- GCN/BACODINE POSITION NOTICE
TITLE: GCN/SAX_WFC BURST POSITION NOTICE
NOTICE_DATE: Tue 11 Dec 01 23:50:02 UT
NOTICE_TYPE: SAX-WFC Initial
GRB_DATE: 12254 TJD; 345 DOY; 01/12/11
GRB_TIME: 68961.00 SOD {19:09:21.00} UT
GRB_SAX_RA: 168.812d {+11h 15m 15s} (J2000),
168.836d {+11h 15m 21s} (current),
168.194d {+11h 12m 46s} (1950)
GRB_SAX_DEC: -21.935d {-21d 56' 05"} (J2000),
-21.946d {-21d 56' 43"} (current),
-21.662d {-21d 39' 43"} (1950)
GRB_SAX_ERROR: 0.083 [deg radius (stat+sys), 1-sigma]
GRB_SAX_INTEN: unknown
SUN_POSTN: 258.93d {+17h 15m 43s} -23.05d {-23d 02' 53"}
SUN_DIST: 81.67 [deg]
MOON_POSTN: 220.30d {+14h 41m 13s} -11.75d {-11d 45' 01"}
MOON_DIST: 50.07 [deg]
COMMENTS: SAX-WFC GRB Coordinates.
COMMENTS: X-ray Rich GRB detected in WFC1 (XRF011211)
- red DSS finding chart
ps-file
- GCN notice #1188 = BeppoSAX mail n. 01/15
BeppoSAX Alert: GRB011211(=XRF011211)
On Dec. 11, 19:09:21 UT an X-ray rich GRB (XRF011211) has been
detected in BeppoSAX WFC1
Preliminary coordinates are:
R.A.(2000)= 168.812
DEC.(2000)= -21.935
The error radius at this stage of analysis is 5'.
Giangiacomo Gandolfi
on behalf of
BeppoSAX Mission Scientist
- GCN/BACODINE POSITION NOTICE
TITLE: GCN/SAX_WFC BURST POSITION NOTICE
NOTICE_DATE: Wed 12 Dec 01 02:16:33 UT
NOTICE_TYPE: SAX-WFC Final
GRB_DATE: 12254 TJD; 345 DOY; 01/12/11
GRB_TIME: 68961.00 SOD {19:09:21.00} UT
GRB_SAX_RA: 168.818d {+11h 15m 16s} (J2000),
168.842d {+11h 15m 22s} (current),
168.200d {+11h 12m 48s} (1950)
GRB_SAX_DEC: -21.929d {-21d 55' 43"} (J2000),
-21.940d {-21d 56' 22"} (current),
-21.656d {-21d 39' 21"} (1950)
GRB_SAX_ERROR: 0.033 [deg radius (stat+sys), 1-sigma]
GRB_SAX_INTEN: unknown
SUN_POSTN: 258.93d {+17h 15m 43s} -23.05d {-23d 02' 53"}
SUN_DIST: 81.66 [deg]
MOON_POSTN: 220.30d {+14h 41m 13s} -11.75d {-11d 45' 01"}
MOON_DIST: 50.07 [deg]
COMMENTS: SAX-WFC GRB Coordinates.
COMMENTS: A BeppoSAX NFI follow-on has been planned and will be very
COMMENTS: soon performed
- GCN notice #1189 = BeppoSAX mail n. 01/16
GRB011211(=XRF011211): BeppoSAX refined positions
Refined coordinates from WFC are:
R.A.(2000)= 168.818
DEC.(2000)= -21.929
The error radius is 2'.
Giangiacomo Gandolfi
on behalf of
BeppoSAX Mission Scientist
- GCN notice #1191
T. Grav, M. W. Hansen (U. of Oslo), H. Pedersen, J. Hjorth, R. Michelsen,
B. L. Jensen (U. of Copenhagen), M. I. Andersen (U. of Oulu),
J. Gorosabel (DSRI), J. U. Fynbo (ESO) report:
We have obtained optical follow-up observations of the SAX error circle of
GRB 011211 (cf. GCN ##1188,1189) with the ALFOSC on the 2.56-m NOT and with
DFOSC on the Danish 1.5m on La Silla starting at about 12.2 December 2001 UT.
