the cores of two galaxy groups: what are they teaching us ?
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THE CORES OF TWO GALAXY THE CORES OF TWO GALAXY GROUPS: WHAT ARE THEY GROUPS: WHAT ARE THEY
TEACHING US ?TEACHING US ?
FABIO GASTALDELLO
UNIBO & UC IRVINE D. BUOTE UCI
W. MATHEWS UCSC
F. BRIGHENTI UNIBO
S. ETTORI OABO
OUTLINEOUTLINECOOLING FLOWS
AGN FEEDBACK
AGN FEEDBACK
AWM 4
SIMPLE MODEL
(DONAHUE ET AL. 05)
AWM 4
MERGERS
? THE CASE OF NGC 5044
COOLING FLOWS VS. AGN FEEDBACKCOOLING FLOWS VS. AGN FEEDBACKA.C. FABIAN
CENTRAL (< 100 KPC) DENSITIES OF RELAXED CLUSTERS HIGH ENOUGH THAT RADIATIVE COOLING TIMES LESS THAN 1010 YR
IN THE ABSENCE OF ANY BALANCING HEAT SOURCE, A COOLING FLOW DEVELOPS
COOLING FLOWS VS. AGN FEEDBACKCOOLING FLOWS VS. AGN FEEDBACKA.C. FABIAN
CENTRAL (< 100 KPC) DENSITIES OF RELAXED CLUSTERS HIGH ENOUGH THAT RADIATIVE COOLING TIMES LESS THAN 109 YR
IN THE ABSENCE OF ANY BALANCING HEAT SOURCE, A COOLING FLOW DEVELOPS
X-RAY OBSERVATIONS BEFORE CHANDRA AND XMM BROADLY CONSISTENTS BUT MASS SINK PROBLEM: INDICATION OF COLD GAS AND STAR FORMATION BUT 10 TO 100 TIMES LOWER THAN INFERRED FROM X-RAYS
GALAXY FORMATION: MUCH OF THE GAS IN THE FORMATION OF MASSIVE GALAXIES BEHAVES AS IN A COOLING FLOW (WHITE & FRENK 91). IF WE CANNOT UNDERSTAND WHAT IS GOING ON IN CLUSTER CORES, THEN WHY SHOULD WE BELIEVE MODELS OF GALAXY FORMATION WHICH RELY ON A SIMILAR PROCESS ?
COOLING FLOWS VS. AGN FEEDBACKCOOLING FLOWS VS. AGN FEEDBACKJ. BINNEY
FOR MORE THAN TWO DECADES THE THEORY OF STEADY STATE COOLING FLOWSHELD UP PROGRESS IN APPRECIATING THE ROLE THAT AGN PLAY IN STRUCTURING GALAXIES. THIS THEORY WAS FINALLY SWEPT AWAY BY DAMNING EVIDENCE FROM CHANDRA AND XMM, BUT ITS INTERNAL CONTRADICTIONS SHOULD HAVE LEFT IT WITHOUT PROPONENTS A DECADE AGO
IT HAS LONG BEEN SUGGESTED THAT COOL CORE PHENOMENON IS FUNDAMENTAL FOR THE GALAXY FORMATION PROCESS. I AGREE, BUT I WANT TO PERSUADE YOU THAT COOL CORES DO NOT TELL US HOW GALAXIES FORMED, BUT WHY THEY CEASED FORMING.
ALTHOUGH SOME LOOSE ENDS REMAIN, I AM IMPRESSED BY THE WAY IN WHICH DISPARATE STRANDS OF THEORY AND OBSERVATIONS ARE COMING TOGETHER TO FORM A COHERENT PICTURE OF GALAXY FORMATION AND THE SYMBIOSIS OF BHs WITH SPHEROIDS AND COOL CORE CLUSTERS
NO COOLING FLOWSNO COOLING FLOWS
Peterson et al. 03
AGN FEEDBACKAGN FEEDBACK
Martin Rees
“I’VE BEEN ESPECIALLY IMPRESSED BY THE CHANDRA X-RAY IMAGES OF GALAXY CLUSTERS. WE SEE HOW GAS IS COOLING DOWN AND HOW THE COOLING IS BEING BALANCED BY TREMENDOUS OUTBURSTS OF JETS AND BUBBLES. THIS IS SOMETHING THAT MOST PEOPLE DIDN’T SUSPECT WAS HAPPENING UNTIL THESE IMAGES REVEALED IT ”
Perseus: Fabian+03,04,05
A2052: Blanton+01,03 Hydra A: McNamara+00
AGN FEEDBACKAGN FEEDBACK
Gas cools down and starts flowing in
BH swallows matter
Jets dissipate, heating gas
Gas stops flowing in BH spins up, producing
jets
BH exhausts fuel; jets stop
Tucker, Tananbaum & Fabian 07
AGN FEEDBACKAGN FEEDBACK
“In this scenario there is a clear dichotomy between active and radio quiet clusters: one would expect the cluster population to bifurcate into systems with strong temperature gradients and feedback and those without either”
Donahue et al. 2005
AWM4 AND AGN FEEDBACKAWM4 AND AGN FEEDBACK
GASTALDELLO ET AL. 2007
AWM4 AND AGN FEEDBACKAWM4 AND AGN FEEDBACK
GASTALDELLO ET AL. 2007
AWM4 AND AGN FEEDBACKAWM4 AND AGN FEEDBACK
GASTALDELLO ET AL. 2007
OPTICAL NEBULAE IN COOL OPTICAL NEBULAE IN COOL CORES: AGN VS. MERGERSCORES: AGN VS. MERGERS
NGC 1275 (Perseus): Conselice+01
NGC 4696 (Centaurus): Crawford+05
OPTICAL NEBULAE IN COOL OPTICAL NEBULAE IN COOL CORES: AGN VS. MERGERSCORES: AGN VS. MERGERS
OPTICAL FILAMENTS, INITIALLY THOUGHT TO HAVE THEIR ORIGIN IN THERMAL INSTABILITIES OF THE COOLING FLOW
GAS, WERE TOO MUCH LUMINOUS,WITH SMALL SPATIAL EXTENT AND DUSTY (SHORT SPUTTERING TIME, 107 yr AT 1
KeV)
A STRAIGHTFORWARD ALTERNATIVE IS THAT THEY WERE ACCRETED FROM ELSEWHERE, FROM A GAS RICH SPIRAL OR DWARF GALAXY (SPARKS+89) OR THEY ARE TRAILS OF SECONDARY GALAXIES PUNCHING THROUGH THE CENTRAL GALAXY MOLECULAR HYDROGEN RESERVOIR (WILMAN+06)
OPTICAL NEBULAE IN COOL OPTICAL NEBULAE IN COOL CORES: AGN VS. MERGERSCORES: AGN VS. MERGERS
2A 0335+096: Donahue+07
OPTICAL NEBULAE IN COOL OPTICAL NEBULAE IN COOL CORES: AGN VS. MERGERSCORES: AGN VS. MERGERS
A2204: Wilman+06
OPTICAL NEBULAE IN COOL OPTICAL NEBULAE IN COOL CORES: AGN VS. MERGERSCORES: AGN VS. MERGERS
NGC1275(Perseus):Conselice+01
“The small scale features of NGC 1275 support the idea that this galaxy experienced a merger with a galaxy that contained a nonnegligible stellar component but likely with a significant lower mass than NGC 1275 ”
OPTICAL NEBULAE IN COOL OPTICAL NEBULAE IN COOL CORES: AGN VS. MERGERSCORES: AGN VS. MERGERS
Perseus: Ettori et al. 98
OPTICAL NEBULAE IN COOL OPTICAL NEBULAE IN COOL CORES: AGN VS. MERGERSCORES: AGN VS. MERGERS
“IN ORDER TO UNDERSTAND THE ORIGIN OF THIS FILAMENTARY STRUCTURE, WE HAVE INVESTIGATED TH
EVOLUTION OF THE HOT ICM GAS PERTURBED BY THE AGN CENTRAL ACTIVITY IN A PERSEUS-LIKE CLUSTER. OUR
SIMULATIONS SHOW THAT A FRACTION OF THE 1-2 KeV GAS PRESENT AT THE CENTER OF CLUSTERS IS TRAPPED AND ENTRAINED BY THE RISING BUOYANT BUBBLE TO HIGHER RADIUS WHERE THE AGN HEATING IS LESS EFFICIENT. THE RADIATIVE COOLING MAKES IT COOL IN A FEW TENS OF Myr BELOW 104 K FORMING COLD FILAMENTARY STRUCTURES IN
THE WAKE AND IN THE RIM OF THE BUBBLES. THIS SCENARIO EXPLAINS THE Hα AND CO EMISSION WITHOUT
CONTRADICTING THE OBSERVED LACK OF 1 KeV GAS.”
REVAZ, COMBES & SALOME’ 07 (arXiv:07114051)
Fabian et al. 2003
OPTICAL NEBULAE IN COOL OPTICAL NEBULAE IN COOL CORES: AGN VS. MERGERSCORES: AGN VS. MERGERS
THE CASE OF NGC 5044THE CASE OF NGC 5044
•NGC 5044 IS A FOSSIL GROUP: ONLY ONE BIG ELLIPTICAL GALAXY SURROUNDED BY DWARFS (MERGER FREE ENVIRONMENT
•IT IS NEARBY ~ 39 Mpc
Buote et al. 2002
THE CASE OF NGC 5044THE CASE OF NGC 5044
•EVIDENCE OF FILAMENTRAY STRUCTURE AND X-RAY CAVITIES
DUST IN NGC 5044 DUST IN NGC 5044
TEMI, BRIGHENTI & MATHEWS 2007
NGC 5044 NGC 5044
NGC 5044 NGC 5044
BLACK : X-ray FILAMENT box #1
RED: X-ray FILAMENT box #3
CONCLUSIONS CONCLUSIONS
AGN FEEDBACK HAS ALL THE FEATURES OF THE RIGHT SOLUTION BUT WE ARE NOT CLOSE TO A CLEAR UNDERSTANDING
AGN FEEDBACK IN GROUPS IS STILL POORLY INVESTIGATED AND THERE ARE SOME PUZZLES, LIKE AWM 4. THE FEEDBACK LOOP IS LIKELY DISTURBED BY MERGERS. THEY CAN BOTH CONTRIBUTE TO THE PHENOMENA IN CLUSTER CORES
IN NGC 5044 WE HAVE EVIDENCE OF THE IMPORTANCE OF DUST IN COOLING THE X-RAY GAS (AND MAYBE BEING RESPONSIBLE OF THE PRODUCTION OF Hα)
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