Spatially resolved X-ray spectroscopy of cooling clusters of galaxies

Kaastra, J. S.; Tamura, Takayuki; Peterson, J. R.; Bleeker, J. A. M.; Ferrigno, C.; Kahn, S. M.; Paerels, F.; Piffaretti, R.; Branduardi‐Raymont, G.; Böhringer, H.

doi:10.1051/0004-6361:20031512

Cited by 214 publications

(309 citation statements)

References 60 publications

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“…XMM-Newton and Chandra have revealed evidence for an active history of interaction between the AGN and ICM in the core of 2A 0335+096. X-ray observations show a complex system of X-ray-emitting structures in the core, including filaments, cool clumps, a metal-rich spiral, and at least five distinct cavities at varying distances and position angles relative to the central galaxy (Mazzotta et al 2003;Bîrzan et al 2004;Kaastra et al 2004;Sanders et al 2009). The total 4pV enthalpy associated with the five cavities is estimated to be 5 × 10 59 erg (Sanders et al 2009).…”

Section: A 0335+096mentioning

confidence: 99%

LOFAR MSSS: The scaling relation between AGN cavity power and radio luminosity at low radio frequencies

Kokotanekov

Wise

Heald

et al. 2017

A&A

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We present a new analysis of the widely used relation between cavity power and radio luminosity in clusters of galaxies with evidence for strong AGN feedback. We study the correlation at low radio frequencies using two new surveys -the First Alternative Data Release of the TIFR GMRT Sky Survey (TGSS ADR1) at 148 MHz and LOFAR's first all-sky survey, the Multifrequency Snapshot Sky Survey (MSSS) at 140 MHz. We find a scaling relation P cav ∝ L β 148 , with a logarithmic slope of β = 0.51 ± 0.14, which is in good agreement with previous results based on data at 327 MHz. The large scatter present in this correlation confirms the conclusion reached at higher frequencies that the total radio luminosity at a single frequency is a poor predictor of the total jet power. Previous studies have shown that the magnitude of this scatter can be reduced when bolometric radio luminosity corrected for spectral aging is used. We show that including additional measurements at 148 MHz alone is insufficient to improve this correction and further reduce the scatter in the correlation. For a subset of four well-resolved sources, we examine the detected extended structures at low frequencies and compare with the morphology known from higher frequency images and Chandra X-ray maps. In Perseus we discuss details in the structures of the radio mini-halo, while in the 2A 0335+096 cluster we observe new diffuse emission associated with multiple X-ray cavities and likely originating from past activity. For A2199 and MS 0735.6+7421, we confirm that the observed low-frequency radio lobes are confined to the extents known from higher frequencies. This new low-frequency analysis highlights the fact that existing cavity power to radio luminosity relations are based on a relatively narrow range of AGN outburst ages. We discuss how the correlation could be extended using low frequency data from the LOFAR Two-metre Sky Survey (LoTSS) in combination with future, complementary deeper X-ray observations.

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Section: A 0335+096mentioning

confidence: 99%

LOFAR MSSS: The scaling relation between AGN cavity power and radio luminosity at low radio frequencies

Kokotanekov

Wise

Heald

et al. 2017

A&A

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“…Therefore, we need multi-temperature models to constrain temperature structures and abundances correctly (e.g. Peterson et al 2003;Kaastra et al 2004). Knowing this, it is remarkable that NGC 5813 shows a single-temperature spectrum in RGS.…”

Section: Temperature Structurementioning

confidence: 99%

The metal contents of two groups of galaxies

Grange

Plaa

Kaastra

et al. 2011

A&A

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Context. The hot gas in clusters and groups of galaxies is continuously being enriched with metals from supernovae and stars. It is well established that the enrichment of the gas with elements from oxygen to iron is mainly caused by supernova explosions. The origins of nitrogen and carbon are still being debated. Possible candidates include massive, metal-rich stars, early generations of massive stars, intermediate-or low-mass stars and asymptotic giant branch (AGB) stars. Aims. In this paper we accurately determine the metal abundances of the gas in the groups of galaxies NGC 5044 and NGC 5813, and discuss the nature of the objects that create these metals. We mainly focus on carbon and nitrogen. Methods. We use spatially-resolved high-resolution X-ray spectroscopy from XMM-Newton. For the spectral fitting, multitemperature hot gas models are used. Results. The abundance ratios of carbon over oxygen and nitrogen over oxygen that we find are high compared to the ratios in the stars in the disk of our Galaxy. The oxygen and nitrogen abundances we derive are similar to what has been found in earlier work on other giant ellipticals in comparable environments. We show that the iron abundances in both our sources have a gradient along the cross-dispersion direction of the reflection grating spectrometer (RGS). Conclusions. We conclude that it is unlikely that the creation of nitrogen and carbon takes place in massive stars, which end their lives as core-collapse supernovae, enriching the medium with oxygen because oxygen should then also be enhanced. Therefore we favour low-and intermediate-mass stars as sources of these elements. The abundances in the hot gas can be explained best by a 30-40% contribution of type Ia supernovae based on the measured oxygen and iron abundances and under the assumption of a Salpeter initial mass function (IMF).

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“…Biffi et al 2011;Lau et al 2009;Vazza et al 2009Vazza et al , 2011Dolag et al 2005), emission measure distribution of the emitting gas (discussed in observational studies by, e.g., Peterson et al 2003;Kaastra et al 2004; and via mock observations of simulated clusters, e.g. Biffi et al 2012).…”

Section: Discussionmentioning

confidence: 99%

Observing simulated galaxy clusters: The prospects of ICM velocity diagnostics

2013

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Non-thermal motions in the intra-cluster medium (ICM) are believed to play a non-negligible role in the pressure support to the total gravitating mass of galaxy clusters. Future high-precision X-ray missions will allow us to directly detect the signature of these motions from highly resolved spectra of the ICM. With this perspective, we will present here a study on a set of clusters extracted from a cosmological hydrodynamical simulation, for which we simulated X-ray observations and characterized them via the non-thermal velocity amplitude of the ICM. We have applied the X-ray virtual telescope PHOX to generate mock observations of the simulated clusters and estimated in an observational fashion global X-ray properties. We included ICM non-thermal motions as additional parameter to further identify non-regular clusters. In particular, the influence of internal gas motions on the location of clusters in the LX-T plane was investigated and was found that objects with the largest amount of non-thermal velocity have on average higher X-ray luminosities.

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Spatially resolved X-ray spectroscopy of cooling clusters of galaxies

Cited by 214 publications

References 60 publications

LOFAR MSSS: The scaling relation between AGN cavity power and radio luminosity at low radio frequencies

LOFAR MSSS: The scaling relation between AGN cavity power and radio luminosity at low radio frequencies

The metal contents of two groups of galaxies

Observing simulated galaxy clusters: The prospects of ICM velocity diagnostics

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