frank krennrich*, for the veritas collaboration (*iowa state university) results from veritas...
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Frank Krennrich*, for the VERITAS Collaboration Frank Krennrich*, for the VERITAS Collaboration
(*Iowa State University) (*Iowa State University)
Results from VERITASResults from VERITAS
New Opportunities at the interface New Opportunities at the interface between particle physics and between particle physics and astronomyastronomy
Tel 1Tel 2
Tel 3Tel 4
VERITAS
OutlineOutlineOutlineOutline
• VERITAS Instrument Performance
• Northern Sky seen in the first year
• Extragalactic science
• Summary
Very Energetic Radiation Imaging Telescope Array SystemVery Energetic Radiation Imaging Telescope Array System
E ~ 100 GeV - 50 TeVE ~ 100 GeV - 50 TeV
AAarea area ~ 10~ 1055 m m22
ang. Res. ~ 3’ - 6’ang. Res. ~ 3’ - 6’
Energy Res. ~ 15%Energy Res. ~ 15%
FOV ~ 3.5FOV ~ 3.500
E ~ 100 GeV - 50 TeVE ~ 100 GeV - 50 TeV
AAarea area ~ 10~ 1055 m m22
ang. Res. ~ 3’ - 6’ang. Res. ~ 3’ - 6’
Energy Res. ~ 15%Energy Res. ~ 15%
FOV ~ 3.5FOV ~ 3.500
VERITAS CollaborationVERITAS CollaborationVERITAS CollaborationVERITAS CollaborationU.S.Adler Planetarium Argonne Nat. Lab. Barnard College DePauw U. Grinnell College Iowa State U. Purdue U. Smithsonian UCLAUCSCU. Of ChicagoU. of DelawareUniv. of IowaU. of MassachusettsU. of UtahWashington U.
CanadaMcGill U.
U.K.Leeds U.
IrelandCork Inst.Tech.Galway-Mayo Inst.N. U. I., GalwayU. College Dublin
+ 25 Associates
Supported by: SI, NSF & DOE (US), PPARC (UK), Supported by: SI, NSF & DOE (US), PPARC (UK), NSERC (Canada), SFI (Ireland) NSERC (Canada), SFI (Ireland)Supported by: SI, NSF & DOE (US), PPARC (UK), Supported by: SI, NSF & DOE (US), PPARC (UK), NSERC (Canada), SFI (Ireland) NSERC (Canada), SFI (Ireland)
VERITAS-4 Construction funded in 2003VERITAS-4 Construction funded in 2003VERITAS-4 Construction funded in 2003VERITAS-4 Construction funded in 2003
VERITAS ObservatoryVERITAS ObservatoryVERITAS ObservatoryVERITAS Observatory
T1Jan 2005T1Jan 2005
T2Spring 2006T2Spring 2006
T3Fall 2006T3Fall 2006
T4Spring 2007T4Spring 2007
TeV Monitoring capability TeV Monitoring capability TeV Monitoring capability TeV Monitoring capability
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VERITAS TelescopeVERITAS TelescopeVERITAS TelescopeVERITAS Telescope
Cont
rol
Room
Davies-Cotton f/1.0 Optics. Total area=110m2
Cont
rol
Room
Davies-Cotton f/1.0 Optics. Total area=110m2
VERITAS TelescopeVERITAS TelescopeVERITAS TelescopeVERITAS Telescope
Stereoscopic EventsStereoscopic EventsStereoscopic EventsStereoscopic Events
Angular ResolutionAngular ResolutionAngular ResolutionAngular Resolution
o
Courtesy Asif Imran
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VERITAS SensitivityVERITAS SensitivityVERITAS SensitivityVERITAS Sensitivity
1% Crab in 47 hours
5% Crab in 2.5 hours
5σ Detection Sensitivity
• Measured sensitivity to the Crab
Nebula at high elevation (>65°)
• HESS ~ 1% Crab in 25 hours
• MAGIC ~ 2% Crab in 50 hours
TeV TeV -ray Sky -ray Sky TeV TeV -ray Sky -ray Sky W Comae
IC 443
Crab Nebula
Mrk 421
Mrk 501
Cas A
1ES 2344+514
LSI +61 303
1ES 0806+524
1ES 1218+304
M87
Key Science QuestionsKey Science QuestionsKey Science QuestionsKey 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
Science ProgramScience ProgramScience ProgramScience Program
Observations:~ 800 hrs / year+ ~ 200 hrs / year moonlight
Discretionary (10%)
Bulk Program (40%)
ToO’sGRB’s (priority)etc.
