February 22 2011: New Alert type for low significance triggers

A new version of the IBAS Alert Distribution system is operational at the INTEGRAL Science Data Center. In addition to the already available functionalities, the new version distributes in real time also Alert Packets for low significance triggers discovered in the field of view of the IBIS imager. The new Alert Packets are called WEAK Alerts and are identified by the field PKT_TYPE=6

Many WEAK alerts will be produced by statistical fluctuations, but there is also a non negligible probability that some of them are due to real astrophysical events. In most cases it is not possible to recognize the GRBs based only on the INTEGRAL data, but the detection of afterglows could confirm some of these events as genuine GRBs.

Several bursts that were confirmed by off-line interactive analysis of the INTEGRAL data produced triggers above the threshold currently adopted for the WEAK alerts. Recent examples include the two short bursts GRB 100703A and GRB 110112B and the long burst GRB 100909A .

WEAK Alert Packets provide a single sky position, with error radius smaller than 4 arcmin. They are intended for robotic telescopes which can react without a negative impact on scheduled observing programmes. The value of SIGMA in the WEAK Alert Packet can be used as a figure of merit.

WEAK Alert Packets may or may not be followed by the usual WAKEUP and/or REFINED Alert Packets, depending on the evolution of the detected signal. WEAK alerts for events belows WAKEUP threshold are neither confirmed nor cancelled with an OFFLINE packet.

The threshold for the distribution of the high significance IBAS triggers remains unchanged at

SIGMA= 8.0 (Alert Packets with PKT_TYPE= 3 (WAKEUP))

while the threshold for the distribution of low significance IBAS triggers is currently set at

SIGMA= 6.5 (Alert Packets with PKT_TYPE= 6 (WEAK))

This threshold corresponds to a rate of a few WEAK Alert Packets per week, but it could be adjusted in the future.

It is recommended that current ibas clients upgrade their IBAS Client Software to the version 2.1.0 (available here) although the previous versions should process WEAK alert without problems.

For more information contact Sandro Mereghetti (sandro at iasf-milano.inaf.it)

July 26 2005: IBAS Server IP Adress Change

As a result of a major network restructuring at the University of Geneva, the IBAS alert server IP address changed from (current IP address)
to (new IP address)

The change took place during INTEGRAL's perigee passage #0339 on July 26 2005.

Apr 19 2005: Change in policy on GRB results

Swift has opened a new era in data right policies: all the Swift GRB data are public and the information derived by the teams of the Swift instruments is immediately disseminated through GCN circulars.
The IBAS Team, supported by several scientists of the GRB community, proposed that a similar policy be applied to all the INTEGRAL GRB data. This issue was discussed by the members of the INTEGRAL Science Working Team (ISWT) who could not approve it since that would violate the rights of accepted guest observers proposals.
However, the ISWT allowed to quickly release more information resulting from the IBAS off-line analysis. The PI's with accepted AO3 proposals on GRBs agreed with this new policy. Following this decisions, in addition to the results distributed for INTEGRAL GRBs up to now (position, duration and peak flux), also the total fluence, peak energy (if it can be determined) and light curve (in the 20-200 keV) will be communicated by the IBAS Team as soon as they can be derived.

Mar 2005: Long lasting emission after the SGR 1806-20 Giant Flare: a gamma-ray afterglow ?

Many satellites observed the December 27 Giant Flare and provided a wealth of new results, such as the burst spectrum, the determination of the total emitted energy (SPI-ACS could provide only a lower limit due to the saturation of the instrument) and the pulse shape of the tail (e.g. Hurley et al. 2005 (RHESSI); Palmer et al. 2005 (Swift)). The SPI-ACS, however, has two advantages compared to the other satellites: its large effective area above 80 keV and the INTEGRAL orbit which allows for long uninterrupted observations. Thanks to these unique properties, the ACS was able to measure a second component after the pulsating tail (t > 400 s). As visible in the figure (yellow: instrumental background, red: Flare tail, blue: high-energy afterglow), the count rate increased again, forming a long bump which peaked around t~700 s and returned to the pre-flare background level at t~3000-4000. The most likely association of this long lasting component to SGR 1806-20 is discussed in a Letter recently accepted for publication in The Astrophysical Journal (Mereghetti et al. 2005).

