GRB170714A

This page lists all entries on GRB170714A in GRBweb

Summary IPN Swift GCN 21340 GCN 21341 GCN 21343 GCN 21345 GCN 21346 GCN 21347 GCN 21350 GCN 21351 GCN 21352 GCN 21353 GCN 21356 GCN 21359 GCN 21360 GCN 21379 GCN 21396 GCN 21424 GCN 21464

Summary table
Variable Value Source
T0 12:25:32 UTC GCN_circulars,Swift Det
ra 34.3499° Swift
decl 1.9914° Swift
pos_error 1.81e-04° Swift
fluence 2.80e-06 erg/cm² Swift
redshift 0.7930
GBM_located False
mjd 57948.51773148148 GCN_circulars,Swift Det
IPN table
GRB_name GRB170714A
ra 34.3208°
decl 1.9833°
pos_error 5.00e-02°
redshift 0.7930
Swift table
GRB_name GRB170714A
t_trigger 12:25:32 UTC
ra 34.3499°
decl 1.9914°
pos_error 1.81e-04°
fluence 2.80e-06 erg/cm²
redshift 0.7930
GCN 21340 table
GRB_name GRB170714A
GCN_number 21340
Detection_method Swift Det
t_trigger 12:25:32 UTC
ra 34.3210°
decl 1.9870°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21340 SUBJECT: GRB 170714A: Swift detection of a burst DATE: 17/07/14 12:52:55 GMT FROM: David Palmer at LANL A. D'Ai (INAF-IASFPA), D. N. Burrows (PSU), A. Cholden-Brown (PSU), V. D'Elia (ASDC), J. A. Kennea (PSU), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester), D. M. Palmer (LANL) and B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team: At 12:25:32 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 170714A (trigger=762535). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 34.321, +1.987 which is RA(J2000) = 02h 17m 17s Dec(J2000) = +01d 59' 14" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). As is usual with an image trigger, the available BAT light curve shows no significant structure. The XRT began observing the field at 12:32:05.3 UT, 392.7 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 34.3498, 1.9901 which is equivalent to: RA(J2000) = +02h 17m 23.95s Dec(J2000) = +01d 59' 24.4" with an uncertainty of 5.0 arcseconds (radius, 90% containment). This location is 104 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 U filter starting 869 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 19.2 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 18.0 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.03. Burst Advocate for this burst is A. D'Ai (antonino.dai AT ifc.inaf.it). 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 21341 table
GRB_name GRB170714A
GCN_number 21341
Detection_method Swift-XRT Det
ra 34.3498°
decl 1.9920°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21341 SUBJECT: GRB 170714A: Enhanced Swift-XRT position DATE: 17/07/14 15:23:59 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 641 s of XRT Photon Counting mode data and 1 UVOT images for GRB 170714A, 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 = 34.34983, +1.99204 which is equivalent to: RA (J2000): 02h 17m 23.96s Dec (J2000): +01d 59' 31.3" with an uncertainty of 1.8 arcsec (radius, 90% confidence). This position may be improved as more data are received. The latest position can be viewed at http://www.swift.ac.uk/xrt_positions. Position enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular was automatically generated, and is an official product of the Swift-XRT team.
GCN 21343 table
GRB_name GRB170714A
GCN_number 21343
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 21343 SUBJECT: GRB 170714A: Swift-XRT refined Analysis DATE: 17/07/15 01:16:20 GMT FROM: Phil Evans at U of Leicester P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A. Cholden-Brown (PSU), S. J. LaPorte (PSU), J.A. Kennea (PSU), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), S.L. Gibson (U. Leicester) and A. D'Ai report on behalf of the Swift-XRT team: We have analysed 8.8 ks of XRT data for GRB 170714A (D'Ai et al. GCN Circ. 21340), from 383 s to 22.6 ks after the BAT trigger. The data comprise 1.3 ks in Windowed Timing (WT) mode (the first 8 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Evans et al. (GCN Circ. 21341). The late-time light curve (from T0+5.0 ks) is consistent with a constant source of mean count rate 1.4e+01 ct/sec. A power-law fit gives an index of 1.7 (+1.8, -2.8). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.588 (+/-0.018). The best-fitting absorption column is 9.3 (+/-0.6) x 10^20 cm^-2, in excess of the Galactic value of 3.6 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 1.73 (+/-0.05) and a best-fitting absorption column of 9.0 (+/-1.5) x 10^20 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.9 x 10^-11 (4.4 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 9.0 (+/-1.5) x 10^20 cm^-2 Galactic foreground: 3.6 x 10^20 cm^-2 Excess significance: 6.1 sigma Photon index: 1.73 (+/-0.05) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00762535. This circular is an official product of the Swift-XRT team.
