astroparticles (cr’s & ) in the nearby universe & virtual observatory … one universe,...
TRANSCRIPT
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Astroparticles (CR’s & ) in the nearby universe& Virtual Observatory… one Universe, two worlds
Giuseppe Longo1,2,3 & Gennaro Miele1,2
1-Department of Physical Sciences – University Federico II Napoli2 - INFN Italian Institute of Nuclear Physics – Napoli Unit
3 - INAF Italian Institute of Astrophysics – Napoli Unit
[email protected]@na.infn.it
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Part I
Why do astroparticles need V.Ob. ?
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….. Because they look at nearby universe(D<100/200 Mpc)
10 TeV
1 TeV100 GeV
Photon interactions at TeV energies give a gamma horizon comparable in size to the GZK horizon
The main interaction is: e+e-
Pair production with e+e- cascading.
The gamma photons scatter on the extra- galactic background light.
kneeknee
anklanklee
UHECR
GZK horizon: CR (E>1018.5 eV) interact with CMB photons and decay
No UHECR’s from D > RGZK ≈ 100 Mpc
UHECR
gamma
Nearby universe means large f.o.v. (i.e., surveys)
for statistics
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Ground based gamma ray Cherenkov telescopes
Cosmic ray showers and Hybrid detectors
….. Because are going through a similar technological breakthrough
(D<100/200 Mpc)
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gamma-ray observatories (with small field-of-view)
CANGAROO III(Australia & Japan)
Spring 20044 telescopes 10
meters ØWoomera, Australia
Windhoek, NamibiaHESS
(Germany & France)
Summer 20024 (16)
telescopes12 meters Ø
Roque delos Muchachos, Canary Islands
MAGICMAGIC(Germany, Spain, Italy)(Germany, Spain, Italy)
Summer 2003Summer 20031 telescope 17 meters 1 telescope 17 meters
ØØMontosa Canyon,Arizona
VERITAS(USA &
England)2005?
7 telescopes10 meters Ø
+ Wide-angle instruments surveying ~ 2-3 sq. deg.
“Threshold”Sens. (1 y)Milagro ~ 2 TeV ~ 0.5 CrabTibet III shower array ~ 3 TeV ~ 1 CrabARGO YBJ 0.5 – 1 TeV ~ 0.5 Crab Crab signal
Tibet array
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“Keck mirror segment” equivalent
UHECR’s telescopes look really WEIRD!
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UHECR - The Pierre Auger Giant Array Observatory
1600 tanks + 24 Fluorescence Telescopes
3000 events yr-1 with energies above 1019 eV 30 events yr-1 above 1020 eVSampling on nanosecond scale; Sampling on nanosecond scale; events last events last 30-100 ns30-100 nsAngular resolution 30’ < p.r. <1.5°Angular resolution 30’ < p.r. <1.5°
ns!ns!
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Gamma rays begin to approach optical resolution
But:
Objects visible in gamma are not always visible in optical light
30 a
rcm
inUHECR’s are still far from itAngular resolution is small
p.r. > 30 ‘
Magnetic fields -> 1.5° < Deflection < 5.0°
In one resolution element,Up to 50.000 potential sources
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One universe
Energetic objects (GRB, SN, BH, AGN, etc.)
Dark Matter composition & distributionCosmological constantsCorrelation functions
&c.
Two worldsAstronomy
Large redshift range
Avalanche of complex dataMissing data
HeterogeneousLow time resolution
High angular resolutionFew large simulations
V.Obs. standardsProblems known
Astroparticles
Local Universe
Fewer and/or simpler dataSparse and uneven sampling
Heterogeneous Medium/high time resolution(Often) low angular resolutionVery many small simulations
No standardsProblems to be explored
Huge technological developmentLarge international collaborations
Proprietary dataSecurity issues
Many common science goals Common methodology of research
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Part II – an example
Identifying the sources of UHECR
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Correlation of the Highest-Energy Cosmic Rays with Nearby Extragalactic Objects by The Pierre Auger Collaboration*
Using data collected at the Pierre Auger Observatory during the past 3.7 years, we demonstrated a correlation between the arrival directions of cosmic rays with energy above 6 x 1019 electron volts and the positions of active galactic nuclei (AGN) lying within 75 megaparsecs. We rejected the hypothesis of an isotropic distribution of these cosmic rays with at least a 99% confidence level from a prescribed a priori test. The correlation we observed is compatible with the hypothesis that the highest-energy
particles originate from nearby extragalactic sources whose flux has not been substantially reduced by interaction with the cosmic background radiation. AGN or objects having a similar spatial distribution are possible sources.
Science 9 November 2007: Vol. 318. no. 5852, pp. 938 - 943
Hundreds of citations in less than 2 months
ground zero for a very harsh debate
mainly Related to how to integrate astroparticle data with astronomical ones !!
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Events(t, E, , )
Deconvolution for magnetic fields
Reconstructed Events(t, E, ’+, ’+)
Matched cataloguesMatched catalogues
Source Source Identifications?Identifications?
Astroparticles world
V.Obs. world
Problems:
1. Low angular resolution of UHECR data(1 event -> hundreds possible sources)
2. Poor knowledge of galactic/extragalactic B fields
Statistical approach to be preferred
Deterministic approach
Ill posed problem GRID
Astronomical cataloguesAstronomical catalogues
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Experiment 1: •UHECRs sources follow the distribution of LSS
(either AGN in clusters or WIMPS in DM haloes)•GZK is on/off (quite a consequence…)•Standard propagation of protons•Magnetic fields not very strong
Since you cannot identify sources, you must work on correlations of asrrival directions
2006, doi:10.1088/1475-7516/2006/01/009 (astro-ph/0510765)
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Propagation of protons
IRAS - PSC
15.000 galaxies with spect. z
Production of protons
Resulting UHECRs flux integrated from a lower threshold of 5x1019 eV
Ecut=30 EeV Ecut=50 EeV
Ecut=70 EeV Ecut=90 EeV
GZK filter (D<200 Mpc)Bright galaxies selection biases, etc…
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0 50 100 150 200 250 300 350
-75
-50
-25
0
25
50
75
How many How many events to events to detect detect
anisotropiesanisotropies? ?
Auger aperture functionAuger aperture function
Montecarlo simulations isotropic Montecarlo simulations isotropic distribution of eventsdistribution of events
200 eventsISOISO
LSSLSS
93 events compatible withIRAS-PSC
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This function vanishes if any of P or 1-P vanishes and has the theorethical maximum value of 1/4. So, the higher its value the more consistent the data are with the underlying hypothesis.
1818
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W
z
3TeV1TeV
3GeV
Window Function
=
Combine W(E,z) and survey
+
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Synthetic sky maps(low-l angular powerspectrum)
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Astronomical cataloguesAstronomical catalogues
Filter on astronomical cataloguesFilter on astronomical catalogues
Specific BoK’s of Specific BoK’s of candidate sources candidate sources
convolution for galactic magnetic fields
Events(t, E, , )predictions
Simulations/convolution extragalactic fields
comparisons
Falsification/validation Falsification/validation BoK’s/HypothesesBoK’s/Hypotheses
GRID
Statistical approach
Astroparticles world
V.Obs. world
Specific candidatesGZKselection effects, etc.
Radio data etc.
Instrumental signature
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Conclusions ?
•Standards (for integration with VO & for simulations) for data federation
•Visualization and analysis tools
•Access to multi-epoch data
•Easier access to astronomical knowledge