Multi-Channel Astrophysics & Cosmology at the Highest Energies

1. Multi-Channel Astrophysics & Cosmology at the Highest Energies Vasiliki PavlidouUniversity of Chicago

2. Outline • The need for multi-channel studies in High-Energy Astrophysics • The next 10 years of High-Energy Messengers • 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

3. g g p g g g g g g n n g g g g g Why multi-channel and multi-wavelenght? Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17

4. Markarian 501 NRAO 530 / 2EG 1735-1312 Reimer & Funk 2006 Bower, Backer, Wright, Forster, Aller, & Aller 1997 Pian, Vacant, Tagliaferri, Ghisellini, Maraschi, Treves, Urry, Fiore, Giommi, Palazzi, Chiappetti, & Samburna 1998 Multi-channel and multi-wavelength studies: a must for high-energy astrophysics • Tested and tried: low energy photons + high energy observationsor 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 Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17

5. High-Energy observations in the Next Decade • GLAST: continuous full-sky coverage in GeV gamma rays • Ground-based TeV telescopes: (CTA/AGIS/HAWC):full sky accessible in TeV gamma rays, high angular resolution • IceCube, KM3NeT: continuous full-sky coverage in TeV neutrinos • Auger South + North: continuous full-sky coverage in UHE CRs, photons, neutrinos • Perks: LIGO, LISA, JWST Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17

6. A success story from cosmology The future: 1. Breaking the degeneracy • What is the origin of cosmic rays? • AGNs, SNRs: hadronic or leptonic processes? • AGNs, leptonic emission: SSC or EC? • AGNs, GRBs: how high do they go? (GLAST, CTs, UHECRs) • 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

7. A success story from neutrino astrophysics The future: 2. Serendipitous discoveries • XXX2017: winning the jackpotnearby 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 • Low-energy multi-wavelength campaign • Neutrino detectors pick up the -spike • 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

8. compilation by Hopkins & Beacom 2006 The future: 3. Low-E astrophysics with high-E observations • The Cosmic Star Formation Rate: how much gas mass is converted to stars per unit time per unit cosmic volume • An essential measure of: baryonic energy production, feedback processes in structure formation • Contributes to reionization • Links all of the messengers of interest! • Traditional measures: SF makes stars - young stars emit in UV, IR Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17

9. Allard, Ave, Busca, Malkan, Olinto, Parizot, Stecker & Yamamoto 2006 Stecker 1999 Kalashev, Semikoz & Sigl 2007 Blain & Natarajan 2000 Starforming galaxies (VP & Fields 2002)Unidentified sources (VP, Siegal-Gaskins, Fields, Olinto & Brown 2007)Blazars (VP & Venters 2007)EGRET gamma-ray background, conservative (Strong et al 2004) Maximal EGRET gamma-ray background (Sreekumar et al 1998) The SF - high-energy connection • Star Formation -> Supernovae -> Cosmic ray acceleration -> interaction with ISM -> ,  • Star Formation -> gamma-ray bursts -> UHECRs?, ,  • Star Formation -> Background starlight (EBL) -> interaction with: , UHECR • EBL imprinted on spectra of: individual -ray sources, -ray background, UHECRs • Cosmogenic ,  Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17

10. Strigari, Beacom, Walker & Zhang 2005 How do we utilize this connection? • Until now: use knowledge of CSFR to predict signal/effects for high-energy telescopes • The future: concurrent high-E observations in different channels allow inversion of the problem: use observations of high-E signal/effects to constrain CSFR • Uncertainties: significant, BUT largely uncorrelated with uncertainties of low-E methods Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17

11. Prodanovic, VP & Fields preliminary CSFR teaser: 15 yrs from now • GLAST has detected: • CSFR peak in gamma-ray background @E ≈ 1 GeV • pileup/suppression of gamma-ray background @ E20GeV • unabsorbed spectra of hundreds of low-z blazars • GLAST+Cerenkov Telescopes have detected: • EBL absorption signatures in high-E tail of hundreds/thousands of high-z blazar spectra • IceCube/KM3NeT have detected: • Cosmogenic neutrino signature • Auger has determined: • Spectrum, composition, sources and their cosmological evolution, acceleration mechanism of UHECRs, • Exact shape of GZK + improved IR CSFR observations by Spitzer, JWST+ good sampling of GRB afterglows, strong constraints of z-distribution of GRBs Vasiliki Pavlidou Ultra high energy photons, protons and neutrinos Penn State, May 17

12. Conclusions • Multi-channel, multi-wavelength observations give unique new insight into high-E astro • 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