GRB250625A

This page lists all entries on GRB250625A in GRBweb

Summary Swift GCN 40824 GCN 40825 GCN 40826 GCN 40827 GCN 40828 GCN 40830 GCN 40831 GCN 40832 GCN 40833 GCN 40834 GCN 40835 GCN 40836

Summary table
Variable Value Source
T0 16:04:56 UTC GCN_circulars,Swift Det
ra 261.5087° Swift
decl 22.2676° Swift
pos_error 2.46e-04° Swift
GBM_located False
mjd 60851.67009259259 GCN_circulars,Swift Det
Swift table
GRB_name GRB250625A
t_trigger 16:04:56 UTC
ra 261.5087°
decl 22.2676°
pos_error 2.46e-04°
GCN 40824 table
GRB_name GRB250625A
GCN_number 40824
Detection_method Fermi GBM final loc
t_trigger 16:04:57 UTC
ra 257.2000°
decl 27.0000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 40824 SUBJECT: GRB 250625A: Fermi GBM Final Real-time Localization DATE: 25/06/25 16:15:37 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 16:04:57 UT on 25 Jun 2025, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 250625A (trigger 772560302.510236 / 250625670). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 257.2, Dec = 27.0 (J2000 degrees, equivalent to J2000 17h 08m, 27d 00'), with a statistical uncertainty of 6.9 degrees. The angle from the Fermi LAT boresight is 28.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2025/bn250625670/quicklook/glg_skymap_all_bn250625670.png The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2025/bn250625670/quicklook/glg_healpix_all_bn250625670.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2025/bn250625670/quicklook/glg_lc_medres34_bn250625670.gif
GCN 40825 table
GRB_name GRB250625A
GCN_number 40825
Detection_method Swift Det
t_trigger 16:04:56 UTC
ra 261.5190°
decl 22.2650°
Circular_text TITLE: GCN CIRCULAR NUMBER: 40825 SUBJECT: GRB 250625A: Swift detection of a burst DATE: 25/06/25 16:20:37 GMT FROM: David Palmer at LANL M. Ferro (INAF-OAB), R. Brivio (INAF-OAB), J. J. DeLaunay (PSU), R. Gupta (NASA GSFC), J. A. Kennea (PSU), D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB) and M. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 16:04:56 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 250625A (trigger=1327910). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 261.519, +22.265 which is RA(J2000) = 17h 26m 04s Dec(J2000) = +22d 15' 55" 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 8 sec. The peak count rate was ~2200 counts/sec (15-350 keV), at ~2 sec after the trigger. The XRT began observing the field at 16:06:56.2 UT, 119.8 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source with an enhanced position: RA, Dec 261.50871, 22.26763 which is equivalent to: RA(J2000) = 17h 26m 02.09s Dec(J2000) = +22d 16' 03.5" with an uncertainty of 1.9 arcseconds (radius, 90% containment). This location is 35 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. We cannot determine whether the source is fading at the present time. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density in excess of the Galactic value (5.47 x 10^20 cm^-2, Willingale et al. 2013), with an excess column of 8 (+10.81/-7.26) x 10^21 cm^-2 (90% confidence). UVOT took a finding chart exposure of 150 seconds with the White filter starting 124 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. The list of sources is typically complete to about 18 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.055. This is co-detection with Fermi/GBM (GCN #40824). Burst Advocate for this burst is M. Ferro (matteo.ferro 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 40826 table
GRB_name GRB250625A
GCN_number 40826
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 40826 SUBJECT: Fermi GRB 250625A: Global MASTER-Net observations report DATE: 25/06/25 21:15:24 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V.Lipunov, E.Gorbovskoy, A.Kuznetsov, K.Zhirkov, I.Panchenko, N.Tiurina, P.Balanutsa, V.Topolev, D.Vlasenko, G.Antipov, A.Sankovich, Yu.Tselik, Ya.Kechin, V.Senik, A.Chasovnikov, K.Labsina, I. Gorbunov (Lomonosov MSU), O.Gress, N.Budnev (ISU), C.Francile, F. Podesta, R.Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), A.Sosnovskij (CrAO), A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity), D.Buckley (SAAO), R.Rebolo (The Instituto de Astrofisica de Canarias), L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez (INAOE, Guillermo Haro Astrophysics Observatory) MASTER-Tavrida robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 250625A ( Fermi GBM team, GCN 40824) errorbox 16256 sec after notice time and 16277 sec after trigger time at 2025-06-25 20:36:14 UT, with upper limit up to 14.7 mag. The observations began at zenith distance = 22 deg. The sun altitude is -20.8 deg. The galactic latitude b = 33 deg., longitude l = 49 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2916483 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 16367 | 2025-06-25 20:36:14 | MASTER-Tavrida | (17h 25m 02.21s , +22d 17m 15.8s) | C | 180 | 14.7 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 40827 table
GRB_name GRB250625A
GCN_number 40827
Detection_method Swift-XRT Det
ra 261.5089°
decl 22.2673°
Circular_text TITLE: GCN CIRCULAR NUMBER: 40827 SUBJECT: GRB 250625A: Enhanced Swift-XRT position DATE: 25/06/25 21:43:16 GMT FROM: Phil Evans at U of Leicester A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) report on behalf of the Swift-XRT team. Using 2454 s of XRT Photon Counting mode data and 3 UVOT images for GRB 250625A, 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 = 261.50887, +22.26729 which is equivalent to: RA (J2000): 17h 26m 2.13s Dec (J2000): +22d 16' 02.3" with an uncertainty of 2.3 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 40828 table
GRB_name GRB250625A
GCN_number 40828
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 40828 SUBJECT: GRB 250625A: SAO RAS possible optical afterglow DATE: 25/06/25 21:47:40 GMT FROM: Alexander Moskvitin at SAO RAS A. Moskvitin, O. Spiridonova (SAO RAS), report on behalf of a GRB follow-up collaboration. We observed the field of the GRB 250625A (The Fermi GBM team, GCN 40824; Ferro et al., GCN 40825) with SAO RAS 1-m telescope Zeiss-1000 equipped with CCD-photometer. We obtained 6 x 300 sec. exposures in Rc band on June 25, 20:39:03--21:12:11 UT (t_mid - T0 = 4.8447 hours). Withtin the enhanced XRT error circle (Beardmore et al., GCN 40827) we detect single object with the coordinates: R.A. (J2000) = 17:26:02.1 Dec. (J2000) = +22:16:03.6 +/- 0".3 and brightness of R = 22.97 +/- 0.17, possible GRB OT. Observations are ongoing to confirm variability of the object. Preliminary photometry is based on the nearby USNO-B1.0 and has not corrected for the Galactic extinction. R.A. Dec. (2000) R2 17:26:06.4 +22:16:29.4 14.75 17:26:03.7 +22:15:09.9 15.42 17:26:10.0 +22:13:56.8 15.03 17:26:01.4 +22:18:39.0 14.59
GCN 40830 table
GRB_name GRB250625A
GCN_number 40830
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 40830 SUBJECT: GRB 250625A: SVOM/VT optical confirmation DATE: 25/06/26 00:20:46 GMT FROM: Liping Xin at NAOC, SVOM L. P. Xin, H. L. Li, Y. L. Qiu, C. Wu, Y.N. Ma, Z. H. Yao, X. H. Han, Y. Xu, J. Wang, P. P. Zhang, W. J. Xie, Y. J. Xiao, H. B. Cai, L. Lan, J. S. Deng, J. Y. Wei (NAOC), J. Palmerio (CEA), A. Li (BNU) report on behalf of the SVOM/VT team SVOM/VT performed a Target of Opportunity observation of GRB 250625A detected by Swift-BAT（Ferro et al., GCN 40825) and Fermi-GBM (GCN #40824). The observation began at 2025-06-25T16:50:36 UTC, 45.7 minutes after the trigger, in the VT_B (400nm-650nm) and VT_R (650nm-1000nm) channels simultaneously. The optical counterpart (Moskvitin et al., GCN 40828) within the errorbox of Swift/XRT (Beardmore et al., GCN 40827) was detected in the 38*70 sec stack image with a magnitude of VT_B=22.5+/-0.15 mag in AB magnitude with a mid time of 69 min after the burst. The counterpart is also detected in VT_R band in the stack image, but it has some contaimination from the blooming light from the nearby bright source. More detailed data analysis is on going. Our photometry was not corrected for Galactic extinction. The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Centre for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. VT was jointly developed by Xi'an Institute of Optics and Precision Mechanics (XIOPM), CAS and National astronomical observatories (NAOC), CAS.
GCN 40831 table
GRB_name GRB250625A
GCN_number 40831
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 40831 SUBJECT: GRB 250625A: NOT z-band upper limit DATE: 25/06/26 00:25:21 GMT FROM: Daniele Bjørn Malesani at Cosmic Dawn Center, Niels Bohr Institute D. B. Malesani (DAWN/NBI and Radboud), A. Martin-Carrillo (UCD), A. de Ugarte Postigo (LAM), G. Corcoran (UCD), B. P. Gompertz (Birmingham), D. Xu (NAOC), M. A. Diaz Teodori (NOT and Turku Univ.), report on behalf of a larger collaboration: We observed the position of the X-ray and optical afterglow (Beardmore et al., GCN 40827; Moskvitin & Spiridonova, GCN 40828) of GRB 250625A (Ferro et al., GCN 40825; Fermi GBM team, GCN 40824) using the Nordic Optical Telescope, using the “standby” StanCam instrument. In a sequence of 3 exposures of 200 s each, with mean time 2025 Jun 25.948 UT (6.67 hr after the trigger), we detect no object consistent with the X-ray afterglow, down to a limiting magnitude z > 21 AB, calibrated against the Pan-STARRS catalog.
GCN 40832 table
GRB_name GRB250625A
GCN_number 40832
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 40832 SUBJECT: Swift GRB 250625A: Global MASTER-Net observations report DATE: 25/06/26 02:24:25 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V.Lipunov, E.Gorbovskoy, A.Kuznetsov, K.Zhirkov, I.Panchenko, N.Tiurina, P.Balanutsa, V.Topolev, D.Vlasenko, G.Antipov, A.Sankovich, Yu.Tselik, Ya.Kechin, V.Senik, A.Chasovnikov, K.Labsina, I. Gorbunov (Lomonosov MSU), O.Gress, N.Budnev (ISU), C.Francile, F. Podesta, R.Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), A.Sosnovskij (CrAO), A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity), D.Buckley (SAAO), R.Rebolo (The Instituto de Astrofisica de Canarias), L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez (INAOE, Guillermo Haro Astrophysics Observatory) MASTER-Tavrida robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, SAI Crimea astronomical station) was pointed to the Swift GRB 250625A ( M. Ferro et al., GCN 40825) errorbox 16240 sec after notice time and 16278 sec after trigger time at 2025-06-25 20:36:14 UT, with upper limit up to 14.7 mag. The observations began at zenith distance = 22 deg. The sun altitude is -20.8 deg. MASTER-OAFA robotic telescope located in Argentina (OAFA observatory of San Juan National University) was pointed to the Swift GRB 250625A errorbox 35307 sec after notice time and 35345 sec after trigger time at 2025-06-26 01:54:01 UT, with upper limit up to 18.9 mag. The observations began at zenith distance = 60 deg. The sun altitude is -53.1 deg. The galactic latitude b = 28 deg., longitude l = 45 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2916460 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 16368 | MASTER-Tavrida | C | 180 | 14.7 | 35435 | MASTER-OAFA | C | 180 | 18.5 | 35630 | MASTER-OAFA | C | 180 | 18.2 | 35825 | MASTER-OAFA | C | 180 | 18.9 | 36026 | MASTER-OAFA | C | 180 | 18.6 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 40833 table
GRB_name GRB250625A
GCN_number 40833
Detection_method Fermi GBM Det
t_trigger 16:04:57.510 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 40833 SUBJECT: GRB250625A: Fermi GBM Observation DATE: 25/06/26 03:47:05 GMT FROM: Matt Godwin Matt Godwin (UAH), O. Mukherjee (USRA) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 16:04:57.51 UT on 25 June 2025, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB250625A (trigger 772560302/250625670). Which was also detected by Swift BAT/XRT (Ferro et al. 2025, GCN 40825) and SVOM/VT (Xin et al. 2025, GCN 40830). The Fermi GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight is 32 degrees. The GBM light curve consists of one strong peak and a few weaker peaks with a duration (T90) of about 5.4 s (50-300 keV). The time-averaged spectrum from T0-2.0 to T0+5.0 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -1.27 +/- 0.05 and the cutoff energy, parameterized as Epeak, is 1301.00 +/- 1190.00 The event fluence (10-1000 keV) in this time interval is (1.8 +/- 0.1)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0-0.13 s in the 10-1000 keV band is 3 +/- 0.2 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog: https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html For Fermi GBM data and info, please visit the official Fermi GBM Support Page: https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"
GCN 40834 table
GRB_name GRB250625A
GCN_number 40834
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 40834 SUBJECT: GRB 250625A: JinShan optical observations DATE: 25/06/26 04:25:58 GMT FROM: Zipei Zhu at NAOC Z.P. Zhu, S.Q. Jiang, X. Liu, J. An, D. Xu (NAOC), S.Y. Fu (HUST), J.Z. Liu (XAO) report on behalf of a large collaboration: We observed the field of GRB 250625A detected by the Fermi/GBM and Swift/BAT (the Fermi GBM Team, GCN 40824; Ferro et al., GCN 40825), using the 100cm-C telescope (100C) of the JinShan project, located at Altay, Xinjiang, China. Observations started at 16:11:04 UT on 2025-06-25, i.e., 6.1 min after the BAT trigger, and a series of frames were obtained in the Sloan r-, i-, z-bands. In the first round of r-band exposures, an uncatalogued optical source is marginally detected within the Swift/XRT enhanced error circle (Beardmore et al., GCN 40827), which is consistent with the reported optical counterpart by SAO RAS (Moskvitin et al., GCN 40828) and SVOM/VT (Xin et al., GCN 40830). The source is not detected in i-band and z-band (see also Malesani et al., GCN 40831), as well as in the second r-band exposures. Our preliminary results are summarized as follows: T-mid (hr) | Filter | Mag 0.387 | r | 22.5 +/- 0.3 1.237 | i | > 21.7 (5$\sigma$) 1.935 | z | > 20.5 (5$\sigma$) 2.761 | r | > 21.1 (5$\sigma$) calibrated with nearby Pan-STARRS stars without the Galactic extinction correction. We acknowledge the excellent support from T.Q. Chen and J.L. He for enabling these observations.
