,\mbox{cm}^{2}$ in the central region. This flattening of the entropy profile in the core region confirms the intermittent heating at the centre by AGN. The diffuse radio emission map at 1.4 GHz using VLA L-band data exhibits highly asymmetric morphology with an edge in the north-west direction coinciding with the X-ray edge seen in the unsharp mask image. The mechanical power injected by the AGN in the form of X-ray cavities is found to be $5.94\times 10^{45}~\mbox{erg}\,\mbox{s}^{-1}$ and is roughly an order of magnitude higher than the energy lost by the ICM in the form of X-ray emission, confirming that AGN feedback is capable enough to quench the cooling flow in this cluster. Galaxies: active (dpeaa)DE-He213 Galaxies: general (dpeaa)DE-He213 Galaxies: clusters: individual: Abell 2390 (dpeaa)DE-He213 Intergalactic medium (dpeaa)DE-He213 X-rays: galaxies: clusters (dpeaa)DE-He213 Vagshette, N. D. verfasserin aut Pawar, P. K. verfasserin aut Patil, M. K. verfasserin aut Enthalten in Astrophysics and space science Dordrecht [u.a.] : Springer Science + Business Media B.V, 1968 359(2015), 2 vom: 25. Sept. (DE-627)268755868 (DE-600)1472548-4 1572-946X nnns volume:359 year:2015 number:2 day:25 month:09 https://dx.doi.org/10.1007/s10509-015-2508-z lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE 39.22 ASE AR 359 2015 2 25 09 |
| allfields_unstemmed |
10.1007/s10509-015-2508-z doi (DE-627)SPR010603867 (SPR)s10509-015-2508-z-e DE-627 ger DE-627 rakwb eng 520 530 620 ASE 39.00 bkl 39.22 bkl Sonkamble, S. S. verfasserin aut X-ray cavities and temperature jumps in the environment of the strong cool core cluster Abell 2390 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We present results based on the systematic analysis of high resolution 95 ks Chandra observations of the strong cool core cluster Abell 2390 at the redshift of $z = 0.228$ that hosts an energetic radio AGN. This analysis has enabled us to investigate five X-ray deficient cavities in the atmosphere of Abell 2390 within central $30''$. Presence of these cavities have been confirmed through a variety of image processing techniques like, the surface brightness profiles, unsharp masked image, as well as 2D elliptical model subtracted residual map. Temperature profile as well as 2D temperature map revealed structures in the distribution of ICM, in the sense that ICM in the NW direction is cooler than that on the SE direction. Temperature jump in all directions is evident near $25''$ (90.5 kpc) corresponding to the average Mach number $1.44\pm 0.05$, while another jump from 7.47 keV to 9.10 keV at $68''$ (246 kpc) in the north-west direction, corresponding to Mach number $1.22\pm 0.06$ and these jumps are associated with the cold fronts. Tricolour map as well as hardness ratio map detects cool gas clumps in the central 30 kpc region of temperature $4.45_{-0.10}^{+0.16}~\mbox{keV}$. The entropy profile derived from the X-ray analysis is found to fall systematically inward in a power-law fashion and exhibits a floor near $12.20\pm 2.54~\mbox{keV}\,\mbox{cm}^{2}$ in the central region. This flattening of the entropy profile in the core region confirms the intermittent heating at the centre by AGN. The diffuse radio emission map at 1.4 GHz using VLA L-band data exhibits highly asymmetric morphology with an edge in the north-west direction coinciding with the X-ray edge seen in the unsharp mask image. The mechanical power injected by the AGN in the form of X-ray cavities is found to be $5.94\times 10^{45}~\mbox{erg}\,\mbox{s}^{-1}$ and is roughly an order of magnitude higher than the energy lost by the ICM in the form of X-ray emission, confirming that AGN feedback is capable enough to quench the cooling flow in this cluster. Galaxies: active (dpeaa)DE-He213 Galaxies: general (dpeaa)DE-He213 Galaxies: clusters: individual: Abell 2390 (dpeaa)DE-He213 Intergalactic medium (dpeaa)DE-He213 X-rays: galaxies: clusters (dpeaa)DE-He213 Vagshette, N. D. verfasserin aut Pawar, P. K. verfasserin aut Patil, M. K. verfasserin aut Enthalten in Astrophysics and space science Dordrecht [u.a.] : Springer Science + Business Media B.V, 1968 359(2015), 2 vom: 25. Sept. (DE-627)268755868 (DE-600)1472548-4 1572-946X nnns volume:359 year:2015 number:2 day:25 month:09 https://dx.doi.org/10.1007/s10509-015-2508-z lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE 39.22 ASE AR 359 2015 2 25 09 |
