Status and perspec-ves of AP in Spain: Cosmology
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Status
and
perspec-ves
of
AP
in
Spain:
Cosmology
Francisco Prada
Campus
of
Interna-onal
Excellence
UAM+CSIC
Ins-tuto
de
Física
Teórica
(UAM/CSIC)
Ins-tuto
de
AstroGsica
de
Andalucía
(CSIC)
Granada,
Nov
27th
2012
Outline • Science mo-va-on • Current and future experiments: Spain par-cipa-on • Theory and Simula-on efforts • Remarks
Accelerated expansion of the Universe
(Ωm , ΩΛ) = (0.27, 0.73)
Hubble Diagram
http://supernova.lbl.gov/ ORM, La Palma -‐ ICTS Acknowledgements
Observational evidences
Matter-Energy
WMAP
Density of the Universe
BOSS
BOSS+WMAP+SN
Top Scientific Objectives
The two highest level questions in the field are the following:
• Is cosmic acceleration caused by a breakdown of GR on cosmological scales, or is it
caused by a new energy component with negative pressure ("dark energy") within
GR?
• If the acceleration is caused by "dark energy," is its energy density constant in space
and time and thus consistent with quantum vacuum energy or does its energy
density evolve in time and/or vary in space?
Main Goals
For physical cosmology, the clearest path forward is to measure the history of cosmic expansion and
the growth of dark matter clustering over a wide range of redshifts with the highest achievable
precision, searching for deviations from the concordance model based on GR and a cosmological
constant for a spatially flat universe, i.e. Lambda Cold Dark Matter (ΛCDM):
H 2 (z)
= !m (1+ z)3 + !r (1+ z)4 + !DE Friedmann equa-on
for
the
expansion of a
H0 2 homogeneous and isotropic flat universe
Supernova surveys measure the distance-redshift relation using "standardized candles" whose
luminosities are calibrated by objects in the local Hubble flow. Redshift surveys (e.g. BOSS and other
upcoming future experiments), on the other hand, employs a "standard ruler," the BAO feature
imprinted on matter/galaxy clustering by sound waves that propagate through the baryon-photon fluid
in the pre-recombination universe .
The current BAO distance-redshift relation. The flat ΛCDM
Measuring DA(z) and H(z) prediction from the best-fit WMAP7 model is also shown.
The BAO scale can be computed, in absolute units, using physics and cosmological parameters that are well constrained by cosmic microwave background measurements. BAO are predicted to appear as a bump in the matter correlation function at a comoving scale corresponding to the sound horizon (r = 153.2 ± 1.7 Mpc; WMAP) or as a damped series of oscillations in the matter power spectrum.
Current & Future Surveys: Galaxies & QSOs
BigBOSS
Euclid
Cosmology from galaxy & QSO surveys
What
are
the
cons-tuents
of
maZer?
What
is
the
physics
of
infla-on?
e.g.
neutrino
mass,
primordial
P(k)
What
is
the
expansion
rate
of
the
Universe?
e.g.
quintessence,
Λ
Understanding
accelera-on
RedshiX-‐Space
distor-ons
How
does
structure
form
Galaxy
RedshiX
within
this
background?
Survey
e.g.
modified
gravity,
GR
Is
the
Universe
homogeneous
on
large
scales?
e.g.
Non-‐Gaussianity
Other
non-‐cosmology
science
e.g.
