GRB_Fermi-WAM-Kanata_2009May.ppt 可視 X 線 γ 線同時観測で探 可視・ X 線・ 線・ γ 線同時観測で探 可視 可視・ 線同時観測で探 線同時観測で探 る γ 線バースト 線バースト (Exploring (Exploring GRBs through Optical, X GRBs through Optical, X- GRBs through Optical, X GRBs through Optical, X ray and Gamma- ray and Gamma -ray ray Observations) Observations) Tsunefumi Tsunefumi Mizuno Mizuno Hiroshima Univ Hiroshima Univ Hiroshima Univ. Hiroshima Univ. 7 May 2009, Tokyo Tech, Japan 7 May 2009, Tokyo Tech, Japan 1 Tsunefumi Mizuno
GRB_Fermi-WAM-Kanata_2009May.ppt Outline Outline • Fermi Gamma-ray Space Telescope � F � Fermi LAT and GBM i LAT d GBM � Burst Advocator • GRBs seen by Fermi � Overview � GRB080916C � GRB080916C � GRB081024B • Kanata Telescope for GRB 2 Tsunefumi Mizuno
GRB_Fermi-WAM-Kanata_2009May.ppt The Fermi Gamma The Fermi Gamma- -ray Space Telescope ray Space Telescope y y p p p p • Launch on 11 June 2008 Launch on 11 June 2008 • LAT (Large Area Telescope) � Energy range: 20 MeV-300 GeV � Effective Area: ~8000 cm 2 � Effective Area: 8000 cm � FOV: 2.4 sr (EGRET 0.5 sr) � Dead time: 26.5 μ s (EGRET 100 ms) • GBM (GLAST Burst Monitor) Consists of 12 NaI and 2 BGO detectors. � Energy range: 8 keV – 30 MeV � Energy range: 8 keV – 30 MeV � Field of view: 9.5 str � Initial localization: <15 deg in 2s Spectrum more than 7 energy decades !! 3 Tsunefumi Mizuno
GRB_Fermi-WAM-Kanata_2009May.ppt Burst Advocator Burst Advocator � Scientists serve as “Burst Advocator” and cover 24 hrs/day and 7 dyas/week � Japanese B/A consists of young members from 3 institutes; institutes; � Masanori Ohno, Rie Sato (ISAS/JAXA), � Yoshitaka Hanabata, Takeshi Uehara and Hiromitsu Takahashi (Hiroshima Univ ) Takahashi (Hiroshima Univ.), � Takeshi Nakamori, Takashi Shimokawabe (Tokyo Tech.) � Report on the LAT visibility and check the LAT data � Successfully issued GCN circular for GRB 090217 and GRB090323 which occurred during Japanese shift. 4 Tsunefumi Mizuno
GRB_Fermi-WAM-Kanata_2009May.ppt Fermi Detection of GRBs Fermi Detection of GRBs • GBM : GRB detection rate is ~200/yr. (08/11/2008 – 03/10/2009 116 GCN Circulars) 03/10/2009 116 GCN Circulars) • LAT : 7 GRBs detected until May 2009 and notified to GCN Circulars. Detection rate is ~10/yr. Circulars. Detection rate is 10/yr. GRB080825C (GCN8183, Bouvier et al.) GRB080916C* (GCN8246, Tajima et al.) (Abdo et al. 2009 Sci, 323, 1688) ( , j ) ( , , ) GRB081024B (GCN8407, Omodei et al.) (short GRB w/ GeV photons) GRB081215A (GCN8684, McEnery et al.) GRB090217 GRB090217 (GCN8903, Ohno et al.) (GCN8903 Ohno et al ) 2 LAT GRBs w/ WAM detection GRB090323* (GCN9021, Ohno et al.) GRB090328* (GCN9044, McEnery et al.; GCN9077, Cutini et al.) 4 GRBs w/ GeV photons 3 GRBs w/ redshift (*) 2 GRBs w/ GCN by Japanease BA 5 Tsunefumi Mizuno
