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Gamma-ray bursts in the era of multi-messenger astronomy Zsolt Bagoly ELTE, Dept. of Physics for Complex Systems ELFT Summer School18 2018-09-05 ELFT Summer School18 Gamma-ray bursts in the era of multi-messenger astronomy 1 / 101

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Gamma-ray bursts in the era of multi-messenger astronomy

Zsolt Bagoly

ELTE, Dept. of Physics for Complex Systems ELFT Summer School’18

2018-09-05

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 1 / 101

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Collaborators Bagoly Zsolt, Csabai István, Dobos László, Rácz István, Kóbori József, Szécsi Dorottya ELTE KRFT, Balázs Lajos, Tóth L. Viktor, Zahorecz Sarolta, Pintér Sándor ELTE CsTsz./CSFKI KTM, Lichtenberger János ELTE Geofizikai Tsz. Horváth István NKE HHK Tusnády Gábor MTA Rényi Intézet Mészáros Attila, Jakub ˇ Ripa Károly Egyetem, Mészáros Péter Penn State University, Veres Péter NASA Huntsville, Jon Hakkila Charleston College, Yasuo Doi Univ. of Tokyo, Maria Cunningham, Paul Jones UNSW, OTKA F029461, OTKA T034549, OTKA T048870, OTKA T077795, OTKA/NKTH A08-77719 és A08-77815, OTKA NN111016, OTKA NN114560 GAUK 46307, MSM0021620860, P209/10/0734, CRGJ13/98:113200004, GA ˇ CR grant 202/98/0522 NASA NAG5-2857, NASA NAG5-9192, NASA EPSCoR NNX13AD28A

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GRBs

Since 1972 (publication): Vela satellites Properties short (10ms - 100s) gamma flashes

  • Max. fluence 105 keV/cm2

Unique lightcurves Meegan’s first rule: if you observe it, it should exists!

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BATSE lightcurves

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Fermi lightcurves

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 5 / 101

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Energetics

Prompt phase 65% gamma (keV-MeV) 10% gamma (GeV) 7% X-rays radio, optical < 1% Afterglows 7% gamma (keV-MeV) 9% X-rays

  • ptical 2%

radio 0.05% E ≈ 1054(Ω/4π)erg ≈ MNapc2 !

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Satellites

VELA, SMM, Ginga, BATSE, Ulysses, BeppoSAX, Integral, Swift, Fermi ... Gamma detectors (NaI, CsI, etc.): many e−p big mass! International Planetary Network (triangulation) Ballons (yesterday)

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 7 / 101

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BATSE (1991-2000)

On the Compton Observatory 2704 GRB > deg directions Isotropic (?) distribution → extragalactic origin 2-3 groups of GRB no repetition, no afterglow ≈ few GRB/day in our Universe

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 8 / 101

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BeppoSAX

A mission of the Italian Space Agency (ASI) with contribution of NIVR (Netherlands). Launched in April 1996, ended in April 2002 Low Equatorial Orbit: 3.9 inclination, 600 km altitude Wide Field Camera 2-28 keV

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BeppoSAX afterglows

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Neil Gehrels Swift Observatory (2004-)

Penn State University - NASA Rapid response Autonomous operation Several instruments UVOT / XRT / BAT BAT FoV 2 sr (16% of the sky) coded mask 100 GRB/yr X-ray followups

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Coded Mask Telescope

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(GLAST)-Fermi (2008-)

  • kb. 250 GRB/év

10keV - GeV tartomány! GBM: NaI, BGO detektorok LAT: ≈ 10 MeV felett automatikus forgás: ráfordul a forrásra + teljes égletapogatás 3 óránként

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Fermi detectors

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Fermi GeV sky

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Fermi GeV sky

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Afterglows

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Naked eye afterglow

Robotic telescopes with a few sec response time

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Long GRBs’ afterglows

Irregular galaxies

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Short GRBs’ afterglows

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GRB positions in the host galaxy

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GRB redshifts

Today maximum is zmax = 8.26 !

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GRBs are following the star formation rate (?)

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Gamma, X-ray and optical afterglow

You van connect the gamma and the X-ray part of the afterglow ! (Veres 2011)

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Local environment: NH from the X-ray spectra

X-ray afterglow Beppo-Sax: NH changes during the burst (Amati+03)! Swift: NH foreground is a problem!

