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Probing Galaxy-Gas Interactions in Groups and Clusters with Chandra and XMM-Newton

This study explores the dynamics of galaxy-gas interactions within galaxy groups and clusters using X-ray observations from Chandra and XMM-Newton. We present three case studies: NGC 1404 in the Fornax Cluster, NGC 4552 in the Virgo Cluster, and NGC 6872 in the Pavo Group, analyzing their interactions with the intragroup medium (IGM). By examining temperature maps and surface brightness profiles, we gain insights into various phenomena such as ram-pressure stripping and tidal interactions, contributing to our understanding of galaxy evolution in dense environments.

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Probing Galaxy-Gas Interactions in Groups and Clusters with Chandra and XMM-Newton

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  1. Probing the Dynamics of Galaxy-Gas Interactions in Groups and Clusters with Chandra and XMM-Newton Marie Machacek Smithsonian Astrophysical Observatory IGM Workshop 3/8/2005

  2. Thanks to my collaborators Christine Jones William R. Forman Paul Nulsen Ralph Kraft Alexey Vikhlinin Maxim Markevitch Liviu Stirbat

  3. Galaxy-IGM Interactions in Three Systems • Elliptical NGC 1404 Fornax Cluster kT = 1.5 keV Transonic ram-pressure stripping • Elliptical NGC 4552 Virgo Cluster kT = 2.2 keV Supersonic ram-pressure stripping • Spiral NGC 6872 Pavo Group kT = 0.5 keV High velocity encounter

  4. NGC 1404 in Fornax Chandra 0.3-2 keV 134.3 ks NGC 1399 19 Mpc NGC1404 Rp = 54 kpc Dosaj et al. 2002 ; Scharf et al. 2004; Machacek et al. 2005

  5. Temperature Map Surface Brightness Map Tg = 0.55-0.02+0.01 keV A = 0.7-0.1+0.7 Zs

  6. Model Assumptions Vikhlinin et al. 2001; Mazzotta et al. 2001 • N1404 & N1399 in same plane - r ~ rp : stripped tail  ICM dense - sharp edge  inclination angle  not large • N1404 - isothermal sphere - density ng r- • Surface brightness jump  (gng2/cnc2)

  7. Surface Brightness Profile 1.54 =0.5 re=7.64 kpc 0.3, rc=395”

  8. NGC 1404’s Transverse Velocity Tg/Tc = 0.36 ng/nc = 6.0 pg/pc = 2.1 M1 ~ 1.0 v = 657 km/s vr = 450 km/s* vt = 478 km/s  ~ 43˚ Pressure ratio vs Mach Number *Drinkwater et al. 2001

  9. NGC 4552 in Virgo Chandra 54.4 ks 0.5-2 keV Machacek et al. 2005

  10. Surface Brightness Profile =1.29 r1 = 1.29 kpc r2 = 3.12 kpc

  11. Surface Brightness Profile T1 = 0.61 keV T2 = 0.44 keV Ag = 0.6±0.2 Zs r1 = 1.29 kpc Tc = 2.2 keV r2 = 3.12 kpc

  12. NGC 4552’s Transverse Velocity Pressure ratio vs Mach Number Tg/Tc = 0.2 ng/nc = 37 ± 5 pg/pc = 7.3 ± 1.1 M1= 2.1 ± 0.2 v = 1646 km/s vr = -968 km/s* vt = 1331 km/s  ~ 36˚ ± 3˚

  13. Tail Properties • T = 0.57+0.06-0.1 keV • n ~ 0.006 cm-3 >> nc • p ~ a few  pICM • length ~ 10 kpc • bowed

  14. Shock Model for Inner Rings  Emech = 2.4  1055fv ergs Lmech = 5.8  1041fv ers/s Lmech - Lradio  6.4  1041 ergs/s Birzan et al. 2004 Mach = 1.7 t = 1.32 Myr

  15. Tidal InteractionsNGC 6872/ IC 4970 VLT-ANTU+FORS1 ESO Top 20 images

  16. NGC 6872 in Pavo D = 53.5 Mpc vr = 849 km/s* *Martimbeau & Huchra CfA Redshift Survey 2004

  17. Strong Interaction with Pavo XMM pn+mos 0.5-2 keV 32.2 ks Machacek et al. 2005 astro-ph 0411286v2

  18. Trail Properties • Hot T ~1 kev ~2TIGM • Dense n ~ 1.7nIGM • Low abundance A ~ 0.2 ± 0.1 Zs • Large extent ~ 67  90 kpc

  19. Trail Formation Models • Tidal Stripping - distortions of other tracers ? • Ram Pressure Stripping - T high? A low? n < 2 nICM - not like NGC 4552! • Bondi-Hoyle Gravitional Focusing • Turbulent Viscous Stripping

  20. Bondi Gravitational Focusing For NFW profile Mach ~ 3 / flat  long trail no large central peak large gravitating halo ? vcirc ~ ? a = 20 kpc ? sufficient heating ? Tad ~ 1.4 TIGM

  21. Turbulent Viscous Stripping Stripping Rate Energy Extent + Adiabatic expansion v = vr / sin   v ~ 1300 km/s  ~ 40

  22. Signatures in the Trail • Filaments, streamers gas? stars? dust? • Abundance galaxy, IGM or mix? • T & n profile thermalization region? cools, broadens & dims?

  23. Conclusions X-ray Observations of Edges, Tails and Trails • Constrain 3-D motion of galaxy • Show stripping processes in action • Reveal interactions previously overlooked • Differentiate between different stripping processes

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