GRB_Fermi-WAM-Kanata_2009May.ppt GRB080916C GRB080916C • z=4.35 +/- 0.15 8-260 keV (GROND; GCN8257) (GROND; GCN8257) • More than 3000 260 keV-5 MeV LAT photons 145 LAT photons, 145 above 100 MeV and 14 above 1 GeV. LAT (all) Eh=13.2 GeV >100 MeV • Delayed & Delayed & temporary extended (t>200s) HE >1 GeV emission emission 6 Tsunefumi Mizuno
GRB_Fermi-WAM-Kanata_2009May.ppt Implications from GR080916C Implications from GR080916C • Delayed & Extended HE emissions • Fitted by a single Band function. E iso ~ 8.3 x 10 54 ergs, highest ever observed. No conclusive evidence of extra component • Minimum bulk Lorentz factor 840 ±40 (from opacity in bin-’b’) • EBL effect not included • Lorentz invariance violation – 13.2 GeV @ T 0 +16.5 s – M QG > (1.5±0.2) x 10 18 GeV/c 2, 1/10 of the Plank mass GRB080916C Planck mass Pulsar Pulsar GRB GRB AGN AGN GRB GRB AGN AGN min M QG i M (Kaaret 99) (Ellis 06) (Biller 98) (Boggs 04) (Aharonian 08) (GeV) 10 15 10 16 10 17 10 18 10 19 7 Tsunefumi Mizuno
GRB_Fermi-WAM-Kanata_2009May.ppt GRB081024B GRB081024B • The first non-controversial NaI 8 – 260 keV short GRB w/ GeV photons • 11 photons above 100 MeV, Eh=3 GeV BGO • no redshift no redshift 260 keV – 5 MeV • Single Band function, delayed HE onset & delayed HE onset & LAT all events temporary extended HE emission (common feature among LAT GRBs?) among LAT GRBs?) LAT > 100 MeV • Γ min~100 (z=0.1), ~700 (z=3.0) (from opacity in bin- ”b”) -4 -2 0 2 4 6 8 10 8 Tsunefumi Mizuno
GRB_Fermi-WAM-Kanata_2009May.ppt HOWPol on Kanata Telescope HOWPol on Kanata Telescope (1) (1) (Hiroshima One-shot Wide-field Polarimeter) ( ) １露出型偏光撮像（広視野 7’×7’、狭 Filter exchanger Prism exchanger 視野 1’×15’） Focus adj. stage Focal mask Focal mask exchanger CCD dewer Collimator Shutter Camera lens Polarmetric lens and pupil unit exchanger • 2008 年 7 月 28-31 日 ファーストライト � 検出効率： B: 8%, V: 20%, R: 30%, I: 28% ( 望遠鏡、大気込み ) • 2008 年 11 月 4 日～ 定常試験観測開始 • 2008 年 11 月 4 日～ 定常試験観測開始 � 器械偏光 ~4% （第三鏡による偏光面回転のみの補正で 0.6% 精度 が達成） � 試験観測 超新星観測が主（ GRB アラート対応観測は TRISPEC で） � 試験観測、超新星観測が主（ GRB アラ ト対応観測は TRISPEC で） • 2009 年 5 月 3 日～ GRB アラート対応自動観測開始 9 Tsunefumi Mizuno
GRB_Fermi-WAM-Kanata_2009May.ppt HOWPol HOWPol on Kanata Telescope (2) on Kanata Telescope (2) • 2008 年度中は HOWPol での GRB 観測は間に合わず TRISPEC での GRB 観測は 9 例、うち 2 例で detected GRB t_start –t_end Satel. ⊿t comment -------------------------------------------------------------------- 080426 13:30:31-13:50:15 Swift, 428 s, Non-detection, shortburst 080506 080506 17:49:26-19:22:30 Swift, 185 s, R=17.5-19.3 (Uehara+ in prep) 17:49:26 