On February 10, 2000, 08:44:06 UT, the GRBM and WFC1 detected a GRB.
Follow-up observations with BeppoSAX and Chandra revealed a new X-ray source.
- BeppoSAX MAIL n. 00/01 = GCN notice #538
A GRB (GB000210) was detected by the GRBM and WFC1 of BeppoSAX on Feb.10,
around 08:44:06 U.T.
Preliminary coordinates from WFC are:
R.A.(2000)=29.810
DEC(2000)=-40.696
with an error radius of about 3'.
- BeppoSAX MAIL n. 00/02 = GCN notice #539
Refined WFC positions of GRB000210 are
R.A. = 29.812 degrees
Decl. = -40.669 degrees
(equinox 2000). The error radius is about 2'.
We are planning a follow-up with NFI.
- GCN notice #540
M. Stornelli, G. Celidonio, Scientific Operation Centre, Telespazio, Roma,
J.M. Muller, J. In't Zand, Space Research Organization of the Netherlands
(SRON), Utrecht, L. Amati, TESRE/CNR, Bologna, M. Feroci and G. Gandolfi,
IAS/CNR, Roma, report:
The BeppoSAX Gamma Ray Burst Monitor (GRBM) and Wide Field Camera
(WFC unit 1) observed a strong gamma-ray burst on February
10.36396 UT. A preliminary analysis reveals a duration of about 20 s in
the GRBM, with a peak photon countrate of 22083 cts/s in the 40-700 keV
energy band. In the WFC, the duration is the same and the peak flux
is 7.4 Crab (2-26 keV). The position of the X-ray counterpart is R.A. =
01h59m14.9s Decl. = -40d40'.14 (equinox 2000.0) with a 99% error radius of
2'. An NFI follow-up is being carried on.
- GCN notice #542
E. Costa, G. Gandolfi, L. Piro, IAS/CNR, Roma, M.J.S. Smith, Space
Research Organization of the Netherlands (SRON), Utrecht, C. Guidorzi,
Universita' di Ferrara, D. Ricci, G. Tassone and A. Coletta, Scientific
Operation Center, Telespazio, Roma, report:
A BeppoSAX follow-up of GRB000210 started about 8 hr after the burst. A
very preliminary quick look analysis of the first three orbits of the MECS
data at SOC shows an object, previously unknown, inside the refined error
circle of the WFC, without any evidence of decaying behaviour. The source
flux is of the order of 5x10E-13 erg sE-1 cmE-2.
- GCN notice #543
K. Hurley, on behalf of the Ulysses GRB team, M. Feroci and
B. Preger, on behalf of the BeppoSAX GRBM team, and T. Cline
and E. Mazets, on behalf of the Konus-WIND GRB team, report:
GRB000210 was observed by Ulysses, Konus, and the BeppoSAX
GRBM. Triangulation gives an annulus centered at RA(2000)=
154.970, Decl.(2000)=-41.463, with radius 84.032 +/- 0.017
degrees. This annulus intersects the BeppoSAX WFC error
circle (GCN 540) to form an ~3.7 sq. arcmin. error box
whose corners are given by:
RA DEC
1 h 59 m 05.32 s -40 o 39 ' 19 "
1 h 59 m 12.96 s -40 o 38 ' 11 "
1 h 59 m 07.35 s -40 o 41 ' 32 "
1 h 59 m 23.85 s -40 o 39 ' 05 "
A map has been posted at
ssl.berkeley.edu/ipn3/000210 and is reproduced below. This
triangulation is preliminary, and can be refined considerably.
- GCN notice #544
Michael Garcia (Chandra X-ray Center), Luigi Piro (IAS/CNR),
Gordon Garmire (Penn State), and Joy Nichols (Chandra X-ray Center) report:
The Chandra X-ray Observatory observed the GRB000210 error region
using the ACIS-S detector approximately 21 hours after the GRB (GCN
538). Based on a preliminary analysis of a fraction of the data, we
find a source in the BeppoSAX WFC error region (GCN 539), with
co-ordinates of:
RA=01:59:14.78, DEC = -40:39:33.2 (J2000)
approximate error radius 2 arc-sec. Further analysis of the complete
data set may decrease the error region and should provide a flux
estimate.
- GCN notice #545
J. Gorosabel (DSRI, Copehagen), B.L. Jensen, L.F. Olsen, L. Christensen,
J. Hjorth, H. Pedersen (U. Copenhagen),
M.I. Andersen (U. Oulu), A.O. Jaunsen (U. Oslo) report:
R-band images obtained at the 1.54-m Danish Telescope on Feb 2.03-2.08 contain
a faint object located at alfa(2000)=01 59 15.6 delta(2000)=-40 39 33.8
+/- 2". The position of the obejct is consistent with the X-ray position
determined by Chandra (GCN 544). The magnitude of the object is about
R~23.1+/-0.5. Optical/IR observations are urgently required.
- GCN notice #546
E. Berger (Caltech) and D. A. Frail (NRAO) report on behalf of a
larger collaboration:
On February 10.98 UT we used the VLA to observe a field centered at
the position provided by the SAX WFC (GCN 539 and 540). There are no
radio sources brighter than 0.26 mJy (4-sigma) within the 2-arcminute
radius of the WFC error circle. A limit of 0.13 mJy can be placed on
the absence of a radio source within the 2-arcsecond radius error
circle (GCN 544) of the Chandra X-ray source. Further observations are
planned.
- GCN notice #547
J. Gorosabel (DSRI, Copenhagen),
B.L. Jensen, J. Hjorth, L. Fogh Olsen, L. Christensen (U. of Copenhagen),
M.I. Andersen (U. of Oulo), A.O. Jaunsen (U. of Oslo) report:
We ask that the previous message (GCN #545) concerning an optical detection
at the position of the Chandra X-ray source is disregarded. As a matter of
fact, we do not detect any object at the X-ray position given by Chandra (GCN
#544) in our combined 3000s 1.54-m Danish Telescope R-band image (obtained
on Feb 11.05 2000 UT) down to a limit of R~23.3. An image of the field is
available at: http://www.astro.ku.dk/~brian_j/grb/grb000210
- GCN notice #548
Michael Garcia (Chandra X-ray Center),
Gordon Garmire (Penn State), Luigi Piro (IAS/CNR) report:
There is a possible error in the position of the x-ray afterglow
of GRB000210 as reported in GCN544. The error is approximately
8 arcsec in the spacecraft Z direction, which in this case is
RA. The true position may be 8 arcsec to the East, or:
RA=01:59:15.5, DEC = -40:39:33.2 (J2000)
We note that U0450_00688875, ra= 01 59 29.84 dec=-40 43 26.0,
rmag=15.2 would be correctly located by Chandra if this error is included.
Note that this new position agrees with the optical source mentioned
in GCN 545 and 547.
- GCN notice #549
R. M. Kippen (University of Alabama in Huntsville) reports on behalf
of the BATSE GRB team:
GRB 000210 (GCN 540) occurred at a time when the BATSE on-board
trigger system was intensionally disabled. However, the burst is
clearly detected at Feb 10.36396 UT in the continuous data with
1.024 s resolution. These data show the event consisted of a strong
pulse with T50 and T90 durations of 4.1 s and 12.3 s, respectively.
The burst's peak flux (50-300 keV; integrated over 1.024 s) and
fluence (>20 keV) are 29.9 photons cmE-2 sE-1 and 8.5 x 10E-5 erg
cmE-2, respectively---ranking it in the top 1% (3%) of the BATSE GRB
flux (fluence) distribution. The spectral hardness is average for
bursts of similar duration. The BATSE burst location is consistent
with those measured by BeppoSAX (GCN 540) and IPN (SAX/Konus/Ulysses;
GCN 543). The lightcurve for this event is available at:
http://gammaray.msfc.nasa.gov/~kippen/batserbr/brbr_obs.html
- GCN notice #553
E. Costa, Istituto di Astrofisica Spaziale, CNR, Rome,
L.A. Antonelli, Osservatorio Astronomico di Roma, Rome,
J. in 't Zand, Space Research Organization Netherlands, Utrecht;
M. Stornelli, D. Ricci, M.R. Daniele, M. Capalbi, BeppoSAX Science
Operations Center, Telespazio, Rome; M. Feroci, G. Gandolfi, Istituto di
Astrofisica Spaziale, CNR, Rome, E. Pian, ITESRE, CNR, Bologna, report:
GRB 000210 was observed with the Narrow Field Instruments (NFI) on board
BeppoSAX from Feb. 10.66 UT to 11.98 UT (starting 7.2 hrs after the
burst trigger time). In the combined image of both Medium-Energy
Concentrator Spectrometers, taken over the whole observation, a point
source, showing an unambiguous fading behaviour, is detected with a
position of R.A. = 01h59m15.9s, Decl. = -40d39'29" (Eq. 2000.0) and an
error circle of 50''. This is consistent with the position given by
Chandra in an observation performed during the central part of BeppoSAX
observation (GCN #548) and with the position of the optical object
reported in GCN #545. In the first 30,000 s of the observation the
object flux (2-10 keV) is about 4.5E-13 erg/cmE2/s. In the last 40,000 s
of the observation the source has faded of about a factor three but a
fainter soft source, located at about 2 arcmin NE from the X-ray
afterglow, contributes a flux not negligible. Therefore an evaluation
of the flux and the decay law needs a more refined analysis.
