Fermi_CTAmeeting_2011-09.ppt Fermi Fermi GeV GeV ガンマ線衛星 ガンマ線衛星 による 3 年間の成果 による 年間の成果 Sep. 30, 2011@ICRR (Multi-Messenger Astrophysics and CTA) and CTA) T. Mizuno ( 広島大学 理学部 -> ( 広島大学 理学部 > 宇宙科学センター ) On behalf of the Fermi-LAT collaboration /27 1 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt Fermi Gamma Fermi Gamma- -ray Space Telescope ray Space Telescope • Fermi = LAT + GBM • LAT = “GeV” Gamma-ray Space Telescope LAT “G V” G S T l (20 MeV ~ >300 GeV ) 2008.06 launch 2008.08 Sci. Operation 3c454.3 Cape Canaveral, 1873 sources Abdo+, ApJS submitted Florida /27 2 arXiv:1108.1435 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt Fermi- Fermi -LAT Performance LAT Performance • New Dataset and Response (Pass7) – Improved Aeff in low Energy Improved Aeff in low Energy – In-orbit calibration of PSF http://www.slac.stanford.edu/exp/glast/groups/canda/lat_Performance.htm p p g g p Effective Area PSF comparable to PSF of IACT (>10 GeV) 1 year Integral Sensitivity (>10GeV): ~0.05 Crab (Atwood+09) /27 3 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt Fermi Fermi- -LAT Publications LAT Publications • Publications by Fermi-LAT members (C t I II III (Cat I+II+III, as of mid-Sep. 2011) f id S 2011) 2008 2009 2010 2011 ~200 papers already published 6 7 6-7 papers/month / th http://www-glast.stanford.edu/cgi-bin/pubpub /27 4 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt 2FGL: Second Source Catalog 2FGL: Second Source Catalog • 1873 sources (~4 σ significance) – 127 firm identifications and 1170 reliable associations 127 firm identifications and 1170 reliable associations – 576 unassociated with known γ -ray source class please pay attention to flags (e.g., 126 possibly confused with diffuse emission) Preliminary Abdo+, ApJS submitted arXiv:1108.1435 /27 5 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt Kifune Kifune Plot Plot • # of sources exponentially increases in GeV • Future: 1000 sources in TeV by CTA!? • Future: 1000 sources in TeV by CTA!? (200 publications) HE γ -rays E VHE γ -rays /27 6 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt Source Classes in 2FGL Source Classes in 2FGL • # of known blazars and pulsars continue to grow • 12 spatially extended sources (LMC/SMC SNR and • 12 spatially extended sources (LMC/SMC, SNR and PWN) SNR GC, HMB, Pulsars 4% 6% normal gal. etc. 1% 1% Non-blazar AGN 1% Bl Blazars Unknown 57% 31% >=50% are blazars /27 7 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt Source Classes in Fermi Source Classes in Fermi- -LAT Publications LAT Publications • Publications by Fermi-LAT members (Cat I+II+III, as of mid-Sep. 2011) (C t I II III f id S 2011) Well balanced # of papers: AGN~Galactic AGN~Galactic Diffuse~GRB~DMNP http://www-glast.stanford.edu/cgi-bin/pubpub /27 8 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt Source Classes in Fermi Source Classes in Fermi- -LAT Publications LAT Publications • Publications by Fermi-LAT members (C t I II III (Cat I+II+III, as of mid-Sep. 2011) f id S 2011) Well balanced covered by this talk # of papers: AGN~Galactic AGN~Galactic Diffuse~GRB~DMNP http://www-glast.stanford.edu/cgi-bin/pubpub /27 9 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt Diffuse Emission Seen by LAT Diffuse Emission Seen by LAT • Local diffuse emission is compatible with directly measured CRs directly measured CRs • “dark gas” is confirmed by F Fermi-LAT data i LAT d t • More CRs than expected in outer Galaxy outer Galaxy Abdo+10, ApJ 710, 133 Ackermann+11, ApJ 726, 81 • Freshly-accelerated CRs in Cygnus region Abdo+09, PRL 103, 251101 (CA: Johannesson, Porter, Strong ) /27 10 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt The Cygnus Region (MILAGRO) The Cygnus Region (MILAGRO) • Very rich region of massive-star formation at 1.4 kpc • Two sources + diffuse emission at TeV (MILAGRO) • Two sources + diffuse emission at TeV (MILAGRO) – correlation with matter density – diffuse flux exceeds the prediction by local CR MGRO J2031+41 EGRET MILAGRO MGRO J2019+37 Abdo+07, ApJL 658, 33 /27 Abdo+08, ApJ 688, 1078 11 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt The Cygnus Region (VERITAS) The Cygnus Region (VERITAS) • Very rich region of massive-star formation at 1.4 kpc • Cyg OB1 association seen by VERITAS • Cyg OB1 association seen by VERITAS – CTB87 resolved – plus complex region, likely powered by multiple sources (Good PSF is essential) (Good PSF is essential) VERITAS MGRO J2031+41 MGRO J2019+37 Aliu+11 (ICRC2011) Abdo+07, ApJL 658, 33 /27 Abdo+08, ApJ 688, 1078 12 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt The Cygnus Region (Fermi) The Cygnus Region (Fermi) • Very rich region of massive-star formation at 1.4 kpc • Detailed study by Fermi-LAT • Detailed study by Fermi-LAT – GeV diffuse (on average) consistent with local CR spectrum, despite the conspicuous star formation activity Total > 10 GeV MGRO J2031+41 (Gamma-ray Image) MGRO J2019+37 Preliminary e a y Ackermann+11 submitted Glon (deg) 85 80 75 /27 13 T. Mizuno et al. (CA: Tibaldo, Grenier)