Sky Survey(Cygnus region) BLAZARS SNRs/PWN Dark Matter
Key Science Projects (50%)
Science Groups:
Astroparticle Physics Blazars Dark Matter Extragal. Sources Galactic Compact Galactic Diffuse GRB’s PWN & SNR’s Unidentifieds
recent discoveries recent discoveries
Multiwavelength ScienceMultiwavelength Science
EBL EBL
recent discoveries recent discoveries
Multiwavelength ScienceMultiwavelength Science
EBL EBL
Extragalactic Science Extragalactic Science Extragalactic Science Extragalactic Science
1ES 0806+5241ES 0806+5241ES 0806+5241ES 0806+524
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ATEL#1415
Prelim
inary
P. Cogan, in preparation
- “ “best candidate” TeV best candidate” TeV
BL Lacs (Costamante & BL Lacs (Costamante &
Ghisellini 2002) Ghisellini 2002)
- HBL- HBL
- z = 0.138- z = 0.138
- 5.8 - 5.8 in ~ 40 hours in ~ 40 hours
- flux ~ 0.01 Crab- flux ~ 0.01 Crab
- weakest VERITAS blazar - weakest VERITAS blazar
W ComaeW ComaeW ComaeW Comae
Courtesy of M. Beilicke
- radio 1971, X-ray 1980radio 1971, X-ray 1980
- IBL (between LBL- HBL)- IBL (between LBL- HBL)
- seen by EGRET: - seen by EGRET:
0.1 -10 (27) GeV 0.1 -10 (27) GeV
- z = 0.102- z = 0.102
- 4.9 - 4.9 in ~ 40 hours in ~ 40 hours
- outburst March 08- outburst March 08
(> 8 (> 8 detection) detection)
- Quasi-- Quasi-simulataneous simulataneous
X-ray data (Swift) X-ray data (Swift)
ATEL#1422
W ComaeW ComaeW ComaeW Comae
Courtesy of M. Beilicke
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W ComaeW ComaeW ComaeW Comae
Courtesy of M. Beilicke
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t 1.290.28 days
W ComaeW ComaeW ComaeW Comae
Courtesy of M. Beilicke
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dNdE
E 3.810.35stat
W ComaeW ComaeW ComaeW Comae
Quasi-simultaneous data March 14/15 2008Quasi-simultaneous data March 14/15 2008from AAVSO, UVOT, XRT, VERITASfrom AAVSO, UVOT, XRT, VERITAS
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- one-zone SSC/one-zone SSC/
weak B-field weak B-field
- EC model/ - EC model/
B ~ 0.3 G B ~ 0.3 G
- GeV/TeV obs.- GeV/TeV obs.
critical critical
M87M87M87M87HSTM87 - Giant elliptical GalaxyGiant elliptical Galaxy
- D ~ 16 Mpc- D ~ 16 Mpc
- Misaligned jet (<20- Misaligned jet (<20oo) )
- First non-blazar VHE - First non-blazar VHE
source outside galaxy source outside galaxy
- Candidate UHE cosmic - Candidate UHE cosmic
ray accelerator ray accelerator
- Synch. X-ray source - Synch. X-ray source
-> E >10 TeV electrons -> E >10 TeV electrons
- close up view of a jet!- close up view of a jet!
4 4 evidence (HEGRA 03) evidence (HEGRA 03)
M87M87
- UHE cosmic rays? UHE cosmic rays?
- Synchr. Proton Blazar?- Synchr. Proton Blazar?
- Synchr. Self Compton- Synchr. Self Compton
- inv. Compton in kpc jet- inv. Compton in kpc jet (no time variations) (no time variations)
- annihilation of SS dark matter- annihilation of SS dark matter
- Where do TeV photons originate?- Where do TeV photons originate?
p π0
+
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M87M87M87M87
- M87 under the M87 under the “microscope” in “microscope” in radio-optical-X-ray radio-optical-X-ray- variable in X-rays- variable in X-rays- TeV “image” is not - TeV “image” is not resolved resolved
15 “15 “
80 pc80 pc
M87M87M87M87
15 “15 “
80 pc80 pc
M87M87M87M87- M87 under the M87 under the “microscope” in “microscope” in radio-optical-X-ray radio-optical-X-ray- variable in X-rays- variable in X-rays- TeV “image” is not - TeV “image” is not resolved resolved
VHE/X-ray VHE/X-ray LongLong-Term-TermCorrelationCorrelation
Acciari et al. (VERITAS collaboration),ApJ, 679, 1427 (2008)
M87M87M87M87
VHE/X-ray VHE/X-ray ShortShort-Term-TermCorrelationCorrelation
Hui et al 2008 (VERITAS collaboration), in preparation
M87M87M87M87
VHE/X-ray Long-term Light CurveVHE/X-ray Long-term Light Curve
Hui et al 2008 (VERITAS collaboration)
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Joint campaignJoint campaignHESS/MAGIC/VERITAS HESS/MAGIC/VERITAS > 120 h in 2008> 120 h in 2008Stay tuned!Stay tuned!
