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
363 triggers 103 GRBs 2432 & 146 GRBs 1255 GRBs 934 GRBs triggers ~150 GRBs 2992 GRBs
Since 1967 more than 40 satellites registered GRB by various detectors in different energy bands. 1991 – 1999 CRGO: ►OSSE 0.05–10 MeV ►COMPTEL 0.7–30 MeV ►EGRET/TASCS 1-200 MeV EGRET/spark chambers 0.02-30 GeV ►BATSE (SD&LAD) 0.01-10 MeV
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 GRB910503 (BATSE trigger #143) on BATSE and EGRET data.
GRB WITH HIGH ENERGY TAILS ON CGRO DATA 15 GRB has E>120 MeV (Kaneko et al, 2008) 3 GRB with Emax ~130140 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
Correlations: Hard to soft и hardness-intensity evolution for most part of GRB with Band and Pl spectra Spectral evolution for typical burst GRB910927
GRB WITH HIGH ENERGY TAILS ON CGRO DATA 15 GRB has E>120 MeV (Kaneko et al, 2008) 3 GRB with Emax ~130140 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.
In some GRB spectra the new spectral components not corresponded to Band model was found GRB 941017: 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
GRB WITH HIGH ENERGY TAILS ON CGRO DATA 15 GRB has E>120 MeV (Kaneko et al, 2008) 3 GRB with Emax ~130140 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, 941017 and 980923)
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 GRB920622 (BATSE trigger #1663) on BATSE, COMPTEL and EGRET data.
GRB WITH HIGH ENERGY TAILS ON CGRO DATA 15 GRB has E>120 MeV (Kaneko et al, 2008) 3 GRB with Emax ~130140 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, 941017 and 980923) 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
Registration of GRB940217 by EGRET and ULYSESS GRB940217 (BATSE trigger #2831, t90150s) 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 GRB940217 by EGRET and ULYSESS Evidence of TeV emission from GRB 970417a using data from the Milagrito: photons with energies ~650 GeV were detected
TeV emission!? GRB WITH HIGH ENERGY TAILS ON CGRO DATA 15 GRB has E>120 MeV (Kaneko et al, 2008) 3 GRB with Emax ~130140 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, 941017 and 980923) 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!?
Fermi & AGILE: 3 spectral breaks should be introduced E1 – band E2 – HE component E3 - low energy component (tens of keV)
The temporal profiles of GRB 080825C, GRB 090525 and GRB 090902B by: (a) LAT data and (b) GBM data (21 GRB).
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
GRB080514B on AGILE data [а) 30 MeV - 30 GeV (GRID), b) 300-700 MeV (MCAL), c) 18-60 keV (SA)]
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
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. 107.08, 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
GRB170405A (18:39:48 UT) in energy range 15-350 keV on Swift/BAT data (t90=165 32 s) and in energy band 50-300 keV on Fermi/GBM data (t90= 81.601 0.923 s)
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
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
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 10-102 GeV from ~2.7% up to 2% from ~0.12о up to ~0.02о > 102 GeV 2% <0.02о
the additional and lateral apertures characteristics Aperture type Energy band Energy resolution Angular resolution Additional 1-10 MeV from 3% up to 2% ~5о 10-102 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% -
Modeling of the dependence of altitude on the satellite coordinates during satellite moving in the Earth magnetosphere (perigee ~500 km, apogee ~300000 km, inclination 51,8 in the beginning period)
The evolution of the perigee and apogee altitudes of the working orbit with time Initial orbit parameters: -the apogee is 300 000 km; -the perigee is 500 km; -the inclination is 51.4. After ~5 months the orbit will transform to circular with a radius of ~150 000 km.
Background… trapped protons E>100 keV Hp=500 km, Ha= 500 km, i=20o, period=1.57 hour like Fermi 1 day flight Ha= 300000 km, Hp= 500km, i=51.8o, period= 171.35 hours like GAMMA-400 30 day flight
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;
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
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;
Thank you for attention!