Table Of ContentRadio mode AGN
feedback observations in
massive central galaxies
Becky Canning, Heidelberg, July 2014
1
Multiphase media in X-ray
bright galaxies
Low redshift, X-ray bright,
massive (central) galaxies
!
Masses ~1011-1012 solar
masses
Single SSP models
suggest ages of ~ 10
billion years
SFRs typically <0.1-1 solar
mass per year (often upper
limits from Galex - without
correction for old stellar
populations)
No recent wet mergers
2
Multiphase media in X-ray
bright galaxies
Low redshift, X-ray bright,
24 A.C. Edge
massive (central) galaxies
!
Masses ~1011-1012 solar
masses
Single SSP models
suggest ages of ~ 10
billion years
SFRs typically <1 solar
mass per year (often upper
limits from Galex - without
correction for old stellar
populations)
Figure 9.Moleculargasestimateplotted againstopticallinEedlugmei neots itayl.. T2h0e0s1tarsarenewdetections presented here,the squaresare
No recent wet medetrecgtionesorfsothercentralclustergalaxiesandtheupperlimitsarefromthisworkandtheliterature.Thedashedlinemarksalinewith
aconstantratioofmoleculargasmasstoopticallineemissionandisnotafittothedata.
3
Figure 10.Moleculargas estimate plotted against global massflow rate. The symbols and lineare as inFigure 9. Not allpoints are
plottedasmassflowratesarenotknownforalldetectionsandupperlimits.
⃝c 0000RAS,MNRAS000,000–000
Multiphase media in X-ray
bright galaxies
Low redshift, X-ray bright,
24 A.C. Edge
massive (central) galaxies
! What is the gases relation to!
Masses ~1011-1012 solar
AGN feedback?!
masses
!
Single SSP models
What is the origin of the gas?!
suggest ages of ~ 10
!
billion years
Why isn’t it forming stars?
SFRs typically <1 solar
mass per year (often upper
limits from Galex - without
correction for old stellar
populations)
Figure 9.Moleculargasestimateplotted againstopticallinEedlugmei neots itayl.. T2h0e0s1tarsarenewdetections presented here,the squaresare
No recent wet medetrecgtionesorfsothercentralclustergalaxiesandtheupperlimitsarefromthisworkandtheliterature.Thedashedlinemarksalinewith
aconstantratioofmoleculargasmasstoopticallineemissionandisnotafittothedata.
4
Figure 10.Moleculargas estimate plotted against global massflow rate. The symbols and lineare as inFigure 9. Not allpoints are
plottedasmassflowratesarenotknownforalldetectionsandupperlimits.
⃝c 0000RAS,MNRAS000,000–000
Combine: HST optical/UV
Abell 3581!
JVLA and GMRT radio data
z=0.0218 (95 Mpc)
Chandra X-ray data
SOAR optical imaging
VIMOS spectroscopy
Canning et al. 2013
5
Cool-core group - some heating is required!
50’’ ~ 20 kpc
Chandra X-ray
6
L in the core ~ P in inner bubbles!
X cav
2.1x1042 ergs-1 ~ 2.2x1042 ergs-1
Multiple bubbles - AGN timescales
Duty cycles - high (70% to 100%)
Birzan et al. 2004, Rafferty et al. 2006!
Duty cycle is ~100%
Dunn et al. 2006
JVLA 1.4 GHz
Chandra X-ray
7
See also Birzan+04, Rafferty+06+08, Dunn+F,06,07
AGN feedback in Abell 3581 5
AGN feedback in Abell 3581 5
~108 solar masses of gas H alpha
~106 solar masses of dust
Figure2.Left:NetnarrowbandH↵emissionimage,takenwiththeSOARtelescope,oftheBGGinAbell3581afterremovalofcontinuumemissionwiththe
CTIO6520/76filter.Right:TheunsharpmaskedH↵emissionimage.Theinitialimagehasbeensmoothedbya2Dgaussianwith� =1arcsec,subtracted
fromtheoriginalandbinnedby4pixels(0.6”)ineachdirection.
Figure2.Left:NetnarrowbandH↵emissionimage,takenwiththeSOARtelescope,oftheBGGinAbell3581afterremovalofcontinuumemissionwiththe
CTIO6520/76filter.Right:TheunsharpmaskedH↵emissionimage.Theinitialimagehasbeensmoothedbya2DDgaususianswitth� =1arcsec,subtracted
fromtheoriginalandbinnedby4pixels(0.6”)ineachdirection.
8
Figure3.Left:HSTF555Wimagewithasmoothellipticalisophotalmodelsubtracted.Thedarkfeaturepiercingnorth-souththroughthenucleusandturning
towardsthesouth-eastisabsorptionfromaprominentdustlane.Right:F300Ximageofthesameregion.Theredcircleshowsayoungstarclusternotseen
inthevisible(F555WandF814W)images.Thestarclustercoincideswiththenortherndustlane.
Figure3.Left:HSTF555Wimagewithasmoothellipticalisophotalmodelsubtracted.Thedarkfeaturepiercingnorth-souththroughthenucleusandturning
towardsthesouth-eastisabsorptionfromaprominentdustlane.Right:F300Ximageofthesameregion.Theredcircleshowsayoungstarclusternotseen
inthevisible(F555WandF814W)images.Thestarclustercoincideswiththenortherndustlane.
Figure4.Left:ThecentralregionofthenetH↵imageoverlaidwithcontoursofdustabsorption.ThedustcloselycoincideswiththeinnerH↵filaments.
Right:TherelativedustattenuationinthebrightestclustergalaxyinunitsofE(B V)magnitudesaftercorrectionforGalacticreddening.Contoursof
�
L-bandJVLAradioemission,whichfilltheinnerX-raycavities,areoverlaid.Theangularscaleisthesameasthelefthandpanel.
Figure4.Left:ThecentralregionofthenetH↵imageoverlaidwithcontoursofdustabsorption.ThedustcloselycoincideswiththeinnerH↵filaments.
Right:TherelativedustattenuationinthebrightestclustergalaxyinunitsofE(B V)magnitudesaftercorrectionforGalacticreddening.Contoursof
�
L-bandJVLAradioemission,whichfilltheinnerX-raycavities,areoverlaid.Theangularscaleisthesameasthelefthandpanel.
c 0000RAS,MNRAS000,000–000
�
c 0000RAS,MNRAS000,000–000
�
How can radio mode feedback
affect galaxy evolution
Quiescence: Keeping hot gas hot
!
But cool and cold gas are observed in massive X-ray
bright galaxies.
!
Argue here that this gas originates from the hot gas
and is heated/redistributed in the galaxy by RM AGN
feedback. So RM feedback also important for ‘quenching’
(preventing cool/cold gas from forming stars).
9
JVLA 1.4 GHz
10
Description:Masses ~1011-1012 solar masses. Single SSP models suggest ages of ~ 10 billion years. SFRs typically
