GRB180205A

This page lists all entries on GRB180205A in GRBweb

Summary Fermi GBM IPN Swift GCN 22381 GCN 22382 GCN 22383 GCN 22384 GCN 22386 GCN 22387 GCN 22388 GCN 22390 GCN 22391 GCN 22392 GCN 22393 GCN 22394 GCN 22395 GCN 22396 GCN 22397 GCN 22398 GCN 22401 GCN 22403 GCN 22404 GCN 22411 GCN 22414 GCN 22430

Summary table
Variable Value Source
GRB_name_Fermi GRB180205184
T0 4:25:23.601 UTC Fermi_GBM
ra 126.8198° Swift
decl 11.5419° Swift
pos_error 5.44e-05° Swift
T90 15.36 s Fermi_GBM
T90_error 1.448 s Fermi_GBM
T90_start 4:25:23.601 UTC Fermi_GBM
fluence 2.06e-06 erg/cm² Fermi_GBM
fluence_error 9.85e-08 erg/cm² Fermi_GBM
redshift 1.4090 GCN_circulars,Optical
T100 21.199 s
GBM_located False
mjd 58154.1843009375 Fermi_GBM
Fermi GBM table
GRB_name_Fermi GRB180205184
trigger_name bn180205184
ra 126.8208°
decl 11.5419°
datum 2018-02-05
t_trigger 4:25:25.393 UTC
T90 15.36 s
T90_error 1.448 s
T90_start 4:25:23.601 UTC
fluence 2.06e-06 erg/cm²
fluence_error 9.85e-08 erg/cm²
flux_1024 4.74e+00 erg/cm²/s
flux_1024_error 2.92e-01 erg/cm²/s
flux_1024_time 3.71e+00 erg/cm²/s
flux_64 7.38e+00 erg/cm²/s
flux_64_error 1.31e+00 erg/cm²/s
IPN table
GRB_name GRB180205A
ra 126.8208°
decl 11.5500°
pos_error 5.00e-02°
redshift 1.4090
Swift table
GRB_name GRB180205A
t_trigger 4:25:29.300 UTC
ra 126.8198°
decl 11.5419°
pos_error 5.44e-05°
T90 15.5 s
fluence 1.00e-06 erg/cm²
redshift 1.4090
GCN 22381 table
GRB_name GRB180205A
GCN_number 22381
Detection_method Swift Det
t_trigger 4:28:23.600 UTC
ra 126.8206°
decl 11.5419°
Circular_text TITLE: GCN CIRCULAR NUMBER: 22381 SUBJECT: GRB 180205A: Swift detection of a burst with a bright optical counterpart DATE: 18/02/05 04:45:57 GMT FROM: David Palmer at LANL P. A. Evans (U Leicester), J. A. Kennea (PSU), K. L. Page (U Leicester) and D. M. Palmer (LANL) report on behalf of the Neil Gehrels Swift Observatory Team: BAT has detected GRB 180205A (trigger #808625), leading to a slew and follow-up observations by Swift. However, due to missing telemetry packets, no further BAT information is available at this time. The XRT began observing the field at 04:28:23.6 UT. XRT found a bright, uncatalogued X-ray source located at RA, Dec 126.8206, 11.5419 which is equivalent to: RA(J2000) = +08h 27m 16.94s Dec(J2000) = +11d 32' 30.8" with an uncertainty of 5.6 arcseconds (radius, 90% containment). No event data are yet available to determine the column density using X-ray spectroscopy. The initial flux in the 2.5 s image was 9.50e-10 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter at 04:28:30.79 UT. There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at RA(J2000) = 08:27:16.73 = 126.81970 DEC(J2000) = +11:32:30.7 = 11.54185 with a 90%-confidence error radius of about 0.61 arc sec. This position is 3.2 arc sec. from the center of the XRT error circle. The estimated magnitude is 15.65 with a 1-sigma error of about 0.14. No correction has been made for the expected extinction corresponding to E(B-V) of 0.03. Burst Advocate for this burst is P. A. Evans (pae9 AT star.le.ac.uk). 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/too.html.)