galaxy
forma-on
&
evolu-on
10
Current & Future Surveys: CMB & X-rays
South Pole Telescope eROSITA
Current & Future Surveys:
21cm fluctuations and 21cm redshift surveys
LOFAR
MWA
SKA
Approved ongoing and future cosmology projects
SURVEYS Method Leading Status
[S] VIPERS RSD EU 2009-2015
[S] SDSS-III BOSS BAO/RSD/Lya USA 2009-2014
[Ipz] VST/KIDS WL, SN, Clusters, EU 2011-2016
BAO
[Ipz] DES WL, SN, Clusters, USA Late 2012-2017
BAO
[S] HETDEX BAO USA 2013-2015
[S] eBOSS BAO/RSD/Lya USA 2014-2020
[Ipz] Subaru HSC WL, SN, Cluster Japan ----
[S] Subaru PFS BAO Japan ----
[I+S] Euclid WL, BAO, SN EU 2020-2027
[S] BigBOSS BAO/RSD/Lya USA 2018-2022
[S] 4MOST BAO EU 2018-2022
[Ipz] LSST WL, SN, Clustering USA 2020-2030
[Ipz] PAU BAO Spain construction
[Ipz] J-PAS BAO Spain construction
[R] DESpec BAO/RSD USA ----
[X] eROSITA Clusters EU 2014-2019
[R] LOFAR Radio sources, EU 2013-2018
21cm fluctuations
[R] SKA 21cm galaxy survey Global 2019-onwards
[I] SCP SNe USA 2014-2017
[I] SN Factory, PFT, SNe USA Up to 2018
QUEST
[I] SkyMapper SNe Australia 2014-2019
[I] Pan-Starrs PS1 WL, SNe, USA 2010-onwards
Clustering
[M] Planck CMB EU ongoing
[M] SPT, ACT (CMB) SZ, Pol USA ongoing
[M] Quijote (CMB) Pol Spain ongoing
[21cm] EDGES,BOABAB, 21cm fluctuations USA/Australia ongoing
PAPER, MWA
[S] spectroscopic, [I] imaging, [Ipz] imaging photo-z,
[X] X-ray, [M] Microwave, [21cm] neutral hydrogen 21cmDark energy: theoretical aspects
Model Building & Simulations
Is there a more fundamental theory for cosmic acceleration?
Gµν
+
GµνMG = 8πG (Tµν +Tµν DE)
Modified
gravity
Dark
energy
Mul.Dark
Run
1
Working Projects or in Commissioning Phase
with Spanish ParticipationSDSS-‐III
Collabora-on:
BOSS = Baryon Oscillation Spectroscopic Survey
Spanish Participation Group (IFIC,
UB-ICREA, MultiDark: IFT-UAM/CSIC)
First BOSS spectroscopic data release, DR9 @ Jul 2012
http://www.sdss3.org/BOSS Galaxy clustering statistics
Turnover in the power spectrum
Anderson
et
al.
2012
Wiggles in the power spectrum
SDSS-‐III/BOSS
P(k)
Galaxy Sky Map
Sanchez
et
al.
2012
2-‐pt
CF
Bump in the CF
http://www.sdss3.org/
Galaxy Redshifts Zero Crossing in the CF
17
BOSS Ly-alpha forest results
The Lyman-alpha forest is detected through the
imprint of hydrogen cloud absorpt
ion lines on the light from background quasars.
http://www.sdss3.org/
Baryon
Acous.c
Oscilla.ons
in
the
Ly-‐alpha
forest
of
BOSS
quasarsBOSS Cosmology: first results from DR9!
Ωm –ωDE plane for LDCM redshift The BAO distance-redshift relation divided by the best-fit
-independent value of wDE flat, CDM prediction from WMAP (grey band)
Ly-‐alpha
http://www.sdss3.org/
ω0–ωa plane by allowing for
variations on wDE(a)DES:
The
DARK
ENERGY
SURVEY
•
Southern
Hemisphere
5000
deg2
galaxy
survey
in
5
bands
(g,r,I,z,Y)
Op-cal
and
NIR
•
World
leader.
Involves
groups
in
USA,
Spain,
UK,
Brazil,
Germany,
Switzerland.
