Cooling and Feedback in Early-Type Galaxies (and Groups) C. Jones, W. Forman, E. Churazov, P....
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Transcript of Cooling and Feedback in Early-Type Galaxies (and Groups) C. Jones, W. Forman, E. Churazov, P....
![Page 1: Cooling and Feedback in Early-Type Galaxies (and Groups) C. Jones, W. Forman, E. Churazov, P. Nulsen, R. Kraft X-ray emission from early-type galaxies.](https://reader036.fdocuments.net/reader036/viewer/2022062620/551a3898550346545e8b4cde/html5/thumbnails/1.jpg)
Cooling and Feedback in Early-Type Galaxies (and Groups)
C. Jones, W. Forman, E. Churazov, P. Nulsen, R. Kraft
X-ray emission from early-type galaxies = hot gas + stars + LMXBs
• Heating by radio lobes (e.g. Cen A)• Results from a Chandra survey of ~160 galaxies -
30% of very luminous galaxies have cavities; 80% have X-ray emission from the nucleus
•AGN outbursts heat and remove gas (e.g. NGC1316)•Is non-thermal pressure support important?
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Hot Gas in Early-type Galaxies - The Einstein EraPrior to Einstein observations, early type galaxies were considered to be gas free, with the gas from stellar mass loss removed by SN driven winds.
Einstein observations showed extended, ~1 keV gas halos with gas masses up to 10 10 Msun , Strong correlation of LX and LB but much scatter. (e.g. Forman et al. 1979, 1985, Canizares et al. 1986)
High central gas densities => short cooling times and infall rates of 0.02-3 Msun/year (Nulsen et al. 1984, Thomas et al. 1986 )
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Hot Gas in Early-type Galaxies - The ROSAT Era
Large ROSAT surveys - 293 galaxies (Beuing et al. 1999); 401 galaxies (O’Sullivan et al. 2001) -low temperature systems have reduced gas fraction
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Hot Gas in Early-type Galaxies - The Chandra - XMM-Newton Era
High spatial resolution shows evidence of AGN outbursts - cavities, shocks/ripples jets, nuclear emission
M84 X-ray + Radio Contours
(Finoguenov & Jones 2001)
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NGC4649 A normal elliptical in Virgo
As expected -- Hot ISM
and binary X-ray sources .Chandra ACIS-S
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With Chandra resolution, X-ray emission can be untangled into stars, LMXBs and hot gas
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Chandra can resolve bright LMXBs
NGC3379 - Revnivtzev et al
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Unresolved X-ray emission in low mass early-type galaxies
Revnivtzev et al A&A 2008
Unresolved X-ray emission is constant per unit stellar mass (top)and per unit K-band luminosity(bottom)
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Use X-ray spectrum to decompose emission
Revnivtzev et al A&A 2008
M32 (dwarf) NGC3379 M87
Spectra normalized to K-band luminosity
Upper gray stripe is LMXBs (Gilfanov 2004)Lower blue stripe is stars
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Hot Gas, Stars & LMXBs in Early-type Galaxies
ROSAT (O’Sullivan et al 2001) Chandra (Revnivtsev et al. )
In luminous ellipticals, most of the X-ray emission is from hot gas,but in the low mass ellipticals, most of the emission is stars and LMXBs
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Galaxies with Hot X-ray Coronae AGN outbursts -- cavities and rising bubbles, shocks Turbulence and non-thermal pressure support?
X-ray and radio emission Sun et al. 2004 Multiple outbursts in N5813
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Centaurus A – Bubbles and Jets
•Nearest active galaxy (3.4 Mpc; 1’’=17pc); Merger with gas rich galaxy
•250 X-ray point sources + nucleus + jet + knots
•X-ray jet with opposing bubble
•Diffuse emission – kT=0.3 keV – typical for “faint”galaxy
•Radio contours show interaction of radio plasma and origin of bubble
Bubble diameter 3 kpc
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Centaurus A – Bubbles and Jets
Deep (600 ksec) Chandra observation (PI Kraft)
•Diffuse emission – kT=0.3 keV , jet, counter-jet , lobes
•Absorption lanes
Bubble diameter 3 kpc
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The Jet in Centaurus A
Many X-ray (blue) knots correspond to radio (red) knots (Hardcastle et al. 2003)
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Centaurus A – Bubbles and Jets
•Counter-jet
•Southern lobe - sharp, smooth
Bubble diameter 3 kpc
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Centaurus A - Southwest Radio Lobe
•Model X-ray bubble as driven by expansion of radio plasma
•Gas temperature in lobe ~2.9 keV (in ISM kT = 0.3 keV)
•Shell gas density 2 10-2 cm-3 (In ISM ~ 2 10-3 cm-3)
•Shell overpressured (2 10-10 dyn cm-2; in ISM ~10-12, in lobe ~10-11)
•Bubble expanding supersonically at Mach 8.5 (2400 km/sec)
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Chandra images of Cen A inner lobes with radio contours
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Cen A lobes (inner and middle)
XMM image shows over-pressured X-ray regions in northern lobe. Northern inner lobe has “popped”. (Kraft et al. 2008)
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Examples of outbursts in early type galaxies -- ages 2 106 - 5 107 years In galaxies most rims are cool. - few shocks.
