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Fermi Analysis Benoit Lott Centre dEtudes Nuclaires de Bordeaux- Gradignan lott@cenbg.in2p3.fr Atelier CTA Oct. 2017 Outline The Fermi Large Area Telescope (LAT) Highlights Performance LAT data Standard analysis

  1. Fermi Analysis Benoit Lott Centre d’Etudes Nucléaires de Bordeaux- Gradignan lott@cenbg.in2p3.fr Atelier CTA Oct. 2017

  2. Outline The Fermi Large Area Telescope (LAT) • Highlights • Performance • LAT data • Standard analysis •

  3. Compton Observatory / EGRET legacy April 5, 1991 – June 4, 2000 3rd EGRET catalog 271 sources AGN – blazars (70) unidentified Pulsars (7) LMC X25 lower sensitivity than Fermi LAT Atelier CTA Oct. 2017

  4. The Large Area Telescope on board the Fermi satellite (launch: June 11, 2008) γ incoming gamma ray Crédit: NASA e - e + pair Atelier CTA Oct. 2017

  5. June 11, 2008 Launch from Cape Kennedy altitude: 565 km inclination: 25.6° orbital period: 91 min Atelier CTA Oct. 2017

  6. Atelier CTA Oct. 2017

  7. The Fermi LAT Atelier CTA Oct. 2017

  8. Tracker Atelier CTA Oct. 2017

  9. Photons gamma dans le LAT Les croix vertes indiquent les positions détectées des particules chargées, les lignes bleues indiquent les trajectoires reconstruites à partir des traces, et la ligne jaune montre la direction estimée du photon gamma. Les croix rouges indiquent les dépôts d'énergie détectés dans le calorimètre. Atelier CTA Oct. 2017

  10. Novel features The Fermi-LAT allows for unprecedented studies about • morphology • spectra • variability in the GeV band Atelier CTA Oct. 2017

  11. Fermi highlights and discoveries Atelier CTA Oct. 2017

  12. GC excess (992/3031) Atelier CTA Oct. 2017

  13. 9-year sky map E>1 GeV Atelier CTA Oct. 2017

  14. 3FGL (E>100 MeV) 4 years of data, 3031 sources Atelier CTA Oct. 2017

  15. 3FHL (E> 10 GeV) 7 years of data, 1556 sources Atelier CTA Oct. 2017

  16. Source catalogs Catalog Energy Data Sources Unasso- Event Release Range Interval ciated Selection Date (GeV) (m) 0FGL 0.2-100 3 205 37 (18%) P6V1 Feb. 2009 DIFFUSE 1FGL 0.1-100 11 1451 630 (43%) P6V3 DIFFUSE Feb. 2010 2FGL 0.1-100 24 1873 649 (35%) P7V6 Aug. 2011 SOURCE 1FHL 10-500 36 511 65 (13%) P7V6 Jun. 2013 CLEAN 3FGL 0.1-300 48 3031 992 (33%) P7V15 Jan. 2015 SOURCE 2FHL 50-2000 80 360 48 (14%) P8 SOURCE Aug. 2015 3FHL 10-2000 84 1556 176 (11%) P8 SOURCE Mar. 2017 4FGL 0.1-1000 96 ~7500 ~2500(30%)? P8 SOURCE Jan. 2018? Atelier CTA Oct. 2017

  17. Age: a few millions years Remnant of a jet ? Intense episod of star formation? Atelier CTA Oct. 2017 Fusion of a secondary black hole?

  18. Excess around Galactic Center Fluctuation analysis favors the presence of a large population of unresolved sources (e.g., MSPs) Bartels+16 Ackermann+17 Atelier CTA Oct. 2017

  19. Pulsars Summary Statistics Total number of pulsars: 205 Young, radio selected : 53 Young, gamma selected : 54 Young, X-ray selected : 5 Total number young PSRs : 112 MSP, radio selected : 92 MSP, gamma selected : 1 Total number of MSPs : 93 Total number of binaries : 73 Found in radio searches of LAT sources : 54 EGRET/COMPTEL pulsars: 7 Atelier CTA Oct. 2017

  20. Shell SNRs Hewitt14 Atelier CTA Oct. 2017

  21. Highlights of AGN results • Over 1600 dected AGNs, 98% of them being blazars. FSRQs FSRQs • Possible existence of a « Blazar Sequence »: connection between luminosity and maximum particle energy Mrk421 • Luminosity functions: evolutionary link between species? disk vs BH spin power? • Continuous monitoring: Ajello+ 12 • variability times scales probed from minutes to years • unique ressource for the community (time-resolved SEDs) • Spectral curvature of many FSRQS: intrincic curvature of electron energy distributions FSRQs BL Lacs BL Lacs • Resolution of extended radiogalaxies: Cen A BCUs • Probing of EBL and IGMF • Periocity of PG 1153+113 Atelier CTA Oct. 2017