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Galactic NH foreground

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Energetics

Full GRB spectra

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Testing the Quantum Gravity

Lorentz invariance: c is constant! What if we can measure? GRB080916C z = 4.35 FERMI LAT: 13.2 GeV photon observed! E > 100 MeV photons delayed (≈ 5 sec regarding the E < 1 MeV photons)

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 29 / 101

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Testing the Quantum Gravity

GRB080916C FERMI LAT E > 100 MeV photons delayed (≈ 5 sec regarding the E < 1 MeV photons) MQG > 1.3x1018GeV/c2,

  • kb. 10% MPlanck

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Models

fireball model internal and external shockwaves with magnetic field extreme relativistic (99.999c) barion-poor jet

m1 ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 31 / 101

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Sources

Long GRBs: collapsar model High mass Wolf-Rayet star collapse

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Collapsar

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Collapsar jet

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Short (Intermdiate?) GRB Progenitor Models

Compact binary mergers (NS-NS or NS-BH or BH-BH) Wide age distribution Star-forming and dead galaxies Star-forming galaxies (delay?)

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Merging neutron stars

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Jet structure and view angle effects

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Jet angle sizes

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Groups of GRBs

Parameters Event length: T90 is the time between 5% and 95% of the cumulated counts SEmin,Emax energy (fluence) e.g. for the Swift BAT the chanels are 15 − 25 − 50 − 100 − 150 keV Hij: hardness H32 = S50−100keV

S25−50keV

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How many kinds of GRBs do we have?

BATSE early data homogenous data: long and short bimodality confirmed Later > 6 years’ data + other satellites (BeppoSAX, Swift): Horvath, Mukherjee+, Horvath+, Tarnopolski, Ripa ... several groups/many papers

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BATSE groups

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Intermediate GRB group

Swift groups and the XRFs: Veres+10 Questions: diffrence in jet structure/engine/physical parameters

  • r selection effects /whole phenomena?

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GRBs and the SGR 1900+14

Woods & Thompson, (2004)

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SN-Kilonova-GRB unified view

Margutti+12

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GRBs’ Sky Distribution

Distant objects: excellent (!?) for mapping the Universe! Many problems: sky exposure, systematics, theory vs. observation. BATSE GRBs’ Sky Distribution

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Fermi GRBs’ Sky Distribution

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BATSE Groups Sky Distribution

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BATSE Groups Sky Distribution

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Galactic distribution of 404 GRBs with measured z

The disk of the Galaxy hinders the optical follow-up. There’s no significant difference between Northern and Southern Galactic hemispheres’ z distribution. The two-sample Kolmogorov-Smirnov test gives 0.1155 for the p-value.

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3D: radial z distribution from the data

GRBs are following the star formation rate (?)

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Large Gamma-ray Burst Cluster at 1.6 z < 2.1

Horvath+15 applied angular test on the 8 z/distance groups, and we applied k-th nearest neighbour analysis and the bootstrap point radius method on the dataset. Nearest-neighbour tests identify pairing consistent the large, loose GRB cluster in the redshift range 1.6 < z 2.1. The scale on which the clustering occurs is disturbingly large, about 2-3 Gpc: the underlying distribution of matter suggested by this cluster is big enough to question standard assumptions about Universal homogeneity and isotropy.

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Large Gamma-ray Burst Cluster at 1.6 z < 2.1

360 300 240 180 120 60 + 90 + 60 + 30

  • 90
  • 60
  • 30

1.6< z< 2.1

The distribution of GRBs in the redshift range 1.6 < z 2.1. The cluster direction is approx l = 88o, b = 63o.

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 52 / 101

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The Sky Exposure Function of the GRBs

Reconstructed empirical Sky Exposure Function of the 404 GRBs with

  • distance. In normalized units, optimal Gaussian smoothing applied.

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A ring-like structure at 0.78 < z < 0.86 displayed by GRBs

Balázs+16 motivated by the Large Gamma-ray Burst Cluster, analyzed the k-th nearest neighbour in the sample further. Instead of the slices in the redshift space the k-th Next Neighbor Statistics was used to determine the spatial density of the GRBs. The values of k = 8, 10, 12, 14 were used to calculate the mean and variance of the local density at every GRB location.

