GRB090618A

This page lists all entries on GRB090618A in GRBweb

Summary Fermi GBM IPN Swift GCN 9512 GCN 9513 GCN 9514 GCN 9515 GCN 9517 GCN 9518 GCN 9519 GCN 9520 GCN 9521 GCN 9522 GCN 9524 GCN 9526 GCN 9527 GCN 9528 GCN 9529 GCN 9530 GCN 9531 GCN 9532 GCN 9533 GCN 9534 GCN 9535 GCN 9536 GCN 9537 GCN 9538 GCN 9539 GCN 9541 GCN 9542 GCN 9548 GCN 9553 GCN 9563 GCN 9568 GCN 9570 GCN 9575 GCN 9576 GCN 9592 GCN 9597 GCN 9613 GCN 9665

Summary table
Variable Value Source
GRB_name_Fermi GRB090618353
T0 8:28:24.974 UTC GCN_circulars,Konus-Wind Det
ra 293.9945° Swift
decl 78.3568° Swift
pos_error 9.58e-05° Swift
T90 112.386 s Fermi_GBM
T90_error 1.086 s Fermi_GBM
T90_start 8:28:34.595 UTC Fermi_GBM
fluence 2.68e-04 erg/cm² Fermi_GBM
fluence_error 4.29e-07 erg/cm² Fermi_GBM
redshift 0.5400
T100 122.007 s
GBM_located False
mjd 55000.353066828706 GCN_circulars,Konus-Wind Det
Fermi GBM table
GRB_name_Fermi GRB090618353
trigger_name bn090618353
ra 293.9900°
decl 78.3575°
pos_error 2.53e+00°
datum 2009-06-18
t_trigger 8:28:26.659 UTC
T90 112.386 s
T90_error 1.086 s
T90_start 8:28:34.595 UTC
fluence 2.68e-04 erg/cm²
fluence_error 4.29e-07 erg/cm²
flux_1024 6.87e+01 erg/cm²/s
flux_1024_error 1.14e+00 erg/cm²/s
flux_1024_time 6.34e+01 erg/cm²/s
flux_64 7.62e+01 erg/cm²/s
flux_64_error 4.75e+00 erg/cm²/s
IPN table
GRB_name GRB090618A
ra 294.0208°
decl 78.3500°
pos_error 5.00e-02°
redshift 0.5400
Swift table
GRB_name GRB090618A
t_trigger 8:28:29 UTC
ra 293.9945°
decl 78.3568°
pos_error 9.58e-05°
T90 113.2 s
fluence 1.05e-04 erg/cm²
redshift 0.5400
GCN 9512 table
GRB_name GRB090618A
GCN_number 9512
Detection_method Swift Det
t_trigger 8:28:29 UTC
ra 294.0210°
decl 78.3530°
Circular_text TITLE: GCN CIRCULAR NUMBER: 9512 SUBJECT: GRB 090618: Swift detection of a bright burst with optical afterglow DATE: 09/06/18 08:48:39 GMT FROM: Jamie A. Kennea at PSU/Swift-XRT P. Schady (MSSL-UCL), W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester), S. Campana (INAF-OAB), P.A. Curran (MSSL-UCL), C. Guidorzi (U Ferrara), J. A. Kennea (PSU), J. Mao (INAF-OAB), R. Margutti (Univ Bicocca&OAB), J. P. Osborne (U Leicester), K. L. Page (U Leicester), P. Romano (INAF-IASFPA), M. H. Siegel (PSU), G. Stratta (ASDC) and T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team: At 08:28:29 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 090618 (trigger=355083). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 294.021, +78.353 which is RA(J2000) = 19h 36m 05s Dec(J2000) = +78d 21' 13" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed multi peak structure with a duration of about 130 sec. The peak count rate was ~40,000 counts/sec (15-350 keV), at 80 sec after the trigger. The XRT began observing the field at 08:30:30.8 UT, 120.9 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 293.9897, +78.3576 which is equivalent to: RA(J2000) = 19h 35m 57.52s Dec(J2000) = +78d 21' 27.3" with an uncertainty of 4.7 arcseconds (radius, 90% containment). This location is 28 arcseconds from the BAT onboard position, within the BAT error circle. No event data are yet available to determine the column density using X-ray spectroscopy. UVOT took a finding chart exposure of 150 seconds with the White filter starting 128 seconds after the BAT trigger. There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at RA(J2000) = 19:35:58.69 = 293.99456 DEC(J2000) = +78:21:24.3 = 78.35676 with a 90%-confidence error radius of about 0.74 arc sec. This position is 4.6 arc sec. from the center of the XRT error circle. The estimated magnitude is 14.36 with a 1-sigma error of about 0.01. No correction has been made for the expected extinction corresponding to E(B-V) of 0.09. Burst Advocate for this burst is P. Schady (ps AT mssl.ucl.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 9513 table
GRB_name GRB090618A
GCN_number 9513
Detection_method Optical
ra 293.9945°
decl 78.3568°
Circular_text TITLE: GCN CIRCULAR NUMBER: 9513 SUBJECT: GRB090618: P60 Optical Afterglow DATE: 09/06/18 08:49:37 GMT FROM: S. Bradley Cenko at Caltech S. B. Cenko (UC Berkeley) reports on behalf of a larger collaboration: We have imaged the field of GRB090618 (Swift trigger 355083) with the automated Palomar 60-inch telescope beginning at 08:30 UT on 18 June 2009 (approximately 2 minutes after the burst). At the edge of the XRT error circle we detect a bright point source with coordinates: RA: 19:35:58.68 Dec: +78:21:24.4 (J2000) Using several SDSS stars in the field as reference, we estimate an initial magnitude of r' ~ 13.8. Given the brightness of the source, we consider it highly likely to be the optical afterglow of GRB090618. Further observations are ongoing.
GCN 9514 table
GRB_name GRB090618A
GCN_number 9514
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 9514 SUBJECT: GRB 090618: KAIT optical afterglow DATE: 09/06/18 08:52:20 GMT FROM: Daniel Perley at U.C. Berkeley D. A. Perley reports on behalf of the KAIT GRB team: The Katzman Automatic Imaging Telescope (KAIT) responded to GRB 090618 and began taking data at 08:31:10 (UT). A bright (~14th magnitude) optical afterglow is visible in the initial set of exposures at the following position: RA 19:35:58.80 dec +78:21:25.5 Further follow-up is in progress.
