GRB100414A

This page lists all entries on GRB100414A in GRBweb

Summary Fermi GBM IPN Fermi LAT GCN 10594 GCN 10595 GCN 10598 GCN 10599 GCN 10601 GCN 10603 GCN 10605 GCN 10606 GCN 10607 GCN 10608 GCN 10609 GCN 10610 GCN 10618 GCN 10632 GCN 10641 GCN 10649 GCN 10697 GCN 10698

Summary table
Variable Value Source
GRB_name_Fermi GRB100414097
T0 2:20:21 UTC Fermi_LAT
ra 192.1248° Fermi_LAT
decl 8.6930° Fermi_LAT
pos_error 1.39e-04° Fermi_LAT
T90 26.497 s Fermi_GBM
T90_error 2.073 s Fermi_GBM
T90_start 2:20:23.842 UTC Fermi_GBM
fluence 8.85e-05 erg/cm² Fermi_GBM
fluence_error 1.86e-07 erg/cm² Fermi_GBM
redshift 1.3680
T100 29.339 s
GBM_located False
mjd 55300.09746527778 Fermi_LAT
Fermi GBM table
GRB_name_Fermi GRB100414097
trigger_name bn100414097
ra 192.1121°
decl 8.6917°
pos_error 2.56e+00°
datum 2010-04-14
t_trigger 2:20:21.986 UTC
T90 26.497 s
T90_error 2.073 s
T90_start 2:20:23.842 UTC
fluence 8.85e-05 erg/cm²
fluence_error 1.86e-07 erg/cm²
flux_1024 2.19e+01 erg/cm²/s
flux_1024_error 2.41e-01 erg/cm²/s
flux_1024_time 2.33e+01 erg/cm²/s
flux_64 2.82e+01 erg/cm²/s
flux_64_error 1.05e+00 erg/cm²/s
IPN table
GRB_name GRB100414A
ra 183.6167°
decl 20.4500°
pos_error 1.83e-01°
redshift 1.3680
Fermi LAT table
GRB_name_Fermi GRB100414097
GRB_name GRB100414A
MET 292904423.0
datum 2010-04-14
t_trigger 2:20:21 UTC
ra 192.1248°
decl 8.6930°
pos_error 1.39e-04°
GCN 10594 table
GRB_name GRB100414A
GCN_number 10594
Detection_method Fermi LAT Det
t_trigger 2:20:21 UTC
ra 191.5900°
decl 8.5700°
Circular_text TITLE: GCN CIRCULAR NUMBER: 10594 SUBJECT: GRB100414A: Fermi LAT detection DATE: 10/04/14 22:23:42 GMT FROM: Nicola Omodei at INFN(Pisa)/GLAST Hiromitsu Takahashi (Hiroshima Univ.), Masanori Ohno (ISAS/JAXA), Nicola Omodei (Stanford Univ.) report on behalf of the Fermi Large Area Telescope collaboration At 02:20:21 UT on 14th April 2010, the Fermi Large Area Telescope (LAT) detected gamma rays from the long GRB 100414A, which was triggered and located by the Fermi Gamma-ray Burst Monitor (GBM) (trigger 292904423/100414.097). At the time of the trigger the GRB was approximately at 70 degrees with respect to the LAT boresight which is close the edge of the LAT field of view. The GBM trigger caused an Autonomous Repoint Request, and the spacecraft moved to point at the GBM location. The data from the Fermi LAT show significantly detected emission from a transient point source as late as 300 seconds after the GBM trigger. The best LAT on-ground localization is found to be RA,Dec= 191.59, 8.57; (12:46:21.60, 08:34:12.0, J2000) with a 90% containment radius of 0.18 deg (statistical; 68% containment radius: 0.14 deg, preliminary systematic error is less than 0.1 deg). More than 20 photons above 100 MeV are observed within 300 seconds, and the highest energy photon coincident with the GRB position is a 4 GeV event which is observed 40 seconds after the GBM trigger. Further analysis is ongoing. The point of contact for this burst is Hiromitsu Takahashi (hirotaka@hep01.hepl.hiroshima-u.ac.jp) 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.
