GRB240123A

This page lists all entries on GRB240123A in GRBweb

Summary IPN Swift GCN 35602 GCN 35605 GCN 35609 GCN 35610 GCN 35612 GCN 35616 GCN 35618 GCN 35620 GCN 35622 GCN 35624 GCN 35628 GCN 35631

Summary table
Variable Value Source
T0 11:05:46 UTC GCN_circulars,Swift Det
ra 199.3469° Swift
decl 60.6179° Swift
pos_error 2.59e-05° Swift
GBM_located False
mjd 60332.46233796296 GCN_circulars,Swift Det
IPN table
GRB_name GRB240123A
ra 199.3167°
decl 60.6333°
pos_error 5.00e-02°
Swift table
GRB_name GRB240123A
t_trigger 11:05:46 UTC
ra 199.3469°
decl 60.6179°
pos_error 2.59e-05°
GCN 35602 table
GRB_name GRB240123A
GCN_number 35602
Detection_method Swift Det
t_trigger 11:05:46 UTC
ra 199.3190°
decl 60.6320°
Circular_text TITLE: GCN CIRCULAR NUMBER: 35602 SUBJECT: GRB 240123A: Swift detection of a burst with a possible optical counterpart DATE: 24/01/23 11:34:56 GMT FROM: Antonino D'Ai' at IASF-PA A. D'Ai (INAF-IASFPA), E. Ambrosi (INAF-IASFPA), V. D'Elia (SSDC & INAF-OAR), J.D. Gropp (PSU), J. A. Kennea (PSU), A. Y. Lien (U Tampa), A. Melandri (INAF-OAR), K. L. Page (U Leicester), T. M. Parsotan (GSFC/UMBC/CRESSTII) and B. Sbarufatti (INAF-OAB) report on behalf of the Neil Gehrels Swift Observatory Team: At 11:05:46 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 240123A (trigger=1210276). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 199.319, +60.632 which is RA(J2000) = 13h 17m 16s Dec(J2000) = +60d 37' 53" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a complex structure with a duration of about 25 sec. The peak count rate was ~500 counts/sec (15-350 keV), at ~5 sec after the trigger. The XRT began observing the field at 11:08:08.6 UT, 141.8 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source located at RA, Dec 199.34797, 60.61894 which is equivalent to: RA(J2000) = 13h 17m 23.51s Dec(J2000) = +60d 37' 08.2" with an uncertainty of 3.8 arcseconds (radius, 90% containment). This location is 69 arcseconds from the BAT onboard position, within the BAT error circle. 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 in excess of the Galactic value (1.45 x 10^20 cm^-2, Willingale et al. 2013), with an excess column of 2.7 (+2.69/-2.33) x 10^21 cm^-2 (90% confidence). The initial flux in the 2.5 s image was 7.30e-10 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 151 seconds after the BAT trigger. There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at RA(J2000) = 13:17:23.25 = 199.3468 DEC(J2000) = +60:37:04.4 = 60.6179 with a 90%-confidence error radius of about 0.2 arc sec. This position is 4.3 arc sec. from the center of the XRT error circle. The estimated magnitude is 19.9 with a 1-sigma error of about 0.2. No correction has been made for the expected extinction. Burst Advocate for this burst is A. D'Ai (antonino.dai AT inaf.it). 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/)
GCN 35605 table
GRB_name GRB240123A
GCN_number 35605
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 35605 SUBJECT: GRB 240123A: Mondy optical afterglow observations DATE: 24/01/23 15:52:15 GMT FROM: Alexei Pozanenko at IKI, Moscow N. Pankov (HSE, IKI), A. Pozanenko (IKI), E. Klunko (ISTP), S. Belkin (IKI) report on behalf of GRB IKI FuN: We observed the field of GRB 231117A (D'Ai et al., GCN 35602) with AZT-33IK telescope of Mondy observatory in R-filter starting on 2024-01-23 (UT) 14:00:48. We clearly detect a new fading object at coordinates (J2000) 13 17 23.87 +60 37 05.3 with uncertainties of 0.2 arcsec which is slightly differ from coordinates reported by UVOT (D'Ai et al., GCN 35602). The object is absent in SDSS catalogue. Preliminary photometry is following Date UT start t-T0 Exp. Filter OT Err. (mid, days) (s) 2024-01-23 14:00:48 0.126415 7x120 R 19.07 0.10 20.9 2024-01-23 14:20:48 0.144479 13x120 R 19.25 0.10 21.3 2024-01-23 14:46:49 0.163934 15x120 R 19.37 0.11 21.3 The photometry is based on nearby USNO-B1.0 R2 stars.