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k-th nearest neighbour χ2

k values

2000 4000 6000 8000 10 20 30 40

distance (Mpc) chisquare df=8

95.0% 99.0% 99.9% 2000 4000 6000 8000 10 20 30 40

distance (Mpc) chisquare df=10

95.0% 99.0% 99.9% 2000 4000 6000 8000 10 20 30 40

distance (Mpc) chisquare df=12

95.0% 99.0% 99.9% 2000 4000 6000 8000 10 20 30 40

distance (Mpc) chisquare df=14

95.0% 99.0% 99.9%

For k = 8, 10, 12, 14 degrees of freedom, 1000 resamplings.

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A Ring-like structure at 0.78 < z < 0.86

Angular distribution of GRBs in galactic coordinates for k = 12.

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A Ring-like structure at 0.78 < z < 0.86

Ring with a diameter of 1720 Mpc, displayed by 9 gamma ray bursts (GRBs) Exceeding by a factor of five the transition scale to the homogeneous and isotropic distribution Major diameter of 43o, minor diameter of 30o Distance of 2770 Mpc in the 0.78 < z < 0.86 redshift range Probability of 2 × 10−6 of being the result of a random fluctuation in the GRB count rate. This ring-shaped feature is large enough to contradict the cosmological principle. The physical mechanism responsible for causing it is unknown.

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A Ring-like structure at 0.78 < z < 0.86

The Ring can be a projection of a spheroidal structure, if each host galaxy has a period of 2.5 × 108 years during which the GRB rate is enhanced.

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A Ring-like structure at 0.78 < z < 0.86

Is there any other ring?

  • ●
  • ●
  • ●
  • ●
  • ●
  • ●
  • 0.1

0.2 0.3 0.4 0.5 5 10 15

R (ring area) Concentration level

  • Ring area versus concentration level

GRB ring

  • ●
  • Ring area versus concentration level

GRB ring

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The Sky Exposure Function of the GRBs

Reconstructed empirical Sky Exposure Function of the 404 GRBs with

  • distance. In normalized units, optimal Gaussian smoothing applied.

Mirrored!

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The spatial two-point correlation function of GRBs

2 4 6 8 500 1000 1500 2000 2500 3000 3500 4000 Spatial Two-point Correlation function (normalized) comoving distance (Mpc) GRB dataset MC simulations with 3σ errors

  • 2

2 4 6 8 10 12 50 100 150 200 250 300 350 400 450 500 550 600 650 700 750 800 850 900 950 1000 MC simulations with 3σ errors

The spatial two-point correlation function for GRBs. Two GRBs, at a distance of ≈ 56 Mpc GRB RA(deg) Dec(deg) l(deg) b (deg) z GRB020819B 351.8310 6.2655 88.4946

  • 50.8949

0.410 GRB050803 350.6577 5.7857 86.5225

  • 50.6999

0.422

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Gravitational waves I.

GW150914 Triggered on 14/09/2015 09:50:45.391 UTC., z = 0.093(+0.030/0.036).

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Gravitational waves II.

LVT151012 Triggered on 02/10/2015 09:54:43.44 UTC, z = 0.20(+0.09/ − 0.09).

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Electromagnetic transients related to the GW events

GW150914: Fermi counterpart (Connaughton+16) Inspired ADWO

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GW150914 Fermi EM counterpart

Energy spectra (Connaughton+16)

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GW150914 Fermi NaI sums: Connaughton+16

800 900 1000

4.4-12keV

3600 3800 4000 4200 4400

12-27keV

2200 2400 2600 2800

27-50keV

1600 1700 1800 1900 2000 2100

50-100keV

1400 1500 1600 1700 1800

100-290keV

400 500

290-540keV 10 5 5 10

500 600

540-980keV 10 5 5 10

400 500 600

980-2000keV Seconds from GW T0 Counts per Second

  • Fig. 5.— De

te cte d count rate s summe d ove r NaI de te ctors in 8 e ne rgy channe ls, as a function of time re lative to the start of the GW e ve nt GW150914. Shading highlights the inte rval containing GW150914-GBM. Timebinsare1.024sin duration, with the0.256sCTIME lightcurveove rplotte d in gre e n, and the re d line indicate s the background le ve l.

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GW150914 Fermi BGO sums: Connaughton+16

700 800 900 1000

0.11-0.42MeV

600 700 800 0.42-0.95MeV 700 800 900

0.95-2.1MeV

300 400

2.1-4.7MeV

50 100

4.7-9.9MeV

50

9.9-22MeV 10 5 5 10

50

22-38MeV 10 5 5 10

100 200

38-50MeV Seconds from GW T0 Counts per Second

  • Fig. 6.— De

te cte d count rate s summe d ove r BGO de te ctors in 8 e ne rgy channe ls, as a function of time re lative to the start of the GW e ve nt GW150914. Shading highlights the inte rval containing GW150914-GBM. Timebinsare1.024sin duration, with the0.256sCTIME lightcurveove rplotte d in gre e n, and the re d line indicate s the background le ve l.