GCN 22382 table
GRB_name GRB180205A
GCN_number 22382
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 22382 SUBJECT: GRB 180205A: KAIT optical afterglow confirmation DATE: 18/02/05 05:15:27 GMT FROM: Weikang Zheng at UC Berkeley WeiKang Zheng and Alex Filippenko (UC Berkeley) report on behalf of the KAIT GRB team: The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at Lick Observatory, responded to Swift GRB 180205A (Evans, et al.,GCN 22381), starting at 04:31:40 UT immediately after receiving the trigger. Observations were performed with an automatic sequence in the clear (roughly R), V, and I filters, and the exposure time was 20 s per imag. We detect the bright optical afterglow reported by UVOT (Evans, et al.,GCN 22381). It faded from clear ~15.6 mag from our first clear band image to ~16.8 mag 22.5 minutes later, we therefore confirm it to be the optical afterglow of GRB 180205A.
GCN 22383 table
GRB_name GRB180205A
GCN_number 22383
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 22383 SUBJECT: GRB 180205A: GROND detection of the NIR/optical afterglow DATE: 18/02/05 06:02:56 GMT FROM: Jan Bolmer at MPE/Garching J. Bolmer (ESO/MPE) and D.A. Kann (HETH/IAA-CSIC) report: We observed the field of GRB 180205A (Swift trigger 808625; P.A. Evans et al., GCN 22381) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla Observatory (Chile). Observations started at 04:38 UT on February 05, 2018, 13 minutes after the GRB trigger. They were performed at an average seeing of 1".1 and at an average airmass of 1.33. We clearly detect the NIR/optical transient of GRB 181205A reported also by Zheng et al., GCN 22382. Based on total exposures of 200 seconds in g’r'i'z’ and 180 seconds in JHK at a midtime of 04:43 UT, 17 minutes after the burst, we measure the following preliminary magnitudes (AB magnitude system): g' = 16.83 +/- 0.01 mag, r' = 16.68 +/- 0.01 mag, i' = 16.56 +/- 0.01 mag, z' = 16.38 +/- 0.01 mag, J = 16.22 +/- 0.02 mag, H = 16.05 +/- 0.02 mag, and K = 16.08 +/- 0.14 mag. Magnitudes and are calibrated against PanSTARRS and 2MASS field stars and are not corrected for the Galactic foreground extinction corresponding to a reddening of E_(B-V)= 0.03 mag in the direction of the burst (Schlegel et al. 1998). Observations are continuing. We thank Markus Rabus for the excellent support from La Silla.
GCN 22384 table
GRB_name GRB180205A
GCN_number 22384
Detection_method Optical
redshift 1.4090
Circular_text TITLE: GCN CIRCULAR NUMBER: 22384 SUBJECT: GRB 180205A: VLT/X-shooter redshift DATE: 18/02/05 10:09:25 GMT FROM: Nial Tanvir at U.Leicester N. R. Tanvir (U. Leicester), K. E. Heintz (U. Iceland, DARK/NBI), J. Selsing (DARK/NBI), J. Japelj (API, U. Amsterdam), J. Bolmer (ESO/MPE), D. A. Kann (HETH/IAA-CSIC), D. Xu (NAOC), A. de Ugarte Postigo (HETH/IAA-CSIC and DARK/NBI), D. Malesani (DARK/NBI), J. P. U. Fynbo (NBI), G. Pugliese (API, U. Amsterdam) report on behalf of the STARGATE Consortium: We observed the bright optical counterpart of the Swift GRB 180205A (Evans et al. GCN 22381; Zheng et al. GCN 22382; Bolmer et al. GCN 22383) with the ESO Very Large Telescope UT 2 (Kueyen) equipped with the X-shooter spectrograph, covering the wavelength range 3500-24000 AA. Observations started on February 05.25 UT (approx 1.5 hr after the GRB) and consisted of 4 exposures of 600 s each. The spectrum exhibits many absorption features including C II, Si II, Si II*, Al II, Fe II, Mg II, Mg I at a common redshift of z=1.409. We conclude this is the redshift of the GRB. We acknowledge the expert support from the ESO observing staff, in particular Jesus Corral-Santana and Cedric Ledoux.
