Extragalactic Astrophysics & Cosmology

Staff: Vincenzo ANTONUCCIO-DELOGU (47 yo., ricercatore astronomo) Ugo BECCIANI (ricercatore astronomo) Alfio BONANNO (ricercatore astronomo)

Postdoctoral fellows: Alessio ROMEO (COMETA fell.) 1/5/2007 → 31/10/2008 Stephane PAULIN-HENRIKSSON (Marie Curie fellow) 1/1/2005 – 31/12/2006

Senior fellows: Dietrich ELSTNER (Marie Curie Fellow/AIP, Postdam, Germany) (2 months) Vadim URPIN (Marie Curie Fellow/St. Petersburg, Russia) (7 months)

Activities 2004 → present

This talk: Scientific achievements Next talk (U. Becciani): Technological support activities Our approach: A synergetic effort, where specific tools are developed in support of science (e.g.VisIVO for cosmological N-body simuls.)

Marie Curie Transfer-Of-Knowledge Project (01/08/2004, 4 years)

COSMOlogy and computational astrophysics at

CaTania astrophysical observatory

Accountable, truly monitored by partners, EC and Peer Reviewers (PRs) Main Target (agreed with PRs): ''...Build up a group with a visible scientific profile which can be, in the long-term, competitive and involve young researchers..'' Strategy: a) NEW research topics – not a prosecution of past activities, not already within the mainstream of other italian groups, BUT not marginal, high impact!

b) Flowchart: 1st and 2nd year: mainly development 3rd and 4th year: production, dissemination and young researchers' training

Partners: University of Oxford (UK) Prof. J. SILK Astrophysikalische Inst. Potsdam (Germany) Dr. S. GOTTLOEBER

COSMOCT: Research

GF in extreme environments (Voids)

Red Sequence, Galaxies-IGM interplay, Fossil groups

Weak Gravitational LensingAGN feedback

MHD instab., Black holes, Early Universe

LX-T relation Iron profiles

I) INTRA-CLUSTER MEDIUM I) INTRA-CLUSTER MEDIUM Cosmological+hydrodynamical simulations of clusters and groups Cosmological+hydrodynamical simulations of clusters and groups

of galaxies of galaxies (2006, MNRAS 371, 548)(2006, MNRAS 371, 548)

modelsobservs.

Role of SN feedback and IMF in modelling the thermal and chemical properties of ICM:

T and S profiles, scaling relations (LX-T), cold

fraction, M/L, metal gradients

need enhanced feedback to balance cooling ⇒ lowers X-ray emissivity

& strengthens iron diffusion in the ICM

LF EVOLUTION

passive (L) + dynamic (M)

Monolithic Hierarchical

LF in B & K band

Mass Function:merging onto CD

II) GALAXY POPULATIONS II) GALAXY POPULATIONS (2005, (2005, MNRAS 361, 983MNRAS 361, 983))

z=0 <--> z=1

III) RED SEQUENCE

Colour-MagnitudeColour-Magnitude

Metallicity-LuminosityMetallicity-Luminosity:fainter metal-poorer

Age distribution: no trend (brighter are coeval)

Metallicity-MassMetallicity-Mass

“Coma”

GAP ↓

CD

IV) FOSSIL GROUPSIV) FOSSIL GROUPS

(2005, ApJ 630, L109)

• Lower star formation, assembled earlier: “fossilness” (gap) opens at z~0.7

New MHD instability in differentially rotating disks:New MHD instability in differentially rotating disks:

(Bonanno & Urpin, ApJ, 2007)(Bonanno & Urpin, ApJ, 2007)

The only necessary condition is a

non vanishing toroidal and poloidal

field in a differentially rotating plasma

Efficient when the sound speed is of

the order of the Alfven speed.

Not suppressed by a strong field

Dispersion relation of the new

instability

Unstable (Re() > 0

Spacetime structure of an evaporating BH:Spacetime structure of an evaporating BH:The final state of the Hawking process The final state of the Hawking process

(Bonanno & Reuter Phys. Rev. D, 2006)(Bonanno & Reuter Phys. Rev. D, 2006)

The final state of the evaporation is

a cold Planck size remnant according

to Quantum Einstein Gravity

Final state: a single particle m ~

mplanck

Penrose diagram of the BH

evolution

Quantum Gravity in the Early Universe:Quantum Gravity in the Early Universe:Astrophysical consequences of non-perturbative renormalization of quantum gravity Astrophysical consequences of non-perturbative renormalization of quantum gravity

(Bonanno & Reuter Phys. Rev. D 2007)(Bonanno & Reuter Phys. Rev. D 2007)

Time

•Planck epoch

now

The entropy of the Universe as a

quantum gravity effect in the Early

Universe

Inflation is produced without

scalar field in a short time interval

No reheating is needed to explain

the CMB spectrum

Ent

rop

y

Galaxy populations in Voids(G. Sorrentino, V. A.-D. and A. Rifatto, A&A 460, 673 [2006])

Question: Is galaxy formation in Voids different from Clusters? (ref.: Peebles 2001)

Tools: 1) > 90,000 gal. (r, u-r) and spectra from SDSS-DR42) ~ 7,000 gals. in Voids - truly 3D selection!

