| Summary table |
|---|
| Variable |
Value |
Source |
| GRB_name_Fermi |
GRB100401297 |
|
| T0 |
7:07:25.585 UTC |
Fermi_GBM |
| ra |
290.8130° |
Swift |
| decl |
-8.2570° |
Swift |
| pos_error |
1.55e-02° |
Swift |
| T90 |
92.416 s |
Fermi_GBM |
| T90_error |
4.291 s |
Fermi_GBM |
| T90_start |
7:07:25.585 UTC |
Fermi_GBM |
| fluence |
1.90e-06 erg/cm² |
Fermi_GBM |
| fluence_error |
2.76e-08 erg/cm² |
Fermi_GBM |
| T100 |
92.416 s |
|
| GBM_located |
False |
|
| mjd |
55287.29682390046 |
Fermi_GBM |
| Fermi GBM table |
|---|
| GRB_name_Fermi |
GRB100401297 |
| trigger_name |
bn100401297 |
| ra |
290.8000° |
| decl |
-8.3000° |
| pos_error |
6.79e+00° |
| datum |
2010-04-01 |
| t_trigger |
7:07:32.241 UTC |
| T90 |
92.416 s |
| T90_error |
4.291 s |
| T90_start |
7:07:25.585 UTC |
| fluence |
1.90e-06 erg/cm² |
| fluence_error |
2.76e-08 erg/cm² |
| flux_1024 |
4.08e+00 erg/cm²/s |
| flux_1024_error |
2.08e-01 erg/cm²/s |
| flux_1024_time |
-1.28e-01 erg/cm²/s |
| flux_64 |
6.01e+00 erg/cm²/s |
| flux_64_error |
1.11e+00 erg/cm²/s |
| IPN table |
|---|
| GRB_name |
GRB100401A |
| ra |
290.8125° |
| decl |
-8.2500° |
| pos_error |
3.33e-02° |
| Swift table |
|---|
| GRB_name |
GRB100401A |
| t_trigger |
7:07:31.900 UTC |
| ra |
290.8130° |
| decl |
-8.2570° |
| pos_error |
1.55e-02° |
| GCN 10567 table |
|---|
| GRB_name |
GRB100401A |
| GCN_number |
10567 |
| Detection_method |
Swift-BAT Det |
| ra |
290.8130° |
| decl |
-8.2570° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 10567
SUBJECT: GRB 100401A Burst, possibly short, detected in ground analysis of BAT data
DATE: 10/04/02 19:57:49 GMT
FROM: Jay R. Cummings at NASA/GSFC/Swift
J. R. Cummings (GSFC/UMBC), N. Gehrels (NASA/GSFC), F. E. Marshall (NASA/GSFC)
on behalf of the Swift team
At 2010-04-01T07:07:31.9 BAT detected a rate increase (trigger# 417974).
The source was found with insufficient significance onboard to trigger
an automated burst response. A significant source was found in ground
analysis at RA, Dec 290.813, -8.257, which is:
RA (J2000) 19h 23m 15.5s
Dec (J2000) -08d 15' 25"
with an estimated uncertainty of 2 arcmin radius (90% containment). The
source was 10% coded in the BAT field of view.
As seen in BAT, the burst had a single square-shaped pulse of about
2 seconds duration.
The spectrum from 15 to 150 keV is best fit by a simple power law function
with a photon index of 1.7 +- 0.2. We note that this is softer than is
typical for "short, hard" GRBs. The fluence was (3.6 +- 1.2) erg/cm2. The
1-second peak flux was 2.4 photons/cm2.
Since this burst was not detected with sufficient significance onboard,
there are no automated data products. A Swift TOO is in progress.
|
| GCN 10568 table |
|---|
| GRB_name |
GRB100401A |
| GCN_number |
10568 |
| Detection_method |
Fermi GBM Det |
| t_trigger |
7:07:32.240 UTC |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 10568
SUBJECT: GRB 100401A: Fermi GBM detection
DATE: 10/04/02 22:59:08 GMT
FROM: Adam Goldstein at Fermi-GBM/UAH
A. Goldstein (UAH) and D. Gruber (MPE)
report on behalf of the Fermi GBM Team:
"At 07:07:32.24 UT on 1 April 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 100401A (trigger 291798454 / 100401297)
which was also detected by the Swift-BAT (J.R. Cummings et al. 2010,
GCN 10567). The GBM on-ground location is consistent with the
Swift-BAT position. The angle from the Fermi LAT boresight is 45 degrees.