GCN 9515 table
GRB_name GRB090618A
GCN_number 9515
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 9515 SUBJECT: GRB 090618: ROTSE-III Detection of Optical Counterpart DATE: 09/06/18 08:57:11 GMT FROM: Wiphu Rujopakarn at U AZ/Steward W. Rujopakarn (Steward), T. Guver (U Arizona), S. B. Pandey (Michigan), and F. Yuan (Michigan) report on behalf of the ROTSE collaboration: ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB 090618 (Swift trigger 355083, Schady et al., GCN 9512). The first image was at 08:28:53.7 UT, 23.9 s after the burst (6.7 s after the GCN notice time). The unfiltered images are calibrated relative to USNO A2.0. We detect a 14.1 magnitude source with coordinates: 19:35:58.65 +78:21:24.03 (J2000), with positional uncertainty of 1" or better start UT mag mlim(of image) ---------------------------------- 08:28:29.8 14.1 16.2 This source is not visible in DSS (second epoch), 2MASS or the MPChecker database. Continuing observations are in progress.
GCN 9517 table
GRB_name GRB090618A
GCN_number 9517
Detection_method KAIT
Circular_text TITLE: GCN CIRCULAR NUMBER: 9517 SUBJECT: GRB 090618: OA behavior from KAIT DATE: 09/06/18 11:21:26 GMT FROM: Weidong Li at UC Berkeley KAIT/LOSS W. Li, D. A. Perley, and A. V. Filippenko, University of California at Berkeley, on behalf of the KAIT GRB team: We have analyzed the KAIT observations on GRB 090618 (GCN 9512) as reported in GCN 9514. Our first 2s unfiltered observation started at 08:29:44 UT, 75 s after the BAT trigger. The OA as reported in GCN 9512, 9513, 9514, and 9515 is clearly detected. Subsequent observations show that the OA declined and reached a bottom at t=92 s, then brightened and reached a peak at t=120 s. After the peak, the OA declined as a smooth power-law, with an obvous change of decay index at t ~ 600 s (from alpha = -1.08 +/- 0.05 to -0.70 +/- 0.02). Selected photometry, all unfiltered calibrated to the R band via USNO B1: t_mid(seconds) exp(s) mag mag_err --------------------------------------- 76 2.0 13.61 0.03 92 2.0 13.99 0.04 117 2.0 13.50 0.03 237 20.0 14.02 0.02 436 20.0 14.73 0.02 729 20.0 15.26 0.02 2601 20.0 16.22 0.02 7329 120.0 17.02 0.03
GCN 9518 table
GRB_name GRB090618A
GCN_number 9518
Detection_method Other
redshift 0.5400
Circular_text TITLE: GCN CIRCULAR NUMBER: 9518 SUBJECT: GRB 090618: Lick/KAST Spectroscopy DATE: 09/06/18 12:37:12 GMT FROM: S. Bradley Cenko at Caltech S. B. Cenko, D. A. Perley (UC Berkeley), V. Junkkarinen, M. Burbidge (UC San Diego), and K. Miller (UCO Lick Observatory) report on behalf of a larger collaboration: We have obtained a spectrum of the afterglow (GCNs 9512, 9513, 9514, 9515) of GRB 090618 with the KAST spectrograph on the 3-m Shane telescope at Lick Observatory. Observations began at 08:48 UT on 18 June 2009, approximately 20 minutes after the burst. On the blue channel (using the 830/3460 grism, providing wavelength coverage from 3200 - 4400 A), we detect a number of strong absorption features that we identify as Mg II, Mg I, and Fe II at a common redshift of z = 0.54. We believe this likely to be the redshift of the GRB, as the lack of Lyman-alpha absorption limits the GRB host to lie at z <~ 1.6. Further analysis is in progress.
GCN 9519 table
GRB_name GRB090618A
GCN_number 9519
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 9519 SUBJECT: Optical observations of GRB 090618 DATE: 09/06/18 12:37:13 GMT FROM: Alberto Carraminana at AzTEC A. Carraminana (INAOE), C. Alvarez Ochoa (UNACh) and G. Miramon (OAGH-INAOE) report: We clearly detected the optical counterpart of GRB 090618 (GCN 9512) with the 2.1m telescope of the Observatorio Astrofisico Guillermo Haro at Cananea, Sonora, Mexico. Observations started at 08:43 UT, 14 minutes after the BAT trigger and continued until dawn. Observations were made under non photometric conditions. We measured a lineal faddening of the burst compared to a reference star of amplitude 0.5 magnitudes between t=870s to 1600s. A non calibrated graph is available at http://www.inaoep.mx/~alberto/gamma/grb090618_lc.jpg Spectroscopic data were also obtained and are under analysis.
GCN 9520 table
GRB_name GRB090618A
GCN_number 9520
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 9520 SUBJECT: GRB 090618 Faulkes Telescope North observations DATE: 09/06/18 13:32:21 GMT FROM: David Bersier at Liverpool John Moores U A.Melandri (Liverpool JMU), C. Guidorzi (U. Ferrara), D. Bersier, Z. Cano, I.A. Steele, C.G. Mundell (Liverpool JMU), P. O'Brien, N. Tanvir (U. Leicester) on behalf of a larger collaboration report: We have been monitoring the field of GRB090618 (Swift trigger 355083), with the Faulkes Telescope North (Hawaii), starting ~80 minutes after the trigger time (Schady et al. GCN 9512). Observations were performed with BVRi filters. The optical afterglow reported by Cenko (GCN 9513), Perley (GCN 9514) and Rujopakarn et al. (GCN 9515) is clearly visible and detected in all filters. We find a magnitude of R=17.01 0.03 (at 2.5 hrs after the burst) and R=17.25 0.05 (at 3.1 hrs). We confirm the decay of alpha~0.7 reported by Li et al. (GCN 9517). Observations are continuing.
GCN 9521 table
GRB_name GRB090618A
GCN_number 9521
Detection_method Swift-XRT Det
ra 293.9930°
decl 78.3570°
Circular_text TITLE: GCN CIRCULAR NUMBER: 9521 SUBJECT: GRB 090618: Enhanced Swift-XRT position DATE: 09/06/18 15:00:51 GMT FROM: Phil Evans at U of Leicester P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) report on behalf of the Swift-XRT team. Using 2422 s of XRT Photon Counting mode data and 5 UVOT images for GRB 090618, 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 = 293.99304, +78.35702 which is equivalent to: RA (J2000): 19h 35m 58.33s Dec (J2000): +78d 21' 25.3" with an uncertainty of 1.7 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, arXiv:0812.3662). This circular was automatically generated, and is an official product of the Swift-XRT team.
GCN 9522 table
GRB_name GRB090618A
GCN_number 9522
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 9522 SUBJECT: GRB 090618: LOAO R-band Observation DATE: 09/06/18 15:01:20 GMT FROM: Myungshin Im at Seoul Nat U M. Im, W.K. Park (CEOU/Seoul National Univ) and Y. Urata (NCU) on behalf of EAFON team. We observed GRB090618 (Schady et al. GCN 9512) in R using the 1.0m telescope at Mt. Lemmon (Arizona, US) operated by the Korea Astronomy Space Science Institute. The observation started about 50min after the BAT trigger. The first image taken with the mid-point at June 18, 09:52 UT (53m42s after the BAT trigger) shows a clear detection of the afterglow at R=15.9 +- 0.1 mag, reported earlier by a number of groups (GCN 9513, 9514, 9515, 9520). The photometry was calibrated against R1mag of USNO-B1 stars in the vicinity of GRB. More data were taken, and they are being analyzed. We thank the LOAO operator, Y. Baek for her assistance of this observation.
GCN 9524 table
GRB_name GRB090618A
GCN_number 9524
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 9524 SUBJECT: GRB 090618: AGILE observations DATE: 09/06/18 15:21:44 GMT FROM: Marco Feroci at IASF/INAF F. Longo, E. Moretti, G. Barbiellini, E. Vallazza (INFN Trieste), M.Trifoglio, A. Bulgarelli, F. Gianotti F. Fuschino, M. Marisaldi, C.Labanti, M.Galli, G.DiCocco (INAF/IASF Bologna), S. Cutini, C. Pittori (ASDC), M.Tavani, E.Striani, G. Pucella, F. D'Ammando, V.Vittorini, A. Argan, A. Trois, G. Piano, S. Sabatini (INAF/IASF Rome), E. Del Monte, M. Feroci, Y. Evangelista, I. Donnarumma, L. Pacciani, P. Soffitta, E. Costa, F.Lazzarotto, I. Lapshov, M. Rapisarda (INAF/IASF Rome) A. Giuliani, A. Chen, S. Mereghetti, F. Perotti, P. Caraveo (INAF/IASF Milano), A. Pellizzoni, M. Pilia (INAF/OA Cagliari), S. Vercellone (INAF/IASF Palermo), P. Picozza, A. Morselli (INFN Roma-2), M. Prest (Universita' dell'Insubria), P. Lipari, D. Zanello (INFN Roma-1), A. Rappoldi, P. Cattaneo (INFN Pavia) and P. Giommi, P. Santolamazza, F. Verrecchia (ASDC) and L. Salotti (ASI), on behalf of the AGILE Team, report: The AGILE satellite detected GRB 090618 (P. Schady et al. GCN #9512) at about 36 degrees off axis. Super-AGILE, operating in the 18-60 keV energy range, triggered and localized the burst in the 1-D region of the field of view at a position consistent with the Swift/BAT localization. The emission from this bright GRB with a complex lightcurve was detected at high significance despite the large off-axis direction. AGILE-MCAL, operating in the 350 keV - 100 MeV energy range, triggered this GRB at 08:28:24.772 UT (T0). The MCAL overall burst duration is about 100 sec. The burst is composed by three main pulses, the brightest starting at T0+62sec and lasting about 14 seconds. The total MCAL spectrum between T0 and T0+120 sec can be fit by a simple powerlaw with photon index 3.16 (-0.30, +0.39) (90% c.l.), with reduced chi^2 0.99 (9 d.o.f.), in the 0.5-10 MeV energy range. The estimated fluence is (3.2 +/- 0.6) 10^{-5} erg cm^-2 in the same energy range. From a preliminary analysis of the AGILE-GRID data in the energy range 30 MeV-30 GeV no significant gamma-ray emission above 30 MeV is detected in the GRB error box during both the first and second main pulse for a total duration of about 130 sec. A preliminary upper limit is 0.1 ph cm^-2 over a 130 s duration. GRB 090618 provides a clear evidence for a class of GRBs bright below a few MeV, showing the lack of significant gamma-ray emission above 30 MeV.
GCN 9526 table
GRB_name GRB090618A
GCN_number 9526
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 9526 SUBJECT: GRB 090618: SDSS host detection DATE: 09/06/18 16:52:52 GMT FROM: Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst Daniele Malesani (DARK/NBI) reports: I inspected the SDSS images of the field of GRB 090618 (Schady et al., GCN 9512). A faint object is visible in the r and i frames at the position of the optical afterglow (e.g. Schady et al., GCN 9512; Cenko, GCN 9513), likely the host galaxy of the GRB. Nothing convincing is visible in the u, g, and z images. Compared to nearby SDSS stars, the magnitudes are r = 22.7 +- 0.3 and i = 22.2 +- 0.4. The bright host magnitude is consistent with the low redshift reported by Cenko et al. (GCN 9518) A supernova as bright as SN 1998bw (Galama et al. 1998, Nature, 395, 670) would peak at r(AB) ~ 23.6 at z=0.54.
GCN 9527 table
GRB_name GRB090618A
GCN_number 9527
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 9527 SUBJECT: GRB090618: Swift/UVOT bright afterglow detection DATE: 09/06/18 19:00:10 GMT FROM: Patricia Schady at MSSL/Swift P. Schady (MSSL-UCL) reports on behalf of the Swift UVOT team: The Swift/UVOT began settled observations of the field of GRB 090618 129s after the BAT trigger (Schady et al., GCN Circ. 9512) and a decaying source is detected in all UVOT filters at the position reported in Schady et al. (GCN Circ. 9512), consistent with refined XRT error circle (Evans et al., GCN Circ. 9521) as well as the optical afterglow position reported in a number of other GCNs (GCN Circ. 9512, 9514, 9515). The detection of the afterglow of GRB 090618 in all filters puts an upper limit on the redshift of z < 1.7, consistent with the redshift constraints reported by Cenko et al. (GCN Circ. 9518). The magnitudes for the first UVOT observation of GRB 090618 in each filter are as follows: Filter T_start(s) T_stop(s) Exp(s) Mag white 129 279 147 14.27+/-0.01 v 671 691 19 15.60+/-0.09 b 596 616 19 15.92+/-0.06 u 340 590 246 14.62+/-0.01 uvw1 720 740 19 15.09+/-0.08 uvm2 695 715 19 15.23+/-0.12 uvw2 647 667 19 15.27+/-0.10 The values quoted above are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.09 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 9528 table
GRB_name GRB090618A
GCN_number 9528
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 9528 SUBJECT: GRB090618: Swift-XRT team refined analysis DATE: 09/06/18 19:06:26 GMT FROM: Andy Beardmore at U Leicester A.P. Beardmore (U. Leicester) and P. Schady (MSSL-UCL) report on behalf of the Swift-XRT team: We have analysed 12.3 ks of Swift-XRT data for GRB 090618 (Schady et al. GCN Circ. 9512), from 124 s to 25.7 ks after the BAT trigger. The data span five orbits and comprise 2.3 ks in Windowed Timing (WT) mode and 10.0 ks in Photon Counting (PC) mode. The UVOT-enhanced XRT position for this burst was reported by Evans et al. (GCN 9521). The burst was initially very bright in X-rays, observed at a rate of ~8000 count s^-1, and decayed rapidly with a slope of ~6, before breaking at T+310 s to a shallower decay slope of 0.71 +/- 0.02. A further break is seen at T+4700 s with the decay steepening to 1.22 +/- 0.05. The WT spectrum from T+250 s to T+1065 s can be fit by an absorbed powerlaw with a photon index of 2.11 +/- 0.03 and intrinsic absorption of (1.78 +/- 0.14) x 10^21 cm^-2 (at z=0.54, Cenko et al., GCN 9518), in addition to the Galactic column of 5.8 x 10^20 cm^-2 in the direction of the source (Kalberla et al. 2005). The observed 0.3-10 keV flux for this model is (8.2 +0.2 -0.1) x 10^-10 erg cm^-2 s^-1. The corresponding unabsorbed flux is (1.16 +/- 0.02) x 10^-9 erg cm^-2 s^-1. If the light curve continues to decay at the same rate we predict a count rate of 0.13 count s^-1 at T+24 hours, which corresponds to an observed (unabsorbed) 0.3-10 keV flux of 4.9 x 10^-12 (7.2 x 10^-12) erg cm^-2 s^-1. The results of the XRT team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00355083. This circular is an official product of the Swift-XRT team.
