- GCN NOTICE
TITLE: GCN/FERMI NOTICE
NOTICE_DATE: Thu 02 May 13 07:51:37 UT
NOTICE_TYPE: Fermi-GBM Flight Position
RECORD_NUM: 44
TRIGGER_NUM: 389173874
GRB_RA: 57.817d {+03h 51m 16s} (J2000),
58.096d {+03h 52m 23s} (current),
56.775d {+03h 47m 06s} (1950)
GRB_DEC: +59.767d {+59d 46' 00"} (J2000),
+59.806d {+59d 48' 22"} (current),
+59.616d {+59d 36' 59"} (1950)
GRB_ERROR: 14.88 [deg radius, statistical plus systematic]
GRB_INTEN: 109 [cnts/sec]
DATA_SIGNIF: 7.00 [sigma]
INTEG_TIME: 2.048 [sec]
GRB_DATE: 16414 TJD; 122 DOY; 13/05/02
GRB_TIME: 28271.76 SOD {07:51:11.76} UT
GRB_PHI: 236.98 [deg]
GRB_THETA: 35.00 [deg]
DATA_TIME_SCALE: 2.0480 [sec]
HARD_RATIO: 1.11
LOC_ALGORITHM: 3 (version number of)
MOST_LIKELY: 51% Distant Particles
2nd_MOST_LIKELY: 45% GRB
DETECTORS: 0,0,0, 0,0,0, 1,1,0, 0,0,0, 0,0,
SUN_POSTN: 39.64d {+02h 38m 33s} +15.46d {+15d 27' 32"}
SUN_DIST: 46.36 [deg] Sun_angle= -1.2 [hr] (East of Sun)
MOON_POSTN: 311.15d {+20h 44m 36s} -12.63d {-12d 37' 43"}
MOON_DIST: 109.39 [deg]
MOON_ILLUM: 52 [%]
GAL_COORDS: 143.84, 4.41 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 69.95, 38.55 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS: Fermi-GBM Flight-calculated Coordinates.
COMMENTS: This trigger occurred at longitude,latitude = 72.32,-24.93 [deg].
- GCN NOTICE
TITLE: GCN/FERMI NOTICE
NOTICE_DATE: Thu 02 May 13 07:51:50 UT
NOTICE_TYPE: Fermi-GBM Flight Position
RECORD_NUM: 57
TRIGGER_NUM: 389173874
GRB_RA: 51.150d {+03h 24m 36s} (J2000),
51.443d {+03h 25m 46s} (current),
50.058d {+03h 20m 14s} (1950)
GRB_DEC: +64.633d {+64d 37' 60"} (J2000),
+64.680d {+64d 40' 47"} (current),
+64.457d {+64d 27' 24"} (1950)
GRB_ERROR: 4.25 [deg radius, statistical plus systematic]
GRB_INTEN: 1031 [cnts/sec]
DATA_SIGNIF: 49.90 [sigma]
INTEG_TIME: 1.024 [sec]
GRB_DATE: 16414 TJD; 122 DOY; 13/05/02
GRB_TIME: 28271.76 SOD {07:51:11.76} UT
GRB_PHI: 243.00 [deg]
GRB_THETA: 40.00 [deg]
DATA_TIME_SCALE: 1.0240 [sec]
HARD_RATIO: 0.38
LOC_ALGORITHM: 3 (version number of)
MOST_LIKELY: 58% Distant Particles
2nd_MOST_LIKELY: 39% GRB
DETECTORS: 0,0,0, 0,0,0, 1,1,0, 0,0,0, 0,0,
SUN_POSTN: 39.64d {+02h 38m 33s} +15.46d {+15d 27' 33"}
SUN_DIST: 49.88 [deg] Sun_angle= -0.8 [hr] (East of Sun)
MOON_POSTN: 311.15d {+20h 44m 36s} -12.63d {-12d 37' 41"}
MOON_DIST: 105.79 [deg]
MOON_ILLUM: 52 [%]
GAL_COORDS: 138.43, 6.47 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 68.01, 44.13 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS: Fermi-GBM Flight-calculated Coordinates.
COMMENTS: This trigger occurred at longitude,latitude = 72.32,-24.93 [deg].