1ES 2344+5141ES 2344+5141ES 2344+5141ES 2344+514
- HBL- HBL- z = 0.044- z = 0.044- discovered- discovered 1995 by 1995 by Whipple Whipple- 0.07 Crab- 0.07 Crab
- VERITAS Observations Oct. 07 - Jan. 08VERITAS Observations Oct. 07 - Jan. 08- 20.5 - 20.5 detection detection- Swift: highest known X-ray flux on Dec. 8 07- Swift: highest known X-ray flux on Dec. 8 07- VHE flux on Dec. 6/7 07: 0.41 Crab- VHE flux on Dec. 6/7 07: 0.41 Crab
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Mrk 421Mrk 421Mrk 421Mrk 421
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ATEL#1506
- HBL- HBL- z = 0.031- z = 0.031- “old faithful”- “old faithful”- Early 2008:- Early 2008: 0.3 - 10 Crab 0.3 - 10 Crab- TeV monitor of - TeV monitor of transients transients
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1ES 1218+30.41ES 1218+30.41ES 1218+30.41ES 1218+30.4
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Courtesy of M. Beilicke Courtesy of P. Fortin
dNdE
E 3.090.34 stat
z=0.182
Probing CosmologyProbing CosmologyProbing CosmologyProbing Cosmology
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Blazar: Blazar:
DN/DE ~ EDN/DE ~ E-2-2
Absorption: Absorption: exp (-exp (-(E(E))))
E ~ 1 TeVE ~ 1 TeV
~ 1 eV~ 1 eV
Nikishov, JETP, 14, 2 (1962)Nikishov, JETP, 14, 2 (1962)Gould & Schreder, Phys. Rev. Gould & Schreder, Phys. Rev. 155, 1408 (1967)155, 1408 (1967)Stecker, de Jager & Salamon, ApJ, Stecker, de Jager & Salamon, ApJ, 390, L42 (1992)390, L42 (1992)
Measured Spectrum: Measured Spectrum: dN/dE ~ EdN/dE ~ E-2-2 exp(- exp(-(E(E))))
ee--
ee++
TeV DataTeV DataTeV DataTeV Data
VERITAS
HESS
- blazars with sufficient redshift- good spectral data- sensitive to near and/or mid-IR
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1ES1218+30.4 (HBL)Z = 0.182E ~ 0.2 - 1.5 TeV
1ES1101-232 (HBL)Z = 0.186E ~ 0.2 - 2.9 TeV
1ES0229+200 (HBL)Z = 0.1396E ~ 0.5 - 11.2 TeV
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Aharonian et al. 2006, 2007.
3o
Constraints to Intrinsic SpectraConstraints to Intrinsic SpectraConstraints to Intrinsic SpectraConstraints to Intrinsic Spectra
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New Lower limit from galaxy countsTaking into accountFuzzy fringes of galaxiesLevenson & Wright 2008
For a given measured Blazar spectrum a Higher EBL implies a Harder intrinsic spectra!
Slope of EBL spectrum is Critical for constrainingIntrinsic spectrum!
Levenson & Wright, arXiv:0802.1239v2
Constraints to Intrinsic SpectraConstraints to Intrinsic SpectraConstraints to Intrinsic SpectraConstraints to Intrinsic Spectra
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Constraints to Intrinsic SpectraConstraints to Intrinsic SpectraConstraints to Intrinsic SpectraConstraints to Intrinsic Spectra
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Constraints to Intrinsic SpectraConstraints to Intrinsic SpectraConstraints to Intrinsic SpectraConstraints to Intrinsic Spectra
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Constraints to Intrinsic SpectraConstraints to Intrinsic SpectraConstraints to Intrinsic SpectraConstraints to Intrinsic Spectra
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EBL Lower Limits & EBL Lower Limits & Blazar Spectra Blazar Spectra
EBL Lower Limits & EBL Lower Limits & Blazar Spectra Blazar Spectra
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TeV blazars seem to exhibit extremely hard spectra dN/dE ~ E-1.28+-0.20
or harder!
FK, Dwek & Imran, submitted to ApJ
SummarySummarySummarySummary
• 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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