In R-band images a new point source, not visible in the DSS-2 (red), is
detected at RA (J2000) = 11:15:17.98, Dec(J2000) = -21:56:56.2 with an
estimated error of +- 1". The magnitude is about R = 19. Given the proximity
to the refined SAX WFC position and its absence in DSS, the source is likely
the afterglow of GRB 011211.
The above findings are preliminary. More details will be reported later.
Images will be made available at
http://www.astro.ku.dk/~brian_j/grb/grb011211
R-band 3x300s exposure taken with the NOT on 2001, December 12.2.
The OT is marked at the centre of the image, surrounded by the
XMM-Newton 10" error-circle reported by Santos-Lleo et al. (GCN#1192).
- GCN notice #1192
M. Santos-Lleo, N. Loiseau, P. Rodriguez, B. Altieri,
and N. Schartel report:
QLA (Quick-Look-Analysis) analysis of the XMM-Newton observation
of GRB011211 (G. Gandolfi et al. GCN 1188 and 1189) shows the
presence of a source in the WFC error box:
S1 (J2000): R.A. = 11h 15m 17.9s Decl. = -21 56' 57.5"
with an estimated EPIC/pn countrate of 0.02 [counts/sec].
At this stage of reduction the error is expected to be less than 10".
Refined coordinates will be distributed as soon as the final attitude
reconstruction is obtained.
- GCN notice #1193
Fading of the optical source associated of XRF 011211
J. S. Bloom and Edo Berger report on behalf of the larger
Caltech-NRAO-CARA GRB Collaboration:
"Following the report of a new bright source (Grav et al. GCN #1191) in
the field of XRF 011211 (Gandolfi et al. GCN #1188, GCN #1189; Santos-Lleo
et al. GCN #1192) we began observing the source position with the Palomar
200" + JCAM dual-band optical imager on 12 Dec 01, 10:48 UT in very poor
observing conditions. In Sloan-r', the source is clearly fainter than the
three objects to the northwest (the source plus the three objects appear
to be of comparable brightness on the Grav et al. finding chart). This
confirms the transient nature of the source discovered by Grav et al. and
helps solidify its association with XRF 011211.
The source was also detected the Sloan g' filter, suggesting an origin
z <~ 4.3.
A finding chart with a single g' and r' integration (110s and 100s
exposure) may be found at:
http://www.astro.caltech.edu/~jsb/xrf011211.gif
This message may be cited.
- GCN notice #1195
B. L. Jensen, H. Pedersen, J. Hjorth, R. Michelsen (U. of Copenhagen),
T. Grav, M. W. Hansen (U. of Oslo), J. U. Fynbo (ESO),
M. Weidinger (U. of Aarhus), M. I. Andersen (U. of Oulu) and
J. Gorosabel (DSRI) report:
We have performed aperture photometry of the afterglow candidate for
GRB 011211 reported in GCN#1191 (Grav et al.), and obtain the
following results based on a preliminary photometric calibration:
For USNO-star U0675_11427359 at RA,Dec (J2000) = (11:15:19.00,
-21:58:04.9) we obtain:
I = 17.07, R = 17.90, V = 18.18, B = 18.65
For the afterglow candidate we measure:
Tel. Date (UT) exp filter mag.
=========================================
NOT-2.5m Dec.12.22 900s R 20.07
NOT-2.5m Dec.12.28 300s B 21.41
NOT-2.5m Dec.12.28 300s g-i 20.09
NOT-2.5m Dec.12.29 300s V 21.14
DK-1.5m Dec.12.28 4200s R 20.12
DK-1.5m Dec.12.36 300s V 21.21
Conservative errors on the absolute photometry is ~0.15 mag, due
to lack of precise calibration. Errors relative to the USNO-star
are around a few percent.
Further images will be made available at
http://www.astro.ku.dk/~brian_j/grb/grb011211.
- GCN notice #1197
A. Henden (USRA/USNO) reports on behalf of the USNO GRB team:
We have acquired BVRcIc all-sky photometry for
an 11x11 arcmin field that is approximately centered on
the position of the candiate optical transient reported
by Grav et al. (GCN 1191) with the USNOFS 1.0-m telescope
on one photometric (but poor seeing) night. Stars brighter than
V=13.5 are saturated and should be used with care.
