Extragalactic Astrophysics

1
Extragalactic Astrophysics Cosmology
Activities 2004 ? present

• 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)?

• 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.)?

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Marie Curie Transfer-Of-Knowledge Project
(01/08/2004, 4 years)? COSMOlogy and
computational astrophysics at CaTania
astrophysical observatory

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

• 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
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COSMOCT Research
AGN feedback
Weak Gravitational Lensing
Red Sequence, Galaxies-IGM interplay, Fossil
groups
GF in extreme environments (Voids)
MHD instab., Black holes, Early Universe
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I) INTRA-CLUSTER MEDIUM Cosmologicalhydrodynam
ical simulations of clusters and groups of
galaxies (2006, MNRAS 371, 548)?
observs.
models
LX-T relation
Iron profiles
need enhanced feedback to balance cooling ?
lowers X-ray emissivity strengthens iron
diffusion in the ICM

• 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

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II) GALAXY POPULATIONS (2005, MNRAS 361, 983)?
LF EVOLUTION passive (L) dynamic (M)
Monolithic Hierarchical
z0 lt--gt z1
Mass Function merging onto CD
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III) RED SEQUENCE
Colour-Magnitude
Metallicity-Mass
Coma
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IV) FOSSIL GROUPS (2005, ApJ 630, L109)

• Lower star formation, assembled earlier
  fossilness (gap) opens at z0.7

GAP ?
CD

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New MHD instability in differentially rotating
disks (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

Unstable (Re(?) gt 0
Dispersion relation of the new instability
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Spacetime structure of an evaporating BH The
final state of the Hawking process (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
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Quantum Gravity in the Early Universe Astrophysic
al consequences of non-perturbative
renormalization of quantum gravity (Bonanno
Reuter Phys. Rev. D 2007)?

• 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

• Planck epoch

Entropy
now
Time
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Galaxy populations in Voids (G. Sorrentino, V.
A.-D. and A. Rifatto, AA 460, 673 2006)?
Question Is galaxy formation in Voids different
from Clusters? (ref. Peebles 2001)?
Environm. density
Tools 1) gt 90,000 gal. (r, u-r) and spectra
from SDSS-DR4 2) 7,000 gals. in Voids - truly
3D selection!
Void
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)?
Cluster centers
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Why Weak Lensing ?

• 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)?

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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

Bkg. gals.
Lens (gravity)?
WL Shear Pipeline
???????ltimagesgt...
?
Input
observer
Mass Map
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• Weak Gravitational Lensing
• I. The KBS/OACt pipeline
• MNRAS, 376, 13 2007 AA 467, 427 2007

?

Shape 2nd order moments
Reduced shear
Source ? Observed Qij
?
?

• ????rg

Smoothed Qij
Source ??Observed ?
Linear appr. (Weak Lensing)?
q??????stellar shapes
?
Smearing ? anisotr. PSF
?
original contribs. to KSB from OACt pipeline
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Weak Gravitational Lensing
STEP2 almost isotropic PSF

• 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)?

WL DM contours
AA 467, 427 2007
Ellipticals
MNRAS,submitted (09/07)?

• Dark Matter in Abell 209 substructure!
• WL mass reconstruction
• MWL(ltRvir) 7.7 (4.3, -2.7) h70-1 ?1014M?
• MX 3.3 ? 0.55 ??1015 h70-1 M?
• (MxgtMWL see e.g. Cypriano et al. 2004)?

Spirals
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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

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Simulations of rel. jet-cloud interactions (V.
A.-D. and J. Silk, MNRAS 2007, accepted)?
27 h-1 kpc

• FLASH 2.5 / Adaptive Mesh refin., lmesh 7.25
  h-1 pc
• SD '93 cool. func., th. cond (10-1 Spitzer),
  Z0.3

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Cloud compression within the cocoon

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

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AGN-induced suppression of star formation

1043 lt Pjet lt 1046 ergs sec-1, ne 1 e- cm-3
10-2 lt ne lt 1 e- cm-3, Pjet 1043

• 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)?

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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.
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COSMOCT Workshops/Schools

• 1st INAF-COSMOCT Autumn School on Gravitational
  Lensing
• Acireale (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 Astrophysics
• Catania, 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 Modelling
• Vulcano Island (Me), 19-23/5, 2008

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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