[vsnet-grb-info 4526] GRB 070411: TLS data shows plateau, flares
GCN Circulars
gcncirc at capella.gsfc.nasa.gov
Fri Apr 13 09:48:28 JST 2007
TITLE: GCN CIRCULAR
NUMBER: 6295
SUBJECT: GRB 070411: TLS data shows plateau, flares
DATE: 07/04/13 00:48:22 GMT
FROM: Alexander Kann at TLS Tautenburg <kann at tls-tautenburg.de>
--Alt-Boundary-493.7941328
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D. A. Kann, U. Laux, S. Klose, H. Meusinger, S. Schulze (TLS
Tautenburg) and J. Greiner (MPE, Garching) report:
The afterglow of the Swift GRB 070411 (Moretti et al., GCN
6267) was observed with the Tautenburg 1.34m Schmidt
telescope in RRM mode starting 342 seconds after the trigger
(Kann et al., GCN 6268).
A total of 18 observations were obtained before the afterglow
become unobservable. We performed aperature photometry
vs. two unsaturated and isolated USNO B1.0 stars (R1
magnitudes):
RA = 07:09:17.16, Dec. = +01:04:35.9, assuming R = 15.55
RA = 07:09:28.54, Dec. = +01:03:57.1, assuming R = 16.25
We derive the following magnitudes (mean exposure times
after the burst have been derived logarithmically):
dt Start Exposure R mag dR
(days) (SOD) (seconds)
0.0049994 73095 180 18.03 0.05
0.0076498 73324 180 18.12 0.03
0.0103234 73555 180 18.18 0.03
0.0129739 73784 180 18.17 0.05
0.0156244 74013 180 18.43 0.07
0.0182864 74243 180 18.79 0.05
0.0209485 74473 180 18.83 0.07
0.0235989 74702 180 18.95 0.08
0.0262494 74931 180 19.23 0.07
0.0288999 75160 180 19.38 0.09
0.0315503 75389 180 19.75 0.12
0.0342008 75618 180 20.00 0.16
0.0368512 75847 180 19.83 0.12
0.0395017 76076 180 19.88 0.15
0.0421522 76305 180 20.13 0.19
0.0472965 76540 600 20.64 0.23
0.0548081 77189 600 19.91 0.14
0.0623197 77838 600 19.96 0.15
Adding further R and CR data (Rykoff et al., GCN 6269,
Gomboc et al., GCN 6271, Jelinek, Nuez, & Castro-Tirado,
GCN 6272, Berger et al., GCN 6278, Mikuz, Skvarc, &
Dintinjana, GCN 6288), we find:
The afterglow may be rising early on, looking at the earliest
detections from Crni Vrh, ROTSE and Tautenburg.
The afterglow then goes over into a plateau phase (decay
alpha= 0.14 +/- 0.1). In our data, we do not see the strong
rebrightening detected by ROTSE (Rykoff et al., GCN 6269).
At 0.014 +/- 0.001 days, the afterglow breaks and begins a
decay with alpha = 1.54 +\- 0.16 up to about 0.03 days, where a
possible flare occurs.
At about 0.05 days, the afterglow seems to rebrighten strongly,
our data here are in full accordance with those of the Liverpool
telescope (Gomboc et al., GCN 6271) and the IAC80 (Jelinek,
Nuez, & Castro-Tirado, GCN 6272).
Further photometric follow-up of this GRB is warranted.
This message may be cited.
