1 / 28

AGN FEEDBACK IN GALAXY GROUPS — THE CASE OF HCG 62 —

AGN FEEDBACK IN GALAXY GROUPS — THE CASE OF HCG 62 —. Myriam Gitti (SAO-CfA). In collaboration with: E. O'Sullivan (SAO-CfA) , S. Giacintucci (SAO-CfA) , L. David (SAO-CfA) , J. Vrtilek (SAO-CfA) , S. Raychaudhury (Univ. Birmingham), P. Nulsen (SAO-CfA)

pakuna
Télécharger la présentation

AGN FEEDBACK IN GALAXY GROUPS — THE CASE OF HCG 62 —

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. AGN FEEDBACK IN GALAXY GROUPS — THE CASE OF HCG 62 — Myriam Gitti (SAO-CfA) In collaboration with: E. O'Sullivan (SAO-CfA), S. Giacintucci (SAO-CfA), L. David (SAO-CfA), J. Vrtilek (SAO-CfA), S. Raychaudhury (Univ. Birmingham), P. Nulsen (SAO-CfA) With thanks to: C. Jones (SAO-CfA), W. Forman (SAO-CfA), T. Ponman (Univ. Birmingham) Myriam Gitti - Chandra's First Decade of Discovery

  2. Cooling Flow cooling and accretion onto a central BH AGN outburst cooling is reestablished cooling is arrested system settles down Cooling flow regulation in galaxy clusters and groups MS0735.6+7421 Main candidate to solve the “Cooling Flow Problem”: Feedback by central AGN McNamara et al. 05, 09 McNamara & Nulsen 07 Gitti et al. 07 Rich clusters: detection of X-ray cavities and AGN-driven shocks  dominant contribution from (recurrent) outbursts from the central AGN, hosted by the cD galaxy at the center of (almost) every cool core clusters Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  3. Why do galaxy groups matter? Groups are the location of most galaxies in the Universe (Eke et al. 2004) NGC 5044 NGC 4636 Chandra 0.3-2.0 keV Examining outbursts in systems smaller than the well-studied rich clusters is valuable for a number of reasons: • shallow group potentiallarge impact on intragroup medium; • low pressure environmentmore apparent radio/thermal gas interaction; • significant influence on galaxy evolution Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  4. The project: a joint X-ray / radio study For a sample of 18 X-ray bright groups of galaxies: X-ray data: archival Chandra and/or XMM-Newton observations Low frequency radio data: GMRT observations at 150, 235, 327 & 610 MHz   geometry, physical state, and energetics of the hot gas loci of energy injection, history of AGN outbursts through spectral aging of electrons NGC 507 NGC 507 NGC 507 * How do X-ray and radio structures correlate? * What are the properties of the central radio source and what do they imply for ages, outburst cycles,..? * What are the effects of AGN at various phases of activity? * What are the mechanisms of energy injection? Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA GMRT 610 MHz on Chandra