GCN 22386 table
GRB_name GRB180205A
GCN_number 22386
Detection_method Fermi GBM Det
t_trigger 4:25:25.390 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 22386 SUBJECT: GRB 180205A: Fermi GBM observation DATE: 18/02/05 19:12:58 GMT FROM: Andreas von Kienlin at MPE A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team: "At 04:25:25.39 UT on 05 February 2018, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 180205A (trigger 539497530 / 180205184), which was also detected by the Swift/BAT (Evans et al. 2008, GCN 22381) The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight at the GBM trigger time is 94 degrees. The GBM light curve shows several pulses with a duration (T90) of about 15 s (50-300 keV). The GBM detectors were turned off for SAA entry about 70 seconds after the trigger. The time-averaged spectrum from T0-2.048 s to T0+9.216 s is well fit by a power law function with an exponential high-energy cutoff. The power law index is -1.38 +/- 0.15 and the cutoff energy, parameterized as Epeak, is 85.0 +/- 14.4 keV The event fluence (10-1000 keV) in this time interval is (1.5 +/- 1.4)E-06 erg/cm^2. The 1.024-sec peak photon flux measured starting from T0+3.71204 s in the 10-1000 keV band is 4.7 +/- 0.3 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 22387 table
GRB_name GRB180205A
GCN_number 22387
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 22387 SUBJECT: GRB 180205A: Mondy optical observations DATE: 18/02/05 19:19:37 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Volnova (IKI), A. Pozanenko (IKI), E. Klunko (ISTP), E. Mazaeva (IKI) report on behalf of of larger GRB follow-up collaboration: We observed the field of GRB 180205A (Evans et al., GCN 22381) with AZT-33IK telescope of Sayan observatory (Mondy). We took several images in R-filter starting on Feb. 05 (UT) 12:54:29. The afterglow of GRB 180205A (Evans et al., GCN 22381; Zheng et al., GCN 22382; Bolmer et al., GCN 22383) is clearly detected in a stacked image. Preliminary photometry is following. Date UT start t-T0 Filter Exp. OT Err. UL (mid, days) (s) 2018-02-05 12:54:29 0.372* R 30*120 19.47 0.07 21.8 * The time after XRT observation start at (UT) 04:28:23.69. The photometry is based on several nearby SDSS DR9 stars SDSS_id R_Lupton J082719.98+113324.0 16.206 0.013 J082717.26+113400.0 16.092 0.013 J082715.06+113230.6 15.553 0.013
GCN 22388 table
GRB_name GRB180205A
GCN_number 22388
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 22388 SUBJECT: GRB 180205A: VLT polarimetry DATE: 18/02/05 19:20:24 GMT FROM: Klaas Wiersema at U of Warwick K. Wiersema (Warwick) & S. Covino (INAF / OAB) report on behalf of the Stargate consortium: We observed the afterglow of GRB 180205A (Evans et al. GCN 22381; Zheng et al. GCN 22382; Bolmer et al. GCN 22383, Tanvir et al. GCN 22384) with the ESO Very Large Telescope equipped with FORS2. We obtained a set of imaging polarimetry observations in R band, starting at 07:07 UT (approximately 2.67 hours after burst). Using archival calibration data, we find a low level of polarisation, P ~ 0.9%, similar to the majority of late-time GRB afterglow measurements (Covino & Gotz 2016, A&AT 29, 205). We acknowledge excellent support from the ESO staff.
