BOOTES: A stereoscopic robotic ground support facility

Castro‐Tirado, A. J.; Jelínek, M.; Sanguino, Tomás de Jesús Mateo; Postigo, A. de Ugarte

doi:10.1002/asna.200410333

Cited by 10 publications

(6 citation statements)

References 5 publications

(4 reference statements)

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“…Our very first observations of XRF 050824 were obtained with the BOOTES-1B 30 cm robotic telescope (e.g., Castro-Tirado et al 2004) in southern Spain, which detected the burst from 10.6 min after the high energy event in several R-band exposures. However, since these images were not processed until later, the actual discovery was instead made via the studies we initiated 38 min after the burst (Gorosabel et al 2005) using the 1.5 m telescope at the Observatorio de Sierra Nevada (OSN).…”

Section: Photometrymentioning

confidence: 99%

The nature of the X-ray flash of August 24 2005

Sollerman

Fynbo

Gorosabel

et al. 2007

A&A

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Aims. Our aim is to investigate the nature of the X-Ray Flash (XRF) of August 24, 2005. Methods. We present comprehensive photometric R-band observations of the fading optical afterglow of XRF 050824, from 11 min to 104 days after the burst. In addition we present observations taken during the first day in the BRIK bands and two epochs of spectroscopy. We also analyse available X-ray data. Results. The R-band lightcurve of the afterglow resembles the lightcurves of long duration Gamma-Ray Bursts (GRBs), i.e., a powerlaw, albeit with a rather shallow slope of α = 0.6 (F ν ∝ t −α ). Our late R-band images reveal the host galaxy. The rest-frame B-band luminosity is ∼0.5 L * . The star-formation rate as determined from the [O II] emission line is ∼1.8 M yr −1 . When accounting for the host contribution, the slope is α = 0.65 ± 0.01 and a break in the lightcurve is suggested. A potential lightcurve bump at 2 weeks can be interpreted as a supernova only if this is a supernova with a fast rise and a fast decay. However, the overall fit still shows excess scatter in the lightcurve in the form of wiggles and bumps. The flat lightcurves in the optical and X-rays could be explained by a continuous energy injection scenario, with an on-axis viewing angle and a wide jet opening angle (θ j > ∼ 10• ). If the energy injections are episodic this could potentially help explain the bumps and wiggles. Spectroscopy of the afterglow gives a redshift of z = 0.828 ± 0.005 from both absorption and emission lines. The spectral energy distribution (SED) of the afterglow has a power-law (F ν ∝ ν −β ) shape with slope β = 0.56 ± 0.04. This can be compared to the X-ray spectral index which is β X = 1.0 ± 0.1. The curvature of the SED constrains the dust reddening towards the burst to A v < 0.5 mag.

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Section: Photometrymentioning

confidence: 99%

The nature of the X-ray flash of August 24 2005

Sollerman

Fynbo

Gorosabel

et al. 2007

A&A

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“…The BOOTES-1 very wide field camera, located at Estación de Sondeos Atmosféricos (INTA-CEDEA) in Huelva (Spain), observed the region of the sky containing the Swift/BAT error box of GRB 050509b as part of its routine observing schedule (Castro-Tirado et al 2004). A 30 s exposure started at 04:00:00 UT (19 s prior to the onset of the 40 ms short burst), with the following frame starting at 04:01:00 UT.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

GRB 050509b: the elusive optical/nIR/mm afterglow of a short-duration GRB

Castro-Tirado

Postigo

Gorosabel

et al. 2005

A&A

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Abstract. We present multiwavelength (optical/near infrared/millimetre) observations of a short duration gamma-ray burst detected by Swift (GRB 050509b) collected between 0 seconds and ∼18.8 days after the event. No optical, near infrared or millimetre emission has been detected in spite of the well localised X-ray afterglow, confirming the elusiveness of the short duration events. We also discuss the possibility of the burst being located in a cluster of galaxies at z = 0.225 or beyond. In the former case, the spectral energy distribution of the neighbouring, potential host galaxy, favours a system harbouring an evolved dominant stellar population (age ∼360 Myr), unlike most long duration GRB host galaxies observed so far, i.e. thus giving support to a compact binary merger origin. Any underlying supernova that could be associated with this particular event should have been at least 3 magnitudes fainter than the type Ib/c SN 1998bw and 2.3 mag fainter than a typical type Ia SN.

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“…The real experiment has been made with four telescopes: Mini-Mega TORTORA (MMT) [20], from The Special Astrophysical Observatory in Russia; BART [21] located at the Astronomical institute AVČR at Ondřejov; BOOTES-1A [22], from the BOOTES network in Huelva; and CATA 500, a telescope from the Universidad de Chile located in the Cerro Tololo Inter-American Observatory.…”

Section: Resultsmentioning

confidence: 99%

GlSch

López-Casado

Pulgar

Cabello-Castillo

et al. 2015

Proceedings of the 30th Annual ACM Symposium on Applied Computing

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The aim of the Gloria Scheduler (GlSch) is to manage a heterogeneous network of robotic telescopes for citizen science, helping users to get involved in astronomy research. The main advantage of this scheduler is the ability to connect with different third-party local schedulers. This is carried out using a hybrid distributed-centralised architecture, which is described in this paper. Moreover, it describes the information workflow at different levels from the end-users request to telescopes. Finally, an experiment with different telescopes has been performed, and its results are also analysed in this paper.

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BOOTES: A stereoscopic robotic ground support facility

Cited by 10 publications

References 5 publications

The nature of the X-ray flash of August 24 2005

The nature of the X-ray flash of August 24 2005

GRB 050509b: the elusive optical/nIR/mm afterglow of a short-duration GRB

GlSch

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