GCN 35609 table
GRB_name GRB240123A
GCN_number 35609
Detection_method correction
Circular_text TITLE: GCN CIRCULAR NUMBER: 35609 SUBJECT: GRB 240123A: Mondy continued optical observations + correction of the GRB name in GCN 35605 DATE: 24/01/23 18:06:11 GMT FROM: Alexei Pozanenko at IKI, Moscow N. Pankov (HSE, IKI), A. Pozanenko (IKI), E. Klunko (ISTP), S. Belkin (IKI) report on behalf of GRB IKI FuN: We continued to observe the afterglow of GRB 240123A (D'Ai et al., GCN 35602) with AZT-33IK telescope of Mondy observatory in R-filter originally started on 2024-01-23 (UT) 14:00:48 (Pankov et al., GCN 35605). We confirm the afterglow decay, which detected previously (D'Ai et al., GCN 35602; Pankov et al., GCN 35605). Preliminary photometry of the afterglow is following Date UT start t-T0 Exp. Filter OT Err. UL(3sigma) (mid, days) (s) 2024-01-23 16:03:39 0.227009 29x120 R 19.87 0.10 21.9 The photometry is based on nearby USNO-B1.0 R2 stars. We are also reporting the incorrect name of the GRB in GCN Circular No. 35605. The correct name of the GRB in GCN Circular #3560 should be GRB 240123A.
GCN 35610 table
GRB_name GRB240123A
GCN_number 35610
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 35610 SUBJECT: Fermi GBM Sub-Threshold Detection of GRB 240123A DATE: 24/01/23 19:36:21 GMT FROM: Lorenzo Scotton at UAH L. Scotton (UAH) reports on behalf of the Fermi-GBM Team: Swift-BAT detected GRB 240123A at 11:05:46 UT (D'Ai et al. 2024, GCN 35602). There was no Fermi-GBM onboard trigger around the event. An automated, blind search for short gamma-ray bursts below the onboard triggering threshold in Fermi-GBM identified no counterparts. The GBM targeted search [1], the most sensitive, coherent search for GRB-like signals identified a transient most significantly on the 8.192 s timescale, with a false alarm rate of 3.9e-05 Hz and a location consistent with the Swift-BAT event, using the standard search protocol with a S/N of 13. The GBM targeted search event was found with the highest significance with a "normal" spectrum (Band function with Epeak = 230 keV, alpha = -1.0, beta = -2.3) for a GRB. [1] Goldstein et al. 2019 arXiv:1903.12597
GCN 35612 table
GRB_name GRB240123A
GCN_number 35612
Detection_method Swift-XRT Other
ra 199.3473°
decl 60.6184°
Circular_text TITLE: GCN CIRCULAR NUMBER: 35612 SUBJECT: GRB 240123A: Swift-XRT refined Analysis DATE: 24/01/23 22:11:25 GMT FROM: Phil Evans at U of Leicester M. Capalbi (INAF-IASFPA), M. Perri (SSDC & INAF-OAR), J. D. Gropp (PSU), S. Dichiara (PSU), J.A. Kennea (PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), V. D'Elia (SSDC & INAF-OAR) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 6.5 ks of XRT data for GRB 240123A, from 131 s to 23.7 ks after the BAT trigger. The data comprise 164 s in Windowed Timing (WT) mode (the first 8 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The refined XRT position is RA, Dec = 199.3473, +60.6184 which is equivalent to: RA (J2000): 13 17 23.34 Dec(J2000): +60 37 06.1 with an uncertainty of 3.5 arcsec (radius, 90% confidence). The light curve can be modelled with a series of power-law decays. The initial decay index is alpha=7.2 (+0.8, -2.8). At T+145 s the decay flattens to an alpha of 0.3 (+1.0, -1.8). The light curve breaks again at T+183 s to a decay with alpha=2.91 (+0.20, -0.19), before a final break at T+635 s s after which the decay index is 0.58 (+/-0.08). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 2.35 (+0.09, -0.07). The best-fitting absorption column is consistent with the Galactic value of 1.4 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 2.01 (+0.17, -0.13) and a best-fitting absorption column of 2.3 (+3.3, -0.9) x 10^20 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.2 x 10^-11 (3.4 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 2.3 (+3.3, -0.9) x 10^20 cm^-2 Galactic foreground: 1.4 x 10^20 cm^-2 Excess significance: <1.6 sigma Photon index: 2.01 (+0.17, -0.13) If the light curve continues to decay with a power-law decay index of 0.58, the count rate at T+24 hours will be 0.028 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.0 x 10^-13 (9.6 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/01210276. This circular is an official product of the Swift-XRT team.
GCN 35616 table
GRB_name GRB240123A
GCN_number 35616
Detection_method Swift-XRT Det
ra 199.3486°
decl 60.6185°
Circular_text TITLE: GCN CIRCULAR NUMBER: 35616 SUBJECT: GRB 240123A: Enhanced Swift-XRT position DATE: 24/01/24 03:40:02 GMT FROM: Phil Evans at U of Leicester J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) report on behalf of the Swift-XRT team. Using 596 s of XRT Photon Counting mode data and 1 UVOT images for GRB 240123A, 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 = 199.34861, +60.61849 which is equivalent to: RA (J2000): 13h 17m 23.67s Dec (J2000): +60d 37' 06.6" with an uncertainty of 2.1 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.
GCN 35618 table
GRB_name GRB240123A
GCN_number 35618
Detection_method MITSuME
ra 199.3495°
decl 60.6181°
Circular_text TITLE: GCN CIRCULAR NUMBER: 35618 SUBJECT: GRB 240123A : MITSuME Akeno optical afterglow candidate detection DATE: 24/01/24 08:57:45 GMT FROM: Mahito Sasada at Tokyo Institute of Technology M. Sasada, I. Takahashi, N. Higuchi, M. Niwano, S. Sato, S. Hayatsu, H. Takei, H. Seki, Y. Yatsu and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration: We observed the field of GRB 240123A (D'Ai et al. GCN 35602) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope Akeno. The observation with a series of 60 sec exposures started at 2024-01-23 15:09:01 UT (4.05 hours after the Swift/BAT trigger). We stacked the images in good conditions. An optical candidate of the afterglow can be found at the location of (RA, Dec) = (199.3495, 60.6181) near the Swift/XRT error position (Capalbi et al. GCN 35612). Here we report magnitudes by the aperture photometry at the position. T0+[hours] | MID-UT | T-EXP[sec] | magnitudes of aperture photometry ---------------------------------------------------------------------------------------------------------------- 5.0 | 2024-01-23 16:05:41 | 5880 | g’=19.83+/-0.17, Rc=19.35+/-0.11, Ic=19.24+/-0.13 ---------------------------------------------------------------------------------------------------------------- T0+ : Elapsed time after the trigger T-EXP: Total Exposure time The position of the optical candidate is consistent with Pankov et al., GCN 35605. We used the PS1 catalog for flux calibration. The catalog magnitudes in PS1 g, r and i bands were converted to our g'-, Rc- and Ic-band magnitudes following Tonry et al. (2012), Table 6. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al. 2021, PASJ, Vol.73, Issue 1, Pages 4-24; https://github.com/MNiwano/Eclaire).
GCN 35620 table
GRB_name GRB240123A
GCN_number 35620
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 35620 SUBJECT: GRB 240123A: Mondy continued optical observations and the PL decay index DATE: 24/01/24 15:44:05 GMT FROM: Alexei Pozanenko at IKI, Moscow N. Pankov (HSE, IKI), A. Pozanenko (IKI), E. Klunko (ISTP), S. Belkin (IKI) report on behalf of GRB IKI FuN: We continued to observe the afterglow of GRB 240123A (D'Ai et al., GCN 35602; Pankov et al., GCN 35605, GCN 35609; Sasada et al., GCN 35618; Moskvitin at al., GCN 35619) with AZT-33IK telescope of Mondy observatory in R-filter. Using previously reported photometry (Pankov et al., GCN 35605, GCN 35609; Moskvitin at al., GCN 35619) and photometry obtained on t-T0 0.400722 we approximate the light curve with a PL model with the index of PL alpha = -1.1, see Figure at http://grb.rssi.ru/GRB240123A/GRB240123A_LC_approximation.jpg
GCN 35622 table
GRB_name GRB240123A
GCN_number 35622
Detection_method Swift-BAT Det
ra 199.2870°
decl 60.6070°
Circular_text TITLE: GCN CIRCULAR NUMBER: 35622 SUBJECT: GRB 240123A: Swift-BAT refined analysis DATE: 24/01/24 18:12:15 GMT FROM: Amy T. Parsotan (GSFC), S. D. Barthelmy (GSFC), A. D'Ai (INAF-IASFPA), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa), C. B. Markwardt (GSFC), M. J. Moss (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU) (i.e. the Swift-BAT team): Using the data set from T-240 to T+820 sec from the recent telemetry downlink, we report further analysis of BAT GRB 240123A (trigger #1210276) (D'Ai, et al., GCN Circ. 35602). The BAT ground-calculated position is RA, Dec = 199.287, 60.607 deg which is RA(J2000) = 13h 17m 08.9s Dec(J2000) = +60d 36' 25.6" with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment). The partial coding was 31%. The mask-weighted light curve shows some weak emission with complex structures that starts at ~T0 and ends at ~T+140 s. The main peak occurs at ~T+5 s. T90 (15-350 keV) is 115.30 +- 54.93 sec (estimated error including systematics). The time-averaged spectrum from T-0.69 to T+140.46 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.69 +- 0.23. The fluence in the 15-150 keV band is 1.6 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+5.49 sec in the 15-150 keV band is 1.1 +- 0.3 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/1210276/BA/