  5. Group Name 235 MHz 610 MHz Group Name 235 MHz 610 MHz UGC 408 X X NGC 3411 X X NGC 315 X X NGC 4636 X X NGC 383 X X HCG 62 X X NGC 507 X X * NGC 5044 X X NGC 741 X X NGC 5813 X - HCG 15 X X NGC 5846 - X NGC 1407 X X * AWM 4 X X NGC 6269 X X NGC 1587 X X NGC 7626 X X MKW 2 X X Targets and status of the GMRT observations observed at 150 MHz All have Chandra and/or XMM data • Temperatures 1-3 keV • All have at least NVSS 1.4 GHz data initially • Presence of X-ray or radio structure indicative of AGN interaction with hot gas observed at 327 MHz Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  6. Group Name 235 MHz 610 MHz Group Name 235 MHz 610 MHz UGC 408 X X NGC 3411 X X NGC 315 X X NGC 4636 X X NGC 383 X X NGC 507 X X NGC 741 X X NGC 5813 X - HCG 15 X X NGC 5846 - X AWM 4 X X NGC 1587 X X NGC 6269 X X NGC 7626 X X MKW 2 X X Targets and status of the GMRT observations NGC 4636 Baldi et al. 2009 HCG 62 Gitti et al. in prep. *NGC 5044 David et al. 2009 NGC 1407X X *AWM 4Giacintucci et al. 2008 MKW 2 Giacintucci et al. 2007 * see posters ! David et al. Giacintucci et al. Vrtilek et al. Data for all groups will be presented in Giacintucci et al. in prep. New Chandra data O’Sullivan et al. in prep. Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  7. Chandra NGC4778 NGC4776 NGC4761 NGC4764 (Morita et al. 02) 1=17 kpc DSS The compact group of galaxies HCG 62(z = 0.014) • One of the most intrinsically luminous of the 100 Hickson compact groups: LX ≈ 1043 erg s-1 • VLA 1.4 GHz : S = 6.6 mJy • Very clear, small X-ray cavities (radio ghost) — first detection in a galaxy group — (Vrtilek et al. 02) beam=1812 lowest contour at 0.3 mJy/beam • central region dominated by 4 early-type galaxies • NGC 4778 possibly interacting with NGC 4761 (Spavone et al. 06) Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  8. X-RAY DATA:Chandra 50 ks(2000) raw 0.5-2.0 keV ACIS Unsharp masked image Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  9. X-RAY DATA:XMM90 ks(2007) mosaic 0.5-2.0 keV MOS+PN Unsharp masked image Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  10. 235610 = 1.42 (new!)RADIO DATA: GMRT 2h(2008) P610 =5.41021 W Hz-1 P235 =2.11022 W Hz-1 beam=14"x14" beam=14"x12" XMM Chandra beam=14"x14" beam=14"x12" 610 MHz: r.m.s. = 65 Jy/beam S = 12.8 mJy (6.9 mJy core) 235 MHz: r.m.s. = 230 Jy/beam S = 49.6 mJy (15.1 mJy core) (Giacintucci et al., in prep.) Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  11. X-RAY / RADIO INTERACTION – Pressure – – Energy budget – Pcav =3.91042 erg s-1 LICM=1.81042 erg s-1 The AGN outburst is currently supplying about twice the power lost by radiation within the cooling region (Rafferty et al. 06) L[10MHz-10GHz]= 41038 erg s-1 The radio luminosity is much less than the mechanical power  radiative efficiency ~ 10-4 Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  12. X-RAY / RADIO INTERACTION – Pressure – – Energy budget – Cavity N: PX / Pradio ~ 4 Cavity S: PX / Pradio ~ 2 The cavities are close to pressure balance Pcav =3.91042 erg s-1 LICM=1.81042 erg s-1 The AGN outburst is currently supplying about twice the power lost by radiation within the cooling region (Rafferty et al. 06) Vice versa: Epr = k Eel k = [6-27]required for pressure equilibrium  “light”hadronic jets L[10MHz-10GHz]= 41038 erg s-1 The radio luminosity is much less than the mechanical power  radiative efficiency ~ 10-4 Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  13. SHOCK FRONT Chandra SB profile Shock model - fit to SB Rshock=35.7 kpc (Gitti, O’Sullivan, Giacintucci et al., in prep.) Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  14. SHOCK FRONT Chandra T profile post-shock pre-shock post-shock pre-shock • Shock model properties: • Mach = 1.45 • Energy = 6.21057 erg • Age = 2.7107 yr • Power = 7.31042 erg s-1 ~2Pcav measured ~15% T jump across the front (Gitti, O’Sullivan, Giacintucci et al., in prep.) Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  15. SHOCK FRONT Chandra vs. XMM T profile Things only Chandra can see! :) post-shock pre-shock post-shock pre-shock • Shock model properties: • Mach = 1.45 • Energy = 6.21057 erg • Age = 2.7107 yr • Power = 7.31042 erg s-1 ~2Pcav XMM measured ~15% T jump across the front Chandra (Gitti, O’Sullivan, Giacintucci et al., in prep.) Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  16. Fit to Chandra SB ne jump ~ 2 Chandra T profile A cold front? Rfront = 20 kpc Work in progress… Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  17. TEMPERATURE MAP Cool region along the N cavity limbs why not in the S one? maybe heated by the passage of the shock asymmetric shock? Chandra spectral map (XMM consistent) Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  18. Fe-ABUNDANCE MAP Arc-like region of enriched material at ~2 from the center – stripping from central galaxies? – tidal interaction? (see Gu et al 2007) but also.. possible Fe abundance overestimate due to non-Maxwellian electron distributions near the shock (Kaastra et al. 2009) cs ~ 500 km s-1 Chandra spectral map (XMM consistent) Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  19. Summary • Elliptical-dominated galaxy groups are an ideal laboratory to investigate AGN-driven feedback: • Groups show generally similar phenomenology to clusters, with many radio and X-ray features that are the direct result of AGN activity • Groups are an important/dominant locus for evolution of baryonic material • Our analysis of HCG 62 demonstrates the power of a combined X-ray / (low-frequency) radio approach to the feedback problem: – Low-frequency radio emission detected in the cavities – “Light” hadronic jets (k~10-30) – Detection of shock front with M ~ 1.45, Eshock~3Ecav • A similar study will be carried out for other individual interesting groups in the sample (e.g., NGC 3411, NGC 1407, NGC 741..) • Statistical analysis and study of X-ray/radio properties of the whole group sample (in progress..) Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  20. Myriam Gitti - Chandra's First Decade of Discovery

  21. lowest contour at 1 lowest contour at 2 CHANDRA + GMRT 235 MHz lowest contour at 2 Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  22. CHANDRA + VLA 1.4 GHz beam=1814; lowest contour at 0.7 mJy/beam Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  23. SHOCK FRONT  T profile (90% c.l.) Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  24. SHOCK FRONT  spectra post-shock: T = 1.51 keV pre-shock: T = 1.33 keV Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  25. SHOCK FRONT  T map (from energy of blended Fe-L line) Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  26. COLD FRONT  T profile (90% c.l.) Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  27. Azimuthally-averaged SB profile Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

  28. Properties of group members • NGG4778 (HCG 62a): S0 galaxy with kinem. and morph. peculiarities • rotation curve not symmetric with respect to the center; velocity dispersion: 380 km/s (center), ~300 km/s (r>5), ~420 km/s (r~25  to SW) • nuclear counterrotation, distorted kinematics in the outer halo, and X-ray group properties suggest that NGC 4778 may be the product of a recent minor merger, likely with a small late-type galaxy (Spavone et al. 06) • hierarchical mergers of cluster galaxies might power the emission line gas in the center of the group members • H emission observed in NCG4778 (also in NCG4776 and NCG4761); • L(H ) ~ 1039 erg s-1 (in each galaxy)  total mass of ionized gas ~ 104 Msun • (Valluri & Anupama 96) • No evidence of AGN activity in the X-ray data (no point source) in NGC 4778 Myriam Gitti - Chandra's First Decade of Discovery Myriam Gitti — Chandra’s First Decade of Discovery — 23 September 2009, Boston MA

More Related