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Marie Machacek Smithsonian Astrophysical Observatory

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. Thanks to my collaborators. Christine Jones William R. Forman Paul Nulsen Ralph Kraft

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Marie Machacek Smithsonian Astrophysical Observatory

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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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