We have placed the photometric data on our anonymous ftp site:
ftp://ftp.nofs.navy.mil/pub/outgoing/aah/grb/grb011211.dat
The current photometry has a potential external zero-point
error of about two percent. The astrometry in this file
is based on linear plate solutions with respect to USNO-A2.0.
The internal errors are less than 100mas.
In particular, the comparison star U0675_11427359 that was
used to calibrate their field can be found in the .dat file
with the following magnitudes:
B = 18.65 V = 18.11 R = 17.76 I = 17.42
with estimated photometric errors of about 4 percent, including
the zeropoint errors quoted above.
Further calibration of this field will be performed when
weather conditions improve.
- GCN notice #1199
GRB 011211, Optical Observations
I. Soszynski (Warsaw University Observatory),
S. Holland, P. M. Garnavich (Notre Dame)
D. Bersier, S. Jha, K. Z. Stanek (Harvard-Smithsonian Center
for Astrophysics),
We have obtained deep VRI images of the field containing GRB
011211 using the OGLE 1.3-metre telescope (using the 8k x 8k OGLE-III
mosaic) at the Las Campanas Observatory on Dec. 12 and Dec. 13 UT.
The optical afterglow of GRB 011211 (Grav et al. 2001, GCN 1191) is
visible on all of our images. We performed PSF photometry on each
image and calibrated data using the VRI magnitudes for USNO star
U0675_11427359 given by Henden (2001, GCN 1197). Preliminary
magnitudes, relative to the USNO star, are:
Band Date Start UT Mag err Exptime(s)
-----------------------------------------------
V Dec 12 07:16:02 20.79 0.05 600
V Dec 13 06:19:28 21.71 0.09 600
R Dec 12 05:55:55 20.10 0.08 180
R Dec 12 06:04:34 20.41 0.04 600
R Dec 12 06:33:59 20.43 0.05 600
R Dec 12 06:59:04 20.35 0.03 600
R Dec 12 07:39:27 20.40 0.04 600
R Dec 13 05:43:15 21.48 0.11 600
R Dec 13 08:09:13 21.52 0.07 600
I Dec 12 06:18:16 19.95 0.06 600
I Dec 12 06:47:12 19.92 0.07 600
I Dec 12 07:27:46 19.96 0.05 600
I Dec 12 07:51:13 20.10 0.06 600
I Dec 13 06:03:48 20.80 0.11 600
I Dec 13 08:23:44 20.94 0.12 600
The quoted uncertainties are internal errors only and do not include
uncertainties in the calibration of the USNO star. The frame-to-frame
variation in several stars located near the optical afterglow and the
USNO star is approximately 0.03 mag.
The optical afterglow faded by approximately one mag between
approximately Dec. 12.3 and Dec. 13.3 in each of the V, R, and I
bands. The decays are well fit by single power laws with slopes of
-0.80 +/- 0.12 in the V band, -0.93 +/- 0.06 in the R band, and -0.74
+/- 0.08 in the I band. If we include the V and R data from Jensen et
al. (2001, GCN 1195) the slopes change by less than one sigma. We see
no evidence for a break in the light curve. A plot of the VRI light
curves and the best-fitting single power laws is available at
http://www.nd.edu/~sholland/grb/grb011211/ogle_fit.eps.
We do not detect any evidence for a host galaxy at the location
of the proposed optical afterglow.
This message may be cited.
- GCN notice #1200
A. Fruchter (STScI), P. Vreeswijk (A'dam), J. Rhoads, and I. Burud (STScI)
report for a larger collaboration:
We have observed the optical counterpart of GRB (XRF) 011211 (GCN 1188, 1191)
using the FORS2 spectrograph on the Yepun (VLT4) 8-m telescope of the European
Southern Observatory. We find an absorption line system corresponding to a
redshift of z=2.14 superposed on the continuum emission. Hydrogen Lyman
alpha, as well as the absorption lines of several metals including C, Fe and
Si, are clearly detected.
- GCN notice #1202
S.G. Bhargavi & R. Cowsik (IIA, Bangalore) report:
The afterglow of GRB(xrf) 011211 [GCN 1188,1191]
was observed under clear sky conditions using the
2.34m as well as 1-m telescopes at VBO, kavalur.
on 12th and 13th Dec, 2001
Aperture photometry using USNO star (Jensen et al, GCN 1195)
for some of the (VBT) images follows
Dec 12.9006 R 600s 20.77 +- 0.06
Dec 12.9403 V 1200s 21.59 +- 0.06
Dec 12.9819 B 1800s 22.07 +- 0.09
Dec 12.9979 R 600s 21.12 +- 0.08
this message may be cited.
- GCN notice #1203
F. Fiore, G.L. Israel, L.A. Antonelli, L. Stella (OA Roma), S. Covino,
P. Saracco, G. Ghisellini (OA Brera), A. Buzzoni, T. Oliva (TNG),
E. Pian (OA Trieste), E. Palazzi, N. Masetti (ITeSRe, CNR, Bologna)
on behalf of a larger collaboration, report:
"Spectra of the OT (Grav et al.: GCN #1191) of GRB011211 in the
350-750nm range (total exposure time of about 1hr) were obtained with
the 3.5m Telescopio Nazionale Galileo (TNG) equipped with DOLORES +
grism #1 on Dec. 13.27 (UT). The source was relatively faint, V~21.7,
and the signal to noise of our spectra does not allow the detection
of faint absorption lines. The continuum is peaked in the blue band,
and consistent with the V-R of 0.2 measured by Soszynski et al.
(GCN #1199) at the time of the TNG observation. A break is evident
shortward of about 400nm which may be interpreted as Lyman-alpha
forest blanketing at a redshift of about z=2.1, consistent with
that reported by Fruchter et al. (GCN #1200).
Further analysis is in progress.
This message may be cited."
- GCN notice #1204
GRB 011211: Evidence for an Optical Break
S. Holland (Notre Dame), P. Berlind, D. Bersier, S. Jha, K. Z. Stanek
(Harvard-Smithsonian Center for Astrophysics), I. Soszynski (Warsaw
University Observatory), P. M. Garnavich (Notre Dame) report:
We have obtained deep VRI images of the field containing GRB
011211 using the 1.2-meter telescope with the 4Shooter at the Fred
Lawrence Whipple Observatory on Dec. 14.5 UT. The optical afterglow
of GRB 011211 is not visible on any of our images. The predicted
magnitudes, based on the power-law fits of Soszynski et al. (2001, GCN
1199), and the estimated limiting magnitudes of our images are give
below.
Filter Predicted Limiting Magnitude
V 22.10 22.3 +/- 0.2
R 21.99 22.4 +/- 0.2
I 21.25 21.0 +/- 0.2
These magnitudes are relative to the VRI magnitudes for USNO star
U0675_11427359 given by Henden (2001, GCN 1197).
Our non-detection suggests that there has been a break in the
light curve of the optical afterglow of GRB 011211. The break
occurred between 1.5 and 2.7 days after the burst (between Dec. 13.3
and Dec. 14.5). The R-band limiting magnitude suggests that the slope
after the break is at least -1.4. The V- and I-band limiting
magnitudes are consistent with no break.
This message may be cited.
- GCN notice #1209
M. Gladders (OCIW), S. Holland, P. M. Garnavich (Notre Dame),
S. Jha, K. Z. Stanek, D. Bersier (CfA), L. F. Barrientos (U. Catolica)
Spectra of the candidate afterglow of GRB 011211 (Grav et al. GCN 1191)
were obtained with the Magellan 6.5m Walter Baade telescope and
LDSS-2 imaging spectrograph on 2001, Dec. 13.3 (UT). The spectra
cover the range 400 nm to 900 nm at a resolution of 1.2 nm (FWHM).
Four exposures, each with an exposure time of 620s, were fully reduced
and combined. The final spectrum shows a smooth continuum
except for a number of narrow absorption lines in the blue.
Observed ID z
-------- --------- ----
524.8 nm Al II (167.1) 2.141
486.5 C IV (154.9) 2.141
479.4 Si II (152.7) 2.140
439.3 Si IV (139.8) 2.142
409.1 O I/Si II (130.3) 2.140
A broad, unidentified feature is seen at 460.0 nm (146.5 nm rest frame).
These identifications confirm the redshift of z=2.14 found by
Fruchter et al. (GCN 1200).
R-band images were also obtained in imaging mode on
Dec. 12 and 13 (UT). Assuming R=17.76 U0675_11427359
given by Henden (2001, GCN 1197) we find the following
magnitudes for the probable afterglow:
Dec. 12.25 20.28 +/-0.02
Dec. 12.34 20.58 +/-0.02
Dec. 13.31 21.46 +/-0.04
which provide a power law index of 0.9, consistent with the
optical decline rates found by Soszynski et al. (GCN 1199) for
the same time interval.