| allfieldsGer |
10.1007/s10509-015-2508-z doi (DE-627)SPR010603867 (SPR)s10509-015-2508-z-e DE-627 ger DE-627 rakwb eng 520 530 620 ASE 39.00 bkl 39.22 bkl Sonkamble, S. S. verfasserin aut X-ray cavities and temperature jumps in the environment of the strong cool core cluster Abell 2390 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We present results based on the systematic analysis of high resolution 95 ks Chandra observations of the strong cool core cluster Abell 2390 at the redshift of $z = 0.228$ that hosts an energetic radio AGN. This analysis has enabled us to investigate five X-ray deficient cavities in the atmosphere of Abell 2390 within central $30''$. Presence of these cavities have been confirmed through a variety of image processing techniques like, the surface brightness profiles, unsharp masked image, as well as 2D elliptical model subtracted residual map. Temperature profile as well as 2D temperature map revealed structures in the distribution of ICM, in the sense that ICM in the NW direction is cooler than that on the SE direction. Temperature jump in all directions is evident near $25''$ (90.5 kpc) corresponding to the average Mach number $1.44\pm 0.05$, while another jump from 7.47 keV to 9.10 keV at $68''$ (246 kpc) in the north-west direction, corresponding to Mach number $1.22\pm 0.06$ and these jumps are associated with the cold fronts. Tricolour map as well as hardness ratio map detects cool gas clumps in the central 30 kpc region of temperature $4.45_{-0.10}^{+0.16}~\mbox{keV}$. The entropy profile derived from the X-ray analysis is found to fall systematically inward in a power-law fashion and exhibits a floor near $12.20\pm 2.54~\mbox{keV}\,\mbox{cm}^{2}$ in the central region. This flattening of the entropy profile in the core region confirms the intermittent heating at the centre by AGN. The diffuse radio emission map at 1.4 GHz using VLA L-band data exhibits highly asymmetric morphology with an edge in the north-west direction coinciding with the X-ray edge seen in the unsharp mask image. The mechanical power injected by the AGN in the form of X-ray cavities is found to be $5.94\times 10^{45}~\mbox{erg}\,\mbox{s}^{-1}$ and is roughly an order of magnitude higher than the energy lost by the ICM in the form of X-ray emission, confirming that AGN feedback is capable enough to quench the cooling flow in this cluster. Galaxies: active (dpeaa)DE-He213 Galaxies: general (dpeaa)DE-He213 Galaxies: clusters: individual: Abell 2390 (dpeaa)DE-He213 Intergalactic medium (dpeaa)DE-He213 X-rays: galaxies: clusters (dpeaa)DE-He213 Vagshette, N. D. verfasserin aut Pawar, P. K. verfasserin aut Patil, M. K. verfasserin aut Enthalten in Astrophysics and space science Dordrecht [u.a.] : Springer Science + Business Media B.V, 1968 359(2015), 2 vom: 25. Sept. (DE-627)268755868 (DE-600)1472548-4 1572-946X nnns volume:359 year:2015 number:2 day:25 month:09 https://dx.doi.org/10.1007/s10509-015-2508-z lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE 39.22 ASE AR 359 2015 2 25 09 |
| allfieldsSound |
10.1007/s10509-015-2508-z doi (DE-627)SPR010603867 (SPR)s10509-015-2508-z-e DE-627 ger DE-627 rakwb eng 520 530 620 ASE 39.00 bkl 39.22 bkl Sonkamble, S. S. verfasserin aut X-ray cavities and temperature jumps in the environment of the strong cool core cluster Abell 2390 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We present results based on the systematic analysis of high resolution 95 ks Chandra observations of the strong cool core cluster Abell 2390 at the redshift of $z = 0.228$ that hosts an energetic radio AGN. This analysis has enabled us to investigate five X-ray deficient cavities in the atmosphere of Abell 2390 within central $30''$. Presence of these cavities have been confirmed through a variety of image processing techniques like, the surface