Fermi_CTAmeeting_2011-09.ppt The Cygnus Region (Fermi) The Cygnus Region (Fermi) • Very rich region of massive-star formation at 1.4 kpc • Known sources and diffuse gammas subtracted • Known sources and diffuse gammas subtracted – Extended hard (>10 GeV) excess revealed in OB2 association – Spatial relation with infrared suggests the interstellar origin point sources, γ Cygni MGRO J2031+41 and diffuse emission removed (Gamma-ray Image) MGRO J2019+37 Preliminary e a y Glon (deg) 85 80 75 Ackermann+11 submitted /27 14 T. Mizuno et al. (CA: Tibaldo, Grenier)
Fermi_CTAmeeting_2011-09.ppt Energy Spectrum Energy Spectrum • CRs with local spectrum are too weak or too soft • Hard freshly accelerated CRs are required • Hard, freshly accelerated CRs are required – E -2.4 (hadron) or E -2.7 (lepton) – their origin and propagation to be studied by GeV/TeV obs. LAT γ -rays (10-100 GeV) Preliminary γ Cygni (Gamma-ray Spectrum) (G S t ) MILAGRO (Gamma-ray Image) H II x IC from IC from Local CR Local CR Cyg OB2 Preliminary /27 15 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt Starburst Galaxies Starburst Galaxies • High gas density and star-formation rate • Detected by H E S S (NGC 253) and VERITAS (M82) • Detected by H.E.S.S. (NGC 253) and VERITAS (M82) in TeV M82 (VERITAS) M82 (VERITAS) NGC253 (H E S S ) NGC253 (H.E.S.S.) Acciari+09, Nature 462, 770 Acero+09, Science 326, 1080 /27 16 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt Starburst Galaxies Starburst Galaxies • High gas density and star-formation rate • Detected by H E S S (NGC 253) and VERITAS (M82) • Detected by H.E.S.S. (NGC 253) and VERITAS (M82) in TeV • Hard spectrum by Fermi+IACT Γ =1.95 (Fermi best fit PL) Γ =2.2 Abdo+10, ApJL709, 152 /27 17 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt SB + Local Group Galaxies SB + Local Group Galaxies • LMC, SMC and M31 detected by Fermi-LAT • Correlation between SFR and L γ over wide range in • Correlation between SFR and L γ over wide range in galaxy properties. • L γ less correlated with gas mass. L γ ~ SFR α L SFR α =1.4+/-0.3 Abdo+10, A&A 523, L2 (CA: Bechtol, Knodlseder, Martin) /27 18 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt Recent Update Recent Update • A sample of 69 is examined: confirm the relation between star-formation rate and L γ SFR-L γ relation and hard spectrum implies hadron calorimetry • – NB MW is escape limited – need theoretical work and future obs. N1068 N4945 N4945 M82 N253 M3 M31 MW MW LMC SMC Preliminary Ackermann+11 submitted /27 (CA: Bechtol, Cillis, Funk, Torres) 19 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt Fermi GRBs as of 2011- Fermi GRBs as of 2011 -08 08- -01 01 • In 3 years ~0.6/day ~0 6/day – 682 GBM GRBs (345 in LAT FOV) 682 GBM GRBs (345 in LAT FOV) – 32 LAT GRBs (19 with >10 photons >100 MeV) ~0.6/month fewer than expected expected (Band+09) Preliminary /27 20 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt Summary of LAT GRBs Summary of LAT GRBs • aaa • 32 GRBs by LAT, 19 with >10 γ s above 100 MeV b 100 M V • Most of GRBs show delayed HE onset and HE afterglow nd HE ft l • Some bursts have an extra spectral ~30 30 component component Preliminary e a y /27 21 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt Common feature of GRBs Common feature of GRBs • Delayed HE onset and GRB 080916C (long) Abdo et al. 2009, Science 323, 1688 temporary extended emission are commonly seen • Some GRBs show extra spectral component (090510, 090902B, 090926A) LAT (>100MeV) GBM Delay in HE onset: 4-5 s • LAT Aeff ~ 0.8m 2 (<10 -4 of CTA Aeff) • Large Aeff is of great benefit to study extra component, extended emission and quantum Gravity. /27 22 T. Mizuno et al.
Fermi_CTAmeeting_2011-09.ppt Prospect of GRB with CTA Prospect of GRB with CTA • ~1 GRB/yr • Energy threshold is important • Energy threshold is important Bouvier+11 (ICRC2011) lower Eth and larger Aeff /27 23 T. Mizuno et al.
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