GCN 21345 table
GRB_name GRB170714A
GCN_number 21345
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 21345 SUBJECT: GRB 170714A: Bastille Day Burst: ULGRB or RTDE? DATE: 17/07/15 03:48:00 GMT FROM: Alexander Kann at TLS Tautenburg D. A. Kann, A. de Ugarte Postigo, L. Izzo, and C. C. Thoene (HETH/IAA-CSIC) report: GRB 170714A (D'Ai et al. GCN #21340) exhibits very variable behavior in its X-ray light curve beyond what is reported by D'Avanzo et al. (GCN #21343). We especially point out a very rapid decay at ~ 18ks, from ~5 ct/s to 0.01 ct/s in about 1.3 ks. Even after this steep decay, which is a typical sign of central-engine turn-off, the XRT light curve shows flaring activity of a factor of ~5. All this activity is usually the sign of an active central engine. This highly variable behavior is reminiscent of two types of sources: Ultra-long GRBs like GRBs 101225A, 111209A and 130925A (e.g., Thoene et al., Nature, 480, 72; Gendre et al., ApJ, 766, 30; Levan et al., ApJ, 781, 13; Greiner et al., A&A, 568, A75; Kann et al., A&A, submitted, arXiv:1706.00601) or relativistic tidal disruption events such as Sw J1644 (e.g., Levan et al., Science, 333, 199). So far no optical source has been reported, and the X-ray afterglow shows signs of additional absorption (D'Avanzo et al., GCN #21343), which may be indicative of a reddened source in the center of its host and therefore a RTDE. On the other hand, the source is significantly brighter than Sw J1644, and no obvious host galaxy is seen in SDSS or PanSTARRS pre-imaging. The hosts of GRBs 101225A and 111209A were also very faint, and GRB 130925A showed very strong absorption. If this event is an ULGRB, the flaring activity persists for nearly 40ks until now, making it significantly longer than even GRB 111209A. Despite the inclement visibility, observations of this source are strongly encouraged.
GCN 21346 table
GRB_name GRB170714A
GCN_number 21346
Detection_method Other
ra 34.3500°
decl 1.9915°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21346 SUBJECT: GRB 170714A: z-band afterglow candidate for OSIRIS/GTC DATE: 17/07/15 06:37:17 GMT FROM: Antonio de Ugarte Postigo at IAA-CSIC A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), D. A. Kann L. Izzo, C. C. Thoene (HETH/IAA-CSIC), N. Castro-Rodriguez (GTC, IAC, ULL), A. Marante, J. A. Melian (GTC) report: We observed the field of GRB 170714A (D'Ai et al. GCN 21340), an ULGRB or RTDE candidate (Kann et al., GCN 21345) with OSIRIS at the 10.4m GTC telescope in La Palma (Spain). Observations consisted in several short exposures in i and z filters. The observations were not easy, as the field was located 30 deg away from the 68% illuminated Moon, implying a very high background. In the combined z-band frame, with mean epoch at 05:10:24 UT (16.75 hr after the burst) we detect a single object within the refined XRT error box (Evans et al. GCN 21341) which is not present in PanSTARRS imaging, with coordinates (J2000): R.A.: 02:17:23.99 Dec.: +01:59:29.51 and a magnitude of z(AB)=22.3+/-0.2, which we identify as the possible GRB afterglow, although we cannot make any statement about variability at this time. In our preliminary analysis we do not detect the object in any other band, implying a possible strong reddening. Further follow up, especially in NIR bands is encouraged.