525
nights
in
5
years
FIRST
LIGHT
IN
SEPTEMBER
2012
Credit: Dark Energy Survey Collaboration
Main
Spanish
Contribu.ons
to
DES
•
Electronics:
–
Design
of
the
Clock
&
Bias
(CIEMAT),
Transi-on
(IFAE/CIEMAT)
and
Master
Control
(IFAE)
Boards
–
Produc-on
and
commissioning
of
the
whole
read-‐out
electronics
for
the
camera:
108
boards,
finished
in
fall
2010
(IFAE/CIEMAT)
–
CCD
characteriza-on
(CIEMAT/IFAE/IEEC)
–
Guider:
develop,
integrate
and
commission
the
camera
guider
algorithm
(IEEC)
•
Simula.ons:
–
Large
scale
simula-ons
of
the
universe
(ICE-‐CSIC)
–
Data
management
(PIC)
–
Data
quality
checks
(CIEMAT)
•
Science:
–
Large
scale
structure
(ICE-‐CSIC,
IEEC,
UAM,
CIEMAT)
–
Photo-‐z
(IEEC,
IFAE)
–
Supernovae
(IFAE)
DES
Science
Reach
Four
Probes
of
Dark
Energy
Forecast
Constraints
on
DE
• Galaxy
Clusters
DES
Equa-on
of
State
• ~100,000
clusters
to
z>1
• Synergy
with
SPT,
VHS
• Sensi-ve
to
growth
of
structure
and
geometry
• Weak
Lensing
• Shape
measurements
of
200
million
galaxies
• Sensi-ve
to
growth
of
structure
and
geometry
• Baryon
Acous.c
Oscilla.ons
Planck
prior
assumed
• 300
million
galaxies
to
z
=
1
and
beyond
• Sensi-ve
to
geometry
• Supernovae
• 30
sq
deg
-me-‐domain
survey
Factor
3-‐5
improvement
over
• ~4000
well-‐sampled
SNe
Ia
to
z
~1
Stage
II
DETF
Figure
of
Merit
• Sensi-ve
to
geometry
The Planck mission
ØMedium
size
mission
of
the
ESA
scien-fic
program.
ØPlanck will provide all-sky measurements
of the microwave sky with unprecedented
sensitivity, resolution and spectral range.
ØTwo instruments (each one provided by an
international consortium):
• Low Frequency Instrument, LFI
PI: R. Mandolesi, INAF/IASF, Bologna Herschel
LFI is still functioning (until 2013-2014)
• High Frequency Instrument, HFI
PI: J.L. Puget, IAS, Paris Planck
HFI was switched-off on January 2012
ØSpanish contribution to the two
instruments
Ø Launched, together with Herschel, in an
Ariane 5: 14 May, 2009Spanish contribution to the instruments
Ø IFCA (UC-CSIC) + DICOM (UC) + DTSC (UPC), E. Martínez-
González (Co-I LFI), E. Artal (technical responsible)
BEM (Back End Module) of the 30 and 44 GHz radiometers
Ø IAC, R. Rebolo (Co-I LFI)
REBA (Radiometer Electronic Box Assembly), REBA
software and software of data compression onboard of LFI
Ø Univ. of Granada, E. Battaner (Co-I HFI)
Preregulator for the 4 K cooling system of the HFI
There
is
also
an
important
Spanish
contribu-on
to
the
scien-fic
exploita-on
of
the
data!
Scientific Objectives of the Planck mission Ø Measure the temperature and polarization anisotropies with unprecedented resolution and sensitivity Ø Determine the cosmological parameters with errors of ≤ 1%: ΩΛ, Ωm, Ωb, H0, τ, ns, A Ø Confirm (or maybe rule out) the concordance model Ø Determine the inflationary model parameters Ø Constrain the gravitational wave background Ø Test the isotropy and Gaussian hypotheses (e.g. search for topological defects)
Full sky maps of foreground emission
after 1 year mission
Planck all channels
First
cosmological
results
will
be
published
in
early
2013
(probably
March)!
The QUIJOTE CMB experiment
IP:
Rafael
Rebolo
Scien-fic
goals:
* FGI and second telescope funded by the project Consolider-Ingenio 2010 “EPI”
First
light
of
the
Instrument
I
(MFI)
on
November
6th,
2012.
Instrument
II
(TGI)
expected
for
end
2013.
Instrument
III
(FGI)
expected
for
mid
2014.
