# A Decade of GRB Follow-Up by BOOTES in Spain (2003–2013)

Authors: Martin Jelínek; Alberto J. Castro-Tirado; Ronan Cunniffe; Javier Gorosabel; Stanislav Vítek; Petr Kubánek; Antonio de Ugarte Postigo; Sergey Guziy; Juan C. Tello; Petr Páta; Rubén Sánchez-Ramírez; Samantha Oates; Soomin Jeong; Jan Štrobl; Sebastián Castillo-Carrión; Tomás Mateo Sanguino; Ovidio Rabaza; Dolores Pérez-Ramírez; Rafael Fernández-Muñoz; Benito A. de la Morena Carretero; René Hudec; Víctor Reglero; Lola Sabau-Graziati
Journal: Advances in Astronomy
 (2016)

---

## Abstract

This article covers ten years of GRB follow-ups by the Spanish BOOTES stations: 71 follow-ups providing 23 detections. Follow-ups by BOOTES-1B from 2005 to 2008 were given in a previous article and are here reviewed and updated, and additional detection data points are included as the former article merely stated their existence. The all-sky cameras CASSANDRA have not yet detected any GRB optical afterglows, but limits are reported where available.


---

## Body

## 1. Introduction

Ever since the discovery of Gamma-ray bursts (GRB) in 1967 [1], it was hoped to discover their counterparts at other wavelengths. The early GRB-related transient searching methods varied (wide-field optical systems as well as deep searches were being employed) but, given the coarse gamma-ray-based GRB localizations provided, generally lacked either sensitivity or good reaction time. The eventual discovery of GRB optical counterparts was done only when an X-ray follow-up telescope was available on the BeppoSAX satellite [2]. The optical afterglow could then be searched for with a large telescope in a small errorbox provided by the discovery of the X-ray afterglow. The first optical afterglow of a gamma-ray burst was discovered this way in 1997 [3].Since then, astronomers have been trying to minimize the time delay between receiving the position and the start of observations—by both personal dedication and by automating the telescope reaction. The ultimate step in automation, to minimize the time delay, is a full robotization of the observatory to eliminate any human intervention in the follow-up process. This way, the reaction time can be minimized from ~10-minute limit that can be achieved with a human operated telescope to below 10 seconds. With improvements in computational methods and in image processing speed, blind (non-follow-up) wide-field methods are starting to be practical in the search for optical transients. Although limited in magnitude range, they have already provided important observations of the optical emission simultaneous to the gamma-ray production of a GRB [4].Since 1997, the robotic telescope network BOOTES has been part of the effort to follow up gamma-ray burst events [5]. As of now, the network of robotic telescopes BOOTES consists of six telescopes around the globe, dedicated primarily to GRB afterglow follow-up. We present the results of our GRB follow-up programme by two telescopes of the network—BOOTES-1B and BOOTES-2—and by the respective stationary very-wide-field cameras (CASSANDRA). This text covers eleven years of GRB follow-ups: 71 follow-ups providing 21 detections.Different instruments have been part of BOOTES during the years in question: a 30 cm telescope which was used for most of the time at BOOTES-1 station but at periods also at BOOTES-2, the fast-moving 60 cm telescope at BOOTES-2 (Telma), and also two all-sky cameras, CASSANDRA1 at BOOTES-1 and CASSANDRA2 at BOOTES-2. Results from CASSANDRAs are included where available, without paying attention to the complete sample.This article is a follow-up of a previous article, that is, Jelínek et al. [6], which provided detailed description of evolution of BOOTES-1B, and analysis of efficiency of a system dedicated to GRB follow-up based on real data obtained during four years between 2005 and 2008. This work is a catalogue of BOOTES-1B and BOOTES-2 GRB observations between 2003 and 2013; it is complete in providing information about successfully followed up events but does not provide analysis of missed triggers as did the previous article.


### 1.1. BOOTES-1B

BOOTES-1 observatory is located at the atmospheric sounding station at El Arenosillo, Huelva, Spain (at lat.: 37°06′14′′N, long.: 06°44′02′′W). Over time, distinct system configurations were used, including also two 8-inch S-C telescopes, as described in Jelínek et al. [6]; the primary instrument of BOOTES-1B is a D
=
30 cm Schmidt-Cassegrain optical tube assembly with a CCD camera. Prior to June 15, 2007, Bessel V
R
I filters were being used as noted with the observations, any observations obtained after this date have been obtained without filter (C or clear). We calibrate these observations against R-band, which, in the case of no color evolution of the optical counterpart, is expected to result in a small (~0.1 mag) constant offset in magnitude.


