//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9374 SUBJECT: GRB 090516: Swift detection of a burst DATE: 09/05/16 08:49:10 GMT FROM: David Palmer at LANL B. A. Rowlinson (U Leicester), A. P. Beardmore (U Leicester), P. A. Evans (U Leicester), C. Guidorzi (U Ferrara), J. A. Kennea (PSU), P. T. O'Brien (U Leicester), K. L. Page (U Leicester), D. M. Palmer (LANL), P. Romano (INAF-IASFPA) and T. Sakamoto (NASA/UMBC) report on behalf of the Swift Team: At 08:27:50 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 090516 (trigger=352190). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 138.271, -11.858 which is RA(J2000) = 09h 13m 05s Dec(J2000) = -11d 51' 27" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a multiple-peaked structure with a duration of at least 150 sec. The peak count rate was ~1000 counts/sec (15-350 keV), at ~5 sec after the trigger, with additional prominent peaks at T+35, T+90 and T+135. The XRT began observing the field at 08:30:37.4 UT, 166.7 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source located at RA, Dec 138.26119, -11.85480 which is equivalent to: RA(J2000) = 09h 13m 2.69s Dec(J2000) = -11d 51' 17.3" with an uncertainty of 4.1 arcseconds (radius, 90% containment). This location is 36 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. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density consistent with the Galactic value of 4.47e+20 cm^-2 (Kalberla et al. 2005). The initial flux in the 0.1 s image was 1.96e-08 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 176 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 0.05. Burst Advocate for this burst is B. A. Rowlinson (bar7 AT star.le.ac.uk). Please contact the BA by email if you require additional information regarding Swift followup of this burst. In extremely urgent cases, after trying the Burst Advocate, you can contact the Swift PI by phone (see Swift TOO web site for information: http://www.swift.psu.edu/too.html.) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9375 SUBJECT: GRB 090516: Faulkes Telescope South optical afterglow DATE: 09/05/16 10:08:59 GMT FROM: Cristiano Guidorzi at Ferrara U,Italy C. Guidorzi (U. Ferrara), I. A. Steele, A. Melandri, D. Bersier, C.J. Mottram, C.G. Mundell, R.J. Smith (Liverpool JMU), A. Gomboc (U. Ljubljana), P. O'Brien, N. Bannister, N. Tanvir (U. Leicester) on behalf of a large collaboration report: The 2-m Faulkes Telescope South reacted to the Swift burst GRB 090516 (trigger=352190, Rowlinson et al. GCN 9374). Observations started about 16.9 min after the trigger time with filters BRi. Within the XRT error circle we found a fading source at the following position (J2000): RA: 09:13:02.62 Dec: -11:51:15.4 with an initial approximate magnitude of R~19 at 17 minutes post trigger. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9376 SUBJECT: GRB 090516: Enhanced Swift-XRT position DATE: 09/05/16 14:06:48 GMT FROM: Phil Evans at U of Leicester A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) report on behalf of the Swift-XRT team. Using 2534 s of XRT Photon Counting mode data and 5 UVOT images for GRB 090516, 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 = 138.26050, -11.85442 which is equivalent to: RA (J2000): 09h 13m 2.52s Dec (J2000): -11d 51' 15.9" with an uncertainty of 1.5 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. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9377 SUBJECT: GRB 090516: Swift/UVOT Observations DATE: 09/05/16 18:45:43 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) and B. A. Rowlinson (Leicester) report on behalf of the Swift/UVOT team. The Swift/UVOT began observing the field of GRB 090516 171s after the BAT trigger (Beardmore et al., GCN Circ. 9374). Data summed from the first and second orbits does not reveal a source at the refined position of the X-ray afterglow (Beardmore et al., GCN Circ. 9376). The 3-sigma upper limits for the finding chart (fc) and summed exposures are reported below: FILTER T_start(s) T_stop Exposure Mag/3UL ============================================================= white fc 171 321 147 > 20.85 white 3843 5478 393 > 21.06 v 4254 5890 393 > 19.63 b 585 601 15 > 18.74 b 5073 5273 196 > 20.32 u 329 579 245 > 20.12 u 4868 6384 274 > 20.20 uvw1 4664 6301 393 > 20.36 uvm2 4458 6096 393 > 20.18 uvw2 4049 5685 393 > 20.41 ================================================================= The above magnitudes are not corrected for the Galactic extinction corresponding to a reddening of E_{B-V} = 0.05 (Schlegel et al., 1998, ApJS, 500, 525). The photometry is on the UVOT photometric system described in Poole et al. (2008, MNRAS, 383, 627). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9378 SUBJECT: GRB 090516: Swift XRT refined analysis DATE: 09/05/16 20:04:01 GMT FROM: Antonia Rowlinson at U.of Leicester B. A. Rowlinson and P. Evans (U Leicester) report on behalf of the Swift-XRT team: We have analysed 3.0 ks of XRT data for GRB 090516 (Rowlinson et al. GCN Circ. 9374), from 170 s to 6.4 ks after the BAT trigger. The data comprise 327 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Beardmore et al. (GCN. Circ 9376). The light curve can be modelled with a power-law decay with two flares superimposed on it. The initial decay index is alpha=3.27 (+0.11, -0.10). At T+601 (+138, -52) s the decay flattens to an alpha of 0.93 (+0.11, -0.10). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 2.09 (+/-0.04). The best-fitting absorption column is 1.57 (+0.10, -0.09) x 10^21 cm^-2, in excess of the Galactic value of 4.5 x 10^20 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index of 2.09 (+0.13, -0.12) and a best-fitting absorption column of 9.6 (+2.6, -2.5) x 10^20 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.6 x 10^-11 (4.8 x 10^-11) erg cm^-2 count^-1. If the light curve continues to decay with a power-law decay index of 0.93, the count rate at T+24 hours will be 0.03 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x 10^-12 (1.4 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/00352190. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9379 SUBJECT: GRB 090516: NOT optical observations DATE: 09/05/16 22:47:41 GMT FROM: Javier Gorosabel at IAA-CSIC J. Gorosabel (IAA-CSIC), de Ugarte Postigo (ESO, Santiago), D. Montes (UCM, Madrid), A. Klutsch (UCM, Madrid), A.J. Castro-Tirado (IAA-CSIC), report on behalf of a larger collaboration: We observed the optical afterglow of GRB 090516 (Guidorzi et al. GCN 9375) with the 2.5m NOT(+STANCAM) telescope. On May 16.889 UT (12.9 hours post GRB) the afterglow shows an R-band magnitude of R=21.3+/-0.1 against USNO-B1.0 field stars. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9381 SUBJECT: GRB 090516: VLT redshift DATE: 09/05/17 02:47:56 GMT FROM: Antonio Deugarte at IAA-CSIC A. de Ugarte Postigo (ESO), J. Gorosabel (IAA/CSIC), D. Malesani, J.P.U. Fynbo (DARK/NBI), A. J. Levan (Univ. Warwick), report on behalf of a larger collaboration: We observed the optical afterglow of GRB 090516 (Rowlinson et al., GCN 9374; Guidorzi et al., GCN 9375) with the ESO VLT equipped with FORS2. Observations started on 2009 May 16.989 UT (15.1 hr after the GRB). In the acquisition image, the afterglow is well detected with R ~ 21.2, consistent with the NOT measurement (Gorosabel et al., GCN 9379). Two spectra lasting 30 min each were acquired with the grism 300V, covering the wavelength range 3500-9200 AA. In a preliminary analysis we detect the Lyman limit, a strong Ly-alpha absorption as well as a number of strong absorption lines (SII, OI, CII, SiIV, CIV, AlII etc.) at a redshift of z=3.9. We acknowledge excellent support from the observing staff in Paranal, in particular Alain Smette, Leo Rivas and Gianni Marconi. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9382 SUBJECT: GRB 090516: GROND OBSERVATIONS DATE: 09/05/17 05:00:40 GMT FROM: Andrea Rossi at TLS Tautenburg A. Rossi (Tautenburg), P. Afonso and J.Greiner (both MPE Garching) report on behalf of the GROND team: We observed the field of GRB 090516 (Swift trigger 352190, B. Rowlinson et al.,GCN #9374) simultaneously in g'r'i'z'JHK with GROND mounted at the 2.2m ESO/MPI telescope at La Silla Observatory (Chile). Observations started on 16 May 2009 at 23:04 UT, 14.6 h after the burst. We detect the afterglow at a position consistent with the enhanced XRT error circle (A. Beardmore et al., GCN #9376) and NOT (J. Gorosabel et al., GCN #9379) and Faulkes Telescope detections (C. Guidorzi et al., GCN #9375). With an exposure time of 20min in JHK and 25min in griz, preliminary photometry yields the following AB magnitudes: g =23.60 +-0.1 r =21.44 +-0.1 i =20.38 +-0.1 z =19.95 +-0.1 J =19.6 +-0.1 H =19.2 +-0.1 K =19.1 +-0.2 The quoted error is statistical only. There is an additional systematic error in the absolute calibration using the GROND zero points and 2MASS field stars which is expected to be in the 0.2 mag range. Quoted magnitudes are not corrected for the galactic foreground extinction corresponding to a reddening of E_(B-V)=0.05. Preliminary results fitting the SED with Hyperz give for no reddening a z ~ 4.5 and for best fitting solution a photometric redshift of 4.1 +- 0.3, with SMC reddening of A_v = 0.4. This SMC photometric redshift is compatible with VLT's spectroscpic redshift of z = 3.9 (A. de Ugarte Postigo et al. GCN #9381). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9383 SUBJECT: GRB 090516: VLT spectrum (correction & update) DATE: 09/05/17 08:38:02 GMT FROM: Antonio Deugarte at IAA-CSIC A. de Ugarte Postigo (ESO), J. Gorosabel (IAA/CSIC), D. Malesani, J.P.U. Fynbo (DARK/NBI), A. J. Levan (Univ. Warwick), report on behalf of a larger collaboration: We have reanalysed the spectrum of the afterglow of GRB 090516 (Rowlinson et al., GCN 9374; Guidorzi et al., GCN 9375) obtained with the ESO VLT (de Ugarte Postigo et al. GCN 9381). Due to an error in the preliminary reduction, the wavelength calibration had an offset that has been now corrected. In our new analysis we detect a strong Ly-alpha absorption together with absorption lines of NV, SII, SiII, NiII, CI, SiIV, CIV, FeII, AlII, AlIII as well as SiII* at a redshift of 4.109+/-0.002, which we identify as the redshift of the afterglow. This is in agreement with the photometric redshift obtained with GROND (Rossi et al. GCN 9382). The spectrum also shows an intervening system at z=2.697+/-0.002, characterised by the presence of several FeII absorption lines. [GCN OPS NOTE(17may09): Per author's request, the Subject line was changed from "091516" to "090516". And in the first sentence from "090416" to "090516".] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9384 SUBJECT: GRB 090516: Swift-BAT refined analysis DATE: 09/05/17 16:59:56 GMT FROM: Scott Barthelmy at NASA/GSFC 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), B. A. Rowlinson (U Leicester), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team): Using the data set from T-240 to T+963 sec from recent telemetry downlinks, we report further analysis of BAT GRB 090516 (trigger #352190) (Rowlings, et al., GCN Circ. 9374). The BAT ground-calculated position is RA, Dec = 138.246, -11.848 deg, which is RA(J2000) = 09h 12m 59.1s Dec(J2000) = -11d 50' 51.4" with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment). The partial coding was 9%. The mask-weighted light curve shows several overlapping peaks starting at ~T-20 sec witht he last peak at ~T+180 sec, and then decaying to background at ~T+330 sec. The burst went out of the BAT FOV at T+700 sec when Swift did a pre-programmed slew. T90 (15-350 keV) is 210 +- 65 sec (estimated error including systematics). The time-averaged spectrum from T-15.5 to T+288.5 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.84 +- 0.11. The fluence in the 15-150 keV band is 9.0 +- 0.6 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+7.98 sec in the 15-150 keV band is 1.6 +- 0.2 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/352190/BA/ [GCN OPS NOTE(17may09): Per author's request, the TBDs in the first sentence in the third paragraph were replaced with the actual times.] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9391 SUBJECT: GRB 090516, RIMOTS optical upper limits DATE: 09/05/18 13:29:42 GMT FROM: Norisuke Ohmori at Miyazaki U N. Ohmori, E. Sonoda, K. Kono, H. hayasi, A. Daikyuji, Y. Nisioka, K. Noda, M. Yamauchi (University of Miyazaki) We have observed the field covering the error circle of GRB090516 (Swift trigger 352190, GCN 9374, Rowlinson et al.) with the unfiltered CCD camera on the 30-cm telescope at University of Miyazaki. The observation was started 11:16:08 UT (1.8 hr after the Swift trigger), under cloudy condition. First image was obtained at 11:17:11 UT (1.8 hr after the Swift trigger). We have compared our data of 30 sec exposures with the USNO-A2.0 catalog. There is no new source at the reported position. (GCN 9374, B. A. Rowlinson et al. GCN 9375, C. Guidorzi et al. GCN 9376, A. P. Beardmore et al. GCN 9379, J. Gorosabel et al. GCN 9381, A. de Ugarte Postigo et al.) the upper limits are as follows: --------------------------------------------------------------- Start(UT) End(UT) Num. of frames Limit (mag.) --------------------------------------------------------------- 11:16:08 11:17:11 1 15.6 11:16:08 12:04:00 21 17.7 --------------------------------------------------------------- //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9396 SUBJECT: GRB 090516: Observations from Stardome Observatory DATE: 09/05/19 06:10:37 GMT FROM: Antonio Deugarte at IAA-CSIC G. W. Christie (Stardome, New Zealand), A. de Ugarte Postigo (ESO, Chile) and T. Natusch (Stardome, New Zealand) on behalf of a larger collaboration report: We observed the field of GRB 090516 (Rowlinson et al. GCN 9374) with the Stardome 0.4m telescope located in Auckland (New Zealand) starting at 09:25UT. We used a SG530 filter that transmits wavelengths above 5300 Angstroms and a SBIG ST-L-6303E CCD (KAF-6303E detector). A 9x300s combined exposure with mean epoch 16.4080 May (80 minutes after the burst) shows an object at the position of the afterglow (Guidorzi et al. GCN 9375) measured at R = 20.8 +/- 0.2 as compared to USNO-B1.0 stars. We note that with the GRB at a redshift of 4.1 (de Ugarte Postigo et al. GCN 9383), Ly-alpha falls within the R-band, so that comparison of clear and very broad band filters such as ours with R-band has to be handled with care. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9413 SUBJECT: GRB 090516B: Fermi GBM detection DATE: 09/05/20 17:04:52 GMT FROM: Sheila McBreen at MPE Sheila McBreen (UCD/MPE) reports on behalf of the Fermi GBM Team: "At 03:17:20.17 UT on 16 May 2009, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 090516B (trigger 264136642 / 090516137). The on-ground calculated location, using the GBM trigger data, is RA = 122.2, DEC = -71.62 (J2000 degrees, equivalent to 08 h 09 m, -71 d 37 '), with an uncertainty of 2.6 degrees (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 45 degrees. The GBM light curve consists of several overlapping peaks from the trigger to about 140 s and possible weak emission out to about 350 s. The time-averaged spectrum from T0 s to T0+138 s is adequately fit by a power law function with an exponential high energy cutoff. The power law index is -1.01 (+/-0.06) and the cutoff energy, parameterized as Epeak, is 327.0 (+/-58.7) keV (chi squared 419 for 359 d.o.f.). The event fluence (8-1000 keV) in this time interval is (3.0 +/- 0.1)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+80 s in the 8-1000 keV band is 4.0 +/- 0.2 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9415 SUBJECT: GRB 090516: Fermi GBM observation DATE: 09/05/21 08:51:16 GMT FROM: Sheila McBreen at MPE Sheila McBreen (UCD/MPE) reports on behalf of the Fermi GBM Team: "At 08:27:58.35 UT on 16 May 2009, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 090516 (trigger 264155280 / 090516353). which was also detected by the Swift-BAT (Rowlinson et al. 2009, GCN 9374). The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight is 20 degrees. The GBM light curve consists of about five overlapping pulses from T0-50 s to T+120 s. There is continued weak emission until about T0+300 s (8-1000 keV). Due to a large change in the spacecraft pointing during this long burst, a time averaged spectrum could not be fit. Instead three spectral intervals from -50 to 20 sec, 20 to 60 sec and 60 to 120 seconds were selected. The first interval was well fit by a power law function with an exponential high energy cutoff. The power law index is -1.51 ( +/-0.11 ) and the cutoff energy, parameterized as Epeak, is 185.6 (+98.4/-42.5) keV. The second and third intervals are adequately fit by a Band function. The parameters for interval two are alpha = -1.03 (+0.26/-0.31) , Epeak = 51.4 (+20.1, -11.4), beta= -2.1 ( +0.1/-0.2) and for the third interval, alpha = 0.30 (+1.30/ - 0.78), Epeak = 27.87 +/- 5.0), beta = -2.64 +/-0.4. The sum of the event fluence (8-1000 keV) in these time intervals is (2.3 +/- 0.5)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+28.6 s in the 8-1000 keV band is 5.3 +/- 0.2 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9418 SUBJECT: GRB 090516C: Fermi GBM detection DATE: 09/05/21 23:32:21 GMT FROM: Alexander van der Horst at NASA/MSFC A.J. van der Horst (NASA/MSFC/ORAU) reports on behalf of the Fermi GBM Team: "At 20:28:40.05 UT on 16 May 2009, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 090516C (trigger 264198522 / 090516.853). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 15.7, Dec = -13.7 (J2000 degrees, equivalent to J2000 1h03m, -13d41'), with a statistical uncertainty of 3.5 degrees (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 69 degrees. The GBM light curve consists of one short spike and some smaller peaks, with a total duration (T90) of 15 s (8-1000 keV). The time-averaged spectrum from T0+0.00 to T0+15.26 s is adequately fit by a power law with an exponential high-energy cutoff. The index is -1.51 +/- 0.08 and the cutoff energy, parameterized as Epeak, is 210 +/- 68 keV (chi squared 372 for 360 d.o.f.). The Band function provides a significantly better fit (chi squared 365 for 359 d.o.f.) with a lower Epeak value, but the low-energy index alpha and the amplitude are poorly constrained: alpha is -0.44 +/- 0.81, beta is -1.81 +/- 0.06, and Epeak is 38 +/- 14. The fluence (8-1000 keV) in this interval is (4.0 +/- 0.3)E-6 erg/cm^2. The 1-sec peak photon flux measured starting from T0+0.0s in the 8-1000 keV band is 7.7 +/- 0.4 ph/s/cm^2. The spectral and temporal analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 9422 SUBJECT: GRB 090516A: Konus-Wind and Swift/BAT joint spectral analysis DATE: 09/05/24 17:27:29 GMT FROM: Takanori Sakamoto at NASA/GSFC T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester), J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), K. McLean (GSFC/UMD), D. Palmer (LANL), G. Sato (GSFC/ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), and T. Ukwatta (GWU) V. Pal'shin, S. Golenetskii, R.Aptekar, E. Mazets, D. Frederiks, and T. Cline on behalf of the Konus-Wind team, report: We performed the Konus-Wind and the Swift/BAT joint spectral analysis of GRB 090516A (Swift/BAT trigger #352190: Rowlinson et al., GCN Circ. 9374, Baumgartner et al. GCN Circ. 9384). Since the Konus-Wind observed this GRB in the waiting mode, we only have 3 channel spectral data for the Konus-Wind which cover the energy range from 20 keV to 1.2 MeV. The joint spectral analysis of the Konus-Wind and the Swift/BAT data allows us to derive the broad-band spectral parameters of this burst. The time interval of the spectral data for each instrument is chosen from T0(BAT)-12.2 to T0(BAT)+96.7 sec where T0(BAT) is the trigger time of BAT at 08:27:50.8 UTC. The energy ranges which we used in the joint spectral analysis are 20-1200 keV and 14-150 keV for the Konus-Wind and the Swift/BAT respectively. The spectral data of two instruments are fitted with the spectral model multiplied by the constant factor to take into account the systematic effective area uncertainties in the response matrices of each instrument. The spectrum is well fitted with a power-law with exponential cutoff model: dN/dE ~ E^{alpha}*exp(-(2+alpha)*E/Epeak). The constant factors of each instrument agree within 10%. No systematic residual from the best fit model is seen in the spectral data of each instrument. The best fit spectral parameters are: alpha = -1.5 (-0.3/+0.2) and Epeak = 190 (-65/+230) keV (chi2/dof = 54/56). The best fit spectral parameters for the GRB (Band) model fixing beta = -2.5 are: alpha = -1.5 (-0.2/+0.3), and Epeak = 190 (-75/+270) keV (chi2/dof = 55/56). The energy fluence in the 15-1200 keV band calculated by a power-law with exponential cutoff model for this 107.9 sec interval is (1.5 +/- 0.3)x10^-5 erg/cm2. Assuming z = 4.109 (de Ugarte Postigo et al. GCN Circ. 9383) 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 = 6.5 (-1.1/+1.4) x10^53 erg in 1 keV to 10 MeV at the GRB rest frame extrapolating the best Band function fit fixing beta = -2.5. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB090516/ All the quoted errors are at the 90% confidence level.