brightness profiles, unsharp masked image, as well as 2D elliptical model subtracted residual map. Temperature profile as well as 2D temperature map revealed structures in the distribution of ICM, in the sense that ICM in the NW direction is cooler than that on the SE direction. Temperature jump in all directions is evident near $25''$ (90.5 kpc) corresponding to the average Mach number $1.44\pm 0.05$, while another jump from 7.47 keV to 9.10 keV at $68''$ (246 kpc) in the north-west direction, corresponding to Mach number $1.22\pm 0.06$ and these jumps are associated with the cold fronts. Tricolour map as well as hardness ratio map detects cool gas clumps in the central 30 kpc region of temperature $4.45_{-0.10}^{+0.16}~\mbox{keV}$. The entropy profile derived from the X-ray analysis is found to fall systematically inward in a power-law fashion and exhibits a floor near $12.20\pm 2.54~\mbox{keV}\,\mbox{cm}^{2}$ in the central region. This flattening of the entropy profile in the core region confirms the intermittent heating at the centre by AGN. The diffuse radio emission map at 1.4 GHz using VLA L-band data exhibits highly asymmetric morphology with an edge in the north-west direction coinciding with the X-ray edge seen in the unsharp mask image. The mechanical power injected by the AGN in the form of X-ray cavities is found to be $5.94\times 10^{45}~\mbox{erg}\,\mbox{s}^{-1}$ and is roughly an order of magnitude higher than the energy lost by the ICM in the form of X-ray emission, confirming that AGN feedback is capable enough to quench the cooling flow in this cluster. Galaxies: active (dpeaa)DE-He213 Galaxies: general (dpeaa)DE-He213 Galaxies: clusters: individual: Abell 2390 (dpeaa)DE-He213 Intergalactic medium (dpeaa)DE-He213 X-rays: galaxies: clusters (dpeaa)DE-He213 Vagshette, N. D. verfasserin aut Pawar, P. K. verfasserin aut Patil, M. K. verfasserin aut Enthalten in Astrophysics and space science Dordrecht [u.a.] : Springer Science + Business Media B.V, 1968 359(2015), 2 vom: 25. Sept. (DE-627)268755868 (DE-600)1472548-4 1572-946X nnns volume:359 year:2015 number:2 day:25 month:09 https://dx.doi.org/10.1007/s10509-015-2508-z lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE 39.22 ASE AR 359 2015 2 25 09 |
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Enthalten in Astrophysics and space science 359(2015), 2 vom: 25. Sept. volume:359 year:2015 number:2 day:25 month:09 |
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Galaxies: active Galaxies: general Galaxies: clusters: individual: Abell 2390 Intergalactic medium X-rays: galaxies: clusters |
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Astrophysics and space science |
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Sonkamble, S. S. @@aut@@ Vagshette, N. D. @@aut@@ Pawar, P. K. @@aut@@ Patil, M. K. @@aut@@ |
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Sonkamble, S. S. |
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Sonkamble, S. S. ddc 520 bkl 39.00 bkl 39.22 misc Galaxies: active misc Galaxies: general misc Galaxies: clusters: individual: Abell 2390 misc Intergalactic medium misc X-rays: galaxies: clusters X-ray cavities and temperature jumps in the environment of the strong cool core cluster Abell 2390 |
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520 530 620 ASE 39.00 bkl 39.22 bkl X-ray cavities and temperature jumps in the environment of the strong cool core cluster Abell 2390 Galaxies: active (dpeaa)DE-He213 Galaxies: general (dpeaa)DE-He213 Galaxies: clusters: individual: Abell 2390 (dpeaa)DE-He213 Intergalactic medium (dpeaa)DE-He213 X-rays: galaxies: clusters (dpeaa)DE-He213 |
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ddc 520 bkl 39.00 bkl 39.22 misc Galaxies: active misc Galaxies: general misc Galaxies: clusters: individual: Abell 2390 misc Intergalactic medium misc X-rays: galaxies: clusters |
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X-ray cavities and temperature jumps in the environment of the strong cool core cluster Abell 2390 |
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X-ray cavities and temperature jumps in the environment of the strong cool core cluster Abell 2390 |
