Irina Zhuravleva
Phys Sci Res Assoc, Kavli Institute for Particle Astrophysics and Cosmology
Academic Appointments
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Phys Sci Res Assoc, Kavli Institute for Particle Astrophysics and Cosmology
Honors & Awards
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The Ernest Rutherford Fellowship, STFC (June 2016)
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The Otto Hahn Medal, Max Planck Society (May 2013)
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International Max Planck Research School fellowship, Max Planck Institute for Astrophysics (Sep 2008)
Current Research and Scholarly Interests
High-energy astrophysics, physics of intracluster medium, AGN feedback, turbulence, transport processes, high-resolution X-ray spectroscopy, radiative transfer
All Publications
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Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster
ASTROPHYSICAL JOURNAL LETTERS
2017; 837 (1)
View details for DOI 10.3847/2041-8213/aa61fa
View details for Web of Science ID 000396122600001
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Arithmetic with X-ray images of galaxy clusters: effective equation of state for small-scale perturbations in the ICM
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2016; 463 (1): 1057-1067
View details for DOI 10.1093/mnras/stw2044
View details for Web of Science ID 000386464900082
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Insights into the location and dynamics of the coolest X-ray emitting gas in clusters of galaxies
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2016; 461 (2): 2077-2084
View details for DOI 10.1093/mnras/stw1444
View details for Web of Science ID 000383273600070
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Deep Chandra study of the truncated cool core of the Ophiuchus cluster
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2016; 460 (3): 2752-2764
View details for DOI 10.1093/mnras/stw1171
View details for Web of Science ID 000381204600036
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The quiescent intracluster medium in the core of the Perseus cluster
NATURE
2016; 535 (7610): 117-?
Abstract
Clusters of galaxies are the most massive gravitationally bound objects in the Universe and are still forming. They are thus important probes of cosmological parameters and many astrophysical processes. However, knowledge of the dynamics of the pervasive hot gas, the mass of which is much larger than the combined mass of all the stars in the cluster, is lacking. Such knowledge would enable insights into the injection of mechanical energy by the central supermassive black hole and the use of hydrostatic equilibrium for determining cluster masses. X-rays from the core of the Perseus cluster are emitted by the 50-million-kelvin diffuse hot plasma filling its gravitational potential well. The active galactic nucleus of the central galaxy NGC 1275 is pumping jetted energy into the surrounding intracluster medium, creating buoyant bubbles filled with relativistic plasma. These bubbles probably induce motions in the intracluster medium and heat the inner gas, preventing runaway radiative cooling--a process known as active galactic nucleus feedback. Here we report X-ray observations of the core of the Perseus cluster, which reveal a remarkably quiescent atmosphere in which the gas has a line-of-sight velocity dispersion of 164 ± 10 kilometres per second in the region 30-60 kiloparsecs from the central nucleus. A gradient in the line-of-sight velocity of 150 ± 70 kilometres per second is found across the 60-kiloparsec image of the cluster core. Turbulent pressure support in the gas is four per cent of the thermodynamic pressure, with large-scale shear at most doubling this estimate. We infer that a total cluster mass determined from hydrostatic equilibrium in a central region would require little correction for turbulent pressure.