GCN 40835 table
GRB_name GRB250625A
GCN_number 40835
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 40835 SUBJECT: GRB 250625A: Swift-XRT refined Analysis DATE: 25/06/26 05:57:53 GMT FROM: Phil Evans at U of Leicester S. Dichiara (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), M. Capalbi (INAF-OAR), M. Perri (SSDC & INAF-OAR), V. D'Elia (SSDC & INAF-OAR), J.A. Kennea (PSU), D.N. Burrows (PSU) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 6.0 ks of XRT data for GRB 250625A, from 123 s to 45.1 ks after the trigger. The data comprise 58 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The light curve can be modelled with a series of power-law decays. The initial decay index is alpha=0.8 (+1.1, -1.2). At T+174 s the decay steepens to an alpha of 6.3 (+/-1.7) before breaking again at T+238 s to a final decay with index alpha=1.19 (+0.17, -0.15). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.68 (+0.32, -0.29). The best-fitting absorption column is 1.7 (+1.3, -1.0) x 10^21 cm^-2, in excess of the Galactic value of 5.5 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 4.3 x 10^-11 (5.2 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 1.7 (+1.3, -1.0) x 10^21 cm^-2 Galactic foreground: 5.5 x 10^20 cm^-2 Excess significance: 1.9 sigma Photon index: 1.68 (+0.32, -0.29) If the light curve continues to decay with a power-law decay index of 1.19, the count rate at T+24 hours will be 5.0 x 10^-4 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.2 x 10^-14 (2.6 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/01327910. This circular is an official product of the Swift-XRT team.
GCN 40836 table
GRB_name GRB250625A
GCN_number 40836
Detection_method Fermi LAT Det
t_trigger 16:04:57.510 UTC
ra 261.2000°
decl 22.4000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 40836 SUBJECT: GRB 250625A: Fermi-LAT detection DATE: 25/06/26 08:10:58 GMT FROM: Davide Depalo at Politecnico and INFN Bari N. Di Lalla (Stanford Univ.), A. Holzmann Airasca (UniTrento and INFN Bari), R. Gupta (NASA GSFC), and D. Depalo (Politecnico and INFN Bari) report on behalf of the Fermi-LAT Collaboration: On June 25, 2025, Fermi-LAT detected high-energy emission from GRB 250625A, which was also detected by Fermi-GBM (trigger 772560301 / 250625670, GCN 40824), Swift-BAT/XRT (GCN 40825) and SVOM/VT (GCN 40830). The best LAT on-ground location is found to be: RA, Dec = 261.2, 22.4 (J2000) with an error radius of 0.6 deg (90 % containment, statistical error only). This was 32 deg from the LAT boresight at the time of the GBM trigger (T0 = 16:04:57.51 UT). The data from the Fermi-LAT shows a significant increase in the event rate that is spatially and temporally correlated with the GBM emission with high significance. The photon flux above 100 MeV in the time interval 0 - 100 s after the GBM trigger is (1.12 ± 0.48) E-5 ph/cm2/s. The estimated photon index above 100 MeV is -2.00 ± 0.38. The highest-energy photon is a 580 MeV event which is observed ~ 27 seconds after the GBM trigger. The Fermi-LAT point of contact for this burst is Davide Depalo (d.depalo2@phd.poliba.it). 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.