1 Possible indirect evidence for axion-like particles from far away AGN? Alessandro De Angelis INFN, INAF and Udine University Photon propagation Observation.

Slides:



Advertisements
Similar presentations
Many different acceleration mechanisms: Fermi 1, Fermi 2, shear,... (Fermi acceleration at shock: most standard, nice powerlaw, few free parameters) main.
Advertisements

Neutrinos from cosmological cosmic rays: A parameter space analysis Diego González-Díaz, Ricardo Vázquez, Enrique Zas Department of Particle Physics, Santiago.
A Multi - wavelength Study of Blazars with WIYN- VERITAS-IceCube Kirsten L. Larson The College of Wooster Advisor: Teresa Montaruli University of Madison-Wisconsin.
Longterm X-ray observation of Blazars with MAXI Naoki Isobe (Kyoto University; & MAXI
Blazar Gamma-ray absorption by cosmic radiation fields GRB Fermi z~60-6 CTA Susumu Inoue (Kyoto University) with (more than) a little help from my friends.
Observations of the AGN 1ES with the MAGIC telescope The MAGIC Telescope 1ES Results from the observations Conclusion The MAGIC Telescope.
MAGIC TeV blazars and Extragalactic Background Light Daniel Mazin on behalf of the MAGIC collaboration Max-Planck-Institut für Physik, Munich.
Upper Limit on the Cosmological  - Ray Background Yoshiyuki Inoue (Stanford) Kunihito Ioka (KEK) 1.
TeV blazars and their distance E. Prandini, Padova University & INFN G. Bonnoli, L. Maraschi, M. Mariotti and F. Tavecchio Cosmic Radiation Fields - Sources.
Karsten Berger On behalf of the MAGIC Collaboration.
Blazars as beamlights to probe the EBL Problem: EBL, emitted SED: both unknown ! Aim: measure n EBL (z) at different redshifts  local normalization, cosmic.
Naoki Isobe, Yoshihiro Ueda (Kyoto University) Kousuke Sugimori, Nobuyuki Kawai (Tokyo Tech.) Hitishi Negoro (Nihon Univ.) Mutsumi Sugizaki, Masaru Matsuoka.
Markus B ӧ ttcher Ohio University Athens, OH VHE Gamma-Ray Induced Pair Cascades in Blazars and Radio Galaxies.
Andreas Ringwald, DESY 27 th DESY PRC Closed Session, DESY, Hamburg, 26 October 2011 Towards a comprehensive summary Physics Case for WISP Searches.
H.E.S.S. observations of AGN “probing extreme environments with extreme radiation” Anthony Brown National Astronomy Meeting, 2006 H.E.S.S. = High Energy.
Models for non-HBL VHE Gamma-Ray Blazars Markus Böttcher Ohio University, Athens, OH, USA “TeV Particle Astrophysics” SLAC, Menlo Park, CA, July 13 – 17,
TeVPA, SLAC, 2009 Pratik Majumdar DESY, Zeuthen (for the MAGIC Collaboration) Outline:  MAGIC Telescope  Observations of High redshift AGNs  Conclusions.
Gamma-Ray Luminosity Function of Blazars and the Cosmic Gamma-Ray Background: Evidence for the Luminosity-Dependent Density Evolution Takuro Narumoto (Department.
MACRO Atmospheric Neutrinos Barry Barish 5 May 00 1.Neutrino oscillations 2.WIMPs 3.Astrophysical point sources.
Multi-wavelength AGN spectra and modeling Paolo Giommi ASI.
1 Tuning in to Nature’s Tevatrons Stella Bradbury, University of Leeds T e V  -ray Astronomy the atmospheric Cherenkov technique the Whipple 10m telescope.
Observations of 3C 279 with the MAGIC telescope M.Teshima 1, E.Prandini 2, M.Errando, D. Kranich 4, P.Majumdar 1, M.Mariotti 2 and V.Scalzotto 2 for the.
The Origin of the Extragalactic Background Light: Constraints from High Energy Gamma-Ray Observations ? P. Coppi Yale University.
1 1 Alessandro De Angelis, INAF INFN/Univ. Udine & IST Milano 09 Dark matter Rapid variability Does c depend on the photon energy? Anomalies in the propagation.
Recent results from MAGIC Alessandro de Angelis Univ. Udine, INFN Trieste Bremen, July 2010 Alessandro de Angelis Univ. Udine, INFN Trieste Bremen, July.
Long-term monitor on Mrk 421 using ARGO-YBJ experiment S.Z Chen (IHEP/CAS/China, On behalf of the ARGO-YBJ collaboration  1. Introduction.
4. Einstein Angle and Magnification The angular deflection for a relativistic neutrino with mass m ʋ that passes by a compact lens of mass M with impact.
Studying emission mechanisms of AGN Dr. Karsten Berger Fermi School, June ©NASA.
Recent TeV Observations of Blazars & Connections to GLAST Frank Krennrich Iowa State University VERITAS Collaboration GSFC, October 24, 2002 AGN.
Leptonic and Hadronic Modeling of Gamma-Ray Blazars Markus Böttcher and Anita Reimer North-West University Universit ӓ t Innsbruck Potchefstroom, Innsbruck.
