////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  1072
SUBJECT: Possible burst from SGR1806-20
DATE:    01/06/26 23:21:40 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@sunspot.ssl.berkeley.edu>

K. Hurley, on behalf of the Ulysses GRB team, reports:

In addition to observing the burst from SGR1806-20 on 2001 June 23
at 57293 s UT (GCN 1070), Ulysses observed a later event whose
origin is likely to be this same SGR.  This burst would have had
an Earth-crossing time of 61056.8 s.  Its duration was ~0.032
s, and its 25-100 keV fluence was ~2x10^-7 erg/cm^2.  It had
a peak flux over 0.032 s of ~6x10^-6 erg/cm^2 s.  To our knowledge,
no other instrument observed this event so we cannot be absolutely
certain of its origin, but based on its time history and proximity
in time to the previous burst, its origin is likely to be SGR1806-20,
rather than SGR1900+14 (GCN 1071).

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  1222
SUBJECT: IPN observations of SGR1806-20
DATE:    02/01/25 20:48:02 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@sunspot.ssl.berkeley.edu>

K. Hurley, on behalf of the Ulysses GRB team, and C. Guidorzi,
E. Montanari, F. Frontera, and M. Feroci, on behalf of the BeppoSAX
GRBM team, report:

Ulysses and BeppoSAX have detected a series of short duration
bursts which appear to originate from SGR1806-20:

DATE    TIME    ULYSSES  BEPPOSAX
____    ____    _______  ________

020117  81678*  YES      IN SAA AND EARTH-BLOCKED
020118  71671   YES      YES
020122  38418*  YES      NO DATA

*TIME AT ULYSSES, WHICH WAS ABOUT 1250 LIGHT-SECONDS FROM EARTH;
EARTH-CROSSING TIME FOR SGR1806 IS ABOUT 107 S LATER

The only burst which could be triangulated was the one on
January 18, and its position agrees with that of SGR1806-20.
The burst on January 22 was particularly intense.  If all
of these events are indeed from SGR1806-20, this may signal
a resurgence of activity from this source. 

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  1233
SUBJECT: IPN detection of further activity from SGR1806-20
DATE:    02/01/29 00:34:27 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@sunspot.ssl.berkeley.edu>

K. Hurley, on behalf of the Ulysses GRB team, E. Mazets and
S. Golenetskii, on behalf of the Konus-Wind GRB team, and C. Guidorzi,
E. Montanari, F. Frontera, and M. Feroci, on behalf of the BeppoSAX
GRBM team, report:

The IPN continues to detect activity which is probably from SGR1806-20.  
The updated event list is now:


DATE    TIME    ULYSSES  BEPPOSAX    KONUS
____    ____    _______  ________    _____

020117  81788   YES      IN SAA      WEAK RESPONSE
020118  71671   YES      YES         YES
020122  38499   YES      NO DATA     YES
020124  79251*  YES
020125  36444*  YES

*TIME AT ULYSSES, WHICH WAS ABOUT 1250 LIGHT-SECONDS FROM EARTH;
EARTH-CROSSING TIME FOR SGR1806 IS ABOUT 75 S LATER

The bursts on the 17th, 18th, and 22nd have all been triangulated to
annuli which are consistent with the position of SGR1806.  The bursts
on the 24th and 25th are definitely SGR-like, in that their durations
are ~30 ms; there are too few photons in the Ulysses data to determine
their spectra, however.  We are searching for confirmation of them in
the GRBM and KONUS data, which will allow triangulation.


////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  1391
SUBJECT: IPN triangulation of a burst from SGR1806-20
DATE:    02/05/16 00:18:36 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@sunspot.ssl.berkeley.edu>

K. Hurley, on behalf of the Ulysses GRB team, and 

D. Smith, R. Lin, J. McTiernan, R. Schwartz, C. Wigger, W. Hajdas,
and A. Zehnder, on behalf of the RHESSI GRB team, report:

Ulysses and RHESSI observed a burst on May 15 at 01:26:41 UT with ~20
ms duration.  Triangulation gives an annulus which is consistent with
the position of SGR1806-20.  Ulysses has in addition observed numerous
short events over the past several days.  Although none could be
triangulated, this may suggest that SGR1806-20 is entering a new period
of activity.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  1396
SUBJECT: IPN detection of possible bursts from SGR1806-20
DATE:    02/05/27 23:19:13 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@sunspot.ssl.berkeley.edu>

K. Hurley, on behalf of the Ulysses GRB team,

E. Mazets and S. Golenetskii, on behalf of the Konus-Wind GRB
team, and

T. Cline, on behalf of the Ulysses and Konus teams, report:

Two short bursts were detected on May 25 which, due to their proximity
in time to an earlier burst from SGR1806-20 (see GCN 1391), may also be
from this SGR.  The first was at ~16014 s and was observed by Konus-Wind;
the second was detected by Ulysses and was at 43615 s (Ulysses time;
the spacecraft was ~1850 light-seconds from Earth).  If the second
event came from SGR1806-20, its Earth-crossing time would have been
~1047 s earlier, or ~42568 s.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  1726
SUBJECT: IPN detection of renewed activity from SGR1806-20
DATE:    02/12/07 20:31:06 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@sunspot.ssl.berkeley.edu>

K. Hurley, on behalf of the Ulysses GRB team, 

E. Mazets and S. Golenetskii, on behalf of the Konus-Wind GRB team, and

T. Cline, on behalf of the Ulysses and Konus GRB teams, report:

Ulysses has observed 5 short, intense SGR-like bursts on December
5 and 6.  So far, one of these events has also been reported
by Konus-Wind, and the center line of its triangulation annulus
passes ~10" from the position of SGR1806-20, and >5 degrees
from that of SGR1900+14.  We conclude that this burst indeed
originates from SGR1806-20.  As there is a hint of continuing
activity from SGR1900+14, we cannot at this point be certain
of the origin of the other events, but will attempt to determine
this as soon as possible.

The times of these events were:

December 5, 2002:  02828 s *
		   12925 s *
		   32992 s **
		   72064 s *
December 6, 2002:  63291 s *

* crossing time at Ulysses; subtract ~418 s to get Earth-crossing
  time if the source was SGR1806-20

** event also observed by Konus; this is the Earth-crossing time

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  1764
SUBJECT: IPN detection of continued activity from SGR1806-20
DATE:    02/12/17 21:58:18 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@sunspot.ssl.berkeley.edu>

K. Hurley and T. Cline, on behalf of the Ulysses GRB team, and

V. Pal'shin, E. Mazets, and S. Golenetskii, on behalf of the Helicon-
Coronas GRB team, report:

Ulysses and Helicon  observed this burst at 40754 seconds.  As observed
by Ulysses, it had a duration of approximately 0.25 seconds, a 25-100
keV fluence of approximately  6.4E-06 erg/cm2, and a peak flux of
approximately  7.4E-06 erg/cm2 s over 0.25 seconds.

We have triangulated it to a preliminary annulus centered  at RA,
Decl(2000)= 3.003,  -36.081 degrees, whose radius is 78.796 +/-  0.034
degrees (3 sigma ).  As the center line of this annulus passes within
14" of the position of SGR1806-20, we conclude that it was the source
of this burst.  Prior to this, the last confirmed burst from this SGR
was on December 5 (GCN 1726).

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2283
SUBJECT: HETE detection of burst from SGR1806-20
DATE:    03/06/16 18:22:18 GMT
FROM:    Roland Vanderspek at MIT  <roland@space.mit.edu>

K. Hurley, J-L. Atteia, N. Kawai, D. Lamb, G. Ricker, and S. Woosley on 
behalf of the HETE Science Team;

C. Barraud, M. Boer, J-F Olive, and J-P Dezalay on behalf of the HETE 
FREGATE Team;

N. Butler, G. Crew, J. Doty, G. Prigozhin, R. Vanderspek, J. Villasenor, 
T. Cline, J. G. Jernigan, A. Levine, F. Martel, E. Morgan, G. Monnelly,
G. Azzibrouck, J. Braga, R. Manchanda, and G. Pizzichini, on behalf of
the HETE Operations and HETE Optical-SXC Teams;

M. Suzuki, C. Graziani, Y. Shirasaki, T. Donaghy, M. Matsuoka, K. Torii,
T. Tamagawa, T. Sakamoto, A. Yoshida, E. Fenimore, M. Galassi,
Y. Nakagawa, R. Satoh, Y. Urata, T. Yamazaki and Y. Yamamoto, on behalf 
of the HETE WXM Team report:


HETE Trigger H2734, detected at 04:14:29 UT on 9 June 2003, was
due to a short burst from SGR1806-20.  This burst had a duration 
of ~100 ms and a 30-100 keV fluence of 6 x 10^-8 erg/cm2.  The 
position was not circulated automatically because the spacecraft
aspect had not yet been determined.

This detection may indicate the onset of a new period of activity 
for this SGR.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2297
SUBJECT: IPN detection of renewed activity from SGR1806-20
DATE:    03/07/14 18:51:10 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@sunspot.ssl.berkeley.edu>

K. Hurley and T. Cline, on behalf of the Ulysses and HETE GRB teams,

D. M. Smith, R. P. Lin, J. McTiernan, R. Schwartz, C. Wigger, W.
Hajdas, and A. Zehnder, on behalf of the RHESSI GRB team,

A. von Kienlin, G. Lichti, and A. Rau, on behalf of the
INTEGRAL SPI-ACS GRB team, and

G. Ricker, J-L Atteia, N. Kawai, D. Lamb, S. Woosley, J. Doty, R.
Vanderspek, J. Villasenor, G. Crew, G. Monnelly, N. Butler, J.G.
Jernigan, A. Levine, F. Martel, E. Morgan, G. Prigozhin, J. Braga, R.
Manchanda, G.  Pizzichini, Y. Shirasaki, C. Graziani, M. Matsuoka, T.
Tamagawa, K. Torii, T. Sakamoto, A. Yoshida, E. Fenimore, M. Galassi,
T. Tavenner, T.  Donaghy, M. Boer, J-F Olive, and J-P Dezalay, on
behalf of the HETE GRB team, report:

Ulysses, INTEGRAL (SPI-ACS), RHESSI, and HETE have observed
two events whose arrival directions are consistent with that
of SGR1806-20:

DATE	UT	ANNULUS	 ANNULUS    ANNULUS    deltaR	DISTANCE  DURATION  PEAK FLUX  FLUENCE  SPACECRAFT  
        S.	RA(2000) DEC(2000)  RADIUS    (3 SIGMA)  DEG.	   S.       erg/cm2s   erg/cm2
030712 76693.0  335.440 -27.794     57.625     0.017    0.003     0.180     5E-6       4E-6	ULYSSES, RHESSI, INTEGRAL
030713 77470.8  335.566 -27.667	    57.749     0.017    0.0001    0.032     1E-6       1E-7     ULYSSES, HETE(2763)

The annulus half-width is deltaR; distance is the angular distance between the centerline
of the annulus and the position of SGR1806-20; duration is the duration as observed
by Ulysses; peak fluxes and fluences are as observed by Ulysses, and are over 0.03125 s, 
and 25-100 keV.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2306
SUBJECT: RXTE PCA Observations of SGR1806-20 Region
DATE:    03/07/18 02:53:20 GMT
FROM:    Craig Markwardt at GSFC  <craigm@milkyway.gsfc.nasa.gov>

RXTE PCA Observations of SGR 1806-20 Region

A. Ibrahim (GWU/GSFC), C. Markwardt (UMD/GSFC), J. Swank (GSFC), 
K. Hurley (UCB), T. Cline (GSFC), & W. Parke (GWU)

Report:

In response to the burst activity reported by IPN on Jul 14 (GCN
2297), we pointed the RXTE PCA at the position of SGR 1806-20 on Jul
15, 11:35-12:20 UT.  A 0.4 mCrab pulsed flux was detected with a
period of 5.54 s +/- 0.01 s.  The PCA saw 3.5 mCrab total flux, but as
much as half is due to Galactic ridge emission in the field of view,
so that the pulsed fraction could exceed 20%.  The large difference
between the pulse period and the last observed pulse period of SGR
1806-20 (Woods et al. 2002, ApJ, 576, 381) suggests that a new pulsar
is present.  There are no known pulsars with that period in the 1.2
deg radius field of view of the PCA and we can rule out the nearby
candidate SGR 1801-23 (Cline et al. 2000, ApJ, 531, 407).  If the new
pulsar were responsible for the recent bursts, there would be three
SGRs in a small region. However it is possible that both SGR 1806-20
and another pulsar are active simultaneously.  PCA scanning
observations are planned.

This message is citeable.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2309
SUBJECT: SGR 1806-20, submm observations
DATE:    03/07/19 05:22:38 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

S. Klose (@SEST), B. Stecklum, & H. Linz, Thuringer Landessternwarte Tautenburg,
J. Greiner, MPE Garching,

report:


We observed the field of SGR 1806-20 with the Swedish-ESO Submillimetre Telescope
(SEST) at La Silla, Chile, on July 18/19, 0:35 - 2:10 UT. The observations were
performed with the SIMBA Imaging Bolometer Array at a wavelength of 1.2mm and started
approximately 45 min after an outburst was recorded from SGR 1806 by HETE 2 and
ended approximately 1.5 hrs before the next outburst was recorded (Hurley et al.,
GCN 2308). A superposition of 4 maps (400 x 600 arcsec), 8 min mapping time each,
does not reveal any source at the position of the SGR down to a flux density limit
of approximately 100 mJy.



////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2311
SUBJECT: Konus-Wind detection of the bursts from SGR1806-20 region
DATE:    03/07/22 13:47:11 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin,
D. Frederiks (all Ioffe Institute), T. Cline (NASA GSFC),
and K.Hurley (UCB) on behalf of the Konus-Wind team, report:

A short soft burst was detected on 030719 by Konus-Wind starting at
83914.490s UT. The event had a duration of 0.25s, a soft energy
spectrum ~ E^(-1)exp(-E/Eo) with Eo = 18.5 +/- 1 keV, fluence of 5x10-6
erg sm-2 and peak flux of 3x10-5 erg cm-2 s-1, evaluated both
in 15-300 keV range.

