1. Perspectives of GRBs registration due gamma-telescope GAMMA-400
I.V. Arkhangelskaja,
A. I. Arkhangelskiy1, 2, E. N. Chasovikov1, M. D. Kheymits1,
Y. T. Yurkin1, A. M. Galper1,2, O. D. Dalkarov2,
A. V. Bakaldin3, Yu. V. Gusakov2, A. E. Egorov2,
S. I. Suchkov2, N. P. Topchiev2, A. A. Leonov1,2,
M. F. Runtso1, N. Yu. Pappe2, Yu. I. Stozhkov2,
P. U. Naumov1, I. V. Chernysheva1, 2, V. G. Zverev1
1) National Research Nuclear University MEPhI, Moscow, Russia
2) Lebedev Physical Institute, Russian Academy of Sciences
3) Scientific Research Institute for System Analysis, Russian Academy of Sciences

2. 363 triggers
103 GRBs
2432 & 146 GRBs
1255 GRBs
934 GRBs triggers
~150 GRBs
2992 GRBs

3. Since 1967 more than 40 satellites registered GRB by various detectors in different energy bands.
1991 – 1999  CRGO: ►OSSE –10 MeV
►COMPTEL –30 MeV
►EGRET/TASCS MeV
EGRET/spark chambers GeV
►BATSE (SD&LAD) MeV

4. The temporal profiles of
GRB high energy emission were registered for 15 events
1991 by common analysis of CGRO data  GRB with presence of high energy component (more than some MeV) in spectra
(43 BATSE GRB with f>10 ph/cm2s for E>300keV  26 can be seen by EGRET
and 25 has E>2 MeV
15 has E>120 MeV).
Some tens GRB were detected simultaneously by all 4 experiments onboard CGRO (BATSE, COMPTEL, OSSE and EGRET) 
the widest energy range for -emission registration on satellite experiment for the same GRB was ~10 keV  ~20 GeV.
The temporal profiles of
GRB (BATSE trigger #143)
on BATSE and EGRET data.

5. GRB WITH HIGH ENERGY TAILS ON CGRO DATA
15 GRB has E>120 MeV (Kaneko et al, 2008)
3 GRB with Emax ~130140 MeV no emission E>200 MeV
the widest energy range for -emission registration on satellite experiment for the same GRB was ~10 keV  ~20 GeV

6. Correlations: Hard to soft и hardness-intensity evolution for most part of GRB with Band and Pl spectra
Spectral evolution for typical burst GRB910927

7. GRB WITH HIGH ENERGY TAILS ON CGRO DATA
15 GRB has E>120 MeV (Kaneko et al, 2008)
3 GRB with Emax ~130140 MeV no emission E>200 MeV
the widest energy range for -emission registration on satellite experiment for the same GRB was ~10 keV  ~20 GeV
spectral pparameters are typically decreasing monotonically while the flux rises and falls or its behavior corresponds to flux temporal profile.

8. In some GRB spectra the new spectral components not corresponded to Band model was found
GRB : the common structure of temporal profiles not in agreement in various energy bands:
HE tail
The temporal profiles on BATSE and EGRET data of GRB941017

9. GRB WITH HIGH ENERGY TAILS ON CGRO DATA
15 GRB has E>120 MeV (Kaneko et al, 2008)
3 GRB with Emax ~130140 MeV no emission E>200 MeV
the widest energy range for -emission registration on satellite experiment for the same GRB was ~10 keV  ~20 GeV
spectral pparameters are typically decreasing monotonically while the flux rises and falls or its behavior corresponds to flux temporal profile.
some GRB - new additional spectral component (920902, and )

10. The temporal profiles of
Most part of GRB:
common structure of temporal profiles consistent in various energy bands:
the same amount of global peaks
Peaks were in similarity: approximate ratio of relative peaks intensity are the same too:
first  lowest, last  highest
intensity
The temporal profiles of
GRB (BATSE trigger #1663)
on BATSE, COMPTEL and EGRET data.