Void

Environm. density

Cluster centers

Morph-dens. Rel. (Oemler)

RESULTS: 1) No specific “Void Pop.” found (cf. Peebles, 2001)

2) SF efficiency higher in Voids (cf. Baldry et al., 2004; Bernardi et al., 2003)

Dark Energy Task Force (DETF http://home.fnal.gov/~rocky/DETF/) +

ESO-ESA Working Group on Fundamental Cosmology:Weak Lensing is complementary to BAO as primary tool to assess Geometry and Matter content of the Universe

ESA/Cosmic Vision DUNE mission selected (merging with SPACE, October '07)

Why Weak Lensing ?

What is Weak Gravitational Lensing ?

A pure GR tool to detect and measure Dark Matter Challenge: measure dev. from isotropic distr. of background (z 2-

3) galaxy images shapes with rel. accuracy ~ 10-3

“Lens” (gravity)

observer

Bkg. gals.

WL Shear Pipeline:

<images>...

Input

Mass Map

Weak Gravitational Lensing

I. The KBS+/OACt pipeline MNRAS, 376, 13 [2007]; A&A 467, 427 [2007]

Shape: 2nd order moments Source ↔ Observed Qij

Reduced shear

Source ↔Observed

Smoothed Qij

• r

g

Linear appr. (Weak Lensing)

Smearing ↔ anisotr. PSF

qstellar shapes

: original contribs. to KSB+ from OACt pipeline

Weak Gravitational Lensing STEP2 project: KSB+/OACt, TS

and JB are the only marginally (to 1) compatible with ideal result (bias≃2%, June '07) Anisotropic PSF: KSB+/OACt

improves (bias 1.5%)

MNRAS,submitted (09/07)

STEP2: almost isotropic PSF

Dark Matter in Abell 209 substructure!WL mass reconstruction:M

WL(<R

vir) =7.7 (+4.3, -2.7) h

70-1 1014M⨀

MX = 3.3 0.55 1015 h

70-1 M⨀

(Mx>M

WL: see e.g. Cypriano et al. [2004])

A&A 467, 427 [2007]Ellipticals

Spirals

WL DM contours

Active Galactic Nuclei feedback:How Black Holes change their host galaxies

Relativistic jets

from BHs enter the

Interstellar medium

and shock the

existing clouds

Silk (2005): high -z

jet-induced star

formation

Simulations of rel. jet-cloud interactions(V. A.-D. and J. Silk, MNRAS 2007, accepted)

FLASH 2.5 / Adaptive Mesh refin., lmesh

= 7.25 h-1 pc

SD '93 cool. func., th. cond (10-1 * Spitzer), Z=0.3

27 h-1 kpc

Cloud compression within the cocoon

• Multicloud simulations Model of the ISM Suppression/Stimulation of Star Formation Rate

1043 < Pjet < 1046 ergs sec-1, ne = 1 e- cm-3

AGN-induced suppression of star formation

Effective on tjet ~ few times 106 yrs., typical of the observed rejuvenation effects in CM diagram of Early Type gals. (Kaviraj et al., 2006; Schawinski et al, astro-ph 0709.3015)

10-2 < ne < 1 e- cm-3, Pjet = 1043

COSMOCT: Teaching/Training activities

V. A.-D: a) Sabbatical leave to Oxford (1/8/2006-31/7/2007) b) Course: “Introduction to Phys. Cosmology”, Scuola Superiore di Catania, (2nd semester AY 2007-2008)

U. Becciani: a) Graduate course: “Computational Physics”, University of Catania, School of Grad. Studies in Physics (AY 2006-2007)

A. Bonanno: a) Leave to AI Potsdam (1/6-31/7/2006) b) Course: “General Relativity”, University of Catania, (1st semester AY 2007-2008)

Note: not paid courses.

COSMOCT: Workshops/Schools

1st INAF-COSMOCT Autumn School on Gravitational LensingAcireale (CT), 30/10-3/11 2006 http://www.oact.inaf.it/gl/ 8 lecturers from Europe, 3 from USA 30 participants from all EU countries

Workshop on MHD Laboratory Experiments for Geophysics and AstrophysicsCatania, 1-3/10/2007 http://www.oact.inaf.it/couette07/index.html 60 participants

Oxford-COSMOCT Workshop on AGN feedback on host galaxies: Observations and ModellingVulcano Island (Me), 19-23/5, 2008

COSMOCT: Collaborations

Dark UNiverse Explorer (DUNE) – selected by ESA/Cosmic Vision (+ SPACE) Simulations of effectiveness of WL mass reconstr. of Clusters V. A.-D, S. Paulin-Henriksson (DUNE/WL WG)

ESO: Multi-band deep survey of 2 FG candidates NGC5044 & RXJ0116 with WFI at ESO 2.2m

STEP 2,3 (Heymanns et al., 2004 ongoing) KSB+/OACt test of different WL pipelines

Starting: INAF-IASF, Palermo (A. Pagliaro, B. Sacco, C. Maccarrone) + INFN/CT (AUGER, A. Insolia/ G. Medina-Tanco, UAM): Simulations of p acceleration from jets' hotspots