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Time-resolved SEDs of Blazar FlaresAnnika Kreikenbohm, D. Dorner, M. Kadler, M. Kreter, T. Beuchert, N. Gehrels, D. Glawion, I. Kreykenbohm, M. Langejahn, K. Leiter, K. Mannheim, C. Müller, S. Richter, J. Wilms, and the FACT Collaboration
The X-ray Universe 2017, Rome, Italy
Annika Kreikenbohm “Time-Resolved SEDs of Blazar Flares“ The X-ray Universe 2017
Leptonic or Lepto-Hadronic?
SED created with ASDC SED Builder v8.2
Non-Simultaneous SED of Mrk 421 (for recent extensive MWL studies, see e.g., Abdo+ 2011b, 2014; Ahnen+ 2016; Aleksic+ 2015; Balokovic+ 2016; Bartoli+ 2016; Cheng+ 2015; Furniss+ 2015; Fraija+ 2015; Hovatta+ 2015; Kaku-wa+2015; Kataoka+ 2016; Lico+ 2014; Paliya+ 2015; Pian+2014; Sinha+ 2015, 2016; Zheng+ 2014; Zhu+ 2016; ...)
Annika Kreikenbohm “Time-Resolved SEDs of Blazar Flares“ The X-ray Universe 2017
Leptonic or Lepto-Hadronic?
SED created with ASDC SED Builder v8.2
Non-Simultaneous SED of Mrk 421 (for recent extensive MWL studies, see e.g., Abdo+ 2011b, 2014; Ahnen+ 2016; Aleksic+ 2015; Balokovic+ 2016; Bartoli+ 2016; Cheng+ 2015; Furniss+ 2015; Fraija+ 2015; Hovatta+ 2015; Kaku-wa+2015; Kataoka+ 2016; Lico+ 2014; Paliya+ 2015; Pian+2014; Sinha+ 2015, 2016; Zheng+ 2014; Zhu+ 2016; ...)
e-,e+ synchrotron emission
Annika Kreikenbohm “Time-Resolved SEDs of Blazar Flares“ The X-ray Universe 2017
Leptonic or Lepto-Hadronic?
SED created with ASDC SED Builder v8.2
Non-Simultaneous SED of Mrk 421 (for recent extensive MWL studies, see e.g., Abdo+ 2011b, 2014; Ahnen+ 2016; Aleksic+ 2015; Balokovic+ 2016; Bartoli+ 2016; Cheng+ 2015; Furniss+ 2015; Fraija+ 2015; Hovatta+ 2015; Kaku-wa+2015; Kataoka+ 2016; Lico+ 2014; Paliya+ 2015; Pian+2014; Sinha+ 2015, 2016; Zheng+ 2014; Zhu+ 2016; ...)
?e-,e+ synchrotron emission
Annika Kreikenbohm “Time-Resolved SEDs of Blazar Flares“ The X-ray Universe 2017
Leptonic or Lepto-Hadronic?
SED created with ASDC SED Builder v8.2
Non-Simultaneous SED of Mrk 421 (for recent extensive MWL studies, see e.g., Abdo+ 2011b, 2014; Ahnen+ 2016; Aleksic+ 2015; Balokovic+ 2016; Bartoli+ 2016; Cheng+ 2015; Furniss+ 2015; Fraija+ 2015; Hovatta+ 2015; Kaku-wa+2015; Kataoka+ 2016; Lico+ 2014; Paliya+ 2015; Pian+2014; Sinha+ 2015, 2016; Zheng+ 2014; Zhu+ 2016; ...)
?e-,e+ synchrotron emission
IC/ EC emission?
Proton synchrotron?photo-hadronic?