GCN 9529 table
GRB_name GRB090618A
GCN_number 9529
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 9529 SUBJECT: GRB 090618: SARA observations DATE: 09/06/18 23:00:02 GMT FROM: Adria C. Updike at Clemson U Adria Updike, Sean Brittain, Dieter Hartmann (Clemson University), Andrew Colson, Renata Cumbee, Brianne Hackett, Josiah Lewis, and Marten Kronberg (SARA REU) report: We observed the field of GRB 090618 (Schady et al., GCN 9512) using the 0.9m SARA telescope at Kitt Peak National Observatory beginning 1.5 hours after the trigger and continuing for 2 hours. Our observations consisted of 45 sec exposures in the I and R bands. The afterglow was detected in every image. Magnitudes are given below as compared to the USNOB.1 catalog. Time is given in seconds after the trigger; exposure time in seconds. Time Filter Exp Mag ------------------------------------ 5400 I 45 16.2 +/- 0.05 6300 R 45 16.8 +/- 0.05 Further observations are planned. http://www.saraobservatory.org/
GCN 9530 table
GRB_name GRB090618A
GCN_number 9530
Detection_method Swift-BAT Det
ra 294.0080°
decl 78.3520°
Circular_text TITLE: GCN CIRCULAR NUMBER: 9530 SUBJECT: GRB 090618: Swift-BAT refined analysis DATE: 09/06/19 00:43:00 GMT FROM: Tilan Ukwatta at GSFC/GWU W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), P. Schady (MSSL-UCL), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team): Using the data set from T-5 to T+320 sec from the recent telemetry downlink, we report further analysis of BAT GRB 090618 (trigger #355083) (Schady, et al., GCN Circ. 9512). The BAT ground-calculated position is RA, Dec = 294.008, 78.352 deg, which is RA(J2000) = 19h 36m 01.8s Dec(J2000) = +78d 21' 07.1" with an uncertainty of 0.46 arcmin, (radius, sys+stat, 90% containment). The partial coding was 62.5%. The mask-weighted light curve shows two episodes with four prominent peaks. The first episode is a smooth 50 sec peak starting at T-5 sec, and ends at T+45 sec. The second episode is about 275 second long and consists of three overlapping peaks. The second episode starts at ~T+45 sec, the first peak is around T+62 sec, the second peak is around T+80, and the third is around T+112 and finally ends at T+320 sec. Our T90 (15-350 keV) is 113.2 +/- 0.6 sec (estimated error including systematics). The time-averaged spectrum from T-5 to T+109 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.712 +/- 0.018. The fluence in the 15-150 keV band is 1.06 +/- 0.01 x 10^-4 erg/cm2. The 1-sec peak photon flux measured from T+65.12 sec in the 15-150 keV band is 38.9 +/- 0.8 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/355083/BA/
GCN 9531 table
GRB_name GRB090618A
GCN_number 9531
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 9531 SUBJECT: GRB090618 - Continued optical monitoring and light curve break DATE: 09/06/19 08:56:19 GMT FROM: Zach Cano at ARI/John Moores Liverpool Z. Cano (Liverpool JMU), C. Guidorzi (U. Ferrara), D. Bersier, A. Melandri, I.A. Steele, R.J. Smith, C. Mundell (Liverpool JMU) report, on behalf of a large collaboration: Following our report of observations (GCN 9520) we continued monitoring the field of GRB090618 (Swift trigger 355083) on the Liverpool Telescope (La Palma) from 13.6 hours to 17.9 hours post burst in R and i bands. Below is a summary of a few R-band images: t_exp t-T0 R-mag 300s 13.6 hours 18.9 0.1 300s 15.6 hours 19.1 0.1 300s 17.9 hours 19.3 0.1 The calibration is still preliminary and determined against stars in the USNO catalog. We note a break in the R-band light curve, and find a decay index of alpha~1.4 by 17.9 hours post burst, as compared to alpha~0.7 previously reported (GCNs 9517, 9520).
GCN 9532 table
GRB_name GRB090618A
GCN_number 9532
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 9532 SUBJECT: GRB 090618 15GHz radio detection DATE: 09/06/19 09:50:32 GMT FROM: Guy Pooley at MRAO, Cambridge, UK Guy Pooley (Cavendish Astrophysics, U. Cambridge) reports on behalf of the AMI collaboration: The AMI Large Array (the rebuilt Ryle Telescope) was used to observe the field of GRB 090618 (Schady et al, GCN9512) on 2009 June 19 from 02h45m to 05h45m UT (18.25 to 21.25h after the burst) using the position from Cenko et al (GCN9213). The observing band was 14.6 to 17.5 GHz and the rms noise 85 microJy. The angular resolution is approx. 50" x 20". We make a clear detection of a source at the position of the GRB with a flux density 550 microJy. A split of the data suggests that the flux density increased from 425 to 640 microJy between the first and second halves of the observation, but this is barely statistically significant. There is no radio source visible at that position in the NVSS (1.4GHz). This report may be quoted in publications.