GCN 10595 table
GRB_name GRB100414A
GCN_number 10595
Detection_method Fermi GBM Det
t_trigger 2:20:21.990 UTC
ra 184.5100°
decl 9.6500°
Circular_text TITLE: GCN CIRCULAR NUMBER: 10595 SUBJECT: GRB 100414A: Fermi GBM detection DATE: 10/04/14 23:06:12 GMT FROM: Suzanne Foley at MPE S. Foley (MPE) reports on behalf of the Fermi GBM Team: "At 02:20:21.99 UT on 14 April 2010, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 100414A (trigger 292904423 / 100414097). The Fermi Observatory executed a maneuver following this trigger and tracked the burst location for the next 5 hours, subject to Earth-angle constraints. The on-ground calculated location, using the GBM trigger data, is RA = 184.51, DEC = 9.65 (J2000 degrees, equivalent to 12 h 18 m, 09 d 39 '), with an uncertainty of 1.0 degree (radius, 1-sigma containment, statistical only; there is additionally a systematic error which is currently estimated to be 2 to 3 degrees). The angle from the Fermi LAT boresight is 65 degrees. The GBM light curve consists of one main pulse with a duration (T90) of about 26.4 (+/-1.6) s (50-300 keV). The time-averaged spectrum from T0+2.3 s to T0+28.9 s is well fit by a power law function with an exponential high energy cutoff. The power law index is -0.58 (+/- 0.01) and the cutoff energy, parameterized as Epeak, is 627.6 (+12.5/-12.1) keV (CSTAT 1075.2 for 480 d.o.f.). The event fluence (8-1000 keV) in this time interval is (1.29 +/- 0.02)E-4 erg/cm^2. The 1-sec peak photon flux measured starting from T0+22.8 s in the 8-1000 keV band is 18.22 +/- 0.24 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 10598 table
GRB_name GRB100414A
GCN_number 10598
Detection_method correction
Circular_text TITLE: GCN CIRCULAR NUMBER: 10598 SUBJECT: Konus-Wind observation of GRB 100414A (correction to GCN 10597) DATE: 10/04/15 13:26:42 GMT FROM: Dmitry Frederiks at Ioffe Institute D. Frederiks, on behalf of Konus-Wind team, report: The correct designation of the burst reported in the GCN 10597 is GRB 100414A (not GRB 100414B).
GCN 10599 table
GRB_name GRB100414A
GCN_number 10599
Detection_method IPN Triangulation
Circular_text TITLE: GCN CIRCULAR NUMBER: 10599 SUBJECT: GRB 100414A: IPN Localization DATE: 10/04/15 22:05:36 GMT FROM: Valerie Connaughton at MSFC 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, K. Yamaoka, M. Ohno, Y. Fukazawa, T. Takahashi, M. Tashiro, Y. Terada, T. Murakami, K. Makishima, and Y. Hanabata on behalf of the Suzaku-WAM team, V. Connaughton, M.S. Briggs and C.A. Meegan on behalf of the Fermi GBM team, and K. Hurley report: The long GRB 100414A, seen by Fermi/LAT (Takahashi et al., GCN 10594) Fermi/GBM (Foley, GCN 10595), and Konus-Wind (Golenetskii et al., GCN 10597) was also detected by Suzaku WAM so far. Triangulation gives a Konus-WAM annulus centered at RA(2000)=223.490 (14h 53m 58s) Dec(2000)=-18.645 (-18d 38' 42"), whose radius is 41.329 0.588 deg (3 sigma); and a Konus-GBM annulus centered at RA(2000)=223.527 (14h 54m 06s) Dec(2000)=-18.436 (-18d 26' 09"), whose radius is 41.123 0.262 deg (3 sigma). These annuli are parallel and cannot be used to define a small error box. The Konus-GBM annulus is entirely contained within the the Konus-WAM annulus in the region around the Fermi/LAT localization. The center of the LAT position (RA,Dec,Err = 191.59, 8.57, 0.18 deg) is 0.377 deg from the center line of the annulus. A figure of the triangulated localization can be seen at: http://gammaray.nsstc.nasa.gov/gbm/science/ipn_plots/GRB100414A_IPN.png This localization may be refined with the arrival of data from more distant spacecraft. Swift is following up this localization using information from the IPN triangulation and further processing from the Fermi LAT team.