After accounting for the background, estimated from a linear fit to the ACS count rate for t<0 s and t>4000 s, the time profile decay in the interval t=500-4000 s can be reasonably well described by a power law F~t-0.85. The fluence in the 400-4000 s time interval is 1.6x1044 erg for E>3 keV, approximately equal to that contained in the pulsating tail (assuming a distance of 15 kpc).
The Giant Flare from SGR 1806-20, behaves in many respect as a scaled down version of a GRB. An afterglow, due to interaction of the relativistically ejected material with the surrounding medium, is expected, and it has indeed been observed in the radio band (Cameron et al. 2005, Gaensler et al. 2005). It is likely that the long lasting emission detected with the ACS is the early part of this afterglow, seen here for the first time in the hard X-ray / soft gamma-ray band (E>80 keV).

Jan 2005: GRB 041219A prompt IR flash

The case of GRB 041219A demonstrates once more that INTEGRAL GRBs can be very interesting: thanks to the rapid IBAS localization of this long lasting burst, the RAPTOR automatic telescope could observe it in the optical simultaneously with the gamma-ray emission. This is only the second burst for which the prompt optical emission has been observed. Surprisingly the properties in the optical of these two bursts are very different (see the paper by Vestrand et al. 2005 to appear in Nature). GRB 041219A was also seen by Swift, which had been launched just one month earlier, but was not yet distributing localizations in real time.

Dec 27 2004: Giant Flare from SGR 1806-20

The first Giant Flare from the soft gamma-ray repeater SGR 1806-20 has been discovered with INTEGRAL on December 27 (see GCN Circ. 2920).
The IBAS programs monitoring the light curves of the SPI ACS triggered on a short event at 21:28:02 UT (see light curve ) also seen by Konus-Wind (GCN Circ. 2922). About 143 seconds later a rapid increase in the SPI ACS count rate was detected.

In less than 150 msec the flux reached a peak count rate of 2x10^6 counts/s (compared to a background level of 88,000 counts/s ). The initial spike, lasting about 1.5 s, was followed by a long tail in which pulsations at 7.57 s are clearly detected.
SPI ACS 1806-20 Light Curve

The flux decline is well fit by an exponential with decay time of about 80 s. Variations in the shape of the pulse profile are also visible.

Nov 30 2004:

A new version of the IBAS alert distribution system has been recently implemented at the ISDC. This new version has the capability to distribute Alert Packets for different classes of sources which trigger the GRB detection programs.

The IBAS users interested in alerts from non-GRB sources should register at the ISDC Web pages in order to select the classes of sources of interest. They can also download a new version of the IBAS Client Software (although not stricly needed, this will allow them to fully exploit the new information in the Alert Packets for non-GRB sources).

The IBAS users interested in Alerts only for Gamma-Ray Bursts will continue to receive them, without the need of installing the new version of the IBAS Client Software.

Up to now the following source classes have been defined:

A list of the sources included by IBAS in these classes can be seen below. The new Alert Packets will contain the source name and type in the comment field. They will also include an extra field containing the source type number. Backward compatibility with old versions of the IBAS Client is ensured. For further details see the IBAS Client 2.0.0 User Manual.

Future developments will include the possibility to receive Alert Packets for ''GRB candidates'', i.e. the triggers which are currently sligthly below the significance threshold for automatic alert delivery.