- GCN notice #554
SG Bhargavi, Geetanjali Gauba and R Cowsik
(Indian Institute of Astrophysics, Bangalore, India 560034) report:
We observed the field of GRB000210 (GCN # 539, 540) using 2.34m
Vainu Bappu Telescope (FOV =10') in R and V band filters on
10th and 11th Feb, 2000.
On Feb 10, between 14.35-15.18 UT we took 4 frames in R (each 300sec) and
a V frame of 600sec. On Feb 11, between 13.66-15.275 UT we took one V (900s)
and several R frames of short exposures. Observations were made at airmass >
2.2 and with high background from Moon.
At the limit of R=18.0 we donot detect any object at the position of
Chandra's x-ray source (GCN # 544, 548) in the combined frames.
- GCN notice #560
D. McConnell, R. Subrahmanyan, M.H. Wieringa, R.M. Wark (ATNF),
D. A. Frail (NRAO), E. Berger and S. R. Kulkarni (Caltech) report:
We obtained a 8.2 hour integration with the Australia Telescope
Compact Array (ATCA) on February 12.31 UT. In addition, shorter
integrations were obtained at 8.46 GHz with the Very Large Array on
February 10.99, Feb 14.90, Feb 15.03 UT. Both the ATCA and VLA imaged
a field that fully covers the 50-arcsecond error circle of the fading
NFI X-ray source, as reported by Costa et al. (GCN 553). There are no
radio sources in the NFI above a 4-sigma level on any of the four
days. The rms noise levels are 65 microJy (Feb. 10.99), 55 microJy
(Feb. 12.31), 35 microJy (Feb. 14.90), and 38 microJy (Feb. 15.03).
Adding together the data taken on February 14 and 15, we obtain an
upper limit of 55 microJy (2-sigma) for the flux density of any radio
afterglow at the position of the Chandra X-ray source (Garcia, Garmire
and Piro GCN 548).
- GCN notice #782
Gordon Garmire (Penn State Universtiy), Luigi Piro (IAS/CNR), Giulia
Stratta (IAS/CNR), Michael Garcia(Chandra X-ray Center), and Joy Nichols
(Chandra X-ray Center) report:
Following the reprocessing of the Chandra observation of GRB000210 by the
Chandra X-ray Center (CXC), the best position of the GRB is
RA=01h 59m 15.6s DEC= -40d 39' 32.5"
(equinox 2000).
Using 5 stars detected in X-rays and comparing their positions to the USNO
A2 and 2MASS catalog positions, the GRB position is derived to be
RA= 01h 59m 15.7s DEC= -40d 39' 32.3"
with an estimated error of 1.6"
The two measurements are consistent within the error and also
in agreement with the optical candidate proposed by Gorosabel et al (GCN
#545)
- GCN notice #783
J. Gorosabel (DSRI, Copenhagen), J. Hjorth, B. L. Jensen (U. of Copenhagen),
J. P. U. Fynbo, A. O. Jaunsen (ESO), M. I. Andersen (U. of Oulu),
S. Holland (U. of Aarhus), and N. Lund (DSRI, Copenhagen) report:
We have carried out optical observations of the corrected Chandra X-ray
position of GRB 000210 (Garcia et al., GCN #548) with the 1.54-m Danish
Telescope at La Silla, as follows:
Date (Aug. 2000 UT) Filter Exp.(s) Seeing(")
----------------------------------------------------
22.293 - 22.411 R 7x900 2.2
23.226 - 23.290 R 5x900 2.3
24.235 - 24.303 R 4x900 3.0
26.291 - 26.430 V 9x900 1.5
27.213 - 27.236 I 2x900 1.4
28.211 - 28.241 I 2x1200 1.4
29.207 - 29.300 I 7x1200 1.1
30.223 - 30.242 I 1200 1.1
31.213 - 31.245 B 2x1200 1.5
----------------------------------------------------
The optical source coincident with the Chandra position (Gorosabel et al.,
GCN #545) is clearly detected in the co-added R, V and I-band images.
Astrometry based on the USNO-A2.0 catalogue yields for the object
RA(J2000) = 01h 59m 15.60s
Dec(J2000) = -40d 39' 32.8"
with an uncertainty of +/- 1". The position is consistent with the two
updated Chandra positions derived by Garmire et al. (GCN #782). A comparison
of the co-added R-band image with the R-band image taken on Feb 11.03 - 11.08
2000 UT (GCN #545) reveals a magnitude variation of 0.03 +/- 0.30 mag.
Therefore, the object remains constant in brightness within the photometric
errors. We derive a preliminary magnitude of R = 23.5 +/- 0.2 for the
object.
- BeppoSAX image from
http://www.ias.rm.cnr.it/ias-home/sax/grb000210.html
- Radio detection (ApJ 577, 680)
- Redshift z = 0.8463 from one single line (OII) of host galaxy
(ApJ 577, 680); later confirmed via photo-z of host SED (A&A 400, 127)
Previous IAU Circulars 