GCN 10601 table
GRB_name GRB100414A
GCN_number 10601
Detection_method Swift-XRT Other
ra 192.1120°
decl 8.6917°
Circular_text TITLE: GCN CIRCULAR NUMBER: 10601 SUBJECT: GRB 100414A: Swift-XRT detection of a possible X-ray afterglow DATE: 10/04/16 20:02:44 GMT FROM: Kim Page at U.of Leicester K.L. Page (U. Leicester), J. L. Racusin (NASA/GSFC), J.A. Kennea (PSU) and J.K. Cannizzo (NASA/UMBC) report on behalf of the Swift-XRT team: Following a Target of Opportunity request, Swift started observing the field of the Fermi GBM- and LAT-detected GRB 100414A about 48 hours after the trigger (GCN Circs. 10594, 10595). In 1.4 ks of data there is an uncatalogued source detected within the XRT field of view, at a position of RA, Dec = 192.11199, 8.69172, which is equivalent to RA (J2000): 12 48 26.88 Dec (J2000): +08 41 30.2 with an uncertainty of 3.8 arcsec (radius, 90% containment). The source is at a count rate of 0.022 +/- 0.004 count s^-1 (0.3-10 keV), corresponding to an observed flux of ~1.31x10^-12 erg cm^-2 s^-1; however, with the limited data collected so far, it is not possible to determine whether this source is fading.
GCN 10603 table
GRB_name GRB100414A
GCN_number 10603
Detection_method Fermi LAT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 10603 SUBJECT: GRB 100414A: Palomar Transient Factory Observations DATE: 10/04/16 22:06:46 GMT FROM: S. Bradley Cenko at Caltech S. B. Cenko (UC Berkeley), A. Rau (MPE Garching), E. O. Ofek (Caltech), P. E. Nugent (LBNL), J. Greiner (MPE Garching), and S. R. Kulkarni (Caltech) report on behalf of a larger collaboration: We have imaged the Fermi-LAT localization of GRB 100414A (Takahashi et al., GCN 10594; Foley, GCN 10595) with the automated Palomar 48 inch Schmidt telescope as part of the Palomar Transient Factory (PTF; Law et al, PASP, 1395; Rau et al, PASP 121, 1334) survey. A 60 s R-band image was obtained beginning at 7:53 UT on 15 April 2010 (~ 29.5 hours after the burst trigger), followed approximately an hour later by another 60 s image of the identical field. Digital subtraction with respect to a stacked pre-explosion P48 reference image reveals no afterglow candidate to a limiting magnitude of R > 21.0 mag within the 90% LAT localization region (Takahashi et al., GCN 10594). We note, however, that our imaging does not cover the location of the potential XRT afterglow candidate identified by Page et al. (GCN 10601).
GCN 10605 table
GRB_name GRB100414A
GCN_number 10605
Detection_method Swift-XRT Det
ra 192.1127°
decl 8.6931°
Circular_text TITLE: GCN CIRCULAR NUMBER: 10605 SUBJECT: GRB 100414A: Enhanced Swift-XRT position of candidate afterglow DATE: 10/04/17 07:37:24 GMT FROM: Kim Page at U.of Leicester K.L. Page, P.A. Evans and M.R. Goad (U. Leicester) report on behalf of the Swift-XRT team: Using 3686 s of XRT Photon Counting mode data and 3 UVOT images, 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 = 192.11266, 8.69309 which is equivalent to: RA (J2000): 12 48 27.04 Dec (J2000): +08 41 35.1 with an uncertainty of 2.0 arcsec (radius, 90% confidence). This position may be improved as more data are received. Position enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). Please note that we still cannot confirm that this source is fading. This circular is an official product of the Swift-XRT team.
