XRISM velocity maps of Abell 3571 show subsonic gas motions and thermodynamic asymmetry consistent with early-phase sloshing from an off-axis minor merger with Abell 3572 as candidate perturber.
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14 Pith papers cite this work, alongside 51 external citations. Polarity classification is still indexing.
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Time-resolved XRISM spectroscopy of NGC 4395 reveals variable inner-disk Fe Kα emission interpreted as Lense-Thirring precession, favoring low black hole mass (~9e3 solar masses) and moderate spin (a≳0.6).
XRISM observations of Abell 1795 show line-of-sight velocity dispersion falling from 114 km/s in the core to 68 km/s at 320 kpc, near-zero bulk velocities, multiphase gas, and 14% resonant suppression of the Fe XXV w line.
Phase-resolved high-resolution spectroscopy of M82 X-2 with XRISM Resolve finds broader Fe Kα line during pulse peak, indicating origin in the accretion flow with velocity dispersion of about 1700 km/s.
XRISM/Resolve data on Mrk 509 show a tentative 3.6-sigma infalling absorber at 11000 km/s located within thousands of gravitational radii, interpreted as raining clumps from a failed wind.
XRISM spectroscopy of AM Herculis reveals bulk velocity and temperature gradients in the radiative cooling accretion column, with derived shock temperature of 24 keV, velocity of 1116 km/s, and density of 5-6 x 10^15 cm^-3.
XRISM observations show the core of Abell 2199 is kinematically coherent with low turbulence, where turbulent heating may offset ~20% of radiative cooling losses.
XRISM multi-epoch spectra of NGC 4151 yield a 3.5-day lag in the narrow Fe Kα line flux, consistent with a broad-line-region origin and giving M_BH/f_X ≈ 2×10^7 solar masses.
XRISM spectroscopy of NGC 4388 shows the Fe Kα line arising from the torus, inner torus edge, and BLR at distinct radii, with absorption revealing a gravitationally bound failed wind.
BLiSS blindly detects, ranks, and optionally identifies emission-line candidates in 1D X-ray spectra via empirical baselines, Gaussian fits, and GMM reliability scores from synthetic null spectra.
TNG-Cluster simulations find that in galaxy cluster centers turbulence accounts for under half the total velocity dispersion (typically 50-75 km/s), is mostly subsonic, provides sub-percent pressure support, and is primarily driven by SMBH feedback.
XRISM observation of 3C 111 finds weak Fe Kβ possibly caused by blueshifted absorption from an ionized wind at 4600 or 17200 km/s, with kinetic power 10^41-10^44 erg/s smaller than the jet power.
XRISM measurements indicate turbulent dissipation from jets struggles to balance cooling in cluster atmospheres except possibly in limited inner regions of systems like Hydra A.
XRISM kinematics measurements in A3571 find low uniform velocity dispersion whose implied turbulent heating offsets cooling, with sloshing as a major contributor.
citing papers explorer
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Sloshing Motions in Abell 3571 Revealed by XRISM/Resolve Velocity Mapping
XRISM velocity maps of Abell 3571 show subsonic gas motions and thermodynamic asymmetry consistent with early-phase sloshing from an off-axis minor merger with Abell 3572 as candidate perturber.
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XRISM Time-resolved Fe K$\alpha$ Spectroscopy of NGC 4395: Time-variable Inner-disk Emission
Time-resolved XRISM spectroscopy of NGC 4395 reveals variable inner-disk Fe Kα emission interpreted as Lense-Thirring precession, favoring low black hole mass (~9e3 solar masses) and moderate spin (a≳0.6).
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XRISM Observations of Abell 1795: Evidence for Low Turbulence and Resonant Scattering
XRISM observations of Abell 1795 show line-of-sight velocity dispersion falling from 114 km/s in the core to 68 km/s at 320 kpc, near-zero bulk velocities, multiphase gas, and 14% resonant suppression of the Fe XXV w line.
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The First Insights into an Ultraluminous X-ray Pulsar with XRISM: Phase-Resolved High-Resolution Spectroscopy of the Fe K-shell Band of M82 X-2
Phase-resolved high-resolution spectroscopy of M82 X-2 with XRISM Resolve finds broader Fe Kα line during pulse peak, indicating origin in the accretion flow with velocity dispersion of about 1700 km/s.
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Is XRISM/Resolve probing a "raining" absorber in Mrk 509?
XRISM/Resolve data on Mrk 509 show a tentative 3.6-sigma infalling absorber at 11000 km/s located within thousands of gravitational radii, interpreted as raining clumps from a failed wind.
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Plasma Dynamics of Radiative Cooling Accretion Flow in AM Herculis with XRISM
XRISM spectroscopy of AM Herculis reveals bulk velocity and temperature gradients in the radiative cooling accretion column, with derived shock temperature of 24 keV, velocity of 1116 km/s, and density of 5-6 x 10^15 cm^-3.
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XRISM Reveals a Kinematically Coherent Core System of the Nearby Cool-Core Cluster Abell 2199
XRISM observations show the core of Abell 2199 is kinematically coherent with low turbulence, where turbulent heating may offset ~20% of radiative cooling losses.
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Reverberation in the Narrow Fe K${\alpha}$ Line in the Seyfert Galaxy NGC 4151 with XRISM
XRISM multi-epoch spectra of NGC 4151 yield a 3.5-day lag in the narrow Fe Kα line flux, consistent with a broad-line-region origin and giving M_BH/f_X ≈ 2×10^7 solar masses.
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Complex Nuclear Structure in Seyfert 2 Galaxy NGC 4388 Revealed by XRISM Observation
XRISM spectroscopy of NGC 4388 shows the Fe Kα line arising from the torus, inner torus edge, and BLR at distinct radii, with absorption revealing a gravitationally bound failed wind.
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Blind Line Search System: BLiSS
BLiSS blindly detects, ranks, and optionally identifies emission-line candidates in 1D X-ray spectra via empirical baselines, Gaussian fits, and GMM reliability scores from synthetic null spectra.
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Bulk vs. turbulent motions at the centres of galaxy clusters: AGN-driven turbulence according to TNG-Cluster
TNG-Cluster simulations find that in galaxy cluster centers turbulence accounts for under half the total velocity dispersion (typically 50-75 km/s), is mostly subsonic, provides sub-percent pressure support, and is primarily driven by SMBH feedback.
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A Weak Fe K$\beta$ Emission Line in the Broad-Line Radio Galaxy 3C 111 Observed with XRISM: An Ionized Wind Absorption Feature?
XRISM observation of 3C 111 finds weak Fe Kβ possibly caused by blueshifted absorption from an ionized wind at 4600 or 17200 km/s, with kinetic power 10^41-10^44 erg/s smaller than the jet power.
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Are X-ray Atmospheres Heated by Turbulent Dissipation? XRISM Constraints
XRISM measurements indicate turbulent dissipation from jets struggles to balance cooling in cluster atmospheres except possibly in limited inner regions of systems like Hydra A.
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Kinematics of Weak Cool-Core Cluster A3571 Observed with XRISM: Low Cooling Rate Balanced by Low Heating Rate
XRISM kinematics measurements in A3571 find low uniform velocity dispersion whose implied turbulent heating offsets cooling, with sloshing as a major contributor.