1. G.Andrea Caliandro – CRISM 2011 1 G.A. Caliandro 1, L. Falletti 2, J. Cohen-Tanugi 2 and E. Nuss 2 on behalf of the Fermi LAT Collaboration and the Pulsar Timing Consortium 1 Institut de Ciències de l'Espai (IEEC-CSIC) 2 LUPM – Université Montpellier 2 / CNRS-IN2P3 Unraveling HESS J1745-303 with new results from the Fermi-LAT telescope

2. G.Andrea Caliandro – CRISM 2011 2 HESS J1745-303 HESS J1745-303 is classified as unidentified extended source Very complex morphology, which presents 3 identified emission regions (A, B, and C) –Not well understood yet whether the emission is composed of different or a single source –Similar spectral indices have been found for the three peaks in the VHE range Full emission Region A 3EG J1744-3011 F. Aharonian et al., A&A 483, 509–517 (2008) VHE counterpart candidates: –SNR G359.1-0.5 –SNR G359.0-0.9 –PSR J1747-2958 –PSR B1742-30

3. G.Andrea Caliandro – CRISM 2011 3 Environment HESS J1745-303 is at the edge of the overall 12CO distribution along the Galactic Center. The northern part of the HESS source coincides with a local peak of the molecular cloud. The HI gas wraps the CO molecular cloud. Indeed they are physically connected. But in the southern part of the HESS source the CO emission is absent. Hayakawa et al. 2011arXiv1105.5207H 12 CO J=2–1 map HI emission 12 CO J=2–1 map G359.1-0.5 Hayakawa et al. 2011, arXiv:1105.5207

4. G.Andrea Caliandro – CRISM 2011 4 Fermi-LAT data analysis In the Fermi-LAT data a significant excess spatially coincident with HESS J1745-303 was claimed by Hui, et al., (2011, arXiv:1104.4836) The morphology of the excess in the GeV energy range shows complex features, that jointly with the properties of the ISM, can help in the understanding of this source At E>1GeV the emission come mainly from region A, and the morphology is quite similar to the VHE emission At slightly higher energies (E>3GeV), the morphology changes significantly. Region A is not dominant anymore at these energy. On the contrary, the emission come from the southern part of the HESS source. Modeling the excess at E>3GeV with point-like sources, two detections turn out. –src1 : TS~43, Flux(E>0.1GeV) = (6.±3.) 10-8 cm-2 s-1 –src2 : TS~70, Flux(E>0.1GeV) = (8.±3.) 10-8 cm-2 s-1 PRELIMINARY E>1GeV E>3GeV

5. G.Andrea Caliandro – CRISM 2011 5 Summary A significant excess observed by Fermi-LAT is spatially coincident with HESS J1745-303. We studied the morphology of this excess, discovering that at high energies (E>3GeV) the emission is near the regions B, and C, while at lower energy the emission is close to region A, where the VHE gamma rays are dominant. The Fermi-LAT results, with the CO and HI maps, strongly point toward a different nature of the emission coming from region A, with respect to regions B and C. Further in-depth analyses are on-going within the Fermi-LAT collaboration to fully characterize the GeV emission spatially coincident with HESS J1745-303, especially with respect to region A.

6. G.Andrea Caliandro – CRISM 2011 6 Hui, et al., 2011, arXiv:1104.4836 They claimed a detection at 18 and 6 sigma in 1-20GeV and 10-20 GeV, respectively They found that a symple power-law with photon index ~- 2.6 describe the spectrum for E>1GeV calculated with unbinned gtlike for a point source at the nominal position of the HESS source TS maps centered at the nominal position of HESS J1745-303 The blue circle represents the 1 positional error circle determined by gtfindsrc.

7. G.Andrea Caliandro – CRISM 2011 7 MC and HI masses (Hayakawa et al. 2011, arXiv:1105.5207) 12 CO mass = 1.6 x 10 6 M ⊙ –Within the 4 significance contours –Distance of 8.5kpc –Conversion factor N(H 2 )/W( 12 CO 1-0 ) = 7.0 x 10 19 cm -2 (K km s -1 ) -1 HI mass –Optically thin hypothesis: ~ 1 x 10 4 M ⊙ –Optically thik hypothesis: ~ 7 x 10 4 M ⊙