The QUIJOTE CMB consortium
( http://www.iac.es/project/cmb/quijote )
Ins.tuto
de
AstroXsica
de
Canarias
R.
Rebolo
(PI),
J.A.
Rubiño-‐Marvn
(PS),
R.
Génova-‐Santos,
R.
Hoyland
(InstS),
A.
Perez
(PM),
F.
Gómez-‐Reñasco,
M.
Aguiar,
C.
López-‐Caraballo,
A.
Pelaez,
V.
Sanchez,
A.
Vega,
T.
Viera
Ins.tuto
de
Física
de
Cantabria
E.
Marvnez-‐González,
P.
Vielva,
D.
Herranz,
F.J.
Casas,
B.
Barreiro,
R.
Fernández-‐Cobos,
M.
López-‐Caniego,
D.
Or-z
García
Departamento
Ingeniería
de
Comunicaciones
E.
Artal,
B.
Aja,
J.L.
Cano,
L.
de
la
Fuente,
A.
Mediavilla,
J.P.
Pascual,
E.
Villa
Jodrell
Bank
Observatory
L.
Piccirillo,
B.
Maffei,
G.
Pisano,
R.A.
Watson,
R.
Davis,
R.
Davies,
C.
Dickinson
University
of
Cambridge
M.
Hobson,
M.
Brown,
A.
Challinor,
K.
Grainge,
A.
Lasenby,
R.
Saunders,
P.
ScoZ
IDOM
G.
Murga,
C.
Gómez,
A.Gómez,
J.
Ariño,
R.
Sanquirce,
J.Pan,
A.
Vizcargüenaga
Projects
in
Construc-on,
Design
&
R&D
phase
with
Spanish
Par-cipa-on
BigBOSS: The Ground-Based Stage IV BAO Experiment
• Currently BOSS is covering ~ 6h-3Gpc3
Spain
was
invited
at
the
start
1.5M galaxies Of
the
Project
• BigBOSS will cover ~ 50h-3Gpc3
20M galaxies
(unprecedented volume & statistics to test for indications of new physics)
• BigBOSS will cover 14,000 deg2
32
BigBOSS: Status, Progress, and Plans
• Announcement of Opportunity for Large Science Programs Providing New
Observing Capabilities for the Mayall 4m Telescope on Kitt Peak
Letters of intent (LoI), March 2010 à 500 nights awarded
• CD-0 granted (Successful Review in Dec’11)
- Science Case
- Preliminary design
- R&D
• CD-1 is coming soon …
- Conceptual design report (and review) KPNO
Mayall
4m
- Complete R&D
- Complete cost and schedule baseline
- Construction foreseen for 2014
- First Light 2018
BigBOSS has key international partners:
China, Spain [positioners]
France [spectrograph]
33
Spain [focal plate]
UK [optics, fibers]The BigBOSS Dark Energy Survey
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BigBOSS Collaboration
… and growing!
US Members:
Brookhaven National Laboratory, Carnegie Mellon University, Fermi National Accelerator
Laboratory, Johns Hopkins University, Lawrence Berkeley National Laboratory, National
Optical Astronomy Observatory, New York University, The Ohio State University, SLAC
National Accelerator Laboratory, University of California, Berkeley, University of Kansas,
University of Michigan, University of Pittsburgh, University of Utah, Yale University, Harvard
International Institutions:
Ewha Womans University, Korea; French Participation Group; Goettigen Univ., Mexico
Participation group; Spanish Participation Group; Shanghai Astronomical Observatory, UK
Participation Group; University of Science and Technology of China.BigBOSS in Spain
BigBOSS
Spain
Par.cipa.on
Group
(BSPG):
•
Campus
de
Excelencia
Internacional
UAM+CSIC
Contact:
F.
Prada
(BSPG
Spokesperson)
-‐
Ins-tuto
de
Física
Teórica,
IFT-‐UAM/CSIC
Contact:
A.
González-‐Arroyo
-‐
HCTLab,
Escuela
Politécnica
Superior,
EPS-‐UAM
Contact:
G.
