//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10581 SUBJECT: GRB 100413A: Swift detection of a burst DATE: 10/04/13 17:51:18 GMT FROM: Scott Barthelmy at NASA/GSFC S. T. Holland (CRESST/USRA/GSFC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), S. Campana (INAF-OAB), M. M. Chester (PSU), P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU), E. A. Hoversten (PSU), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL), V. Mangano (INAF-IASFPA), J. Mao (INAF-OAB), F. E. Marshall (NASA/GSFC), P. T. O'Brien (U Leicester), K. L. Page (U Leicester), D. M. Palmer (LANL), J. L. Racusin (NASA/GSFC), A. Rowlinson (U Leicester), B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU), M. Stamatikos (OSU/NASA/GSFC), M. A. Stark (PSU), R. L. C. Starling (U Leicester), M. C. Stroh (PSU), G. Tagliaferri (INAF-OAB), E. Troja (NASA/GSFC/ORAU) and T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team: At 17:33:28 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 100413A (trigger=419404). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 266.217, +15.837 which is RA(J2000) = 17h 44m 52s Dec(J2000) = +15d 50' 14" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a single peak with a duration of about 15 sec. The peak count rate was ~700 counts/sec (15-350 keV), at ~1 sec after the trigger. The XRT began observing the field at 17:35:48.4 UT, 140.0 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source located at RA, Dec 266.22043, 15.83309 which is equivalent to: RA(J2000) = 17h 44m 52.90s Dec(J2000) = +15d 49' 59.1" with an uncertainty of 3.8 arcseconds (radius, 90% containment). This location is 18 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 http://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 (7.3e+20 cm^-2, Kalberla et al. 2005), with an excess column of 2 (+1.81/-1.60) x 10^21 cm^-2 (90% confidence). The initial flux in the 2.5 s image was 6.30e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 149 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 0.11. Burst Advocate for this burst is S. T. Holland (Stephen.T.Holland AT nasa.gov). 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.) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10582 SUBJECT: GRB 100413A: MASTER-Net optical observations DATE: 10/04/13 19:34:34 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs K.Ivanov, S.Yazev, N.M.Budnev, E.Konstantinov, V.Lenok, O.Gres, O. Irkutsk State University K.Ivanov, S.Yazev, N.M.Budnev, E.Konstantinov, V.Lenok, O.Gres, O. Chuvalaev Irkutsk State University V.Yurkov, Yu.Sergienko, D.Varda, A.Garusina Blagoveschensk Educational State University, Blagoveschensk E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina, D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov, D.Zemnukhov, M. Kornilov Sternberg Astronomical Institute, Moscow State University A. Tlatov, A.V. Parhomenko, D. Dormidontov Kislovodsk Solar Station of the Pulkovo Observatory V.Krushinski, I.Zalozhnih, T.Kopytova, A.Popov Ural State University, Kourovka Two MASTER robotic telescopes (MASTER-Net: http://observ.pereplet.ru, testing telescopes) located at Baykal-Tunka and Blagoveschensk was responted to the GRB 100413A (Swift Bat alert, Holland et al, GCN CIRC 10581) 32 sec after Notice time and 65 s after the GRB time. There is now OT on the first 20-s exposition time unfiltered images inside Swift XRT error box (Holland et al., GCN CIRC 10581) brighter 17.0 (Blagoveschensk) and 16.6 (Baykal-Tunka). The message may be cited. mailto: lipunov@sai.msu.ru //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10583 SUBJECT: GRB 100413: xinglong TNT optical upper limit DATE: 10/04/13 19:49:41 GMT FROM: L.P. Xin at NAOC L.P. Xin, H. Liu, Y.L. Qiu, J.Y. Wei,J. Wang, J.S. Deng, C. Wu, J.Y. Hu, W.K. Zheng on behalf of EAFON report: We began to observe GRB100413 (Holland et al., GCN 10581, Ivanov et al. GCN 10582) with Xinglong TNT telescope at 17:44:03(UT),10min 35s after the burst. A series of white, R band images were obtained. No new source (Ivanov et al. GCN 10582) is found in the XRT errorbars within the combined 20*20s white band data. The 3 sigma upper limit is about 20.6 mag derived from USNO-B1.0,at the mean time of 13 min after the burst. Further observations are encouraging. This message may be cited. For more information about Xinglong GRBs Follow-up observations, please visit the website: http://www.xinglong-naoc.org/grb/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10584 SUBJECT: GRB 100413A: Enhanced Swift-XRT position DATE: 10/04/13 20:59:31 GMT FROM: Phil Evans at U of Leicester M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team. Using 952 s of XRT Photon Counting mode data and 1 UVOT images for GRB 100413A, 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 = 266.22175, +15.83400 which is equivalent to: RA (J2000): 17h 44m 53.22s Dec (J2000): +15d 50' 02.4" with an uncertainty of 1.8 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. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10585 SUBJECT: GRB 100413A: Swift-BAT initial refined analysis DATE: 10/04/13 21:07:15 GMT FROM: Scott Barthelmy at NASA/GSFC M. Stamatikos (GSFC/ORAU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), S. T. Holland (CRESST/USRA/GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), J. Tueller (GSFC), T. N. Ukwatta (GWU) (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 100413A (trigger #419404) (Holland, et al., GCN Circ. 10581). The BAT ground-calculated position is RA, Dec = 266.223, 15.833 deg, which is RA(J2000) = 17h 44m 53.4s Dec(J2000) = +15d 50' 00.3" with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment). The partial coding was 48%. The mask-weighted light curve shows multiple overlapping peaks in two main clusters of peaks. It starts at ~T-45 sec, with the first cluster ending at ~T+40 sec. The second cluster starts around T+90 sec, peaks around T+100 sec, and ends later than T+240 sec. The emission does not return to background between the two clusters. We are issuing this refined circular prior to receiving all the data, because there is a backlog in the downlinking of the data and it will be many hours until receive the data past T+240 sec. These results will be updated when we receive the full data set. Using this partial data set, the time-averaged spectrum from T-1.5 to T+213.1 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.17 +- 0.07. The fluence in the 15-150 keV band is 6.2 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+116.78 sec in the 15-150 keV band is 0.7 +- 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/419404/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10586 SUBJECT: GRB 100413A: Swift-XRT Refined Analysis DATE: 10/04/14 08:16:31 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester) and S. T. Holland (CRESST/USRA/GSFC) report on behalf of the Swift-XRT team: We have analysed 5.3 ks of XRT data for GRB 100413A (Holland et al. GCN Circ. 10581), from 129 s to 30.4 ks after the BAT trigger. The data comprise 551 s in Windowed Timing (WT) mode (the first 9 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Goad et al. (GCN. Circ 10584). The light curve can be modelled with a series of power-law decays. The initial decay index is alpha=2.53 (+/- 0.07). At T+430 s the decay flattens to an alpha of 1.20 (+/- 0.04). The light curve breaks again at T+9980 s to a poorly-constrained final decay with alpha=2.3 (-0.5, positive error is unconstrained). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.83 (+/-0.06). The best-fitting absorption column is 2.42 (+0.19, -0.18) x 10^21 cm^-2, in excess of the Galactic value of 7.3 x 10^20 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index of 2.06 (+0.13, -0.12) and a best-fitting absorption column of 3.1 (+/-0.4) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.5 x 10^-11 (7.4 x 10^-11) erg cm^-2 count^-1. If the light curve continues to decay with a power-law decay index of 2.3, the count rate at T+24 hours will be 2.02 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.1 x 10^-14 (1.5 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/00419404. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10587 SUBJECT: GRB 100413A: SARA upper limit DATE: 10/04/14 09:29:16 GMT FROM: Adria C. Updike at Clemson U Adria C. Updike, Dieter H. Hartmann (Clemson University), Loris Magnani (UGA), and Chris De Pree (Agnes Scott College) report: We observed the field of GRB 100413A (Holland et al., GCN 10581) with the 0.9m SARA-North telescope at KPNO beginning at 06:57 UT on April 14, 2010 (13.4 hours after the trigger) at high airmass and continuing for 40 minutes. At the location of the enhanced XRT error circle (Goad et al., GCN 10584) we do not detect any new sources in stacked I-band images down to a limiting magnitude of I ~ 19 (as compared to the USNO B1.0 catalog). No further observations are planned. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10588 SUBJECT: Tentative redshift of GRB100413A from X-ray data DATE: 10/04/14 10:39:40 GMT FROM: Sergio Campana at INAF-OAB S. Campana (INAF-OAB), P.A. Evans (U. Leicester) and S. T. Holland (CRESST/USRA/GSFC) report on behalf of the Swift-XRT team: Swift XRT observed GRB 100413A (Holland et al. 2010, GCN 10581) in Windowed Timing (WT) mode in the 146-550 s time interval. During this interval the 1.5-10 keV to 0.3-1.5 keV hardness ratio slightly decayed, testifying for small spectral variations. We assume a Galactic column density of 7.3x10^20 cm^-2 (Kalberla et al. 2005, A&A 440 775) and fit the WT spectrum with an absorbed (tbabs*ztbabs) cutoff power law model within XSPEC (the cutoff power law model provides much better results in terms of column density evaluation with respect to a simple power law model when small spectral variations are present). Data were grouped to have 30 counts per spectral bin. The resulting fit is good (reduced chi2=0.9, 194 dof). Filtering the data for single pixel events does not change the results. In the intrinsic column density vs. redshift plane there is a low significance (3 sigma) solution at low redshifts but the minimum lies at higher redshifts with a 2 sigma confidence level solution of z=3.9+1.7-0.7 and N_H(z)=(5.5+9.8-2.1)x1022 cm-2. Thus, even if we cannot exclude that GRB100413A is at low redshift, a high redshift (z~4), highly absorbed (N_H(z)~6x1022 cm-2) solution is preferred. This compares well with the non-detection with UVOT (Holland et al. 2010) and other robotic telescopes. The contour plot is available at http://www.brera.inaf.it/utenti/campana/100413.gif //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10589 SUBJECT: GRB 100413A: Faulkes Telescope South observations DATE: 10/04/14 12:39:48 GMT FROM: Cristiano Guidorzi at Ferrara U,Italy C. Guidorzi (U. Ferrara), R.J. Smith (Liverpool JMU), N. Tanvir (U. Leicester), I.A. Steele, S. Kobayashi, C.G. Mundell, D. Bersier, Z. Cano, N.R. Clay, A. Melandri, C.J. Mottram (Liverpool JMU), A. Gomboc (U. Ljubljana) report on behalf of a large collaboration: On 2010 April 13 at 17:37:19 UT the 2-m Faulkes Telescope South automatically began observing the Swift GRB 100413A (Holland et al., GCN Circ. 10581) using the BVR, i' filters, corresponding to 231 s after the burst trigger time. Inside the XRT error circle (Goad et al. GCN Circ. 10584) we do not detect any source at the following limiting magnitudes: Mid time from Total Exp Filter Magnitude trigger (min) (s) ------------------------------------------------ 04.52 3x10 R > 19.8 28.6 540 R > 22.2 33.2 520 i > 21.3 ------------------------------------------------ Magnitudes have been calibrated from nearby USNOB-1 stars, using the R2 and I magnitudes. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10590 SUBJECT: Konus-Wind observation of GRB 100413A DATE: 10/04/14 13:39:18 GMT FROM: Valentin Pal'shin at Ioffe Inst S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind team report: The long GRB 100413A (Swift-BAT trigger #419404: Holland et al., GCN 10581; Stamatikos et al., GCN 10585) was detected by Konus-Wind in the waiting mode. The burst light curve shows a multipeaked structure with a total duration of ~220 s. As observed by Konus-Wind, the burst had a fluence of (2.66 +/- 0.23)x10^-5 erg/cm2 (in the 20 - 1200 keV energy range). Modeling the K-W 3-channel time-integrated spectrum (from T0-3 s to T0+212 s) by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) yields alpha = -1.01 ± 0.06, Ep = 446 +/- 123 keV. All the quoted errors are estimated at the 1 sigma confidence level. The K-W light curve of this burst is available at http://www.ioffe.rssi.ru/LEA/GRBs/GRB100413A/ Assuming z ~ 3.9 (Campana, Evans, and Holland, GCN 10588) and a standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M = 0.27, Omega_Lambda = 0.73, the isotropic energy release is E_iso ~8x10^53 erg, and Ep_rest ~2200 keV. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10591 SUBJECT: GRB 100413A: Swift/UVOT Upper Limits DATE: 10/04/14 17:07:25 GMT FROM: Frank Marshall at GSFC F.E. Marshall (NASA/GSFC) and S.T. Holland (CRESST/USRA/GSFC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 100413A 150 s after the BAT trigger (Holland et al., GCN Circ. 10581). No optical afterglow consistent with the enhanced XRT position (Goad et al., GCN Circ. 10584) is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC) exposures and subsequent exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white_FC 150 300 147 >20.5 u_FC 308 558 246 >20.5 white 150 6231 589 >21.8 v 639 6641 490 >20.4 b 564 7321 353 >20.7 u 308 7256 717 >20.7 w1 688 7051 471 >20.5 m2 663 6846 490 >20.4 w2 614 6436 491 >20.8 The values quoted above are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.11 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10592 SUBJECT: GRB 100413A: GROND Upper limits DATE: 10/04/14 17:10:42 GMT FROM: Thomas Kruehler at MPE/MPI Robert Filgas, Thomas Kruehler, Jochen Greiner and Abdullah Yoldas (all MPE Garching) report on behalf of the GROND team: We observed the field of GRB 100413A (Swift trigger 419404; Holland et al., GCN #10581) simultaneously in g'r'i'z'JHK with GROND (Greiner et al., 2008, PASP 120, 405) mounted at the 2.2 m MPI/ESO telescope at La Silla Observatory (Chile). Observations started at 05:43 UT on April 14, 12 hours after the GRB trigger, and continued for 2.5 hours. They were performed at an average seeing of 1" under clear sky conditions. In stacked images of 125 min total integration time in g'r'i'z' and 100 min in JHK, we do not detect a source within the Swift/XRT error circle (Goad et al., GCN #10584) down to the following 3 sigma limiting magnitudes (all in the AB system): g' > 25.3, r' > 25.2, i' > 24.6, z' > 24.3, J > 22.5, H > 22.1 and K > 21.1 These limits were derived by calibrating the images against the GROND zeropoints and 2MASS field stars and are not corrected for the Galactic foreground extinction corresponding to a reddening of E_(B-V)= 0.11 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10600 SUBJECT: GRB 100413A: Swift-BAT final refined analysis DATE: 10/04/15 23:08:38 GMT FROM: Scott Barthelmy at NASA/GSFC S. D. Barthelmy (GSFC), T. Sakamoto (GSFC/UMBC), S. T. Holland (CRESST/USRA/GSFC) (for the Swift-BAT team): The full data set for this burst has been downlinked. Using the data set from T-239 to T+963 sec, we report final analysis of BAT GRB 100413A (trigger #419404) (Holland, et al, GCN Circ 10581 and Stamatikos, GCN Circ 10585). The BAT ground-calculated position is RA, Dec = 266.223, 15.835 deg, which is RA(J2000) = 17h 44m 53.6s Dec(J2000) = +15d 50' 04.6" with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment). The partial coding was 48%. The mask-weighted light curve shows multiple overlapping peaks in two main clusters of peaks. It starts at ~T-45 sec, with the