- GCN NOTICE
TITLE: GCN/FERMI NOTICE
NOTICE_DATE: Thu 02 May 13 07:51:55 UT
NOTICE_TYPE: Fermi-GBM Flight Position
RECORD_NUM: 68
TRIGGER_NUM: 389173874
GRB_RA: 52.650d {+03h 30m 36s} (J2000),
52.946d {+03h 31m 47s} (current),
51.547d {+03h 26m 11s} (1950)
GRB_DEC: +64.667d {+64d 40' 00"} (J2000),
+64.712d {+64d 42' 42"} (current),
+64.496d {+64d 29' 44"} (1950)
GRB_ERROR: 4.00 [deg radius, statistical plus systematic]
GRB_INTEN: 1407 [cnts/sec]
DATA_SIGNIF: 138.20 [sigma]
INTEG_TIME: 4.096 [sec]
GRB_DATE: 16414 TJD; 122 DOY; 13/05/02
GRB_TIME: 28271.76 SOD {07:51:11.76} UT
GRB_PHI: 243.00 [deg]
GRB_THETA: 40.00 [deg]
DATA_TIME_SCALE: 4.0960 [sec]
HARD_RATIO: 0.54
LOC_ALGORITHM: 3 (version number of)
MOST_LIKELY: 59% Distant Particles
2nd_MOST_LIKELY: 38% GRB
DETECTORS: 0,0,0, 0,0,0, 1,1,0, 0,0,0, 0,0,
SUN_POSTN: 39.64d {+02h 38m 33s} +15.46d {+15d 27' 33"}
SUN_DIST: 50.08 [deg] Sun_angle= -0.9 [hr] (East of Sun)
MOON_POSTN: 311.15d {+20h 44m 37s} -12.63d {-12d 37' 40"}
MOON_DIST: 106.43 [deg]
MOON_ILLUM: 52 [%]
GAL_COORDS: 138.94, 6.86 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 68.87, 43.94 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS: Fermi-GBM Flight-calculated Coordinates.
COMMENTS: This trigger occurred at longitude,latitude = 72.32,-24.93 [deg].
- GCN Circular #14530
A. Von Kienlin (MPE) and G. Younes (NASA/USRA) report on behalf of the Fermi GBM Team:
"At 07:51:11.76 UT on April 2 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130502B (trigger 389173874 / 130502327).
The on-ground calculated location, using the GBM trigger
data, is RA = 74.5, DEC = 70.6 (J2000 degrees), with an uncertainty
of 1.0 degree (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 47 degrees.
This burst was also independently detected by INTEGRAL SPI-ACS.
The GBM light curve consists of multiple spikes
with a duration (T90) of about 24 s (50-300 keV).
The time-averaged spectrum from T0-4.1 s to T0+71.7 s is
best fit by a Band function with Epeak = 323.00 +/- 7.00 keV,
alpha = -0.75 +/- 0.01, and beta = -2.47 +/- 0.07.
The event fluence (10-1000 keV) in this time interval is
(1.21 +/- 0.01)E-04 erg/cm^2. The 1.024 sec peak photon flux
measured starting from T0+30.3 s in the 8-1000 keV band
is 45.8 +/- 0.5 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
- GCN Circular #14532
GRB 130502B: Fermi-LAT detection of a burst
D. Kocevski (NASA/GSFC), G. Vianello (Stanford), J. Chiang (SLAC), J. Racusin (NASA/GSFC), and E. Troja (CRESST) report on behalf of the Fermi-LAT team:
At 07:51:11 UT on 2nd May 2013, Fermi-LAT detected high energy emission from GRB 130502B, which was also detected by Fermi-GBM (trigger 389173874/130502327) (GCN 14530) .
The best LAT on-ground location is found to be RA, DEC 66.648, 71.0841 (J2000) with an error radius of 0.093 deg (68% containment, statistical error only), this was about ~45 deg from the LAT boresight at the time of the trigger. The data from the Fermi-LAT show a multi-peaked light curve consistent with the GBM data. More than 100 photons above 100 MeV are observed within 200 seconds with a TS of > 158. The multi-peak structure is clearly seen in the non-standard LAT Low Energy (LLE) data selection, with a significance of ~8 sigma. The highest energy LAT photon consistent with the burst position has an energy of 30 GeV and arrived ~220s after the trigger.
A Swift TOO request has been submitted.
The Fermi LAT point of contact for this burst is Daniel Kocevski (daniel.kocevski@nasa.gov).
The Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
- GCN Circular #14540
A. Melandri (INAF-OAB) and S. Immler (NASA/CRESST/GSFC) report on behalf of the Swift-XRT team:
We have analysed 3.4 ks of XRT data for the Fermi/LAT-detected burst:
GRB 130502B, from 55.1 ks to 67.9 ks after the Fermi/LAT trigger. The
data are entirely in Photon Counting (PC) mode. An X-ray source is
detected within the Fermi/LAT error circle. Using 3614 s of PC mode
data and 6 UVOT images, we find an enhanced XRT position (using the
XRT-UVOT alignment and matching UVOT field sources to the USNO-B1
catalogue): RA, Dec = 66.76207, +71.06071 which is equivalent to:
RA (J2000): 04h 27m 02.90s
Dec(J2000): +71d 03' 38.5"
with an uncertainty of 1.5 arcsec (radius, 90% confidence). This
position is 157 arcsec from the Fermi/LAT position. The light curve is
consistent with a constant source of mean count rate 1.1e-01 ct/sec. A
power-law fit gives an index of 0.8 (+/-1.3).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.88 (+0.28, -0.26). The
best-fitting absorption column is 2.8 (+1.0, -0.9) x 10^21 cm^-2, in
excess of the Galactic value of 1.1 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 4.3 x 10^-11 (6.3 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 2.8 (+1.0, -0.9) x 10^21 cm^-2
Galactic foreground: 1.1 x 10^21 cm^-2
Excess significance: 3.1 sigma
Photon index: 1.88 (+0.28, -0.26)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020266.
This circular is an official product of the Swift-XRT team.
- GCN Circular #14541
S. B. Cenko (UC Berkeley), D. A. Perley, and L. P. Singer (Caltech) report
on behalf of a larger collaboration:
We imaged the field of the Fermi GBM (Von Kienlin et al., GCN 14530) and
LAT (Kocevski et al., GCN 14532) GRB130502B with the robotic Palomar 60
inch telescope. Observations began at 03:34 UT on 3 May 2013 (~ 0.82 d
after the GBM trigger) and were obtained under poor seeing conditions. We
detect no significant emission at the position of the candidate X-ray
afterglow (Melandri et al., GCN 14540). Using nearby point sources from
the USNO-B1 catalog for reference, we measure an upper limit of r' > 20.4
mag at this time.
- GCN Circular #14542
S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:
The long-duration intense GRB 130502B
(Fermi-GBM detection: von Kienlin et al., GCN 14530;
Fermi-LAT detection: Kocevski et al., GCN 14532)
triggered Konus-Wind at T0=3D28272.763s UT (07:51:12.763)
The light curve shows a bright multi-peaked structure
from ~T0 s to ~T0+30s.
The emission is seen up to 10 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130502_T28272/
As observed by Konus-Wind, the burst
had a fluence of (1.13 =B1 0.04)x10-4 erg/cm2,
and a 64-ms peak flux, measured from T0+29.944s,
of (1.81 =B1 0.08)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The time-integrated spectrum (measured from T0 to T0+27.392 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.84 =B1 0.04,
the high energy photon index beta = -2.7 =B1 0.1,
the peak energy Ep =3D 293 =B1 9 keV,
chi2 = 107/91 dof.
The spectrum at the maximum count rate
(measured from T0+26.624 to T0+27.392 s)
is best fit in the 20 keV - 15 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -0.81 =B1 0.06,
the peak energy Ep =3D 264 =B1 14 keV,
chi2 = 104/93 dof.
All the quoted results are preliminary.
- GCN Circular #14544
A. A. Breeveld (MSSL-UCL) and S. Immler (NASA/CRESST/GSFC)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 130502B
55101 s after the LAT trigger (Kocevski et al., GCN Circ. 14532). No
optical afterglow consistent with the refined XRT position (Melandri et
al., GCN Circ. 14540) is detected in the UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial
exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
white_FC 55101 55208 105 >20.3
white 55101 89746 4493 >22.1
The magnitudes in the table are not corrected for the Galactic
extinction due to the reddening of E(B-V) = 0.21 in the direction of the
burst (Schlegel et al. 1998).
- GCN Circular #14546
K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team,
S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks,
D. Svinkin, and T. Cline on behalf of the Konus-Wind team,
D. M. Smith, on behalf of the RHESSI GRB team,
A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C.
Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,
K. Yamaoka, M. Ohno, Y. Hanabata, Y. Fukazawa, T. Takahashi, M. Tashiro,
Y. Terada, T. Murakami, and K. Makishima on behalf of the Suzaku WAM team,
S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer, on behalf of
the Swift-BAT team,
E. Del Monte, I. Donnarumma, Y. Evangelista, M. Feroci, I. Lapshov,
F. Lazzarotto, and M. Marisaldi, on behalf of the AGILE Team, and
V. Connaughton, M. S. Briggs, C. Meegan, and V. Pelassa,
on behalf of the Fermi GBM team, report:
GRB 130502B (von Kienlin et al., GCN 14530, Kocevski et al., GCN 14532,
Golenetskii et al., GCN 14542) has been observed by AGILE MCAL, Fermi
GBM, INTEGRAL (SPI-ACS), Konus-Wind, MESSENGER (GRNS), RHESSI, Suzaku
WAM, and Swift BAT (outside the coded field of view), so far. We have
triangulated it to a long, narrow error box which reduces the
size of the LAT (statistical-only) error circle (GCN 14532) and produces
the following error box:
RA(2000) DEC(2000)
CENTER: 66.6391 deg = 04 h 26 m 33 s 71.0809 deg = 71 d 04 ' 51 "
CORNERS: 66.8800 deg = 04 h 27 m 31 s 71.0295 deg = 71 d 01 ' 46 "
66.4487 deg = 04 h 25 m 48 s 71.1511 deg = 71 d 09 ' 04 "
66.8267 deg = 04 h 27 m 18 s 71.0114 deg = 71 d 00 ' 41 "
66.4008 deg = 04 h 25 m 36 s 71.1314 deg = 71 d 07 ' 53 "
The area of this box is about 17 square arcminutes, and it contains the
Swift-XRT source (Melandri et al., GCN 14540). Maps have been posted at
ssl.berkeley.edu/ipn3/130502
The triangulation can be improved.
- GCN Circular #14552
D. Malesani (DARK/NBI), P. D'Avanzo (INAF/OABr), S. Covino (INAF/OABr),
A. Melandri (INAF/OABr), V. D'Elia (INAF/OAR and ASI/ASDC), S. Campana
(INAF/OABr), D. Fugazza (INAF/OABr), G. Tagliaferri (INAF/OABr), B. Blu,
L. Di Fabrizio (INAF/FGG), C. P. Padilla-Torres (INAF/FGG), report on
behalf of the CIBO collaboration:
We observed the field of the LAT-detected GRB 130502B (Von Kienlin &
Younes, GCN 14530; Kocevski et al., GCN 14532; Golenetskii et al., GCN
14542) with the TNG equipped with the DOLoRes imager. Observations were
carried out starting on 2013 May 3.872 UT (1.54 days after the trigger),
for a total of 30 min on source in the R band, at a high airmass of
around 2.2. The seeing was 1.2".
No bright object is detected inside the X-ray error circle (Melandri &
Immler, GCN 14540; see also http://www.swift.ac.uk/xrt_positions/), down
to a 3-sigma limit of R = 23.7 (calibration based on several nearby USNO
stars). However, a faint flux enhancement is seen consistent with the
XRT position, at coordinates (J2000):
RA = 04:27:02.82
Dec = +71:03:38.5
A finding chart is shown at
http://www.astro.ku.dk/~malesani/GRB/130502B/GRB130502B_finder.jpg
We estimate the magnitude of this marginally detected source to be R =
24.7 +- 0.5. At the moment, we have no information about its
variability, and it could be either the GRB counterpart or its host galaxy.
Last, independently of the reality of the object, this GRB can be
classified as dark. Considering the limit R > 23.7, and a Galactic
extinction A_V = 0.57 (Schlafly & Finkbeiner 2011, ApJ, 737, 103), the
optical-to-X-ray spectral index is beta_OX < 0.47 (if the object is
real, then beta_OX = 0.34 +- 0.07). The presence of significant excess
column density in the X-ray spectrum (Melandri & Immler, GCN 14540; see
also https://www.swift.ac.uk/team/xrt_spectra/00020266/) suggests an
extinguished event.
- GCN Circular #14555
A. Melandri (INAF-OAB) and S. Immler (NASA/CRESST/GSFC) report on
behalf of the Swift-XRT team:
We have analysed 8.3 ks of XRT data for the Fermi/LAT-detected burst:
GRB 130502B (Kocevski et al. GCN Circ. 14532), from 55.1 ks to 101.8
ks after the Fermi/LAT trigger.