11. GRB WITH HIGH ENERGY TAILS ON CGRO DATA
15 GRB has E>120 MeV (Kaneko et al, 2008)
3 GRB with Emax ~130140 MeV no emission E>200 MeV
the widest energy range for -emission registration on satellite experiment for the same GRB was ~10 keV  ~20 GeV
spectral pparameters are typically decreasing monotonically while the flux rises and falls or its behavior corresponds to flux temporal profile.
some GRB - new additional spectral component (920902, and )
mostly common structure of temporal profiles is similar in various energy bands (exluding GRB with no-Band component in the spectra):
the same amount of global peaks
approximate ratio of relative peaks intensity are the same too

12. Registration of GRB940217 by EGRET and ULYSESS
GRB (BATSE trigger #2831, t90150s)
γ-ray emission (> 50 MeV) till 1.5 hours after start of burst, highest-observed energy: 18 GeV
temporal profiles with different time structure in various energy bands  extended emission
Registration of GRB by EGRET and ULYSESS
Evidence of TeV emission from GRB a using data from the Milagrito: photons with energies ~650 GeV were detected

13. TeV emission!? GRB WITH HIGH ENERGY TAILS ON CGRO DATA
15 GRB has E>120 MeV (Kaneko et al, 2008)
3 GRB with Emax ~130140 MeV no emission E>200 MeV
the widest energy range for -emission registration on satellite experiment for the same GRB was ~10 keV  ~20 GeV
spectral pparameters are typically decreasing monotonically while the flux rises and falls or its behavior corresponds to flux temporal profile.
some GRB - new additional spectral component (920902, and )
mostly common structure of temporal profiles is similar in various energy bands (exluding GRB with no-Band component in the spectra):
the same amount of global peaks
approximate ratio of relative peaks intensity are the same too
some GRB  extended high energy emission Emax ~18 GeV
TeV emission!?

14. Fermi & AGILE: 3 spectral breaks should be introduced
E1 – band
E2 – HE component
E3 - low energy component (tens of keV)

15. The temporal profiles of GRB C, GRB and GRB B by: (a) LAT data and (b) GBM data (21 GRB).

16. PRESENT TIME  gamma-emission: satellite experiments Fermi and AGILE.
all properties founded during CGRO and AVS-F database analysis
Additional HE component in GRB spectra
Extension of HE component to low energy region down to tens keV?
Both short and long GRB has extended emission
Precursors in wide energy band
High energy precursors

17. GRB080514B on AGILE data [а) 30 MeV - 30 GeV (GRID), b) 300-700 MeV (MCAL), c) 18-60 keV (SA)]

18. PRESENT TIME  gamma-emission: satellite experiments Fermi and AGILE.
all properties founded during CGRO and AVS-F database analysis
Additional HE component in GRB spectra
Extension of HE component to low energy region down to tens keV?
Both short and long GRB has extended emission
Precursors in wide energy band
High energy precursors

19. What is the difference between an ultra-long GRB and a long GRB?
How to predict that an event will be an ultralong GRB, i.e. duration more than 3 hours, while
high-energy detectors are recording only the first tens of seconds? Joyce, Quianah T.; Gendre, Bruce; Orange, N. Brice
American Astronomical Society, AAS Meeting #231, id , 2018
background physical origin
for -emission detectors
onboard low altitude
satellites defined by:
diffuse cosmic -emission,
atmospheric -rays,
-emission formed in interactions
of charged particles
(both prompt
or activation)
and Earth albedo
Neutrons
Time,s

20. GRB170405A (18:39:48 UT) in energy range keV on Swift/BAT data (t90=165  32 s) and in energy band
keV on Fermi/GBM data
(t90=  s)

22. GRB registration by GAMMA-400 telescope:
high energy and
time resolution
main aperture
converter & TOF
high angular resolution 
ground strip track in C
analysis
anticoincidence – ACtop,
AClat
additional aperture
CC1 & S2 & LD
angular resolution 
ground strip track in CC1
analysis
anticoincidence –S2,S3,LD
side aperture
angular resolution
(similar to BATSE)
calorimeter structure
anticoindence – S3, S4, LD

