ICREA Workshop on the High Energy Emission from pulsars and their ...

<strong>ICREA</strong> <strong>Workshop</strong> on the High Energy Emission from pulsars and their systems1st Session of the Sant Cugat Forum on Astrophysics – Sant Cugat, April 12-16, 2010

In the 30-100 MeV AGILEsensitivity is competitive(500 cm 2 eff. Area for timing).The 1 GeV Fermi sensitivity ismuch better than the AGILE one.

AGILE counts > FermiE AGILEE>1 GeVPellizzoni et al. 2009Abdo et al. 2009

The “soft” γ-pulsar B1509-58AGILE (Pilia et al.)Fermi (Abdo et al.)

The “soft” γ-pulsar B1509-58Pellizzoni et al., 2009; Abdo et al., 2010Pilia et al., 2010, submittedCOMPTELAGILEA new class of “soft” gamma-ray pulsars?

Bright Gamma-ray Pulsars (E>50 MeV)GemingaCrabVela

AGILEMt. Pleasant(Hobart, Tasmania)

40000 pulsed countscollected from Vela PSR(Pellizzoni et al. 2009).5000 ToAs from radioobservations by Mt.Pleasant radiotelescope(Hobart, Tasmania).P GAMMA -P RADIO

Vela Pulsar hides nearly 100 squaredegrees of the gamma-ray sky!GemingaCrabVela

Discarding eventswithin time intervalscorresponding to pulsephase (0.05-0.65)No pulsed gamma-rayemission detectedoutside this intervalas reported byprevious observationswith EGRET, AGILEand FERMI

Discarding eventswithin time intervalscorresponding to pulsephase (0.05-0.65)No pulsed gamma-rayemission detectedoutside this intervalas reported byprevious observationswith EGRET, AGILEand FERMI

Discarding eventswithin time intervalscorresponding to pulsephase (0.05-0.65)No pulsed gamma-rayemission detectedoutside this intervalas reported byprevious observationswith EGRET, AGILEand 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

Chandra

HESSAharonian et al. 2006X-rays-GeV-TeV association

Flux E>100 MeV= 35x10 -8 ph/cm 2 /sLocated 0.5 deg SW Vela PSR and 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 observations in 2011 (www.srt.inaf.it)

~85 Non-Variable EGRET Unidentified Sources

Unidentified gamma-ray sources:PWNe Sync/IC emission?(Pellizzoni et al., 2005, 2009)PWNe are a common phenomenon associated to young and energeticpulsars (but weaker than pulsed emission at GeV).If the pulsar beamed emission does not intersect the line of sightto the observer, the PWN component unhindered by the strongerpulsed emission, could be detectable.E>100 MeVBrightest “undisturbed” pulsars = a class of unidentified sources(A new significant component for the diffuse gamma-ray emission?)

About 40 bright (E ROT >10 35 erg/s) and nearby (dist100 bright and nearby pulsar that couldbe observed as PWN only

HESSRADIOAharonian et al. 2006

HESSAharonian et al. 2006

HESSAharonian et al. 2006

<strong>ICREA</strong> <strong>Workshop</strong> on the High Energy Emission from pulsars and their systems1st Session of the Sant Cugat Forum on Astrophysics – Sant Cugat, April 12-16, 2010