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
Flu
x [
10
2
4
6
8
10
MJD
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
54650 54700 54750 54800 54850 54900 54950 55000
]!
1 s
!2
ph
cm
!8
Flu
x [
10
2
4
6
8
10
MJD
54650 54700 54750 54800 54850 54900 54950 55000
Ph
oto
n in
dex
1.4
1.6
1.8
2
2.2
2.4
7/14/09 DavidPaneque 10
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
7/14/09 DavidPaneque 11
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
7/14/09 DavidPaneque 12
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
No
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!!
7/14/09 DavidPaneque 13
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
No
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
13
Gamma‐ray,FermiE>0.3GeV
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
Hostgalaxynotsubtracted!!
2–Mrk421:mulT‐frequencyacTvity
E [MeV]
210
310
410
510
610
710
]
!1
s!
2d
N/d
E [
erg
cm
2E
!1210
!1110
!1010
E [MeV]
210
310
410
510
610
710
]
!1
s!
2d
N/d
E [
erg
cm
2E
!1210
!1110
!1010
7/14/09 DavidPaneque 14
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
FermiSpectra“upto400GeV“(2evtsinbin150‐400GeV)
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
SpectrumisconsistentwithPowerLawwithphotonindex1.74+/‐0.03
Energycoverageover3ordersofmagnitude(!!)
E [MeV]
210
310
410
510
610
710
]
!1
s!
2d
N/d
E [
erg
cm
2E
!1210
!1110
!1010
7/14/09 DavidPaneque 15
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
]
!1
s!
2d
N/d
E [
erg
cm
2E
!1210
!1110
!1010
7/14/09 DavidPaneque 16
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!!
7/14/09 DavidPaneque 17
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
7/14/09 DavidPaneque 18
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
]!
1 s
!2
ph
cm
!8
Flu
x [
10
0
1
2
3
4
5
6
MJD
54700 54750 54800 54850 54900 54950 55000
Ph
oto
n in
dex
1
1.5
2
2.5
3
3.57/14/09 DavidPaneque 19
3–Mrk501
10dayinterval
RXTE/ASMLightCurve(2‐10keV)
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
]!
1 s
!2
ph
cm
!8
Flu
x [
10
0
1
2
3
4
5
6
MJD
54700 54750 54800 54850 54900 54950 55000
Ph
oto
n in
dex
1
1.5
2
2.5
3
3.5
7/14/09 DavidPaneque 20
3–Mrk501
Flux/Photonindex(E>0.3geV)
10dayinterval
MWcampaign03/15‐07/31
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
3–Mrk501:mulT‐frequencyacTvity
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)
X‐raysfromRXTE(2‐10keV)
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
Gamma‐ray,FermiE>0.3GeV
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
Hostgalaxynotsubtracted!!
E [MeV]
210
310
410
510
610
710
]
!1
s!
2d
N/d
E [
erg
cm
2E
!1210
!1110
!1010
7/14/09 DavidPaneque 22
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
FermiSpectra“upto400GeV“(4evtsinbin150‐400GeV)
WorkongoingtowardstheCombinedGeV‐TeVspectrumfromMrk501.
OverlapGeV‐TeVisalsograntedforthisdataset
400GeV0.1GeV SpectrumisconsistentwithPowerLawwithphotonindex1.72+/‐0.04
Energycoverageover3ordersofmagnitude(!!)
7/14/09 DavidPaneque 23
4–1es1959+650
MJD
54650 54700 54750 54800 54850 54900 54950 55000
]!
1 s
!2
ph
cm
!8
Flu
x [
10
0
1
2
3
4
5
6
MJD
54650 54700 54750 54800 54850 54900 54950 55000
Ph
oto
n in
dex
1
1.5
2
2.5
3
3.5
4
4.5
Flux/Photonindex(E>0.3GeV)
10dayinterval
RXTE/ASMLightCurve(2‐10keV)
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
]!
1 s
!2
ph
cm
!8
Flu
x [
10
0
1
2
3
4
5
6
MJD
54650 54700 54750 54800 54850 54900 54950 55000
Ph
oto
n in
dex
1
1.5
2
2.5
3
3.5
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
MWcampaign09/20‐11/05
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
7/14/09 DavidPaneque 25
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??)
SpectrumisconsistentwithPowerLawwithphotonindex1.96+/‐0.05
Preliminary
7/14/09 DavidPaneque 26
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