GCN 22390 table
GRB_name GRB180205A
GCN_number 22390
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 22390 SUBJECT: GRB 180205A: Nickel telescope optical observations DATE: 18/02/06 00:10:25 GMT FROM: Weikang Zheng at UC Berkeley Edward Falcon, Sameen Yunus, WeiKang Zheng and Alex Filippenko (UC Berkeley) report on behalf of the KAIT GRB team: We observed the field of GRB 180205A (Evans et al., GCN 22381) with the 1-m Nickel telescope located at Lick observatory, California. Observations started about 1.32 hours after the burst and lasted for ~1.4 hours. We detected the optical afterglow (Evans et al. GCN 22381; Zheng et al. GCN 22382; Bolmer et al. GCN 22383; Tanvir et al. GCN 22384; Volnova et al. GCN 22387) in all the images taken with B,V,R and I filters. A preliminary light curve is posted at the following link along with KAIT observations (Zheng et al. GCN 22382): http://astro.berkeley.edu/~zwk/grb/GRB180205A/GRB180205A_nickel_kait.png
GCN 22391 table
GRB_name GRB180205A
GCN_number 22391
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 22391 SUBJECT: GRB 180205A: Further GROND Observations reveal Afterglow is still bright DATE: 18/02/06 02:28:56 GMT FROM: Alexander Kann at IAA-CSIC J. Bolmer (ESO/MPE) and D.A. Kann (HETH/IAA-CSIC) report: We once more observed the field of GRB 180205A (Swift trigger 808625; P.A. Evans et al., GCN 22381) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla Observatory (Chile). Observations started at 01:28 UT on February 06, 2018, 0.8765 days after the GRB trigger. They were performed at an average seeing of 1".1 and at an average airmass of 1.68. Based on total exposures of 1320 seconds in g'r'i'z' and 1200 seconds in JHK at a midtime of 01:40 UT, 0.8854 days after the burst, we measure the following preliminary magnitudes (AB magnitude system): g' = 20.29 +/- 0.03 mag, r' = 20.03 +/- 0.03 mag, i' = 19.81 +/- 0.03 mag, z' = 19.66 +/- 0.03 mag, J = 19.47 +/- 0.12 mag, H = 19.16 +/- 0.19 mag, and K > 17.6 mag. These magnitudes are significantly brighter than the extrapolation of our GROND data from the first night (Bolmer & Kann, GCN 22383). We point out that the Nickel/KAIT light curve (E. Falcon, GCN 22390) shows a plateau phase setting in beyond 10ks, at a time we were not able to observe with GROND anymore. This plateau would explain why the afterglow remains bright. Magnitudes and are calibrated against SDSS and 2MASS field stars and are not corrected for the Galactic foreground extinction corresponding to a reddening of E_(B-V)= 0.03 mag in the direction of the burst (Schlegel et al. 1998). Further observations are encouraged. We thank Markus Rabus for the excellent support from La Silla.
GCN 22392 table
GRB_name GRB180205A
GCN_number 22392
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 22392 SUBJECT: GRB 180205A: Xinglong TNT optical observation DATE: 18/02/06 02:43:28 GMT FROM: L.P. Xin at NAOC L. P. Xin, F. Q. Pi, J. Y. Wei, Y. L. Qiu, J. S. Deng, J. Wang, X. H. Han, X. M. Meng, C. Wu, D. TURPIN, H. L. Li report: We began to observe GRB 180205A (Evens et al., GCN 22381) with Xinglong 0.8-m TNT telescope, China, at 2018-02-05, 16:11:42(UT), about 12.6 hours the burst. We obtained several R-band images with an exposure time of 300 sec for each frame. The optical afterglow (Evens et al., GCN 22381; Zheng et al., GCN 22382; Bolmer et al., GCN 22383, 22391; Tanvir et al., GCN 22384; Volnova et al., GCN 22387, Wiersema et al., GCN 22388; Falcon et al., 22390 ) is clearly detected in our stacked image with 5*300 sec. The brightness is estimated to be about R~19.97 mag calibrated by USNO B1.0 R2 mag at about 12.7 hours after the burst, We acknowledge the excellent support from Xinglong staff Miao Zhang.
