The Fermi Zoo : GRB prompt spectra. Michael S. Briggs (Univ. Alabama in Huntsville) for the Fermi GBM & LAT Teams
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1 The Fermi Zoo : GRB prompt spectra Michael S. Briggs (Univ. Alabama in Huntsville) for the Fermi GBM & LAT Teams Multi-Messenger Workshop KIAA
2 Multi-Messenger Workshop KIAA
3 Before Fermi: CGRO and the Band Spectrum 3 Flux (photons cm 2 s 1 MeV 1 ) BATSE SD0 BATSE SD1 BATSE LAD0 BATSE SD4 OSSE COMPTEL Telescope COMPTEL Burst Mode EGRET TASC GRB E 2 N E (erg cm 2 s 1 ) Photon Energy (MeV) Band et al. 1993; Briggs et al Multi-Messenger Workshop KIAA
4 GRB 9417 Two CGRO instruments: BATSE Large Area Detectors (LADs) and EGRET Total Absorption Shower Counter (TASC) Gonzalez et al GRB GeV photon 90 minutes after the trigger. (Hurley et al. 1994) Multi-Messenger Workshop KIAA
5 Fermi: The Band Function continues? GRB C (Similar: C, A, ) Abdo et al., Science, 2009 Multi-Messenger Workshop KIAA
6 Delayed High-Energy Emission GRB 0905 GRB C Figure 2. AGILE: Giuliani et al., ApJL, 20; Fermi: Ackermann et al., ApJ, 20 Abdo et al., Science, 2009 A general feature: LAT GRB catalog: Ackermann et al 2013 Multi-Messenger Workshop KIAA
7 GRB B: a power-law component 2 Rate (counts s 1 kev 1 ) NaI 0 NaI 1 NaI 2 NaI 9 NaI BGO 0 BGO 1 LAT front LAT back /s) 2 (erg/cm νf ν Sigma Energy (kev) Energy (kev) re 3. Joint fit of GBM and LAT data to interval b,( s).Top 5 Abdo et al., ApJ, 706 (2009); Zhang et al. (2011) 6 7 Multi-Messenger Workshop KIAA
8 GRB A: a power-law with a break 5 /s) 2 νf ν (erg/cm 6 a c d 7 [a]: 0.0 s 3.3 s (Band) [b]: 3.3 s 9.7 s (Band) b [c]: 9.7 s.5 s (Band + CUTPL) [d]:.5 s 21.6 s (Band + PL) Energy (kev) Ackermann et al. ApJ, 729 (2011) Multi-Messenger Workshop KIAA
9 Short GRBs GBM has high sensitivity to short GRBs. t 90 distribution from the first GBM GRB catalog. (Paciesas et al. 2012) Short GRBs are very similar to long GRBs. except: higher Epeak values: Time-integrated Epeak > 2 MeV (Guiriec et al. 20, also Catalog/) Shorter minimum variability timescales (MacLachlan et al. 2013) Multi-Messenger Workshop KIAA
10 GRB 0724B: adding a thermal component to the Band model Δcstat = 95 for 2 dof. Epeak: 352 kev 615 kev α: β: Softer values of αare obtained, which may remove inconsistency with the synchrotron limit. (Ryde & Pe er (2009), Guiriec et al. (2011)). Guiriec et al.(2011) Fig. 2. The time-integrated spectrum of GRB 0724B fitbyabandfunction(toptwopanels)andaband+blackbodyfunction (bottom bottom two panels). The left plots show the count spectra for the two models and the right plots the corresponding deconvolved νf ν spectra. The data points appear as color crosses. Dashed lines indicate the individual spectral functions and solid lines shows the summed model fit. The addition of a BB spectral component over the brightest part of the burst (T s to T s) shows a significant improvement in the fit compared to a Band function by itself, particularly noticeable as the removal of trends with energy in the residuals compared to the Band-only fit. The region between 30 and 40 kev is excluded from the fit owing to calibration issues around the k-edge of the NaI detectors. We have verified this exclusion doesn t affect the recovered parameter values. Multi-Messenger Workshop KIAA 2013
11 What is the nature of the component traditionally fit with the empirical Band function? Multi-Messenger Workshop KIAA
12 Fitting with more physical models: thermal and non-thermal synchrotron & BB Thermal Synchrotron Blackbody Power-Law Synchrotron Blackbody Power-Law Synchrotron Power-Law Synchrotron Blackbody Figure 4. The time-resolved spectra for GRB A. The spectra represent bin a with thermal synchrotron only (top left panel), bin b with power-law synchrotron + blackbody (top right panel), bin c again with power-law synchrotron + blackbody (bottom left panel), and finally bin d with thermal synchrotron + blackbody (bottom right panel). As with Fig. 2, the multiple curves are associated with the e ective area correction. Burgess et al., 2011, 2013 Multi-Messenger Workshop KIAA
13 Or is the emission photospheric instead of synchrotron, at least in some cases? Times: s νf ν [kev cm -2 s -1 ] NaI-0 NaI-1 BGO-0 BGO-1 LAT Back LAT Front Spectral evolution and a multi-color blackbody plus PL model. Ryde et al. (20) Energy [kev] = Multi-Messenger Workshop KIAA
14 ~10 GBM GRBs are within the LAT FoV, of which 35 are detected by the LAT. There is no mystery about which are detected: they are the highest fluence. Of the brightest 30 not detected in the LAT, extrapolations of GBM Band fits predict half should be detected. Why are they not detected? Joint fits give steeper β values: A break improves the fit for a few γγ opacity? The Band model may be inappropriate (see GRB 0724B). Guetta, Piran & Waxman (2011); Beniamini et al. (2011); Ackermann et al., (2012): arxiv: v1 Multi-Messenger Workshop KIAA
15 What does it mean? Delayed HE emission: decreasing opacity or improving particle acceleration? Leptonic models: explain the delayed HE emission via two zones producing photons. (Toma et al., 2009 & 2011) The high-energy component can be explained as synchrontron self-compton (SSC), but what about the related emission below 50 kev? Hadronic models: the delayed HE emission is easy to explain as the time to accelerate the hadrons. But requires very large energy. (Razzaque et al. 2009; Asano et al. 2009) Magnetically-dominated models to explain the dominance of the Band component? (Zhang & Pe er 2009; Zhang et al. 2011) Multi-Messenger Workshop KIAA
16 New almost future LAT Low-Energy Events (LLE) GBM continuous Time-Tagged Events GBM GRB localizations: faster better characterized: core and extended error model: preliminary: 88% of probability with σ sys = 3.6, 12% withσ sys =13.9 Multi-Messenger Workshop KIAA
17 The Future GRB A was observed by Swift and GBM. GBM has the largest field-ofview a future important GRB may only be observed in gamma-rays by GBM. A counterpart of VHE gammas? (e.g., CTA talk by V. Connaughton on Thursday) A Multi-messenger counterpart?: neutrinos (IceCube) or gravitational waves (ALIGO/Virgo)? t 90 = 138 ± 3 s t 50 = 4.1 ± 1.4 s 1 s peak flux: 52 ± 2 γs -1 cm -2 Shaolin Xiong Multi-Messenger Workshop KIAA
18 The Future What we are doing: Working to improve localization accuracy and speed (V. Connaughton) Search continuous TTE for weaker (sub-trigger threshold) short GRBs. What you could do: wide field-of-view, fast-slewing telescopes to use GBM localizations*, use GBM and LAT data. * done for GRB with a BATSE location (Akerlof et al. 1999) & GRB B with a GBM location (Pandey et al. 20). Multi-Messenger Workshop KIAA
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