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GW150914 Fermi EM counterpart

Sky position (Connaughton+16)

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GW150914 observations

Swift (Evans+16) No prompt signal, > 50 hours later Auger (Aab+17) No signal Integral SPI ACS (Savchenko+16, (+previus talks)

66000 68000 70000 72000 74000 76000

  • 10
  • 5

5 10 seconds since LVC trigger, UTC 2015-09-14T09:50:45.39 50 ms 250 ms background

No signal.

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GW150914 Fermi re-analysis

Greiner+16: No signal in the Fermi data Simply sum the data from the 14 detectors for energy spectrum! Rhessi BGO data + ADWO: no signal (Ripa+17)

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Fermi GBM detectors

12 NaI(Tl): 8 keV-∼ 1 MeV, 2 BGO: ∼ 200 keV-∼ 40 MeV 128 energy channels, 2µs time resolution Continous Time Tagged Events (CTTE) since 26/11/2012. Effective area depends on the energy and direction Detector Response Matrix (DRM) transforms the spectrum into counts. Multiple triggers: # of triggered detectors, thresholds (4.5 − 7.5σ) and energy range (25, 50, 100, > 300 keV): ≈ 75 active from the 120.

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Automatized Detector Weight Optimization (ADWO)

The approximate trigger time is known: one signal from many detectors and energy channels. Usually: background modell + spectral signal with DRM, fitted with the binned data. But: we do NOT know the direction/DRM! Naïve solution: sum the data. Simple but NOISY! Optimal summing Only the strong signals/detectors/channels should be added. Which

  • nes are important?

Non-negative weights: ei for the energy and dj for the detectors ( ei = 1, dj = 1).

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SLIDE 73

Signal’s Peak to Background’s Peak Ratio

Let Cij(t) be a background substracted intensity. The composite signal is: S(t) =

  • i,j

eidjCij(t) S(t): the maximum of the signal within the search interval B(t): the maximum outside the interval. Maximize S(t)/B(t), the Signal’s Peak to Background’s Peak Ratio (SPBPR). Nonlinear optimalization. Matlab/Octave code, using fminsearch, (GitHub https://github.com/zbagoly/ADWO).

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SLIDE 74

Analysis of the Fermi data

Energy channels e1 . . . e8: 8 CTIME energy channels (128 CTTE channels summed up) According to Connaughton+16, the limits are 4.4, 12, 27, 50, 100, 290, 540, 980 and 2000 keV Low energy channels are quite noisy → Only the 27-2000 keV range (e3 . . . e8) are taken No BGO data for e3 − e4: 6 × 14 − 2 × 2 = 80 time series. CTTE Filtering Average ≈ 5.8 ms between photons in channels (at GW150914) Smoothing with a 64ms sliding window, 11.2 photons in the window. (Q: What is the optimal kernel for an inhomogenous Poisson process?) Total window: ≈ (−200, 500) s around the event, approx. 1/7 orbit.

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SLIDE 75

Fermi background fit

Szécsi+13: sky sources + geometry + directions with pseudoinverse E.g: GRB091030613 background:

800 900 1000 1100 1200 1300 1400 1500

  • 1000 -800 -600 -400 -200

200 400 600 800 1000 counts/sec time chi2 = 0.973

Here: short signals only → 6th order polynome background (like Connaughton+16).

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SLIDE 76

GW150914: ADWO

(−195, 495)s window around 14/09/2015 09:50:45 UTC. ADWO: maximum is SPBPR=1.911, 474 ms after the GW trigger (no time constraint for ADWO!).

  • 0.5

0.5 1 1.5 2 2.5

  • 3
  • 2
  • 1

1 2 3 Signal Peak to Background Peak Ratio seconds since 14/09/2015 09:50:45.391 UTC

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SLIDE 77

GW150914 Fermi EM counterpart

Connaughton+16:

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SLIDE 78

GW150914: ADWO significance

104 Monte-Carlo (MC) simulation, 86 cases with SPBPR> 1.911. 0.0014 Hz rate of the error The probability is 2.8 × 10−3 Hz × 0.474 s × (1 + ln(6 s/64 ms)) = 0.0075. (Connaughton+16: 0.0022) Rhessi BGO data + ADWO: no signal (Ripa+17)

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 78 / 101

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SLIDE 79

LVT151012: ADWO

(−195, 495)s window around 02/10/2015 09:54:43.44 UTC ADWO: maximum is SPBPR=1.805, 652 ms later.