GCN 22393 table
GRB_name GRB180205A
GCN_number 22393
Detection_method Swift-BAT Det
ra 126.8190°
decl 11.5360°
Circular_text TITLE: GCN CIRCULAR NUMBER: 22393 SUBJECT: GRB 180205A: Swift-BAT refined analysis DATE: 18/02/06 02:57:19 GMT FROM: Amy Lien at GSFC H. A. Krimm (NSF/USRA), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), P. A. Evans (U Leicester), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-240 to T+700 sec from the recent telemetry downlink, we report further analysis of BAT GRB 180205A (trigger #808625) (Evans et al., GCN Circ. 22381). The BAT ground-calculated position is RA, Dec = 126.819, 11.536 deg which is RA(J2000) = 08h 27m 16.5s Dec(J2000) = +11d 32' 11.1" with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment). The partial coding was 50%. The mask-weighted light curve shows a multi-peaked structure that starts at ~T-7 s and ends at ~T+11 s. The two major peaks occur at ~T-5 s and ~T0 s, respectively. T90 (15-350 keV) is 15.5 +- 3.1 sec (estimated error including systematics). The time-averaged spectrum from T-7.04 to T+10.87 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 2.04 +- 0.13. The fluence in the 15-150 keV band is 1.0 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T-0.20 sec in the 15-150 keV band is 3.4 +- 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/808625/BA/
GCN 22394 table
GRB_name GRB180205A
GCN_number 22394
Detection_method Swift-XRT Other
ra 126.8197°
decl 11.5421°
redshift 1.4090
Circular_text TITLE: GCN CIRCULAR NUMBER: 22394 SUBJECT: GRB 180205A: Swift-XRT refined Analysis DATE: 18/02/06 04:46:03 GMT FROM: Phil Evans at U of Leicester K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), A. Tohuvavohu (PSU), S. J. LaPorte (PSU), J.A. Kennea (PSU) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 5.0 ks of XRT data for GRB 180205A (Evans et al. GCN Circ. 22381), from 180 s to 33.8 ks after the BAT trigger. The data comprise 85 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. Using 3849 s of PC mode data and 7 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 = 126.81966, +11.54210 which is equivalent to: RA (J2000): 08h 27m 16.72s Dec(J2000): +11d 32' 31.6" with an uncertainty of 1.5 arcsec (radius, 90% confidence). The light curve can be modelled with an initial power-law decay with an index of alpha=4.8 (+0.6, -0.5), followed by a break at T+279 s to an alpha of 1.00 (+/-0.04). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 2.72 (+0.18, -0.17). The best-fitting absorption column is 8.7 (+2.8, -2.5) x 10^21 cm^-2, at a redshift of 1.409, in addition to the Galactic value of 3.4 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 1.89 (+0.15, -0.14) and a best-fitting absorption column of 3.1 (+3.0, -2.6) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.5 x 10^-11 (4.0 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Galactic foreground: 3.4 x 10^20 cm^-2 Intrinsic column: 3.1 (+3.0, -2.6) x 10^21 cm^-2 at z=1.409 Photon index: 1.89 (+0.15, -0.14) If the light curve continues to decay with a power-law decay index of 1.00, the count rate at T+24 hours will be 0.013 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.5 x 10^-13 (5.2 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/00808625. This circular is an official product of the Swift-XRT team.
GCN 22395 table
GRB_name GRB180205A
GCN_number 22395
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 22395 SUBJECT: GRB 180205A: Nanshan-1m optical observations DATE: 18/02/06 12:02:12 GMT FROM: Dong Xu at NAOC/CAS Z.P. Zhu, H.X. Feng, D. Xu (NAOC), B.Y. Yu (HNU), J.H. Liu, X. Zhang, H.B. Niu, S.G. Ma, J.Z. Liu, A. Esamdin, L. Ma, Y. Zhang (XAO) report on behalf of a larger collaboration: We observed the field of GRB 180205A (Evens et al., GCN 22381) using the 1m telescope located at Nanshan, Xinjiang, China, and 10x60s R-band frames, starting at 16:31:07 UT on 2018-02-05. The optical afterglow (e.g., Evens et al., GCN 22381; Zheng et al., GCN 22382) is clearly detected in our stacked image. Preliminary photometry results are as follows: Tmid-T0 Exposure Filter Mag MagErr (hr) (s) 12.15 10x60 R 19.67 0.10 Photometry is calibrated with nearby SDSS stars, and errors are only statistical values.
