Study of the classical TeV blazars with Fermi: Mrk421, Mrk501, … · 2009-07-15 · Study of the classical TeV blazars with Fermi: Mrk421, Mrk501, 1es1959+650 Outline 1 – Introducon

StudyoftheclassicalTeVblazarswithFermi:Mrk421,Mrk501,1es1959+650

Outline1–Introduc,on(mo,va,ontostudy“classical”TeVblazars)

2–Mrk421

3–Mrk501

4–1es1959

5‐Conclusions

7/14/09 1DavidPaneque

DavidPaneque(SLAC/Kipac)[email protected]

OnbehalfoftheFermicollabora,onandthe

mul,‐frequencycampaignpar,cipants(MAGIC,VERITAS,GASP,OVRO…)

Just a glimpse of some of the (preliminary) results

7/14/09 DavidPaneque 27/14/09 DavidPaneque 2

Large Area Telescope (LAT)

GLAST Burst Monitor (GBM)

Launch: June 11th 2008 Cape Canaveral

Fermi mission (brief overview)

1.8m

1.8mStartofnormalscienceoperaTon:Aug4th2008

DavidPaneque 3

Deepstudiesoffewindividualsources

3c2733c454.3PKS1454PMNJ0948… VeryBrightTeVblazars

Highsignficancedetec,onsDetected>=10agoClassicalTeVsources

3c279,3c66A,BLLac1es1218,PG1553…

PKS2155‐304,1es1959+650Mrk421,Mrk501

“weak”TeVblazarsRela,velylowsignificancedetec,onsInthelast2‐3years!!(thankstobeeerCherenkovTeles.)

Current experimental data allow for a big inter-model and intra-model degeneracy. More and “higher quality” data required to constrain models.

•  Leptonic vs hadronic emission models

•  Acceleration/cooling in single or multi-zone; close or far from BH

• Production of flares (which are the shortest timescales)

• Role of external photon fields

•  Intrinsic spectra vs EBL-affected spectra

•  Time-resolved emission models

•  etc,etc, etc …

DavidPaneque 4

Recently, we had two “performance jumps” with respect to the past:

New Generation of IACTs online since ~4 years (low Eth, high sensitivity)

LAT in operation since almost 1 year (~30 times more sensitive than EGRET)

Culprits for the relatively poor knowledge of these objects 1 - Time-evolving broad band spectra

2 - Poor sensitivity to study high-energy part (E>0.1 GeV)

Coordination of instruments covering different energies needed

Large observation times (with EGRET and “old” IACTs) were required for signal detection Data NOT simultaneous, and most of our HBL knowledge relates to the high state

1–Shortintro(moTvaTontostudy“classical”TeVblazars)

EnhancedobservaTonalcapabilitycanbeusedtoimproveourknowledgeonHBLs

~100TmesmoresensiTveatE>~10GeV

DavidPaneque 5

Dominantgamma‐rayemissionmechanismisbelievedtohavealeptonicorigin(SSC),atleastinhigh(flaring)state

‐FastvariaTons(downtohoursandsub‐hoursinVHE)‐Xrays‐Gamma‐rayscorrelaTon(ingeneral)

ThingsweknowaboutthoseclassicalTeVsources(andHBLsingeneral)

ExcellentlaboratoryforstudyingHighEnergyblazaremission

Stronggammaraysources&&Nearbyobjects;z<~0.1;“low”EBLabsorpTon,wesee“almost”intrinsicfeatures

Mrk 421, Mrk 501, 1ES1959+650 and PKS2155-304

Knowledgeacquiredwiththoseobjectscould(inprinciple)beappliedtootherobjects(fainterand/orlargerz)

1- Motivation to observe (again) the classical TeV blazars

Exquisite characterization of the high energy component, which can be detected with Fermi and Cherenkov Telescopes (20 MeV – 20 TeV)

DavidPaneque 6

Dominantgamma‐rayemissionmechanismisbelievedtohavealeptonicorigin(SSC),atleastinhigh(flaring)state