### 1.2. BOOTES-2

BOOTES-2 is located at CSIC’s experimental station La Mayora (Instituto de Hortofruticultura Subtropical y Mediterránea- (IHSM-) CSIC) (at lat.: 36°45′33′′N, long.: 04°02′27′′W), 240 km from BOOTES-1. It was originally equipped with an identical 30 cm Schmidt-Cassegrain telescope to that at BOOTES-1B. In 2007 the telescope was upgraded to a lightweight 60 cm Ritchey-Chrètien telescope on a fast-slewing NTM-500 mount, both provided by Astelco. The camera was upgraded at the same time to an Andor iXon1024
×
1024 EMCCD, and in 2012 the capabilities were extended yet again to low resolution spectroscopy, by the installation of the imaging spectrograph COLORES of our own design and construction [7]. Bessel magnitudes are calibrated to Vega system, SDSS to AB.


## 1.1. BOOTES-1B

BOOTES-1 observatory is located at the atmospheric sounding station at El Arenosillo, Huelva, Spain (at lat.: 37°06′14′′N, long.: 06°44′02′′W). Over time, distinct system configurations were used, including also two 8-inch S-C telescopes, as described in Jelínek et al. [6]; the primary instrument of BOOTES-1B is a D
=
30 cm Schmidt-Cassegrain optical tube assembly with a CCD camera. Prior to June 15, 2007, Bessel V
R
I filters were being used as noted with the observations, any observations obtained after this date have been obtained without filter (C or clear). We calibrate these observations against R-band, which, in the case of no color evolution of the optical counterpart, is expected to result in a small (~0.1 mag) constant offset in magnitude.


## 1.2. BOOTES-2

BOOTES-2 is located at CSIC’s experimental station La Mayora (Instituto de Hortofruticultura Subtropical y Mediterránea- (IHSM-) CSIC) (at lat.: 36°45′33′′N, long.: 04°02′27′′W), 240 km from BOOTES-1. It was originally equipped with an identical 30 cm Schmidt-Cassegrain telescope to that at BOOTES-1B. In 2007 the telescope was upgraded to a lightweight 60 cm Ritchey-Chrètien telescope on a fast-slewing NTM-500 mount, both provided by Astelco. The camera was upgraded at the same time to an Andor iXon1024
×
1024 EMCCD, and in 2012 the capabilities were extended yet again to low resolution spectroscopy, by the installation of the imaging spectrograph COLORES of our own design and construction [7]. Bessel magnitudes are calibrated to Vega system, SDSS to AB.