GCN 22396 table
GRB_name GRB180205A
GCN_number 22396
Detection_method Swift-UVOT Det
ra 126.8197°
decl 11.5419°
Circular_text TITLE: GCN CIRCULAR NUMBER: 22396 SUBJECT: GRB 180205A: Swift/UVOT Detection DATE: 18/02/06 12:58:32 GMT FROM: Sam Emery at MSSL-UCL S.W.K. Emery (UCL-MSSL) and P. A. Evans (U Leicester) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 180205A 182 s after the BAT trigger (Evans et al., GCN Circ. 22381). A fading source consistent with the XRT position (Page et al., GCN Circ. 22394), also detected by (Zheng et al. GCN 22382; Bolmer et al. GCN 22383; Tanvir et al. GCN 22384; Volnova et al. GCN 22387; Falcon et al. GCN 22390; Xin et al. 22392; Zhu et al. GCN 22395) is detected in the initial UVOT exposures. The preliminary UVOT position is: RA (J2000) = 08:27:16.74 = 126.81975 (deg.) Dec (J2000) = +11:32:30.9 = 11.54191 (deg.) with an estimated uncertainty of 0.42 arc sec. (radius, 90% confidence). Preliminary detections using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding chart (FC) exposure and the early exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white_FC 182 331 147 15.75 +/- 0.02 white 540 732 36 16.33 +/- 0.02 v 158 612 52 16.11 +/- 0.09 b 515 710 39 16.65 +/- 0.07 u 490 686 39 16.82 +/- 0.07 uvw1 466 661 39 16.04 +/- 0.10 uvm2 441 636 39 16.32 +/- 0.15 uvw2 391 585 39 17.06 +/- 0.17 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.03 in the direction of the burst (Schlegel et al. 1998).
GCN 22397 table
GRB_name GRB180205A
GCN_number 22397
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 22397 SUBJECT: GRB 180205A: Optical observations DATE: 18/02/06 14:45:44 GMT FROM: Myungshin Im at Seoul Nat U Myungshin Im, Changsu Choi, Gregory S. Paek, Sung A O, Sophia Kim (CEOU/SNU), Yuji Urata (NCU), H.-I. Sung (KASI) on behalf of a larger collaboration We observed the afterglow of GRB 180205A (Evans et al., GCN 22381; Zheng et al. GCN 22382; Bolmer et al. GCN 22383; Tanvir et al. GCN 22384; Volnova et al. GCN 22387; Falcon et al. GCN 22380; Xin et al. 22392; Zhu et al. 22395; Emery et al. 22396) with the 1-m telescope at the Mt. Lemmon Optical Astronomy Observatory (LOAO) and the 0.8m and 0.25 telescopes at the McDonald Observatory. The observation started at about 1 hour after the initial alert, using B, V, R, I, z, and Y filters. The observation continued throughout the night. We clearly identify the optical afterglow in these bands, and ​a ​ preliminary photometry in R-band shows R ~ 18 mag at 1.3 hours post-burst. Further observations and analysis are being carried out ​, including telescopes in Korea​ . Additional ​results ​ will be reported ​ as they become available​ .
GCN 22398 table
GRB_name GRB180205A
GCN_number 22398
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 22398 SUBJECT: GRB 180205A: confirmation of Swift-BAT trigger time. DATE: 18/02/06 16:04:12 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester) and D.M. Palmer (LANL) report on behalf of the Swift team: Due to a telemetry gap, the trigger time of GRB 180205A was not reported in the early GCN Circulars. The BAT trigger time was 04:25:29.3 UT (on 2018 Feb 5). We apologise for any inconvenience caused by the omission. This circular is an official product of the Swift team. [GCN OPS NOTE(06feb18): Per author's request, "UT" was added to the time listed in the second sentence.]
GCN 22401 table
GRB_name GRB180205A
GCN_number 22401
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 22401 SUBJECT: GRB 180205A optical observations DATE: 18/02/07 10:52:14 GMT FROM: Arto Oksanen at Nyrola Obs., Finland Arto Oksanen (Hankasalmi Obs., Hankasalmi, Finland) and D. Malesani (DARK/NBI) report the following observations of GRB 180205A (Evans et al., GCN 22381): A. Oksanen observed the location of GRB 180205A using the Hankasalmi Observatory 0.4-m Richey-Chretien telescope with an SBIG STL-1001E camera. Forty 60-second frames were obtained with clear filter between 18:19 UT and 19:41 UT on 2018 February 5. The afterglow is detected in co-added image. Photometry of co-added image yields the following: t-t0(d) m(CR) err(CR) 0.605 19.43 0.06 Photometry was performed using comparison stars from the Pan-STARRS survey (Chambers et al. 2016; arXiv:1612.05560), after adopting the conversion formulae by Lupton (2005).
