TITLE: GCN CIRCULAR
NUMBER: 35475
SUBJECT: GRB 240102A: Swift/UVOT Upper Limits
DATE: 24/01/03 15:38:51 GMT
FROM: Alexander Belles at PSU <aub1461(a)psu.edu>
A. Belles (PSU) and J. D. Gropp (PSU)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 240102A
113 s after the BAT trigger (Gropp et al., GCN Circ. 35461).
No optical afterglow consistent with the XRT position
(Goad et al., GCN Circ. 35471) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
white_FC 135 285 147 >20.7
u_FC 294 544 246 >19.9
white 135 1196 353 >21.1
v 113 1246 90 >18.8
b 550 1172 58 >19.5
u 294 1314 299 >20.0
w1 676 1295 78 >19.0
m2 823 1270 58 >18.7
w2 600 1221 78 >19.3
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.176 in the direction of the burst
(Schlegel et al. 1998).
View this GCN Circular online at https://gcn.nasa.gov/circulars/35475.
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TITLE: GCN CIRCULAR
NUMBER: 35474
SUBJECT: GRB 231230A: Swift-BAT refined analysis
DATE: 24/01/03 14:07:21 GMT
FROM: Hans Krimm at NSF/NASA-GSFC <hkrimm(a)nsf.gov>
S. Laha (GSFC/UMBC), S. D. Barthelmy (GSFC), H. A. Krimm (NSF),
A. Y. Lien (U Tampa), C. B. Markwardt (GSFC), M. J. Moss (GSFC),
D. M. Palmer (LANL), T. Parsotan (GSFC/UMBC), T. Sakamoto (AGU),
M. Stamatikos (OSU) (i.e. the Swift-BAT team):
Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 231230A (trigger #1205319)
(Moss, et al., GCN Circ. 35436). The BAT ground-calculated position is
RA, Dec = 245.223, 58.132 deg which is
RA(J2000) = 16h 20m 53.5s
Dec(J2000) = +58d 07' 54.2"
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 35%.
The mask-weighted light curve shows a complex structure extending from
around T+0 to T+20. T90 (15-350 keV) is 15.2 +- 0.9 sec (estimated error including systematics).
The time-averaged spectrum from T+0.26 to T+17.26 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.28 +- 0.10. The fluence in the 15-150 keV band is 2.1 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+7.64 sec in the 15-150 keV band
is 2.2 +- 0.4 ph/cm2/sec. All the quoted errors are at the 90% confidence
level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1205319/BA/
View this GCN Circular online at https://gcn.nasa.gov/circulars/35474.
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TITLE: GCN CIRCULAR
NUMBER: 35473
SUBJECT: GRB 240101A: Swift-BAT refined analysis
DATE: 24/01/03 14:06:48 GMT
FROM: Hans Krimm at NSF/NASA-GSFC <hkrimm(a)nsf.gov>
A. Y. Lien (U Tampa), S. D. Barthelmy (GSFC), S. B. Cenko (GSFC),
H. A. Krimm (NSF), S. Laha (GSFC/UMBC), C. B. Markwardt (GSFC),
M. J. Moss (GSFC), D. M. Palmer (LANL), T. Parsotan (GSFC/UMBC),
T. Sakamoto (AGU), M. Stamatikos (OSU) (i.e. the Swift-BAT team):
Using the data set from T-10 to T+242 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 240101A (trigger #1205708)
(Cenko, et al., GCN Circ. 35448). The trigger time, which was unavailable in the
first circular was 2024-01-01 at 14:20:17.331 UTC. The BAT ground-calculated position is
RA, Dec = 10.289, 8.540 deg which is
RA(J2000) = 00h 41m 09.5s
Dec(J2000) = +08d 32' 25.3"
with an uncertainty of 3.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 66%.
The mask-weighted light curve shows a weak, complex structure lasting from
About T-5 to T+10 seconds. T90 (15-350 keV) is 15.8 +- 6.1 sec (estimated error
including systematics).
The time-averaged spectrum from T-1.94 to T+20.28 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
2.03 +- 0.34. The fluence in the 15-150 keV band is 3.3 +- 0.7 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+2.11 sec in the 15-150 keV band
is 0.9 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence
level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1205708/BA/
View this GCN Circular online at https://gcn.nasa.gov/circulars/35473.
