S. Ettori

Chandra imaging of the complex X-ray core of the Perseus cluster

ABSTRACT We report subarcsec-resolution X-ray imaging of the core ofthe Perseus cluster around thegalaxy NGC1275 with the Chandra X-ray Observatory. The ROSAT-discovered holes asso-ciated with the radio lobes have X-ray bright rims which are cooler than the surrounding gasand not due to shocks. The holes themselves may contain some hotter gas. We map strongphotoelectric absorption across the Northern lobe and rim due to a small infalling irregulargalaxy, known as the high velocity system. Two outer holes, one of which was previouslyknown, are identified with recently found spurs of low-frequency radio emission. The spiralappearance of the X-ray cooler gas and the outer optical parts of NGC1275 may be due toangular momentum in the cooling flow.Key words: galaxies: individual: Perseus – cooling flows – galaxies: in dividual: NGC1275– X-rays: galaxies 1 INTRODUCTIONThe Perseus cluster, Abell426, at a redshift z = 0.0183 or dis-tance about 100 Mpc is the brightest cluster in the sky in X-rays. Ithosts the nearest large cooling flow (e.g. Fabian et al 1981; A llenet al 1990; Fabian et al 1994). X-ray analysis of ASCA spectrain-dicates that the mass deposition rate is about 300M

Deep inside the core of Abell 1795: the Chandra view

We present X-ray spatial and spectral analysis of the Chandra data from the central of the cluster of galaxies Abell 1795. The plasma temperature rises outwards by a factor of 3, whereas the iron abundance decreases by a factor of 4. The spatial distribution of oxygen, neon, sulphur, silicon and iron shows that supernovae Type Ia dominate the metal enrichment process of the cluster plasma within the inner 150xa0kpc. Resolving both the gas density and temperature in nine radial bins, we recover the gravitational mass density profile and show that it flattens within 100xa0kpc as ρDM∝r-0.6 with a power-law index flatter than −1 at >3σ level. The observed motion of the central galaxy and the presence of excesses and deficits along the north–south direction in the brightness distribution indicate that the central cluster region is not relaxed. In the absence of any non-gravitational heating source, the data from the inner ∼200xa0kpc indicate the presence of a cooling flow with an integrated mass deposition rate of about 100xa0M⊙xa0yr−1. Over the same cluster region, the observed rate of 74xa0M⊙xa0yr−1 is consistent with the recent XMM-Newton Reflection Grating Spectrometer limit of 150xa0M⊙xa0yr−1.

Scaling laws in X-ray galaxy clusters at redshift between 0.4 and 1.3

We present a study of the integrated physical properties of a sample of 28xa0X-ray galaxy clusters observed with Chandra u2000at a redshift betweenxa00.4 andxa01.3. In particular, we have twelve objects in the redshift range 0.4–0.6, five betweenxa00.6 andxa00.8, seven between 0.8 and 1 and four at

On the Iron content in rich nearby Clusters of Galaxies

z>1.0

Chandra measurements of the distribution of mass in the luminous lensing cluster Abell 2390

, compounding the largest sample available for such a study. We focus particularly on the properties and evolution of the X-ray scaling laws. We fit both a single and a double

Chandra imaging of the X-ray core of Abell 1795

beta-

Testing the connection between the X-ray and submillimetre source populations using Chandra

model with the former which provides a good representation of the observed surface brightness profiles, indicating that these clusters do not show any significant excess in their central brightness. By using the best-fit parameters of the

Mass profiles and concentration-dark matter relation in X-ray luminous galaxy clusters

beta-

Chandra X-ray observations of the 3C 295 cluster core

model together with the measured emission-weighted temperature (in the range 3–11xa0keV), we recover gas luminosity, gas mass and total gravitating mass out toxa0 R 500 . We observe scaling relations steeper than expected from the self-similar model by a significant (>

The XXL Survey I. Scientific motivations - XMM-Newton observing plan - Follow-up observations and simulation programme

3 sigma