GCN 10606 table
GRB_name GRB100414A
GCN_number 10606
Detection_method Fermi LAT Other
ra 192.1248°
decl 8.6930°
redshift 1.3680
Circular_text TITLE: GCN CIRCULAR NUMBER: 10606 SUBJECT: GRB 100414A: Gemini-N candidate and redshift DATE: 10/04/17 08:16:49 GMT FROM: Antonino Cucchiara at PSU A. Cucchiara and D. B. Fox (PSU) report on behalf of a larger collaboration: "Starting on 2010 April 17.26 UT we used the GMOS spectrograph on the Gemini North 8-m telescope to observe the field of the Fermi-LAT GRB 100414A (Takahashi et al. GCN 10594). In our 5 min i'-band observation we detected a bright source inside the refined XRT error circle (Page et al., GCN 10605) at the following coordinate: RA: 12:48:29.96 Dec: +8:41:34.91 with 0.5" uncertainty in both directions. Using two USNO-B1 stars we obtain i' = 20.37 +- 0.03 mag for this object. A sequence of 2x1200s spectra were also obtained with the same instrument, covering a spectral range of 4000-8000A. A series of metal absorption features were identified (FeII2374, FeII2383,FeII2587,MnII2594, FeII2600, MgII2796,2803,MgI2853) at the common redshift of z= 1.368. We therefore suggest this as the redshift of GRB 100414A. Further observations are planned. We thank the Gemini staff for performing this observation, in particular A. Fritz."
GCN 10607 table
GRB_name GRB100414A
GCN_number 10607
Detection_method GROND
ra 192.1122°
decl 8.6929°
Circular_text TITLE: GCN CIRCULAR NUMBER: 10607 SUBJECT: GRB 100414A: GROND Detection of the Optical Afterglow DATE: 10/04/17 09:53:25 GMT FROM: Thomas Kruehler at MPE/MPI Robert Filgas, Thomas Kruehler and Jochen Greiner (all MPE Garching) report on behalf of the GROND team: We observed the field of GRB 100414A (Fermi GBM/LAT trigger 292904423/100414.097; Takahashi et al., GCN #10594, Foley, GCN #10595) 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 03:11 UT on April 17, 73 hours after the GRB trigger, and were performed through thick cloud coverage. We detect the optical afterglow reported by Cucchiara & Fox (GCN #10606) in the optical bands. To reiterate the position, we measure RA (J2000) = 12 h 48 m 26.93 s DEC (J2000) = +08d 41' 34.4" with an uncertainty of 0.5" in each coordinate against SDSS astrometry and inside the enhanced XRT error circle reported by Page et al. (GCN #10605). Based on 4 min of total exposure, we estimate preliminary magnitudes (all in AB system) of g' = 21.3 +- 0.1 mag, r' = 20.9 +- 0.1 mag Given magnitudes are calibrated against SDSS field stars and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.03 mag in the direction of the burst (Schlegel et al. 1998).
GCN 10608 table
GRB_name GRB100414A
GCN_number 10608
Detection_method correction
ra 192.1123°
decl 8.6930°
Circular_text TITLE: GCN CIRCULAR NUMBER: 10608 SUBJECT: GRB 100414A: Gemini-N observation (correction) DATE: 10/04/17 14:40:20 GMT FROM: Antonino Cucchiara at PSU A. Cucchiara (PSU) reports on behalf of a larger collaboration: "We noted a typo in the coordinate reported in GCN 10606. The correct position of the GRB 100414A optical transient in our Gemini-N image is: RA: 12:48:26.96 Dec: +08:41:34.91 We thank W. Landsman for pointing this out to us and we apologize for any confusion this may have caused."
GCN 10609 table
GRB_name GRB100414A
GCN_number 10609
Detection_method Swift-UVOT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 10609 SUBJECT: GRB 100414A: Swift/UVOT Observations DATE: 10/04/17 15:56:44 GMT FROM: Wayne Landsman at GSFC/SSAI W. Landsman (GSFC) and J. Cannizzo (GSFC) report on behalf of the Swift/UVOT team: The Swift/UVOT began observations of the field of GRB 100414A 40.4 hours after the Fermi LAT and GBM-detected trigger (Takahashi et al. GCN Circ. 10594, Foley et al., GCN Circ. 10595). We detect the source reported by Cucchiara & Fox (GCN Circ. 10606, 10608) and Filgas et al. (GCN Circ. 10607) Combining our white observations into exposures beginning at 40.4 and 53.2 hours, we find evidence for source fading. Filter T_start (hr) Exp(s) Mag Err White 40.38 765 20.54 +/- 0.10 White 53.20 3531 20.86 +/- 0.06 These observations are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.03 mag in the direction of the burst (Schlegel et al. 1998). The photometry is on the UVOT photometric system described in Poole et al.(2008, MNRAS, 383,627).
