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ATHENA WFI and XIFU Observations of the


Fornax and Virgo Clusters Gas Dynamics Merger History and Elemental EnrichmentR Kraft1Y Su1T Fish21A Sheardown2E Roediger21W Forman1C Jones1P Nulsen1E Churazov3 S Randall1 EBulbul11Smithsonian Astrop

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Document on Subject : "ATHENA WFI and XIFU Observations of the"— Transcript:

1 ATHENA WFI and XIFU Observations of the
ATHENA WFI and XIFU Observations of the Fornax and Virgo Clusters: Gas Dynamics, Merger History, and Elemental Enrichment R. Kraft 1 , Y. Su 1 , T. Fish 2,1 , A. Sheardown 2 , E. Roediger 2,1 , W. Forman 1 , C. Jones 1 , P. Nulsen 1 , E. Churazov 3 , S. Randall 1 , E . Bulbul 1 1 Smithsonian Astrophys

2 ical Observatory 2 E. A. Milne Cente
ical Observatory 2 E. A. Milne Center for Astrophysics, Hull University 3 Max Planck Institute for Astrophysics ABSTRACT: The Fornax cluster is a cool (kT~1.5 keV ), nearby cluster (d~20 Mpc ) that is in the late stage of merging with a small group. In this presentation, we describe how an Athena WFI survey of t

3 he cluster gas to the virial radius c
he cluster gas to the virial radius combined with specifically targeted XIFU observations would transform our understanding of the merger history, gas dynamics, and the distribution of heavy elemen ts in the ICM. Due to its proximity, angular size, high surface brightness, and relatively cool temperature, the Fornax clust

4 er is one of the key benchmarks that
er is one of the key benchmarks that informs our understanding of the dynamics of groups and poor clusters. This cluster has been deeply observed by both Chandra and XMM - Newton, and we created detailed hydrodynamical simulations of the infall and merger of NGC 1404 into the Fornax cluster. These data and simulat

5 ions will be used to make detailed predi
ions will be used to make detailed predictions for mock Athena observations of this cluster. F orn ax is the perfect Athena target - cool, nearby, clean merger - for understanding the microphysics, enrichment, and evolution of the plasma that is the dominant baryonic component of the Universe and which is fully reveal

6 ed in galaxy clusters as it is heated to
ed in galaxy clusters as it is heated to the virial temperature. ATHENA studies of nearby groups and clusters • Nearby clusters offer highest linear resolution and sensitivity – can probe spatial scales inaccessible in other targets. • Difficult to study globally with current generation of X - ray observator

7 ies because they are too extended (degr
ies because they are too extended (degrees). • ATHENA is well - suited for these investigations because of the large effective area and FOV of the WFI and the high spectral resolution of the XIFU. • Lots of consideration has been given to Perseus and Coma clusters, but all of the nearby clusters and groups will be

8 f antastic ATHENA targets. • Goal of
f antastic ATHENA targets. • Goal of this talk – describe some potential investigations of individual galaxies and global properties of the Fornax and Virgo clusters (or, how to have fun with FLASH and SIXTE) The Fornax and Virgo Clusters X MM - Newton mosaic of the Fornax cluster (left – d L =20 Mpc , Su+

9 2017) and ROSAT mosaic of the Virgo clu
2017) and ROSAT mosaic of the Virgo cluster (right – d L =17 Mpc , Bohringer+1995). 1.35 Mpc = 4 150 k pc = 25’ k B T~1.5 keV k B T~2.5 keV Zoom - in on the Fornax Cluster • Simulation of infall of NGC 1404 into Fornax cluster using FLASH (Sheardown+2018) • Non - magnetic, inviscid

10 • Includes gravity solver • Init
• Includes gravity solver • Initial conditions derived from X - ray observations (temperature and surface brightness) and stellar profiles • Properties of ram - pressure stripped core and sloshing cold front match observations quite well Time slice of temperature and density – present epoch Simu

11 lated WFI mosaic of Fornax Cluster deri
lated WFI mosaic of Fornax Cluster derived using FLASH simulation + SIXTE Simulated 5x5 mosaic of 70 ks WFI observations of Fornax cluster Simulated WFI mosaic of Fornax Cluster derived using FLASH simulation + SIXTE Simulated 5x5 mosaic of 70 ks WFI observations of Fornax cluster and large scale surface brig

12 htness profile Background level R vi
htness profile Background level R vir Simulated WFI mosaic of Fornax Cluster derived using FLASH simulation + SIXTE Simulated 5x5 mosaic of 70 ks WFI observations of Fornax cluster Simulated WFI mosaic of Fornax Cluster derived using FLASH simulation + SIXTE Simulated 5x5 mosaic of 70 ks WFI observat

13 ions of Fornax cluster Observations an
ions of Fornax cluster Observations and simulations of Virgo Cluster sloshing cold front Surface brightness of simulated Virgo cluster sloshing cold front derived from inviscid (top row) and viscous (bottom row) hydrodynamic simulations (Roediger+2013). Deep (500 ks ) Chandra observation of Virgo cluster sloshing

14 cold front (Werner+2016). Linear featur
cold front (Werner+2016). Linear features along front suggestive of magnetic compression/ filamentation . Time slice of temperature and density – present epoch Time slice of temperature and density Ram pressure stripping of N1404 tail and stolen atmosphere Deep (200 ks ) Chandra observation of NGC 4552 in the

15 Virgo cluster (left – Kraft+2017)
Virgo cluster (left – Kraft+2017) and simulated images of ram pressure stripping assuming viscous and inviscid ICM (right - Roediger+2015). Ram pressure stripping of N1404 tail and stolen atmosphere 70 ks ATHENA WFI observations of NGC 1404 derived from FLASH simulation. The present epoch is shown in the

16 left figure and a an earlier (~300 Myr
left figure and a an earlier (~300 Myr ) epoch in the right. NGC 4472 – infalling into Virgo cluster – most optically luminous galaxy in the local Universe Suzaku (left) and XMM - Newton (right) temperature map mosaics of NGC 4472 (Su+ in preparation). Is this the first or second infall for NGC 4472?

17 XIFU observation of subsonic gas motion
XIFU observation of subsonic gas motions in NGC 1404 Simulated XIFU image of NGC 1404 using FLASH simulation (left), velocity map derived from XIFU spectrum (center), and broadband spectrum of emission. Distorted radio galaxy 3C 28 in double cluster Abell 115 (W. Forman+2017) Take - away points • The combinatio

18 n of the ATHENA WFI, the XIFU, and spec
n of the ATHENA WFI, the XIFU, and specifically - tailored (magneto - )hydrodynamic simulations will be a powerful combination for understanding gas dynamics in galaxy clusters • The entire assembly history of (all of) the nearby clusters will be revealed by ATHENA • ATHENA will transform our understanding microphys