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Frank Krennrich*, for the VERITAS Collaboration (*Iowa State University)

Results from VERITAS New Opportunities at the interface between particle physics and astronomy. Tel 4. Tel 3. Tel 1. Tel 2. VERITAS. Frank Krennrich*, for the VERITAS Collaboration (*Iowa State University). Outline. VERITAS Instrument Performance Northern Sky seen in the first year

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Frank Krennrich*, for the VERITAS Collaboration (*Iowa State University)

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  1. Results from VERITAS New Opportunities at the interface between particle physics and astronomy Tel 4 Tel 3 Tel 1 Tel 2 VERITAS Frank Krennrich*, for the VERITAS Collaboration (*Iowa State University)

  2. Outline • VERITAS Instrument Performance • Northern Sky seen in the first year • Extragalactic science • Summary

  3. Very Energetic Radiation Imaging Telescope Array System E ~ 100 GeV - 50 TeVAarea ~ 105 m2ang. Res. ~ 3’ - 6’Energy Res. ~ 15%FOV ~ 3.50

  4. VERITAS Collaboration U.S. Adler Planetarium Argonne Nat. Lab. Barnard College DePauw U. Grinnell College Iowa State U. Purdue U. Smithsonian UCLA UCSC U. Of Chicago U. of Delaware Univ. of Iowa U. of Massachusetts U. of Utah Washington U. Canada McGill U. U.K. Leeds U. Ireland Cork Inst.Tech. Galway-Mayo Inst. N. U. I., Galway U. College Dublin + 25 Associates Supported by: SI, NSF & DOE (US), PPARC (UK), NSERC (Canada), SFI (Ireland) VERITAS-4 Construction funded in 2003

  5. VERITAS Observatory T2 Spring 2006 T3 Fall 2006 T4 Spring 2007 T1 Jan 2005

  6. TeV Monitoring capability 7km

  7. VERITAS Telescope Davies-Cotton f/1.0 Optics. Total area=110m2 Control Room

  8. VERITAS Telescope Davies-Cotton f/1.0 Optics. Total area=110m2 Control Room

  9. Stereoscopic Events

  10. Angular Resolution o Courtesy Asif Imran

  11. VERITAS Sensitivity 5σ Detection Sensitivity 1% Crab in 47 hours 5% Crab in 2.5 hours • Measured sensitivity to theCrab Nebula at high elevation (>65°) • HESS ~ 1% Crab in 25 hours • MAGIC ~ 2% Crab in 50 hours

  12. TeV -ray Sky W Comae Mrk 421 1ES 1218+304 Mrk 501 M87 1ES 0806+524 LSI +61 303 IC 443 Crab Nebula Cas A 1ES 2344+514

  13. Key Science Questions • Origin of Cosmic rays - galactic/Extragalactic • Relativistic Jets & Black holes - leptonic vs. hadronic jets • Dark Matter - Neutralino Annihil. Signature - LHC - direct detection - Storage • TeV beam in extragalactic space - test dispersion relation of light - Q.G. - how far do we see? Opacity? - Probe Cosmic Infrared Background

  14. Science Program Observations: ~ 800 hrs / year + ~ 200 hrs / year moonlight Science Groups: Astroparticle Physics Blazars Dark Matter Extragal. Sources Galactic Compact Galactic Diffuse GRB’s PWN & SNR’s Unidentifieds Bulk Program (40%) Discretionary (10%) ToO’s GRB’s (priority) etc. Key Science Projects (50%) Sky Survey (Cygnus region) SNRs/PWN Dark Matter BLAZARS

  15. recent discoveries Multiwavelength ScienceEBL Extragalactic Science

  16. 1ES 0806+524 ATEL#1415 • “best candidate” TeV BL Lacs (Costamante & Ghisellini 2002)- HBL- z = 0.138- 5.8  in ~ 40 hours - flux ~ 0.01 Crab- weakest VERITAS blazar Preliminary P. Cogan, in preparation

  17. W Comae ATEL#1422 • radio 1971, X-ray 1980- IBL (between LBL- HBL)- seen by EGRET: 0.1 -10 (27) GeV- z = 0.102- 4.9  in ~ 40 hours - outburst March 08 (> 8  detection)- Quasi-simulataneous X-ray data (Swift) Courtesy of M. Beilicke

