ABUNDANCE PATTERNS IN THE INTERSTELLAR MEDIUM OF EARLY-TYPE GALAXIES OBSERVED WITH<i>SUZAKU</i>

Konami, Saori; Matsushita, Kyoko; Nagino, Ryo; Tamagawa, Toru

doi:10.1088/0004-637x/783/1/8

Cited by 14 publications

(24 citation statements)

References 82 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…These new results contradict previous papers (e.g. Rasmussen & Ponman 2009;Bregman et al 2010;Sun 2012;Yates et al 2017), which reported systematically lower Fe abundances in groups and/or ellipticals with respect to the hotter clusters of galaxies (although Konami et al (2014) reported similar average Fe abundances as reported here, albeit for ellipticals only). Rather than spex, most of those previous studies used many (very different) versions of apec to fit their data, making a direct comparison with this work difficult.…”

Section: Implications For the Iron Content In Ellipticals Groups Andcontrasting

confidence: 74%

Mass-invariance of the iron enrichment in the hot haloes of massive ellipticals, groups, and clusters of galaxies

Mernier

Plaa

Werner

et al. 2018

Monthly Notices of the Royal Astronomical Society: Letters

View full text Add to dashboard Cite

X-ray measurements find systematically lower Fe abundances in the X-ray emitting haloes pervading groups (kT 1.7 keV) than in clusters of galaxies. These results have been difficult to reconcile with theoretical predictions. However, models using incomplete atomic data or the assumption of isothermal plasmas may have biased the best fit Fe abundance in groups and giant elliptical galaxies low. In this work, we take advantage of a major update of the atomic code in the spectral fitting package spex to re-evaluate the Fe abundance in 43 clusters, groups, and elliptical galaxies (the CHEERS sample) in a self-consistent analysis and within a common radius of 0.1r 500 . For the first time, we report a remarkably similar average Fe enrichment in all these systems. Unlike previous results, this strongly suggests that metals are synthesised and transported in these haloes with the same average efficiency across two orders of magnitude in total mass. We show that the previous metallicity measurements in low temperature systems were biased low due to incomplete atomic data in the spectral fitting codes. The reasons for such a code-related Fe bias, also implying previously unconsidered biases in the emission measure and temperature structure, are discussed.

show abstract

Section: Implications For the Iron Content In Ellipticals Groups Andcontrasting

confidence: 74%

Mass-invariance of the iron enrichment in the hot haloes of massive ellipticals, groups, and clusters of galaxies

Mernier

Plaa

Werner

et al. 2018

Monthly Notices of the Royal Astronomical Society: Letters

View full text Add to dashboard Cite

show abstract

“…The next generation of X-ray observatories, including Chandra, XMM-Newton and Suzaku, considerably increased the accuracy of these measurements (see e.g. Böhringer et al 2001;Molendi and Gastaldello 2001;Finoguenov et al 2002;Buote et al 2003;Sanders and Fabian 2006a;Werner et al 2006b;de Plaa et al 2006;de Plaa et al 2007;Rasmussen and Ponman 2007;Simionescu et al 2009;De Grandi and Molendi 2009;Bulbul et al 2012;Sasaki et al 2014;Konami et al 2014;Mernier et al , 2016aThölken et al 2016). The Reflection Grating Spectrometer (RGS) instrument onboard XMM-Newton allowed to formally identify C (Werner et al 2006a), N, and Ne (Xu et al 2002) emission lines in the ICM.…”

Section: Metals In the Icm: A Brief Historymentioning

confidence: 99%

Enrichment of the Hot Intracluster Medium: Observations

et al. 2018

View full text Add to dashboard Cite

Four decades ago, the firm detection of an Fe-K emission feature in the X-ray spectrum of the Perseus cluster revealed the presence of iron in its hot intracluster medium (ICM). With more advanced missions successfully launched over the last 20 years, this discovery has been extended to many other metals and to the hot atmospheres of many other galaxy clusters, groups, and giant elliptical galaxies, as evidence that the elemental bricks of life -synthesized by stars and supernovae -are also found at the largest scales of the Universe. Because the ICM, emitting in X-rays, is in collisional ionisation equilibrium, its elemental abundances can in principle be accurately measured. These abundance measurements, in turn, are valuable to constrain the physics and environmental conditions of the Type Ia and core-collapse supernovae that exploded and enriched the ICM over the entire cluster volume. On the other hand, the spatial distribution of metals across the ICM constitutes a remarkable signature of the chemical history and evolution of clusters, groups, and ellipticals. Here, we summarise the most significant achievements in measuring elemental abundances in the ICM, from the very first attempts up to the era of XMM-Newton, Chandra, and Suzaku and the unprecedented results obtained by Hitomi. We also discuss the current systematic limitations of these measurements and how the future missions XRISM and Athena will further improve our current knowledge of the ICM enrichment.

show abstract

“…From the density distribution, the temperature profile follows with the assumptions that the gas is in hydrostatic equilibrium and distributed isotropically (see Moster et al 2011). Every gas particle is also given initial metal abundances, such that the radial metallicity profile follows that of the stars, but with a slightly lower metallicity peak of 93% solar at the centre (following Konami et al 2014). The hot gas halo has the same spin parameter as the dark matter halo (λgas = 0.033).…”

Section: Initial Conditionsmentioning

confidence: 99%

Active galactic nuclei feedback, quiescence and circumgalactic medium metal enrichment in early-type galaxies

Eisenreich

Naab

Choi

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present three-dimensional hydrodynamical simulations showing the effect of kinetic and radiative AGN feedback on a model galaxy representing a massive quiescent low-redshift early-type galaxy of M * = 8.41 × 10 10 M , harbouring a M BH = 4 × 10 8 M black hole surrounded by a cooling gaseous halo. We show that, for a total baryon fraction of ∼ 20% of the cosmological value, feedback from the AGN can keep the galaxy quiescent for about 4.35 Gyr and with properties consistent with black hole mass and X-ray luminosity scaling relations. However, this can only be achieved if the AGN feedback model includes both kinetic and radiative feedback modes. The simulation with only kinetic feedback fails to keep the model galaxy fully quiescent, while one with only radiative feedback leads to excessive black-hole growth. For higher baryon fractions (e.g. 50% of the cosmological value), the Xray luminosities exceed observed values by at least one order of magnitude, and rapid cooling results in a star-forming galaxy. The AGN plays a major role in keeping the circumgalactic gas at observed metallicities of Z/Z 0.3 within the central ∼ 30 kpc by venting nuclear gas enriched with metals from residual star formation activity. As indicated by previous cosmological simulations, our results are consistent with a model for which the black hole mass and the total baryon fraction are set at higher redshifts z > 1 and the AGN alone can keep the model galaxy on observed scaling relations. Models without AGN feedback violate both the quiescence criterion as well as CGM metallicity constraints.

show abstract

ABUNDANCE PATTERNS IN THE INTERSTELLAR MEDIUM OF EARLY-TYPE GALAXIES OBSERVED WITHSUZAKU

Cited by 14 publications

References 82 publications

Mass-invariance of the iron enrichment in the hot haloes of massive ellipticals, groups, and clusters of galaxies

Mass-invariance of the iron enrichment in the hot haloes of massive ellipticals, groups, and clusters of galaxies

Enrichment of the Hot Intracluster Medium: Observations

Active galactic nuclei feedback, quiescence and circumgalactic medium metal enrichment in early-type galaxies

Contact Info

Product

Resources

About