GCN 10610 table
GRB_name GRB100414A
GCN_number 10610
Detection_method Suzaku WAM Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 10610 SUBJECT: GRB 100414A: Suzaku WAM observation of the prompt emission DATE: 10/04/17 19:42:41 GMT FROM: Kazutaka Yamaoka at Aoyama Gakuin U T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.), K. Yamaoka (Aoyama Gakuin U.), S. Sugita (Nagoya U), Y. Terada, M. Tashiro, S. Hong, A. Endo, K. Onda, T. Sugasahara, W. Iwakiri (Saitama U.), M. Ohno, M. Kokubun, T. Takahashi (ISAS/JAXA), Y. E. Nakagawa, M. Suzuki, T. Tamagawa (RIKEN), N. Ohmori, A. Daikyuji, E. Sonoda, K. Kono, H. Hayashi, K. Noda, Y. Nishioka, M. Yamauchi (Univ. of Miyazaki), N. Vasquez (Tokyo Tech.), Y. Urata, H. M. Lin, P. Tsai (NCU), T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo), on behalf of the Suzaku WAM team, report: The bright long, Fermi-LAT GRB 100414A (Takahashi et al., GCN 10594; Fermi/GBM trigger #292904423 / 100414097; Foley, GCN 10595) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 02:20:22.879 UT (=T0). The observed light curve shows a multi-peaked structure starting at T0-1.5 s, ending at T0+24.5 s with a duration (T90) of about 22 seconds. The fluence in 100 - 1000 keV was 4.88(-0.36, +0.13)x10-5 erg/cm^2. The 1-s peak flux measured from T0+22.5 s was 6.13(-0.79, +0.40) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-1.5 s to T0+24.5 s is well fitted by a GRB Band model as follows. the low-energy photon index alpha: -0.56(-0.29, +0.37), the high-energy photon index beta: -3.05(-0.53, +0.30), and the peak energy Epeak: 612(-53, +55) keV (chi^2/d.o.f = 34/23). Due to the brightness of this burst, a 3% systematic error was added for low energy channels. In addition, there might be some calibration uncertainties in these spectral parameters because GRB photons came to the WAM detector by passing through the large Ne dewar of the X-ray micro-calorimeter (XRS). All the errors are quoted at 90% confidence level. The light curves for this burst are available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html
GCN 10618 table
GRB_name GRB100414A
GCN_number 10618
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 10618 SUBJECT: GRB100414A: SAO RAS optical observations DATE: 10/04/19 07:34:18 GMT FROM: Vladimir Sokolov at SAO RAS A. Moskvitin, T. Fatkhullin, V. Sokolov (SAO RAS Niznijh Arkhyz, Russia), on behalf of a larger colaboration, report: We observed an OT (Cucchiara & Fox, GCN Circ. 10606, 10608; Filgas, Kruehler & Greiner, GCN Circ. 10607; Landsman & Cannizzo, GCN Circ. 10609) of GRB 100414A with the Zeiss-1000 telescope of SAO RAS, Russia. Observations started 87.31 hours after the Fermi LAT and GBM triggers (Takahashi et al., GCN Circ. 10594; Foley, GCN Circ. 10595). We obtained 12 x 300 sec images both in Rc and V bands with the airmass 1.2-1.7 under good weather conditions. Calibration was carried out with 8 SDSS nearby stars, whose magnitudes were transformed according to formulae from http://www.sdss.org/dr5/algorithms/sdssUBVRITransform.html (Lupon 2005). Rc = 21.40 +/- 0.09 (17:39:01 -- 19:05:27 UT, mean epoch = April, 17.765), V = 21.75 +/- 0.08 (19:08:49 -- 20:31:05 UT, mean epoch = April, 17.826). These magnitudes are not corrected for the expected Galactic extinction reported in Landsman & Cannizzo, GCN Circ. 10609. This message may be cited.
GCN 10632 table
GRB_name GRB100414A
GCN_number 10632
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 10632 SUBJECT: GRB 100414A: Confirmation of the X-ray afterglow DATE: 10/04/20 10:06:01 GMT FROM: Kim Page at U.of Leicester K.L. Page (U. Leicester) and J.K. Cannizzo (NASA/UMBC) report on behalf of the Swift-XRT team: A second Swift-XRT observation of the Fermi-detected GRB 100414A (GCN Circs 10594 and 10595) was performed on 2001-04-19, 5.7 days after the trigger. The source reported by Page et al. (GCN Circs 10601, 10605) is no longer detected, with a 3-sigma upper limit on the count rate of 4.5x10^-3 count s^-1 (corresponding to an observed flux of 2.5x10^-13 erg cm^-2 s^-1). This non-detection sets a lower limit on the decay slope of alpha > 1.5. With this fading, we can confirm that this source is the X-ray afterglow of GRB 100414A. This circular is an official product of the Swift-XRT team.