The fits images and spectra are available at
http://www.astro.utoronto.ca/~gladders/GRB/
This message may be cited.
- GCN notice #1211
V. Simon, R. Hudec (Astronomical Institute AV CR, Ondrejov) and
G. Pizzichini, N. Masetti (ITESRE, Bologna) report:
We have determined the color indices of the optical afterglow of
GRB011211 from the available data (GCN 1199, GCN 1200, GCN 1209),
using the calibration by Henden et al. (GCN 1197). The interpolation
method described in Simon et al. (2001, A&A, 377, 450) was used. The
indices of the afterglow of GRB011211 are:
t-To=0.503 days: V-R=0.39; R-I=0.42
t-To=1.183 days: B-V=0.52; V-R=0.44; R-I=0.53
t-To=1.463 days: V-R=0.28; R-I=0.60
The typical error of these indices is about 0.10 - 0.15 mag.
The Galactic reddening E(B-V)=0.042, determined from the maps by
Schlegel et al. (1998, ApJ, 500, 525), is comparable to the
errors of the measurements and can be neglected here.
These indices are close to the mean values of a sample of 17
afterglows (Simon et al. 2001) which yield (B-V)o=0.47+/-0.17,
(V-R)o=0.40+/-0.13, (R-I)o=0.46+/-0.18. This suggests that the
shape of the spectrum of the afterglow of GRB011211 is very similar
to the other afterglows and that its intrinsic reddening (that is
inside the host galaxy) must be again quite small (Simon et al.
2001). The search for the host galaxy and the determination
of its type are therefore encouraged.
- GCN notice #1213
GRB011211: Detection of the Probable Host Galaxy
Ingunn Burud, James Rhoads, Andrew Fruchter (STScI) and
Jens Hjorth (Copenhagen) report on behalf of
GRACE (Gamma-Ray Afterglow Collaboration at Eso):
We have obtained a deep R-band image (1 hour integration) of
GRB011211 from the VLT+FORS2 on Dec. 21.79 in 0."65 seeing.
We find that the source at the position of the afterglow is now
an extended object. By deconvolving the image (using the technique
of Magain, Courbin & Sohy, 1998, ApJ, 494, 452) we find the OT
to be superposed on an apparent host galaxy. The OT is offset
from the center of the host by 0."5 to the southeast.
The total magnitude of the system is R = 24.2 +/- 0.2, with the
magnitude of the host estimated at R = 25.0 +/- 0.3 and that of the
OT R = 24.8 +/- 0.3.
The image may be found at:
http://www.stsci.edu/~burud/Web/GRB/grb011211.html
- GCN notice #1214
S. Covino, G. Ghisellini, P. Saracco, G. Tagliaferri, F. Zerbi
(Observ. of Brera, Milan, Italy); S. Di Serego, A. Cimatti (Observ. of Arcetri,
Florence, Italy); F. Fiore, G.L. Israel, L. Stella (Observ. of Monte Porzio,
Rome, Italy); N. Kawai (RICHEN, Japan); D. Lazzati (IoA, Cambridge, UK); S.
Ortolani (University of Padua, Italy); L. Pasquini (ESO, Garching, Munich,
Germany); G. Ricker (MIT, USA); R. Gilmozzi, E. Pompei (ESO, Paranal, Chile)
report:
On 2001 December 13.29 we observed the optical counterpart to the X-ray
rich GRB011211 that was reported by Grav et al. (GCN 1191). The observations
were performed with the ESO VLT-3 (Melipal) telescope equipped with FORS1
with a Bessel R band filter in the imaging polarimetry mode. The transient
source is clearly detected and the acquisition image allowed to derive the
Bessel V magnitude of the transient, V=21.81 +/- 0.06, with respect to the
USNO star U0675_11427359 (Henden, GCN 1197).
Polarimetric measurements were performed by means of PSF fitting and
aperture techniques for the optical transient and a number of field stars in
order to estimate the average Galactic dust induced field polarization.
The result is that the optical transient polarization is consistent with zero
within the observational uncertainties. We estimate an upper limit to the
linear polarization of the OT of about 2.5%. Further analyses are in progress.