  18. W Comae Courtesy of M. Beilicke

  19. W Comae Courtesy of M. Beilicke

  20. W Comae Courtesy of M. Beilicke

  21. W Comae • one-zone SSC/ weak B-field- EC model/ B ~ 0.3 G - GeV/TeV obs. critical Quasi-simultaneous data March 14/15 2008from AAVSO, UVOT, XRT, VERITAS

  22. HST M87 M87 • Giant elliptical Galaxy- D ~ 16 Mpc- Misaligned jet (<20o) - First non-blazar VHE source outside galaxy- Candidate UHE cosmic ray accelerator- Synch. X-ray source -> E >10 TeV electrons- close up view of a jet! 4  evidence (HEGRA 03) M87

  23. M87 g p π0 • UHE cosmic rays? - Synchr. Proton Blazar?- Synchr. Self Compton- inv. Compton in kpc jet (no time variations)- annihilation of SS dark matter- Where do TeV photons originate? g + 

  24. M87 • M87 under the “microscope” in radio-optical-X-ray- variable in X-rays- TeV “image” is not resolved 15 “ 80 pc

  25. M87 • M87 under the “microscope” in radio-optical-X-ray- variable in X-rays- TeV “image” is not resolved 15 “ 80 pc

  26. M87 VHE/X-ray Long-Term Correlation VHE/X-ray Short-Term Correlation Acciari et al. (VERITAS collaboration), ApJ, 679, 1427 (2008) Hui et al 2008 (VERITAS collaboration), in preparation

  27. M87 VHE/X-ray Long-term Light Curve Joint campaign HESS/MAGIC/VERITAS > 120 h in 2008 Stay tuned! Hui et al 2008 (VERITAS collaboration)

  28. 1ES 2344+514 - HBL- z = 0.044- discovered 1995 by Whipple- 0.07 Crab • VERITAS Observations Oct. 07 - Jan. 08- 20.5  detection- Swift: highest known X-ray flux on Dec. 8 07- VHE flux on Dec. 6/7 07: 0.41 Crab

  29. 7km Mrk 421 - HBL- z = 0.031- “old faithful”- Early 2008: 0.3 - 10 Crab- TeV monitor of transients ATEL#1506

  30. 1ES 1218+30.4 Courtesy of P. Fortin Courtesy of M. Beilicke z=0.182

  31. e- e+ Probing Cosmology Nikishov, JETP, 14, 2 (1962) Gould & Schreder, Phys. Rev. 155, 1408 (1967) Stecker, de Jager & Salamon, ApJ, 390, L42 (1992) Blazar: DN/DE ~ E-2 E ~ 1 TeV ~ 1 eV Absorption: exp (-(E)) Measured Spectrum: dN/dE ~ E-2 exp(-(E ))

  32. TeV Data • blazars with sufficient redshift • good spectral data • sensitive to near and/or mid-IR VERITAS 1ES1218+30.4 (HBL) Z = 0.182 E ~ 0.2 - 1.5 TeV 3o 1ES1101-232 (HBL) Z = 0.186 E ~ 0.2 - 2.9 TeV HESS 1ES0229+200 (HBL) Z = 0.1396 E ~ 0.5 - 11.2 TeV Aharonian et al. 2006, 2007.

  33. Constraints to Intrinsic Spectra New Lower limit from galaxy counts Taking into account Fuzzy fringes of galaxies Levenson & Wright 2008 For a given measured Blazar spectrum a Higher EBL implies a Harder intrinsic spectra! Slope of EBL spectrum is Critical for constraining Intrinsic spectrum! Levenson & Wright, arXiv:0802.1239v2

  34. Constraints to Intrinsic Spectra

  35. Constraints to Intrinsic Spectra

  36. Constraints to Intrinsic Spectra

  37. Constraints to Intrinsic Spectra

  38. EBL Lower Limits & Blazar Spectra TeV blazars seem to exhibit extremely hard spectra dN/dE ~ E-1.28+-0.20 or harder! FK, Dwek & Imran, submitted to ApJ

  39. Summary • VERITAS Performs well! 0.01 Crab (47 hr); ang. Res. ~ 0.1deg. • Seen ~ dozen sources in the Northern Sky • Broad Science program • Detailed studies of M87 • Discovery of W Comae; study of IBLs • Hard spectra of distant blazars • EBL studies

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