Soft Gamma Repeater 1900+14

This SGR was discovered first with KONUS....
...later observed with BATSE....IPN synthesis location...ROSAT source... IR sources

Previous IAU Circulars (NOT complete)

• IAUC 6929 Ulysses/KONUS-Wind location of events between May 26 - 30, 1998
• IAUC 6933 infrared observations show no variability
• IAUC 7001 pulsations of 5.16 sec with ASCA and PCA
• IAUC 7002 pulsations of 5.15 sec in large flare detected with GGS-Wind spacecraft; ASM detection
• IAUC 7003 pulsations and 10 higher flux in RXTE pointing
• IAUC 7004 large GGS-Wind flare triangulated with Ulysses; lightcurve
• IAUC 7005 triangulated with 6 spacecrafts; BeppoSAX GRBM detection
• IAUC 7023 226 ms radio pulsar at 19h07m21s.1, Decl. = +9d18'41" (+/- 2')
• IAUC 7032 89-s pulsar XTE J1906+09 is different from SGR 1900+14
• IAUC 7110 5.1 sec pulsations from PSR J1907+0919
• ApJ 510 (1999) L107 Hurley etal: Reactivation and Precise Interplanetary Network Localization of the Soft Gamma Repeater SGR 1900+14
• ApJ 510 (1999) L111 Hurley etal: ASCA Discovery of an X-Ray Pulsar in the Error Box of SGR 1900+14
• ApJ 510 (1999) L115 Kouveliotou etal: Discovery of a Magnetar Associated with the Soft Gamma Repeater SGR 1900+14
• ApJ 510 (1999) L119 Murakami etal: Accurate Position of SGR 1900+14 by Bursts and Changes in Pulse Period and Folded Pulse Profile with ASCA
• ApJ 515 (1999) L9 Feroci etal: A Giant Outburst from SGR 1900+14 Observed with the BeppoSAX Gamma-Ray Burst Monitor
• astro-ph/9905195 Mazets etal: The Activity of the Soft Gamma Repeater SGR~1900+14 in 1998 from Konus-Wind Observations: 1. Short Recurrent Bursts
• astro-ph/9905196 Mazets etal: The Activity of the Soft Gamma Repeater SGR~1900+14 in 1998 from Konus-Wind Observations: 2. The Giant August 27 Outburst
• ApJ 518 (1999) L103 BeppoSAX Observations of SGR 1900+14 in Quiescence and during an Active Period
• astro-ph/9907173 Woods etal: Variable Spin-down in the Soft Gamma Repeater SGR 1900+14 and Correlations withBurst Activity
• astro-ph/9909276 Woods etal: Hard Burst Emission from the Soft Gamma Repeater SGR 1900+14
• astro-ph/9910062 Gogus etal: Statistical properties of SGR 1900+14 bursts
• astro-ph/9912487 Feroci etal: BeppoSAX and Ulysses data on the giant flare from SGR 1900+14

• The triangulation of the May 1998 events gives a preliminary annulus whose center is at R.A. = 21h58m18s, Decl. = -11o18'.4 (equinox 2000.0), and whose radius is 47.269 +/- 0.019 deg. An image may be found at http://ssl.berkeley.edu/ipn3/sgr1900+14/.
• GCN notice #120
  A. Henden, C. Luginbuhl and F. Vrba (U.S. Naval Observatory Flagstaff Station) report that they have obtained extensive I-band and J-band observations of the near-IR sources and surrounding field associated with SGR1900+14 both before and after the recent onset of activity. None of the observations coincide with bursts detected by BATSE, and no unusual photometric behavior has been detected though reductions are ongoing. A new eclipsing binary has been detected nearby, however, at RA 19:07:16.85 DEC +09:18:50.4 (J2000), about 39.0 arcseconds SE of the M supergiant pair. The binary is about I=19.1 out of eclipse, and has been observed through several eclipses of about 0.4mag depth. The period is either about 1.07day or some integer fraction. This binary appears as the star labelled 'J' in Figure 1 of Vrba et. al. ApJ 468:225 (1996). We bring this star to the attention of other observers in the hope that it not send anyone on a wild goose chase if it is detected as a variable in observations of this gamma-ray burst location.
• GCN notice #121
  D. A. Frail, National Radio Astronomy Observatory and S. R. Kulkarni, California Institute of Technology report:
  The recent renewed activity from SGR1900+14 (GCN #94) and the newly-discovered SGR1627-41 (GCN #107) prompted VLA radio observations at 8.46 GHz on 1998 June 25. For SGR1900+14 we observed a field centered on the proposed X-ray/infrared counterpart (Hurley et al. ApJ, 463, L13, 1996, Vrba et al. ApJ, 468, 225, 1996). For SGR1627-41 we observed the 95 arcsec diameter supernova remnant CTB33 (IAU Circ. 6948), most recently studied by Sarma, Goss, Green & Frail (ApJ, 483, 335, 1997). The synthesized beam was approximately 1 arcsec. The interferometer is insensitive to extended structure on angular scales larger than 20 arcsec. No point sources were visible above 200 microJy and 345 microJy (4-sigma) for the SGR1900+14 and SGR1627-41, respectively. These interferometer observations are less sensitive to angular scales larger than 20 arcsec.
• ASCA position of the 5.16 sec pulsar (from IAUC 7001): R.A. = 19h07m14s, Decl. = +9o19'.3
• GCN notice #153
  M. Feroci, P. Soffitta, E. Costa, Istituto di Astrofisica Spaziale, CNR, Rome, and F. Frontera, Istituto Tecnologie e Studio Radiazioni Extraterrestri, CNR, Bologna, on behalf of the BeppoSAX/GRBM team, and M. Tavani, Istituto di Fisica Cosmica, CNR, Milano, and Columbia Astrophysics Laboratory, New York, report:
  The Gamma-Ray Burst Monitor (GRBM) onboard BeppoSAX was triggered by the event reported by Cline et al. (IAUC 7002) on Aug. 27.4321259. The event showed a fast rise (<1s) and an exponential-like decay, lasting more than 300s. The event was observed at an off-set angle of about 56 degrees from the axis of GRBM unit 1, and showed a peak intensity in (40-700 keV) of about 64000 c/s. The event was clearly detected above 100 keV. A preliminary analysis shows that the spectrum is hard during the initial 1s, followed by a sudden softening. Subsequent spectral evolution shows a progressive hardening. The near-5s periodicity reported by Cline et al. (IAUC 7002) is evident in the GRBM data for the entire duration of the event. In addition, starting from about 35s after the event onset, the GRBM clearly detected a periodic pattern of subpulses for each near-5s oscillation. The repetitive pattern is made of four subpulses of period near-1s.
• Ulysses lightcurve of strong flare on Aug. 27, 1998: