what igm knows about the star-formation... an x-ray perspective

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


Alexis Finoguenov

Ponman, Sanderson, Finoguenov 2003

0.65

Modified scaling: S~T

local groups local clusters Clusters@z=0.3

!

!


Alexis Finoguenov


Alexis Finoguenov

Turbulence

Star-formation feedback

Z=0 Z=2

Borgani, AF, Kay, Ponman, Springel, Tozzi, Voit


Alexis Finoguenov

AGN feedback

Z=0 Z=2


Alexis Finoguenov

Feedback exceeding cooling threshold

Z=0 Z=2


Alexis Finoguenov

!

!

!


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!


Alexis Finoguenov

S

R

HCG 90HCG 90

Trinchieri et al. 2003


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Finding groups at high z:

status report


Alexis Finoguenov

eLH


Alexis Finoguenov

eCDFS


Alexis Finoguenov

Prob. of halo mass structures vs field size

cosm

os

==> > 1 degto sample all structures


Alexis Finoguenov

CosmosSurvey

2 q degrees


Alexis Finoguenov

Most of the structure shows upMost of the structure shows up in XMM imagesin XMM images

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


Alexis Finoguenov

Galaxiesvs

X-raysandWeak

lensing


Alexis Finoguenov

Z ~ 0.73 cluster : DM lensing & X-ray


Alexis Finoguenov

luminous early-type ==> dense core of LSS

COSMOS : environment <==> evolution


Alexis Finoguenov

Galaxy groups w/ XMM at z > 0.5 (h) and z<0.5 (l) : ACS images


Alexis Finoguenov

ABC of Metals in clusters: distribution


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


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


Alexis Finoguenov

A 3667:Metallicity vs entropy


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


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


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


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


Alexis Finoguenov

Galaxy Population and Environment

Kodama et al. 2001

Clusters accumulate the products of early star formation


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


Alexis Finoguenov

Mass-to-light ratios


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


Alexis Finoguenov

Metal Budget

@Z=0


Alexis Finoguenov

Coma outskirts

Finoguenov, Briel, Henry 2003


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.


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


Alexis Finoguenov

Thank you!

what igm knows about the star-formation... an x-ray perspective

Documents

high z

alexis finoguenovhcg

alexis finoguenovfeedback

lssrole of clusters

various clusters

noncooling flow clusters

fe abundance

solar abundances finoguenov