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Sonkamble, S. S. |
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Astrophysics and space science |
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Sonkamble, S. S. Vagshette, N. D. Pawar, P. K. Patil, M. K. |
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10.1007/s10509-015-2508-z |
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x-ray cavities and temperature jumps in the environment of the strong cool core cluster abell 2390 |
| title_auth |
X-ray cavities and temperature jumps in the environment of the strong cool core cluster Abell 2390 |
| abstract |
Abstract We present results based on the systematic analysis of high resolution 95 ks Chandra observations of the strong cool core cluster Abell 2390 at the redshift of $z = 0.228$ that hosts an energetic radio AGN. This analysis has enabled us to investigate five X-ray deficient cavities in the atmosphere of Abell 2390 within central $30''$. Presence of these cavities have been confirmed through a variety of image processing techniques like, the surface brightness profiles, unsharp masked image, as well as 2D elliptical model subtracted residual map. Temperature profile as well as 2D temperature map revealed structures in the distribution of ICM, in the sense that ICM in the NW direction is cooler than that on the SE direction. Temperature jump in all directions is evident near $25''$ (90.5 kpc) corresponding to the average Mach number $1.44\pm 0.05$, while another jump from 7.47 keV to 9.10 keV at $68''$ (246 kpc) in the north-west direction, corresponding to Mach number $1.22\pm 0.06$ and these jumps are associated with the cold fronts. Tricolour map as well as hardness ratio map detects cool gas clumps in the central 30 kpc region of temperature $4.45_{-0.10}^{+0.16}~\mbox{keV}$. The entropy profile derived from the X-ray analysis is found to fall systematically inward in a power-law fashion and exhibits a floor near $12.20\pm 2.54~\mbox{keV}\,\mbox{cm}^{2}$ in the central region. This flattening of the entropy profile in the core region confirms the intermittent heating at the centre by AGN. The diffuse radio emission map at 1.4 GHz using VLA L-band data exhibits highly asymmetric morphology with an edge in the north-west direction coinciding with the X-ray edge seen in the unsharp mask image. The mechanical power injected by the AGN in the form of X-ray cavities is found to be $5.94\times 10^{45}~\mbox{erg}\,\mbox{s}^{-1}$ and is roughly an order of magnitude higher than the energy lost by the ICM in the form of X-ray emission, confirming that AGN feedback is capable enough to quench the cooling flow in this cluster. |
| abstractGer |
Abstract We present results based on the systematic analysis of high resolution 95 ks Chandra observations of the strong cool core cluster Abell 2390 at the redshift of $z = 0.228$ that hosts an energetic radio AGN. This analysis has enabled us to investigate five X-ray deficient cavities in the atmosphere of Abell 2390 within central $30''$. Presence of these cavities have been confirmed through a variety of image processing techniques like, the surface brightness profiles, unsharp masked image, as well as 2D elliptical model subtracted residual map. Temperature profile as well as 2D temperature map revealed structures in the distribution of ICM, in the sense that ICM in the NW direction is cooler than that on the SE direction. Temperature jump in all directions is evident near $25''$ (90.5 kpc) corresponding to the average Mach number $1.44\pm 0.05$, while another jump from 7.47 keV to 9.10 keV at $68''$ (246 kpc) in the north-west direction, corresponding to Mach number $1.22\pm 0.06$ and these jumps are associated with the cold fronts. Tricolour map as well as hardness ratio map detects cool gas clumps in the central 30 kpc region of temperature $4.45_{-0.10}^{+0.16}~\mbox{keV}$. The entropy profile derived from the X-ray analysis is found to fall systematically inward in a power-law fashion and exhibits a floor near $12.20\pm 2.54~\mbox{keV}\,\mbox{cm}^{2}$ in the central region. This flattening of the entropy profile in the core region confirms the intermittent heating at the centre by AGN. The diffuse radio emission map at 1.4 GHz using VLA L-band data exhibits highly asymmetric morphology with an edge in the north-west direction coinciding with the X-ray edge seen in the unsharp mask image. The mechanical power injected by the AGN in the form of X-ray cavities is found to be $5.94\times 10^{45}~\mbox{erg}\,\mbox{s}^{-1}$ and is roughly an order of magnitude higher than the energy lost by the ICM in the form of X-ray emission, confirming that AGN feedback is capable enough to quench the cooling flow in this cluster. |
| abstract_unstemmed |
Abstract We present results based on the systematic analysis of high resolution 95 ks Chandra observations of the strong cool core cluster Abell 2390 at the redshift of $z = 0.228$ that hosts an energetic radio AGN. This analysis has enabled us to investigate five X-ray deficient cavities in the atmosphere of Abell 2390 within central $30''$. Presence of these cavities have been confirmed through a variety of image processing techniques like, the surface brightness profiles, unsharp masked image, as well as 2D elliptical model subtracted residual map. Temperature profile as well as 2D temperature map revealed structures in the distribution of ICM, in the sense that ICM in the NW direction is cooler than that on the SE direction. Temperature jump in all directions is evident near $25''$ (90.5 kpc) corresponding to the average Mach number $1.44\pm 0.05$, while another jump from 7.47 keV to 9.10 keV at $68''$ (246 kpc) in the north-west direction, corresponding to Mach number $1.22\pm 0.06$ and these jumps are associated with the cold fronts. Tricolour map as well as hardness ratio map detects cool gas clumps in the central 30 kpc region of temperature $4.45_{-0.10}^{+0.16}~\mbox{keV}$. The entropy profile derived from the X-ray analysis is found to fall systematically inward in a power-law fashion and exhibits a floor near $12.20\pm 2.54~\mbox{keV}\,\mbox{cm}^{2}$ in the central region. This flattening of the entropy profile in the core region confirms the intermittent heating at the centre by AGN. The diffuse radio emission map at 1.4 GHz using VLA L-band data exhibits highly asymmetric morphology with an edge in the north-west direction coinciding with the X-ray edge seen in the unsharp mask image. The mechanical power injected by the AGN in the form of X-ray cavities is found to be $5.94\times 10^{45}~\mbox{erg}\,\mbox{s}^{-1}$ and is roughly an order of magnitude higher than the energy lost by the ICM in the form of X-ray emission, confirming that AGN feedback is capable enough to quench the cooling flow in this cluster. |
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| title_short |
X-ray cavities and temperature jumps in the environment of the strong cool core cluster Abell 2390 |
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S.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">X-ray cavities and temperature jumps in the environment of the strong cool core cluster Abell 2390</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2015</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract We present results based on the systematic analysis of high resolution 95 ks Chandra observations of the strong cool core cluster Abell 2390 at the redshift of $z = 0.228$ that hosts an energetic radio AGN. 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The entropy profile derived from the X-ray analysis is found to fall systematically inward in a power-law fashion and exhibits a floor near $12.20\pm 2.54~\mbox{keV}\,\mbox{cm}^{2}$ in the central region. This flattening of the entropy profile in the core region confirms the intermittent heating at the centre by AGN. The diffuse radio emission map at 1.4 GHz using VLA L-band data exhibits highly asymmetric morphology with an edge in the north-west direction coinciding with the X-ray edge seen in the unsharp mask image. 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