Apparently the burst originates from the SGR1806-20 or from its close
vicinity in accordance with observations of the burst activity reported
in GCN 2306, 2307, and 2308.

Two weak soft events were detected by Konus-Wind in the background
mode on 030720 at 08:07:12 and 22:34:19. The last event was
detected by HETE (H2773). Estimated time delay is consistent with 
SGR1806-20 position.




////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2354
SUBJECT: IPN detection of continued activity from SGR1806-20
DATE:    03/08/18 23:28:52 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@sunspot.ssl.berkeley.edu>

K. Hurley and T. Cline, on behalf of the Ulysses and Mars Odyssey GRB
teams,

I. Mitrofanov, S. Charyshnikov, V. Grinkov, A. Kozyrev, M. Litvak, and
A. Sanin, on behalf of the HEND-Odyssey GRB team, and

W. Boynton, C. Fellows, K. Harshman, C. Shinohara and R. Starr, on
behalf of the GRS-Odyssey GRB team, report:

Ulysses and Mars Odyssey (HEND) observed this unusually long SGR
burst.  As observed by Ulysses, it had a duration of approximately 1
second, a 25-100 keV fluence of approximately  7.3E-06 erg/cm2, and a
peak flux of approximately  1.9E-05 erg/cm2 s over 0.25 seconds.

We have triangulated it to a preliminary annulus centered at RA,
Decl(2000)=340.644, -22.919 degrees, whose radius is 63.096 +/-0.013
degrees (3 sigma).  As the center line of this annulus passes 0.003
degrees from the position of SGR1806-20, we consider it most likely
that this event originated from that SGR.  If so, the Earth-crossing
time was 50231 seconds.  However, due to the present configuration of
the IPN, Ulysses/Mars, Mars/Earth, and Ulysses/Earth annuli which are
consistent with the position of SGR1806-20 will also be consistent with
portions of the error circle for the possible new SGR, 1808-20 (GCN
2351).  Depending on the exact position of SGR1808-20, however, the
converse is not necessarily true.  Thus it may be possible to confirm
the existence of this new source with the IPN if it bursts again.  The
situation is illustrated with a map which has been posted at
ssl.berkeley.edu/ipn3/030818.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2372
SUBJECT: INTEGRAL ToO OBSERVATIONS OF SGR1806-20: CALL FOR CORRELATED OBSERVATIONS
DATE:    03/08/29 22:10:44 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@sunspot.ssl.berkeley.edu>

K. Hurley and D. Hartmann, on behalf of a large collaboration, report:

A 240 ksec INTEGRAL target of opportunity observation of SGR1806-20 has
been scheduled for 2003 September 03, starting at 22:45 UT.
Simultaneous observations at all wavelengths, but particularly in the
NIR (bearing in mind that the reddening is AV=29 mag), are encouraged.
The best position for this SGR is the one obtained by Chandra
(Eikenberry et al., ApJ 563, L133, 2001; Kaplan et al., ApJ 564, 935,
2002):

RA(2000)=18 h 08 m 39.32 s, Decl(2000)=-20 o 24 ' 39.5 "

Updates to the INTEGRAL schedule will be posted at:

http://astro.estec.esa.nl/integral_webapps/index.jsp?future

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2376
SUBJECT: Radio Observations of SGR1806-20
DATE:    03/09/04 15:41:11 GMT
FROM:    Dale A. Frail at NRAO  <dfrail@nrao.edu>

M. P. Rupen and D. A. Frail (NRAO) report on behalf of a larger
collaboration:

"Using the VLA at 8.5 GHz we imaged a 60-arcsec region centered on the
Chandra position for SGR 1806-20 (Kaplan et al., ApJ 564, 935, 2002).
This short 9 min integration was made on 2003 September 3.15 UT,
concurrent with a planned 240 ksec INTEGRAL target of opportunity
observation (GCN#2372). No radio source was detected at or near this
position. The rms noise was 55 microJy/beam, for a beam size of
450 x 240 mas (p.a. 12 degrees). The min/max within the Chandra
0.3 arcsec error circle were (-121,+153) microJy/beam. No further
observations are planned."


////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2377
SUBJECT: IBAS detection of bursts from SGR 1806-20 
DATE:    03/09/04 16:49:09 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@mi.iasf.cnr.it>

S.Mereghetti (IASF, Milano), D.Gotz (IASF, Milano) for the ISDC IBAS
Localization Team

and

K.Hurley, on behalf of the INTEGRAL SGR TOO collaboration, report


During INTEGRAL TOO observations of the region of SGR 1806-20, performed
from 2003 September 3 22:45 UT to September 4 02:54 UT, two bursts have
been detected and localized by IBAS.

The first burst occurred on September 4 at 00:53:43.9 UT at coordinates
R.A. = 18 08 43.6 Dec.= -20 23 28 (J2000).

The second one occurred at 01:15:56.9 UT at coordinates R.A. = 18 08 34.3
Dec.= -20 26 25.

These localizations have an uncertainty of about 3 arcmin. Therefore the
bursts can be confidently associated with SGR 1806-20 and not with
SGR 1808-20 (GCN 2351).

Both bursts were detected with IBIS/ISGRI in the 15-100 keV range and had
a duration of about 200 ms. Their fluences in the 25-100 keV range were
about 2x10-9 ergs cm-2 and 2x10-8 ergs cm-2.

The TOO INTEGRAL observation of this region (GCN 2372) will continue until
September 7 at 03:05 UT.

Continued ground-based observations of this region are encouraged.

This message can be cited.



////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2408
SUBJECT: A burst from SGR 1806-20 detected with IBAS
DATE:    03/10/07 08:19:08 GMT
FROM:    Diego Gotz at IASF-CNR  <diego@mi.iasf.cnr.it>

D.Gotz (IASF, Milano), S. Mereghetti (IASF, Milano) and M. Beck (ISDC) for
the ISDC IBAS Localization Team

and

F. Mirabel (CEA, Saclay) and the INTEGRAL Science Working Team report

During INTEGRAL Galactic Center Deep Exposure a burst originating from SGR
1806-20 has been detected and localized with IBAS at 18:51:27.41 on
October 6 2003.

The burst was detected with IBIS/ISGRI in the 15-100 keV range and has
a duration of about 60 ms.

The fluence in the 25-100 keV energy band is about 3x10-8 ergs cm-2.

This message can be cited.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2414
SUBJECT: IPN detection of continued activity from SGR1806-20
DATE:    03/10/09 00:02:33 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@sunspot.ssl.berkeley.edu>

K. Hurley and T. Cline, on behalf of the Ulysses and Konus GRB teams,
and

E. Mazets and S. Golenetskii, on behalf of the Konus-Wind GRB team,
report:

Ulysses and Konus-Wind observed this event at 12424 seconds on October
08.  As observed by Ulysses, it had a duration of approximately  0.1
seconds, a 25-100 keV fluence of approximately  1.2E-06 erg/cm2, and a
peak flux of approximately  1.8E-05 erg/cm2 s over 0.03125 seconds.
It was followed approximately 50 seconds later by a second event
with roughly one-third the intensity.

We have triangulated it to a preliminary annulus centered  at RA,
Decl(2000)= 347.828, -18.495 degrees, whose radius is 70.687 +/-  0.010
degrees (3 sigma).

The center line of this annulus passes 0.001 degrees from the position
of SGR1806-20, and 0.117 degrees from the position of the AXP XTE
J1810-197, excluding the latter as a possible source.  This burst
probably originated from SGR1806-20, but we note that the annulus also
intersects the error circle of the possible new SGR1808-20.

This localization may be improved.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2415
SUBJECT: SGR 1806-20 bursts with INTEGRAL and IBAS announcement on Soft Gamma-Ray Repeaters
DATE:    03/10/09 08:29:46 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@mi.iasf.cnr.it>

S. Mereghetti, D.Gotz (IASF, Milano)  and M. Beck (ISDC) for the ISDC IBAS
Localization Team, F. Mirabel (CEA, Saclay)  and the INTEGRAL Science
Working Team report:

During INTEGRAL Core Program observations of the Galactic Center region,
IBAS has detected several bursts from SGR 1806-20. They are summarized in
the following Table.

The positions derived by IBAS with typical errors smaller than 3 arcmin
confirm that all of them originated from SGR 1806-20 and not from the
nearby sources SGR 1808-20 (GCN 2351)  or XTE J1810-197 (IAUC 8168, IAUC
8190).

The bursts were detected with the IBIS/ISGRI instrument in the 15-100 keV
energy range.


Date October 2003      	25-100 keV Fluence      Duration
Day      UT              (erg cm-2)               (s)

6    18:51:27.4           3 x 10-8                0.06      GCN 2408
8    03:27:03.9           4 x 10-7                0.2       (*)
8    03:27:56.1           3 x 10-7		  0.2       (*)
8    20:22:06.5           4 x 10-8                0.1

(*) IPN observations of this burst have been reported (GCN 2414)


In the near future IBAS will start to distribute automatic Alert Packets
for SGR bursts detected with high significance.  This will allow rapid
follow-up observations at other wavelengths.  The source coordinates in
the Alert Packets will allow IBAS users to distinguish such events from
classical GRBs.

This message can be cited.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2419
SUBJECT: Ongoing Bursting Activity from SGR 1806-20 detected with IBAS
DATE:    03/10/15 12:46:32 GMT
FROM:    Diego Gotz at IASF-CNR  <diego@mi.iasf.cnr.it>

D. Gotz, S. Mereghetti (IASF, Milano) and M. Beck (ISDC) for the ISDC IBAS
Localization Team, F. Mirabel (CEA, Saclay)  and the INTEGRAL Science
Working Team report:

Several more bursts from SGR 1806-20 have been detected by IBAS during
INTEGRAL Core Program Galactic Center Deep Exposure. Their times,
preliminary fluences and durations are summarized in the following table.

The positions of the bursts are all consistent with SGR 1806-20 within 2
arcmin.

The bursts were detected with the IBIS/ISGRI instrument in the 15-100 keV
energy range.


Date October 2003       25-100 keV Fluence      Duration
Day      UT               (erg cm-2)              (s)

11    01:26:27.07         1.0 x 10-8              0.1
14    14:31:45.41	  2.0 x 10-8		  0.1
15    02:35:19.66	  2.0 x 10-8	          0.1
15    04:55:00.88	  2.0 x 10-7		  0.18
15    07:37:47.57         3.0 x 10-8              0.1 (*)
15    07:55:52.97         1.5 x 10-8		  0.1
15    07:56:21.07	  1.0 x 10-8		  2 x 0.1 (**)
15    10:19:31.94         4.0 x 10-8		  0.13
15    11:00:28.77         4.0 x 10-8              0.15
15    11:17:05.32	  2.0 x 10-8		  0.2

(*) This burst is preceeded by a small precursor lasting ~0.05 s

(**) This burst consists of two distinct peaks, lasting ~0.1 s each,
separated by ~0.2 s. The fluence given is for the first one. The second is
has a smaller peak flux, but is harder.

This message can be cited.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2451
SUBJECT: IPN detection of activity from SGR1806-20
DATE:    03/11/18 18:02:21 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@sunspot.ssl.berkeley.edu>

K. Hurley and T. Cline, on behalf of the Ulysses, Konus, and Mars
Odyssey GRB teams,

E. Mazets and S. Golenetskii, on behalf of the Konus-Wind GRB team,

I. Mitrofanov, S. Charyshnikov, V. Grinkov, A. Kozyrev, M. Litvak, and
A. Sanin, on behalf of the HEND-Odyssey GRB team, and

W. Boynton, C. Fellows, K. Harshman, C. Shinohara and R. Starr, on
behalf of the GRS/Odyssey GRB team, report:

Konus-Wind and Mars Odyssey-HEND  observed this GRB at 26660 seconds on
14 November 2003.  As observed by Konus, it had a duration of
approximately 1.4 seconds, an 18-200 keV fluence of approximately
3.6E+-05 erg/cm2, and a peak flux of approximately 6.3E-05 erg/cm2 s.

We have triangulated it to a preliminary annulus centered at RA, Decl
(2000) =  344.192, -8.447 degrees, whose radius is 70.299 +/-  0.036
degrees (3 sigma).   As the center line of this annulus passes 0.009
degrees from the position of SGR1806-20, and 0.092 degrees from the
center of the error circle of SGR1808-20, we conclude that the origin
of this burst was most likely SGR1806-20.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2504
SUBJECT: IPN triangulation of an intermediate burst from SGR1806-20
DATE:    04/01/01 21:01:07 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@sunspot.ssl.berkeley.edu>

K. Hurley and T. Cline, on behalf of the Ulysses, Mars Odyssey, and
Konus GRB teams,

S. Golenetskii, E. Mazets, V. Pal'shin, and D. Frederiks on behalf of
the Konus-Wind and Helicon/Coronas-F teams,

I. Mitrofanov, S. Charyshnikov, V. Grinkov, A. Kozyrev, M. Litvak, and
A. Sanin, on behalf of the HEND-Odyssey GRB team,

W. Boynton, C. Fellows, K. Harshman, C. Shinohara and R. Starr, on
behalf of the GRS-Odyssey GRB team, and

D. M. Smith, R. P. Lin, J. McTiernan, R. Schwartz, C. Wigger, W.
Hajdas, and A. Zehnder, on behalf of the RHESSI GRB team, report:

Konus-Wind, Helicon, Mars Odyssey - HEND, and RHESSI observed this
burst at 60913 s on 28 December 2003.  As observed by Konus, its
duration was 1.1s, its 15-200 keV fluence was 3x10^(-5) erg/cm2, and
its peak flux was 8.6x10^(-5) erg/cm2 s.  It had a soft spectrum, with
kT=20 keV.

Using Konus and Odyssey data, we have triangulated it to a preliminary
annulus centered at RA, Decl(2000)=186.046, -2.629 degrees, whose
radius is 85.436 +/- 0.028 degrees (3 sigma).  As the centerline of
this annulus passes 0.011 degrees from the position of SGR1806-20, we
believe that this event is an intermediate burst from that source.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2541
SUBJECT: INTEGRAL detection of activity from SGR1806-20
DATE:    04/03/09 11:03:32 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@mi.iasf.cnr.it>

S Mereghetti, D.Gotz, M. Beck and J.Borkowski on behalf of the IBAS
Localization Team, S.Shaw and K.Pottschmidt on behalf of the INTEGRAL
Science Data Centre and F.Mirabel on behalf the INTEGRAL Science Working
Team report:

The IBAS alert n.1563 corresponds to a short burst (0.2 seconds)  with
preliminary position within 1 arcminutes from the soft gamma-ray repeater
SGR1806-20.