‐FastvariaTons(downtohoursandsub‐hoursinVHE)‐Xrays‐Gamma‐rayscorrelaTon(ingeneral)

ThingsweknowaboutthoseclassicalTeVsources(andHBLsingeneral)

ExcellentlaboratoryforstudyingHighEnergyblazaremission

Stronggammaraysources&&Nearbyobjects;z<~0.1;“low”EBLabsorpTon,wesee“almost”intrinsicfeatures

Mrk 421, Mrk 501, 1ES1959+650 and PKS2155-304

Knowledgeacquiredwiththoseobjectscould(inprinciple)beappliedtootherobjects(fainterand/orlargerz)

1- Motivation to observe (again) the classical TeV blazars

Exquisite characterization of the high energy component, which can be detected with Fermi and Cherenkov Telescopes (20 MeV – 20 TeV)

AcceptedinApJ(0903.2924)Chiangetal,Thisconference(Tuesday)

Preliminaryresultsinthistalk

DavidPaneque 7

2–Mrk421

Sourceisrela,velylowatX‐rays

RXTE/ASMLightCurve(2‐10keV)LAT

AlldetecTonsofEGRET(9yearsofoperaTon)

RA=166.11;DEC=38.20Z=0.031Firstextragalac,cTeVemieer(Punch et al, 1992, Nature 358, 477)

Knowntobeoneofthefastestvaryinggamma‐raysources(Gaidos, J.A. et al1996, Nature 383, 319; and many other publicaHons).

DetecTonsignificance(EGRET)<~5sigma

MJD

54650 54700 54750 54800 54850 54900 54950 55000

]!

1 s

!2

ph

cm

!8

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x [

10

2

4

6

8

10

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54650 54700 54750 54800 54850 54900 54950 55000

Ph

oto

n in

dex

1.4

1.6

1.8

2

2.2

2.4

DavidPaneque 8

10dayinterval

Jan1st,2009

Sourceisrela,velylowatX‐rays,butveryclearlydetectedwithFermi(on 10‐day Hme intervals, signal typically >10 sigma)

RXTE/ASMLightCurve(2‐10keV)LAT

AlldetecTonsofEGRET(9yearsofoperaTon)

Fermi‐LATsystemaTcallyresolvesMrk421on10‐dayTmescales(regardlessofacTvity)

E>0.3GeV

RA=166.11;DEC=38.20Z=0.031Firstextragalac,cTeVemieer(Punch et al, 1992, Nature 358, 477)

Knowntobeoneofthefastestvaryinggamma‐raysources(Gaidos, J.A. et al1996, Nature 383, 319; and many other publicaHons).

2–Mrk421

Aug4th,2008

Preliminary

Preliminary

7/14/09 DavidPaneque 9

Lightcurvein2‐dayTmebinsFracTonalVariabilityvsEnergy(usingVaughanetal2003)

E>0.2GeV

Becauseofthebrightnessofthissource,LATcanresolveitalsoon,mescalesasshortas2days…andmuchshorterwhenitflares

DatafromAugust4th2008TllJan20th2009(5.5months)

Outofthe852‐day,meintervals:‐ Detectedon79(93%)above3sigmas‐ Detectedon62(73%)above5sigmas

‐ “Hint”ofincreaseofFvarvsenergy‐To be repeated with enHre data set

0.2GeV 0.63GeV 2.0GeV 20GeV

GreatpotenTaltostudySEDvariaTonsinshortTmescaleswithourMWpartners

2–Mrk421ICRC2009D.Panequeetal

MJD

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1.4

1.6

1.8

2

2.2

2.4


Flux/Photonindex(E>0.3GeV)

10dayinterval

MWcampaign01/20‐05/31

Becauseofthehighbrightnessofthissourceingamma‐rays,weaimedatfollowingthemul,‐frequencyac,vityofthesourceonshort,mescales:

OneobservaTonevery2daysBigeffortfrommanygroups!