## 2. Optical Follow-Up of GRB Events

Here we will detail the individual results for each of the 23 events followed up and detected in 2003–2013. Each GRB is given a short introductory paragraph as a reminder of the basic observational properties of the event. Although we do not discuss the properties at other wavelengths, we try to include a comprehensive reference of literature relevant to each burst. As GCN reports usually summarise the relevant GCN circular traffic, we have omitted the raw GCN circulars except for events for which a GCN report or other more exhaustive paper is unavailable.Further 48 follow-ups which resulted in detection limits are included in Tables1 and 2 but are not given any further attention.Table 1
BOOTES-1B GRBs in a table.
GRB
Δ
T
Number of points
Result
Ref.
030913
2 h
V
>
17.5, C
>
12
050215B
22 m
V
>
16.5, I
>
15.0
050505
47 m
V
>
19
050509A
64 m
V
>
14.9
050509B
62 s
V
>
11.5
050525A
12 m†
1
16.5
±
0.4
[8]
050528
71 s
V
>
13.8, I
>
13.0
050824
10 m
4
R
=
18.2
±
0.3
[9]
050904
2 m
R
>
18.2
[10]
050922C
4 m
3
R
=
14.6
±
0.4
051109A
55 s
6
R
=
15.7
±
0.4
051211B
42 s
R
>
14
051221B
4 m
R
>
16
060421
61 s
R
>
14
061110B
11 m
R
>
18
071101
55 s
C
>
17.0
071109
59 s
C
>
13.0
080330
6 m
6
C
=
16.5
±
0.2
080413A
61 s
61
C
≃
13.3
080430
34 s
1
C
≃
15.5
080603B
1 h
11
C
≃
17.4
[11]
080605
44 s
28
C
≃
14.7
[12]
081003B
41 s
C
>
17.6
090313
12 h
1
C
≃
18.3
090519
99 s
C
>
17.6
090813
53 s
1
C
≃
17.9
090814A
3 m†
C
>
15.8
090814B
53 s†
C
>
17.5
090817
24 m
C
>
16.7
100906A
106 s
C
>
16.5
110205A
102 s
16
C
∼
14
[13]
110212A
50 s
C
>
13.0
110213A
15 h
1
C
=
18.3
±
0.2
110411A
24 s
C
>
17.8
111016A
1.25 h
C
>
17.8
120326A
40 m
1
C
∼
19.5
120327A
41 m†
6
C
=
17.5
120328A
7.5 m
C
>
16
120521C
11.7 m
C
>
20.5
120711B
107 s
C
>
18.2
120729A
10 h
C
>
19.0
121017A
79 s
C
>
19.0
121024A
40 m
1
C
=
18.2
±
0.5
121209A
42 s†
C
>
16.5
130122A
28 m
C
>
18.4
Note. † marks alerts covered in real time by wide-field camera CASSANDRA-1.Table 2
BOOTES-2 GRBs in a table.
GRB
Δ
T
Number of points
Result
Ref.
080603B
20
R
≃
17.4
[11]
080605
5
R
≃
14.7
[12]
090817
145 s
R
>
18.3
090904A
86 s
R
>
16.1
091202
5.5 h
R
>
18.3
100219A
6.3 h
C
>
18.3
100418A
1.8 h
11
C
=
19.3
100522A
625 s
C
>
15.5
100526A
4 h
r
′
>
14
100614A
6.9 m
C
>
18
100901A
10 h
10
C
=
17.52
±
0.08
100915A
106 s
C
>
16.5
101020A
5.1 h
r
′
>
18.0
101112A
595 s
15
C
=
15.5
110106B
10.3 m
C
>
16.5
110205A
15 m
13
R
∼
14
[13]
110212A
32 m
R
>
16.5
110223A
228 s
R
>
17.6
120729A
13.25 h
R
>
19.4
120805A
25 m
R
>
18.5
120816A
66 m
R
>
18
121001A
32 m
I
>
19.7
121017A
3 m
C
>
18.5, i
′
>
19.5
130418A
1.5 h
21
C
=
16.8
±
0.06
130505A
11.94 h
1
R
C
=
19.26
±
0.06
130606A
13 m
21
i
′
=
16.7
±
0.3
130608A
2.3 h
C
>
18.8
130612A
4.8 m
C
>
18.6
130806A
40 s
C
>
18.3
131202A
4.25 h
i
′
>
19.7One by one, we show all the successful follow-ups that these telescopes have performed during the first ten years of theSwift era and since the transition of the BOOTES network to the RTS-2 [14] observatory control system, which was for the first time installed at BOOTES-2 in 2003 and during the summer of 2004 at BOOTES-1.GRB 050525A (A Bright Low-Redshift (
z
=
0.606
) Localized by Swift [15]). Plenty of optical observations were obtained, including the signature of the associated supernova sn2005nc [8, 16].GRB 050525A was the first BOOTES-1B burst for which a detection was obtained. The telescope started the first exposure 28 s after receiving the notice, 383 s after the GRB trigger. An optical afterglow withV
≃
16 was detected. A weak detection of a bright GRB implied a reexamination of observing strategies employed by BOOTES. The largest, 30 cm telescope was changed to make R-band imaging instead of using the field spectrograph to greatly improve sensitivity in terms of limiting magnitude. The 20 cm telescopes were still observing with V
+
I filters (for details see [6]); see Table 3.Table 3
GRB 050525A: observing log of BOOTES-1B.
Δ
T [h]
exp [s]
mag
dmag
Filter
0.195
39
×
10 s
16.51
0.39
R