GCN 21347 table
GRB_name GRB170714A
GCN_number 21347
Detection_method Swift-BAT Det
ra 34.3220°
decl 1.9620°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21347 SUBJECT: GRB 170714A, Swift-BAT refined analysis DATE: 17/07/15 15:32:14 GMT FROM: Amy Lien at GSFC D. M. Palmer (LANL), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), A. D'Ai (INAF-IASFPA), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-239 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 170714A (trigger #762535) (D'Ai et al., GCN Circ. 21340). The BAT ground-calculated position is RA, Dec = 34.322, 1.962 deg which is RA(J2000) = 02h 17m 17.3s Dec(J2000) = +01d 57' 43.3" with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment). The partial coding was 61%. The mask-weighted light curve shows continuous weak emission that starts at ~ T-70 s and lasts beyond the end of the event data (T+963 s). The time-averaged spectrum from T-72.9 to T+464.4 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.76 +- 0.17. The fluence in the 15-150 keV band is 2.8 +- 0.3 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+262.88 sec in the 15-150 keV band is 0.4 +- 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/762535/BA/
GCN 21350 table
GRB_name GRB170714A
GCN_number 21350
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 21350 SUBJECT: GRB 170714A: TNG NIR observations DATE: 17/07/17 14:05:22 GMT FROM: Paolo D'Avanzo at INAF-OAB P. D'Avanzo, A. Melandri (INAF-OAB), V. D'Elia (INAF/OAR & ASI/ASDC), G. Mainella, W. Boschin (INAF-TNG) report on behalf of the CIBO collaboration: We observed the field of GRB 170714A (D'Ai et al. GCN 21340) with the 3.6m Telescopio Nazionale Galileo (TNG) equipped with NICS. Observations were carried out in the near-infrared with the J filter under poor weather conditions (clouds and calima). Observations started on Jul 16 at 04:05:03 UT (~1.65 days after the burst) and consisted in a series of images for a total exposure time of 17 minutes. No source is detected in the refined XRT error circle (Evans et al. GCN 21341). In particular we could not detect the candidate afterglow reported by de Ugarte Postigo et al. (GCN. 21346). For the coadded image we estimate a preliminary 3sigma upper limit of J > 19.6 mag (AB, calibrated against the 2MASS catalogue).
GCN 21351 table
GRB_name GRB170714A
GCN_number 21351
Detection_method Swift-UVOT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 21351 SUBJECT: GRB 170714A: Swift/UVOT Observations DATE: 17/07/17 19:28:04 GMT FROM: Frank Marshall at GSFC F. E. Marshall (NASA/GSFC) and A. D'Ai (INAF-IASFPA) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 170714A 384 s after the BAT trigger (D'Ai et al., GCN Circ. 21340). There is weak evidence for a fading source consistent with the position of the z-band afterglow candidate reported by de Ugarte Postigo et al. (GCN Circ. 21346). Preliminary detections and 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag v 384 1695 175 >18.6 b 496 1644 155 20.0 +/- 0.33 b 5390 24672 1011 >20.3 u 471 1619 284 20.1 +/- 0.35 u 5185 30412 2351 20.4 +/- 0.18 u 81432 92912 1509 >20.7 w1 446 1594 136 >21.0 m2 6006 29000 2637 >20.9 w2 5596 34449 3032 >22.0 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.03 in the direction of the burst (Schlegel et al. 1998). [GCN OPS NOTE(17jul17): Per author's request, please see GCN Circ 21353 for corrections to the above table.]
GCN 21352 table
GRB_name GRB170714A
GCN_number 21352
Detection_method VLA Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 21352 SUBJECT: GRB170714A: VLA Observations of the Bastille Day Ultra-long Burst DATE: 17/07/17 19:51:14 GMT FROM: Assaf Horesh at Hebrew U, Jerusalem A. Horesh (HUJI), S. B. Cenko (NASA/GSFC), A. Levan (U. Warwick), and N. Tanvir (U. Leicester) report: We observed the ultra-long gamma-ray burst (T90 > 1000s; D’Ai et al. GCN 21340; Evans et al. GCN 21341; Kann et al. GCN 21345; Palmer et al. GCN 21347) with the Jansky Very Large Array (VLA). Our observation was undertaken on 2017 July 16 in the C configuration. We do not detect radio emission at the enhanced XRT position of the source, with a 3 sigma detection limit of 75 micro-Jy at a central frequency of 7.5 GHz. Future VLA observations are planned under our program to search for late-time emission. We thank the VLA staff for scheduling this target of opportunity.