--Alt-Boundary-493.7941328
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<span style=" font-size:10pt">
D. A. Kann, U. Laux, S. Klose, H. Meusinger, S. Schulze (TLS
Tautenburg) and J. Greiner (MPE, Garching) report:</span></font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
<br />
</span>
</font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
The afterglow of the Swift GRB 070411 (Moretti et al., GCN
6267) was observed with the Tautenburg 1.34m Schmidt
telescope in RRM mode starting 342 seconds after the trigger
(Kann et al., GCN 6268).</span></font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
<br />
</span>
</font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
A total of 18 observations were obtained before the afterglow
become unobservable. We performed aperature photometry
vs. two unsaturated and isolated USNO B1.0 stars (R1
magnitudes):</span></font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
<br />
</span>
</font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
RA = 07:09:17.16, Dec. = +01:04:35.9, assuming R = 15.55</span></font>
</div>
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<font face="Arial" size="2">
<span style=" font-size:10pt">
<br />
</span>
</font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
RA = 07:09:28.54, Dec. = +01:03:57.1, assuming R = 16.25</span></font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
<br />
</span>
</font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
We derive the following magnitudes (mean exposure times
after the burst have been derived logarithmically):</span></font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
<br />
</span>
</font>
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<span style=" font-size:10pt">
dt         Start     Exposure          R mag  dR</span></font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
(days)   (SOD)   (seconds)</span></font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
<br />
</span>
</font>
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<font face="Arial" size="2">
<span style=" font-size:10pt">
0.0049994        73095   180       18.03    0.05</span></font>
</div>
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<span style=" font-size:10pt">
0.0076498        73324   180       18.12    0.03</span></font>
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0.0103234        73555   180       18.18    0.03</span></font>
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0.0129739        73784   180       18.17    0.05</span></font>
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<font face="Arial" size="2">
<span style=" font-size:10pt">
0.0156244        74013   180       18.43    0.07</span></font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
0.0182864        74243   180       18.79    0.05</span></font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
0.0209485        74473   180       18.83    0.07</span></font>
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<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
0.0235989        74702   180       18.95    0.08</span></font>
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<span style=" font-size:10pt">
0.0262494        74931   180       19.23    0.07</span></font>
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<font face="Arial" size="2">
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0.0288999        75160   180       19.38    0.09</span></font>
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0.0315503        75389   180       19.75    0.12</span></font>
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0.0342008        75618   180       20.00    0.16</span></font>
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0.0368512        75847   180       19.83    0.12</span></font>
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0.0395017        76076   180       19.88    0.15</span></font>
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0.0421522        76305   180       20.13    0.19</span></font>
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0.0472965        76540   600       20.64    0.23</span></font>
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0.0548081        77189   600       19.91    0.14</span></font>
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<font face="Arial" size="2">
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0.0623197        77838   600       19.96    0.15</span></font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
<br />
</span>
</font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
Adding further R and CR data (Rykoff et al., GCN 6269,
Gomboc et al., GCN 6271, Jelinek, Nuez, & Castro-Tirado,
GCN 6272, Berger et al., GCN 6278, Mikuz, Skvarc, &
Dintinjana, GCN 6288), we find:</span></font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
<br />
</span>
</font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
The afterglow may be rising early on, looking at the earliest
detections from Crni Vrh, ROTSE and Tautenburg.</span></font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
<br />
</span>
</font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
The afterglow then goes over into a plateau phase (decay
alpha= 0.14 +/- 0.1). In our data, we do not see the strong
rebrightening detected by ROTSE (Rykoff et al., GCN 6269).</span></font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
<br />
</span>
</font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
At 0.014 +/- 0.001 days, the afterglow breaks and begins a
decay with alpha = 1.54 +\- 0.16 up to about 0.03 days, where a
possible flare occurs.</span></font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
<br />
</span>
</font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
At about 0.05 days, the afterglow seems to rebrighten strongly,
our data here are in full accordance with those of the Liverpool
telescope (Gomboc et al., GCN 6271) and the IAC80 (Jelinek,
Nuez, & Castro-Tirado, GCN 6272).</span></font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
<br />
</span>
</font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
Further photometric follow-up of this GRB is warranted.</span></font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
<br />
</span>
</font>
</div>
<div align="left">
<font face="Arial" size="2">
<span style=" font-size:10pt">
This message may be cited.</span></font>
</div>
</body>
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