  • 0.5

0.5 1 1.5 2 2.5

  • 3
  • 2
  • 1

1 2 3 Signal Peak to Background Peak Ratio seconds since 12/10/2015 09:54:43.555 UTC ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 79 / 101

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SLIDE 80

LVT151012

ADWO significance 104 Monte-Ca/lo (MC) simulations, 308 cases with SPBPR> 1.805. Error rate is 0.0051 Hz. The probability is 0.01 Hz × 0.652 s × (1 + ln(6 s/64 ms)) = 0.037. No lighning/TGF. Fermi group (Racusin+16) No signal was detected

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 80 / 101

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SLIDE 81

GW150914: investigation of the daily background

Fermi: no signal 61.4 ks CTTE data, same day, no re-pointing, 6s window.

0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1 1 2 3 4 5 6 softness (e3+e4+e5) Signal Peak to Background Peak Ratio GW150914 LVT151012 GRB150522B

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 81 / 101

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SLIDE 82

GW121226; ADWO

Triggered on 26/12/2015 03:38:53.647 UTC. ADWO: maximum is SPBPR=1.321, probably noise.

  • 0.02
  • 0.01

0.01 0.02 0.03 0.04

  • 30
  • 20
  • 10

10 20 30 40 50 60 ADWO lightcurve seconds since GW121226

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SLIDE 83

GW121226; ADWO

Triggered on 26/12/2015 03:38:53.647 UTC. ADWO: maximum is SPBPR=1.321, probably noise.

  • 0.8
  • 0.6
  • 0.4
  • 0.2

0.2 0.4 0.6 0.8 1 1.2 1.4

  • 3
  • 2
  • 1

1 2 3 Signal Peak to Background Peak Ratio Seconds since 26/12/2015 03:38:53.647 UTC

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 82 / 101

slide-84
SLIDE 84

GW121226

Fermi group (Racusin+16) No signal detected Auger (Aab+17) No signal

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 83 / 101

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SLIDE 85

GW170104: Fermi (Burns+17,Fermi collaboration+17)

Good GBM exposure (≈ 82.4%) : GBM upper limit: (5.2 − 9.4) × 10−7erg cm−2s−1 (10-1000 keV) LAT upper limit: (0.2 − 13) × 10−9erg cm−2s−1 (0.1-1 GeV) GBM most significant candidate: 5.4 s before the T0, false alarm rate

  • f ≈ 0.003 Hz.

Longer term structure for tens of seconds in the low energy channels around T0.

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 84 / 101

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SLIDE 86

GW170104 EM observations: AGILE (Verrecchia+17)

Good exposure (≈ 36%) around T0: SA detector No gamma-ray transient near T0 over timescales of 2, 20 and 200 seconds. Upper limit: (1.5 − 6.6) × 10−8erg cm−2 (depending on the direction)

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 85 / 101

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SLIDE 87

GW170104 EM observations: AGILE MCAL detector

3 short timescale events/features E2: strongest at T = −0.46s, above 1.4 MeV E2 event’s post-trial probability is 3.4σ If real, total energy is 10−7 smaller than the total black hole rest mass!

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 86 / 101

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SLIDE 88

GW170104: ADWO

GBM data: (−200, 140)s interval around 04/01/2017 10:11:58.599 UTC. ADWO: maximum is SPBPR=1.51, at T ≈ −50ms, in the noise. AstroSat-CZTI and GROWTH (Bhalerao+17) CZTI upper limit: ≈ 4.5 × 10−7erg cm−2s−1 for a 1 s timescale

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 87 / 101

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SLIDE 89

Fast Radio Bursts (preliminary)

FRB121102 repeating source, Chatterjee+17 8 ADWO period, good seeing, multiple SPBPR,

  • Max. SPBPR=≈ 1.81, at the limit, probably noise.

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 88 / 101

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SLIDE 90

GW170814: ADWO

GBM data: (−50, 250)s interval (particle event at ≈ −50s) ADWO: maximum is SPBPR=1.28, in the noise.