GCN 21353 table
GRB_name GRB170714A
GCN_number 21353
Detection_method Swift-UVOT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 21353 SUBJECT: Correction to GCN Circular 21351: GRB 170714A: Swift/UVOT Observations DATE: 17/07/17 21:37:38 GMT FROM: Frank Marshall at GSFC F. E. Marshall (NASA/GSFC) reports on behalf of the Swift/UVOT team: Some of the Swift UVOT exposures of GRB 170714A previously reported by Marshall and D'Ai (GCN Circular 21351) contain readout streaks due to nearby bright sources. These streaks make the determination of magnitudes very difficult, and this effect was not accounted for in the previous analysis. The affected exposures have been removed from the corrected table given below. As a result, the most significant detection of a source with UVOT has been removed, and there is now only weak evidence for a UVOT source at the position of the z-band afterglow candidate reported by de Ugarte Postigo et al. (GCN Circ. 21346). Preliminary detections and 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag v 397 1695 175 >18.6 b 496 1644 155 20.0 +/- 0.33 b 92917 93309 382 >20.3 u 471 1619 284 20.1 +/- 0.35 u 81432 92912 1509 >20.7 w1 446 1594 136 >21.0 m2 76276 98985 2438 >21.3 w2 74458 86274 1771 >21.5 I apologize for any confusion caused by the earlier report.
GCN 21356 table
GRB_name GRB170714A
GCN_number 21356
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 21356 SUBJECT: GRB 170714A: NOEMA non-detection of the Bastille Day Burst DATE: 17/07/18 14:30:07 GMT FROM: Antonio de Ugarte Postigo at IAA-CSIC A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), D.A. Kann (HETH/IAA-CSIC), S. Schulze (Weizmann Institute), L. Izzo, C.C. Thoene (HETH/IAA-CSIC) and M. Krips (IRAM) report: We observed the field of GRB 170714A (D'Ai et al. GCN 21340) using the NOrthern Extended Millimeter Array (NOEMA, Plateau de Bure, France) tuned at 92.5 GHz. Observations were performed between 3:10 and 5:15 UT on 17 July 2017 (2.66 days after the burst) and consisted of 1.33 hr on target with a bandwidth of 3.6 GHz and using 8 antennas. We do not detect any source consistent with the afterglow position (de Ugarte Postigo et al. GCN 21346) down to a 3-sigma limit of 150 uJy. We do note the presence of an unrelated source 12” Northwest of the afterglow position with a flux density of ~0.19 mJy, which is coincident with an extended source in our GTC images. This burst has been proposed to be either an ultra-long GRB or a relativistic tidal-disruption event (Kann et al., GCN 21345). We note that this deep non-detection, together with the non-detection from the VLA (Horesh et al. GCN 21352) are consistent with a scenario of an ULGRB like GRBs 101225A, 111209A and 130925A, which have been faint at radio wavelengths (Frail, GCN 11550, Zauderer et al., GCN 11770; Hancock et al., GCNs 12664, 12804; Horesh et al. 2015, ApJ, 812, 86). Relativistic tidal-disruption events such as Sw J1644 and SwJ2058 have been found to be much brighter in radio wavelengths (e.g., Zauderer et al. 2011, Nature, 476, 425, Berger et al. 2012, ApJ, 748, 36, Zauderer et al., 2013, ApJ, 767, 152; Cenko et al. 2012, ApJ, 753, 77).