A plot in the Q and U Stokes' vector plane for the field objects is shown at
the URL:
http://www.merate.mi.astro.it/~covino/GRB011211/GRB_POL.jpg.
The OT is in red.
This message is citeable.
- GCN notice #1215
F. Frontera, Physics Dept. University of Ferrara, Ferrara and Istituto
Astrofisica Spaziale and Fisica Cosmica (IASF), CNR, Bologna; L. Amati,
IASF, CNR, Bologna; C. Guidorzi and E. Montanari, Physics Dept,
University of Ferrara; E. Costa, M. Feroci, L. Piro, IASF, CNR, Rome; J.
Heise, Space Research Organization Netherlands (SRON), Utrecht; and J.J.M.
in 't Zand, Astronomical Institute and SRON, Utrecht, report:
With reference to the GRB011211(=XRF011211) (GCN 1188, 1189), a detailed
analysis of the BeppoSAX GRBM data shows a very shallow long event in the
40-700 keV band with two peaks and a total duration of about 270 s,
similar to that measured in X-rays (2-28 keV) with the BeppoSAX WFC. The
quick look analysis could not single out such long and faint signal. The
40--700 peak flux (with 8 s bins) is about 0.5 x10^-7~erg/cm^2 s, while
its fluence is about 5x10^-6 erg/cm^2. The X/gamma fluence ratio is
similar to that found in a number of ordinary GRBs detected by BeppoSAX.
The distinguishing features of GRB011211 are its long duration (the
longest event localized with BeppoSAX) and its faintness both in X- and
gamma-rays. We conclude that this event cannot be classified as an X--ray
flash. From the measured redshift (z = 2.14, Fruchter et al. GCN 1200),
the gamma ray energy released, assuming isotropy, is 6.3x10^52 erg,
assuming a Friedman-Robertson-Walker cosmology with H0=65 Km/s Mpc and
Omega_m=0.3.
This message can be cited.
- GCN notice #1303
A. Henden (USRA/USNO) reports on behalf of the USNO GRB team:
We have acquired additional BVRcIc all-sky photometry for
an 11x11 arcmin field that is approximately centered on
the position of the optical transient for GRB011211 reported
by Grav et al. (GCN 1191) with the USNOFS 1.0-m telescope.
The field was observed on two more nights,
with the new dataset posted at:
ftp://ftp.nofs.navy.mil/pub/outgoing/aah/grb/grb011211.dat
Stars brighter than V=13.5 are saturated and should be used with care.
The current photometry has a potential external zero-point
error of about one percent. The astrometry in this file
is based on linear plate solutions with respect to USNO-A2.0.
The internal errors are less than 100mas.
The two new nights have shown that the photometry
reported in GCN 1197 has larger error than originally estimated,
most likely caused by a combination of the very poor seeing,
high airmass and approaching dawn. For example, the
comparison star U0675_11427359 that was used by Grav et al.and
Jensen et al. (GCN 1195) to calibrate their field can be found
in the new .dat file with the following magnitudes:
GCN 1195 (Jensen) B = 18.65 V = 18.18 R = 17.90 I = 17.07
GCN 1197 (Henden) B = 18.65 V = 18.11 R = 17.76 I = 17.42
new result B = 18.48 V = 18.00 R = 17.70 I = 17.37
We apologize for the lateness of this correction, but this
winter has had unusually few photometric nights. This is
the first case in several dozen calibrations that we have
performed for the GRB community in which the final dataset
differed from the initial dataset by more than a couple of percent.
- GCN notice #1311
D.W. Fox, J.S. Bloom, and S.R. Kulkarni (Caltech) report on behalf of
a larger collaboration:
"We have imaged the optical afterglow (GCN 1191) and presumed host
galaxy of GRB011211 (GCN 1215) with the Hubble Space Telescope and
STIS (Clear) instrument for 5133s on December 25.8 UT. The host
galaxy is clearly detected and extends for roughly 0.5 arcsec
northeast of the afterglow.
Our observations confirm the result of Burud et al. (GCN 1213), with
the caveat that the afterglow offset is approximately 0.3 arcsec and
to the southwest rather than the southeast of the host galaxy.
A GIF image of the near field may be found at:
http://www.astro.caltech.edu/~derekfox/grb011211/
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