MWcampaignorganized(4+monthslong):hsps://confluence.slac.stanford.edu/display/GLAMCOG/Campaign+on+Mrk421+(Jan+2009+to+May+2009)

Preliminary

Preliminary

Radio:OVRO,Effelsberg,Noto…Infrared:WIRO,OpTcal:GASP,GRT,MITSuMe…X‐ray:Swiu,RXTEGamma‐ray:FermiVHE:MAGIC,VERITAS

2–Mrk421


hsp://www.slac.stanford.edu/~dpaneque/MW_Mrk421_2009/Obs.html

ObservaTonsandpreliminaryfluxesupdatedonce/twiceaweekDifferent instruments could plan ahead when to observe the source RequestaddiTonalobservaTonsifsourceshowsoutstandingacTvity

ObservaTonsperformed/plannedduringtheMWcampaignavailableontheweb

ThisTme,nobigfluxvariaTonsduringthese~4.5months


2–Mrk421:mulT‐frequencyacTvity

Gamma‐ray,FermiE>0.3GeV

Preliminary(quick&dirtyanalysis)fromvariousinstruments

MJD

54840 54860 54880 54900 54920 54940 54960 54980 55000

No

rm

alized

Flu

x

0.85

0.9

0.95

1

1.05

1.1

OVRO

MJD

54840 54860 54880 54900 54920 54940 54960 54980 55000

No

rm

alized

Flu

x

0.4

0.6

0.8

1

1.2

1.4

GASP

GRT

UVOT!w2

MJD

54840 54860 54880 54900 54920 54940 54960 54980 55000

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rm

alized

Flu

x

0

0.5

1

1.5

2

2.5

3

RXTE/PCA

MJD

54840 54860 54880 54900 54920 54940 54960 54980 55000

No

rm

alized

Flu

x0

0.5

1

1.5

2

2.5

3MAGIC

WHIPPLE

OVRO(15GHz)

OpTcal(RandUV)

X‐raysfromRXTE(2‐10keV)

GASPGRTSwiu‐UVOT

VHE MAGIC(E>0.15TeV)Whipple(E>0.4TeV)

LowacTvityatVHE:~0.5CrabButvariabilityclearlyseen:Min/Maxvalues:~0.1‐1Crab

Someofthefluxesaretheresultofautoma,cprocedures(nochecks)PropermulT‐frequencydatareducTonwillhappenduringthenextmonths

Hostgalaxynotsubtracted!!


MJD

54840 54860 54880 54900 54920 54940 54960 54980 55000

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rm

alized

Flu

x

0.85

0.9

0.95

1

1.05

1.1

OVRO

MJD

54840 54860 54880 54900 54920 54940 54960 54980 55000

No

rm

alized

Flu

x

0.4

0.6

0.8

1

1.2

1.4

GASP

GRT

UVOT!w2

MJD

54840 54860 54880 54900 54920 54940 54960 54980 55000

No

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alized

Flu

x

0

0.5

1

1.5

2

2.5

3

RXTE/PCA

MJD

54840 54860 54880 54900 54920 54940 54960 54980 55000

No

rm

alized

Flu

x0

0.5

1

1.5

2

2.5

3MAGIC

WHIPPLE

OVRO(15GHz)

OpTcal(RandUV)


GASPGRTSwiu‐UVOT

13


VHE MAGIC(E>0.15TeV)Whipple(E>0.4TeV)

LowacTvityatVHE:~0.5CrabButvariabilityclearlyseen:Min/Maxvalues:~0.1‐1Crab

Preliminary(quick&dirtyanalysis)fromvariousinstrumentsSomeofthefluxesaretheresultofautoma,cprocedures(nochecks)

PropermulT‐frequencydatareducTonwillhappenduringthenextmonths



E [MeV]

210

310

410

510

610

710

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s!

2d

N/d

E [

erg

cm

2E

!1210

!1110

!1010

E [MeV]

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s!