GCN 9533 table
GRB_name GRB090618A
GCN_number 9533
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 9533 SUBJECT: VLA radio detection of GRB 090618 DATE: 09/06/19 14:04:59 GMT FROM: Poonam Chandra at U Virginia/NRAO Poonam Chandra (RMC) and Dale A. Frail (NRAO) report on behalf of a larger collaboration: "We used the Very Large Array to observe the field of view toward the GRB 090618 (GCN 9512) at a frequency of 8.46 GHz on 2009 June 19.33 UT. We observed the radio afterglow of the GRB at P60 optical afterglow position reported by Cenko et al. (GCN 9513). The GRB radio afterglow flux density is 383+/-47 uJy. 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 9534 table
GRB_name GRB090618A
GCN_number 9534
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 9534 SUBJECT: GRB 090618, Swift-BAT refined spectral analysis DATE: 09/06/19 18:13:00 GMT FROM: Tilan Ukwatta at GSFC/GWU T. Sakamoto (GSFC/UMBC), T. N. Ukwatta (GWU/GSFC), S. D. Barthelmy (GSFC), (i.e. the Swift-BAT team): Using the data set from T-373 to T+962 sec from the recent telemetry downlink, we report further spectral analysis of BAT GRB 090618 (trigger #355083) (Schady, et al., GCN Circ. 9512). The time-averaged spectrum from T-4.4 to T+213.6 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 1.42 +/- 0.08, and Epeak of 134 +/- 19 keV (chi squared 14.6 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 1.05 +/- 0.01 x 10^-04 erg/cm2 and the 1-sec peak flux measured from T+65.38 sec in the 15-150 keV band is 38.8 +/- 0.8 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.72 +/- 0.02 (chi squared 55.8 for 57 d.o.f.). 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/355083/BA/
GCN 9535 table
GRB_name GRB090618A
GCN_number 9535
Detection_method Fermi GBM Det
t_trigger 8:28:26.660 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 9535 SUBJECT: GRB 090618: Fermi GBM observation DATE: 09/06/19 22:55:39 GMT FROM: Sheila McBreen at MPE Sheila McBreen (UCD/MPE) reports on behalf of the Fermi GBM Team: "At 08:28:26.66 UT on 18 June 2009, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 090618 (trigger 267006508 / 090618353) which was also detected by Swift/BAT (Schady et al. 2009, GCN 9512) and AGILE (Longo et al. 2009, GCN 9524). The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight is 133 degrees. The GBM light curve consists of 4 pulses with a duration of about 155 s (8-1000 keV). The time-averaged spectrum from T0 to T0+140 s is adequately fit by a Band function with Epeak = 155.5 (+11.1/-10.5) keV, alpha = -1.26 (+0.06/-0.02), and beta = -2.50 (+0.15/-0.33). We observe significant spectral evolution within the fitted time interval. The event fluence (8-1000 keV) in this time interval is (2.70 +/- 0.06)E-4 erg/cm^2. Using standard cosmology (Omega_matter = 0.27, Omega_lambda = 0.73, H0=71) and the reported redshift of 0.54 (Cenko et al. 2009, GCN 9518) the isotropic equivalent energy in the 8-1000 keV band is E_iso = 2.0E+53 erg. The 1-sec peak photon flux measured starting from T0+63 s in the 8-1000 keV band is 73.4 +/- 2.0 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 9536 table
GRB_name GRB090618A
GCN_number 9536
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 9536 SUBJECT: GRB090618: OAA-OAUV Optical observations DATE: 09/06/19 23:05:06 GMT FROM: Alberto Fernandez-Soto at IFCA (CSIC/UC,Santander) A. Fernandez-Soto (IFCA-Santander), V. Peris (OAUV-Valencia), and J. Alonso-Lorite (OAUV-Valencia) report: We have observed the field of GRB090618 (Schady et al., GCN 9512) with the OAUV-0.4m telescope at the Observatorio Astronomico de Aras (OAA) in Aras de Alpuente (Valencia, Spain). Observations began after local sunset on June 18 (UT 19:32, (t-t0)~11.1 hours). We took 23 four-minute exposures using a Johnson R filter. The individual frames have been combined in five groups. The afterglow reported in GCN9512 and confirmed by Cenko et al. (GCN 9513) is clearly detected in all five images, with magnitudes and times: UT(middle) Exposure R Error ---------- -------- ----- ----- 21:30:03 5x4min 18.67 0.14 21:50:51 5x4min 18.57 0.09 22:42:14 4x4min 18.62 0.09 23:21:44 5x4min 18.92 0.13 23:45:19 2x4min 18.96 0.13 All magnitudes have been calibrated using stars in the field and the USNO-B1 catalog (R1 mags). Our results agree with those reported by Cano et al. (GCN 9531), and support the presence of a break in the R-band decay, which happened at (t-t0) ~ 14.6 hours. A lightcurve combining our data and previous GCNs is posted at http://ayalga.uv.es/~fsoto/grb090618 OAA is operated by the Observatori Astronomic de la Universitat de Valencia (OAUV).
GCN 9537 table
GRB_name GRB090618A
GCN_number 9537
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 9537 SUBJECT: GRB090618, underlying supernova search DATE: 09/06/20 09:08:39 GMT FROM: Arnon Dar at Technion-Israel Inst. of Tech S. Dado and A. Dar report: The inferred photon spectral index Gamma=2.01+/-0.05 of the early time X-ray afterglow of the relatively nearby bright GRB090618 (z=1.54, GCN 9518) from the Swift XRT observations (Evans et al. http://www.swift.ac.uk/xrt_spectra/00355083/) implies, in the CB model (e.g. ApJ 696 (2009), 994), an asymptotic achromatic power-law decline of the afterglow with a spectral index beta=1.01+/-0.05 and a temporal index alpha=beta+1/2=1.51+/-0.05. The R-band light curve of the anticipated underlying supernova akin to SN1998bw is expected to reach maximum brightness magnitude R=23.9 (Galactic extinction included) around July 10, 2009 (approximately 22 days after GRB090618). Using the latest optical measurements reported in GCN 9531 and GCN 9536, the GRB afterglow is expected to decay by July 10, 2009 to a magnitude R=24.6+/-0.20 yielding R=23.4+/-0.3 for the optical transient superposed on a bright host galaxy with r=22.7 +/- 0.3 (GCN 9526). Like in the case of GRB 030319 (ApJ 594 (2003), L89), the search for an underlying supernova (GCN 9526) in GRB060618 may be more successful using large telescopes with high resolution for photometric and/or spectroscopic follow up measurements of its optical afterglow.
GCN 9538 table
GRB_name GRB090618A
GCN_number 9538
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 9538 SUBJECT: GRB 090618 : WSRT radio detection DATE: 09/06/20 19:59:19 GMT FROM: Atish Kamble at U. of Amsterdam Atish Kamble (University of Amsterdam), A.J. van der Horst (NASA/ORAU) and Ralph Wijiers (University of Amsterdam) reports on behalf of a larger collaboration : "We observed the position of GRB 090618 afterglow at 4.9 GHz using the Westerbork Synthesis Radio Telescope between June 19.78 to 20.30 UT i.e. 1.7 days after the burst (GCN 9512, GCN 9532, GCN 9533). The radio afterglow was clearly detected and its measured flux density is about 501 +/- 47 microJy. We would like to thank the WSRT staff for scheduling and carrying out these observations."
