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X-IGM vs starformation
Alexis Finoguenov
What IGM knows about the star-formation... An X-ray perspective.
A. Finoguenov (MPE)• Bookkeeping of energy and metal ejection
• IMF+AGN-cooling• Tracing the LSS• Role of clusters in the chemical evolution of the Universe
Studying the Cosmic Galaxy and Star Formation History
galaxypopulation
Protocluster
star bursts at z ~ 3 - 7
Cluster
early type galaxies at z ~ 0 (with a very old stellar population)
FeSi
entropy
Star formation rate
X-IGM vs starformation
Alexis Finoguenov
Ponman, Sanderson, Finoguenov 2003
0.65
Modified scaling: S~T
local groups local clusters Clusters@z=0.3
!
!
X-IGM vs starformation
Alexis Finoguenov
X-IGM vs starformation
Alexis Finoguenov
X-IGM vs starformation
Alexis Finoguenov
Turbulence
Star-formation feedback
Z=0 Z=2
Borgani, AF, Kay, Ponman, Springel, Tozzi, Voit
X-IGM vs starformation
Alexis Finoguenov
AGN feedback
Z=0 Z=2
X-IGM vs starformation
Alexis Finoguenov
Feedback exceeding cooling threshold
Z=0 Z=2
X-IGM vs starformation
Alexis Finoguenov
!
!
!
X-IGM vs starformation
Alexis Finoguenov
Reproduction of Reproduction of scaling in simulations scaling in simulations
with galactic windwith galactic wind
300 km/s
800 km/s
800 km/s
300 km/s!
X-IGM vs starformation
Alexis Finoguenov
S
R
HCG 90HCG 90
Trinchieri et al. 2003
X-IGM vs starformation
Alexis Finoguenov
Finding groups at high z:
status report
X-IGM vs starformation
Alexis Finoguenov
eLH
X-IGM vs starformation
Alexis Finoguenov
eCDFS
X-IGM vs starformation
Alexis Finoguenov
Prob. of halo mass structures vs field size
cosm
os
==> > 1 degto sample all structures
X-IGM vs starformation
Alexis Finoguenov
CosmosSurvey
2 q degrees
X-IGM vs starformation
Alexis Finoguenov
Most of the structure shows upMost of the structure shows up in XMM imagesin XMM images
Median z
Median z
XMM
red -- 0.5-2 kev
green -- 2-4.5 kev
blue -- 4.5-10kev
1000 sources detected
Diffuse
sources
Galaxiesvs
X-rays
X-IGM vs starformation
Alexis Finoguenov
Galaxiesvs
X-raysandWeak
lensing
X-IGM vs starformation
Alexis Finoguenov
Z ~ 0.73 cluster : DM lensing & X-ray
X-IGM vs starformation
Alexis Finoguenov
luminous early-type ==> dense core of LSS
COSMOS : environment <==> evolution
X-IGM vs starformation
Alexis Finoguenov
Galaxy groups w/ XMM at z > 0.5 (h) and z<0.5 (l) : ACS images
X-IGM vs starformation
Alexis Finoguenov
ABC of Metals in clusters: distribution
X-IGM vs starformation
Alexis Finoguenov
Abundance Gradients (Beppo-SAX)
Metallicity Gradients in non-cooling flow clusters and cooling flow clusters [DeGrandi & Molendi 2001]
- these metallicity measurements refer essentially to the Fe abundance !
Clusters without cooling flows
Clusters with cooling flows
X-IGM vs starformation
Alexis Finoguenov
Finoguenov et al. 2000Finoguenov et al. 2000
•The central enhancement is more The central enhancement is more enriched by SN Ia than the outer enriched by SN Ia than the outer parts of the ICM parts of the ICM
• In the outer regions the metals in In the outer regions the metals in the ICM are dominated by the the ICM are dominated by the contribution from SN IIcontribution from SN II ! !
