Transcript GRB051103 and GRB070201 as Giant Flares from SGR in Nearby

Cosmic Gamma-Ray bursts studies with Ioffe Institute Konus experiments
R.L. Aptekar, S.V. Golenetskii, D.D. Frederiks, E.P. Mazets, V.D. Pal’shin
Ioffe Institute, Saint Petersburg, Russia
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Study and analysis of the cosmic gamma-ray bursts from the
interplanetary missions Venera 11-14 in 1979-1983: determination of
main observational feature of the burts. Soft gamma-repeaters (SGR)
were discovered.
Russian-American Konus-Wind experiment: of many years
uninterrupted observations of cosmic gamma-ray bursts and soft
gamma-repeaters.
Konus-Wind experiment: correlative observations of cosmic gammaray bursts with the Kosmos and Coronas spacecraft.The research on
the 27 December 2004 flare was the first examlpe of studying Moonreflected X-ray and gamma-radiation coming from a source outside the
Solar System. SGR sources in the galaxies M81 and M31were
discovered.
Russian-American Konus-Wind experiment, which has already been
operating for more than 17 years, provides important and often unique
data regarding the various characteristics of GRBs in the 20 keV to 15
MeV energy range.
Future Ioffe Institute Konus experiments
One of earliest confirmation of the GRB discovery was obtained on January
17, 1972 using the Kosmos-461 data (Mazets et al., JETP Lett., 1973)
The Konus experiments on board the Venera 11 to 14 deep space
missions in 1979 to 1983
Left: determination of the source direction of a gamma burst with a system of gamma detectors with
anisotropic angular sensitivity;
Right: Block diagram of the Konus instrumentation. A sensor system of six scintillation detectors with
a close to cosine angular sensitivity pattern arranged along six axes of the spacecraft.
The Konus experiments on board the Venera 11 to 14 deep space missions in
1979 to 1983.
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Konus observations of the
temporal structures of GRBs
revealed of the existence of a
separate class of short bursts,
demonstrating the so-called
«bimodal» duration distribution
(Mazets et al., A&Sp.Sci.
1981).
The Konus experiments on board the Venera 11 to 14 deep space
missions in 1979 to 1983: it was for the first time shown that that
the GRB distribution over the celestial sphere is random
Konus, Venera 11-14 deep space
missions( Mazets and Golenetskii
Astrophys and Space Space Physics
Rev., 1988)
BАТSЕ, CGRO
(Paciesas et al.,
Ap.J., 1996)
The Konus experiments on board the Venera 11 to 14 deep space
missions in 1979 to 1983.
Observations on Venera 13 and 14 reveal
a strong correlations between temporal
and spectral behavior of GRBs
(Golenetskii et al., Nature, 1983).
The Konus experiments on board the Venera 11 to 14 deep space missions in
1979 to 1983: soft gamma-repeaters were discovered.
Giant flare of SGR0526-66 was observed on
March 5, 1979г.( Mazets et al., , Nature, 1979)
Repeated bursts from SGR0526-66,
(Golenetskii et al.,Nature, 1983)
Joint Russian-American Konus-Wind experiment
S/c «Wind», 1994 – up to now
The orbit of s/c excepts an interferences from radiation belts and the
Earth shadowing.
Schematic view of the Konus-Wind gamma-ray detector
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The gamma-ray detector
is a NaI(Tl) crystal 5
inches in diameter ans 3
inches in hight, placed
into a aluminum container
with a beryllium entrance
window. The crystal
scintillator is viewed by a
photomultiplier tube
through a 20 mm thick
lead glass.
(Aptekar et al., Space
Science Rev.,1995)
Konus-Wind Gamma-Ray Burst Experiment on
US GGS-Wind spacecraft
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Two detectors S1 and S2:
NaI(Tl) 13 cm diameter, 7.5 cm height, 12.5 cm Be entrance window.
Located on opposite faces of spacecraft, observing correspondingly the southern
and northern celestial hemispheres
Burst mode:
Time history analyzer: resolution 2ms – 256 ms, total duration 230s
12 – 50 keV
4096 ch
50 – 200 keV 4096 ch
200 – 770 keV 4096 ch
Pulse Height analyzer: accumulation time 64ms – 8.192 s, duration 79 – 492 s
PHA1 12 – 770 keV
63 ch quasilog scale
PHA2 0.2 – 10 MeV
63 ch quasilog scale
Background mode: accumulation time 1.47 – 2.94 s
Count rate:
12 – 50 keV
50 – 200 keV
200 – 770 keV
> 10 MeV
In flight detector gain stability monitoring
Spectral and temporal analysis of GRBs characteristics detected by KonusWind experiment.