Further off-line data analysis is in progress.

This message is citeable.


////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2542
SUBJECT: IBAS results on a burst from SGR1806-20
DATE:    04/03/09 11:50:46 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@mi.iasf.cnr.it>

D. Gotz, S. Mereghetti (IASF, Milano) for the ISDC IBAS Localization Team,
F. Mirabel (CEA, Saclay)  and the INTEGRAL Science Working Team report:

We confirm that the burst of IBAS alert n.1563 (GCN 2541) originated from
SGR1806-20.

The burst was detected with the IBIS/ISGRI instrument in the 15-100 keV
energy range, during the INTEGRAL Core Program Galactic Center Deep
Exposure, at 10:24:08.35 UT of March 9.

The preliminary estimate of the burst fluence in the 15-100 keV energy
range is 2.2 x 10-7 erg cm-2.

We remind that IBAS is also distributing real time Alert Packets for
bursts from known SGR positions (see ISDC Newsletter n. 14
http://isdc.unige.ch/Newsletter/N/#ibas and GCN 2415).

SGR 1806-20 will be in the INTEGRAL field of view for various time
intervals in the next few days, thus possibly giving rise to other IBAS
alerts.

This message can be cited.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2558
SUBJECT: Summary of recent bursts from SGR 1806-20 detected by INTEGRAL
DATE:    04/03/31 15:13:38 GMT
FROM:    Diego Gotz at IASF-CNR  <diego@mi.iasf.cnr.it>

D. Gotz, S. Mereghetti (IASF, Milano), M. Beck (ISDC) on behalf of the
IBAS Localization Team, N. Mowlavi and S. Shaw on behalf of the INTEGRAL
Science Data Centre and the INTEGRAL Science Working Team report:

SGR 1806-20 has been moderately active after the burst of March 9 (Gotz et
al. GCN 2542). The times of the bursts discovered with IBAS in the
IBIS/ISGRI data are the following:

Start time (UT)			IBAS Alert Number
--------------------------------------------------
2004-03-09T10:24:08.35		1563     (GCN 2541, 2542)
2004-03-16T13:02:06.43		1677
2004-03-20T06:34:35.05		1685
2004-03-20T17:57:01.83		*
2004-03-29T06:15:40.97		*
2004-03-29T11:46:47.50		*
2004-03-30T17:03:05.81          1716,1717

(*) These bursts have been detected with significance below the threshold
for automatic delivery of IBAS Alert Packets

The burst of March 30 was among the brightest detected by INTEGRAL from
this Soft Gamma-Ray Repeater. It consisted of a main peak lasting about
0.11 s, followed by a smaller peak 0.1 s later. The fluence of the main
peak was about 3 x 10-7 erg cm-2 (15-100 keV).

This message can be cited.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2603
SUBJECT: IPN triangulation of an intense intermediate burst from SGR1806-20
DATE:    04/05/21 20:13:06 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@sunspot.ssl.berkeley.edu>

K. Hurley and T. Cline, on behalf of the Ulysses and Konus GRB teams,

E. Mazets and S. Golenetskii, on behalf of the Konus-Wind GRB team, and

D. M. Smith, R. P. Lin, J. McTiernan, R. Schwartz, C. Wigger, W.
Hajdas, and A. Zehnder, on behalf of the RHESSI GRB team, report:

Konus and RHESSI observed this soft-spectrum burst at 72247 s on May 19
2004.  Ulysses was off.  Its duration was 1.3 s, its fluence was ~2.8 x
10^-5 erg/cm^2, and its peak flux was ~3.3 x 10^-5 erg/cm^2 s.  We have
triangulated it to an annulus centered at RA, Decl(2000)=250.249,
-19.744 degrees, whose radius is 20.792  +/-  2.019 degrees.  As the
center line of this annulus passes only 0.2 degrees from the position
of SGR1806-20, we believe that it is the source of this event.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2604
SUBJECT: Activivty of SGR 1806-20
DATE:    04/05/28 13:46:43 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks
on behalf of Konus-Wind and Helicon/Coronas-F teams,

T. Cline on behalf of the Konus-Wind team, and

A. Rau, A. von Kienlin, G. Lichti on behalf of the INTEGRAL SPI-ACS
GRB team report:

Recently, Konus-Wind has detected seven SGR-like bursts
in the trigger mode:

  Date   Time,     Duration,   Fluence,       Peak Flux,           kT****
         s UT          s      (20-200 keV)   (20-200 keV)          keV
                              ergs/cm2       ergs/cm2 s
-----------------------------------------------------------------------
040427   47089.452  0.176  (3.43 +/- 0.07)E-6 (2.58 +/- 0.22)E-5 19+/-3

040519*  72250.485  1.376  (2.74 +/- 0.02)E-5 (3.19 +/- 0.09)E-5 21+/-2

040522** 31696.702  0.176  (2.16 +/- 0.06)E-6 (2.82 +/- 0.17)E-5 16+/-5

040522   45772.875  0.136  (1.33 +/- 0.04)E-6 (1.59 +/- 0.12)E-5 25+/-6

040523   50502.964  0.552  (4.32 +/- 0.09)E-6 (2.94 +/- 0.14)E-5 16+/-5

040525*** 12976.933 0.592  (8.74 +/- 0.12)E-6 (3.06 +/- 0.11)E-5 23+/-4

040526   29173.030  0.752  (5.88 +/- 0.11)E-6 (1.41 +/- 0.09)E-5 16+/-5
------------------------------------------------------------------------
*   - this burst was localized, the most like source
       of the burst is SGR 1806-20 (GCN 2603).
**  - this burst was also detected by Helicon-Coronas-F in the
       background mode. Estimated time delay is consistent with
       SGR 1806-20 position.
*** - this burst was also detected by INTEGRAL SPI-ACS.
       We have triangulated it to an annulus centered at
       RA(2000) = 259.389 deg, Decl(2000) = -17.958 deg,
       whose radius is 12.616 +/- 1.770 deg (3 sigma).
       The center line of this annulus passes 0.4 degrees from
       the position of SGR 1806-20.
**** - the last column contains the values of spectral parameter kT
        for the OTTB spectral model: dN/dE ~ E^{-1} exp(-E/kT)


Additionally, a number of SGR-like bursts (short and soft)
were detected by both Konus detectors S1 and S2
in the background mode:

  Date      Time,
         s UT  (hh:mm:ss)
---------------------------
040519  25976 (07:12:56)
040519  86378 (23:59:38)
040520  44823 (12:27:03)
040522   2693 (00:44:53)
040522  30582 (08:29:42)
040522  80762 (22:26:02)
040522  83738 (23:15:38)
040523  18673 (05:11:13)
040523  39091 (10:51:31)
040523  40937 (11:22:17)
040523  65789 (18:16:29)

The Konus ecliptic latitude response indicates
that the source of the bursts is near ecliptic plane.

All these data lead to the supposal
that the all these bursts originated from SGR 1806-20,
which, hereby, has entered a new phase of activity
in the hard X-ray.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2607
SUBJECT: SGR 1806-20, potential NIR counterpart
DATE:    04/06/08 11:56:28 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

C. Kouveliotou (NASA/MSFC),
S. Klose (Thuringer Landessternwarte Tautenburg),
S. Wachter (Spitzer Science Center),
P. Woods (USRA, NASA/MSFC),
S. Patel (USRA, NASA/MSFC),
J. Greiner (MPE Garching),
B. Stecklum (Thuringer Landessternwarte Tautenburg), and
M. van der Klis (University of Amsterdam)


report:


Following the recent activiation in X-rays of SGR 1806-20, we
triggered a Target of Opportunity Observation of the source at ESO
with VLT/ISAAC. Observations were performed in the Ks band on May 28,
6:24 UT - 6:50 UT. Altogether 14 images were taken, 1 min integrated
exposure time each. For the final data analysis we used those images
with the best seeing (8 of the 14 images).

Within the 0.7 arcsec Chandra error circle as reported by Eikenberry
et al. (ApJ 563, L133; their figure 3d), we identify an isolated point
source with Ks = 19.6 +/- 0.4. This source might match the position of
source 'B' in Eikenberry et al., while their source 'A', which is at the
edge of the Chandra error circle, is resolved into at least two
components. We tentatively identify either object B or the second
component of object A as the potential K-band counterpart of SGR 1806-20.
However, further observations are needed during quiescence of the SGR to
determine whether one of the two sources is variable in order to firmly
establish a connection with SGR 1806-20.

We are deebly indebted the ESO staff at Paranal, in particular Poshak
Gandhi, for performing the observations.


This message can be cited.


////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2609
SUBJECT: SGR 1806-20: no IR variability of the proposed counterparts
DATE:    04/06/09 17:33:11 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <covino@merate.mi.astro.it>

G.L. Israel, R. Mignani, S. Covino, S. Campana, L. Stella, N. Rea, V.
Testa, G. Marconi on behalf of a larger team
    
report:
     
We have imaged in J, H and Ks bands with VLT/NACO the field of SGR
1806-20 on March 9th, 10th, 16th and 17th 2004. Observations were
activated after the X-ray burst that occurred on March 9th (Mereghetti
et al., GCN 2541). We have detected several sources within the Chandra
error circle reported in Eikenberry et al. 2001 (ApJ 563, L133)
including those reported in GCN 2607 (Kouveliotou et al.). 
         
The monitoring of these objects did not show any variability more
significant than 2sigma in the Ks band on time scales from hours up to
days. The limiting Ks magnitude was about 21.5.
         
Both the lack of IR variability correlated to the X-ray burst activity
and the relatively high IR flux for the proposed counterparts (GCN 2607)
suggest that these objects are unlikely the IR counterpart to SGR
1806-20. 
          

This message can be cited.



////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2633
SUBJECT: Ongoing activity of SGR 1806-20
DATE:    04/07/29 17:31:04 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks
on behalf of Konus-Wind and Helicon/Coronas-F teams,

T. Cline on behalf of the Konus-Wind team, and

A. Rau, A. von Kienlin, G. Lichti on behalf of the INTEGRAL SPI-ACS
GRB team report:

Since last SGR burst 040615, listed in GCN 2611,
Konus-Wind has detected seven SGR-like bursts
in the trigger mode:

   Date   Time,     Duration,   Fluence,       Peak Flux,           kT*
          s UT          s      (20-200 keV)   (20-200 keV)          keV
                               ergs/cm2       ergs/cm2 s
-----------------------------------------------------------------------
040617   48377.157  0.104  (1.16 +/- 0.04)E-6 (2.28 +/- 0.14)E-5 23+/-3

040622   70209.587  0.332  (5.49 +/- 0.09)E-6 (3.59 +/- 0.18)E-5 17+/-1

040623   81361.257  0.440  (2.49 +/- 0.07)E-6 (1.74 +/- 0.13)E-5 17+/-2

040707   17546.478  0.696  (7.65 +/- 0.12)E-6 (1.86 +/- 0.10)E-5 18+/-1

040719   45188.316  0.264  (3.81 +/- 0.07)E-6 (2.44 +/- 0.21)E-5 20+/-2

040723   42259.178  0.192  (7.51 +/- 0.11)E-6 (5.63 +/- 0.19)E-5 20+/-1

040728     544.709  0.328  (4.36 +/- 0.09)E-6 (2.64 +/- 0.13)E-5 15+/-2
------------------------------------------------------------------------
* - the last column contains the values of spectral parameter kT
         for the OTTB spectral model: dN/dE ~ E^{-1} exp(-E/kT)

The last burst was also detected by INTEGRAL SPI-ACS at 539.761 s UT.
We have triangulated it to an annulus centered at
RA(2000) = 302.741 deg, Decl(2000) = -19.181 deg,
whose radius is 28.900 +/- 0.478 deg (3 sigma).
As the center line of this annulus passes 0.14 degrees from
the position of SGR 1806-20, we believe that it is the source of this
event.

The Konus ecliptic latitude response indicates
that the source of the remaining bursts is near ecliptic plane,
so we suppose, that they are also originated from SGR 1806-20.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2647
SUBJECT: Bursting activity from SGR 1806-20 detected with IBAS
DATE:    04/08/17 09:51:38 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@mi.iasf.cnr.it>

S. Mereghetti, D.Gotz (IASF, Milano), N. Mowlavi, S. Shaw (ISDC),
and K.Hurley (UCB/SSL) report:

Two weak bursts from SGR 1806-20 have been detected with the IBIS/ISGRI
instrument at UT 04:56:19.3 and 05:59:51.3 of 2004 Aug 17.

Both bursts lasted 0.1 s and had a fluence of about 1.5x10-8 erg cm-2
(15-100 keV).

They had significance below the threshold for automatic delivery of IBAS
Alert Packets.
INTEGRAL will continue to observe SGR 1806-20 until 03:10 UT of Aug 19.
If stronger bursts from this source are detected, automatic Alert Packets
will be distributed in real time (expected delay of 10-20 s)

This message can be cited.


////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2665
SUBJECT: Increase of SGR 1806-20 activity
DATE:    04/08/26 15:19:46 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks
on behalf of Konus-Wind and Helicon/Coronas-F teams,

T. Cline on behalf of the Konus-Wind team, and

A. Rau, A. von Kienlin, G. Lichti on behalf of the INTEGRAL SPI-ACS
GRB team report:


Recently the increase of bursting activity from SGR 1806-20
was detected by Konus-Wind, INTEGRAL SPI-ACS, and Helicon-Coronas-F.

Konus-Wind has detected 7 bursts in the trigger mode and 5 bursts
in the background mode.
Additional SGR-like burst was detected by Helicon-Coronas-F in
the background mode and triggered INTEGRAL SPI-ACS
(the burst was missed by Konus-Wind due to data read out).

The most recent burst detected on August 25 at 85512.611 s UT
is the brightest burst ever observed by Konus-Wind from SGR 1806-20.