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TITLE: GCN CIRCULAR
NUMBER: 35472
SUBJECT: GRB 240101B: Swift-BAT refined analysis
DATE: 24/01/03 14:03:29 GMT
FROM: Hans Krimm at NSF/NASA-GSFC <hkrimm(a)nsf.gov>
C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), S. B. Cenko (GSFC),
H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa),
M. J. Moss (GSFC), D. M. Palmer (LANL), T. Parsotan (GSFC/UMBC),
T. Sakamoto (AGU), M. Stamatikos (OSU) (i.e. the Swift-BAT team):
Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 240101B (trigger #1205744)
(Cenko, et al., GCN Circ. 35449). The BAT ground-calculated position is
RA, Dec = 352.147, 51.646 deg which is
RA(J2000) = 23h 28m 35.3s
Dec(J2000) = +51d 38' 46.9"
with an uncertainty of 3.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
The mask-weighted light curve shows a single peak from approximately T+0
To T+18 seconds. There is a possible precursor at T-50 sec.
T90 (15-350 keV) is 43.1 +- 12.6 sec (estimated error including systematics).
The time-averaged spectrum from T+2.18 to T+48.32 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.70 +- 0.26. The fluence in the 15-150 keV band is 4.6 +- 0.8 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+10.28 sec in the 15-150 keV band
is 0.5 +- 0.1 ph/cm2/sec. All the quoted errors are at the 90% confidence
level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1205744/BA/
View this GCN Circular online at https://gcn.nasa.gov/circulars/35472.
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TITLE: GCN CIRCULAR
NUMBER: 35471
SUBJECT: GRB 240102A: Enhanced Swift-XRT position
DATE: 24/01/03 10:00:18 GMT
FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk>
M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester)
report on behalf of the Swift-XRT team.
Using 4654 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 240102A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 96.83931, -20.04096 which is equivalent
to:
RA (J2000): 06h 27m 21.43s
Dec (J2000): -20d 02' 27.5"
with an uncertainty of 2.2 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35471.
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TITLE: GCN CIRCULAR
NUMBER: 35470
SUBJECT: GRB 240101B: Swift-XRT refined Analysis
DATE: 24/01/03 09:51:11 GMT
FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk>
J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore
(U. Leicester), T. Sbarrato (INAF-OAB), P. D'Avanzo (INAF-OAB), M.G.
Bernardini (INAF-OAB), S. Dichiara (PSU), J.A. Kennea (PSU), A.
Tohuvavohu (U. Toronto) and P.A. Evans report on behalf of the
Swift-XRT team:
We have analysed 6.9 ks of XRT data for GRB 240101B, from 138 s to
126.6 ks after the BAT trigger. The data comprise 189 s in Windowed
Timing (WT) mode (the first 12 s were taken while Swift was slewing)
with the remainder in Photon Counting (PC) mode.
The late-time light curve (from T0+5.0 ks) can be modelled with a
power-law decay with a decay index of alpha=0.80 (+0.33, -0.29).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.28 (+0.14, -0.13). The
best-fitting absorption column is 6.5 (+/-0.8) x 10^21 cm^-2, in
excess of the Galactic value of 2.9 x 10^21 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.39 (+0.29, -0.27)
and a best-fitting absorption column of 7.9 (+2.0, -1.8) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 3.8 x 10^-11 (9.4 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 7.9 (+2.0, -1.8) x 10^21 cm^-2
Galactic foreground: 2.9 x 10^21 cm^-2
Excess significance: 4.7 sigma
Photon index: 2.39 (+0.29, -0.27)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01205744.
This circular is an official product of the Swift-XRT team.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35470.
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TITLE: GCN CIRCULAR
NUMBER: 35469
SUBJECT: GRB 240102A: Swift-XRT refined Analysis
DATE: 24/01/03 07:00:54 GMT
FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk>
J. D. Gropp (PSU), J.P. Osborne (U. Leicester), K.L. Page (U.
Leicester), A. Melandri (INAF-OAR), T. Sbarrato (INAF-OAB), P. D'Avanzo
(INAF-OAB), S. Dichiara (PSU), J.A. Kennea (PSU) and P.A. Evans report
on behalf of the Swift-XRT team:
We have analysed 6.6 ks of XRT data for GRB 240102A, from 113 s to 28.3
ks after the BAT trigger. The data comprise 91 s in Windowed Timing
(WT) mode (the first 10 s were taken while Swift was slewing) with the
remainder in Photon Counting (PC) mode. The best available XRT position
(using the promptly downlinked event data, the XRT-UVOT alignment and
matching UVOT field sources to the USNO-B1 catalogue) is RA, Dec =
96.83800, -20.04076 which is equivalent to:
RA (J2000): 06 27 21.12
Dec(J2000): -20 02 26.7
with an uncertainty of 1.9 arcsec (radius, 90% confidence).
The late-time light curve (from T0+4.7 ks) can be modelled with a
power-law decay with a decay index of alpha=0.5 (+/-0.3).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.74 (+0.11, -0.10). The
best-fitting absorption column is 3.3 (+0.6, -0.5) x 10^21 cm^-2, in
excess of the Galactic value of 2.3 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 4.3 x 10^-11 (5.7 x 10^-11) erg
cm^-2 count^-1.