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Between 1994 November and 2012 May, the Konus-Wind experiment has detected about 2000
GRBs in the trigger mode. Hardness ratios, peak intensities, and temporal parameters, such as
(T50, T90) durations and spectral lags are determined for this bursts sample. We argue that
T50 is more robust measure for bursts classification than T90. Figures show both types of
such distributions for the detected bursts.
Spectral and temporal analysis of GRBs characteristics detected by KonusWind experiment.
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The discrepancy of long and short GRBs in terms of hardness-duration
distribution was analyzed. A comparison was made for 225 bright short
GRBs and for 708 bright long GRBs.
Short gamma-ray bursts with extended emission observed with the KonusWind experiment.
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The existence of “short” gamma-ray bursts accompanied by soft low-intensity emission
persisting for tens of seconds was firstly reliably demonstrated in the Konus Catalog in 2002.
Later it was confirmed by BAT/Swift instrument and was named extended emission (EE). A
comprehensive analysis of short GRBs with EE was performed. It was shown that short GRBs
with EE constitute 30% from total number of short GRBs. The initial pulse (left panel) and EE
of the burst with the extremely bright EE of GRB070207
The Konus-Wind observations of extremely long gamma-ray burst on April 7, 2008
The extremely long GRB080407 was
investigated thoroughly by Konus-Wind
experiment together with IPN spacecraft. The
observations reveal two distinct emission
episodes separated by ~ 1500 s long period
of quiescence. The total duration of the burst
is about 2100 s. The measured burst fluence
is ~ 4x10-4 erg cm-2 .
GRB041211 – long burst with a complex structure
Simultaneous observations of GRB050717 by Konus-Wind and
BAT(Swift)
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An intensity and long
GRB050717 was observed by
Konus-Wind in the energy range
21 кэВ – 1300 keV and by BATSwift in the energy range 15350 keV. The joint spectral fit is
presented. This GRB has a
record peak energy value
Ep=2400 keV.
(H. Krimm et al., Ap.J., 2006)
Simultaneous observations of GRB080721 by Konus-Wind and
BAT(Swift)
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Light curves (left) and joint spectral fit : ВАТ(Swift) in the energy range 15-350
keV и Konus-Wind in the energy range 21keV - 7.0 MeV (MNRS, 2009)
Optical and gamma-radiation of GRBs
Optical and gamma emission of the GRB
050820A, obtained by RAPTOR telescope of
Los-Alamos Labotatory (upper picture) and
by Konus-Wind experiment (low picture). Both
type of radiation was detected simultaneously
(Vestrand et al., Nature, 2006).
Optical andgamma-radiation of GRB080319B
The Konus-Wind gamma-ray light curve is presented together with optical data of Tortora
telescope. Optical flash begins and ends at about the same times, providing strong evidence
that both originate at the same times (Racusin et al., Nature, 2008).
Konus-Wind and Helicon (CORONAS-F) simultaneous observations of giant
flare from SGR1806-20 on December 27, 2004
The Konus-Wind detector was evidently saturated for over 1.5 s. The Helicon detector was screened by the Earth
from direct exposure of initial pulse of the giant flare, but clearly recorded its reflection from the Moon surface. It
allowed, for the first time, reliably reconstructing the temporal profile of the initial pulse of giant flare and determining
its energy parameters.
Konus-Wind and Helicon (CORONAS-F) simultaneous observations of giant flare from
SGR1806-20 on December 27, 2004
The full isotropic energy release Q=2,3х1046 erg and the peak luminosity L=3,5х1047 эрг с-1 (Frederiks et al.,
Astronomy Lett., 2007)
Konus-Wind observations of GRB 051103
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The light curve of GRB051103
recorded in the energy range 18 –
1100 keV with time resolution of
2 ms.
The burst is in shape of a single
pulse with a steep leading edge
(≤ 6 ms) and a quasi-exponential
decay (τ ~ 50 ms). The total
burst duration is ~ 170 ms
The burst had been the brightest
GRB observed by Konus-Wind in
11 years, its peak count rate on 2
ms scale in 18 – 1100 keV
reached ~ 1.5 x105 s-1
Konus-Wind observations of GRB 051103
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The IPN box of GRB051103 (Golenetskii etal.
2005) is superimposed on 21-cm map of the
M81/M82/NGC3077 group and the positions of
X-ray sources discovered in the galaxy M81
and its vicinity (Swartz et al. 2003)
The Chandra X-ray observatory surveyed the
M81galaxy and revealed 177 X-ray sources
with luminosities >1037erg s-1 (Swartz et al.
2003). 14 of then fall within the IPN box.
The values of the fluence and peak flux
corresponds to an isotropic energy output
Q=7x1046 erg and an isotropic peak luminosity
L=4x1048 erg s-1 if the source of GRB051103 is
situated in M81/M82 group at D=3.6 Mpc
Frederiks et al., Astronomy Letters, 2007
VLA 21cm map: http://www.astro.umass.edu/myun
Konus-Wind observations of GRB 070201
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The light curve of GRB070201 recorded
in the energy range 17 – 1130 keV with
time resolution of 2 ms
It displays a narrow pulse with a steep
leading edge (~ 20 ms) followed by
prolonged decay up to 180 ms.