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 89 / 101

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SLIDE 91

GW170817A: ADWO

GBM data: (−100, 100)s interval (SAA entry) ADWO: maximum is SPBPR=2.6902, strong signal!

  • 1
  • 0.5

0.5 1 1.5 2 2.5 3

  • 10
  • 5

5 10 SPBPR t (since GRB170817A trigger)

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 90 / 101

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SLIDE 92

GW170817A

Fermi (Goldstein, Veres +17)

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 91 / 101

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SLIDE 93

GRB groups and the GRB170817A/GW170817

  • 1

1 2 3

  • 1.0
  • 0.8
  • 0.6
  • 0.4
  • 0.2

0.0 0.2 0.4 0.6 0.8 1.0

short intermediate long GRB 170817A lg Spectral Hardness lg T90

GRB170817A/GW170817 in the intermediate group!

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 92 / 101

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SLIDE 94

ADWO Summary

Efficient method looking for transients (GRB, GW, FRB, IceCUBE (no counterparts), . . .) Method impovements

  • ptimal smoothing filter/kernel
  • ptimalized energy channels, DRM constraints

direction determination (huge errors?) multi-messenger data Other transients (s)GRBs, non-triggered (s)GRBs, non-triggered GW

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 93 / 101

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SLIDE 95

ADWO efficiency

0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1 1 2 3 4 5 6 softness (e3+e4+e5) Signal Peak to Background Peak Ratio GW150914 GRB160301788 GRB150921153 LVT151012 GW170104 GW121226 GRB150522B GW170814 GRB170817A

Red: 61.4 ks good CTTE data (14/09/2015) („background”?!) Blue: Fermi’s (s)GRB triggers, T90<15s

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 94 / 101

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SLIDE 96

Fermi (s)GRB Supergalactic Distribution

Short (T90<5s) GRBs with ADWO hard (SR<0.4) peak spectrum, no measured redshift

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 95 / 101

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SLIDE 97

Future Missions: SVOM

Cordier+18

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 96 / 101

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SLIDE 98

Future Missions: Theseus

ESA M5 proposal ≈ 2028, 400M EUR budget IR, X-ray and gamma detectors high-z magas events (optical + HE)

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 97 / 101

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SLIDE 99

Theseus Star Formation Rate

Amati+18

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 98 / 101

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SLIDE 100

Theseus Redshifts

Amati+18

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 99 / 101

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SLIDE 101

Untriggered GRB 478557956

Fermi CTIME quicklook

150. 175. 200. 225. 250. 275. 300. 325. 350. counts per bin N0 50 to 538 keV sGRB ver 95a of 2016 Oct 14 run on 2016-10-15 12:49:58 T0 = 478557956.424000 = 2016-03-01 20:45:52.424000 Algr: 2: P01 of F0013: glg_tte_b0_160301788_v00 150. 175. 200. 225. 250. 275. 300. 325. 350. counts per bin N1 50 to 537 keV 150. 175. 200. 225. 250. 275. 300. 325. 350. counts per bin N2 51 to 538 keV

  • 10
  • 5

5 10 0.704 s bins. T0 = MET 478557956.424000 150. 175. 200. 225. 250. 275. 300. 325. 350. counts per bin N3 50 to 539 keV 150. 175. 200. 225. 250. 275. 300. 325. 350. counts per bin N0 50 to 538 keV sGRB ver 95a of 2016 Oct 14 run on 2016-10-15 12:49:58 T0 = 478557956.424000 = 2016-03-01 20:45:52.424000 Algr: 2: P01 of F0013: glg_tte_b0_160301788_v00 150. 175. 200. 225. 250. 275. 300. 325. 350. counts per bin N1 50 to 537 keV 150. 175. 200. 225. 250. 275. 300. 325. 350. counts per bin N2 51 to 538 keV

  • 10
  • 5

5 10 0.704 s bins. T0 = MET 478557956.424000 150. 175. 200. 225. 250. 275. 300. 325. 350. counts per bin N3 50 to 539 keV

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 100 / 101

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SLIDE 102

Untriggered GRB 478557956

ADWO CTTE quicklook

  • 0.04
  • 0.02

0.02 0.04 0.06 0.08

  • 3
  • 2
  • 1

1 2 3 Signal/Background Peak Ratio seconds since MET 478557956.424 (bn160301788))

SPBPR=2.008

ELFT Summer School’18 Gamma-ray bursts in the era of multi-messenger astronomy 101 / 101