GCN 22403 table
GRB_name GRB180205A
GCN_number 22403
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 22403 SUBJECT: GRB 180205A: AbAO optical observations DATE: 18/02/08 07:52:59 GMT FROM: Alexei Pozanenko at IKI, Moscow E. Mazaeva (IKI), A. Pozanenko (IKI), A. Volnova (IKI), R. Inasaridze (AbAO), V. Ayvazian (AbAO), O. Kvaratskhelia (AbAO), G. Inasaridze (AbAO), I. Molotov (KIAM), report on behalf of larger GRB follow-up collaboration: We observed the field of GRB 180205A (Evans et al., GCN 22381) with AS-32 (0.7m) telescope of Abastumani Observatory starting on Feb., 06 (UT) 23:53:51. We obtained several unfiltered images starting on Feb. 05 (UT) 12:54:29. The afterglow of GRB 180205A (Evans et al., GCN 22381; Zheng et al. GCN 22382; Bolmer et al. GCN 22383; Tanvir et al. GCN 22384; Volnova et al. GCN 22387; Falcon et al. GCN 22380; Xin et al. 22392; Zhu et al. 22395; Emery et al. 22396; Im et al., GCN 22397) is clearly detected in a stacked image. Preliminary photometry is following. Date UT start t-T0 Filter Exp. OT Err. UL (mid, days) (s) 2018-02-06 17:09:23 1.54515 CR 24*60 20.32 0.10 21.2 The photometry is based on several nearby SDSS DR9 stars SDSS_id R_Lupton J082719.98+113324.0 16.206 0.013 J082717.26+113400.0 16.092 0.013 J082715.06+113230.6 15.553 0.013
GCN 22404 table
GRB_name GRB180205A
GCN_number 22404
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 22404 SUBJECT: GRB180205A: Optical observations with DOAO 1m telescope DATE: 18/02/08 13:46:01 GMT FROM: Myungshin Im at Seoul Nat U Changsu Choi, Myungshin Im (CEOU/SNU), Tae-Woo Kim, Wonseok Kang (KYSC), on behalf of a larger collaboration. We observed the field of GRB 180205A (Evans et al., GCN 22381) with the 1m telescope of Deokheung Optical Astronomy Observatory (DOAO) in Korea, starting from 2018/02/05 11:22:11 for three consecutive nights. We obtained B, V, R-band images and clearly detected the afterglow in a series of 300s exposure images. The afterglow in R band The afterglow is dimming at a rate of about 0.75 mag per day fon average rom 02/05 to 02/07 (Evans et al., GCN 22381; Zheng et al. GCN 22382; Bolmer et al. GCN 22383; Tanvir et al. GCN 22384; Volnova et al. GCN 22387; Falcon et al. GCN 22380; Xin et al. GCN 22392; Zhu et al. GCN 22395; Emery et al. GCN 22396; Im et al., GCN 22397; Oksanen et al. 22401; Mazaeva et al., GCN 22403). Date UT mid Filter Exp. Mag(Vega) Err 2018-02-05 11:14:41 R 300s 19.47 0.12 2018-02-05 11:56:58 R 300s 19.48 0.08 2018-02-06 12:04:55 R 1200s 20.38 0.05 2018-02-06 14:07:30 R 1200s 20.29 0.04 2018-02-07 12:20:31 R 1200s 20.88 0.06 2018-02-07 13:57:28 R 1200s 21.14 0.07 The photometric calibration is based on the APASS stars within 6' radius from GRB. The observation is continuing.
