the x-ray universe 2017, rome, italy time-resolved seds of ... · annika reikenbohm time-resolved...

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; ...)





e-,e+ synchrotron emission





?e-,e+ synchrotron emission





?e-,e+ synchrotron emission

IC/ EC emission?

Proton synchrotron?photo-hadronic?


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


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


– 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


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]


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]


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?


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


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


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


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

the x-ray universe 2017, rome, italy time-resolved seds of ... · annika reikenbohm time-resolved...

Documents