GCN 10641 table
GRB_name GRB100414A
GCN_number 10641
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 10641 SUBJECT: GRB 100414A: CFHT optical observations DATE: 10/04/21 10:17:20 GMT FROM: Yuji Urata at Nat. Central U. Y. Urata (NCU) and K.Y Huang (ASIAA) on behalf of EAFON report; "We observed the location of the GRB100414A optical afterglow (Cucchiara et al. 10608) with CFHT on the night of April 19 (5.2 day after the trigger) and 20 (6.2 day). The g', r' and i' band images show the afterglow clearly. We estimate preliminary magnitudes of r'=22.46+/-0.05 (5.19 day) and r'=22.84+/-0.05 (6.17 day) against the SDSS field stars. Combined with the photometric results reported by Filgas et al (10607) and Cucchiara (10606), the optical afterglow light curves are well described by a simple power law decay with the temporal index about 2.5."
GCN 10649 table
GRB_name GRB100414A
GCN_number 10649
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 10649 SUBJECT: GRB 100414A: Radio Afterglow Detection with the Expanded VLA DATE: 10/04/22 17:44:55 GMT FROM: Poonam Chandra at Royal Mil. College Canada Poonam Chandra (RMC), Dale A. Frail (NRAO), S. Bradley Cenko (Berkeley) and Fiona Harrison (Caltech) report on behalf of a larger collaboration: We used the Expanded Very Large Array (EVLA) to observe the Fermi burst GRB 100414A (Takahashi et al, GCN 10594 Foley GCN 10595) on 2010 Apr 19 UT Within the revised XRT error circle (Goad et al GCN 10605). We detect the GRB afterglow with a flux density of 406 +/- 22 uJy. The EVLA is undergoing active commissioning and as such these results should be considered preliminary=2E 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. [GCN OPS NOTE(22apr10): Per author's request, the "13A" in the Subject line was changed to "14A".]
GCN 10697 table
GRB_name GRB100414A
GCN_number 10697
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 10697 SUBJECT: GRB 100414A : WSRT Radio Detection DATE: 10/04/28 14:58:30 GMT FROM: Atish Kamble at U. of Amsterdam A.P. Kamble (U of Amsterdam), A.J. van der Horst (NASA/MSFC/ORAU), R.A.M.J. Wijers, E. Rol (U of Amsterdam), C. Kouveliotou (NASA/MSFC) and K. Wiersema (U of Leicester) report on behalf of a larger collaboration : "We observed the field of Fermi GBM/LAT burst GRB 100414A (GCN 10594, 10595, 10649) using the Westerbork Synthesis Radio Telescope at 4.8 GHz from April 27, 16.0 UT to April 28, 04.0 UT, i.e. 13.57 to 14.1 days after the burst. We detect the radio afterglow with flux density of 420 +/- 38 microJy at the position of the optical afterglow detected by GROND (GCN 10607). We would like to thank the WSRT staff for rapidly scheduling and obtaining these observations."
GCN 10698 table
GRB_name GRB100414A
GCN_number 10698
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 10698 SUBJECT: GRB 100414A : EVLA Radio Detection DATE: 10/04/28 16:10:57 GMT FROM: Dale A. Frail at NRAO Dale A. Frail (NRAO), Poonam Chandra (RMC), S. Bradley Cenko (Berkeley) and Fiona Harrison (Caltech) report on behalf of a larger collaboration: "We used the Expanded Very Large Array (EVLA) to observe the field of view towards the Fermi GBM/LAT burst GRB 100414A (GCN 10594, 10595, 10649) on April 27.18 UT at a center frequency of 8.46 GHz. We detect the radio afterglow with flux density of 397 15 microJy at the position of the optical afterglow detected by GROND (GCN 10607). Further observations are planned. The EVLA is still undergoing active commissioning and we caution that these results should be considered preliminary. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc."