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Transcript
Multi-Channel Astrophysics & Cosmology at the Highest Energies Vasiliki Pavlidou University of Chicago Outline o The need for multi-channel studies in High-Energy Astrophysics o The next 10 years of High-Energy Messengers o What to look forward to: Breaking the degeneracy: AGNs, SNRs, GRBs, UHECRs Serendipitous discoveries Astrophysics with high-energy observations: measuring cosmic star formation Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17 Why multi-channel and multiwavelenght? Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17 Multi-channel and multi-wavelength studies: a must for high-energy astrophysics NRAO 530 / 2EG 1735-1312 o Tested and tried: low energy Markarian photons + high energy observations 501 or GeV + TeV photons source identifications (GRBs, gamma-ray loud blazars, pulsars, PWN) better monitoring of system variability, local conditions large spectral dynamical range, better tests for emission models Pian, Vacant, Tagliaferri, Ghisellini, Maraschi, Treves, Bower, Backer, Wright, Forster, Aller, & Aller 1997 Urry, Fiore, Giommi, Palazzi, Chiappetti, & Samburna 1998 Reimer & Funk 2006 Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17 High-Energy observations in the Next Decade o GLAST: continuous full-sky coverage in GeV gamma rays o Ground-based TeV telescopes: (CTA/AGIS/HAWC): full sky accessible in TeV gamma rays, high angular resolution o IceCube, KM3NeT: continuous full-sky coverage in TeV neutrinos o Auger South + North: continuous full-sky coverage in UHE CRs, photons, neutrinos o Perks: LIGO, LISA, JWST Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17 The future: 1. Breaking the degeneracy o o o o What is the origin of cosmic rays? AGNs, SNRs: hadronic or leptonic processes? AGNs, leptonic emission: SSC or EC? A success story AGNs, GRBs: how high do they go? (GLAST, CTs, from cosmology UHECRs) o What is making the highest energy particles? Top-down or bottom up? UHECRs, GLAST Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17 The future: 2. Serendipitous discoveries o XXX2017: winning the jackpot nearby transient (merger between compact objects ?) GLAST detects it as a very bright transient gamma-ray source. Follow up with Cherenkov detectors - high angular resolution. LIGO detects gravitational wave emission; nature of progenitor known at high confidence A success story Low-energy multi-wavelength campaign from neutrino Neutrino detectors pick up the -spike astrophysics Auger picks up the UHE particle signature (time broadening small and understood!) Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17 The future: 3. Low-E astrophysics with high-E observations o The Cosmic Star Formation Rate: how much gas mass is converted to stars per unit time per unit cosmic volume o An essential measure of: baryonic energy production, feedback processes in structure formation o Contributes to reionization o Links all of the messengers of interest! o Traditional measures: SF makes stars - young stars emit in UV, IR compilation by Hopkins & Beacom 2006 Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17 The SF - high-energy connection Ave, Busca,ray Malkan, Olinto, o Star Formation -> Supernovae ->Allard, Cosmic acceleration Parizot, Stecker & Yamamoto 2006 > interaction with ISM -> , o Star Formation -> gamma-ray bursts -> UHECRs?, , o Star Formation -> Background starlight (EBL) -> interaction with: , UHECR EBL imprinted on spectra of: individual -ray sources, -ray Blain & Natarajan 2000 Kalashev, SemikozUHECRs & Sigl 2007galaxies (VP & Fields 2002) background, Starforming Stecker Unidentified sources (VP, 1999 Siegal-Gaskins, Fields, Olinto & Brown 2007) Cosmogenic Blazars , (VP & Venters 2007) EGRET gamma-ray background, conservative (Strong et al 2004) Maximal EGRET gamma-ray background (Sreekumar et al 1998) Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17 How do we utilize this connection? o Until now: use knowledge of CSFR to predict signal/effects for high-energy telescopes o The future: concurrent high-E observations in different channels allow inversion of the problem: use observations of high-E signal/effects to constrain CSFR o Uncertainties: significant, BUT largely uncorrelated with uncertainties of low-E methods Strigari, Beacom, Walker & Zhang 2005 Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17 CSFR teaser: 15 yrs from now o GLAST has detected: CSFR peak in gamma-ray background @E ≈ 1 GeV pileup/suppression of gamma-ray background @ E20GeV unabsorbed spectra of hundreds of low-z blazars + improved IR CSFR observations by o GLAST+Cerenkov Telescopes have detected: Spitzer, JWST EBL absorption signatures in high-E tail of hundreds/thousands of + good high-z blazarsampling spectra of GRB afterglows, strong constraints of z-distribution of GRBs o IceCube/KM3NeT have detected: Cosmogenic neutrino signature o Auger has determined: Prodanovic, VP & Fields preliminary Spectrum, composition, sources and their cosmological evolution, acceleration mechanism of UHECRs, Exact shape of GZK Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17 Conclusions o Multi-channel, multi-wavelength observations give unique new insight into high-E astro o The time to do high-energy astrophysics is now: Combined data from different upcoming instruments + improved low-E observations => unprecedented possibilities for: multi-channel, multi-wavelength monitoring of the high-E sky, resolution of model degeneracies A new era: high-E observations can quantitatively map the cosmic history of baryonic energy generation and feedback Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17