TITLE: GCN CIRCULAR
NUMBER: 35465
SUBJECT: GRB240102A: BOOTES-6/DPRT optical upper limit
DATE: 24/01/02 23:18:38 GMT
FROM: Youdong HU at IAA-CSIC <huyoudong072(a)hotmail.com>
Y.-D. Hu, E. Fernandez-Garcia, I. Perez-Garcia, M.D. Caballero-Garcia, R. Sanchez-Ramirez, S. Guziy, S.-Y. Wu and A. J. Castro-Tirado (IAA-CSIC, Granada), P. J. Meintjes and H. J. van Heerden (UFS, South Africa), A. Martin-Carrillo and L. Hanlon (UCD, Ireland) and C. J. Perez del Pulgar (UMA, Malaga), on behalf of a larger collaboration, report:
Following the detection of GRB 240102A by Swift (Gropp et al. GCNC 35461), the BOOTES-6/DPRT 0.6m robotic telescope at Boyden Observatory in Maselspoort (South Africa) observed the GRB location starting on Jan. 2, 18:41 UT (~ 1.1 hours after trigger) in different optical bands. No new optical source is detected on the co-added images (2 x 60 s, clear-filter) within the Swift/XRT error box down to 20.2 mag. Further imaging is ongoing.
We thank the staff at Boyden Observatory for their excellent support.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35465.
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TITLE: GCN CIRCULAR
NUMBER: 35463
SUBJECT: GRB 240101B: MarSEC Observatory, Vicenza, Italy, UPPER LIMIT
DATE: 24/01/02 20:34:34 GMT
FROM: I. Peretto at MarSEC (Marana Space Explorer Center) <ricerca(a)marsec.org>
Ivo Peretto (MarSEC, Marana Space Explorer Center, Marana Di Crespadoro, VI, Italy)
Member of:
UAI/SSV - Unione Astrofili Italiani/Sezione Stelle Variabili, GRB section.
AAVSO (American Association Variable Stars Observers)
In collaboration with: Stefano Lora (MarSEC, Marana Space Explorer Center, Marana di Crespadoro, VI, Italy)
report:
We imaged the field of GRB 240101B detected by SWIFT(trigger=1205744)
with the telescope 14” RC Officine Stellari of MarSEC (Marana Space Explorer Center).
The observations with a series of 120 sec exposures started at 2024-01-01 21:42:43 UT, 77 min. after the GRB trigger, with a Ritchey-Chretien telescope D=360 mm f/ 8.
at the following position:
RA(J2000) = 23h 28m 12s
Dec(J2000) = +51d 38' 43"
Weather conditions were medium with Moon illuminated 70% at 2° from the horizon.
We co-added 30 exposures of 120 sec each.
Start T0+ End T0+ V lim.
77 min 137 min 20.12
We did not found any optical counterpart in A.R. 23 28 12, DEC. +51 38 43 position and in the error box of the XRT candidate.
ref.: S. B. Cenko (GSFC) et al., GCN Circular 35449
Magnitudes were estimated with the Gaia DR3 and
are not corrected for galactic dust extinction.
Reference:
https://www.marsec.org/
The message may be cited.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35463.
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TITLE: GCN CIRCULAR
NUMBER: 35462
SUBJECT: IceCube-Cascade 231230A: Upper limits from a search for additional neutrino events in IceCube
DATE: 24/01/02 20:32:16 GMT
FROM: Jessie Thwaites at IceCube/U Wisc-Madison <thwaites(a)wisc.edu>
The IceCube Collaboration (http://icecube.wisc.edu/) reports:
IceCube has performed a search [1] for additional track-like muon neutrino events arriving from the direction of IceCube-Cascade 231230A (https://gcn.gsfc.nasa.gov/notices_amon_icecube_cascade/138802_36470430.amon) in a time range of 1000 seconds centered on the alert event time (2023-12-30 09:33:26.570 UTC to 2023-12-30 09:50:06.570 UTC) during which IceCube was collecting good quality data. Excluding the event that prompted the alert, zero track-like events are found within the 90% containment region of IceCube-Cascade 231230A. The IceCube sensitivity to neutrino point sources with an E^-2.5 spectrum (E^2 dN/dE at 1 TeV) within the locations spanned by the 90% spatial containment region of IceCube-Cascade 231230A ranges from 1.3e-01 to 3.3e-01 GeV cm^-2 in a 1000 second time window. 90% of events IceCube would detect from a source at this declination with an E^-2.5 spectrum have energies in the approximate energy range between 2e+02 GeV and 2e+05 GeV.
A subsequent search was performed including 2 days of data centered on the alert event time (2023-12-29 09:41:46.570 UTC to 2023-12-31 09:41:46.570 UTC). In this case, we report a p-value of 0.10, consistent with no significant excess of track events. The IceCube sensitivity to neutrino point sources with an E^-2.5 spectrum (E^2 dN/dE at 1 TeV) within the locations spanned by the 90% spatial containment region of IceCube-Cascade 231230A ranges from 1.5e-01 to 3.4e-01 GeV cm^-2 in a 2 day time window.
The IceCube Neutrino Observatory is a cubic-kilometer neutrino detector operating at the geographic South Pole, Antarctica. The IceCube realtime alert point of contact can be reached at roc(a)icecube.wisc.edu.
[1] IceCube Collaboration, R. Abbasi et al., ApJ 910 4 (2021)
View this GCN Circular online at https://gcn.nasa.gov/circulars/35462.
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TITLE: GCN CIRCULAR
NUMBER: 35461
SUBJECT: GRB 240102A: Swift detection of a burst
DATE: 24/01/02 18:19:27 GMT
FROM: K.L. Page at U Leicester <klp5(a)leicester.ac.uk>
J.D. Gropp (PSU), S. Dichiara (PSU), J. A. Kennea (PSU),
K. L. Page (U Leicester) and M. A. Williams (PSU) report on behalf of
the Neil Gehrels Swift Observatory Team:
At 17:34:55 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 240102A (trigger=1205899). Swift slewed immediately to the
burst. The BAT on-board calculated location is
RA, Dec 96.846, -20.024 which is
RA(J2000) = 06h 27m 23.0s
Dec(J2000) = -20d 01' 26.4"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). We currently have no information regarding the
BAT light-curve.
The XRT began observing the field at 17:37:00.6 UT, 125 seconds
after the BAT trigger. Using promptly downlinked data we find an
uncatalogued X-ray source with an enhanced position: RA, Dec 96.83800,
-20.04076 which is equivalent to:
RA(J2000) = 06h 27m 21.12s
Dec(J2000) = -20d 02' 26.7"
with an uncertainty of 1.9 arcseconds (radius, 90% containment). This
position is 66 arc-seconds from the BAT localization. This
position may be improved as more data are received; the latest position
is available at https://www.swift.ac.uk/sper.
A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.34
x 10^21 cm^-2 (Willingale et al. 2013).
No afterglow is detected in the initial UVOT data products.
Burst Advocate for this burst is J.D. Gropp (jdg44 AT psu.edu).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)
View this GCN Circular online at https://gcn.nasa.gov/circulars/35461.
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TITLE: GCN CIRCULAR
NUMBER: 35460
SUBJECT: GRB 240101A: Terskol Zeiss-2000 optical observations
DATE: 24/01/02 16:26:17 GMT
FROM: Alexei Pozanenko at IKI, Moscow <apozanen(a)iki.rssi.ru>
A. Volnova (IKI), P. Phorunzij (INASAN), A. Pozanenko (IKI), N. Pankov (IKI, HSE), S. Belkin (IKI, HSE) report on behalf of GRB IKI FuN:
We observed the GRB 240101A (Cenko et al., GCN 35448) with Zeiss-2000 telescope of Terskol observatory starting on 2024-01-01 (UT) 16:10:24. Within enhanced Enhanced Swift-XRT position (Beardmore et al., GCN 35452) we do not detect any optical objects. However we marginally detected the object at coordinates (J2000) 00:41:23.50 +8:30:58.48, which is 3.4 arcsec from XRT position (Beardmore et al., GCN 35452). Preliminary photometry of the marginally detected object is following.
Date UT start t-T0 Filter Exp. OT Err. UL.
(mid, days) (s) S/N
2024-01-01 16:10:24 0.1823 R 19*60 23.7 2.0 23.0
The photometry is based on the nearby PS1 stars photometry (Lupton transformations)
RA Dec c R(Lupton)
00:41:22.24 +08:31:56.6 16.277 +/- 0.012
00:41:17.90 +08:31:41.5 18.013 +/- 0.014
View this GCN Circular online at https://gcn.nasa.gov/circulars/35460.
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TITLE: GCN CIRCULAR
NUMBER: 35459
SUBJECT: GRB 240101C: GRBAlpha detection
DATE: 24/01/02 15:28:27 GMT
FROM: Marianna Dafčíková at Masaryk University <500025(a)mail.muni.cz>
M. Dafcikova, J. Ripa (Masaryk U.), A. Pal (Konkoly Observatory), N. Werner (Masaryk U.), M. Ohno, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak (Konkoly Observatory), N. Husarikova, F. Munz , M. Topinka, M. Kolar, L. Szakszonova, J.-P. Breuer, F. Hroch (Masaryk U.), T. Urbanec, M. Kasal, A. Povalac (Brno U. of Technology), J. Hudec, J. Kapus, M. Frajt (Spacemanic s.r.o), R. Laszlo, M. Koleda (Needronix s.r.o), M. Smelko, P. Hanak, P. Lipovsky (Technical U. of Kosice), G. Galgoczi (Wigner Research Center/Eotvos U.), Y. Uchida, H. Poon, H. Matake (Hiroshima U.), N. Uchida (ISAS/JAXA), T. Bozoki (Eotvos U.), G. Dalya (Eotvos U.), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), G. Friss (Eotvos U.), Y. Fukazawa, K. Hirose (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), K. Kapas (Eotvos U.), L. L. Kiss (Konkoly Observatory), T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), J. Takatsy (Eotvos U.), K. Torigoe (Hiroshima U.), N. Kogiso, M. Yoneyama (Osaka Metropolitan U.), M. Moritaki (U. Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration.
The short-duration GRB 240101C (Fermi/GBM detection: GCN 35451; INTEGRAL/SPI-ACS peak detection at 2024-01-01 ~12:57:24 UT) was observed by the GRBAlpha 1U CubeSat (Pal et al. 2023, A&A, 677, 40; arXiv:2302.10048).
The detection was confirmed at the peak time 2024-01-01 12:57:24 UTC. The T90 duration measured by GRBAlpha is 1 s and the overall significance during T90 reaches 4.9 sigma in the 120-400 keV band.
The light curve obtained by GRBAlpha is available here: https://grbalpha.konkoly.hu/static/share/GRB240101C_GCN.pdf
All GRBAlpha detections are listed at: https://monoceros.physics.muni.cz/hea/GRBAlpha/
GRBAlpha, launched on 2021 March 22, is a demonstration mission for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). The detector of GRBAlpha consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy range from ~50 keV to ~1000 keV. To increase the duty cycle and the downlink rate, the upgrade of the on-board data acquisition software stack is in progress. The ground segment is also supported by the radio amateur community and it takes advantage of the SatNOGS network for increased data downlink volume.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35459.
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TITLE: GCN CIRCULAR
NUMBER: 35458
SUBJECT: GRB 240101B: Swift/UVOT Upper Limits
DATE: 24/01/02 12:11:38 GMT
FROM: Paul Kuin at MSSL <npkuin(a)gmail.com>
N. P. M. Kuin (UCL-MSSL) and S. B. Cenko (GSFC)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 240101B
110 s after the BAT trigger (Cenko et al., GCN Circ. 35449).
No optical afterglow consistent with the XRT position
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 134 284 147 >21.1
u_FC 294 543 246 >20.1
white 134 1718 411 >21.8
v 110 1595 130 >19.2
b 549 1693 117 >20.5
u 294 1669 343 >20.2
w1 675 1644 117 >19.3
m2 648 1619 97 >21.0
w2 599 1741 134 >19.3
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.287 in the direction of the burst
(Schlegel et al. 1998).
View this GCN Circular online at https://gcn.nasa.gov/circulars/35458.
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TITLE: GCN CIRCULAR
NUMBER: 35457
SUBJECT: GRB 240101A: Swift/UVOT Upper Limits
DATE: 24/01/02 12:10:21 GMT
FROM: Paul Kuin at MSSL <npkuin(a)gmail.com>
N. P. M. Kuin (UCL-MSSL) and S. B. Cenko (GSFC)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 240101A
168 s after the BAT trigger (Cenko et al., GCN Circ. 35448).
No optical afterglow consistent with the BAT position
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 168 318 147 >20.4
white 168 1053 334 >20.8
v 656 4661 236 >18.7
b 582 773 39 >18.9
u 729 749 19 >18.3
w1 705 5071 236 >19.5
w2 804 824 19 >18.7
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.059 in the direction of the burst
(Schlegel et al. 1998).
View this GCN Circular online at https://gcn.nasa.gov/circulars/35457.
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TITLE: GCN CIRCULAR
NUMBER: 35456
SUBJECT: GRB 240101A: Swift-XRT refined Analysis
DATE: 24/01/02 11:11:51 GMT
FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk>
D.N. Burrows (PSU), J. D. Gropp (PSU), A.P. Beardmore (U. Leicester),
J.P. Osborne (U. Leicester), A. D'Ai (INAF-IASFPA), A. Melandri
(INAF-OAR), T. Sbarrato (INAF-OAB), S. Dichiara (PSU) and P.A. Evans
report on behalf of the Swift-XRT team:
We have analysed 6.8 ks of XRT data for GRB 240101A, from 142 s to 57.6
ks after the BAT trigger. The data are entirely in Photon Counting
(PC) mode.
The light curve can be modelled with a power-law decay with a decay
index of alpha=1.06 (+0.08, -0.07).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.1 (+/-0.3). The
best-fitting absorption column is 4.3 (+1.8, -1.5) x 10^21 cm^-2, in
excess of the Galactic value of 5.8 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 3.9 x 10^-11 (6.5 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 4.3 (+1.8, -1.5) x 10^21 cm^-2
Galactic foreground: 5.8 x 10^20 cm^-2
Excess significance: 4.1 sigma
Photon index: 2.1 (+/-0.3)
If the light curve continues to decay with a power-law decay index of
1.06, the count rate at T+24 hours will be 1.4 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.6 x
10^-14 (9.3 x 10^-14) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01205708.
This circular is an official product of the Swift-XRT team.
View this GCN Circular online at https://gcn.nasa.gov/circulars/35456.
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