The maximum count rate occurs in a ≤
2 ms.
The maximum count rate was ~6x105
s-1
Konus-Wind observations of GRB 070201
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UV image of the M31 galaxy (Thilker et
al. 2005) and 3σ IPN error box of
GRB070201
Twenty-two sources from an XMMNewton X-ray survey of M31 fall within
the error box (Pietch, 2005)
The values of the fluence and peak flux
corresponds to an isotropic energy
output Q=1x1045 erg and an isotropic
peak luminosity L=1.2x1047 erg s-1 if
the source of GRB070201 is situated in
M31 at D=780 kpc
Aptekar et al., Ap.J., 2009
GALEX synthesized M31 UV image (Thilker et al. 2005)
Giant flare on 1998 August 27 (SGR 1900+14)
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Time and energy
characteristics of the August
27 event.
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Top: Background subtracted light
curve of the outburst. Horizontal
sections with triangles specify
count rates averaged over the
period. The sloped dashed line is a
plot of exp(-t/t) for t = 91.5 s.
Bottom: Horizontal sections with
squares specify kT averaged over
the period.
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Hurley et al., Nature, 1999
Giant flare on June 18, 1998 (SGR 1627-41)
Time and energy characteristics of
the June 18 event.
Top: Background subtracted light curve of
the outburst.
Bottom: Spectral evolution during the
burst.
Mazets et al., Ap.J.L., 1999
Burst series on 1998 May 30 (SGR 1900+14)
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89 days before the giant fare
on August 27
Total fluence (>20keV)
S=5.610-5 erg cm-2
[Energy release Q=1.11042
erg]
Mazets et al., Astronomy
Letters, 1999
Burst series on 5 October 2004 from SGR 1806-20
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83 days before the giant flare
The series was also detected by
INTEGRAL (IBIS/ISGRI)
Frederiks et al., Astronomy Letter,
2007
Konus-Wind observations of GRB110918A: it is the most intense long GRB in the
history of Konus-Wind observations since November, 1994
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As observed by Konus-Wind, the burst had a
20-10000 keV fluence of 7.5x10-4
erg/cm2,and 16-ms peak flux of 9.2x10-4
erg/cm2/s.
GRB were observed also by INTEGRAL (SPIACS), Mars Odyssey (HEND), and MESSENGER
(GRNS). Localized by IPN to the 62 sq arcmin
box. A bright X-ray source was found on the
edge of the IPN box in Swift/XRT TOO
observations which were started ~1.5 days
after the trigger. Following the XRT detection,
a bright optical counterpart was found
(Swift/UVOT, INT, GROND, Gemini-N and
more) and it's redshift was determined
(z=0.982: Gemini-N, GTC).
The burst intensity allows a precise analysis of
the light curves and a fine-scale time-resolved
spectral fitting (see Figure). A detailed analysis
of the Konus-Wind prompt gamma-ray
detection, together with the refined IPN
localization and results of the ~50 days-long
afterglow monitoring by Swift/XRT and
Swift/UVOT can be found soon in the
forthcoming paper (Frederiks et al., 2012,
in preparation).
Konus-UF is one of the future Ioffe Institute experiments in the field of GRB
study. It is planned that Konus-UF will be accomodate on board Spectr-UF
space mission (the World Space Observatory)
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The Konus-UF instruments consists from
two detector units Konus-UF-DS1 and
Konus-UF-DS2 and electronic unit KonusUF-BE.
The each Konus-UF detector will be
allocate such manner in order to observe
the half of hemisphere.
The energy range of Konus-UF instrument
is from 10 keV up to 10 MeV.
The instrument will have a detailed
program for measuring of time and
spectral characteristics of GRBs.
It is planned that Spectr-UF mission will
be launched in 2016 year.
The Konus-UF detector unit drawing
The main parts of the detector: 1 – NaI(Tl) cristal 5’’ in diameter by 3’’ in hight, 2 – beryllium entrance window,
4 – lead glass, 6 – photomultiplier, 12, 13, 14 – electronic boards.
Conclusions
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The early Konus experiments onboard the Venera 11-14 deep space missions had
firstly revealed many of the basic characteristic of GRBs.
Joint Russian-American Konus-Wind experiment, which has already been
operating for more than 17 years, provides important and often unique data
regarding the various characteristics of GRBs in the 20 keV to 15 MeV energy
range.
The Konus-UF experiment is planned for launch in 2016. It will give us an
opportunity to continue very effective research into extremely explosive
phenomena in the Universe.