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N/d

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erg

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2E

!1210

!1110

!1010


Aug4th,2008–June10th,2009

Jan20,2009–April30,2009

FermiSpectra“upto400GeV“(6evtsinbin150‐400GeV)

Preliminary

Preliminary

2–Mrk421:FermispectraInforma,ononMWcampaignorganizedonthisobject:hsps://confluence.slac.stanford.edu/display/GLAMCOG/Campaign+on+Mrk421+(Jan+2009+to+May+2009)

Preliminary


400GeV0.1GeV

400GeV0.1GeV

SpectrumisconsistentwithPowerLawwithphotonindex1.79+/‐0.02

Fit dominated by the lower energies Turn over at the highest energies might be hidden in low photon count


Energycoverageover3ordersofmagnitude(!!)

E [MeV]

210

310

410

510

610

710

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!1

s!

2d

N/d

E [

erg

cm

2E

!1210

!1110

!1010


Fermi~100days/5.(FoV~20%)=

20“effecTve”days

MAGIC~27hoursofdatanot‐EBLcorrected

Preliminary

First“simultaneous”GeV‐TeVspectrumofMrk421

Goodagreementbetweenthese2differentinstruments.Energycoverageof5ordersofmagnitudewithoutGAPS.Importantformodelingofthesource

80GeV 400GeVOverlappingregion

caveat

Jan20,2009–April30,2009

E [MeV]

210

310

410

510

610

710

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!1

s!

2d

N/d

E [

erg

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2E

!1210

!1110

!1010


Fermi~100days/5.(FoV~20%)=

20“effecTve”days

MAGIC~27hoursofdatanot‐EBLcorrected

Preliminary

First“simultaneous”GeV‐TeVspectrumofMrk421

80GeV 400GeVOverlappingregion

caveat

Jan20,2009–April30,2009

OneofthegoalsofFermi:closingthegapbetweensatelliteandgroundgamma‐rayinstruments:MissionAccomplished!!


Dataanalysisongoing…

2–Mrk421Informa,ononMWcampaignorganizedonthisobject:hsps://confluence.slac.stanford.edu/display/GLAMCOG/Campaign+on+Mrk421+(Jan+2009+to+May+2009)

OverallSEDduringthecampaign(Jan20th–April30th)

Variousradioinstruments

WIRO(IR)

Op,cal+SwisUV

SwiuXRT

SwiuBAT

RXTEPCA

SyncandICpeaksWILLBEfullycharacterizedtightconstrainstoemissionmodels

Fermi

MAGIC


3–Mrk501

RXTE/ASMLightCurve(2‐10keV)

Sourceisrela,velylowatX‐rays,

LATNotpresentin3rdEGRETcatalogueOnlydetecTon(~5sigma)withEGRETwasduringaflarein1996(Kataokaetal1999)EGRETdidnotdetectitduringthebigoutburstin97

1997

RA=253.47;DEC=39.76Z=0.034DiscoveryatVHE:Quinnetal.,1996‐Hugeflarein1997(manypublica,ons)‐ Shortfluxvaria,onsdetectedin2005 MAGIC, Albert et al, 2007

2minbins

~20minMAGIC

MJD

54700 54750 54800 54850 54900 54950 55000

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54700 54750 54800 54850 54900 54950 55000

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1.5

2

2.5

3

3.57/14/09 DavidPaneque 19

3–Mrk501

10dayinterval


Jan1st,2009

Sourceisrela,velylowatX‐rays,butdecentlydetectedwithFermion10day,meinterval

Fluxincrease(2or3)byFebruary2009

LAT

LATsystemaTcallyresolvesMrk501on10‐dayTmescales

Notpresentin3rdEGRETcatalogueOnlydetecTon(~5sigma)withEGRETwasduringaflarein1996(Kataokaetal1999)EGRETdidnotdetectitduringthebigoutburstin97