The GBM light curve consists of an initial bright pulse at trigger time
lasting ~4 s followed by a second, much softer pulse of ~30 s in duration,
approximately 65 s after trigger time. The total duration (T90) is
estimated to be about 100 s (8-1000 keV). The time-averaged spectrum of
the first pulse from T0-1.9 s to T0+3.2 s is best fit by a power law
function with an exponential high energy cutoff. The power law index is
-1.49 +/- 0.17 and the cutoff energy, parameterized as Epeak, is
144.90 +/- 62.20 keV (chi squared 439 for 483 d.o.f.). The first
pulse is equally well fit by a simple power law with index
-1.77 +/- 0.06 (chi squared 444 for 484 d.o.f.). The
time-averaged spectrum of the second pulse from T0+74.9 s to
T0+98.4 s is well fit by a power law function with an exponential
high energy cutoff. The power law index is -1.52 +/- 0.39 and
the cutoff energy, parameterized as Epeak, is 29.34 +/- 8.96 keV
(chi squared 511 for 483 d.o.f.). The second pulse is equally well
fit by a simple power law with index -2.16 +/- 0.11 (chi squared
514 for 484 d.o.f.).
The event fluence (8-1000 keV) over the entire emission is
(2.39 +/- 0.05)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-1.4 s in the 8-1000 keV band
is 3.61 +/- 0.16 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
|
| GCN 10569 table |
|---|
| GRB_name |
GRB100401A |
| GCN_number |
10569 |
| Detection_method |
Swift-XRT Other |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 10569
SUBJECT: Swift/BAT trigger 417974 (GRB100401A): Swift/XRT observations
DATE: 10/04/03 00:55:02 GMT
FROM: Valerio D'Elia at ASDC
G. Stratta and V. D'Elia (ASDC) report on behalf of the Swift Team:
Swift began a target of opportunity observation of
GRB 100401A detected on ground (Cummings et al., GCN #10567)
and by the Fermi/GBM (Goldstein and Gruber, GCN #10568), at
19:33:04 UT on April 2nd, 2010, approximately 36.4 hours after the
Swift/BAT trigger. In about 2 ks of Photon Counting
mode data, no X-ray source is detected inside the BAT
error circle.
This circular is an official product of the Swift-XRT team.
----------------------------------------------------------------
This message was sent using IMP, the Internet Messaging Program.
|
| GCN 10570 table |
|---|
| GRB_name |
GRB100401A |
| GCN_number |
10570 |
| Detection_method |
Swift-UVOT Other |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 10570
SUBJECT: GRB 100401A: Swift/UVOT Upper Limit
DATE: 10/04/03 04:46:02 GMT
FROM: Margaret Chester at PSU
M.M. Chester (PSU) and G. Stratta (ASDC) report on behalf of the
Swift/UVOT team:
Swift began a Target of Opportunity observation of GRB 100401A,
detected by Swift/BAT (Cummings et al., GCN Circ. 10567) and by
Fermi/GBM (Goldstein and Gruber, GCN Circ. 10568), on April 2nd,
2010 at 19:33:04 UT, approximately 36 hours after the Swift/BAT
trigger.
No optical afterglow consistent with the BAT position is detected
in the UVOT exposure. The 3-sigma upper limit using the UVOT
photometric system (Poole et al. 2008, MNRAS, 383, 627) is:
Filter T_start(s) T_stop(s) Exp(s) 3-sig UL (mag)
u 131128 133123 1963 >20.8
The value quoted above is not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.29 in the direction of the burst
(Schlegel et al. 1998).
|
| GCN 10577 table |
|---|
| GRB_name |
GRB100401A |
| GCN_number |
10577 |
| Detection_method |
GROND |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 10577
SUBJECT: GRB100401A: GROND Upper Limits
DATE: 10/04/04 23:41:40 GMT
FROM: Paulo M. J. Afonso at MPE
SUBJECT: GRB100401A, GROND Upper Limits
A. Updike (Clemson University), A. Rau, P. Afonso and J. Greiner (all
MPE Garching) report on behalf of the GROND team:
We observed the field of GRB 100401A (Cummings et al., GCN #10567,
Goldstein and Gruber, #GCN 10568) simultaneously in g'r'i'z'JHK with
GROND (Greiner et al. 2008,PASP 120, 405), mounted at the 2.2m ESO/MPI
telescope at La Silla Observatory (Chile).
Observations started on 2010, April 3, at 09:21 UT, 2.09 days after the
burst, and consisted of 20 min in JHK and 24.6 min in g'r'i'z'. A second
epoch was obtained on 2010, April 4, at 09:09 UT, 2.99 days after the burst.
Image subtraction of the two epochs does not reveal a variable source,
down to the following 1st epoch limiting magnitudes (all in AB system):
g' > 23.7
r' > 23.9
i' > 23.4
z' > 23.4
J > 21.8
H > 21.4
K > 20.3
These magnitudes were obtained using 2MASS field stars and GROND
zero-points as reference, and are not corrected for the Galactic
extinction due to the reddening of E(B-V) = 0.29 mag in the direction of
the burst (Schlegel et al. 1998).
|