The following table summarizes the bursts:


Date     Time*,     Duration,   Fluence,       Peak Flux,  Observed by**
           s UT          s      (20-200 keV)   (20-200 keV)
                                ergs/cm2       ergs/cm2 s
-----------------------------------------------------------------------
040814   45466.575  0.18         1.6E-6        2.1E-5       K(tr)

040819   22636.891  0.80         1.4E-5        2.5E-5       K(tr)

040820   71208.277  0.06         9.4E-7        3.1E-5       K(tr)

040821   35217      <3           1.7E-6          -          K(bg), I

040821   61297.013  0.22         2.5E-6        2.0E-5       K(tr), I

040822    9646      <3           5.0E-7          -          K(bg)

040823   22462      <3           8.0E-7          -          K(bg)

040823   36755      <3           5.0E-7          -          K(bg)

040823   40994.643  0.14         1.5E-6        4.5E-5       K(tr)

040823   48073.891  0.70         1.0E-5        4.2E-5   K(tr), I, H(bg)

040823   48363      <2           3.2E-6          -          I, H(bg)

040823   58681      <3           6.0E-7          -          K(bg)

040825   85512.611  1.10         2.1E-5        7.0E-5       K(tr), I
------------------------------------------------------------------------
*  - Konus-Wind (or Helicon) time is given
** - the last column contains the s/c which observed this burst:
     K - Konus-Wind, I - INTEGRAL SPI-ACS,
     H - Helicon-Coronas-F. For Konus and Helicon in the brackets
     the observation mode is given: tr - trigger, bg - background.


The Konus-INTEGRAL annuli for 3 bursts are:

  Date   Time,          Center           Radius
         s UT        RA       DEC   and its uncertainty (3sigma)
		    deg      deg	 deg						
----------------------------------------------------
040821  61297.013  310.141 -16.864   35.724+/-0.678

040823  48073.891  311.668 -14.712   37.647+/-0.762

040825  85512.611  314.503 -14.941   40.588+/-0.454


Because all these annuli pass through the position of SGR 1806-20,
we believe that it is the source of these events.

The Konus ecliptic latitude response indicates
that the source of the remaining bursts (except the missed one)
is near ecliptic plane, so we suppose,
that they are also originated from SGR 1806-20.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2693
SUBJECT: Very bright burst detected from SGR 1806-20
DATE:    04/09/04 09:25:41 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks,
and T. Cline on behalf of Konus-Wind team,

G. Ricker, J-L Atteia, N. Kawai, D. Lamb, S. Woosley, J. Doty, R.
Vanderspek, J. Villasenor, G. Crew, N. Butler, J.G.  Jernigan, F.
Martel, G. Prigozhin, A. Dullighan, J. Braga, R.  Manchanda, G.
Pizzichini, Y.  Shirasaki, C. Graziani, M. Matsuoka, T.  Tamagawa, T.
Sakamoto, A.  Yoshida, E. Fenimore, M. Galassi, T.  Donaghy, C.
Barraud, M. Boer, J-F Olive, and J-P Dezalay, on behalf of the HETE GRB
team, and

K. Hurley on behalf of the IPN team report:

A very bright SGR burst was detected by Konus-Wind on August 28
at 42581.338 s UT.
This burst also triggered HETE at 42569.952 s UT (H3514).
We have triangulated it to an annulus centered at
RA(2000) = 317.135 deg, Decl(2000) = -17.624 deg,
whose radius is 42.448 +/- 1.601 deg (3 sigma).
As this annulus includes the position of SGR 1806-20
and Konus ecliptic latitude response indicates
that the burst source lays near ecliptic plane,
we believe that SGR 1806-20 is the source of this event.

As observed by Konus-Wind, the burst had a duration of 0.7 s, a
fluence  ~4.0x10^-5 erg/cm^2, and  a peak flux ~1x10^-4 erg/cm^2 s
(both in 20-200 keV range).

The value of the spectral parameter kT for an OTTB spectral model
(dN/dE ~ E^{-1} exp(-E/kT)) was 26 keV.

This burst is the brightest one from this SGR detected
so far by Konus-Wind. It is stronger, than the burst on 040825
(GCN 2665) by a factor of about 1.7 in fluence
and peak flux.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2706
SUBJECT: An intense burst from SGR1806-20
DATE:    04/09/13 11:41:23 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks
on behalf of Konus-Wind and Helicon/Coronas-F teams,

T. Cline on behalf of the Konus-Wind team, and

A. Rau, A. von Kienlin, G. Lichti on behalf of the INTEGRAL SPI-ACS
GRB team report:

An intense SGR-like burst was detected by Konus-Wind on September 10
at 35441.919 s (09:50:41.919) UT and
Helicon-Coronas-F at 35438.674 s (09:50.38.674) UT.
We have triangulated it to an annulus centered at
RA(2000) = 325.353 deg, Decl(2000) = -13.289 deg,
whose radius is 51.241 +/- 0.156 deg (3 sigma).

This burst was also observed by Integral SPI-ACS.
The Konus-Wind - INTEGRAL triangulation annulus is:
RA(2000) = 322.942 deg,
Decl(2000) = -8.645 deg,
Radius = 50.227 +/- 0.328 degrees (3 sigma).

These annuli intersect to form two error boxes,
one of which may be eliminated by the Konus
ecliptic latitude response. The remaining error
box includes the position of SGR 1806-20,
so we believe that it is the source of this event.

Additionaly, two SGR-like bursts were detected recently by Konus-Wind.
The Konus ecliptic latitude response indicates
that the source of these bursts is near ecliptic plane, so we suppose,
that they are also originated from SGR 1806-20.


The following table summarizes the bursts
(as observed by Konus-Wind):

Date     Time*,     Duration,   Fluence,       Peak Flux,
           s UT          s      (20-200 keV)   (20-200 keV)
                                ergs/cm2       ergs/cm2 s
-----------------------------------------------------------------------
040830  23313.143  0.14         2.4E-6        3.6E-5

040908  45466.575  0.33         8.3E-6        5.0E-5

040910  35441.919  0.58         1.7E-5        4.6E-5
------------------------------------------------------------------------

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2760
SUBJECT: SGR 1806-20 still active
DATE:    04/10/04 09:46:14 GMT
FROM:    Diego Gotz at IASF-CNR  <diego@mi.iasf.cnr.it>

D. Gotz, S. Mereghetti (IASF-Milano) and F. Mirabel (SAP, Saclay) report:

The soft repeater SGR 1806-20 continues to be in an active bursting state.
Six bursts have been detected by IBAS during INTEGRAL Galactic Center Core
Program observations, performed between September 30 and October 2, 2004.

Burst times, approximate durations, and fluences (15-100 keV) are reported
below:

Time UT				Duration (s)	Fluence (erg cm-2)

2004-09-30T13:03:42.07		0.3		4.0E-8
2004-10-01T06:03:29.81		0.2		5.0E-8
2004-10-01T18:45:53.28		0.1		4.5E-8
2004-10-01T22:03:13.29		0.1		1.2E-7
2004-10-02T02:47:29.10		0.15		1.5E-7
2004-10-02T10:10:26.96		0.2		4.5E-7


Being the source very active, IBAS Alert messages regarding SGR 1806-20
are still disabled.

This message can be cited.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2763
SUBJECT: Very strong outburst from SGR 1806-20 detected with INTEGRAL
DATE:    04/10/05 14:49:51 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@mi.iasf.cnr.it>

S. Mereghetti, D. Gotz (IASF-Milano), J.Borkowski (CAMK-Torun), M.Beck
(ISDC-Versoix) on behalf of the IBAS Localization Team and F.I.Mirabel
(SAp-Saclay) on behalf of the INTEGRAL Science Working Team report:

A strong increase in the activity of SGR 1806-20 has been detcted by IBAS
starting at 13:57 UT of October 5.  The activity consists of an
approximately 6 min long, multipeaked outburst, followed by a few shorter
bursts.

During the peaks of the long outburst the counting rate in the IBIS/ISGRI
detector saturates the available telemetry.

Analysis is in progress to estimate the  event fluence and spectrum.

Rapid observations at other wavelengths are encouraged.

This message can be cited.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2764
SUBJECT: Bursts from SGR 1806-20: Preliminary INTEGRAL results
DATE:    04/10/05 16:17:17 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@mi.iasf.cnr.it>

D. Gotz, S. Mereghetti (IASF-Milano), F.I Mirabel (SAp-Saclay) report:

The activity from SGR 1806-20 reported in GCN Circ. 2763 consists of at
least two main bursts whose peak flux and detailed temporal structure
are uncertain due to satellite telemetry saturation. Both are detected up
to at least 200 keV in the IBIS/ISGRI instrument.

The first burst starts at 13:56:43 UT and lasts about 20 s.
Its spectrum over the 15-200 keV range is well fit by an Optically Thin
Thermal Bremsstrahlung model with temperature kT = 45+/-3 keV.
A preliminary analysis gives a lower limit on its fluence of about 1.e-5
erg/cm2 (15-100 keV).

The second burst starts at 13:59:33 UT and lasts about 40 s.
Its OTTB temperature is  kT = 57+/-3 keV and the preliminary
lower limit on its fluence is  2.e-5 erg/cm2 (15-100 keV).

This message can be cited.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2823
SUBJECT: Bright bursts from SGR1806-20
DATE:    04/10/19 13:27:31 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks
on behalf of Konus-Wind and Helicon/Coronas-F teams,

T. Cline on behalf of the Konus-Wind team, and

A. Rau, A. von Kienlin, G. Lichti on behalf of the INTEGRAL SPI-ACS
GRB team report:

Two bright SGR-like events were detected by Konus-Wind on
October 16 at 66284.062s UT and October 17 at 23771.551s UT.

Both events were also detected by INTEGRAL SPI-ACS,
Wind-INTEGRAL triangulation gives the following annuli:

The first event:
Alpha = 191.74323
Delta =-17.37563
Radius = 75.32431 +/-0.37658
The annulus passes 0.021 deg (0.17 sigma) from SGR 1806-20.

The second event:
Alpha = 191.85595
Delta =-16.48234
Radius = 75.45488 +/- 0.27746
The annulus passes 0.053 deg (0.57 sigma) from SGR 1806-20.

According to the Konus-Wind data the first event on 041016 had
a duration of 0.12 sec, fluence 6.4x10-6 erg cm-2, and peak flux
8.5x10-5 erg cm-2 s-1, both in 20-200 keV range.
OTTB fit gives parameter kT = 26.5 +/- 1.5 keV

The 041017 event had a duration of main pulse of 1.6 sec,
fluence 6.5x10-5 erg cm-2, and peak flux 6.7x10-5 erg cm-2 s-1, both in 
20-200 keV range. A considerable spectral evolution was observed,
OTTB fit gives the following values of kT during event:
------------------------------------
Time after trigger          kT
       sec                   keV
------------------------------------
0 - 0.256s              24.1 +/- 0.5
0.256 - 0.768s          20.4 +/- 0.5
0.768 - 1.6s            17.5 +/- 0.7
------------------------------------

Following the main pulse there were two weaker events
(times are given after the trigger), at +11.287 s (fluence ~2x10-7 erg
cm-2) and at +157.2s (fluence ~4.5x10-7 erg cm-2).

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2831
SUBJECT: Summary of the recent bursts from SGR 1806-20
DATE:    04/11/04 14:12:33 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks
on behalf of Konus-Wind and Helicon/Coronas-F teams,

T. Cline on behalf of the Konus-Wind team, and

A. Rau, A. von Kienlin, G. Lichti on behalf of the INTEGRAL SPI-ACS
GRB team report:


SGR 1806-20 remains in the active state. Since the last SGR burst
041017, listed in GCN 2823, Konus-Wind and Helicon-Coronas-F have
detected seven SGR-like bursts in the trigger mode. Two of them were
also detected by INTEGRAL SPI-ACS.

The most recent intense SGR burst was detected by Helicon-Coronas-F
today (041104) at 04:17:08.929 UT. Konus-Wind data aren't available
yet.

The following table summarizes the bursts:

Date      Time,    Instr*  Duration,   Fluence,     Peak Flux,   kT**
           s UT                s      (20-200 keV)  (20-200 keV)  keV
                                       ergs/cm2      ergs/cm2 s
-----------------------------------------------------------------------
041026    76305.409  K     0.54      3.0E-6        2.4E-5     21.4+/-1.2

041027    35196.737  K     0.55      5.0E-6        2.6E-5     18.6+/-1.1

041029    22099.384  K     0.16      2.5e-6        3.4E-5     17.7+/-1.3

041031(a) 57535.834  H     0.056     4.7e-7        1.2e-5     17.8+/-1.6

041031    61900.552  K, I  0.70      1.2e-5        4.4e-5     18.9+/-0.6

041102(b) 26875.713  K     0.19      1.1e-5        9.9e-5     22.6+/-1.2

041104(c) 15428.929  H, I  1.6       1.9e-5        2.0e-5     21.8+/-0.5
------------------------------------------------------------------------
*  -   the intrument, which detected the burst:
        K   = Konus-Wind
        H   = Helicon-Coronas-F
        I   = INTEGRAL SPI-ACS

**  -  the last column contains the values of spectral parameter kT
        for the OTTB spectral model: dN/dE ~ E^{-1} exp(-E/kT)

(a) -  this burst was also observed by Konus-Wind in the
        background mode. Estimated time delay is consistent with
        SGR 1806-20 position.
(b) -  this burst was also observed by Helicon-Coronas-F in the
        background mode. Estimated time delay is consistent with
        SGR 1806-20 position.
(c) -  We have triangulated it to Coronas-INTEGRAL annulus centered at
        RA(2000) = 225.846 deg, Decl(2000) = 44.432 deg,
        whose radius is 77.4  4.0 deg (3 sigma).
        The center line of this annulus passes 0.02 degrees from
        the position of SGR 1806-20.

The Konus-Wind ecliptic latitude response indicates
that the source of the remaining bursts is near ecliptic plane,
so we suppose, that they are also originated from SGR 1806-20.

The peak flux of the burst on 041102 was nearly the same as
the peak flux of the brighest burst  detected by Konus-Wind
from SGR 1806-20 on 040828 (GCN 2693).