19:22:30 S ift 185 R 17 5 19 3 (U h i ) 080810 13:16:23-19:39:17 Swift, 371 s, R=13.9-18.7 (Uehara+ in prep) 080905 12:01:32-12:58:06 Swift, 157 s, Non-detection 081012 13:16:17-14:06:13 Swift, 353 s, Non-detection 081211 15:22:22-15:40:37 Swift, 3.6 hr, Non-detection 081211 15:22:22 15:40:37 S ift 3 6 h N d t ti 081211B 15:47:29-15:49:02 Swift, 14.5 hr, Non-detection 081222 13:09:15-13:21:14 Swift, 8.3 hr, Non-detection 090217 14:20:13-16:00:17 Fermi, 9.4 hr, Cloudy, non-detection 090404 16:02:44-16:21:13 Swift, 374 s, Cloudy, non-detection 090410 18:48:50-19:01:18 Swift, 1.8 hr, Low-altitude, non-detection 090417B 15:31:49-15:38:18 Swift, 706 s, Non-detection 090418 12:35:35-12:38:19 Swift, 1.5 hr, Cloudy, non-detection 090418 12:35:35 12:38:19 Swift 1 5 hr Cloudy non detection 090426 12:54:09-13:28:22 Swift, 322 s, non-detection z=2.609 ⊿t は衛星のトリガーから露出開始（t_start）までの経過時間 10 Tsunefumi Mizuno
GRB_Fermi-WAM-Kanata_2009May.ppt HOWPol HOWPol on Kanata Telescope (3) on Kanata Telescope (3) GRB 080506 ： X 線フレアと相関し GRB 080810 ：ゆっくりと青くなっ ない可視残光 ていく可視残光 Ｘ線 Ｘ線 可視・近赤外 外 緑 可視Ｖ 青 近赤Ｊ 水 近赤Ｋｓ • 2009 年 5 月 3 日から GRB 対応観測（但し狭視野モード用のウォラ ストンプリズムを視野マスク無しで使用するため背景スカイが 4 ト プリズムを視野 ク無し 使用するため背景 カイが 倍高くなり観測限界は悪い） • 2009-2010 年度 公募研究「明るいガンマ線バースト初期残光の 年度 募研究 明 線 初期 光 偏光分光測光同時モニター」にて広視野モード用のウォラスト ンプリズムを導入予定 ( 川端の講演 ) 11 Tsunefumi Mizuno
GRB_Fermi-WAM-Kanata_2009May.ppt Summary Summary • Fermi GBM detects ~0.5GRB/day and LAT ~10 GRBs/year • 7 LAT GRBs above 100 MeV � 4 GRB � 4 GRBs w/ GeV photons, one short (GRB081024B) / G V h t h t (GRB081024B) � 2 GRBs w/ WAM detection, 3 w/ redshift • GRB080916C w/ maximum E iso ever observed • GRB080916C w/ maximum E ever observed � 14 photons > GeV, Γ min >=900, M QG >1.3x10 18 GeV/c 2 • GRB081024B is the first short GRB with photons above 1 GeV. GRB081024B is the first short GRB with photons above 1 GeV. � Γ min =100 (for z=0.1) and 700 (for z=3.0) � Single Band function, delayed HE onset and extended HE emission => common feature? • HOWPol on Kanata Telescope is now ready (on May 3, 2009) � 9 GRBs observed, 2 GRBs detected in 2008/4-2009/3 by TRISPEC 12 Tsunefumi Mizuno
GRB_Fermi-WAM-Kanata_2009May.ppt B Backup Slides k Slid 13 Tsunefumi Mizuno
GRB_Fermi-WAM-Kanata_2009May.ppt Spectral Analysis Spectral Analysis Spectrum at T0+0.1 – T0+0.8s GBM 2 nd pulse (including maximum energy photon of i h t f 3.0 GeV) can be fitted by a Band Function. α = -0.9053 ± 0.203 β = -1.993 ± 0.0768 β Ep = 819.2 ± 547.0 keV No strong evidence of additional high energy component. g gy p 10 10 3 10 4 10 5 10 2 10 6 ( keV) (1MeV) (1GeV) 14 Tsunefumi Mizuno
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