Note. Published by Resmi et al. [8].This burst was covered in real time by both all-sky cameras of BOOTES (CASSANDRA1 and CASSANDRA2), providing an unfiltered limit of >9.0 [17].BOOTES observation of this GRB is included in Resmi et al. [8].GRB 050824 (A Dim Burst Detected by Swift). The optical afterglow of this GRB is discovered with the 1.5 m telescope at OSN; redshift z
=
0.83 as determined by VLT [9].BOOTES-1B was the first telescope to observe this optical transient, starting 636 s after the trigger withR
≃
17.5. The weather was not stable and the focus not perfect, but BOOTES-1B worked as expected. In the end, several hours of data were obtained. BOOTES observation of this GRB is included in Sollerman et al. [9]; see Table 4 and Figure 1.Table 4
GRB 050824: observing log of BOOTES-1B.
Δ
T [h]
exp [s]
mag
dmag
Filter
0.1763
2
×
300 s
18.22
0.35
R
0.3462
8
×
300 s
19.11
0.32
R
1.0249
22
×
300 s
19.67
0.33
R
2.9091
31
×
300 s
19.33
0.20
R
Note. Published by Sollerman et al. [9].Figure 1
The optical light curve of GRB 050824; the optical light curve represents the behaviour seen by Sollerman et al. [9].GRB 050922C. ASwift short and intense long burst [18, 19] was observed also byHETE2 [20]. Optical afterglow is m
a
g
~
15; z
=
2.198 [21].Due to clouds, the limiting magnitude of BOOTES-1B dropped from ~17.0 for a 30 s exposure to merely 12.9. The afterglow was eventually detected with theR-band camera (at the 30 cm telescope) during gaps between passing clouds. The first weak detection was obtained 228 s after the GRB trigger and gave R
≃
14.6; see Table 5.Table 5
GRB 050922C: observing log of BOOTES-1B.
Δ
T [h]
exp [s]
mag
dmag
Filter
0.0694
40
14.58
0.35
R
0.3752
900
17.01
0.39
R
0.6193
900
18.53
0.59
RGRB 051109A (A Burst Detected by Swift [23]). The optical afterglow was m
a
g
~
15, and the redshift was determined to be z
=
2.346 [24]. The optical lightcurve was published by Mirabal et al. [22].At BOOTES-1B the image acquisition started 54.8 s after the burst with the 30 cm telescope inR-band and one of the 20 cm telescopes in I-band [25]. There were still a number of performance problems—most importantly synchronization between cameras such that when the telescope position was to be changed, both cameras had to be idle. As the 30 cm telescope was taking shorter exposures, extra exposures could have been made while waiting for the longer exposures being taken at the 20 cm to finish. The 20 cm detection is, after critical revision, only at the level of 2-σ. The R-band observation shows the object until about 20 minutes after the GRB, when it becomes too dim to measure in the vicinity of a 17.5 m nearby star. Mean decay rate observed by BOOTES is α
=
0.63
±
0.06 (F
o
p
t
~
t
-
α).The relatively shallow decay observed by BOOTES is in close agreement with what was observed several minutes later by the 2.4 m MDM (α
=
0.62
±
0.03) and according to an unofficial report [26] there was a decay change later, by about 3 h after the burst to α
=
0.89
±
0
.
05; see Table 6 and Figure 2.Table 6
GRB 051109A: observing log of BOOTES-1B.
Δ
T [s]
exp [s]
mag
dmag
Filter
59.7
10
15.67
0.35
R
122.2
74
16.02
0.19
R
257.9
41
16.65
0.41
R
756.6
205
17.18
0.22
R
1021.5
313
17.68
0.26
R
508.4
908
16.98
0.54
IFigure 2
The optical light curve of GRB 051109A. The dotted line represents the optical decay observed by Mirabal et al. [22].GRB 080330 (A Rather Bright Long Burst Detected by Swift). Afterglow was reported to be detected by UVOT, TAROT, ROTSE-III, Liverpool Telescope, and GROND. Spectroscopic redshift was measured as z
=
1.51 by the NOT [28].This GRB happened during the first day recommissioning of BOOTES-1B after its move from the BOOTES-2 site at La Mayora. The GCN client was not yet operational and at the time of the GRB we were focusing the telescope. The first image was obtained 379 s after the GRB trigger and the optical afterglow was detected with magnitude ~16.3 on the first image. A bug in the centering algorithm caused a loss of part subsequent data. Further detections were obtained starting 21 min after the GRB when the problem was fixed.The light curve (as seen by [27]) seems to show an optical flare and then a possible hydrodynamic peak. The data of BOOTES, however, trace only the final part of this behaviour, where the decay accelerates after passing through the hydrodynamic peak; see Table 7 and Figure 3.Table 7