GCN 9539 table
GRB_name GRB090618A
GCN_number 9539
Detection_method Optical
ra 19.0000°
decl 78.0000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 9539 SUBJECT: GRB 090618: ZTSh optical observations DATE: 09/06/21 01:01:06 GMT FROM: Alexei Pozanenko at IKI, Moscow V. Rumyantsev (CrAO), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration: We observed the afterglow (Schady et al., GCN 9512; Cenko et al., GCN 9513; Perley, GCN 9514; Rujopakarn et al., GCN 9515) of the Swift GRB 090618 between (UT) Jun. 18 19:51 - Jun. 19 00:51 with Shajn telescope of CrAO. We detect afterglow in every BVRI of 60 s exposure images of the series. Coordinates of the afterglow are RA(J2000): 19 35 58.77 Dec(J2000): +78 21 24.2 with uncertainties of 0.3 arcsec. Preliminary photometry of selected images based on USNO-B1.0 star 1683-0077955 (RA=19 36 36.34 Dec=+78 21 07.00) assuming R=16.57 is following: T0+ Filter, Exposure, mag., err. (d) (s) 0.4763 R 60 18.60 +/-0.05 0.5680 R 60 18.87 +/-0.03 0.6496 R 60 19.17 +/-0.04 0.6796 R 60 19.19 +/-0.10 The power low index of light curve approximation between 0.48 - 0.65 days is ~ -1.6, while after 0.65 days after burst onset we observe flattening of the light curve. A finding chart can be found at http://grb.rssi.ru/GRB090618/GRB090618_090618_R_ZTSh.gif
GCN 9541 table
GRB_name GRB090618A
GCN_number 9541
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 9541 SUBJECT: GRB 090618: BOAO V-band Observation DATE: 09/06/21 06:09:55 GMT FROM: Myungshin Im at Seoul Nat U M. Im (CEOU/Seoul National Univ), Y.-B. Jeon (KASI), and Y. Urata (NCU) We observed GRB090618 (Schady et al. GCN 9512) in V using a 15.5cm refractor at Bohyunsan Optical Astronomical Observatory in Korea, operarted by the Korea Astronomy Space Science Institute. A series of exposures were taken starting at 2009 June 18, 11:54:19. The afterglow, identified earlier by many groups (GCN 9513, 9514, 9515, 9520, 9522), was clearly detected at V=17.9 +- 0.1 magnitude at mid-time of 2009 12:55:07 (about 4hr 26.6min after the BAT trigger). The photometry was calibrated against nearby SDSS stars where the transformation of SDSS magnitude to V-band magnitude was carried out using the recipe of Chonis & Gaskell (2008).
GCN 9542 table
GRB_name GRB090618A
GCN_number 9542
Detection_method Other
redshift 0.5400
Circular_text TITLE: GCN CIRCULAR NUMBER: 9542 SUBJECT: GRB090618: Spectrum and photometry from 6.0m BTA DATE: 09/06/21 09:05:13 GMT FROM: Antonio Deugarte at IAA-CSIC T. Fatkhullin, A. Moskvitin (SAO-RAS Niznijh Arkhyz, Russia), A.J. Castro-Tirado (IAA-CSIC Granada), A. de Ugarte Postigo (ESO, INAF/OAB), on behalf of a larger collaboration, report: We have observed the field of GRB090618 (Schady et al., GCN 9512) with the 6-m telescope of the SAO RAS in Caucasus. We obtained B, Rc and Ic images as well as a low-resolution spectrum under non favorable weather conditions. The range and resolution of the spectrum were 3900-9200AA and FWHM=15-17A, respectively. A preliminary processing of the spectrum showed a faint emission line at 5748.55A which we interpret as [OII] 3727A. A corresponding redshift of 0.54 is in full agreement with one obtained by Cenko et al. (GCN 9518). Because of strong night sky OH bands and low resolution of the spectrum we could not clearly detect expected Hbeta and [OIII]4959,5007A lines. The photometry was calibrated using a number of SDSS stars in the field. Below we present a summary of some of our observations: middle date, UT results ------------------------------------------------------- spectrum 19.977 June 2009 [OII]3727A detection Rc 19.941 June 2009 20.51 +/- 0.06 This message can be cited.
GCN 9548 table
GRB_name GRB090618A
GCN_number 9548
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 9548 SUBJECT: GRB 090618: RTT150 optical observations DATE: 09/06/22 09:50:24 GMT FROM: Rodion Burenin at IKI, Moscow A. Galeev, I. Bikmaev, N. Sakhibullin (KSU/AST), R. Burenin, M. Pavlinsky, R. Sunyaev (IKI), I. Khamitov, Z. Eker (TUG), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.) report: We observed the OT (Schady et al., GCN 9512; Cenko et al., GCN 9513; Perley, GCN 9514; Rujopakarn et al., GCN 9515) of the Swift GRB 090618 with Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, TUBITAK National Observatory, Turkey), in BRc bands, starting at 22 Jun, 00:03 UT, i.e. approximately 3.65 days after the burst, using TFOSC. We made 3x900s exposures in Rc band and 2x900 in B band. The OT is detected in all images. Using the same USNO-B1 star as it was used by Rumyantsev and Pozanenko (GCN 9539) we estimate Rc magnitude as m_Rc=21.60+/-0.04 (3.68 days after the burst). The finding chart can be found at: http://hea.iki.rssi.ru/grb/090618/indexeng.html
GCN 9553 table
GRB_name GRB090618A
GCN_number 9553
Detection_method Konus-Wind Det
