| Summary table |
|---|
| Variable |
Value |
Source |
| T0 |
23:51:40 UTC |
GCN_circulars,INTEGRAL |
| ra |
248.6042° |
IPN |
| decl |
-51.8000° |
IPN |
| pos_error |
5.00e-02° |
IPN |
| GBM_located |
False |
|
| mjd |
59045.99421296296 |
GCN_circulars,INTEGRAL |
| IPN table |
|---|
| GRB_name |
GRB200715A |
| ra |
248.6042° |
| decl |
-51.8000° |
| pos_error |
5.00e-02° |
| GCN 28110 table |
|---|
| GRB_name |
GRB200715A |
| GCN_number |
28110 |
| Detection_method |
INTEGRAL |
| t_trigger |
23:51:40 UTC |
| ra |
248.5372° |
| decl |
-51.8392° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 28110
SUBJECT: GRB 200715A : A long GRB detected by INTEGRAL
DATE: 20/07/16 01:45:01 GMT
FROM: Sandro Mereghetti at IASF-Milano/INAF
S.Mereghetti (INAF, IASF-Milano), D.Gotz (CEA, Saclay), E.Bozzo,
C.Ferrigno, V.Savchenko (ISDC, Versoix), L.Ducci (IAAT, Germany and ISDC,
Versoix) and J.Borkowski (CAMK, Torun) report:
a gamma ray burst lasting about 160 s has been detected by IBAS in the
IBIS/ISGRI data at 23:51:40 UT of July 15, 2020.
The refined coordinates (J2000) are:
R.A.= 248.5372 deg
DEC.= -51.8392 deg
with an uncertainty of 1.5 arcmin (90% c.l.).
Due to telemetry saturation, we can provide only lower limits to its peak
flux and fluence.
The peak flux is greater than 1.2 ph/cm2/s (20-200 keV, 1-s integration
time) and the fluence in the same energy range is greater than 1.8e-6
erg/cm2.
A plot of the light curve will be posted at
http://ibas.iasf-milano.inaf.it/IBAS_Results.html
|
| GCN 28111 table |
|---|
| GRB_name |
GRB200715A |
| GCN_number |
28111 |
| Detection_method |
Swift Other |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 28111
SUBJECT: GRB 200715A: Swift ToO observations
DATE: 20/07/16 01:48:23 GMT
FROM: Phil Evans at U of Leicester
P. A. Evans (U. Leicester) reports on behalf of the Swift team:
Swift has initiated a ToO observation of the INTEGRAL GRB 200715A.
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021018
Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. These are
not necessarily related to the INTEGRAL event. Any X-ray source
considered to be a probable afterglow candidate will be reported via a
GCN Circular after manual consideration.
Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).
This circular is an official product of the Swift-XRT team.
|
| GCN 28115 table |
|---|
| GRB_name |
GRB200715A |
| GCN_number |
28115 |
| Detection_method |
Swift-XRT Other |
| ra |
248.5377° |
| decl |
-51.8356° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 28115
SUBJECT: GRB 200715A: Swift-XRT afterglow detection
DATE: 20/07/16 08:44:31 GMT
FROM: Kim Page at U.of Leicester
A. D'Ai (INAF-IASFPA), D.N. Burrows (PSU), J. D. Gropp (PSU), J.A.
Kennea (PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.
Melandri (INAF-OAB), T. Sbarrato (INAF-OAB) and P.A. Evans (U.
Leicester) report on behalf of the Swift-XRT team:
Swift-XRT has performed follow-up observations of the INTEGRAL-detected
burst GRB 200715A (Mereghetti et al. GCN Circ. 28110), collecting 3.3
ks of Photon Counting (PC) mode data between T0+7.5 ks and T0+26.2 ks.
An uncatalogued X-ray source is detected consistent with being within
266 arcsec of the INTEGRAL position and is above the RASS limit, and is
therefore likely the GRB afterglow. The position of this source is RA,
Dec=248.5377, -51.8356 which is equivalent to:
RA (J2000): 16:34:9.04
Dec(J2000): -51:50:08.0
with an uncertainty of 3.7 arcsec (radius, 90% confidence). This
position is 13 arcsec from the INTEGRAL position (Mereghetti et al. GCN
Circ. 28110).
The light curve can be modelled with a power-law decay with a decay
index of alpha=1.06 (+0.32, -0.27).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.1 (+/-0.5). The
best-fitting absorption column is 1.06 (+0.60, -0.29) x 10^22 cm^-2,
consistent with the Galactic value of 7.6 x 10^21 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum is 4.8 x 10^-11 (9.4 x
10^-11) erg cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 1.06 (+0.60, -0.29) x 10^22 cm^-2
Galactic foreground: 7.6 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index: 2.1 (+/-0.5)
If the light curve continues to decay with a power-law decay index of
1.06, the count rate at T+24 hours will be 6.2 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.0 x
10^-13 (5.8 x 10^-13) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00021018.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/00021018.
This circular is an official product of the Swift-XRT team.
|