View details for DOI 10.1038/nature18627
View details for Web of Science ID 000379015600035
View details for PubMedID 27383985
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The nature and energetics of AGN-driven perturbations in the hot gas in the Perseus Cluster
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2016; 458 (3): 2902-2915
View details for DOI 10.1093/mnras/stw520
View details for Web of Science ID 000375799000046
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ON THE NATURE OF X-RAY SURFACE BRIGHTNESS FLUCTUATIONS IN M87
ASTROPHYSICAL JOURNAL
2016; 818 (1)
View details for DOI 10.3847/0004-637X/818/1/14
View details for Web of Science ID 000370370800014
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MAPPING THE GAS TURBULENCE IN THE COMA CLUSTER: PREDICTIONS FOR ASTRO-H
ASTROPHYSICAL JOURNAL
2016; 817 (2)
View details for DOI 10.3847/0004-637X/817/2/110
View details for Web of Science ID 000369437900027
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Deep Chandra observation and numerical studies of the nearest cluster cold front in the sky
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2016; 455 (1): 846-858
View details for DOI 10.1093/mnras/stv2358
View details for Web of Science ID 000368005900091
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A UNIFORM CONTRIBUTION OF CORE-COLLAPSE AND TYPE Ia SUPERNOVAE TO THE CHEMICAL ENRICHMENT PATTERN IN THE OUTSKIRTS OF THE VIRGO CLUSTER
ASTROPHYSICAL JOURNAL LETTERS
2015; 811 (2)
View details for DOI 10.1088/2041-8205/811/2/L25
View details for Web of Science ID 000364478600011
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Gas density fluctuations in the Perseus Cluster: clumping factor and velocity power spectrum
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2015; 450 (4): 4184-4197
View details for DOI 10.1093/mnras/stv900
View details for Web of Science ID 000360824000062
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Gas density fluctuations in the Perseus Cluster: clumping factor and velocity power spectrum
Monthly Notices of the Royal Astronomical Society
2015; 450 (4): 13
View details for DOI 10.1093/mnras/stv900
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Turbulent heating in galaxy clusters brightest in X-rays
NATURE
2014; 515 (7525): 85-?
View details for DOI 10.1038/nature13830
View details for Web of Science ID 000344187500033
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Turbulent heating in galaxy clusters brightest in X-rays.
Nature
2014; 515 (7525): 85-87
Abstract
The hot (10(7) to 10(8) kelvin), X-ray-emitting intracluster medium (ICM) is the dominant baryonic constituent of clusters of galaxies. In the cores of many clusters, radiative energy losses from the ICM occur on timescales much shorter than the age of the system. Unchecked, this cooling would lead to massive accumulations of cold gas and vigorous star formation, in contradiction to observations. Various sources of energy capable of compensating for these cooling losses have been proposed, the most promising being heating by the supermassive black holes in the central galaxies, through inflation of bubbles of relativistic plasma. Regardless of the original source of energy, the question of how this energy is transferred to the ICM remains open. Here we present a plausible solution to this question based on deep X-ray data and a new data analysis method that enable us to evaluate directly the ICM heating rate from the dissipation of turbulence. We find that turbulent heating is sufficient to offset radiative cooling and indeed appears to balance it locally at each radius-it may therefore be the key element in resolving the gas cooling problem in cluster cores and, more universally, in the atmospheres of X-ray-emitting, gas-rich systems on scales from galaxy clusters to groups and elliptical galaxies.
View details for DOI 10.1038/nature13830
View details for PubMedID 25363764
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The relation between gas density and velocity power spectra in galaxy clusters: High-resolution hydrodynamic simulations and the role of conduction
ASTRONOMY & ASTROPHYSICS
2014; 569
View details for DOI 10.1051/0004-6361/201424043
View details for Web of Science ID 000343092100088
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Stellar kinematics of X-ray bright massive elliptical galaxies
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2014; 441 (3): 2013-2033
View details for DOI 10.1093/mnras/stu717
View details for Web of Science ID 000338763600015
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THE RELATION BETWEEN GAS DENSITY AND VELOCITY POWER SPECTRA IN GALAXY CLUSTERS: QUALITATIVE TREATMENT AND COSMOLOGICAL SIMULATIONS
ASTROPHYSICAL JOURNAL LETTERS
2014; 788 (1)
View details for DOI 10.1088/2041-8205/788/1/L13
View details for Web of Science ID 000337134100005
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Azimuthally resolved X-ray spectroscopy to the edge of the Perseus Cluster
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2014; 437 (4): 3939-3961
View details for DOI 10.1093/mnras/stt2209
View details for Web of Science ID 000329177100072