GCN 21359 table
GRB_name GRB170714A
GCN_number 21359
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 21359 SUBJECT: GRB 170714A: Bastille Day Burst redshift from OSIRIS/GTC DATE: 17/07/21 06:36:26 GMT FROM: Antonio de Ugarte Postigo at IAA-CSIC A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), D.A. Kann, L. Izzo, C.C. Thoene (HETH/IAA-CSIC), G. Lombardi S. Geier (GTC, IAC-ULL), A. Garcia, A. Perez (GTC) report: Following the detection of the afterglow (de Ugarte Postigo et al. GCN 21346) of the ultra-long GRB 170714A (D'Ai et al. GCN 21340, Kann et al. GCN 21345) we obtained further NIR and optical observations on 19 and 20 of July, with detections in r, i, z, and H-bands. An object is still observed at the position earlier reported, indicating an important host galaxy contribution. On 21 July, at 4:53 UT (5.69 days after the burst) we obtained spectroscopy of the afterglow/host galaxy with OSIRIS at the 10.4m GTC telescope (La Palma, Spain). Observations consisted of 4x900 s with grism R1000R, covering the range between 5100 and 10000 AA. The combined spectrum shows a weak trace with several superimposed emission lines, which we interpret as due to [OII], [OIII] and H-beta, through which we derive a redshift for the host galaxy, and hence for GRB 170714A, of 0.793.
GCN 21360 table
GRB_name GRB170714A
GCN_number 21360
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 21360 SUBJECT: GRB170714A: ATCA observation DATE: 17/07/22 22:50:47 GMT FROM: Luigi Piro at INAF R. Ricci (INAF/IRA-Bologna), M. Wieringa (ATNF,CSIRO), L. Piro(INAF/IAPS), E. Troja(NASA/GSFC), K. Bannister (ATNF,CSIRO) and B. Gendre (Virgin Islands University) report: We observed the ultra-long gamma-ray burst GRB170714A (D'Ai' et al. GCN 21340; Evans et al. GCN 21341; Kann et al. GCN 21345; Palmer et al. GCN 21347) with ATCA on 2017 July 20 at 17 and 21 GHz. We detect a source ~7" northward of the position of the GRB optical counterpart (de Ugarte Postigo et al. GCN 21346). Given the ATCA configuration, this position is consistent at about 2.5 sigma with the GRB optical counterpart. However, we cannot exclude contamination from the source detected at higher frequency by NOEMA (de Ugarte Postigo et al., GCN 21356), thus we conservatively estimate an upper limit of ~ 50uJy at 19GHz to the radio emission from the GRB. Future ATCA observations are planned under our program on ultralong GRBs (PI:L. Piro). We thank the ATCA staff for scheduling this target of opportunity.
GCN 21379 table
GRB_name GRB170714A
GCN_number 21379
Detection_method Optical
ra 34.3501°
decl 1.9913°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21379 SUBJECT: GRB170714A: XMM observation of the afterglow DATE: 17/07/29 08:33:11 GMT FROM: Luigi Piro at INAF B. Gendre (UVI, USA), L. Piro (IAPS/INAF, Italy), E. Troja (GSFC, USA), R. Ricci (INAF/IRA-Bologna), M. Wieringa (ATNF,CSIRO), K. Bannister (ATNF,CSIRO) report: We observed the field of GRB 170714A (D'Ai et al., GCN 21340) with XMM-Newton between 370,993 and 506,293 seconds post-trigger under our XMM program on ultralong GRBs (PI: Piro). The X-ray afterglow is clearly visible during the whole observation, at the position: RA: 2h17m24.02s DEC: +1d59'28.51" with an error of 1.3" (statistic + systematic, 90% confidence), consistent with the position of the optical counterpart (de Ugarte Postigo et al. GCN 21346) and of XRT (Evans et al. GCN 21341). The observed mean X-ray flux(0.3-10 keV) is 3.7e-14 erg/s/cm2 We thank the ESA and XMM SOC staff for performing this TOO trigger.
GCN 21396 table
GRB_name GRB170714A
GCN_number 21396
Detection_method Swift-XRT Other
ra 34.3499°
decl 1.9916°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21396 SUBJECT: GRB 170714A: Chandra observations DATE: 17/07/31 12:35:17 GMT FROM: Eleonora Troja at GSFC E. Troja (NASA/UMCP), L. Piro (INAF/IASF), B. Gendre (UVI) report on behalf of a larger collaboration: We observed the field of the ultralong GRB 170714A (D'Ai et al., GCN 21340) with the Chandra X-ray Observatory beginning on 2017 Jul 28.67 UT (14 days post-burst) for a total exposure of 14.9 ks. We clearly detect the GRB counterpart with coordinates: RA(J2000) = 02:17:23.97 Dec(J2000) = +01:59:29.72 with a 68% uncertainty of 0.5 arcsec. This position is consistent with the XRT position (http://www.swift.ac.uk/xrt_positions/00762535/), and the optical source reported by de Ugarte Postigo et al. (GCN 21346). By adopting the spectral parameters of the Swift/XRT analysis (D'Avanzo et al., GCN 21343), we estimate an average X-ray flux of ~1.1E-14 erg/cm2/s during our observation. This is consistent with a late-time power-law decay of slope ~-1. We thank Andrea Prestwich, Belinda Wilkes and the CXC staff for rapidly scheduling this observation.
GCN 21424 table
GRB_name GRB170714A
GCN_number 21424
Detection_method Optical
ra 34.3498°
decl 1.9925°
Circular_text TITLE: GCN CIRCULAR NUMBER: 21424 SUBJECT: GRB 170714A: ATCA detection of the radio counterpart DATE: 17/08/08 13:13:31 GMT FROM: Luigi Piro at INAF L. Piro(INAF/IAPS), R. Ricci (INAF/IRA-Bologna), M. Wieringa (ATNF,CSIRO), E. Troja(NASA/GSFC), K. Bannister (ATNF,CSIRO) and B. Gendre (UVI, USA) report: We carried out a second observation of our monitoring campaign of the field of the ultralong GRB 170714A (D'Ai' et al. GCN 21340; Evans et al. GCN 21341; Kann et al. GCN 21345; Palmer et al. GCN 21347) with ATCA on 2017 Aug 4 for 9 hours at 17 and 21 GHz. We detect a source at: RA: 02h17m23.96s Dec: +01:59'32.9" with a 90% error of ~2.5" in DEC and ~0.1" in RA, consistent with the position of the GRB X-ray counterpart by Chandra (Troja et al. GCN 21396) and the optical source reported by de Ugarte Postigo et al. (GCN 21346). We associate this source to the radio afterglow of the burst. The flux measured at 19 GHz is 71 +/- 19 uJy. In comparison to the first ATCA observation (Ricci et al. GCN 21360), the present configuration improves significantly the resolution and allows us to distinguish the radio afterglow from the unrelated source associated to the NOEMA observation (de Ugarte Postigo et al., GCN 21356). We thank the ATCA staff for scheduling this target of opportunity observation.
GCN 21464 table
GRB_name GRB170714A
GCN_number 21464
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 21464 SUBJECT: GRB 170714A: 15 GHz upper limits from AMI DATE: 17/08/11 17:56:56 GMT FROM: Kunal Mooley at Oxford U K. P. Mooley (Hintze Fellow, Oxford), T. D. Staley, R. P. Fender (Oxford), G. E. Anderson (Curtin), T. Cantwell (Manchester), D. Titterington, S. H. Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), K. Grainge, A. Scaife (Manchester) The AMI Large Array robotically triggered on the Swift alert for GRB 170714A (D'Ai et al., GCN 21340) as part of the 4pisky program, and subsequent follow up observations were obtained up to 10 days post-burst. Our observations at 15 GHz on 2017 Jul 15.11, Jul 18.27, Jul 20.23 and Jul 22.25 (UT) do not reveal any radio source at the XRT location (Evans et al., GCN 21341), with 3sigma upper limits of 279 uJy, 172 uJy, 288 uJy and 210 uJy respectively. These upper limits are consistent with the results from previously-reported radio observations (Horesh et al., GCN 21352; Ricci et al., GCN 21360; Piro et al., GCN 21424). We thank the AMI staff for scheduling these observations. The AMI-GRB database is a log of all GRB follow up observations with the AMI, and is available at http://4pisky.org/ami-grb/.