GRB 080330: observing log of BOOTES-1B.
Δ
T [h]
exp [s]
mag
dmag
Filter
0.1061
7
16.52
0.23
Clear
0.3752
210
16.61
0.13
Clear
0.6193
588
17.16
0.14
Clear
0.8547
825
17.45
0.15
Clear
1.0915
862
17.29
0.13
Clear
1.3384
905
17.42
0.16
ClearFigure 3
The optical light curve of GRB 080330. The dotted line shows the light curve as seen by ROTSE-III [27].GRB 080413A. A rather bright GRB was detected bySwift and also bySuzaku-WAM; optical afterglow was detected by ROTSE-III [27]; and redshift z
=
2.433 was detected by VLT+UVES [29].BOOTES-1B started obtaining images of the GRB 080413A just 60.7 s after the trigger (46.3 s after reception of the alert). AnR
≃
13.3 magnitude decaying optical afterglow was found ([30],Jelínek et al., in prep.); see Figure 4.Figure 4
The optical light curve of GRB 080413A.GRB 080430 (A Burst Detected by Swift). It was a widely observed, low-redshift z
≃
0.75 optical afterglow with a slowly decaying optical afterglow [31]. It was observed also at very high energies byMAGIC without detection [32].BOOTES-1B obtained the first image of this GRB 34.4 s after the trigger. An optical transient was detected on combined unfiltered images with a magnitude≃
15.5 [33].GRB 080603B. A long GRB localized bySwift is detected also byKonus-Wind and byINTEGRAL[34]. Bright optical afterglow was observed. Extensive follow-up was carried out. Redshift is z
=
2.69 [35].This GRB happened in Spain during sunset. We obtained first useful images starting one hour after the trigger. AnR
≃
17.4 optical transient was detected with both BOOTES-1B and BOOTES-2; see Figure 5. BOOTES observation of this GRB is included in Jelínek et al. [11]; see Figure 5.Figure 5
The optical light curve of GRB 080603B [11].GRB 080605 (A Long Burst Detected by Swift [36]). The host was found to be a metal enriched star forming galaxy at redshift z
=
1.64 [37] and exhibited the 2175 Å extinction feature [38].GRB 080605 was observed by both BOOTES-1B (28 photometric points) and BOOTES-2 (5 photometric points) starting 44 s after the trigger. A rapidly decaying optical afterglow (α
=
1.27
±
0.04) with R
=
14.7 on the first images was found; see Figure 6. All BOOTES data are included in Jelínek et al. [12]; see Figure 5.Figure 6
The optical light curve of GRB 080605 [12]; the dotted line is behaviour observed by Rumyantsev and Pozanenko [39] and Zafar et al. [38].GRB 090313 (GRB by Swift, No Prompt X-Rays [40]). An optical afterglow peaked at R
~
15.6. Extensive optical + infrared follow-up was carried out. The first GRB to be observed was detected by X-Shooter. Also it was detected by various observatories in radio. Redshift is z
=
3.375 [41, 42].The GRB happened during daytime for BOOTES-1B and it was followed up manually. Due to the proximity of the moon and limitations of then-new CCD camera driver, many 2 s exposures were taken to be combined later. The optical afterglow was detected with magnitude ~18.3 ± 0.4 on a635
×
2s (=21 min) exposure with the midtime 11.96 h after the GRB trigger.GRB 090813. A long GRB bySwift, suspected of being higher-z, observed also byKonus-Wind andFermi-GBM [43]. Optical counterpart was observed by the 1.23 m telescope at Calar Alto with a magnitude of I
=
17.0 [44].BOOTES-1B started observation 53 s after the GRB, taking 10 s unfiltered exposures. The optical transient was weakly detected on a combined image of10
×
10s whose exposure mean time was 630 s after the burst. The optical counterpart was found having R
=
17.9
±
0.3. Given that the previous and subsequent images did not show any OT detection, we might speculate about the optical emission peaking at about this time. Also the brightness is much weaker than what might be expected from the detection by Gorosabel et al. [44], supporting the high-redshift origin; see Table 8.Table 8
GRB 090813: observing log of BOOTES-1B.
Δ
T [h]
exp [s]
mag
dmag
Filter
0.175
10
×
10
17.9
0.3
ClearGRB 100418A. A weak long burst was detected bySwift [45] with a peculiar, late-peaking optical afterglow with z
=
0.6239 [46]. Also it was detected in radio [47].The first image of the GRB location was taken by BOOTES-2 at 21:50 UT (40 min after the GRB trigger). The rising optical afterglow was detected for the first time on an image obtained as a sum of 23 images, with an exposure midtime 107 minutes after the GRB trigger. The optical emission peaked at magnitudeR
=
18.7 another hour later, at an image with the midtime 163 min after the trigger. A slow decay followed, which permitted us to detect the optical counterpart until 8 days after the GRB.Because of a mount problem, many images were lost (pointed somewhere else) and the potential of the telescope was not fully used. Eventually, after combining images when appropriate, 11 photometric points were obtained. A rising part of the optical afterglow was seen that way; see Table9 and Figure 7.Table 9
GRB 100418A: observing log of BOOTES-2.
Δ
T [h]
exp [s]
mag
dmag
Filter
1.78
1638
19.785
0.215
Clear
2.09
597
19.127
0.127
Clear
2.55
534
18.774
0.087
Clear
2.72
656
18.668
0.073
Clear
3.10
239
18.706
0.106
Clear
3.43
238
18.759
0.189
Clear
4.70
3908
19.067
0.108
Clear
6.19
4328
18.897
0.115
Clear
7.39
551
18.493
0.078
Clear
77.3
14830
20.475
0.202
Clear
125.6
12482
20.970
0.208
ClearFigure 7
The bizarre optical light curve of GRB 100418A. Combination of BOOTES and UVOT data [45]. UVOT points were shifted by an arbitrary constant.GRB 100901A (A Long Burst from Swift). Bright, slowly decaying optical afterglow was discovered by UVOT. Redshift is z
=
1.408. It was detected also by SMA at 345 GHz [48–50].The burst happened in daytime in Spain and the position became available only almost ten hours later after the sunset. The afterglow was still well detected with magnitudeR
≃
17.5 at the beginning. BOOTES-2 had some problems with CCD cooling, and some images were useless. The afterglow was detected also the following night with R
=
19.35; see Table 10 and Figure 8.Table 10
GRB 100901A: observing log of BOOTES-2.
Δ
T [h]
exp [s]
mag
dmag
Filter
10.202
268
17.52
0.08
R
10.719
415
17.61
0.07
R
11.230
354
17.67
0.09
R
11.734
238
17.99
0.16
R
12.346
730
17.78
0.13
R
12.980
759
17.68
0.12
R
13.239
759
17.82
0.16
R
13.971
997
18.21
0.12
R
14.611
1101
18.32
0.14
R
33.791
4012
19.35
0.19
RFigure 8
The optical light curve of GRB 100901A. The dotted line representing burst behaviour is based on observations by Gorbovskoy et al. [49], Kann et al. [51], and Rumyantsev et al. [52].GRB 101112A. AnINTEGRAL-localized burst [53] was also detected byFermi-GBM [54],Konus-Wind [55], andSwift-XRT [56]. Optical afterglow was discovered independently by BOOTES-2 and Liverpool Telescope [57]. It was detected also in radio [58].BOOTES-2 reacted to the GRB 101112A and started to observe 47 s after the GRB. A set of 3 s exposures was taken, but due to technical problems with the mount a significant amount of observing time was lost. An optical afterglow was discovered and reported [59]. The optical light curve exhibited first a decay, then a sudden rise to a peak at about 800 s after the trigger, and finally a surprisingly fast decay with α
≃
-
4. This behaviour seemed more like an optical flare than a “proper” GRB afterglow, but there does not seem to be contemporaneous high-energy data to make a firm statement; see Table 11 and Figure 9.Table 11
GRB 101112A: observing log of BOOTES-2.
Δ
T [s]
exp [s]
mag
dmag
Filter
595.0
16
16.00
0.19
r
′
631.8
8
16.10
0.29
r
′
664.9
7
16.46
0.34
r
′
697.8
7
16.30
0.25
r
′
731.0
7
15.52
0.18
r
′
766.1
11
15.56
0.13
r
′
800.9
7
15.52
0.17
r
′
833.8
7
15.24
0.12
r
′
891.2
44
15.92
0.13
r
′
973.7
69
16.33
0.20
r
′
1044.0
69
16.62
0.23
r
′
1124.2
41
17.09
0.36
r
′
1252.7
115
17.44
0.25
r
′
1393.8
116
17.86
0.38
r
′
1629.5
255
18.57
0.48
r
′Figure 9
