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Recent TeV Observations of Blazars & Connectionsto GLAST
Frank Krennrich
Iowa State University
VERITAS Collaboration
GSFC, October 24, 2002
AGN
204/20/23
VERITAS Collaboration:
Frank Krennrich ([email protected])
for the VERITAS collaboration
Collaboration members:Iowa State U.Leeds U. (U.K.)McGill University (Canada)Purdue U.Smithsonian Astrophysical ObservatoryUCLAUniversity College, Dublin (Ireland)U. of ChicagoU. of Utah Washington U.
304/20/23
Outline
Introduction
atmospheric Cherenkov imaging technique
brief overview of TeV blazars Astrophysics results with Whipple 10m telescope
Mrk 421 2000/2001, Mrk 501 1997 spectra
H1426+428, 1ES1959+650 Next generation instrument: VERITAS VERITAS – GLAST connection Summary
404/20/23
History of the Whipple 10m
Imaging Camera 0.01 – 100 TeV
Area ~ 100,000 m2
E ~ 0.2 – 100 TeV
~ 0.2 o
100 optical photons/m2 TeVwithin a few ns
504/20/23
-ray images: - narrow, short, smooth Hadronic images: - broad, long - local muons, patchy hadron rejection: 99.7% (10-3)
-ray proton
Cosmic Ray Rejection Technique
Crab Nebula 7 in 1hour
Courtesy W.Hofmann
604/20/23
Science Highlights: Whipple 10m• 1989 Discovery of TeV photons from the Crab
• 1992 TeV photons from the blazar Mrk 421 z = 0.031
• 1997 Flare of Mrk 501 z = 0.034
• 2001 Discovery of H1426+428 (z = 0.129)
• 2001 Flare Mrk 421
37
109
151
489
489
Weekes et al. 1989, ApJ, 342, 379
Punch et al. 1992, Nature, 358, 477
Gaidos et al. 1996, Nature, 383, 319
Catanese et al. 1997, ApJ, 487, L143
109
• 1996 Giant & short flare from Mrk 421
Krennrich et al. 2002, ApJL, 575, L9 Krennrich et al. 2001, ApJL, 560, L45 ~10 Crab
Horan et al. 2002, ApJ, 571, 753 Petry et al. 2002, ApJ, in press
> 70 “EGRET” blazars at 1 GeV Redshift z = 0.03 – 2.28
zH1426+428Mrk 421
Mrk 501
1ES1959+650
1ES2344+514
3C66
1ES2155-304
TeV blazar
“Whipple”
blazars
at 300 GeV
Mrk 421 0.031
Mrk 501 0.034
1ES2344 0.044
1ES1959 0.048
H1426 0.129
804/20/23
PK
S 2
155-
304 Search for new TeV Blazars:
Mrk
501
Mrk
421
H14
26+
428
1ES1959+650
1ES
2344
+51
4
Costamante, L. & Ghisellini, G. 2001, A&A, 384, 56
904/20/23
Mrk 421 z = 0.031 X-ray BL Weak GeV > 86 TeV
Mrk 501 z = 0.034 X-ray BL Marginal GeV > 40 TeV
1004/20/23
Multiwavelength spectra
Peak: 100 keV/200 GeV X-ray/TeV correlation
Mrk 501 Mrk 421 Peak at 1 keV/~50 GeV X-ray/TeV correlation
Catanese et al., ??? Catanese & Weekes, PASP, 111, 3191193 (1999)
1104/20/23
Mrk 421 in 2000/2001:
23,000 -rays at E> 300 GeV
Courtesy of J. Holder (see also Holder et al., 2001, Proc. 27th ICRC, Hamburg)
1204/20/23
Mrk 421/Mrk 501 spectra
Mrk 501
Mrk 421
dN/dE ~ E- e –(E/ E )
with E0 = 4.6 0.8 TeV
dN/dE ~ E- e –(E/E )
with E0 = 4.3 0.3 TeV
(- 1.4 + 1.7 TeV)syst
Samuelson et al. 1998, ApJL, 501, L17
Krennrich et al. 1999, ApJ, 511, 149
Krennrich et al. 2001, ApJL, 560, L45
0
0
1304/20/23
Mrk 421 <spectral variability>
on average, -ray luminosity peakshifts to larger energieswith increasing flux!
