ICREA Workshop on the High Energy Emission from pulsars and their ...
ICREA Workshop on the High Energy Emission from pulsars and their ...
ICREA Workshop on the High Energy Emission from pulsars and their ...
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<str<strong>on</strong>g>ICREA</str<strong>on</strong>g> <str<strong>on</strong>g>Workshop</str<strong>on</strong>g> <strong>on</strong> <strong>the</strong> <strong>High</strong> <strong>Energy</strong> Emissi<strong>on</strong> <strong>from</strong> <strong>pulsars</strong> <strong>and</strong> <strong>the</strong>ir systems1st Sessi<strong>on</strong> of <strong>the</strong> Sant Cugat Forum <strong>on</strong> Astrophysics – Sant Cugat, April 12-16, 2010
In <strong>the</strong> 30-100 MeV AGILEsensitivity is competitive(500 cm 2 eff. Area for timing).The 1 GeV Fermi sensitivity ismuch better than <strong>the</strong> AGILE <strong>on</strong>e.
AGILE counts > FermiE AGILEE>1 GeVPellizz<strong>on</strong>i et al. 2009Abdo et al. 2009
The “soft” γ-pulsar B1509-58AGILE (Pilia et al.)Fermi (Abdo et al.)
The “soft” γ-pulsar B1509-58Pellizz<strong>on</strong>i et al., 2009; Abdo et al., 2010Pilia et al., 2010, submittedCOMPTELAGILEA new class of “soft” gamma-ray <strong>pulsars</strong>?
Bright Gamma-ray Pulsars (E>50 MeV)GemingaCrabVela
AGILEMt. Pleasant(Hobart, Tasmania)
40000 pulsed countscollected <strong>from</strong> Vela PSR(Pellizz<strong>on</strong>i et al. 2009).5000 ToAs <strong>from</strong> radioobservati<strong>on</strong>s by Mt.Pleasant radiotelescope(Hobart, Tasmania).P GAMMA -P RADIO
Vela Pulsar hides nearly 100 squaredegrees of <strong>the</strong> gamma-ray sky!GemingaCrabVela
Discarding eventswithin time intervalscorresp<strong>on</strong>ding to pulsephase (0.05-0.65)No pulsed gamma-rayemissi<strong>on</strong> detectedoutside this intervalas reported byprevious observati<strong>on</strong>swith EGRET, AGILE<strong>and</strong> FERMI
Discarding eventswithin time intervalscorresp<strong>on</strong>ding to pulsephase (0.05-0.65)No pulsed gamma-rayemissi<strong>on</strong> detectedoutside this intervalas reported byprevious observati<strong>on</strong>swith EGRET, AGILE<strong>and</strong> FERMI
Discarding eventswithin time intervalscorresp<strong>on</strong>ding to pulsephase (0.05-0.65)No pulsed gamma-rayemissi<strong>on</strong> detectedoutside this intervalas reported byprevious observati<strong>on</strong>swith EGRET, AGILE<strong>and</strong> FERMI
Vela
ph/cm 2 /s/sr0.25x0.25 deg bins
l=263.1, b=0.6, 5σ, new unidentified
l=263.9, b=-3.2, 6σ
Ch<strong>and</strong>ra
HESSAhar<strong>on</strong>ian et al. 2006X-rays-GeV-TeV associati<strong>on</strong>
Flux E>100 MeV= 35x10 -8 ph/cm 2 /sLocated 0.5 deg SW Vela PSR <strong>and</strong> 1.5x1 deg “apparent” extent
EGRET U.L.
L AGILE =4x10 33 erg/s (0.1-10 GeV)L HESS =10 33 erg/s
deJager et al., 2008
CMBR FIRStarlight
VELA X in radio (Hales et al., 2004)31 GHz 8.4 GHz 4.8 GHz
8.4 GHz
CMBR FIRStarlightE ph =1 eV
deJager et al., 2008
Sardinia Radio Telescope (64 m dish) by INAF & ASIwill start pulsar observati<strong>on</strong>s in 2011 (www.srt.inaf.it)
~85 N<strong>on</strong>-Variable EGRET Unidentified Sources
Unidentified gamma-ray sources:PWNe Sync/IC emissi<strong>on</strong>?(Pellizz<strong>on</strong>i et al., 2005, 2009)PWNe are a comm<strong>on</strong> phenomen<strong>on</strong> associated to young <strong>and</strong> energetic<strong>pulsars</strong> (but weaker than pulsed emissi<strong>on</strong> at GeV).If <strong>the</strong> pulsar beamed emissi<strong>on</strong> does not intersect <strong>the</strong> line of sightto <strong>the</strong> observer, <strong>the</strong> PWN comp<strong>on</strong>ent unhindered by <strong>the</strong> str<strong>on</strong>gerpulsed emissi<strong>on</strong>, could be detectable.E>100 MeVBrightest “undisturbed” <strong>pulsars</strong> = a class of unidentified sources(A new significant comp<strong>on</strong>ent for <strong>the</strong> diffuse gamma-ray emissi<strong>on</strong>?)
About 40 bright (E ROT >10 35 erg/s) <strong>and</strong> nearby (dist100 bright <strong>and</strong> nearby pulsar that couldbe observed as PWN <strong>on</strong>ly
HESSRADIOAhar<strong>on</strong>ian et al. 2006
HESSAhar<strong>on</strong>ian et al. 2006
HESSAhar<strong>on</strong>ian et al. 2006
<str<strong>on</strong>g>ICREA</str<strong>on</strong>g> <str<strong>on</strong>g>Workshop</str<strong>on</strong>g> <strong>on</strong> <strong>the</strong> <strong>High</strong> <strong>Energy</strong> Emissi<strong>on</strong> <strong>from</strong> <strong>pulsars</strong> <strong>and</strong> <strong>the</strong>ir systems1st Sessi<strong>on</strong> of <strong>the</strong> Sant Cugat Forum <strong>on</strong> Astrophysics – Sant Cugat, April 12-16, 2010