23. Fermi_Technical_Handbook:
"Because GLAST’s ACD is segmented, it can distinguish backsplash, because a backsplash-hit tile will generally not be in the area through which the gamma ray arrived. In addition, the ACD threshold can be operated at a higher level than EGRET’s, also reducing backsplash vetoes."
BUT: The example of 100 GeV gammas energy deposition in AC
only 1 particle from 5 pass AC without any interaction!!
and 1 particle from 5 has direct interaction in the same detector than its impinge two time sensitive layers – backsplash rejection
AC detectors
Energy deposition, MeV
Particle number 67 68 69 70 71
AC_0
AC_13
0,00066
0,1182
0,00067
0,0186
AC_1
AC_14
0,21673
AC_2
AC_15
AC_3
AC_16
AC_4
AC_17
AC_5
AC_18
0,44438
AC_6
AC_19
0,37155
AC_7
AC_20
0,04634
AC_8
AC_21
AC_9
AC_22
AC_10
AC_23
AC_11
AC_24
0,37288
AC_12
AC_25

24. the main aperture characteristics
Energy band
Energy resolution
Angular resolution
20 MeV-0.25 GeV
from ~30% up to ~15%
from ~5о up to ~1.5о
0.25 – 1 GeV
from ~15% up to ~9%
from ~1.5о up to ~0.6о
1 – 10 GeV
from ~9% up to ~2.7%
from ~0.6о up to ~0.12о
GeV
from ~2.7% up to 2%
from ~0.12о up to ~0.02о
> 102 GeV 2%
<0.02о

25. the additional and lateral apertures characteristics
Aperture type
Energy band
Energy resolution
Angular resolution
Additional
1-10 MeV
from 3% up to 2%
~5о
MeV 2%
~4о
0.1-1 GeV
from ~4о up to ~1о (provides by strips in CC1)
> 1 GeV
~0.7о(provides by strips in CC1 and shower axis registration in CC2)
Lateral
0.3-1 MeV
from ~10% up to ~3%
Only for transient events ~5о
1-5 MeV
~3%
Only for transient events ~10о
> 10 MeV
~2% -

26. Modeling of the dependence of altitude on the satellite
coordinates during satellite moving in the Earth
magnetosphere (perigee ~500 km, apogee ~ km, inclination 51,8 in the beginning period)

27. The evolution of the perigee and apogee
altitudes of the working orbit with time
Initial orbit parameters:
-the apogee is km;
-the perigee is 500 km;
-the inclination is 51.4.
After ~5 months the orbit will transform to
circular with a radius of ~ km.

28. Background… trapped protons E>100 keV
Hp=500 km, Ha= 500 km,
i=20o, period=1.57 hour
like Fermi
1 day flight
Ha= km,
Hp= 500km,
i=51.8o, period= hours
like GAMMA-400
30 day flight

29. The list of main research with GAMMA-400 allow advanced studying of GRB:
1) Energy spectra detailed investigation in the wide band :
a) Definition of maximum energy of -quanta registered during GRB;
b) Check of no-Band component presence during burst;
c) Е1 and Е2 spectral breaks positions definition;
d) Spectral indexes evolution investigation and hard to soft tendency check;
e) High energy -quanta spatial distribution studying for particles with E > 100 MeV;
f) Search of possible correlations between Е2 and Е3 spectral breaks positions, burst spectral indexes and other GRB characteristics;
g) Search of spectral features could be associated with mesons decay lines and possible processes in black holes;

30. 3) GRB precursors spectra and temporal profiles investigation
2) Temporal profiles detailed investigation in the wide energy band :
a) characteristic and minimum variability times definition;
b) burst temporal profile shape variation investigation in dependence of energy bands (comparison temporal profiles and characteristic and minimum variability times in the energy bands E > Е2 , Е2 > E > Е1 and Е1 > E > Е3 ) ;
c) GRB duration distribution studying;
d) temporal profiles in various source parts studying if angular resolution allow to recognize any spatial features at burst image in energy band
E > 20 MeV;
e) temporal profiles in lines investigations if several spectral features will be separated;
3) GRB precursors spectra and temporal profiles investigation

31. 4) High energy afterglow spectra detailed investigation:
a) Definition of registered -quanta maximum energy;
b) Possible spectral break position definition;
c) Spectral indexes evolution investigation;
d) High energy -quanta spatial distribution studying for particles with E > 100 MeV;
e) Search of possible correlations between various GRB and its high energy afterglow spectral characteristics;
f) Search of spectral features;
5) High energy afterglow temporal profiles detailed investigation:
characteristic and minimum variability times definition;
temporal profiles in various source parts studying if angular resolution allow to recognize any spatial features at burst image in energy band
E > 100 MeV;
c) temporal profiles in lines investigations if several spectral features will be separated;

32. Thank you for attention!