Glez.
de
Ribera
-‐
Dpto.
de
Física
Teórica,
DFT-‐UAM
Contact:
G.
Yepes
•
Ins-tuto
de
AstroGsica
de
Andalucía,
IAA-‐CSIC
Contact:
J.
Sanchez
•
Ins-tuto
de
AstroGsica
de
Canarias,
IAC
Contact:
C.
Allende-‐Prieto
•
Ins-tut
de
Ciencies
del
Cosmos,
ICC-‐UB
Contact:
J.
Miralda-‐Escudé
•
Observatori
Astronomic
de
la
Univ.
de
Valencia,
OA-‐UV
Contact:
V.
Marvnez
36
BigBOSS Focal Plane System (Spanish Contribution)
Fibers
(pointing down)
Spain
37
BigBOSS Focal Plate
Current technical approach
•
Dimensional
verifica-on
Highly challenging A prototype is needed for (manufacturing
feasibility)
requirements in terms of checking the feasibility as •
Thermal
tes-ng
manufacturing accuracy it is required •
Interface
with
fiber
posi-oners
~
900mm
200mm
;
241
holes!
Sub-‐scale
Demonstrator
Plate
(SDP)
Scale
~1:5
in
diameter
Focal
Plate
BigBOSS
•
SOW
(Statement
of
Work)
for
the
produc-on
of
the
SDP
has
been
sent
to
suppliers
•
Feedback
from
suppliers
on-‐going
…
Quota-ons
to
be
received
next
•
Produc-on
of
the
SDP
(end
2012
/beginning
2013)
•
SDP
verified
(1st
quarter
2013)
IAA-AVS θ-θ 12mm pitch actuator for Big BOSS
• The new θ-θ dependent-axis concept simplify
the R1,R2 positions in the fixed rear part of the
actuator, then easy heat evacuation, cables no
rotate inside actuator, electronics very near the
motor.
• Main characteristics
Pitch: 12mm
Patrol area: 13.856 mm diameter
R1,R2 are 365º and 185º respectively
Precision estimated: +-5 micron at exterior of
patrol area, with preloaded springsIAA-AVS θ-θ 12mm pitch actuator for BigBOSS • Software compensation for induced steps is needed • Torque programmable • Sensor to detect lost steps (collisions) • Low consumption electronics very near to the motor, reprogrammable on air, IRQ to the HOST capability IF collision is detected • All wired topology proposal, from actuator to the HOST FIRST TESTS: Prototype repetitively of 6 micron for R1 and 4 micron for R2, hysteresis minimization with appropriate movement. Currently, some minor mechanical improvements are being done as well as a new electronics is needed for full performance tests.
DESpec:
Dark
Energy
Spectroscopic
Survey
Next
genera-on
spectroscopic
survey:
Follow
up
for
DES
4000-‐fibre
instrument
for
the
4m
Blanco
telescope
Using
DES
op-cs
and
spare
CCDs
Can
improve
DE
FoM
by
3-‐6,making
it
a
DETF
Stage
IV
experiment
Spanish
Groups
of
DES
very
ac.vely
involved:
Electronics,
Science
Strong
Points
of
DESpec:
High
Performance,
low
cost,
low
risk
CTIO
site
Uses
DECam
components
and
other
heritages
Synergy
in
Southern
hemisphere
DES,
LSST
quality
targets
3d
map
pf
sothern
hemisphere
near
start
of
LSST
survey
Gemini,
ESO/VLT,
LCO…
Followup
SPT,
ACT,
SKA:
CMB
lensing/correla-on
Strong
Team
(DES
collabora.on
and
others)
Massive
Spectroscopic
Survey
in
the
Southern
Hemisphere
• 8-‐million
Galaxy
RedshiX
Survey
in
350
nights
– Uniformly
selected
from
deep,
homogeneous
DES
imaging
over
5000
sq.
deg.
(2018+)
• 23-‐million
Galaxy
RedshiX
Survey
in
1000
nights
– Uniformly
selected
from
deep,
homogeneous
LSST
imaging
over
15,000
sq.
deg.