GCN 35624 table
GRB_name GRB240123A
GCN_number 35624
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 35624 SUBJECT: GRB 240123A: further SAO RAS optical observations DATE: 24/01/25 05:12:41 GMT FROM: Moskvitin Alexander at SAO RAS A. S. Moskvitin, O. A. Maslennikova, O. I. Spiridonova (SAO RAS) report on behalf of the GRB follow-up team. We observed the field of GRB 240123A (D'Ai et al., GCN #35602; Scotton, GCN #35610) with the 1-m telescope of SAO RAS equipped with the CCD photometer. We obtained 16 x 300 sec. images in Rc band on Jan 25, 01:55:52 -- 03:30:49 UT (t_mid - T0 = 1.6511 days). The OT (D'Ai et al., GCN #35602; Pankov et al., GCNs #35605, #35609 #35620; Sasada et al., GCN #35618) is detected in our stacked frame with the brightness of R = 22.0 +/- 0.2. The photometry is based on R2 magnitudes of nearby USNO-B1.0 stars.
GCN 35628 table
GRB_name GRB240123A
GCN_number 35628
Detection_method Fermi GBM Det
t_trigger 11:05:49 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 35628 SUBJECT: GRB 240123A: GRBAlpha detection DATE: 24/01/25 14:21:21 GMT FROM: Marianna Dafčíková at Masaryk University <500025@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 long-duration GRB 240123A (Swift/BAT detection: GCN 35602; Fermi/GBM detection: GCN 35610; INTEGRAL/SPI-ACS peak detection at 2024-01-23 ~11:05:47) was observed by the GRBAlpha 1U CubeSat (Pal et al. 2023, A&A, 677, 40; arXiv:2302.10048). The subthreshold detection was confirmed at the peak time 2024-01-23 11:05:49 UTC. The T90 duration measured by GRBAlpha is 8 s and the overall significance during T90 reaches 3.5 sigma. The light curve obtained by GRBAlpha is available here: https://grbalpha.konkoly.hu/static/share/GRB240123A_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.
GCN 35631 table
GRB_name GRB240123A
GCN_number 35631
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 35631 SUBJECT: GRB 240123A: Glowbug gamma-ray detection DATE: 24/01/25 18:11:33 GMT FROM: C.C. Cheung at Naval Research Lab C.C. Cheung, M. Kerr, J.E. Grove, R. Woolf (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge, D. Kocevski (MSFC), and M.S. Briggs (UAH) report: The Glowbug gamma-ray telescope [1,2], operating on the International Space Station, reports the detection of GRB 240123A, which was also detected by Swift/BAT (GCN 35602, 35622), Fermi/GBM (GCN 35610), and GRBAlpha (GCN 35628). Using an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2024-01-23 11:05:48.840 with a duration of 6.1 s and a total significance of about 12.2 sigma. The light curve comprises a single peak. Using a standard power-law function with an exponential high-energy cutoff [3] to model the emission over this duration results in a photon index dN/dE~E^x of x=-0.4 and a cutoff energy ("Epeak") of 719 keV. The modeled 10-10000 keV fluence is 1.3e-06 erg/cm^2. The analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS. Glowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient telescopes developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Program’s STP-H9 to the ISS. The detector comprises 12 large-area (15 cm x 15 cm) CsI:Tl panels covering the surface of a half cube, and two hexagonal (5-cm diameter, 10-cm length) CLLB scintillators, giving it a large field of view (instantaneous FoV ~2/3 sky) over a wide energy band of 50 keV to >2 MeV. [1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959 [2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O [3] Goldstein, A. et al. 2020, ApJ 895, 40, arXiv :1909.03006 Distribution Statement A: Approved for public release. Distribution is unlimited.