GCN 22411 table
GRB_name GRB180205A
GCN_number 22411
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 22411 SUBJECT: GRB 180205A: BAO optical observations DATE: 18/02/11 10:53:10 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Volnova (IKI), A. Novichonok (KIAM), A. Pozanenko (IKI), S. Kotov (SAO RAS), T. Movsesyan (BAO), E. Mazaeva (IKI) report on behalf of of larger GRB follow-up collaboration: We observed the field of GRB 180205A (Evans et al., GCN 22381) with Schmidt-1m telescope of Byurakan Astrophysical Observatory (BAO). We took several images in r (Sloan)-filter starting on Feb. 08 (UT) 12:54:29. The afterglow of GRB 180205A (Evans et al., GCN 22381; Zheng et al. GCN 22382; Bolmer et al. GCN 22383;Tanvir et al. GCN 22384; Volnova et al. GCN 22387; Falcon et al. GCN 22380; Xin et al. GCN 22392; Zhu et al. GCN 22395; Emery et al. GCN 22396; Im et al., GCN 22397; Oksanen et al. 22401; Mazaeva et al., GCN 22403) is clearly detected in a stacked image. Preliminary photometry is following. Date UT start t-T0 Filter Exp. OT Err. UL (mid, days) (s) 2018-02-08 18:00:00 3.59550 r 12*300 21.3 0.2 21.9 The photometry is based on several nearby SDSS DR9 stars SDSS_id r J082719.98+113324.0 16.357 0.005 J082717.26+113400.0 16.292 0.005 J082715.06+113230.6 15.744 0.004
GCN 22414 table
GRB_name GRB180205A
GCN_number 22414
Detection_method Optical
redshift 1.4090
Circular_text TITLE: GCN CIRCULAR NUMBER: 22414 SUBJECT: GRB 180205A: SEDM Observations DATE: 18/02/13 15:30:27 GMT FROM: Virginia Cunningham at U of MD V. Cunningham (U of Maryland), J. D. Neill (Caltech), S. B. Cenko (NASA GSFC), and R. Walters (Caltech) report on behalf of the SEDM team: We observed the optical counterpart to GRB 180205A (Evans et al., GCN 22381) with the Spectral Energy Distribution Machine (SEDM) on the 60 inch telescope at Palomar Observatory. The SEDM is a low resolution (R ~ 100) integral field unit spectrometer with a multi-band (ugri) “rainbow” camera imager (see Blagorodnova et al., 2017, astro-ph/1710.02917). The SEDM began observing the optical counterpart at 04:44 UTC (18 minutes after the burst trigger time). We performed 2 x 1350 s exposures over the wavelength range 3800-10600 A. We see no strong evidence for emission or absorption features at the quoted redshift of z=1.409 (Tanvir et al., GCN 22384). The continuum emission is well-fit by a power law spectrum with index alpha = 0.77 (f_nu ~ nu^-alpha). [GCN OPS NOTE(07sep19): Per author's request, in the last sentence the "alpha = 0.67" was changed to "alpha = 0.77".]
GCN 22430 table
GRB_name GRB180205A
GCN_number 22430
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 22430 SUBJECT: GRB 180205A: Mondy optical observations DATE: 18/02/21 16:55:22 GMT FROM: Alexei Pozanenko at IKI, Moscow E. Mazaeva (IKI), A. Volnova (IKI), A. Pozanenko (IKI), E. Klunko (ISTP) report on behalf of of larger GRB follow-up collaboration: We observed the field of GRB 180205A (Evans et al., GCN 22381) with AZT-33IK telescope of Sayan observatory (Mondy). We obtained several images in R and B-filter on Feb. 05 - Feb. 19. The afterglow of GRB 180205A (Evans et al., GCN 22381; Zheng et al. GCN 22382; Bolmer et al. GCN 22383;Tanvir et al. GCN 22384; Volnova et al. GCN 22387; Falcon et al. GCN 22380; Xin et al. GCN 22392; Zhu et al. GCN 22395; Emery et al. GCN 22396; Im et al., GCN 22397; Oksanen et al. 22401; Mazaeva et al., GCN 22403; Volnova et al., GCN 22411; Cunningham et al., GCN 22414) is detected in stacked images. Preliminary photometry is following. Date UT start t-T0 Filter Exp. OT Err. UL (mid, days) (s) 2018-02-05 15:21:12 0.49438 R 30*120 19.32 0.04 21.9 2018-02-05 16:23:51 0.53094 B 20*120 20.70 0.17 21.3 2018-02-05 20:03:02 0.69011 R 60*60 19.60 0.08 21.7 2018-02-06 16:07:42 1.50850 R 30*120 20.25 0.07 22.0 2018-02-14 15:48:28 9.50557 R 45*120 22.46 0.13 23.9 2018-02-18 13:23:22 13.40481 R 45*120 n/d n/d 23.0 2018-02-19 14:37:56 14.45658 R 45*120 23.6 0.3 23.6 The photometry is based on nearby SDSS DR9 stars SDSS_id R_Lupton J082719.98+113324.0 16.206 0.013 J082717.26+113400.0 16.092 0.013 J082715.06+113230.6 15.553 0.013