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2896
SUBJECT: Very high activity of SGR 1806-20
DATE:    04/12/22 16:57:06 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks and
T. Cline on behalf of the Konus-Wind team, report:

During 21 December more than 30 SGR-like bursts
were detected by Konus-Wind and Helicon-Coronas-F
with peak fluxes varied from 5e-7 to 8e-5 erg /cm2 s.
The time interval between bursts varied from seconds to hours.

The triangulation of several these bursts
indicated that their origin is SGR 1806-20.

This is the second series of bursts from this source.
The previous one was detected on 5 October (GCN 2769).
Now we have the data till 01:28 UT December 22.
The last burst is seen at 00:50:52 s UT in
the Helicon background data.

Details on triangulation and the full list of bursts
with their characteristics will be given later.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2920
SUBJECT: Giant flare from SGR 1806-20 detected by INTEGRAL
DATE:    04/12/29 11:19:07 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@mi.iasf.cnr.it>

J.Borkowski (CAMK, Torun), D. Gotz, S. Mereghetti (IASF, Milano),
N.Mowlavi, S.Shaw, M.Turler (ISDC, Versoix), report:

A large flare most likely coming from the soft repeater SGR 1806-20 has
been detected with INTEGRAL on December 27 at 21:30:26 UT.

The flare caused a large and rapid increase in the count rate of the SPI
ACS which reached a peak flux of 2x10^6 counts/s (compared to a
background level of 88,000 counts/s ).  The initial spike, lasting about
1.5 s, is followed by a 300 s long tail in which pulsations at 7.57 s are
clearly visible.  The IBAS ACS system triggered on a fainter event
occurring about 140 s before the main flare and possibly due to a
precursor from the same source.

No positional information is available with the SPI ACS data. The
shape of the light curve, similar to that of the 27 August 1998 flare
from SGR 1900+14, but with a  periodicity of 7.6 s, indicates
that SGR 1806-20 is the most likely origin of the observed event.
This would be the first giant flare observed from SGR 1806-20.

At the time of the flare, INTEGRAL was pointing at 106 degrees from the
direction of SGR 1806-20, which was outside the fields of view of the
imaging instruments.

See also the News section of  http://ibas.mi.iasf.cnr.it/
for further details of the ongoing analysis

This message can be cited.


////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2921
SUBJECT: IPN localization of giant flare from SGR1806-20
DATE:    04/12/29 12:30:42 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@sunspot.ssl.berkeley.edu>

K. Hurley and T. Cline, on behalf of the Ulysses and Mars Odyssey GRB teams,

I. Mitrofanov, S. Charyshnikov, V. Grinkov, A. Kozyrev, M. Litvak, and
A. Sanin, on behalf of the HEND-Odyssey GRB team, and

W. Boynton, C. Fellows, K. Harshman, C. Shinohara and R. Starr, on
behalf of the GRS-Odyssey GRB team, report:


The giant flare observed by INTEGRAL (SPI-ACS - GCN 2920) was also detected
by Mars Odyssey (GRS).  Data from other IPN spacecraft have not
been received yet.  A very preliminary analysis indicates that 
the arrival time at Odyssey is indeed consistent with an arrival
direction from SGR1806-20.  Further analysis is underway and will
be reported later.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2922
SUBJECT: The giant outburst from SGR 1806-20
DATE:    04/12/29 13:18:07 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

E. Mazets, S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin,  and
T. Cline on behalf of the Konus-Wind team, report:


On December 27, 2004, the Konus-Wind instrument detected a giant flare
from SGR 1806-20. The flare was preceded by a high emission
of recurrent soft bursts. A series of numerous bursts occurred
on October 5. On the analogy of the behaviour of SGR 1900+14 before
the giant flare on 1998 August 27, it was possible to expect,
that SGR 1806-20 is close to generation of a giant flare (GCN 2769).
Another series began on December 21 and lasted until the giant flare.
These bursts were strong in their flux, exhibiting a well pronounced
spectral  variability and in some cases unusual spectral features.
A record of the giant outburst was triggered by a recurrent burst,
which was the strongest in the series. The giant outburst occurred
on 142 s after this trigger. The flare started with a very intense
initial pulse, resulting in overloading of the detector.
It was followed by a long pulsating tail lasted more than 380 s.
A measured period of the pulsations is 7.57  0.07 s,
indicating its increasing since 2000, when value of  7.49 s
was determined in Chandra observations of X-ray  persistent flux
(Kaplan et al., 2002, ApJ, 564, 935) .

Giant outbursts were observed earlier in SGR 0526-66 on 1979 March 5,
in SGR 1627-41 on 1998 June 18, in SGR 1900+14 on 1998 August 27.
The event of December 27 completes this list for all of well known SGRs.
After the outburst, SGR 1806-20 continues to emit recurrent bursts.
A determination of energetic and spectral parameters of the outburst
will take some time because of a huge intensity of the initial pulse.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2923
SUBJECT: Detection of the SGR 1806-20 giant outburst back-scattered by the
DATE:    04/12/29 19:32:36 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks
on behalf of Konus-Wind and Helicon/Coronas-F teams, and
T. Cline on behalf of the Konus-Wind team report:

We present an evidence of Helicon-Coronas-F detection of the giant
outburst from SGR1806-20 which was scattered back from the Moon.
At the time of the outburst SGR1806-20 was occulted by the Earth
for Coronas-F. A short burst triggered Helicon at 21:30:29.303s UT on
Dec 27. A time delay between Konus-Wind and Helicon-Coronas-F detections
is -7.70 s. This value corresponds exactly to burst travelling time from
  the Wind to the Moon and back to the Coronas-F. The spectrum of the
event detected by the Helicon is highly unusual. It looks like a broad
assymetric line peaked at ~100 keV. Apparently such a shape corresponds
to back-scattering peak of a huge initial pulse of the outburst. The
fluence of event is about 7.5x10^-7 erg cm-2 in 25-400 keV range.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2928
SUBJECT: VLA observations of SGR 1806-20
DATE:    05/01/03 20:27:48 GMT
FROM:    Patrick B. Cameron at Caltech  <pbc@astro.caltech.edu>

P. B. Cameron (Caltech) and S. R. Kulkarni (Caltech) report:

"We observed the position of SGR 1806-20 with the Very Large Array (VLA)
in
A-configuration on 2005
Jan 3.81 UT (t ~ 6.9 days after the giant flare, GCN #2920).  We detect a
radio source coincident with the X-ray position reported by
Kaplan et al. (2002, ApJ, 564, 935) at the approximate freqeucnies
and flux densities
listed below.

Freq (GHz)    Flux density (mJy)
--------------------------------
4.86           73
8.46           41

This is a factor of brighter of 100 times brighter at 8.46 GHz than SGR
1900+14 at peak. Further observations are planned.

The National Radio Astronomy Observatory is operated by Associated
Universities, Inc., under cooperative agreement with the National Science
Foundation."

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2930
SUBJECT: VLA observations of SGR 1806-20
DATE:    05/01/03 21:00:02 GMT
FROM:    Patrick B. Cameron at Caltech  <pbc@astro.caltech.edu>

P. B. Cameron (Caltech) and S. R. Kulkarni (Caltech) report:

"We observed the position of SGR 1806-20 with the Very Large Array (VLA)
in A-configuration on 2005 Jan 3.81 UT (t ~ 6.9 days after the giant
flare, GCN #2920).  We detect a radio source coincident with the X-ray
position reported by Kaplan et al. (2002, ApJ, 564, 935) at the
approximate freqeucnies and flux densities listed below.

Freq (GHz)    Flux density (mJy)
--------------------------------
1.43           164

Further observations are planned.

The National Radio Astronomy Observatory is operated by Associated
Universities, Inc., under cooperative agreement with the National Science
Foundation."

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2931
SUBJECT: DETECTION OF POLARIZATION OF THE RADIO EMISSION FROM SGR 1806-20
DATE:    05/01/03 21:16:21 GMT
FROM:    Peter Woods at UAH/MSFC  <peter.woods@msfc.nasa.gov>

DETECTION OF POLARIZATION OF THE RADIO EMISSION FROM SGR 1806-20 

B. M. Gaensler (CfA), C. Kouveliotou (NASA/MSFC, NSSTC), R. Wijers (University
of Amsterdam), M. Garrett (JIVE), M. Finger, P. Woods, S. Patel (USRA, NSSTC),
M. McLaughlin (Jodrell Bank) report on behalf of a larger team:

Further to the reports on the radio emission from SGR 1806-20 (Cameron &
Kulkarni, GCN 2928, and Gaensler et al, GCN 2929, Atel # 373) we detect linear
polarization from the source at 1.4, 4.9, 8.5 GHz at a level of at least 2.6,
0.9, 3.8%, respectively. We caution, however, that these are very preliminary
results and more detailed analysis is underway to account for the possibility
of polarization leakage from the total intensity signal.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2933
SUBJECT: Second-epoch VLA observations of SGR 1806-20
DATE:    05/01/04 15:15:00 GMT
FROM:    Chryssa Kouveliotou at MSFC  <chryssa.kouveliotou-1@nasa.gov>

B. M. Gaensler (CfA), C. Kouveliotou (NASA/MSFC, NSSTC), R. Wijers
(U. Amsterdam), M. Garrett (JIVE), M. Finger, P. Woods, S. Patel (USRA,
NSSTC), M. McLaughlin (Jodrell Bank), R. Fender (U. Southampton),
T. Delaney (CfA) report on behalf of a larger team:

We observed the soft gamma-ray repeater SGR 1806-20 with the Very Large
Array (VLA) in the A-configuration for a second time on January 4,
2005 for one hour (14:15-15:15 UT). We detect the source at the same
coordinates as reported by Gaensler et al. (GCN 2929). Preliminary flux 
levels, including improved estimates of the fluxes reported in GCN 2929, 
are as follows (the numbers in parentheses indicate 3 sigma errors in the 
last decimal points):

Frequency   Flux (2005 Jan 03.8)   Flux (2005 Jan 04.6)
 (GHz)               (mJy)                 (mJy)
---------   --------------------   --------------------
  1.4               172(4)               135(10)
  4.9                80(1)                66(2)    
  8.5                53(1)                38(5) 

These results indicate a decay in the flux at a rate of approximately
1.9 mJy/hour at 1.4 GHz. At the same time the spectrum has remained constant. 
On Jan 3, 2005 the spectral index (in the sense F_nu ~ nu^alpha) was alpha =
-0.65+/-0.05, while on Jan 4, 2005 the spectral index was -0.61+/-0.06.

A reanalysis of the VLA data from 3 Jan 2004 (GCN 2928, 2929) suggests that 
the radio source associated with SGR 1806-20 is slightly extended at both 4.9 
and 8.5 GHz. Assuming that the underlying geometry is an optically thin, spherical 
thin shell, both data-sets independently suggest a source of approximate 
diameter 50-100 milliarcseconds. This implies a projected expansion speed of 
approx (0.3-0.6)c over the 7 days since the initial Giant SGR flare (assuming 
a source distance of 15.1 kpc; Eikenberry, S. et al., ApJ 616, 506, 2004).

Further radio observations of this source with the Westerbork Synthesis
Radio Telescope (WSRT), the MERLIN VLBI network and the Parkes Radio
Observatory are currently underway or are being scheduled and will be 
reported as they are analyzed. We will continue monitoring the source with 
the VLA until it fades below detection level.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2934
SUBJECT: Second Epoch VLA observations of SGR 1806-20
DATE:    05/01/04 17:32:20 GMT
FROM:    Patrick B. Cameron at Caltech  <pbc@astro.caltech.edu>

P. B. Cameron (Caltech) and S. R. Kulkarni (Caltech) report:

"We observed a second epoch of the position of SGR 1806-20 with the Very
Large Array (VLA) in A-configuration on 2005 Jan 4.59 UT (t ~ 7.7 days
after the giant flare, GCN #2920). We again detect a radio source
coincident with the X-ray position reported by Kaplan et al. (2002, ApJ,
564, 935) at the approximate freqeuncies and flux densities listed below.

Freq (GHz)    Flux density (mJy)
--------------------------------
1.43          128 +/- 5
4.86          62 +/- 2
8.46          37 +/- 5

Error Bars are 1 sigma. The combination of these measurements with those
reported 2005 Jan 03 (GCN #2928, #2929, 2930, ATEL 373) suggest a decay
exponent (F ~ t^beta) of beta = -2.2 at 1.4 GHz. The spectral index
(F ~ nu^alpha) has remained constant over the two epochs with alpha =
-0.74 and -0.68.

The National Radio Astronomy Observatory is operated by Associated
Universities, Inc., under cooperative agreement with the National Science
Foundation."

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2935
SUBJECT: Third epoch observations of SGR 1806-20 with VLA
DATE:    05/01/05 16:16:11 GMT
FROM:    Chryssa Kouveliotou at MSFC  <chryssa.kouveliotou-1@nasa.gov>

B. M. Gaensler (CfA), C. Kouveliotou (NASA/MSFC, NSSTC), J. Gelfand (CfA), 
R. Wijers (U. Amsterdam), M. Garrett (JIVE), M. Finger, P. Woods, S. Patel (USRA,
NSSTC), M. McLaughlin (Jodrell Bank), R. Fender (U. Southampton),
T. Delaney (CfA) report on behalf of a larger team:

We observed the soft gamma-ray repeater SGR 1806-20 with the Very Large
Array (VLA) in the A-configuration for a third time on January 5, 2005
for one hour (mean epoch approx 1600 UT).  (See GCN #2928, #2929, #2933;
ATEL #373, #375 for earlier results).

