Planck and Superclusters

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Planck and Superclusters

• Tartu observatory Tuorla observatory

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• Total mass-energy density of the Universe
• Dark energy (73)
• Dark matter(23)
• Baryons(4)

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At zgt2 all baryons are found in the Lya forest,
but about 45 of the baryons zlt2 are missing
(infered from stars,atomic and molecular gas,
dust, plasma in clusters)
Distribution of baryons in the local Universe is
one of the open questions in cosmology.
Nicastro et al. 2008, Science
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• Theoretical and numerical work has been predicted
  most of these missing baryons should be in a
  plasma with temperatures 105 and 107 K in
  filaments connecting the clusters (in regions
  with moderate overdensities) (CenOstriker 1999,
  2006)
• - WHIM (Warm-Hot Intergalactic Medium) -
• An important contribution to the diffuce
  emission and WHIM is expected to reside in
  superclusters (SC).

Croft et al. 2001
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• Detection of WHIM is challenging
• Different methods
• -Soft X-ray emission
• -Absorption lines in X-ray and UV quasar spectra
• -Thermal Sunyaev- Zeldovich effect on CMB photons
  

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• PLANCK
• WG5 Clusters and secondary anisotropies
• -SZ cluster cataloque
• -Multi-wavelength cluster
  science
• -Gravitational lensing
• -Reionisation
• -ISW recovery
• -Large-scale structure

• the intensity change of the
• CMBR caused by
• the SZ-effect is proportional to
• the comptonization parameter y

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• Galaxy clusters y10-4
• Small groups, faint protoclusters y510-6
• Total ltygt1.2 10-6
• ltygtWHIM710-7
• ? 60 of the total value of the y-parameter is
  originated by WHIM gas (half of that closer than
  zlt1).
• Hernandez-Monteagudo et al. 2006
• About 80 of tSZ is generated in collapsed
  structures, 15 in SC and filaments

Refregier and Teyssier 2002
Roncarelli et al. 2007 simulations
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• Studies of diffuse and kinetic SZ signals
  
• Objectives (some of them)_
• Analysis of the residual y-map after cluster
  extraction
• large-scale filamentary structure of the
  WHIM
• individual superclusters

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Hernandez-Monteagudo et al. 2006, ApJ
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Our contribution

• To produse supercluster maps from the
  observations and simulations using
  luminosity-density method 2dF, SDSS, 2MASS,
  UKIDSS.

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Done before

• Einasto et al. 2003, AA, 405, 425
• Einasto et al. 2007, AA, 462, 811
• Tago et al. 2006, AN, 327, 365
• Tago et al. 2007 submitted

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1. Catalogue

• As a basis, a SDSS DR5 catalogue of
• groups and isolated galaxies (Tago et
• al. 2007) for the survey region was used.
• 5740 sq.deg about 14 of the sky
• z0.009 0.12
• Such a catalogue includes all survey
• galaxies, but positions group and
• cluster galaxies at the mean group
• cluster distance, suppressing the
• redshift space fingers.
• SDSS DR6 7425 sq.deg.
• 2dF about 2000 sq.deg.
• 2MASS all sky, near infrared
• PSCz (Iras)

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2. Luminosities

• Calculation of the expected total luminosities of
  galaxies.
• We assume that every galaxy is a visible member
  of a density enhancement
• (group or cluster). This allows to correct the
  galaxy luminosities for the
• observational magnitude limited samples by a
  weighting factor that takes into
• account the luminosities of galaxies outside of
  the visibility window
• LtotLobsWL
• Lobs is the luminosity of an observed galaxy
• WL is the ratio of the expected total
  luminosity to the expected
• luminosity in the visibility window L ?L1,L2
  at the distance of the group
• LF by Norberg et al. (2002) for the 2dFGRS and
  Blanton et al. (2003) for the SDSS.

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• This procedure yields a total mean
• luminosity density that is approximately
• independent of the distance from the
• observer.
• There are also several caveats e.g., the
• narrow magnitude window of the SDSS
• leads to very high correction factors
• using these would make the density
• correction-dominated. Recently we have
• used the rule if (WLgt3) then WL3. This,
• however, limits the region where the
• estimated density is unbiased,
• approximately by 100ltDlt300 ,(Mpc/h).

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3. Density grid

• A Cartesian grid with a step of 1h-1 Mpc (the
  characteristic size of compact galaxy systems --
  groups and clusters) is defined within and around
  the survey volume (grid size optional)

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4. Luminosity density maps

• The luminosity density field is calculated, using
  the 3 dimensional B3 kernel of the radius (1-16
  Mpc/h), centred on the galaxies -- groups. For
  superclusters 8-16 Mpc/h.

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• All-sky map in the Healpix format. Luminosity
  density distribution separated by distance layers
  (example 200-300 Mpc)

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400-500 Mpc
300-400 Mpc
200-300 Mpc
100-200 Mpc
0-100 Mpc
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5. Superclusters

• In order to delimit supercluster, a threshold
  luminosity density D0 (in units of mean
  luminosity density), and a minimal supercluster
  volume V0 were chosen.
• D04.6, V0200 Mpc3/h3 (Einasto et al. 2007 AA
  462, 811, AA 462, 397)

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6. Supercluster maps

• The total supercluster luminosity Ltot was found
  by summing over all the grid
• vertices within supercluster boundaries.
• For every supercluster, the galaxies and groups
  inside the supercluster
• boundaries were selected -? cluster data,
  optical, x-ray, radio

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Individual supercluster maps in the FITS binary
table extension format Tables contains name, ra,
dec, mean distance,total luminosity/mass
estimation, size, reference for known x-ray
clusters, sky map
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