Source List

Type I and II X-ray bursters

Source NameR.A. (J2000)Dec.(J2000)
4U_0512-401 05:14:06.6 -40:02:37.0
4U_0614+091 06:17:07.3 +09:08:13.0
EXO_0748-676 07:48:33.8 -67:45:09.0
SAX_J0835.9+5118 08:35:56.0 +51:18:36.0
MX_0836-429 08:37:23.6 -42:54:02.0
4U_1254-690 12:57:37.2 -69:17:21.0
4U_1323-619 13:26:36.1 -62:08:10.0
Cen_X-4 14:58:22.0 -31:40:08.0
Cir_X-1 15:20:40.9 -57:10:01.0
SAX_J1603.9-7753 16:03:54.0 -77:53:06.0
4U_1608-522 16:12:43.0 -52:25:23.0
4U_1636-536 16:40:55.5 -53:45:05.0
1658-298 17:02:06.3 -29:56:45.0
4U_1702-429 17:06:15.3 -43:02:10.0
4U_1705-440 17:08:54.7 -44:06:02.0
XTE_J1709-267 17:09:30.2 -26:39:27.0
SAX_J1712.6-3739 17:12:34.0 -37:38:36.0
2S_1715-321 17:18:47.4 -32:10:40.0
RXS_J171824.2-402934 17:18:24.1 -40:29:30.4
XTE_J1723-376 17:23:38.0 -37:39:42.0
1724-307 17:27:33.2 -30:48:07.0
GX354-0 17:31:57.4 -33:50:05.0
Rap_Busrt(1730-335) 17:33:24.1 -33:23:16.0
KS_1731-260 17:34:13.0 -26:05:09.0
1732-304 17:35:47.6 -30:28:56.0
SLX_1735-269 17:38:16.0 -27:00:16.0
4U_1735-444 17:38:58.3 -44:27:00.0
KS_1741-293 17:44:49.0 -29:21:06.0
GRS_1741.9-2853 17:45:01.0 -28:54:06.0
A_1742-289 17:45:37.0 -29:01:07.0
A_1742-294 17:46:05.5 -29:30:54.8
SAX_J1747.0-2853 17:47:02.0 -28:52:30.0
GRO_J1744-28 17:44:33.1 -28:44:27.0
SLX_1744-300 17:47:25.9 -30:02:31.0
GX3+1 17:47:56.0 -26:33:49.0
EXO_1745-248 17:48:05.0 -24:46:47.0
4U_1746-370 17:50:12.7 -37:03:08.0
EXO_1747-214 17:50:25.7 -21:25:21.0
SAX_J1748.9-2021 17:48:53.4 -20:21:43.0
SAX_J1750.8-2900 17:50:24.0 -29:02:18.0
SAX_J1752.3-3138 17:52:24.0 -31:37:42.0
XTE_J1806-246 18:06:50.7 -24:35:29.0
SAX_J1808.4-3658 18:08:27.5 -36:58:44.3
SAX_J1810.8-2609 18:10:44.5 -26:09:01.0
GX13+1 18:14:31.1 -17:09:26.0
4U_1812-12(Ser_X-2) 18:15:12.0 -12:05:00.0
GX17+2 18:16:01.4 -14:02:11.0
4U_1820-303 18:23:40.6 -30:21:41.0
GS_1826-238 18:29:28.2 -23:47:49.1
XB_1832-330 18:35:43.6 -32:59:26.8
Ser_X-1 18:39:57.5 +05:02:09.0
4U_1850-087 18:53:04.9 -08:42:20.0
4U_1905+000 19:08:27.0 +00:10:08.0
Aql_X-1 19:11:16.0 +00:35:06.0
4U_1916-053 19:18:48.0 -05:14:09.0
XTE_J2123-058 21:23:14.5 -05:47:52.9
4U_2127+119 21:29:58.3 +12:10:03.0
4U_2129+470 21:31:26.2 +47:17:24.0
Cyg_X-2 21:44:41.2 +38:19:18.0
SAX_J1753.5-2349 17:53:34.0 -23:49:24.0
SAX_J1806.5-2215 18:06:34.0 -22:15:06.0
2S_1711-339 17:14:18.9 -34:02:57.6
SLX_1737-282 17:40:43.0 -28:18:12.0
SAX_J1324.5-6313 13:24:27.0 -63:13:24.0
SAX_J1818.7+1424 18:18:44.0 +14:24:12.0
SAX_J1828.5-1037 18:28:33.0 -10:37:48.0
SAX_J2224.9+5421 22:24:52.0 +54:21:54.0
2S_0918-549 09:20:26.7 -55:12:23.9

Soft Gamma Repeaters and Anomalous X-ray Pulsars

Source NameR.A. (J2000)Dec.(J2000)
SGR_0418+4729 04:18:34.1 +57:32:24.5
SGR_0501+4516 05:01:06.7 +45:16:34.4
SGR_0525-66 05:25:57.0 -66:07:06.0
SGR_1806-20 18:08:39.3 -20:24:39.5
SGR_1900+14 19:07:14.9 +09:19:41.9
SGR_1627-41 16:35:49.8 -47:35:44.0
SGR_1801-23 18:00:58.9 -22:56:48.5
SGR_1833-0832 18:33:44.45 -08:31:08.0
CXO_0100-7211 01:00:43.1 -72:11:33.8
4U_0142+614 01:46:22.4 +61:45:02.8
1E_1048-5937 10:50:07.1 -59:53:21.4
1E_1547.0-5408 15:50:54.1 -54:18:23.7
CXOU_J1647-45 16:47:10.2 -45:52:16.9
RXS_J1708-40 17:08:46.9 -40:08:52.4
XTE_J1810-197 18:09:51.1 -19:43:51.7
1E_1841-045 18:41:19.3 -04:56:11.2
AX_J1844-0258 18:44:53.0 -02:56:40.0
1E_2259+586 23:01:08.3 +58:52:44.5


Last modified: 22-Feb-2011

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