J 2017

Improved measurements of turbulence in the hot gaseous atmospheres of nearby giant elliptical galaxies

OGORZALEK, A., I. ZHURAVLEVA, S. W. ALLEN, C. PINTO, Norbert WERNER et. al.

Basic information

Original name

Improved measurements of turbulence in the hot gaseous atmospheres of nearby giant elliptical galaxies

Authors

OGORZALEK, A. (616 Poland), I. ZHURAVLEVA (643 Russian Federation), S. W. ALLEN (826 United Kingdom of Great Britain and Northern Ireland), C. PINTO (380 Italy), Norbert WERNER (703 Slovakia, guarantor, belonging to the institution), A. MANTZ (840 United States of America), R. CANNING (826 United Kingdom of Great Britain and Northern Ireland), A. C. FABIAN (826 United Kingdom of Great Britain and Northern Ireland), J. S. KAASTRA (528 Netherlands) and J. DE PLAA (528 Netherlands)

Edition

Monthly Notices of the Royal Astronomical Society, Oxford, OXFORD UNIV PRESS, 2017, 0035-8711

Other information

Language

English

Type of outcome

Článek v odborném periodiku

Field of Study

10308 Astronomy

Country of publisher

United Kingdom of Great Britain and Northern Ireland

Confidentiality degree

není předmětem státního či obchodního tajemství

References:

Impact factor

Impact factor: 5.194

RIV identification code

RIV/00216224:14310/17:00099804

Organization unit

Faculty of Science

DOI

UT WoS

000413082900032

Keywords in English

radiative transfer; turbulence; techniques: spectroscopic; galaxies: clusters: intracluster medium; galaxies: kinematics and dynamics; X-rays: galaxies: clusters

Tags

Změněno: 10/11/2022 13:06, Mgr. Marie Šípková, DiS.

Abstract

V originále

We present significantly improved measurements of turbulent velocities in the hot gaseous haloes of nearby giant elliptical galaxies. Using deep XMM-Newton Reflection Grating Spectrometer (RGS) observations and a combination of resonance scattering and direct line broadening methods, we obtain well bounded constraints for 13 galaxies. Assuming that the turbulence is isotropic, we obtain a best-fitting mean 1D turbulent velocity of similar to 110 km s(-1). This implies a typical 3D Mach number similar to 0.45 and a typical non-thermal pressure contribution of similar to 6 per cent in the cores of nearby massive galaxies. The intrinsic scatter around these values is modest-consistent with zero, albeit with large statistical uncertainty-hinting at a common and quasi-continuous mechanism sourcing the velocity structure in these objects. Using conservative estimates of the spatial scales associated with the observed turbulent motions, we find that turbulent heating can be sufficient to offset radiative cooling in the inner regions of these galaxies (< 10 kpc, typically 2-3 kpc). The full potential of our analysis methods will be enabled by future X-ray micro-calorimeter observations.