(2021+)
• Deep,
uniform
mul-band
imaging
from
DES,
LSST
– Enable
efficient,
well-‐understood
selec-on
of
spectroscopic
targets
• Photometric+Spectroscopic
Surveys
over
same
Sky
– Enable
powerful
new
science
beyond
what
either
can
provide
alone
• DESpec
White
Paper
released
Sept.
11
– arXiv:
1209.2451
(Abdalla,
etal)
Massive
Spectroscopy
of
DES
and
LSST
Targets
Enables
New
and
Improved
DE
Probes
Weak
Lensing
and
Redshic-‐Space
Distor.ons:
Powerful
test
of
Dark
Energy
vs
Modified
Gravity
Galaxy
Clustering:
Radial
BAO
for
H(z)
and
improved
DA(z)
Photometric
Redshic
Calibra.on:
Determine
DES
and
LSST
N(z)
from
angular
correla-on
Gaztañaga
et
al.,
2011
Galaxy
clusters
Dynamical
masses
from
velocity
dispersions,
improve
halo
mass-‐
observable
calibra-on,
reduce
the
major
cluster
DE
systema-c
Weak
Lensing
Reduce
systema-cs
from
intrinsic
alignments
Supernovae
Reduce
systema-cs
from
host-‐galaxy
typing
PAU@WHT:
Physics
of
the
Accelera.ng
Universe
• New camera for WHT with 18 2k
x 4k CCDs covering 1 deg ∅ FoV.
• 42 100Å-wide filters covering
4300-8600 Å in 6 movable filter
trays, which also include standard
ugrizY filters.
• As a survey camera, it can cover
~2 deg2 per night in all filters.
• It can provide low-resolution
spectra (Δλ/λ ~ 2%, or R ~ 50) for
>30000 galaxies, 5000 stars,
1000 quasars, 10 galaxy clusters,
per night.
• Expected galaxy redshift
resolution σ(z) ~ 0.003×(1+z)
2.- PAU at the WHT
PI : E. Fernández (UAB/IFAE)
Co-Is: E. Sánchez (CIEMAT), E. Gaztañaga (IEEC/CSIC), R. Miquel (IFAE), J. García-Bellido (IFT/UAM), M. Delfino (PIC)
PAUCam PI: F. Castander PAU
at
the
WHT
Project Manager: C. Padilla; System Engineer: L. Cardiel, DAQ: J. de Vicente; Mechanics: F. Grañena; Control: O. Ballester;
Optics and integration: R. Casas, J. Jiménez.
PAUDm & Science PI: E. Gaztañaga
Simulations: F. Castander; Operation: N. Tonello; Data Reduction: S. Serrano; QA&Validation: I. Sevilla.
The Survey Team:
V. Acín5, D. Alonso4, J. Asorey2, O. Ballester3, A. Bauer2, C. Bonnett2, A. Bueno4, L. Cardiel3, J. Carretero2,
R. Casas2, M. Caubet5, F. Castander2, J. Castilla1, M. Crocce2, M. Delfino5, J.F. de Vicente1, M. Eriksen2, S. Farrens2,
E. Fernández3, J. Flix5, P. Fosalba2, J. García-Bellido4, E. Gaztañaga2, F. Grañena3, A. Izard2, J. Jiménez2, S. Jouvel2, S.
Heinis3, C. Hernández3, K. Hoffman2, C. López2, L. C. López3, F. Madrid2, P. Martí3, G. Martínez1, R. Miquel3, C.
Neissner5, S. Nesseris4, A. Pacheco5, C. Padilla3, C. Pio3, E. Planas5, A. Pujol2, F. J. Rodríguez1, J. Rubio4, E. Sánchez1,
C. Sánchez3, F. J. Sánchez1, D. Sapone4, S. Serrano2, I. Sevilla1, P. Tallada5, N. Tonello5.
1 2
3 4 5
Status
–
Noviembre
2012
PAUCam:
The
Pau
Camera
Main
Characteris.cs
Large
Field
of
View
(1
degree)
Narrow+broad
band
filters
Good
spectral
sensi-vity
Segmented
filter
trays
The
aim
is
to
have
a
working
instrument
ready
by
the
end
of
the
year
2012.