Preliminary flux levels for 2005-Jan-05.66 are as follows:

4.9 GHz: 57(2) mJy
8.5 GHz: 31(2) mJy

The source continues to fade, but at a slower rate consistent with a power law of 
index -1.6(2) at 4.9 GHz. Further observations will take place on January 6.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2937
SUBJECT: ATCA observations of SGR 1806-20
DATE:    05/01/05 21:01:30 GMT
FROM:    Chryssa Kouveliotou at MSFC  <chryssa.kouveliotou-1@nasa.gov>

J. Gelfand (CfA), B. M. Gaensler (CfA), K. Newton-McGee (U. Sydney),
C. Kouveliotou (NASA/MSFC, NSSTC), R. Wijers (U. Amsterdam), M. Garrett (JIVE),
M. Finger, P. Woods, S. Patel (USRA, NSSTC), M. McLaughlin (Jodrell Bank),
R. Fender (U. Southampton), T. Delaney (CfA) report on behalf of a
larger team:

We observed the soft gamma-ray repeater SGR 1806-20 with the Australian
Telescope Compact Array (ATCA) on January 5, 2005 for two hours (mean
epoch approx 2000 UT).  (See GCN #2928, #2929, #2933; ATEL #373, #375
for earlier results).

Preliminary flux levels for 2005-Jan-05.83 are as follows:

2.4 GHz: 87(2) mJy
4.8 GHz: 53(1) mJy
8.6 GHz: 29(1) mJy

We observe a possible break in the source spectrum. The power law spectral index
between 4.8 and 8.6 GHz is -1.0, while between 2.4 and 4.8 GHz the index is -0.7.
Further observations will take place on January 6.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2938
SUBJECT: SGR 1806-20: Temporal and Spectral behavior of radio transient
DATE:    05/01/06 14:01:30 GMT
FROM:    Dale A. Frail at NRAO  <dfrail@nrao.edu>

P. B. Cameron (Caltech) and S. R. Kulkarni (Caltech) report:

"We have carried out a more thorough calibration of the three VLA
epochs of the fading radio source toward SGR 1806-20 (GCN#s 2928,
2929, 2930, 2933, 2934, 2935). Combining this with the data from a
fourth epoch observation made with the Australia Compact Array (GCN#
2937) we do a joint fit of the form: F_nu \propto t^\alpha nu^\beta.

The best fit values are alpha= -1.62+/-0.06 and beta=-0.75+/-0.03.

There is evidence of deviations from this simple power-law behavior.
Fitting the decay rate alpha at each frequency we find a systematic
steepening. The value of alpha is -1.0 at 1.4 GHz, -1.5 at 4.9 GHz,
and -2.2 at 8.5 GHz. This behavior is reminiscent of the broadband
afterglow of GRB 991216 (Frail et al. ApJ, 538, 129). A plot of the
light curves is at: http://www.aoc.nrao.edu/~dfrail/sgr1806lc.eps.


The National Radio Astronomy Observatory is operated by Associated
Universities, Inc., under cooperative agreement with the National
Science Foundation. The Australia Telescope is funded by the
Commonwealth of Australia for operation as a National Facility managed
by CSIRO."

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2939
SUBJECT: SGR 1806-20: Low frequency GMRT results; submission to GCN circulars
DATE:    05/01/06 15:16:20 GMT
FROM:    Poonam Chandra at Tata Inst. Fund.Res.  <poonam@tifr.res.in>

SGR 1806-20: Low frequency GMRT results

P. Chandra (Tata Institute of Fundamental Research (TIFR), Mumbai),
reports the detection of radio emission from the  soft gamma-ray repeater
SGR 1806-20 with the Giant Metrewave Radio Telescope (GMRT) in the
610/235 MHz bands for 1.16 hours on 2005 Jan. 04 (mean epoch approximately
0949 UT). The preliminary flux densites for 2005-Jan-04.409 were:

 608 MHz:  198.9 (11.9) mJy
 240 MHz:  242.6 (14.9) mJy

The last digits in the brackets indicate 1 sigma error bars. She notes
that the power law index beween the two frequencies is: -0.21 (0.09). This
index is substantially flatter than the corresponding power law index
reported in the higher frequency VLA observation on 2005 Jan 4.59 UT by
Cameron and Kulkarni (GCN 2934) (alpha = -0.74 at 1.4 GHz) or -0.61 (0.06)
reported by Gaensler et al at the same time (GCN 2933). Further
observations with the GMRT at other low frequencies are also planned.

[GCN OPS NOTE (06Jan05):  This Circular was delayed by 3 hours
until the submitor could be added to the list.]
////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2940
SUBJECT: Fourth Epoch VLA observations of SGR 1806-20
DATE:    05/01/06 21:28:18 GMT
FROM:    Patrick B. Cameron at Caltech  <pbc@astro.caltech.edu>

P. B. Cameron (Caltech) and S. R. Kulkarni (Caltech) report:

"We observed a fourth epoch of the position of SGR 1806-20 with the Very
Large Array (VLA) in A-configuration on 2005 Jan 6.77 UT (t ~ 9.9 days
after the giant flare. See GCN #2920, #2928, #2929, #2933, #2934, #2935,
ATEL #373, #375).

We find the following preliminary flux densities:

Freq (GHz)    Flux density (mJy)
--------------------------------
1.43	      96 +/- 2
4.86	      39 +/- 2
8.46	      24 +/- 1

Error Bars are 1 sigma. We find an angular size at 8.46 GHz of about 80
mas. We see no variation in this diameter over the last 4 days.

The National Radio Astronomy Observatory is operated by Associated
Universities, Inc., under cooperative agreement with the National Science
Foundation."


////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2941
SUBJECT: Further ATCA observations of SGR 1806-20
DATE:    05/01/07 15:19:09 GMT
FROM:    Bryan Gaensler at Harvard-Smithsonian/CfA  <bgaensler@cfa.harvard.edu>

J. Gelfand (CfA), B. M. Gaensler (CfA), K. Newton-McGee (U. Sydney),
C. Kouveliotou (NASA/MSFC, NSSTC), G, Taylor (NRAO), R. Wijers
(U. Amsterdam), M. Garrett (JIVE), M. Finger, P. Woods, S. Patel (USRA,
NSSTC), M. McLaughlin (Jodrell Bank), R. Fender (U. Southampton) report
on behalf of a larger team:

We observed the soft gamma-ray repeater SGR 1806-20 with the Australia
Telescope Compact Array (ATCA) using five 6-km baselines  on January 6,
2005 (0530-0730 UT and 1930-2130 UT) and on January 7, 2005 (0430-0500
UT).  Preliminary flux levels, are as follows (the number in parentheses
indicates the 1-sigma uncertainty in the last significant figure):

Frequency  Flux (Jan 06.26)    Flux (Jan 06.77)    Flux (Jan 07.20)
 (GHz)     	(mJy)	          (mJy)                 (mJy)
---------   ------------        --------------    -----------------
  1.4          103(2)	           90(2)                86(3)
  2.4		68(2)	           66(2)                54(1)
  4.8           45(2)              38(1)
  6.1                              30(2)
  8.6           23(1)

There is clear evidence for a spectral break from the first two of the
above epochs, possibly decreasing to lower frequencies as a function
of time.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2942
SUBJECT: SGR 1806-20 and extragalactic short-duration GRBs
DATE:    05/01/07 16:31:10 GMT
FROM:    Arnon Dar at Technion-Israel Inst. of Tech  <arnon@physics.technion.ac.il>

If the giant short peak of the giant flare from SGR 1900+14 on 27/12/2004
(GCN 2920, GCN 2923, GCN 2936, GCN2927) at an estimated distance of 
15 kpc  (Corbel and Eikenberg A\&A 419, 191, 2004) could have been seen by
BATSE as a hard, short-duration GRB up to a distance of 80 Mpc (GCN 2936),
then SGRs in external galaxies can be the main source of the hard,
short-duration  GRBs seen by BATSE: The local optical luminosity within
a distance of 80 Mpc is about 10^4 times the Milky Way [MW] luminosity,
(\rho_L=1.84 10^8 h L[sun] Mpc^{-3}; L[MW]=2.4 10^{10} L[sun], where,
h=0.65, is the Hubble constant in units of 100 km/s/Mpc). If the observed
rate from Earth of such bursts per Milky Way luminosity is \sim 1 in 15
years (one since the launch of CGRO), it yields, before correcting for 
triggering efficiency and for sky solid angle coverage, an observable 
rate by BATSE of about 2 hard, short-duration, cosmic GRBs per day,
independent of the beaming angle.





////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2943
SUBJECT: Further VLA observations of SGR 1806-20
DATE:    05/01/07 22:09:14 GMT
FROM:    Bryan Gaensler at Harvard-Smithsonian/CfA  <bgaensler@cfa.harvard.edu>

B. M. Gaensler (CfA), G. Taylor (NRAO), J. Gelfand (CfA), C. Kouveliotou
NASA/MSFC, NSSTC), R. Wijers (U. Amsterdam), M. Garrett (JIVE),  G. Taylor
(NRAO), M. McLaughlin (Jodrell Bank), R. Fender (U. Southampton),
K. Newton-McGee (U. Sydney) report on behalf of a larger team:

We observed the soft gamma-ray repeater SGR 1806-20 with the Very Large
Array (VLA) in its A configuration on 2005, January 7, UT 2100-2200.

Preliminary flux levels at epoch Jan 07.90 are as follows (the numbers
in parentheses indicate 1 sigma errors in the last significant figure):

   Frequency  Flux (Jan 07.90)
    (GHz)          (mJy)     
   ---------   ------------   
     1.4           75(5)
     4.8           28(1) 
     8.6           17(1)

The spectrum is consistent with a single power law over this range of
spectral index -0.81+/-0.05, significantly steeper than when the radio
source was first detected on 2005 Jan 3 (GCN #2928, #2929, $2930).

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2945
SUBJECT: SGR1806-20: Swift-BAT observations of two additional bursts
DATE:    05/01/09 18:11:58 GMT
FROM:    David Palmer at LANL  <palmer@nis.lanl.gov>

D. Palmer (LANL), S. Barthelmy, L. Barbier, J. Cummings (GSFC),
E. Fenimore (LANL), R. Fink (GSFC), N. Gehrels (GSFC), D. Hullinger (GSFC/UMD),
S. Hunsberger (PSU), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD),
P. Matteo (ASDC) K. McLean (LANL), J. Nousek (PSU), P. Meszaros (PSU),
A. Parsons (GSFC), T. Sakamoto (GSFC), G. Sato (ISAS), M. Suzuki (Saitama),
J. Tueller (GSFC)  on behalf of the Swift-BAT team:

During a follow-up observation on the SGR1806-20,
the Burst Alert Telescope (BAT) on Swift has detected two more outbursts,
indicating that this source is still in an active phase 
11 days after the 041227 giant flare.  Each burst was ~0.1 second 
long and was within BAT's partially-coded (35%) field of view
(fully-coded viewing was prevented by the Sun observing constraint).

At 2005-01-07 02:08:21 a small outburst (0.4 counts/cm^2, 15-100 keV)
was localized on-board at RA=272.154, DEC=-20.374 (J2000) (6 arcmin
from the VLA position, Gaensler et al., 2005 GCN#2920).

At 2005-01-07 13:12:27 a larger but softer outburst (1.6 counts/cm^2, 
15-100 keV) was localized on-board at RA=272.156, DEC=-20.409 (J2000)
(0.5 arcmin from the VLA position).

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2946
SUBJECT: SGR 1806-20: Further VLA Observations
DATE:    05/01/10 15:10:43 GMT
FROM:    Patrick B. Cameron at Caltech  <pbc@astro.caltech.edu>

P. B. Cameron (Caltech) and S. R. Kulkarni (Caltech) report:

"We observed the soft gamma-ray repeater SGR 1806-20
with the Very Large Array (VLA) in A-configuration on 2005
Jan 10.60 UT.

We find the following preliminary flux densities:

Freq (GHz)    Flux density (mJy)
--------------------------------
8.46	       8 +/- 1


The National Radio Astronomy Observatory is operated by Associated
Universities, Inc., under cooperative agreement with the National Science
Foundation."


--------------------------------------
P. Brian Cameron
Caltech Astrophysics
Phone: (626) 395-6857

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2947
SUBJECT: SGR 1806-20: Further low frequency GMRT results
DATE:    05/01/13 15:01:53 GMT
FROM:    Poonam Chandra at Tata Inst. Fund.Res.  <poonam@tifr.res.in>

SGR 1806-20: Further low frequency GMRT results

P. Chandra on behalf of GMRT observatory reports the detection of
 radio emission from the SGR 1806-20 with the Giant Metrewave
 Radio Telescope (GMRT) in the 610 MHz band (with resolution 6-10")
on the  following dates:

 608 MHz:
 6 Jan 2005     111.8 (6.6) mJy
 7 Jan 2005     98.8 (29.3) mJy
 8 Jan 2005     83.8 (9.2) mJy
 9 Jan 2005     74.3 (14.5) mJy

The values quoted here are after subtracting the extended emission
contribution from the SGR and doing the Tsys corection by a factor of 1.8.

The modified value of 608 MHz flux density on 4 Jan 2005 observation is
231.7 (16.7) mJy (uncorrected value 199 mJy in reported in GCN 2939).
This new value is after subtracting the extended emission from the
 SGR and modified with Tsys correction factor of 1.8.

We shall report separately the 235 MHz band fluxes of SGR 1806-20
on these days (including 4 Jan 2005 observations (reported in GCN 2939))
treated similarly.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2948
SUBJECT: SGR 1806-20: Further VLA Observations
DATE:    05/01/13 20:20:42 GMT
FROM:    Patrick B. Cameron at Caltech  <pbc@astro.caltech.edu>

On Mon, 10 Jan 2005, P Brian Cameron wrote:

 P. B. Cameron (Caltech) and S. R. Kulkarni (Caltech) report:

 "We observed the soft gamma-ray repeater SGR 1806-20
 with the Very Large Array (VLA) in A-configuration on 2005
 Jan 13.8 UT.

 We find the following preliminary flux densities:

 Freq (GHz)    Flux density (mJy)
 --------------------------------
 8.46	       5.3 +/- 0.4


 The National Radio Astronomy Observatory is operated by Associated
 Universities, Inc., under cooperative agreement with the National Science
 Foundation."

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  2950
SUBJECT: SGR 1806-20: RXTE/PCA pulse frequency during flare
DATE:    05/01/14 18:00:12 GMT
FROM:    Peter Woods at UAH/MSFC  <peter.woods@msfc.nasa.gov>

Pulse Frequency of SGR 1806-20 during the Giant Flare

P.M. Woods, M. Finger, S. Patel (USRA, NSSTC), C. Kouveliotou (NASA/MSFC,
NSSTC), Y. Rephaeli (UCSD), D. Gruber (Eureka), M. Persic (Obs.Ast.Trieste), R.
Rothschild (UCSD), D. Palmer, N. Gehrels, S. Barthelmy, E. Smith, J. Swank, and
C. Markwardt (GSFC) report:

We have re-analyzed the RXTE PCA data of the giant flare of 2004 December 27
from SGR 1806-20.  We find that the pulse period reported in GCN #2927 of 7.579
+/- 0.002 s was strongly biased by pulse profile changes during the tail of
this flare.  Excluding the first ~60 s of the flare where pulse profile changes
are strongest, we measure a barycenter-corrected pulse period of 7.5605 +/-
0.0006 s, significantly different than the previously reported measurement. 



////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  3002
SUBJECT: SGR1806-20: Swift-BAT detection of a large normal burst
DATE:    05/01/30 23:52:20 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <Scott@lheamail.gsfc.nasa.gov>

G. Sato (ISAS), L. Antonelli (INAF-OAR), S. Barthelmy, L. Barbier (GSFC),
M. Cropper (MSSL), J. Cummings (GSFC), E. Fenimore (LANL), R. Fink (GSFC),
M. Galassi (LANL), N. Gehrels (GSFC), D. Hullinger (GSFC/UMD),
H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), P. Meszaros (PSU),
K. McLean (LANL), D. Palmer (LANL), A. Parsons, T. Sakamoto (GSFC),
M. Suzuki (Saitama), J. Tueller (GSFC)  on behalf of the Swift-BAT team:


Swift-BAT triggered on an outburst from SGR1806-20 at 22:38:26.86 UT 30 Jan 05.
This is a large normal burst from this source.  The peak rate is 340,000 cnts/sec
(1-sec average).  There was a single spike with a 0.4-sec rise, a 4.2-sec decay,
with additional emission extending out to ~T+15 sec.  On top of this tail,
there are five spikes at T+7, T+17, T+32, T+85, and T+118sec.
The fluence is ~1x10e-5 erg/cm2 (15-350 keV).  We note that this is
five orders of magnitude smaller than the giant flare from this source
on 27 Dec 04.  Also note that there was a burst from this source
earlier today at 20:45:26 UT with a peak rate of ~4000 cnts/sec
(0.128-sec average) and a duration of ~0.5 sec.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  3070
SUBJECT: Ongoing activity of SGR 1806-20 after the giant flare
DATE:    05/03/05 15:47:16 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks
on behalf of Konus-Wind and Helicon/Coronas-F teams, and
T. Cline on behalf of the Konus-Wind team report:

SGR-like burst 050304 was detected by Konus-Wind
at 10:17:14.537 UT and Helicon-Coronas-F at 10:17:17.941 UT.
We have triangulated it to an annulus centered at
RA(2000) = 321.683 deg, Decl(2000) = -15.478 deg,
whose radius is 47.167  0.092 deg (3 sigma).
As the center line of this annulus passes 0.033 degrees (1.1 sigma)
from the position of SGR 1806-20
and the Konus ecliptic latitude response indicates
that the source of the burst is near ecliptic plane,
we conclude that this burst originated from SGR 1806-20.

The burst had a duration of 0.13 sec,
fluence 7.9x10-7 erg cm-2, and peak flux
8.7x10-6 erg cm-2 s-1, both in 20-200 keV range.
The time-integrated spectrum of the burst can be fitted by the OTTB
spectral model:
dN/dE ~ E^{-1} exp(-E/kT),
with kT = 22  1 keV.


Since the giant flare on 2004 December 27,
Konus-Wind and/or Helicon-Coronas-F has detected
10 SGR-like bursts in the trigger mode,
probably originated from SGR 1806-20.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  3138
SUBJECT: Swift-BAT detection of a bright outburst from SGR1806-20
DATE:    05/03/23 03:31:54 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <Scott@lheamail.gsfc.nasa.gov>

S. Barthelmy, L. Barbier (GSFC), J. Cummings (GSFC/NRA),
E. Fenimore (LANL), N. Gehrels (GSFC), D. Hullinger (UMD),
H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), D. Palmer (LANL),
A. Parsons (GSFC), T. Sakamoto (GSFC/NRC), G. Sato (ISAS),
M. Suzuki (Saitama), J. Tueller (GSFC)
on behalf of the Swift-BAT team:

At 02:38:21.10 2005-03-23 UT Swift-BAT triggered on a bright outburst
from SGR1806-20.  There were two short peaks each ~0.4 sec
in duration, each with a peak count rate of ~160,000 counts/sec.
There was a smaller pre-trigger peak of ~30,000 counts/sec
at T-0.7 sec.  More than 99% of the emission is below 100 keV.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  3343
SUBJECT: Renewal of SGR 1806-20 activity
DATE:    05/05/03 15:18:35 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks
on behalf of Konus-Wind and Helicon/Coronas-F teams, and
T. Cline on behalf of the Konus-Wind team,
and
A. Rau, A. von Kienlin, G. Lichti on behalf of the INTEGRAL SPI-ACS
GRB team report:

On May 2 Konus-Wind detected two SGR-like bursts in the trigger mode.

The first one triggered Konus-Wind at 5376.421 s UT (01:29:36.421). 
It was also detected by INTEGRAL SPI-ACS.
Because the burst was soft, the SPI-ACS response is very weak,
and precise triangulation of this burst is not possible.
We conservatively estimated that the time delay was 3.6 +/- 0.4 s
which is consistent with the expected time delay for SGR 1806-20
(=3.651 s). Additionaly, the Konus ecliptic latitude response
indicates that the burst source is near the ecliptic plane,
so we believe that this burst originated from SGR 1806-20.
The burst is unusually long with a duration of ~4.5 s,
but relatively weak.
As observed by Konus-Wind, the burst had a fluence  ~2.0x10^-5 erg/cm2,
and a peak flux ~6x10^-6 erg/cm2 s (both in 20-200 keV range).
The time-integrated spectrum of the burst is well fitted by the OTTB
spectral model:
dN/dE ~ E^{-1} exp(-E/kT) with kT = 18 +/- 1 keV,
which is typical for this SGR.

The second burst triggered Konus-Wind 
at  18502.741 s  UT (05:08:22.741). 
As observed by Konus-Wind, it had a duration ~1 s,
a fluence  ~4.5x10^-6 erg/cm2, a peak flux ~3.7x10^-6 erg/cm2 s
(both in 20-200 keV range).

Another two SGR-like bursts (soft and short) were observed 
by Konus-Wind in the background mode 
at 5021 s UT (01:23:41) and 16740 s UT (04:39:00) (also on May 2).
The last burst was also detected by Helicon-Corronas-F 
in the background mode.
The estimated time delay is consistent with SGR 1806-20 position.

The Konus ecliptic latitude response indicates
that the source of all these bursts is near the ecliptic plane,
so we suppose, that they are also originated from SGR 1806-20.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  3545
SUBJECT: Konus-Wind observation of an intermediate burst from SGR 1806-20
DATE:    05/06/13 13:29:10 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks
on behalf of Konus-Wind and Helicon/Coronas-F teams, and
T. Cline on behalf of the Konus-Wind team report:

An SGR-like burst 050611 triggered Konus-Wind
at 58099.759 s UT (16:08:19.759).
It was detected and localized by HETE WXM (HETE trigger 3800).
The HETE error box includes the position of SGR 1806-20,
so we conclude that this burst originated from this SGR.

The burst had a duration of ~2.3 sec,
fluence (8.41  0.12)10-6 erg/cm2,
and peak flux on 16-ms time scale (8.6  0.9)10-6 erg/cm2 s
(both in 20-200 keV range).

The time-integrated spectrum of the burst can be fitted by the OTTB
spectral model:
dN/dE ~ E^{-1} exp(-E/kT),
with kT = 19  1 keV.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  4168
SUBJECT: SGR 1806-20: continued moderate activity seen with INTEGRAL
DATE:    05/10/27 08:09:41 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@mi.iasf.cnr.it>

S. Mereghetti (IASF-Milano), D. Gotz (SAP, Saclay), M. Beck (ISDC, 
Versoix), J. Borkowski (CAMK, Torun) on behalf of the IBAS Localization 
Team, and I.F. Mirabel (ESO) on behalf of the INTEGRAL Science Working 
Team report:

The soft gamma-ray repeater SGR 1806-20 continues to be in an active 
bursting state. A few normal short bursts have been detected by IBAS in 
October 2005 (note that SGR 1806-20 was not observed continuously during 
this period; the INTEGRAL observation log can be found at 
http://intweb.esac.esa.int/ ).

Burst times, approximate durations, and fluences (15-100 keV) measured 
with the IBIS/ISGRI instrument are reported below:

Date and  UT       Duration (s)    Fluence (erg cm-2)

2005-10-01T07:47:10   0.1               3E-8
2005-10-04T02:54:14   0.1               2E-8
2005-10-22T03:43:40   0.1               4E-8       
2005-10-22T07:25:37   0.38              9E-7
2005-10-22T08:52:42   0.07              2E-8 
2005-10-25T04:48:31   0.11              2E-8


The burst at 2005-10-22T08:52:42 was followed by a fainter peak 4.4 s 
later, lasting 0.04 s.

We remind that the occurrence of SGR 1806-20 bursts detected with high 
signal to noise ratio is reported in real time with IBAS Alert Packets. 
See http://ibas.mi.iasf.cnr.it/ for an uptated table of all the IBAS 
Alerts and for information on how to receive the Alert Packets for soft 
repeaters and type I bursters.

This message can be cited.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  4310
SUBJECT: Possible resuming of the SGR 1806-20 activity
DATE:    05/12/03 14:37:11 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks
on behalf of Konus-Wind, and
T. Cline on behalf of the Konus-Wind team,

Two SGR-like events were detected recently by the Konus-Wind.

The first one triggered the Konus-Wind on December 1 at 35965.468 s UT 
(09:59:25.468) . It had a duration ~3.6 sec,
a fluence  ~2.0x10^-5 erg/cm2, a peak flux ~1.2x10^-5 erg/cm2 s
(both in 20-200 keV range).
The time-integrated spectrum of the burst is well fit by the OTTB
spectral model:
dN/dE ~ E^{-1} exp(-E/kT) with kT = 19.7  0.6 keV,
which is typical for SGR 1806-20.

The second one occurred on December 3 at 32626.087 s UT (09:03:46.087)
(only ~5 hours ago). It had an unusual long initial pulse
with a duration ~9 sec followed by at least 9 weaker short bursts during 
the 229 sec of the Konus-Wind trigger record. So, this event can be 
classified as a burst series. The Konus-Wind spectral data for this 
event will be available in a day.

The Konus ecliptic latitude response indicates
that the source of these bursts is near the ecliptic plane.
There were no solar flares at these times according to the GOES data.

We suppose, that these events are originated from SGR 1806-20.
But now we can not exclude the other possibilities.

Further analysis using the data from other instruments will clarify
this issue.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  5427
SUBJECT: VLA Upper Limit on Outburst of SGR 1806-20
DATE:    06/08/09 13:14:36 GMT
FROM:    Jim Ulvestad at NRAO  <julvesta@nrao.edu>

E. Fomalont, B. Clark, and J. Ulvestad report on behalf of NRAO:

We have used the NRAO Very Large Array in its B configuration on
behalf of the community for an observation of SGR 1806-20, the
apparent source of GRB 060806 (GCN 5416, Hurley et al. 2006; GCN
5419, Hurley et al. 2006).  The observation epoch was 2006AUG09
at 03:15 UT.  There was no significant detection of a new point
source at the nominal J2000 position of 18:08:39.4, -20:24:39.8
(Taylor et al. 2005, ApJL, 634, L93).  The approximate 5-sigma
upper limits for a new point source are as follows:

1.42 GHz: < 2.0 mJy (limited by confusion)
8.46 GHz: < 0.3 mJy
22.46 GHz: < 1.7 mJy

The raw data will appear in the VLA archive at
http://www.nrao.edu/archive/ at approximately 0:00:00 UT on 2006AUG10,
and are freely available to the community for further processing and
analysis.  An additional community observation is planned for
2006AUG10 to check for a later appearance of a new point source.

The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc.

[GCN OPS NOTE(09aug06): This Circular was delayed 8 hours until the new
account could be added to the list.]
////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  5438
SUBJECT: A dust-scattering halo detected around SGR 1806-20 
DATE:    06/08/11 16:27:31 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

M.R Goad, K.L. Page, O. Godet, P.T. O'Brien, S. Vaughan (U Leicester), and
K. Hurley (Berkeley) report on behalf of the Swift-XRT team:

Analysis of 2.5 ks of Swift-XRT Photon Counting (PC) mode data taken
approximately 31 hours after the latest outburst of SGR 1806-20 (Hurley et
al., GCN Circ. 5419), reveals a dust-scattering halo, with a angular
radius of approximately 120 arcseconds at this time.

The halo is also detected in 14 ks of XRT PC mode data taken 93.5 hours
after the burst. The measured size of the halo at this time, approximately
212 arcseconds, is consistent with theoretical predictions for the
expansion of a dust scattering halo.

There are a number of well-known molecular clouds in the direction of SGR
1806-20 (eg. Corbel et al. 1997, ApJ 478, 624), including the so-called
expanding arm located at a distance of approximately 3 kpc.

Using simple geometrical arguments (eg. Predehl et al. 2000, A&A, 357,
L25), we place a firm upper limit on the distance to the dust scattering
screen of 6.6 kpc.  

Adopting as a lower limit the estimated distance to SGR 1806-20 of 6 kpc
(McClure-Griffiths and Gaensler 2005, ApJL 630, L161), then the dust
scattering screen is located at approximately 3 kpc, consistent with an
origin in the expanding Arm.  If, however, we adopt a distance of 15 kpc
for SGR 1806-20 (Corbel et al. 1997), then the dust scattering screen is
located at ~4.5 kpc.

Another Soft Gamma-ray Repeater, SGR 1900+14, has previously shown a dust 
halo (Kouveliotou et al. 2001, ApJ 558, L47).