Annika Kreikenbohm “Time-Resolved SEDs of Blazar Flares“ The X-ray Universe 2017
Long-Term Monitoring
MWL ToO Program
Time–Resolved SEDs
ToO observationsupon FACT trigger:
Soft X-ray /UV band:Swift (~20ks total)XMM-Newton (~100 ks total)
Hard X-ray/ γ-ray band:INTEGRAL (~500 ks total)Fermi/LAT (continuous)
Apply time-resolved jet emission modes
Provide contraints onjet emission models
TeV band:FACT (since 2012) – daily VHE observations – provides detailed variability information– provides flare alerts
Trigger criterium:VHE FACT rate > 70 evts/hour
X-ray / UV band:Swift (since 2014) – weekly scheduled (~1ks)– monitoring of the low–E emission – test for orphan flares & time lags
Annika Kreikenbohm “Time-Resolved SEDs of Blazar Flares“ The X-ray Universe 2017
Long-Term Monitoring
MWL ToO Program
Time–Resolved SEDs
ToO observationsupon FACT trigger:
Soft X-ray /UV band:Swift (~20ks total)XMM-Newton (~100 ks total)
Hard X-ray/ γ-ray band:INTEGRAL (~500 ks total)Fermi/LAT (continuous)
Apply time-resolved jet emission modes
Provide contraints onjet emission models
TeV band:FACT (since 2012) – daily VHE observations – provides detailed variability information– provides flare alerts
Trigger criterium:VHE FACT rate > 70 evts/hour
X-ray / UV band:Swift (since 2014) – weekly scheduled (~1ks)– monitoring of the low–E emission – test for orphan flares & time lags
FACT
Annika Kreikenbohm “Time-Resolved SEDs of Blazar Flares“ The X-ray Universe 2017
Long-Term Monitoring
MWL ToO Program
Time–Resolved SEDs
ToO observationsupon FACT trigger:
Soft X-ray /UV band:Swift (~20ks total)XMM-Newton (~100 ks total)
Hard X-ray/ γ-ray band:INTEGRAL (~500 ks total)Fermi/LAT (continuous)
Apply time-resolved jet emission modes
Provide contraints onjet emission models
TeV band:FACT (since 2012) – daily VHE observations – provides detailed variability information– provides flare alerts
Trigger criterium:VHE FACT rate > 70 evts/hour
X-ray / UV band:Swift (since 2014) – weekly scheduled (~1ks)– monitoring of the low–E emission – test for orphan flares & time lags
FACT
Annika Kreikenbohm “Time-Resolved SEDs of Blazar Flares“ The X-ray Universe 2017
– Operational since 2011
– Imaging Cherenkov Telescope
– Long-term monitoring of blazars
at TeV energies
– Silicon based photosensors:
_ Stable detector performance
_ Observations during moon light
--> Ideal for monitoring
– FACT sources in the MWL Program:
Mrk 421, Mrk 501, 1ES 1959+650
First G-APD Cherenkov Telescope(TU Dortmund, ISDC Geneva, Universität Würzburg, ETH Zürich)
2200 m a.s.l., MAGIC site, Observatorio del Roque de los Muchachos, La Palma, Canary Islands, Spain
Photo: Thomas Krähenbühl
Annika Kreikenbohm “Time-Resolved SEDs of Blazar Flares“ The X-ray Universe 2017
TIME [MJD]
FACT
EXC
ESS
RATE
[evt
s/hr
]
Long-term VHE light curves (nightly binning)
Mrk 421140
120
100
80
60
40
20
0
20172016201520142013
140
120
100
80
60
40
20
0
Mrk 502140
120
100
80
60
40
20
0
1ES 1959+650
5780057600574005720057000568005660056400
140
120
100
80
60
40
20
0
Excess
Rate
[events
hr−
1]
Excess
Rate
[events
hr−
1]
MJD
Excess
Rate
[events
hr−
1]
Mrk 421
Mrk 501
1ES 1959+650
Annika Kreikenbohm “Time-Resolved SEDs of Blazar Flares“ The X-ray Universe 2017
TIME [MJD]
FACT
EXC
ESS
RATE
[evt
s/hr
]
Long-term VHE light curves (nightly binning)
Mrk 421140
120
100
80
60
40
20
0
20172016201520142013
140
120
100
80
60
40
20
0
Mrk 502140
120
100
80
60
40
20
0
1ES 1959+650
5780057600574005720057000568005660056400
140
120