The optical light curve of GRB 101112A.GRB 110205A (A Very Long and Bright Burst by Swift). Detected also byKonus-Wind andSuzaku-WAM, optical afterglow peaked at R
~
14.0, with extensive multiwavelength follow-up; z
=
2.22
“Textbook burst” [13, 60].BOOTES-1B reacted automatically to theSwift trigger. First 10 s unfiltered exposure was obtained 102 s after the beginning of the GRB (with T
90
=
257 s), that is, while the gamma-ray emission was still taking place. After taking 18 images, the observatory triggered on a false alarm from the rain detector, which caused the observation to be stopped for 20 minutes. After resuming the observation, 3
×
30 s images were obtained and another false alert struck over. This alert was remotely overridden by Kubánek, so that all 20 minutes was not lost. From then on, the observation continued until sunrise. The afterglow is well detected in the images until 2.2 hours after the GRB. 16 photometric points from combined images were eventually published.BOOTES-2 started observations 15 min after the trigger, clearly detecting the afterglow inR-band until 3.2 hours after the burst. 13 photometric points were obtained. The delay was caused by technical problems. BOOTES observations of this GRB are included in Zheng et al. [13]; see Figure 10.Figure 10
The optical light curve of GRB 110205A.GRB 110213A. A bright burst was detected bySwift; it was detected also byKonus-Wind andFermi-GBM. Optical afterglow is R
~
14.6, with extensive follow-up [61].BOOTES-1B started to observe 15 hours after the GRB (the position was below horizon at the time of the trigger) and continued for an hour; eventually,100
×
30s unfiltered images were combined; the OT brightness calibrated against USNO-A2 is 18.3
±
0.3 at the exposure midtime of 15.5 h after the GRB trigger; see Table 12.Table 12
GRB 110213A: observing log of BOOTES-1B.
Δ
T [h]
exp [s]
mag
dmag
Filter
15.5
100
×
30
18.29
0.30
ClearGRB 120326A (A Swift-Detected Burst). Afterglow was discovered by Tarot [62]. It is long-lived optical emission; redshift is z
=
1.78 by GTC. It was detected also byFermi-GBM andSuzaku-WAM (see [63] and the references therein).At BOOTES-1B the mount failed, because of the serial port communication failure. After a manual recovery, 40 minutes after the GRB, images were taken in hope for a detection, but the counterpart with the brightness ofR
~
19.5 was detected only at about 2σ level.GRB 120327A. A bright burst bySwift with an afterglow is discovered by UVOT [64]. Redshift is z
=
2.813 [65]. Extensive optical follow-up was carried out.BOOTES-1B reacted in 41 min (similar failure as the day before: the mount failed, because of the serial port communication failure), obtaining a series of 20 s exposures. These images were combined to get 600 s effective exposures and permitted detection of the afterglow on six such images. The brightness was decaying fromR
=
17.5 to R
=
18.6; see Table 13.Table 13
GRB 120327A: observing log of BOOTES-1B.
Δ
T [h]
exp [s]
mag
dmag
Filter
0.955
654
17.50
0.12
Clear
1.140
674
17.65
0.12
Clear
1.337
748
17.82
0.13
Clear
1.533
660
18.24
0.21
Clear
1.718
673
18.17
0.21
Clear
1.905
656
18.59
0.29
ClearAll-sky camera at BOOTES-1 (CASSANDRA1) covered the event in real time and detected nothing down toR
~
7
.
5
(Zanioni et al. in prep.).GRB 121001A. A bright and longSwift-detected GRB was originally designated as possibly galactic [66]. Afterglow was discovered by Andreev et al. [67].BOOTES-2 observed this trigger starting 32 min after the trigger. An optical afterglow is detected inI-band with I
~
19.7 (Vega) for a sum of images between 20:49 and 21:52 UT [68].GRB 121024A. It is a brightSwift-detected GRB with a bright optical afterglow [69, 70]. It was detected also in radio [71]. Redshift is z
=
2.298 by Tanvir et al. [72].BOOTES-1B observed the optical afterglow of GRB 121024A. The observations started 40 minutes after the GRB trigger. The sum of 20 minutes of unfiltered images with a mean integration time 54 minutes after the GRB shows a weak detection of the optical afterglow with magnitudeR