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Resonant scattering in the Perseus Cluster: spectral model for constraining gas motions with Astro-H
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2013; 435 (4): 3111-3121
View details for DOI 10.1093/mnras/stt1506
View details for Web of Science ID 000325774700027
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DEEP CHANDRA OBSERVATIONS OF A2199: THE INTERPLAY BETWEEN MERGER-INDUCED GAS MOTIONS AND NUCLEAR OUTBURSTS IN A COOL CORE CLUSTER
ASTROPHYSICAL JOURNAL
2013; 775 (2)
View details for DOI 10.1088/0004-637X/775/2/117
View details for Web of Science ID 000324734400037
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Bias from gas inhomogeneities in the pressure profiles as measured from X-ray and Sunyaev-Zeldovich observations
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2013; 431 (1): 954-965
View details for DOI 10.1093/mnras/stt224
View details for Web of Science ID 000318343600095
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Quantifying properties of ICM inhomogeneities
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2013; 428 (4): 3274-3287
View details for DOI 10.1093/mnras/sts275
View details for Web of Science ID 000318232000038
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A Mexican hat with holes: calculating low-resolution power spectra from data with gaps
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2012; 426 (3): 1793-1807
View details for DOI 10.1111/j.1365-2966.2012.21789.x
View details for Web of Science ID 000310063900008
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CHANDRA OBSERVATIONS OF NGC 4342, AN OPTICALLY FAINT, X-RAY GAS-RICH EARLY-TYPE GALAXY
ASTROPHYSICAL JOURNAL
2012; 755 (1)
View details for DOI 10.1088/0004-637X/755/1/25
View details for Web of Science ID 000306909500025
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EXPLORING THE UNUSUALLY HIGH BLACK-HOLE-TO-BULGE MASS RATIOS IN NGC 4342 AND NGC 4291: THE ASYNCHRONOUS GROWTH OF BULGES AND BLACK HOLES
ASTROPHYSICAL JOURNAL
2012; 753 (2)
View details for DOI 10.1088/0004-637X/753/2/140
View details for Web of Science ID 000305912700047
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Testing a simple recipe for estimating galaxy masses from minimal observational data
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2012; 423 (2): 1813-1824
View details for DOI 10.1111/j.1365-2966.2012.21004.x
View details for Web of Science ID 000305070900063
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Constraints on the ICM velocity power spectrum from the X-ray lines width and shift
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2012; 422 (3): 2712-2724
View details for DOI 10.1111/j.1365-2966.2012.20844.x
View details for Web of Science ID 000303858400073
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X-ray surface brightness and gas density fluctuations in the Coma cluster
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2012; 421 (2): 1123-1135
View details for DOI 10.1111/j.1365-2966.2011.20372.x
View details for Web of Science ID 000302695600016
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Estimating turbulent velocities in the elliptical galaxies NGC 5044 and NGC 5813
ASTRONOMY & ASTROPHYSICS
2012; 539
View details for DOI 10.1051/0004-6361/201118404
View details for Web of Science ID 000303262000041
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Resonant scattering in galaxy clusters for anisotropic gas motions on various spatial scales
ASTRONOMY LETTERS-A JOURNAL OF ASTRONOMY AND SPACE ASTROPHYSICS
2011; 37 (3): 141-153
View details for DOI 10.1134/S1063773711010087
View details for Web of Science ID 000288121300001
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Steepening mass profiles, dark matter and environment of X-ray bright elliptical galaxies
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2010; 409 (4): 1362-1378
View details for DOI 10.1111/j.1365-2966.2010.17417.x
View details for Web of Science ID 000284963800005
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Resonant Scattering of X-ray Emission Lines in the Hot Intergalactic Medium
SPACE SCIENCE REVIEWS
2010; 157 (1-4): 193-209
View details for DOI 10.1007/s11214-010-9685-4
View details for Web of Science ID 000288172200013
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Polarization of X-ray lines from galaxy clusters and elliptical galaxies - a way to measure the tangential component of gas velocity
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2010; 403 (1): 129-150
View details for DOI 10.1111/j.1365-2966.2009.16148.x
View details for Web of Science ID 000276351600028
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Constraints on turbulent pressure in the X-ray haloes of giant elliptical galaxies from resonant scattering
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2009; 398 (1): 23-32
View details for DOI 10.1111/j.1365-2966.2009.14860.x
View details for Web of Science ID 000269136800020
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The Sunyaev-Zel'dovich effect in elliptical galaxies
ASTRONOMY REPORTS
2008; 52 (9): 707-713
View details for DOI 10.1134/S1063772908090023
View details for Web of Science ID 000259040500002