The rising bubbles are gently imparting energy to the gas (and dragging up
cool material from the core). NGC4636
3 106 years
2 106 years
5 106 years
107 years
NGC5846
5 106 years
3 106 years
5 107years
NGC507
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In galaxies, outbursts are recent (=> frequent) and impart significant energy to the ISM - enough to balance cooling
AGE of outbursts
PV (ergs)1053 1055 1057 1059
Ages and outburst energy for the 27 galaxies/groups with cavities (Nulsen, Jones, Forman, Churazov & friends)
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X-ray emission detected from the nucleus for ~80% of early-type galaxies from asample of 160 galaxies (Jones et al. 2008)
How common are AGN outbursts?Determine fraction with nuclear X-ray emission
In “normal” early-typegalaxies -
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Galaxies with multiple outbursts
NGC5813 with Chandra (Forman et al. 2008)
Multiple outbursts in Cen A, M87
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Multiple Outbursts in NGC4472
NGC4636
3 106 years
2 106 years
107 years NGC5846
5 106 years
3 106 years
Chandra - inner bubblesBiller et al. XMM - large outer bubbles
Kraft et al. 2008
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XMM-Newton image of elliptical galaxy NGC4472
Rims of X-ray bubbles are cool
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What are the impacts of the outbursts on the gas?
Enough energy to reheat the cooling gas? YES
Enough energy to drive the gas from the galaxies?Not usually, but…
Enough energy to provide non-thermal support to gas?Not in small sample studied so far VLA
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Example --- NGC1316 = Fornax A
Large AGN outbursts can remove gas from galaxies
VLAChandra
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First example --- NGC1316 = Fornax A
AGN Outbursts that Remove Gas
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NGC1316 = Fornax A
AGN Outbursts that Remove Gas
N1316
In N1316, X-ray gas is only in the galaxy core, not the halo.
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NGC1316 = Fornax A
AGN Outbursts that Remove Gas
N1316
Scatter in LX-opt mag relation is partly due to gas removal and partly due to environment (galaxies in the centers of groups)
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Eastern Arm - classical buoyant bubblesSequence of small buoyant bubbles•PV ~ 1054 - 1055 ergs
(M87 see Forman et al 2005, 2007)
4.65 kpc
90 cm (Owen et al.)
1.2-2.5 keV
M87
Do outbursts cause turbulence in the gas?
Is there non-thermal pressure support?
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X-ray vs optical potential profiles (Churazov et al. arXiv0711.4686
Optical X-rays
Stars: gravity Gas: gravity, cosmic rays,magnetic fields, turbulence
0.5’’
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)()(),( rPrTrn ee
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ke
ee
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Deprojected X-ray data: gas temperature and density
Gravitational potential depends only on measured quantities-- temperature & gas densityAnd hydrostatic equilibrium!
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€
ϕ X (r) ≈ 0.93ϕ opt (r)
Kronawitter et al.-- Wu & Tremaine-Romanowsky & Kochanek
X-rayX-ray
)(85.0)( rr optX ϕϕ ≈
N1399
M87
At least in N1399 and M87, non-thermal pressure is not significant
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ConclusionsEnergy input from AGN is common in galaxies- reheats cooling gas, can drive gas from their cores/halos, and is
important for galaxy evolution
In luminous ellipticals, ~30% have cavities => recent outbursts - typical ages are 3 106 to 5 107 years - typical outburst energies (estimated from cavity sizes) are 1055 to
1059 ergs
~80% of all early type galaxies have weak X-ray AGN
Several examples of multiple AGN outbursts (Cen A, N5813, N4472)
But (based on small sample), non-thermal pressure support appears to be small (< 15%)