The object dectected in the first 3.4 ks of XRT data (Melandri &
Immler GCN Circ. 14540) is now clearly fading. The light curve can be
modelled with a power-law decay with a decay index of alpha=1.52
(+/-0.25).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.89 (+/-0.20). The best-
fitting absorption column is 1.73 (+0.78, -0.71) x 10^21 cm^-2, in
addition to the Galactic value of 1.1 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 4.3 x 10^-11 (6.3 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Galactic foreground: 1.1 x 10^21 cm^-2
Intrinsic column: 1.73 (+0.78, -0.71) x 10^20 cm^-2
Photon index: 1.89 (+0.21, -0.20)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020266.
This circular is an official product of the Swift-XRT team.
- GCN Circular #14557
T. Yasuda, M. Tashiro, Y. Terada, Y. Ishida, H. Ueno,
S. Sugimoto (Saitama U.), M. Ohno, K. Takaki, T. Kawano,
R. Nakamura, S. Furui, Y. Fukazawa (Hiroshima U.),
M. Yamauchi, N. Ohmori, M. Akiyama (Univ. of Miyazaki),
K. Yamaoka (Nagoya U.), S. Sugita (Ehime U.),
Y. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA),
W. Iwakiri(RIKEN), Y. Hanabata (ICRR),
Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo)
on behalf of the Suzaku WAM team, report:
The bright, long GRB 130502B (Fermi-GBM detection : von Kienlin and
Younes, GCN 14530; Fermi-LAT detection : Kocevski et al., GCN 14532)
triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 07:51:15.113 UT (=T0).
The observed light curve shows a multi-peaked structure starting at
T0-2 s, ending at T0+34 s with a duration (T90) of about 24 seconds.
The fluence in 100 - 1000 keV was 7.38 (+0.37/-0.29) x10-5 erg/cm^2.
The 1-s peak flux measured from T0+22 s was
14.53 (-0.77/+0.73) photons/cm^2/s in the same energy range.
Preliminary result shows that the time-averaged spectrum from
T0-2 s to T0+34 s is well fitted by a GRB Band model as follows.
the low-energy photon index alpha: -1.04 (+0.49/-0.36),
the high-energy photon index beta: -2.73 (+0.10/-0.12),
and the peak energy Epeak: 359 (+22/-33) keV (chi^2/d.o.f = 65.7/50).
Due to the high flux of this burst, a 3% systematic error was added
for low energy channels.
All the errors are quoted at 90% confidence level.
The light curves for this burst are available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html
- GCN Circular #14591
K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team,
S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks,
D. Svinkin, and T. Cline on behalf of the Konus-Wind team,
I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,
W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on
behalf of the GRS-Odyssey GRB team,
D. M. Smith, on behalf of the RHESSI GRB team,
A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C.
Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,
K. Yamaoka, M. Ohno, Y. Hanabata, Y. Fukazawa, T. Takahashi, M. Tashiro,
Y. Terada, T. Murakami, and K. Makishima on behalf of the Suzaku WAM team,
S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer, on behalf of
the Swift-BAT team,
E. Del Monte, I. Donnarumma, Y. Evangelista, M. Feroci, I. Lapshov,
F. Lazzarotto, and M. Marisaldi, on behalf of the AGILE Team, and
V. Connaughton, M. S. Briggs, C. Meegan, and V. Pelassa,
on behalf of the Fermi GBM team, report:
GRB 130502B (von Kienlin et al., GCN 14530, Kocevski et al., GCN 14532,
Golenetskii et al., GCN 14542, Hurley et al. 14546) was also observed by
Odyssey. Using Odyssey data reduces the size of the previous error box
by about a factor of two:
RA(2000) DEC(2000)
CENTER: 66.714= 4 h 26 m 51 s 71.066= 71 d 03 ' 58 "
CORNERS: 66.893= 4 h 27 m 34 s 71.032= 71 d 01 ' 55 "
67.092= 4 h 28 m 21 s 70.975= 70 d 58 ' 29 "
66.334= 4 h 25 m 20 s 71.156= 71 d 09 ' 22 "
66.535= 4 h 26 m 08 s 71.100= 71 d 05 ' 59 "
The area of this box is about 8 square arcminutes, and it still contains the
Swift-XRT source (Melandri et al., GCN 14540). A new map has been posted at
ssl.berkeley.edu/ipn3/130502
Some improvement in this error box is possible.
Previous IAU Circulars 