Taken from Cenarro’s Talk at RIA-Valencia
Taken from Cenarro’s Talk at RIA-Valencia
Taken from Benitez’s Talk at RIA-Valencia
LSS in LSST Licia Verde ICREA & ICC-‐UB
LSST
in
numbers
• Effec-ve
etendue
319
m2deg2
• FoV
9.9
deg2
• Effec-ve
aperture
6.7m
• Wavelength
coverage
320-‐1080
nm,
filters
u
g
r
I
z
y
• Sky
coverage
20,000
sq
deg
• Single
visit
depth
r
~
24.5
(5
σ
point
source)
• Seeing
0.7
arcsec
in
r
• Each
patch
of
the
sky
observed
2000
-mes
(15s-‐days)
1000
visits
• Photometric
repeatability
5-‐10
millimags
• Astrometric
precision
beZer
than
10
mas
(rsm)
per
visit
per
coord
see
e.g.,
LSST
science
book
at
hZp://arxiv.org/abs/0912.0201
or
hZp://www.lsst.org/lsst/scibook
Licia
Verde
LSS
in
LSST
Dark
energy:
theore.cal
aspects
• A
cosmological
constant
is
a
good
phenomenological
descrip-on
for
cosmic
accelera-on,
but
….
• Naturalness
problem:
natural
par-cle
physics
contribu-ons
• Coincidence
problem:
if
there
is
no
connec-on
between
Λ
and
maZer?
• Is
there
a
more
fundamental
theory
for
cosmic
accelera-on?
Dark
energy:
theore.cal
aspects
Alterna-ve
theories
to
ΛCDM
Gµν
+
GµνMG = 8πG (Tµν +Tµν DE)
Modified
gravity
Dark
energy
• Modified
gravity:
f(R),
brane-‐worlds,
holographic,
Pala-ni,
…
U
AB,
I
CE,
I
EEC,
U
CM,
U
V-‐IFIC,
UAM-‐IFT,
IFF
• Dark
energy:
scalar,
vector,
DBI,
galileons,
coupled
DE-‐DM,
disformal
…
UCM,UAM-‐IFT,UPV
• Inhomogeneous
models
in
GR
without
Λ:
Lemaître-‐Tolman-‐
Bondi
UAM-‐IFT
Dark
Mafer
&
Dark
Energy:
Simula.ons
www.multidark.org
BigMul-Dark
suite
of
cosmological
simula-ons
Large-volume high-res cosmological simulations are
needed. This is a Gran Challenge Project which needs
access to large supercomputers – PRACE in EU – and
databases – VO – to host the simulations products (mock
galaxy catalogues, etc).SPANISH PARTICIPATION: F. CASTANDER & R. REBOLO
Remark
Cosmology is a very active and dynamic field in Spain
(considering the relatively small community)
BUT, “No podemos estar en todo!”
ANSWER
Massive large-area surveys have been at the forefront of
the tremendous progress that has taken place in
cosmology over the last decade. The success of the
SDSS, which with a modest budget has been one of the
world's largest impact observatories in the last decade
clearly demonstrates the importance for the scientific
community of continuing survey development and
implementation. One of the crucial characteristics of the
scientific impact of these surveys is that their
applicability is extremely broad, the discoveries they
lead to are of key importance, while the nature of these
discoveries is often unexpected at the time when the
surveys are planned.
Madrid & Macchetto 2009, arXiv:0901.4552Thanks
to:
Juan Garcia-Bellido (IF- UAM/CSIC),
Licia Verde (ICC-UB), Pilar Ruiz-Lapuente (ICC-UB),
Rafael Rebolo & J.A. Rubiño-Martin (IAC)
Enrique Martinez (IFCA), Gustavo Yepes (UAM),
Antonio Maroto (UCM) and many others …To be continued …
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