  22. Search for dark matter Charles, E. et al. 2016, Phys. Rep., 636, 1 Atelier CTA Oct. 2017

  23. More highlights • Diffuse emission • Fermi bubbles Ajello+ 14 • Extragalactic Gamma-ray Background • CRE spectrum, positron fraction • GRBs • ~150 LAT events • afterglow • detection of very late high-energy photons • time delays • multiple spectral components in prompt emission • constraints on EBL and LIV • Solar physics • Detection of two separate components in the solar emission • Detection of three behind-the-limb solar flares • 2012 March 7 flare: localization, late emission (>20 hr), 4 GeV photon Atelier CTA Oct. 2017

  24. Search for Transients continuous sky survey • >400 ATels • Flare Advocates • FAVA Atelier CTA Oct. 2017

  25. Performance Atelier CTA Oct. 2017

  26. Event classes/types https://fermi.gsfc.nasa.gov/ssc/data/analysis/LAT_essentials.html https://fermi.gsfc.nasa.gov/ssc/data/analysis/documentation/Cicerone/ Tradeoff between statistics and residual-background contamination Different partitions of data according to: • conversion type • PSF • energy dispersion Atelier CTA Oct. 2017

  27. Effective area (Aeff) http://www.slac.stanford.edu/exp/glast/groups/canda/lat_Performance.htm Aeff vs energy Aeff vs incidence angle LAT FoV GBM FoV Atelier CTA Oct. 2017

  28. Point Spread Function (PSF) PSF vs Energy PSF vs incidence angle Atelier CTA Oct. 2017

  29. Energy resolution ∆ E/E vs Energy ∆ E/E vs Incidence angle Atelier CTA Oct. 2017

  30. LAT data Atelier CTA Oct. 2017

  31. Downloading data https://fermi.gsfc.nasa.gov/cgi-bin/ssc/LAT/LATDataQuery.cgi Atelier CTA Oct. 2017

  32. Data cuts Cut on zenith angle to reduce earth-limb background Atelier CTA Oct. 2017

  33. The Fermi-LAT data Explore a weekly data file with the command fv (fits viewer)  fv lat_photon_weekly_wxxx_p302_v001.fits GTI: good time intervals Atelier CTA Oct. 2017

  34. The spacecraft data fv lat_spacecraft_weekly_wxxxx_p202_v001.fits Atelier CTA Oct. 2017

  35. Data analysis Atelier CTA Oct. 2017

  36. Inspecting the ROI Many (overlapping ) sources in the ROI → maximum likelihood! Detected sources are listed in the 3FGL Catalog: http://fermi.gsfc.nasa.gov/ssc/data/access/lat/4yr_catalog/ Atelier CTA Oct. 2017

  37. Likelihood analysis: basics The source model is considered as: This model is folded with the Instrument Response Functions (IRFs) to obtain the predicted counts in the measured quantity space (E’,p’,t’): where  L ( t ) is the combined IRF. is the orientation vector of the spacescraft. The integral is performed over the Source Region, i.e. the sky region encompassing all sources contributing to the Region-of – Interest (ROI). In the standard analysis, only steady sources are considered Atelier CTA Oct. 2017

  38. Likelihood analysis: basics The function to maximize is: where the sum is performed over photons in the ROI. The predicted number of counts is: To save CPU time, a model-independent quantity, « exposure map (cube)» is precomputed: Then Atelier CTA Oct. 2017

  39. Diffuse-emission models 100 MeV • Galactic diffuse model: gll_iem_v06.fits model adjusted to data • Extragalactic diffuse model actually sum of true gamma-ray extragalactic diffuse+ instrumental background Ex: iso_P8R2_SOURCE_V6_v06.txt 10 GeV 34.171 2.52894e-06 2.02085e-09 44.3332 1.2486e-06 6.37177e-10 57.5177 6.14648e-07 4.13763e-10 74.6231 3.09835e-07 2.20674e-10 96.8155 1.58407e-07 1.36949e-10 125.608 9.04064e-08 8.11021e-11 162.963 5.44142e-08 5.50435e-11 211.427 2.96885e-08 3.16824e-11 274.305 1.579e-08 2.14466e-11 355.881 8.43735e-09 1.23411e-11 461.718 4.44418e-09 8.65201e-12 599.03 2.29861e-09 4.88778e-12 ….. Atelier CTA Oct. 2017

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