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  5439
SUBJECT: Second VLA limit on new radio point source in SGR 1806-20
DATE:    06/08/11 21:13:35 GMT
FROM:    Jim Ulvestad at NRAO  <julvesta@nrao.edu>

E. Fomalont, B. Clark, and J. Ulvestad report on behalf of NRAO:

We have used the NRAO Very Large Array in its B configuration on
behalf of the community for a second observation of SGR 1806-20, the
apparent source of GRB 060806 (GCN 5416, Hurley et al. 2006; GCN
5419, Hurley et al. 2006).  As noted in GCN 5426 (Golenitskii et al.
2006), the gamma-ray activity is far below that of the large flare
of December 2004.  The observation epoch for the second VLA
observation was 2006AUG11 at 06:10 UT, and there was no detection
of a new radio point source at the location of SGR 1806-20.
The approximate 5-sigma upper limit at 8.46 GHz was < 0.23 mJy,
consistent with the value of < 0.30 mJy seen two days previously
and reported by us in GCN 5427.  This concludes the planned NRAO
service observations of SGR 1806-20 in response to the recent outburst.

The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  5440
SUBJECT: Image of the dust-scattering halo around SGR 1806-20
DATE:    06/08/12 08:31:07 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page (U. Leicester) & N. Gehrels (NASA/GSFC) report on behalf of the 
Swift-XRT team:

As an addendum to yesterday's GCN Circular (number 5438) about the
detection of a dust-scattering halo around SGR 1806-20, please find
available an image of the expanding halo at:

http://www.swift.ac.uk/SGR1806.shtml

////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  5471
SUBJECT: VLA Upper Limit on Outburst of SGR 1806-20
DATE:    06/08/23 20:17:58 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

test new loadfactor control params.
////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  5471
SUBJECT: VLA Upper Limit on Outburst of SGR 1806-20
DATE:    06/08/23 20:20:16 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

test new loadfactor control params.
////////////////////////////////////////////////////////////////////////
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  5490
SUBJECT: Two bright bursts from SGR 1806-20 detected with IBAS
DATE:    06/08/30 15:48:59 GMT
FROM:    Diego Gotz at IASF-CNR  <dgotz@cea.fr>

D. Gotz (CEA, Saclay) and S. Mereghetti (IASF, Milano), on behalf of the IBAS
Localization Team report:

The INTEGRAL Burst Alert System (IBAS) has detected several bursts from
SGR 1806-20 in the IBIS/ISGRI data, indicating that the source is in an
active state. We report here the properties of the two brightest and
longest bursts, that were detected on August 29, 2006, as well as the
times of the other events detected in the last few days.

The burst detected on Aug 29 at 21:57:43 UT was so bright to fully
saturate the ISGRI telemetry share after about 1 s. This burst was also
detected by the Anti-Coincidence System of the SPI instrument above ~80
keV, where it lasted 2 s. The 20-200 keV spectrum, derived from the the
available IBIS/ISGRI data, can be fitted with a Thermal Bremsstrahlung
(TB) model with a temperature of 22 keV. This is a typical value for the
SGR 1806-20 bursts, but the lower limit on its fluence ( 7E-7 erg/cmsq,
15-100 keV) places this burst among the brightest detected with INTEGRAL
(Gotz et al., 2006, A&A, 445, 313).

The second burst was detected at 22:10:28 UT and lasted 1.2 s. In this
case the telemetry was saturated only partially. The lower limit on the
fluence is 1E-6 erg/cmsq, and the TB temperature is 19 keV.

The times of all the recent IBAS triggers due to bursts from SGR 1806-20
are given below. For 15 of them automatic alert packets have been sent
(see Alerts #3437-3452 at http://ibas.iasf-milano.inaf.it).

2006-08-19T05:57:48

2006-08-25T21:03:31

2006-08-26T02:13:37
2006-08-26T03:23:35
2006-08-26T04:13:22
2006-08-26T04:25:25
2006-08-26T12:32:55
2006-08-26T18:48:47
2006-08-26T22:07:52

2006-08-27T03:14:45
2006-08-27T04:20:10
2006-08-27T08:49:52
2006-08-27T12:25:26
2006-08-27T12:41:34

2006-08-28T13:38:31

2006-08-29T21:57:43
2006-08-29T22:10:28
2006-08-29T22:48:01

2006-08-30T03:16:47
2006-08-30T14:58:39
2006-08-30T15:11:34

INTEGRAL will continue to monitor regularly the region of the Galactic Centre
(at least once every 3 days) until October 26th.

This message can be cited.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN CIRCULAR
NUMBER:  6239
SUBJECT: INTEGRAL ToO Observation of SGR1806-20
DATE:    07/04/02 17:03:03 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

K. Hurley, on behalf of the INTEGRAL AO-4 SGR ToO team, reports:

In view of the recent activity of SGR1806-20 observed by Konus (GCN 6228),
as well as a lower level of activity observed by Swift, we have called
an INTEGRAL target of opportunity observation of this source.  The start
times and durations of the observations are:

Start time, UT          Duration (s)  
2007-04-06 11:33:21.0   109728   
2007-04-07 19:31:06.0   44577     
2007-04-08 08:40:42.0   24003     
2007-04-08 16:06:00.0   30861  

We encourage supporting observations at all wavelengths.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN CIRCULAR
NUMBER:  6264
SUBJECT: Suzaku ToO observation of SGR 1806-20
DATE:    07/04/10 09:45:07 GMT
FROM:    Yujin E. Nakagawa at Aoyama Gakuin U  <yujin@phys.aoyama.ac.jp>

Y. E. Nakagawa, K. Yamaoka, A. Yoshida, S. Sugita (Aoyama Gakuin U.),
T. Mihara (RIKEN), M. Suzuki (ISAS/JAXA),
T. Murakami, D. Yonetoku (Kanazawa U.), M. Nakajima (Nihon U.),
M. Tashiro (Saitama U.), and K. Nakazawa (Univ. of Tokyo) report:

The Suzaku ToO Observation was conducted on SGR 1806-20 with the
narrow field instruments (XIS and HXD) from 15:08:00 on March 30
2007 to 01:30:19 on March 31. Its net exposure was about 20 ks.
This object showed a long burst at 00:24:08 on March 26 2007 which
was detected by the Konus-Wind and the Suzaku-WAM instruments
(Golenetskii et al., GCN 6228).

No bright burst was observable in the light curve during the ToO
observation. The preliminary analyses showed that the flux of the
steady emission in 2-10 keV was about 8.8 x 10^-12 ergs cm^2 s^-1.
By the quick-look analyses with the XIS data, the average spectrum
is well fitted by a single power-law model of the photon index of
~ 2.1 with an interstellar absorption column of ~ 7 x 10^22 cm^-2,
as well as a two blackbody function is acceptable.

We would like to thank the Suzaku team for the immediate ToO
observation and the data processing.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN CIRCULAR
NUMBER:  6804
SUBJECT: SGR1806-20: Swift-BAT detection of enhanced activity
DATE:    07/09/19 21:29:28 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), D. M. Palmer (LANL), T. Sakamoto (NASA/ORAU),
G. Sato (GSFC/ISAS) and M. Stamatikos (NASA/ORAU) report on behalf of
the Swift Team:

At 20:45:10 UT, the Swift Burst Alert Telescope (BAT) triggered and
located the SGR 1806-20 (trigger=291587).  We note that the initial
GCN Notice went out with a dual identification of this source (both
SGR 1900+14 and SGR 1806-20).  This is due to a mismatch error
in the catalog numbers used between the on-board and ground catalogs
for this source.  The real identification is SGR 1806-20.  We also
note that because of a star tracker loss-of-lock error, the flight
position is 10 arcmin off the true position. 
The BAT light curve shows a large initial spike of ~190,000 counts/sec
with an ~2 sec FWZM, followed by 4 smaller spikes: ~2000 cnts/sec
at ~T+3 sec, 10,000 cnts/sec at ~T+5 sec, 50,000 cnts/sec at ~T+14 sec,
and 30,000 cnts/sec at ~T+18 sec. 

Swift-BAT, and other space instruments (e.g. Konus-WIND
and Konus-A, Suzaku-WAM, IBAS, and SuperAGILE) have been
detecting elevated activity from this source over the
past few days. 

Notably, earlier today (at 16:01:12 UT, Trigger #291566)
a 50,000 counts/second burst (250 times the flux of 
the Crab) was detected by BAT,  which made it the 
third largest SGR 'baby' burst (excluding activity 
related to the superburst) imaged by the Swift mission.  
The new Trigger #291587 burst reported here is much larger. 

////////////////////////////////////////////////////////////////////////
TITLE:   GCN CIRCULAR
NUMBER:  6815
SUBJECT: INTEGRAL ToO observations of SGR1806-20
DATE:    07/09/21 23:23:49 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

K. Hurley, on behalf of the INTEGRAL Cycle 4 SGR ToO team, reports:

In view of the continued activity of SGR1806-20, a 206 ks INTEGRAL Target
of Opportunity observation of this source has been scheduled.  The tentative
observation times are:

     Start time           Duration (s)   
2007-09-30 00:06:42.0       106299  
2007-10-01 07:04:45.0        48006  
2007-10-01 21:20:21.0        24003  
2007-10-02 04:42:45.0        27432  

Any major changes to these times will be reported in a future GCN.

Supporting observations at all wavelengths are encouraged.

////////////////////////////////////////////////////////////////////////
TITLE:   GCN CIRCULAR
NUMBER:  6822
SUBJECT: Recent SGR1806-20 Activity
DATE:    07/09/24 20:45:04 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P.
Oleynik, M. Ulanov and T. Cline, on behalf of the Konus-Wind and
Konus-A teams,

D. Palmer, S. Barthelmy, J. Cummings, N. Gehrels, and H. Krimm, on behalf
of the Swift-BAT team,

K. Hurley, A. von Kienlin, G. Lichti, A. Rau, D. Gotz, and S.
Mereghetti, on behalf of the INTEGRAL GRB team,

M. Feroci, P. Soffitta and Y. Evangelista, on behalf of the AGILE team,

K. Yamaoka, M. Ohno, Y.E. Nakagawa, Y. Fukazawa, T. Takahashi, M.
Tashiro, Y. Terada, T. Murakami, and K. Makishima, on behalf of the
Suzaku WAM GRB team,

report:

SGR1806-20 has become very active since September 14 (Barthelmy et al.
GCN 6804).  The following is a partial list of bursts observed by some
of the IPN spacecraft (some weaker IBIS events did not trigger the INTEGRAL
Burst Alert Service).   "Loc" means that the burst was localized by
triangulation to at least a relatively narrow annulus, or by the Swift
BAT or by IBIS.  A "no" in this column means that the event has only
been localized to a relatively wide ecliptic latitude band.

INTEGRAL (GCN 6815) and Chandra target of opportunity observations of
this source are planned, and we encourage supporting observations at
all wavelengths.

Date		Time		Fluence	Observed by 		Loc
                                20-200  (at least)
                                 keV
-------------------------------------------------------------------
20070914	10:46:02	8.2E-7	BAT,IBIS,KW		y
20070914	14:54:47	1.6E-5	KW,KA,SA		y
20070914	14:58:44	1.0E-6	KW			no
20070914	19:57:57	2.8E-6	BAT,KA			y
20070914	21:03:36	4.5E-7	KW			no
20070916	07:08:38	6.5E-7	IBIS,KW			y
20070916	09:48:08	1.0E-6	IBIS,KW			y
20070918	17:08:50	1.6E-5	KW,SA,SPI-ACS,SUZ	y
20070919	10:01:51	1.5E-6	IBIS,KW			y
20070919	15:13:04	6.5E-7	KW			no
20070919	16:01:13	2.4E-6	BAT,KA,KW		y
20070919	16:54:44	9.6E-7	KW			no
20070919	19:34:50	9.0E-7	IBIS,KW			y
20070919	20:45:10	?	BAT,IBIS		y
20070920	04:30:11	1.9E-6	IBIS,KW 		y
20070921	07:11:59	1.4E-6	IBIS,KW			y
20070921	11:45:35	4.0E-7	KW			no
20070923	12:46:15	2.6E-6	KW,KA			no
------------------------------------------------------------------

Some Abbreviations:

BAT: Swift Burst Alert Telescope
IBIS: Imager on Board the INTEGRAL Satellite
KA: Konus-A (Cosmos 2421)
KW: Konus-Wind
SA: Super-AGILE
SPI-ACS: Anticoincidence System of the INTEGRAL Spectrometer
SUZ: Suzaku WAM

////////////////////////////////////////////////////////////////////////
TITLE:   GCN CIRCULAR
NUMBER:  8497
SUBJECT: SGR 1806-20: Fermi GBM detection 
DATE:    08/11/07 17:26:47 GMT
FROM:    Sheila McBreen at MPE  <smcbreen@mpe.mpg.de>

Sheila McBreen (UCD/MPE) and Chryssa Kouveliotou (NASA/MSFC)
report on behalf of the Fermi GBM Team:

"At 05:47:04.08 UT on 06 November 2008, the Fermi Gamma-Ray Burst Monitor
triggered on a soft, short event (trigger 247643225 / 081106241).

The on-ground calculated location, using the GBM trigger
data, is RA = 271.3, DEC = -16.2 (J2000 degrees,
equivalent to 18 h 05 m, -16 d 12 '), with an uncertainty
of 5.6 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error for soft localisations which is currently estimated
to be 5 to 6 degrees). This position is consistent with SGR 1806-20.
The angle from the Fermi LAT boresight is 41 degrees.

The GBM light curve comprises a single peak with a duration of about 80 ms.
The time-averaged spectrum from T0-0.045 s to T0+0.035 s is
adequately fit by a simple power law function with index -2.13 +/- 0.08.
(chi squared 205.1, for 242 d.o.f.) The event fluence (10-100 keV)
in this time interval is (7.9 +/- 0.3)E-8 erg/cm^2.

An optically thin thermal bremsstrahlung (OTTB) function
fits the spectrum equally well (chi squared 203.9 for 242 d.o.f.)
with kT = 36.5 +/-3.9 keV.

The spectral analysis results presented above are preliminary,
Final results will be published in the GBM Magnetar catalog."