Time dependent modeling of AGN emission from inhomogeneous jets with Particle diffusion and localized acceleration Extreme-Astrophysics in an Ever-Changing.
I.Introduction  Recent evidence from Fermi and the VLBA has revealed a strong connection between ɣ -ray emission in AGNs and their parsec-scale radio.
CTA Cherenkov Telescope Array CTA Josep-M.Paredes & Massimo Persic for CTA Consortium Vulcano, May 30, 2009.
5 GHz observations of intraday variability in some AGNs  Huagang Song & Xiang Liu  Urumqi Observation, NAOCAS.
MAGIC Recent AGN Observations. The MAGIC Telescopes Located at La Palma, altitude 2 200m First telescope in operation since 2004 Stereoscopic system in.
A Catalog of Candidate High-redshift Blazars for GLAST
Matteo Palermo “Estimation of the probability of observing a gamma-ray flare based on the analysis of the Fermi data” Student: Matteo Palermo.
MAGIC Results Alessandro De Angelis INFN, IST and University of Udine ECRS Lisboa, September 2006.
REDSHIFT MEASUREMENT OF EXTREMELY BEAMED BL LAC OBJECTS. A PIECE OF EVIDENCE FOR TEV ASTRONOMY AND FUNDAMENTAL PHYSICS. Marco Landoni – Oss. Astronomico.
MA4: HIGH-ENERGY ASTROPHYSICS Critical situation of manpower : 1 person! Only «free research» based in OAT. Big collaborations based elsewhere (Fermi,
Modeling the Emission Processes in Blazars Markus Böttcher Ohio University Athens, OH.
ICRC 2003 First Extragalctic Observations by H.E.S.S. Arache Djannati-Ataï (Collège de France) 1.
44 th Rencontres de Moriond - La Thuile, Valle d’Aosta, February 1-8, 2009 The MAGICextragalactic sky The MAGIC extragalactic sky Barbara De Lotto Università.
Blazars: the gamma-ray view of AGILE on behalf of the AGILE WG-AGN Filippo D’Ammando Università degli Studi di Roma “Tor Vergata” INAF - Istituto di Astrofisica.
LIGHT PSEUDOSCALAR BOSONS, PVLAS AND DOUBLE PULSAR J Marco Roncadelli, INFN – Pavia (Italy)
A new light boson from Cherenkov telescopes observations? A.De Angelis, M. Roncadelli, O. Mansutti.
A new light boson from MAGIC observations? A.De Angelis, O. Mansutti, M. Roncadelli.
Gamma-Ray Burst Working Group Co-conveners: Abe Falcone, Penn State, David A. Williams, UCSC,
VHE  -ray Emission From Nearby FR I Radio Galaxies M. Ostrowski 1 & L. Stawarz 1,2 1 Astronomical Observatory, Jagiellonian University 2 Landessternwarte.
A Simple Analytic Treatment of the Intergalactic Absorption Effect in Blazar  -ray Spectra Introduction Stecker, Malkan, & Scully (2006) have made a detailed.
Sources emitting gamma-rays observed in the MAGIC field of view Jelena-Kristina Željeznjak , Zagreb.
Modeling the SED and variability of 3C66A in Authors: Manasvita Joshi and Markus Böttcher (Ohio University) Abstract: An extensive multi-wavelength.
Anita Reimer, HEPL/Stanford University GLAST-lunch talk, 23 February 2006 On the diffuse AGN contribution to the extragalactic  -ray background (EGRB)
MAGIC Telescopes - Status and Results 2009/ Isabel Braun Institute for Particle Physics, ETH Zürich for the MAGIC collaboration CHIPP Plenary Meeting.
“VERITAS Science Highlights” VERITAS: TeV Astroparticle Physics Array of four 12-m Cherenkov telescopes Unprecedented sensitivity: ~100 GeV to ~30 TeV.
New constraints on light bosons from the high energy universe Denis WOUTERS Service de Physique des Particules Supervisor: Pierre BRUN D. Wouters and P.
MAGIC Max Planck Institut fürPhzsik The MAGIC Telescope ShangYu Sun A. Boller, L. Fortson, N. Galante, D. Paneque and B. Steinke On behalf of the Fermi,
and now for something completely different...
Swift Monitoring of Fermi Blazars and Other Sources
Mathew A. Malkan (UCLA) and Sean T. Scully (JMU)
H.E.S.S. Blazar Observations:
Observation of Pulsars and Plerions with MAGIC
Comment on two topics related to fundamental “exotic” physics with AGN Alessandro De Angelis Brera, March 2012 Testing fundamental spacetime symmetries.
Probing Lorentz Invariance with a VHE-Flare of PKS
Lecture 5 Multi-wavelength cosmic background
Marco Salvati INAF (Istituto Nazionale di Astrofisica)
Songzhan Chen Institute of High Energy Physics (IHEP) Nanjing
Lecture 6: Gamma-Ray Bursts Light extinction: Infrared background.
Fermi LAT Observations of Galactic X-ray binaries
Presentation transcript:

1 Possible indirect evidence for axion-like particles from far away AGN? Alessandro De Angelis INFN, INAF and Udine University Photon propagation Observation of distant AGN Axion-Like Particles & the DaRMa scenario Conclusions The work on axions has been done in collaboration with M. Roncadelli, O. Mansutti and M. Persic

2 Intergalactic absorption of VHE photons Cross section maximized for infrared/optical photons (Extragalactic Background Light) (Heitler 1960)

3 What is the attenuation?  = cos  n  ( ,z) is the spectral energy density of background photons <=EBL MAGIC, Science 2008

4 (An approximation) Neglecting evolutionary effects for simplicity Coppi & Aharonian, ApJ 1997

5 Consequences Since becomes 100 GeV: –The observed flux should be exponentially suppressed at large distances, so that very far-away sources should become invisible as energy increases –The observed flux should be exponentially suppressed at VHE, so that the SED should be steeper than the emitted one.

6 The VHE Universe far away… 35 Sources … PKS z=0.20HESS ES z=0.21MAGIC ES z=0.29 HESS & Fermi 2009 S z=0.31±0.08MAGIC ES z=0.34VERITAS C 66Az=0.44VERITAS C 279 z=0.54 MAGIC 2008

7 The distant quasar 3C 279 Flat spectrum radio quasar at z=0.54 Very bright and strongly variable –Brightest EGRET AGN –Gamma-ray flares in 1991 and Fast time variation (~ 6hr in 1996 flare) MAGIC observations –10 h between Jan.-April 2006 –clear detection on 23 rd Feb. at 6.2σ First FSRQ in TeV  -rays Major jump in redshift

8 The distant quasar 3C 279 is back! New observations after optical outburst in Jan  New flare detected Most distant object ever detected at VHE - two flares (Feb and Jan. 2007) Emission harder than expected -> constrains the EBL, universe more transparent to  -rays than expected

9 Implications on Extragalactic Background Light e-e- e+e+  EBL  VHE blazar IACT

10 At ~0.5 TeV, flux attenuated by 2 orders of magnitude! The measurement of spectral features permits to constrain EBL models: – Power law Γ = 4.1 ± 0.7, measured up to 0.5 TeV  Spectrum sensitive to 0.2 to 2 μm – Assume minimum reasonable index Γ em = 1.5: Upper limit close to lower limit from galaxy count Explanations go –from standard ones very hard emission mechanisms with intrinsic slope < 1.5 (Stecker 2008) Very low EBL –to possible evidence for new physics Oscillation to a particle traveling unimpeded?  → X →  Could it be seen?

11 Oscillation to an Axion-Like Particle –Oscillation during the propagation: DA, Roncadelli & Mansutti [DARMa], PLB2008, PRD2008 –Conversion at the emitter (Hooper et al., PRD2008) –Mixed mechanisms (Sanchez- Conde’ et al., PRD 2009) –…

12 Phenomenology of the oscillations Photon-ALP oscillations are similar to neutrino oscillations but external B is needed Bounds on the parameters M and m: –CAST & astrophysical arguments: M > 1.14 · GeV for m < 0.02 eV –Energetics of SN 1987a M > GeV for m < GeV, model dependent

13 (DA FARE) Which EBL ? First analysis of 3C279: EBL model by Kneiske et al To be updated including Franceschini et al. 2008

14 DARMa: Intergalactic magnetic fields Their morphology is poorly known. It is supposed that they have a domain-like structure with strength ~ 0.5 nG, coherence length ~ 10 Mpc, random orientation in each domain. N.B. - Picture consistent with first AUGER data: strength 0.3 – 0.9 nG for coherence length 1 – 10 Mpc (DA, Persic & Roncadelli, MPLA 2008).

15 Hooper & Serpico (DA FARE)

16 Sanchez-Conde’ et al. (DA FARE)

17 Experimental input from more sources at high z: MAGIC S After trigger, MAGIC observed 2.6h ‣ April 28: Swift reports flux about 50% larger than that observed in 2007 ‣ Apr 29: ATel #1500, MAGIC reports 6.8  discovery Apr F(>400 GeV) ≈25% Crab 3 rd low-peaked VHE blazar after BL Lac & W comae Host galaxy detected: Z=0.31+/-0.08 => 3 rd farthest VHE emitter for which the spectral index has been measured S Trigger in April 2008 Clear signal: 6.8σ New discovery:arXiv

18 Deformation of the SED PKS z=0.20HESS ES z=0.21MAGIC ES z=0.29 HESS & Fermi 2009 S z=0.31±0.08MAGIC ES z=0.34VERITAS C 66Az=0.44VERITAS C 279 z=0.54 MAGIC 2008 …and more new sources are coming into the game (VERITAS, HESS, MAGIC)

19 Other possible explanations related to new physics Kifune 2001: Violation of the Lorentz invariance We should keep in mind that –Extraordinary claims require extraordinary evidence New Scientist, SciAm blog/news, …, and then? –Claims must be followed up What else do we expect? Fundamental implications of unexpected findings? Are we seeing a part of the same big picture?

20 Conclusions The existence of a very light ALP, predicted by many extensions of the SM, naturally explains the observed transparency of the VHE gamma-ray sky. As a bonus, it explains why only the most distant AGN seem to demand an unconventional emission spectrum. The DaRMa prediction, in particular, concerns the spectral change of observed AGN flux at VHE and becomes observable if the TeV band is carefully probed. It can be tested with IACTs, with Fermi, and with EAS

21 ”A textbook example of the merging of particle physics and astronomy into the modern field of astroparticle physics”

22 BACKUP

23 PROPAGATION OVER ONE DOMAIN We work in the short-wavelength approximation, so the beam with energy E is formally a 3-level non relativistic quantum system described by the wave equation with

24 and mixing matrix which in the presence of absorption becomes with

25 Hence the conversion probability reads in terms of the propagation matrix. We find that a nonvanishing conversion probability over the WHOLE range requires with

26 In the present situation, we have and so the mixing matrix reduces to Following Csaki et al. ICAP 05 (2003) 005, we get the explicit form of the propagation matrix.

27 PROPAGATION OVER MANY DOMAINS When all domains are considered at once, one has to allow for the randomness of the direction of B in the n-th domain. Let be the direction of B in the n-th domain with respect to a FIXED fiducial direction for all domains and denote by the evolution matrix in the n-th domain. Then the overall beam propagation is described by

28 We evaluate by numerically computing and iterating the result times by randomly choosing each time. We repeat this procedure times and next average all these realizations of the propagation process over all random angles. So, the PHYSICAL propagation matrix of the beam is

29 Assuming that the initial state of the beam is unpolarized and fully made of photons, the initial beam state is So, we finally get

30 Ideal case z = 1 – EBL of Franceschini et al