100
80
60
40
20
0
Excess
Rate
[events
hr−
1]
Excess
Rate
[events
hr−
1]
MJD
Excess
Rate
[events
hr−
1]
Mrk 421
Mrk 501
1ES 1959+650
FACT, nightly binning14
12
10
8
6
4
2
0
20172016
140
120
100
80
60
40
20
0
Fermi/LAT, 3-day binning6
5
4
3
2
1
0
Swift/XRT observations30
25
20
15
10
5
0
Swift/UVM2
Swift/UVW2
Swift/UVW1
57800577505770057650576005755057500574505740057350
40
35
30
25
20
15
10
5
0
Flux[T
eV/cm
2/s]
F0.1−300GeV
[10−7ph/cm
2/s]
F0.5−10keV
[10−10cgs]
TIME [MJD]
FUV
[mJy]
Annika Kreikenbohm “Time-Resolved SEDs of Blazar Flares“ The X-ray Universe 2017
FACT>750GeV
FERMI/LAT(0.1 – 300) GeV
SWIFT/XRT(0.2 – 10) keV
SWIFT/UVOT(192 – 290) nm
Mrk 421 m
Jy10
-7 ph
/cm2 /s
TeV/
cm2 /s
10-1
0 er
g/cm
2 /s
FACT, nightly binning14
12
10
8
6
4
2
0
20172016
140
120
100
80
60
40
20
0
Fermi/LAT, 3-day binning6
5
4
3
2
1
0
Swift/XRT observations30
25
20
15
10
5
0
Swift/UVM2
Swift/UVW2
Swift/UVW1
57800577505770057650576005755057500574505740057350
40
35
30
25
20
15
10
5
0
Flux[T
eV/cm
2/s]
F0.1−300GeV
[10−7ph/cm
2/s]
F0.5−10keV
[10−10cgs]
TIME [MJD]
FUV
[mJy]
Annika Kreikenbohm “Time-Resolved SEDs of Blazar Flares“ The X-ray Universe 2017
FACT>750GeV
FERMI/LAT(0.1 – 300) GeV
SWIFT/XRT(0.2 – 10) keV
SWIFT/UVOT(192 – 290) nm
Mrk 421 m
Jy10
-7 ph
/cm2 /s
TeV/
cm2 /s
10-1
0 er
g/cm
2 /s
543210
4
3.5
3
2.5
2
1.5
1
0.5
0
F0.1−300GeV [photons/cm2/s]
FUVW
1[10−10erg
/cm
2/s]
Annika Kreikenbohm “Time-Resolved SEDs of Blazar Flares“ The X-ray Universe 2017
Flux variability 2015 – 2017
VHE/HE emission vs. X-ray flux:- tightly correlated flux variations - no time lags!- both outbursts in 2015 and 2017 follow the same correlation
Ultraviolet emission vs. X-ray flux:- no correlation with high energy emission
Different variabili-ty trends in 2015 – 2017?
Annika Kreikenbohm “Time-Resolved SEDs of Blazar Flares“ The X-ray Universe 2017
Synchrotron Peak Energy Evolution 2015 – 2017
2052 101
10
1
0.1
0.01
10-3
Flux (0.5-10) keV [10−10 cgs]
Epeak[keV]
- correlation between X-ray flux and synchrotron peak energy Epeak
- change in the SED between 2015 and 2017 variations
Annika Kreikenbohm “Time-Resolved SEDs of Blazar Flares“ The X-ray Universe 2017
Triggered observationsSwift MJD 57374 - 57378, ~2 ks dailyINTEGRAL MJD 57375 ~165 ks
FACT alert on 2015-Dec-17 (MJD 57373)rate >70evt/h in 10 min binning
Outburst 2015 Dec 17
Mrk 421
574505740057350
60
50
40
30
20
10
0
MJD
Excess
Rate
[events
hr−
1]
MJD57373.16 57373.18 57373.2 57373.22 57373.24 57373.26 57373
Exce
ssra
te [E
vent
s/h]
0
20
40
60
80
100 FACT Preliminarynightly binning
Annika Kreikenbohm “Time-Resolved SEDs of Blazar Flares“ The X-ray Universe 2017
Outburst 2015 Dec 17
[Hz]ν1310 1610 1910 2210 2510 2710
]-1
s-2
[erg
cm
ν Fν
-1310
-1210
-1110
-1010
Swift 2015/12/17Swift 2015/12/18-20INTEGRAL 2015/12/18-20
Fermi-LAT 2015/12/17Fermi-LAT 2015/12/18-20FACT 2015/12/17FACT 2015/12/18-20
Annika Kreikenbohm “Time-Resolved SEDs of Blazar Flares“ The X-ray Universe 2017
SummaryMrk 421
Mrk 501
FACT VHE monitoring provides fast triggers for MWL campaigns (within 30 min)! Complementary information by monitoring by Swift & Fermi. Comprehensive MWL ToO program during outburts.
Time-resolved broad band SEDs of Blazars in VHE outburst!
MWL Campaign is ongoing.
Kreikenbohm et al. in prep. [Hz]ν
1310 1610 1910 2210 2510 2710
]-1
s-2
[erg
cm
ν Fν
-1310
-1210
-1110
-1010
Swift 2015/12/17Swift 2015/12/18-20INTEGRAL 2015/12/18-20
Fermi-LAT 2015/12/17Fermi-LAT 2015/12/18-20FACT 2015/12/17FACT 2015/12/18-20