SN Ia
SN II
[Si/Fe]
Radial Abundance Variations of Fe and Si in Various Clusters and
Groups
X-IGM vs starformation
Alexis Finoguenov
A 3667:Metallicity vs entropy
X-IGM vs starformation
Alexis Finoguenov
Metals in clusters:
sources
XMM Observations of the X-ray Halo of M87
Böhringer et al. 2001, 2002
Matsushita et al. 2002a, b
Finoguenov et al. 2002
Sakelliou et al. 2002
O & Si Abundance Profiles in M87
The O profile is almost flat (consistent with a flat profile within +- 10 %)
The O/Si ratio increases from about 0.4 to 0.7 (from r = 2 – 50 kpc)
- (using MEKAL models)
Si
1-temp
O Si
Matsushita, Finoguenov, Böhringer 2002
2-temp
X-IGM vs starformation
Alexis Finoguenov
Metal Abundances in M87
1´ - 3´
8´ - 16´
Radial Zones :M
eta
ls n
orm
aliz
ed
to s
ola
r ab
un
dan
ces
Finoguenov, Matsushita, Böhringer, Ikebe, Arnaud 2002
Two types of SN as ICM Poluters
SN Type IIM* > 8 Msun
SN Type Ia
Fe- group elements dominate - elements dominate
X-IGM vs starformation
Alexis Finoguenov
Decomposition of the Metal Abundances into Contributions from SN Ia and SN II
SN Ia SN II
Finoguenov, Matsushita, Böhringer et al. 2002 A&A 381, 21
Inner region
Outer region
X-IGM vs starformation
Alexis Finoguenov
Conclusion from the Abundance Pattern• Most of the Fe in the center comes from SN Ia -- This Fe can be produced by SN Ia from M87 within the last 1 - 2 Gyr (with a Cappelaro rate of SN in early type galaxies)
• The abundance pattern clearly favor slow deflagration/detonation models – with incomplete burning of the -elements
• Second order effect: there may be a variation in the types of SN Ia (later SN Ia show on average more -elements -- slower explosions)
• The total Fe contribution by SN II falls about a factor of 1.5-2 short in explaining the wide-spread Fe abundance with classical IMF models
we can test chemical evolution parameters
we can test SN-nucleosynthesis models
Information on the Star Formation Rate in Cluster Early-Type Galaxies
bluer
brighter[Bender et al. ‘98]
[Bender & Ziegler ‘97]
Ellis et al. ‘97
Fundamental plane
Information on the Star Formation Rate in Cluster Early-Type Galaxies
bluer
brighter[Bender et al. ‘98]
[Bender & Ziegler ‘97]
Ellis et al. ‘97
Ellipticals snd S0s in distant clusters are somewhat brighter and bluer than nearby – consistent with passive evolution !
Most star formation at z>3 !!
Fundamental plane
X-IGM vs starformation
Alexis Finoguenov
Galaxy Population and Environment
Kodama et al. 2001
Clusters accumulate the products of early star formation
X-IGM vs starformation
Alexis Finoguenov
Observational aspects of stellar IMF
• mass function of stars• Stellar mass-to-light ratio and ist evolution
• High-mass to intermediate mass star ratio
• Metal production per unit of remaining stellar light
• Weighting among massive stars
X-IGM vs starformation
Alexis Finoguenov
Mass-to-light ratios
X-IGM vs starformation
Alexis Finoguenov
Larson IMF in clusters and metal-poor stars
35.1
1~log
−
⎟⎟⎠
⎞⎜⎜⎝
⎛+
smm
mddN
Padoan IMF
AF, Burkert, Böhringer 2003Hernandez, Ferrara 2002
Z production
weighting
X-IGM vs starformation
Alexis Finoguenov
Metal Budget
@Z=0
X-IGM vs starformation
Alexis Finoguenov
Coma outskirts
Finoguenov, Briel, Henry 2003
X-IGM vs starformation
Alexis Finoguenov
Summary • Fossil records study consistently require both strong feedback and top heavy IMF at high-z
• Protoclusters are sights of missing metals at high-z, which are at high temperatures
• Feedback energy, released at high-z, appears to cool down by now.
• Observations of groups support AGNs as a dominant source of feedback.
• Current deep surveys are capable of finding and study groups at high-z.
X-IGM vs starformation
Alexis Finoguenov
Coauthors
• H.Böhringer, P.Schuecker, M.Zimer, Y.Zhang, G. Hasinger (MPE)
• A.Burkert (LMU)• T. Ponman, J. Osmond (Bham)• S. Borgani, L. Tornatore (Trieste)• V. Springel (MPA)• M. Voit • P.Rosati (ESO)
Roberto AbrahamMasaru AjikiJustin AlpertHerve AusselJosh BarnesAndrew BlainDaniela CalzettiPeter CapakJohn CarlstromChris CarilliAndrea CimattiAndrea ComastriMarcella CorolloEmannuel DaddiRichard EllisMartin ElvisAmr El ZantShawn EwaldMike FallAlexis Finoguenov
Alberto FranceschiniMauro GiavaliscoRichard GriffithsGigi GuzzoGunther HasingerChris ImpeyJean-Paul KneibKarel NelJin KodaAnton KoekemoerAlexie LeauthaudOlivier LeFevreIngo LehmannSimon LillyThorsten LiskerCharles LiuRichard MasseyHenry McCrackenYannick MellierSatoshi MiyazakiBahram MobasherTakashi Murayama
Colin NormanAlexandre RefregierAlvio RenziniJason RhodesMike RichDave SandersShunji SasakiDave SchminovichEva SchinnererNick ScovilleMarco ScodeggioKartik ShethPatrick ShopbellJames TaylorDave ThompsonNeil TysonMeg UrryYoshi TaniguchiLudovic Van WaerbekePaolo VettolaniSimon WhiteLin Yan
COSMOS -- team & collaborators
X-IGM vs starformation
Alexis Finoguenov
Thank you!