Krennrich, F. et al. 2002, ApJL, 575, L9
1404/20/23
<Mrk 501> 1997 vs. Mrk 421 high state
Mrk 501 1997 average
Mrk 421 high state (set I)
spectral index varies but cutoff region remains stable!
imagine instrument with 20 times the sensitivity of Whipple separate constant from variable component
IR-background density
1504/20/23
Mrk 421: spectral variability:
Property of a specific blazar or emission mechanism?
Krennrich et al. 1999, ApJ, 511, 149 Krennrich et al. 2002, ApJL, 575, L9 Fossati et al. 2000, ApJ, 541, 166
X-rayVHE--ray
½ Hourly Spectral Variability:
Feb. 1 Feb. 2 Feb. 27
March 19 March 25 March 27
P = 3.4 x 10-3
P = 4.0 x 10-3 P = 8.5 x 10-4
1804/20/23
X-ray/TeV correlation: Mrk 421
preliminary
TeV lightcurve & TeV spectral variation
X-ray/TeV lightcurve
Courtesy of G. Fossati , J. Buckley & M. Jordan
preliminarypreliminary
VERITAS collaboration (in preparation)
1904/20/23
H1426+428: weak signal ~ 80 mCrab
2000 2000
20012001
from Horan et al. 2002, ApJ, 571, 753
2004/20/23
H1426+428 spectrum:Whipple 2001:dN/dE ~ E-3.50 0.35 0.05
Petry et al. 2002, ApJ, in press
HEGRA 2001:dN/dE ~ E-2.60 0.6 0.05
Whipple+HEGRA:dN/dE ~ E-3.54 0.27 0.05
Aharonian et al. 2002, A&A, 384, L23
Petry et al. 2002, ApJ, in press
2104/20/23
2002 Flares from 1ES1959+650:
IAU circular 7903 (VERITAS collaboration), 2002
Holder et al. 2002, in preparation
2204/20/23
Conclusion from blazar observations
Spectral cutoffs for Mrk 421/501 at ~ 4 TeV: possible evidence for absorption from IR background
or due to internal break due to KN~ E-1 (when hsoft > me c2 )
Spectral variability (Mrk 421): -ray luminosity peak shifts with <flux> increase -flux correlation holds over 5 years! Rapid variability (Mrk421):
tvariability ~ 15 min. ~ 10 emission region 10-4 - 10-5 pc H1426+428: first detection of blazar with z ~ 0.129 at E >300 GeV steep spectrum: dN/dE ~ E-3.54 0.27 0.05
Future: source list steadily growing (5 Whipple blazars) VERITAS
2304/20/23
VERITAS: Very Energetic Radiation Imaging Telescope Array System
50 GeV – 50 TeV Area: = 100,000 m2 (1 TeV) = 40,000 m2 (300 GeV) = 1,000 m2 (50 GeV) Angular res.: 0.03o – 0.14o Energy resolution: 10-18% Observation strategy: pointed exposures
2404/20/23
Arrays of Imaging Telescopes I
- 50 GeV – 50 TeV
- ~ 0.03o @1TeV
~ 0.09o @100GeV
- Flux sensitivity:
15 mCrab @100GeV
5 mCrab @300GeV
80 m
VERITAS
2604/20/23
TECHNICAL PROGRESS
Telescope: mount, mirrors
Camera: PMTs, amps
Electronics: FADCs, trigger
DAQ:High speed Readout & analysis
3104/20/23
GLAST/VERITAS cross-calibration: Crab Nebula
Hillas et al., ApJ, 503, 744 (1998)
GLASTVERITAS
Overlap: 50 GeV – 100 GeV - 1 TeV GLAST: E/E ~ 5-10% @ 10 GeV –100 GeV VERITAS: E/E ~ 20-10% @ 50 GeV-1000 GeV 20-25% uncertainty in the absolute energy of IACTs! fix with GLAST/VERITAS cross- calibration using overlap! GLAST (40 days exposure) 150 (10) photons above 10 (100) GeV 10% accuracy in absolute E
3204/20/23
Connections:
Unified AGN picture
~ several 103 GeV blazars
blazar classification studies
(GeV blazars) Jet models
broad studies
daily-yearly flux variations EBL cutoff
probe 0.1 m – 0.01 m Blazar spectra
20 MeV – 100 GeV
Unified AGN picture
~ 102 sub-TeV blazars
classification studies
(extreme blazars) Jet models
detailed studies
min. - yearly spectral variations EBL cutoff
probe 0.1 m – 50 m Blazar spectra
50 GeV – 50 TeV
GLAST