first cluster ending at ~T+40 sec. The second cluster starts around T+90 sec, peaks around T+100 sec, and ends at ~T+250 sec. The emission does not return to background between the two clusters. T90 (15-350 keV) is 191 +- 14 sec (estimated error including systematics). The time-averaged spectrum from T-3.4 to T+227.4 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.25 +- 0.07. The fluence in the 15-150 keV band is 6.2 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+116.78 sec in the 15-150 keV band is 0.7 +- 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/419404/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10604 SUBJECT: GRB 100413A: Suzaku WAM observation of the prompt emission DATE: 10/04/17 06:53:33 GMT FROM: Satoshi Sugita at Aoyama Gakuin U. S. Sugita (Nagoya U.), K. Yamaoka (Aoyama Gakuin U.), M. Ohno, M. Kokubun, T. Takahashi (ISAS/JAXA), Y. E. Nakagawa, M. Suzuki, T. Tamagawa (RIKEN), N. Vasquez (Tokyo Tech.), Y. Urata, H.M. Lin, P. Tsai (NCU), Y. Nishioka, N. Ohmori, A. Daikyuji, E. Sonoda, K. Kono, K. Noda, M. Yamauchi (Univ. of Miyazaki), T. Sugasahara, M. Tashiro, Y. Terada, W. Iwakiri (Saitama U.), Y. Hanabata, T. Uehara, T. Takahashi, Y. Fukazawa (Hiroshima U.), T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo), S. Hong (Nihon U.), on behalf of the Suzaku WAM team, report The very long GRB 100413A (Swift/BAT trigger #419404 ; Holland et al., GCN 10581) was detected by the the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 2010-04-13 17:33:28 UT (=T0). The observed light curve shows a multi-peaked structure lasting to T0+220s with a duration T90 of about 160 seconds. The fluence in 100 - 1000 keV was 1.59 (-0.83, +0.21) x10^-5 erg/cm^2. The 1-s peak flux measured from T0+118s was 0.38 (-0.27, +0.14) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-2s to T0+213s is well fitted by a power-law with exponential cutoff model: dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with alpha -0.59 (-1.64, +1.27), and Epeak 364 (-55, +98) keV (chi^2/d.o.f. = 37.9/30). All the quoted errors are at statistical 90% confidence level, in which the systematic uncertainties are not included. The light curves with 1-sec time resolution for this burst will be appeared at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10611 SUBJECT: GRB 100413A: Radio Afterglow Detection with the EVLA DATE: 10/04/17 23:59:34 GMT FROM: Derek Fox at PSU Dale A. Frail (NRAO) and Derek Fox (PSU) report on behalf of a larger collaboration: "We used the Expanded Very Large Array (EVLA) to observe the localization of the Swift burst GRB 100413A (Trigger #419404; Holland et al., GCN 10581), an X-ray bright event without any optical or NIR counterpart to deep limits (Xin et al., GCN 10583; Updike et al., GCN 10587; Guidorzi et al., GCN 10589; Filgas et al., GCN 10592). Within the revised XRT error circle (Goad et al., GCN 10584) we detect a single 8.5 GHz radio source with flux density 159 +/- 15 uJy and position R.A. 17:44:53.16, Dec. +15:50:03.2 (J2000), with 1-sigma astrometric uncertainty of +/-0.6 arcsec. The EVLA is undergoing active commissioning and as such these results should be considered preliminary. Further observations are planned. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10623 SUBJECT: GRB 100413A: GMRT observation of radio afterglow DATE: 10/04/19 13:59:21 GMT FROM: Sayan Chakraborti at TIFR,Mumbai,India Sayan Chakraborti, Naveen Yadav and Alak Ray (Tata Institute of Fundamental Research, Mumbai, India) report: We observed the optically dark GRB 100413A, whose radio afterglow has been detected by the EVLA at 8.5 GHz (Frail et al, GCN 10611), with the Giant Metrewave Radio Telescope (GMRT) on April 19.1 UT. We do not find, any source at its position, at the observing frequency of 1.28 GHz, down to the 3 sigma upper limit of 124 uJy. We thank the staff of the GMRT that made this observation possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research.