=
18.2
±
0.5 [73]; see Table 14.Table 14
GRB 121024A: observing log of BOOTES-1B.
Δ
T [h]
exp [s]
mag
dmag
Filter
0.900
1200
18.2
0.5
ClearGRB 130418A. It is a bright and long burst with a well-detected optical afterglow somewhat peculiarly detected after a slew bySwift [74]. Observation byKonus-Wind showed that the burst started already 218 s beforeSwift triggered [75]. Redshift is z
=
1.218 by de Ugarte Postigo et al. [76].BOOTES-2 obtained a large set of unfiltered,r
′-band and i
′-band images starting 1.5 h after the trigger. The optical afterglow is well detected in the images. The light curve is steadily decaying with the power-law index of α
=
-
0.93
±
0.06, with the exception of the beginning, where there is a possible flaring with peak about 0.25 mag brighter than the steady power-law; see Table 15 and Figure 11.Table 15
GRB 130418A: observing log of BOOTES-1B and BOOTES-2.
Δ
T [h]
exp [s]
mag
dmag
Filter
1.514
3
×
15s
17.09
0.08
Clear
1.529
3
×
15s
16.95
0.07
Clear
1.544
3
×
15s
16.90
0.06
Clear
1.558
3
×
15s
16.62
0.07
Clear
1.573
3
×
15s
17.03
0.07
Clear
1.590
4
×
15s
16.92
0.06
Clear
1.610
4
×
15s
17.04
0.07
Clear
1.749
7
×
15s
17.22
0.05
Clear
1.865
60 s
16.92
0.18
r
′
1.884
4
×
15s
17.34
0.09
Clear
2.054
7
×
15s
17.45
0.07
Clear
2.089
7
×
15s
17.46
0.06
Clear
2.209
6
×
15s
17.47
0.07
Clear
2.326
6
×
15s
17.56
0.08
Clear
2.444
6
×
15s
17.71
0.09
Clear
2.562
6
×
15s
17.68
0.08
Clear
2.798
22
×
60s
17.40
0.04
i
′
3.061
15
×
60s
17.90
0.09
r
′
3.333
15
×
60s
17.98
0.09
r
′
3.604
15
×
60s
17.90
0.09
r
′
3.866
15
×
60s
18.05
0.11
r
′
4.130
15
×
60s
18.53
0.19
r
′
4.449
20
×
60s
18.42
0.14
r
′
4.808
20
×
60s
18.61
0.23
r
′Figure 11
The optical light curve of GRB 130418A.GRB 130505A. A bright and intense GRB with a 14 mag optical afterglow was detected bySwift [77]. Redshift is z
=
2.27 as reported by Tanvir et al. [78].BOOTES-2 obtained the first image of this GRB 11.94 h after the trigger. A set of 60 s exposures was obtained. Combining the first hour of images taken, we clearly detect the optical afterglow, and using the calibration provided by Kann et al. [79], we measure R
C
=
19.26
±
0.06; see Table 16.Table 16
GRB 130505A: observing log of BOOTES-2.
Δ
T [h]
exp [s]
mag
dmag
Filter
12.488
51
×
60 s
19.26
0.06
ClearGRB 130606A. A high-redshift GRB was detected bySwift [80], optical afterglow was discovered by BOOTES-2, and redshift is z
=
5.9 by GTC [81].BOOTES-2 reaction to this GRB alert was actually a failure; the system did not respond as well as it should and it had to be manually overridden to perform the observations. The first image has therefore been taken as late as 13 minutes after the trigger. These observations led to a discovery of a bright afterglow not seen bySwift-UVOT and prompted spectroscopic observations by 10.4 m GTC, which show redshift of this event to be z
=
5.9135. Overall, 14 photometric points in i
′-band and 7 in z
′-band were obtained [81]; see Figure 12.Figure 12
The optical light curve of GRB 130606A.i
′-band points were shifted 2.4 mag up to match with the z
′-band points.


## 3. Summary

Eleven years of BOOTES-1B and BOOTES-2 GRB follow-up history are summarised in the textual and tabular form. Each GRB is given a short introductory paragraph as a reminder of the basic optical properties of the event. Although we do not discuss the properties in other wavelengths, we try to include a comprehensive reference of literature relevant to each burst. One by one, we show all the successful follow-ups that these telescopes have performed during the first ten years of theSwift era and the transition of the BOOTES network to the RTS-2 [14] observatory control system, first installed at BOOTES-2 in 2003 and made definitive during the summer of 2004.The BOOTES telescopes, in spite of their moderate apertures (≲60 cm), have proven to detect a significant number of afterglows—together over 20, contributing to the understanding of the early GRB phase.



---

*Source: 1928465-2016-10-10.xml*