1997

2minbins

~20minMAGIC

RA=253.47;DEC=39.76Z=0.034DiscoveryatVHE:Quinnetal.,1996‐Hugeflarein1997(manypublica,ons)‐ Shortfluxvaria,onsdetectedin2005 MAGIC, Albert et al, 2007

Preliminary

Aug4th,2008

MJD

54700 54750 54800 54850 54900 54950 55000

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ph

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!8

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10

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1

2

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5

6

MJD

54700 54750 54800 54850 54900 54950 55000

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n in

dex

1

1.5

2

2.5

3

3.5


3–Mrk501

Flux/Photonindex(E>0.3geV)

10dayinterval


LessbrightthanMrk421atgamma‐rays.

MWcampaignorganized(4+monthslong):hsps://confluence.slac.stanford.edu/display/GLAMCOG/Campaign+on+Mrk501+(March+2009+to+July+2009)

OneobservaTonevery5days

Samplingfrequencyincreaseswhensourceisfoundhigh:We triggered observaHons with various instruments in May when the source was relaHvely high and variable at gamma‐rays during few days

Bigeffortfrommanygroups!

InstrumentsparTcipaTng

Radio:OVRO,Effelsberg,Metsahovi,Noto…Infrared:WIRO,OpTcal:GASP,GRT,MITSuMe,Kanata…X‐ray:Swiu,RXTEGamma‐ray:FermiVHE:MAGIC,VERITAS

Preliminary

7/14/09 DavidPaneque


MJD

54900 54920 54940 54960 54980 55000

No

rm

alized

Flu

x

0.85

0.9

0.95

1

1.05

OVRO

MJD

54900 54920 54940 54960 54980 55000

No

rm

alized

Flu

x

0.6

0.7

0.8

0.9

1

1.1

1.2

1.3

GASP

GRT

UVOT!w2

MJD

54900 54920 54940 54960 54980 55000

No

rm

alized

Flu

x

0.6

0.8

1

1.2

1.4

1.6

RXTE

OVRO(15GHz)

OpTcal(RandUV)


GASPGRTSwiu‐UVOT

MJD

54900 54920 54940 54960 54980 55000

]!

1 s

!2

ph

cm

!8

Flu

x [

10

0

1

2

3

4

5

6

Flux_300MeV_TS4

MJD

54700 54750 54800 54850 54900 54950 55000

Ph

oto

n in

dex

1

1.5

2

2.5

3

3.5

PhotonIndex


MAGIC(E>0.15TeV);Whipple(E>0.4TeV)

LowacTvityatVHE:~0.3CrabButvariabilityclearlyseen:Min/Maxvalues:~0.05‐1Crab(+1nightat2Crab)

MJD54900 54920 54940 54960 54980 55000

No

rmalized

Flu

x

0

1

2

3

4

5

6

MAGIC

Whipple

Preliminary(quick&dirtyanalysis)fromvariousinstrumentsSomeofthefluxesaretheresultofautoma,cprocedures(nochecks)

PropermulT‐frequencydatareducTonwillhappenduringthenextmonths


E [MeV]

210

310

410

510

610

710

]

!1

s!

2d

N/d

E [

erg

cm

2E

!1210

!1110

!1010


3–Mrk501:Fermispectrum

Aug4th,2008–June10th,2009

Informa,ononMWcampaignorganizedonthisobject:hsps://confluence.slac.stanford.edu/display/GLAMCOG/Campaign+on+Mrk501+(March+2009+to+July+2009)

Preliminary


WorkongoingtowardstheCombinedGeV‐TeVspectrumfromMrk501.

OverlapGeV‐TeVisalsograntedforthisdataset

400GeV0.1GeV SpectrumisconsistentwithPowerLawwithphotonindex1.72+/‐0.04

Energycoverageover3ordersofmagnitude(!!)


4–1es1959+650

MJD

54650 54700 54750 54800 54850 54900 54950 55000

]!

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ph

cm

!8

Flu

x [

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2

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4

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6

MJD

54650 54700 54750 54800 54850 54900 54950 55000

Ph

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dex

1

1.5

2

2.5

3

3.5

4

4.5

Flux/Photonindex(E>0.3GeV)

10dayinterval


Jan1st,2009

Sourceisratherweak,butitcanberesolvedin~10day,mescale(lowsignificance)

NeverDetectedwithEGRET(!!!)

LATRA=300.0;DEC=65.14z=0.049Discoveryatgamma:Nishiyamaetal,1999

Orphanflarein2002(Krawcynskietal2004)

X‐rayfluxisrela,velyhighwithrespecttopastobserva,ons,althoughNOTinflare

Preliminary

Aug4th,2008

MJD

54650 54700 54750 54800 54850 54900 54950 55000

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!8

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4

4.57/14/09 DavidPaneque 24

4–1es1959+650NeverDetectedwithEGRET(!!!)

Becauseofthelowbrightnessofthissourceatgamma‐rays,weaimedatproducingessen,allysnapshotsoftheSED(Big difference with the Mrks)

1–Shortcampaign(1.5months)2–DuetovariousreasonswecouldnotgetenoughTeVobserva,ons(2hoursVeritasand1hourMAGIC)

3–Butwecouldget20hours(moon)datawithMAGICinMay/June.

Informa,ononMWcampaignorganizedonthisobject:hsps://confluence.slac.stanford.edu/pages/viewpage.acTon?pageId=28967275

Instrumentspar,cipa,ng

Flux/Photonindex(E>0.3geV)

10dayinterval


Radio:OVRO,Effelsberg,PicoVeleta…OpTcal:GASP,Flagstaff,MITSuMe,Kanata..X‐ray:Swiu,RXTEGamma‐ray:FermiVHE:MAGIC,VERITAS

Preliminary

E [MeV]

210

310

410

510

610

710

]

!1

s!

2d

N/d

E [

erg

cm

2E

!1210

!1110

!1010


4–1es1959+650:FermispectrumNeverDetectedwithEGRET(!!!)

Informa,ononMWcampaignorganizedonthisobject:hsps://confluence.slac.stanford.edu/pages/viewpage.acTon?pageId=28967275

Aug4th,2008–June10th,2009 FermiSpectra“upto150GeV“(3evtsinbin63‐158GeV)

CombinedGeV‐TeVdatawillprobablyhaveaGAPforthissource:

FromFermi:2monthsofdatawillreach<~60GeV

FromMAGIC:Rela,velylargezenithangle(40deg)Moonobserva,onsHigherthresholdenergy(200GeV??)


Preliminary


In‐depthstudyofindividualsourcesisimportanttounderstandthephysicalprocessesoccurringinthoseobjects

Studyoftheclassical(bright)TeVsourceshastheadvantagethat,togetherwiththeIACTs,Fermidataconstrainthehighenergybump

‐Fermidataopensa“newwindow”tostudythoseobjects Spectrareachingenergiesbeyond0.1TeV;overlapwithIACTs ‐CollecTonofMWdataisESSENTIALforunderstandingthosecomplexobjects.

WearecollecTnganexquisitedatasetthatwillsurelyhelpustounderstandtheseextremeobjects,andtheblazarphenomenon.Someoftheresultsalreadyout,manyotherstocome.

5‐ConclusionsFermi in survey mode since beginning of August, boosting our current capabilities to study AGNs. UniformexposureCoverageof20%skyatanyTmeLargeeffecTvearea,smallPSF…

Itbringsdatathatwasnon‐existentbeforeandthusitisexpectedtoconstrainthecurrenttheoreTcalmodelspredicTngthegamma‐rayemission

Staytuned:weliveexciTngTmesforgamma‐rayastronomy

Documents

Study of the classical TeV blazars with Fermi: Mrk421, Mrk501, … · 2009-07-15 · Study of the classical TeV blazars with Fermi: Mrk421, Mrk501, 1es1959+650 Outline 1 – Introducon