t_trigger 8:28:24.974 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 9553 SUBJECT: Konus-Wind and Konus-RF observations of GRB 090618 DATE: 09/06/22 14:41:45 GMT FROM: Dmitry Frederiks at Ioffe Institute S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P. Oleynik, M. Ulanov, and D. Svinkin on behalf of the Konus-Wind and Konus-RF teams, and T. Cline on behalf of the Konus-Wind team, report: The long GRB 090618 (Schady et al. 2009, GCN 9512) triggered Konus-Wind at T0=30504.974 s UT (08:28:24.974), and Konus-RF instrument onboard CORONAS-PHOTON s/c at T0=30507.060 s UT (08:28:27.060). The burst light curve shows a smooth multi-peaked structure with a duration of ~160 s. Significant spectral evolution was observed during the burst. -- As observed by Konus-Wind the burst had a fluence of (2.5 0.06)x10-4 erg/cm2, and a 64-ms peak flux measured from T0+63.616 s of (1.6 0.2)x10-5 erg/cm2/s (both in the 20 keV - 2 MeV energy range). The time-integrated spectrum of the burst (from T0 to T0+142 s) can be fitted (in the 20 keV - 2 MeV range) by GRB (Band) model for which: the low-energy photon index alpha = -1.28 0.02, the high energy photon index beta = -2.66(-0.2, +0.14), the peak energy Ep = 186 8 keV (chi2 = 103/60 dof). The spectrum at the maximum count rate, measured from T0+62.720 to T0+64.0 s, is well fitted (in the 20 keV - 2 MeV range) by GRB (Band) model for which: the low-energy photon index alpha = -0.99 (-0.06, +0.07), the high energy photon index beta = -2.29(-0.5, +0.23), the peak energy Ep = 440 70 keV (chi2 = 52/55 dof). -- As observed by Konus-RF the burst had a fluence of (2.82 0.06)x10-4 erg/cm2 (both in the 20 keV - 2 MeV energy range), and a 500-ms peak flux measured from T0+63.0 s of (1.6 0.1)x10-5 erg/cm2/s (in the 20 keV - 1.5 MeV energy range). The time-integrated spectrum of the burst (from T0-1.4 to T0+113.0 s) can be fitted (in the 20 keV - 2 MeV range) by GRB (Band) model for which: the low-energy photon index alpha = -1.28 0.03, the high energy photon index beta = -3.06(-0.5, +0.3), the peak energy Ep = 220 8 keV (chi2 = 240/132 dof). The spectrum at the maximum count rate, measured from T0+63.0 to T0+63.5 s, is well fitted (in the 20 keV - 1.5 MeV range) by GRB (Band) model for which: the low-energy photon index alpha = -0.89 (-0.1, +0.3), the high energy photon index beta = -2.56(-1.0, +0.6), the peak energy Ep = 385 (-136, +64) keV (chi2 = 78/74 dof). -- All the quoted values are preliminary. The quoted errors are at the 90% confidence level. The light curves of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB090618_T30504/
GCN 9563 table
GRB_name GRB090618A
GCN_number 9563
Detection_method correction
Circular_text TITLE: GCN CIRCULAR NUMBER: 9563 SUBJECT: PAIRITEL observations of GRB 090618 DATE: 09/06/23 01:00:35 GMT FROM: Adam Morgan at U.C. Berkeley A. N. Morgan, C. R. Klein, J. S. Bloom, (UC Berkeley), report: We observed the location of the optical afterglow of GRB 090618 (Schady et al., GCN 9512) with the 1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began at 2009-06-18 08:29:40 UT, 71 seconds after the Swift Trigger, under non-ideal sky conditions. In the initial images, we detect a variable infrared source (identified as the IR afterglow) in individual frames of 7.8 second simultaneous exposures in the J, H, and Ks bands. The preliminary photometry on selected stacks of images yield the following photometry: time post burst exp. filt mag m_err [s] [s] 210 93.6 J 12.7 0.1 210 93.6 H 12.1 0.1 210 93.6 Ks 11.4 0.2 2818 327 J 15.1 0.1 2818 327 H 14.6 0.1 2818 327 Ks 13.7 0.1 10636 585 J 16.2 0.2 10636 585 H 15.7 0.2 10636 585 Ks >14.8 3-sigma Intermittent clouds led to highly variable transmission and sky brightnesses during the PAIRITEL observations. All magnitudes are given in the Vega system, calibrated to 2MASS. No correction for Galactic extinction has been made to the above reported values. Further analysis is ongoing.
GCN 9568 table
GRB_name GRB090618A
GCN_number 9568
Detection_method Suzaku WAM Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 9568 SUBJECT: GRB 090618: Suzaku WAM observation of the prompt emission DATE: 09/06/24 13:05:44 GMT FROM: Kenta Kono at Miyazaki U K. Kono, A. Daikyuji, E. Sonoda, N. Ohmori, H. Hayashi, K. Noda, Y. Nishioka, M. Yamauchi (Univ. of Miyazaki), M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA), K. Yamaoka, S. Sugita (Aoyama Gakuin U.), Y. E. Nakagawa, T. Tamagawa (RIKEN), S. Hong (Nihon U.), N. Vasquez (Tokyo Tech.), Y. Hanabata, T. Uehara, T. Takahashi, Y. Fukazawa (Hiroshima U.), W. Iwakiri, M. Tashiro, Y. Terada, A. Endo, K. Onda, T. Sugasahara (Saitama U.), Y. Urata (NCU), T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo), on behalf of the Suzaku WAM team, report: The bright, long GRB 090618 was detected by the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 08:28:25.592 UT (=T0). The observed light curve shows a multi-peaked structure starting at T0-5 s and ending at T0+149 s, with a duration (T90) of about 105 seconds. The fluence in 100 - 1000 keV was (1.58 $B!^(B 0.07) x10-4 erg/cm2. The 1-s peak flux measured from T0+65 s was 20.7 (-0.9, +0.8) photons/cm2/s and 9.83(-0.36, +0.26) x10-5 erg/cm2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-5 s to T0+149 s is well fitted by a single power-law with a photon index of 2.32 $B!^(B 0.04 (chi2/d.o.f = 51/51). The 1-s peak spectrum is well fitted by a power-law with exponential cutoff model: dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with alpha: 1.21 $B!^(B 0.13, and Epeak: 623 (-39, +44) keV (chi2/d.o.f. = 41/50). Due to the brightness of this burst, a 3% systematic error was added for low energy channels. All the quoted errors are at 90% confidence level, The light curves for this burst are now available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html
GCN 9570 table
GRB_name GRB090618A
GCN_number 9570
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 9570 SUBJECT: GRB 090618: Correction to GCN 9568 DATE: 09/06/24 15:47:37 GMT FROM: Kazutaka Yamaoka at Aoyama Gakuin U K. Kono (Univ. of Miyazaki), on behalf of the Suzaku WAM team, report: There are some garbled characters and a wrong value reported in Kono et al. (GCN 9568). The correct values are as follows: 1-s peak flux : 9.83 (-0.36, +0.26) x 10^-6 erg/cm^2/s The fluence in 100 - 1000 keV: (1.58 +/- 0.07) x 10^-4 erg/cm^2 The photon index for time-averaged spectrum : 2.32 +/- 0.04 alpha for 1-s peak spsctrum: 1.21 +/- 0.13 We apologize for any inconvenience.