A summary of the WT-mode spectrum is thus:
Total column: 3.3 (+0.6, -0.5) x 10^21 cm^-2
Galactic foreground: 2.3 x 10^21 cm^-2
Excess significance: 3.1 sigma
Photon index: 1.74 (+0.11, -0.10)
If the light curve continues to decay with a power-law decay index of
0.5, the count rate at T+24 hours will be 9.8 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.2 x
10^-13 (5.6 x 10^-13) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01205899.
This circular is an official product of the Swift-XRT team.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35469.
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TITLE: GCN CIRCULAR
NUMBER: 35468
SUBJECT: GRB 240102B (Fermi GBM trigger 725926335/240102925) is not a GRB
DATE: 24/01/03 01:42:19 GMT
FROM: Cori Fletcher at USRA <cfletcher(a)usra.edu>
C. Fletcher (USRA) reports on behalf of the Fermi Gamma-ray Burst Monitor Team:
"The Fermi Gamma-ray Burst Monitor (GBM) trigger 725926335/240102925 at 22:12:10.09 UT
on 02 January 2024, tentatively classified as a GRB 240102B (GCN 35464), is in fact not due
to a GRB. This trigger is likely due to particle activity."
View this GCN Circular online at https://gcn.nasa.gov/circulars/35468.
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TITLE: GCN CIRCULAR
NUMBER: 35467
SUBJECT: GRB 240102A: LCOGT Optical Upper Limits
DATE: 24/01/03 01:01:40 GMT
FROM: Robert Strausbaugh at Eastern Illinois University <rstrausbaugh(a)eiu.edu>
R. Strausbaugh (Eastern Illinois University), A. Cucchiara (NASA) report on
behalf of a larger collaboration:
We observed the Swift GRB 240102A (Gropp et al., GCN 35461) field with the LCOGT 1-meter Sinistro instrument at the Teide Observatory, Tenerife site, on January 2, from 23:34 to January 3 00:07 UT (corresponding to 6.00 to 6.55 hours after the GRB trigger time) with the sdss r and i filters.
We performed a series of 3x300s exposures in each band. We do not detect an uncatalogued source within the XRT error region in either band. This result is consistent with other optical upper limits (Hu et al., GCN 35465).
The following 5-sigma upper limits are calculated using the PanSTARRS catalog as reference:
r > 22.9
i > 22.3
These magnitudes are not corrected for galactic extinction.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35467.
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TITLE: GCN CIRCULAR
NUMBER: 35466
SUBJECT: Fermi trigger No 725857207: Global MASTER-Net observations report
DATE: 24/01/03 00:31:01 GMT
FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru>
V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,
G.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij
(Lomonosov Moscow State University, SAI, Physics Department),
R. Podesta, C.Lopez, F. Podesta, C.Francile
(Observatorio Astronomico Felix Aguilar OAFA),
R. Rebolo, M. Serra
(The Instituto de Astrofisica de Canarias),
D. Buckley
(South African Astronomical Observatory),
O.A. Gress, N.M. Budnev, O.Ershova
(Irkutsk State University, API),
L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,
A.R.Corella, L.H.Rodriguez
(INAOE, Guillermo Haro Astrophysics Observatory),
A. Tlatov, D. Dormidontov
(Kislovodsk Solar Station of the Pulkovo Observatory),
V. Yurkov, A. Gabovich
(Blagoveschensk Educational State University)
MASTER-Tunka robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB240102.13 (trigger No 725857207,12h 04m 45.60s , -16d 33m 36.0s, R=1.99) errorbox 29555 sec after notice time and 72382 sec after trigger time at 2024-01-02 23:06:24 UT, with upper limit up to 14.2 mag. The observations began at zenith distance = 71 deg. The sun altitude is -18.3 deg.
The galactic latitude b = 45 deg., longitude l = 288 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=2348394
We obtain a following upper limits.
Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________
72390 | 2024-01-02 23:06:24 | MASTER-Tunka | (12h 08m 29.91s , -19d 22m 13.7s) | C | 15 | 14.1 |
72417 | 2024-01-02 23:06:51 | MASTER-Tunka | (12h 07m 49.80s , -17d 29m 14.6s) | C | 15 | 14.2 |
72445 | 2024-01-02 23:07:21 | MASTER-Tunka | (12h 16m 18.51s , -17d 29m 19.9s) | C | 10 | 14.1 |
72483 | 2024-01-02 23:08:02 | MASTER-Tunka | (11h 53m 08.38s , -15d 34m 47.7s) | C | 5 | 13.7 |
72503 | 2024-01-02 23:08:22 | MASTER-Tunka | (12h 00m 39.66s , -15d 33m 13.3s) | C | 5 | 13.7 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35466.
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