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Small-scale fluctua-ons of ICM proper-es and AGN Feedback Eugene - - PowerPoint PPT Presentation
Small-scale fluctua-ons of ICM proper-es and AGN Feedback Eugene - - PowerPoint PPT Presentation
Small-scale fluctua-ons of ICM proper-es and AGN Feedback Eugene Churazov Chandra images showing signs of AGN Feedback Jones Blanton Fabian Forman F.E),?()>#&)>(,&),.),?()CFG) ) H?#,)D&),?()4?I&D'&).0)#''5(-./G)
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F.E),?()>#&)>(,&),.),?()CFG) ) H?#,)D&),?()4?I&D'&).0)#''5(-./G) ) 1/)E?#,)0.5"),?()(/(5>I)#/6)"."(/,+")#5()5($(#&(6G) ) H?#,)05#'-./).0)(/(5>I)D&)6D&&D4#,(6G) ) J.(&),?()>#&)'..$G)))
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Radia-ve Mechanical Rare explosions Quasi-con-nuous Hot thermal plasma Rela-vis-c par-cles (CR) Collimated, high momentum Low momentum CR in the ICM CR confined to “bubbles” Sound waves No sound waves
Energy release options
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K.&#,UFK1)D"#>().0),?()V(5&(+&)'$+&,(5)
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H()'#/)"(#&+5()W(,)4.E(5)ED,?);+;;$(&)
:.5)</.E/)4.E(5)–),?()&D@().0),?();+;;$(&)D&)6(,(5"D/(6)A#$+().0)!" :.5)</.E/)!)–),?()&D@().0),?();+;;$(&)D&)6(,(5"D/(6);I)4.E(5)
C+.I#/'I)#>#D/&,);+;;$()D/*#-./)
LAGN, M ! LX >> LAGN,R
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g !
2.+4$D/>),.),?()123)
=/(5>I)D&),5#/&0(55(6),.)123)6+5D/>),?()5D&() N#/6)(A(/,+#$$I)6D&&D4#,(6O) ) =/(5>I)'./&(5A#-./)$#E)XY)Z[[\)(]'D(/,) (/(5>I)(L,5#'-./)05.");+;;$(&) Z^! 789)&$.E$I)D/*#,(&);+;;$(&)) ) ) ) 9.)?(#-/>).0),?()123)&.)0#5_) ) `^)C+;;$(&)5D&();+.I#/,$I)
) )8+$$)#/6)9.5,?.A(5P)ab)
)
E = 1 ! !1PV + PV
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#$%" !?.'<) F.,)V$#&"#) 3DLD/>) 123) F.,)V$#&"#) 3DLD/>) !.+/6) E#A(&) V5.4#>#-./) JD&&D4#-./) 2K)D/)123) C+.I#/,)5D&() >%E#A(&)c) ,+5;+$(/'() JD&&D4#-./)
:5.")789),.)123)N?(#,O)(]'D(/'I)
C+;;$(&)2K) !,5(#"D/>)
Z[[\) Z[[\) Z[[\) !" !"
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Can we generate sound waves with a spherical outburst?
E ⇒ RE = E P ⎛ ⎝ ⎜ ⎞ ⎠ ⎟
1/3
tE = RE cs tb
Total energy: Dura-on:
tb << tE ⇒
Sedov-Taylor phase + sound wave with 12.5% of energy
tb >> tE ⇒
No shock-heated gas – 0% of energy in sound waves Tang & EC, 17 See also EC+00,01; Forman+17, Zhuravleva+16
Upper limit on the energy of sound waves is 12.5% (spherical explosion)
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How to test this scenario with observa-ons?
1) Test I: Measure gas veloci-es (subsonic veloci-es) 2) Test II: Measure thermodynamic proper-es of perturba-ons in the ICM (isobaric perturba-ons) 3) Test III: Es-mate dissipa-on rate (hea-ng ~ cooling?)
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1/'5(#&D/>)A($.'D,I)
vk cs !!"k "
! ! HP Hs !1
d(&,)1)e)&+;&./D')A($.'D-(&)
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Gemng gas velocity power spectrum from images
δI I ⇒ P
2D(k) = C × P 3D(k) ⇒ δρ
ρ ⇒ v cs
Zhuravleva+,14b EC+, 2012; Arevalo+, 2012; Gaspari+,2014; Zhuravleva+, 2014a,b
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&'()"*+,)-.)/0",/012.3+-0)1"4)5,+4",/"0()".61)"67"0()"8)1-)+-".3+-0)19"
'()":,064,".6332;612<6/="%20+1)=">?@A"
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Veloci-es on 60 kpc scales
v ≈ 3 (1642 +1502) ≈ 384 km/s ≈ 0.4 cs
“line-of-sight velocity dispersion of 164±10 km/s” “gradient in the line-of-sight velocity of 150±70 km/s across the 60 kpc”
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2."4#5D&./)ED,?)!C)*+',+#-./&)
@ABC@?"D4E-" F"G?HB?"DI."
>?@B" >?@A"
d(&,)1)e)qr)
i?+5#A$(A#cPZn;)
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Isothermal Sound waves, weak shocks Isobaric (gravity waves)
δT T = 0× δn n δT T = 2 3 × δn n δT T = −1× δn n
Test II: “Equa-on of state”
EC+, 2016; Arevalo+, 2016; Zhuravleva+, 2016
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Perseus
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'(&)$(*+"#,-.& /0%00."$1&
2345 &67)-0-89& &343& &:$(*+"#,-.& &;43& &:$(0-#)9&
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'(&:$(0-#)9& /)<*"#<-.&=->"$1&
&;43 &67)-0-89& &34?& &:$(*+"#,-.& &343& &:$(0-#)9&
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d(&,)111e)F(#-/>)5#,()
Cooling=n2!(T) Heating = C!V
1,k 3 k
E(k) = K0! 2/3k!5/3
i?+5#A$(A#cPZn;)
d(&,)111e)qr)
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Summary
In cluster cores mechanical AGN Feedback has efficiency ~100% It drives subsonic mo-ons that can offset gas cooling losses AGN radia-ve output is small In CGM mechanical AGN Feedback can have similar efficiency It may operate at low accre-on rates (no bright AGN) Does not (directly) affect the ISM but affects CGM
H = M
- c2 αM fM ( !
m)+αR fR( ! m)
[ ]
1 <<
R
α
αM ~1
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From clusters to galaxies Churazov+,2005