GCN 9575 table
GRB_name GRB090618A
GCN_number 9575
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 9575 SUBJECT: GRB 090618: SARA Second Epoch Observations DATE: 09/06/25 21:08:25 GMT FROM: Adria C. Updike at Clemson U Adria Updike, Sean Brittain, Dieter Hartmann (Clemson University), Andrew Colson, Renata Cumbee, Brianne Hackett, Josiah Lewis, and Marten Kronberg (SARA REU) report: We re-observed the field of GRB 090618 (Schady et al., GCN 9512) using the 0.9m SARA telescope at Kitt Peak National Observatory beginning 20 hours after the trigger and continuing for 3 hours. Our observations consisted of 45 sec exposures in the R and I bands under good conditions. The afterglow is detected in stacked images. Magnitudes are given below as compared to the USNOB.1 catalog. Time is given in days after the trigger; exposure time in seconds. Time Filter Exp Mag ------------------------------------ 0.84 R 1215 19.4 +/- 0.1 0.86 I 1215 18.8 +/- 0.1 http://www.saraobservatory.org/
GCN 9576 table
GRB_name GRB090618A
GCN_number 9576
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 9576 SUBJECT: GRB090618: HCT optical observations DATE: 09/06/25 21:41:30 GMT FROM: D.K. Sahu at Indian Inst of Astrophysics,Bangalore G.C. Anupama, U.K. Gurugubelli, D.K. Sahu report Optical afterglow of GRB090618 (Schady et al., GCN 9512) was observed with the 2m. Himalayan Chandra Telescope of the Indian Astronomical Observatory, Hanle, India. The optical afterglow was observed in Bessell R filter and it was detected in all the frames. The preliminary magnitude of the optical afterglow, calibrated using the USNO B1 (R1 magnitude) of the nearby stars in the GRB field is as under: Date Mid UT Exposure R Mag Error 18-06-2009 19:29 300sec 18.70 0.07 18-06-2009 19:36 300sec 18.75 0.06 19-06-2009 22:08 2x300+450 20.30 0.09
GCN 9592 table
GRB_name GRB090618A
GCN_number 9592
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 9592 SUBJECT: GRB090618: 15GHz radio emission faded DATE: 09/06/29 11:26:44 GMT FROM: Guy Pooley at MRAO, Cambridge, UK Further to GCN 9532, Guy Pooley (Cavendish Astrophysics, U. Cambridge) reports on behalf of the AMI consortium that the radio emission at 15 GHz from GRB090618 has faded. Data from the AMI Large Array are given below, including data taken on 090619 reported in GCN 9532: yymmdd.ddd hhmm-hhmm S rms UT microJy microJy 090619.073 0245-0415 425 120 090619.208 0415-0545 640 120 090620.182 0340-0505 415 87 090621.275 0536-0736 139 91 090622.175 0328-0457 63 96 090627.021 0013-0048 -127 190 These results may be quoted in publications.
GCN 9597 table
GRB_name GRB090618A
GCN_number 9597
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 9597 SUBJECT: GRB 090618: RTT150 optical observations DATE: 09/06/30 14:12:04 GMT FROM: Irek Khamitov at TUG I. Khamitov, M. Parmaksizoglu, T. Ak, Z. Eker (TUG), Z. Aslan (Kultur Uni.), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.) R. Burenin, M. Pavlinsky, R. Sunyaev (IKI), I. Bikmaev, N. Sakhibullin (KSU/AST), report: We observed the OT (Schady et al., GCN 9512; Cenko et al., GCN 9513; Perley, GCN 9514; Rujopakarn et al., GCN 9515) of the Swift GRB 090618 with Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, TUBITAK National Observatory, Turkey), in Rc band during three nights 25,26 and 27 June 2009 and in B band in 26 June. Every night we made 3x900s exposures in Rc band and in 26 June we made additionally 3x900 in B band. The OT is detected in all stacked images in Rc. The brightness of OT is not changed inside of photometric error. Our preliminary estimate of its magnitude during these observations is m_Rc=22.3+/-0.1 (7.68, 8.64, 9.58 days after the burst). We found no OT on stacked B-image. The limiting magnitude of the frame is mlim_B=23.4 (8.68 days after the burst). -- This message has been scanned for viruses and dangerous content by MailScanner, and is believed to be clean.
GCN 9613 table
GRB_name GRB090618A
GCN_number 9613
Detection_method Optical
ra 19.0000°
decl 78.0000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 9613 SUBJECT: GRB 090618: Mondy optical observations DATE: 09/07/04 00:32:08 GMT FROM: Alexei Pozanenko at IKI, Moscow E. Klunko (ISTP), A. Volnova (SAI MSU), A. Pozanenko (IKI) on behalf of larger GRB follow up collaboration report: We observed the afterglow (Schady et al., GCN 9512; Cenko et al., GCN 9513; Perley, GCN 9514; Rujopakarn et al., GCN 9515) of the Swift GRB 090618 between (UT) Jun. 18 18:14 -- 18:43 with 1.5m telescope of Sayan observatory (Mondy). The afterglow is detected in stacked images. Preliminary photometry of the stacked images based on USNO-B1.0 star 1683-0077955 (RA=19 36 36.34 Dec=+78 21 07.00) assuming R=16.57 is following: T0+ Filter, Exposure, mag., err. (d) (s) 0.4083 R 10x30 18.60 +/-0.10
GCN 9665 table
GRB_name GRB090618A
GCN_number 9665
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 9665 SUBJECT: Detection of GRB 090618 by RT-2 Experiment onboard the CORONAS-PHOTON Satellite DATE: 09/07/15 08:23:22 GMT FROM: Sandip K. Chakrabarti at S.N. Bose Nat. Centre for Basic Sci. Detection of GRB 090618 by RT-2 Experiment onboard the CORONAS-PHOTON Satellite A. R. Rao, J. P. Malkar, M. K. Hingar, V. K. Agrawal (TIFR, Mumbai, India), S. K. Chakrabarti, A. Nandi, D. Debnath, T. C. Kotoch (ICSP, Kolkata, India), T. R. Chidambaram, P. Vinod, S. Sreekumar (VSSC, Thiruvananthapuram, India), Y. D. Kotov, A. S. Buslov, V. N. Yurov, V. G. Tyshkevich, A. I. Arkhangelskij, R. A. Zyatkov (MephI, Moscow, Russia) report: The RT-2 Experiment onboard the CORONAS-PHOTON satellite has clearly detected GRB 090618 (Schady et al., 2009, GCN 9512) which triggered at T0 = 30507.00 sec (UT) (08h 28m 27s). The satellite was in the SHADOW mode (away from the SUN) with GOOD time (away from the polar and SAA regions) observation of 700 sec starting at 08h 23m 27sec (UT) and ending at 08h 36m 46.99sec (UT). The GRB light curve shows a complex profile (Golenetskii et al., 2009, GCN 9553) of time duration of around 150 sec. The burst profile has three main pulses with the brightest pulse (~700 cts/sec) started at T0+65 sec, the second one at T0+85 sec and the last one at T0+115 sec. Both RT-2/S and RT-2/G detectors have registered this multi-structured burst profile of the light curve in the energy band of 60 - 215 keV. In high-energy band of 330 - 1000 keV, the profile becomes simple with a single bright peak at T0+65 sec. It is also noted that the burst width decreases with the increase in the energy band, a quiet natural phenomena of GRB burst profile. The burst was incident at an angle of 77 degrees to the detector axis. It showed the typical Band spectrum with peak energy at about 180 keV and integrated 20 keV - 1MeV flux of 2.8 X 10^-4 ergs/ cm^2. The light curve is available at the web-site: http://csp.res.in/rt2_files/grb090618-lc.html