COATLI: an all-sky robotic optical imager with 0.3 arcsec image quality

Watson, A. M.; Cardona, Salvador Cuevas; Nuñez, Luis Carlos Alvarez; Ángeles, Fernando; Becerra, R. L.; Chapa, Oscar; Farah, Alejandro; Fuentes-Fernández, Jorge; Figueroa, Liliana; Lebre, Rosalía Langarica; Salinas-Quiroz, Fernando; Román-Zúñiga, C.; Ruíz-Diáz-Soto, Jaime; Tejada, Carlos; Tinoco, S.

doi:10.1117/12.2233000

Cited by 6 publications

(8 citation statements)

References 11 publications

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“…The design for the enclosure and platform has be adapted from the COATLI project. 18 We will use an Astelco ARTS station, which consists of a clamshell enclosure on a steel platform. This equipment is simple, robust, requires a minimum of maintainence, and has been proven in extreme conditions.…”

Section: Enclosure Platform and Piermentioning

confidence: 99%

“…We will install this prototype in parallel with the COATLI telescope 18 at the OAN/SPM in September 2016. At this point, we will also substitute a ML50100 CCD with 6 µm or 2 arcsec pixels.…”

Section: Ddoti Prototypementioning

confidence: 99%

“…The design of the control electronics has been adapted from the COATLI project. 18 Each basic imager will be controlled by a MinnowBoard Max computer in an electronics cabinet. The MinnowBoard Max has a dual-core Intel Atom E3800 processor with 2 GB of RAM, 1000BASE-T ethernet, and two USB ports.…”

Section: Control Electronicsmentioning

confidence: 99%

“…The control software will be adapted from the software we have used since 2011 to run the robotic Harold L. Johnson 1.5-meter telescope of the OAN/SPM and the RATIR instrument, 6,19 with modifications from the COATLI project 18 to control the Astelco NTM-500 mount and ARTS enclosure. One necessary modification will be to use the uncertainty maps distributed by the Fermi/GBM team to optimize our search strategy.…”

Section: Control Softwarementioning

confidence: 99%

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DDOTI: the deca-degree optical transient imager

et al. 2016

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DDOTI will be a wide-field robotic imager consisting of six 28-cm telescopes with prime focus CCDs mounted on a common equatorial mount. Each telescope will have a field of view of 12 square degrees, will have 2 arcsec pixels, and will reach a 10-sigma limiting magnitude in 60 seconds of r = 18.7 in dark time and r = 18.0 in bright time. The set of six will provide an instantaneous field of view of about 72 square degrees. DDOTI uses commercial components almost entirely. The first DDOTI will be installed at the Observatorio Astron\'omico Nacional in Sierra San Pedro Mart\'ir, Baja California, M\'exico in early 2017. The main science goals of DDOTI are the localization of the optical transients associated with GRBs detected by the GBM instrument on the Fermi satellite and with gravitational-wave transients. DDOTI will also be used for studies of AGN and YSO variability and to determine the occurrence of hot Jupiters. The principal advantage of DDOTI compared to other similar projects is cost: a single DDOTI installation costs only about US$500,000. This makes it possible to contemplate a global network of DDOTI installations. Such geographic diversity would give earlier access and a higher localization rate. We are actively exploring this option.Comment: To appear in the proceedings of SPIE conference 9910 "Observatory Operations: Strategies, Processes, and Systems VI". 12 page

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Section: Enclosure Platform and Piermentioning

confidence: 99%

Section: Ddoti Prototypementioning

confidence: 99%

Section: Control Electronicsmentioning

confidence: 99%

Section: Control Softwarementioning

confidence: 99%

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DDOTI: the deca-degree optical transient imager

et al. 2016

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“…The long GRB 191016A was detected by Swift/BAT at 04:09:00 UTC on 2019 October 16 (Gropp et al 2019), and its long-lasting afterglow emission was extensively observed in optical wavelengths by our ground-based robotic telescopes RATIR, COATLI, and DDOTI (Butler et al 2012;Watson et al 2012Watson et al , 2016aCuevas et al 2016) at the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir in Baja California in Mexico. In Watson et al (2019a), we reported the discovery of the afterglow with COATLI and its rise and subsequent fade.…”

Section: Introductionmentioning

confidence: 98%

GRB 191016A: The onset of the forward shock and evidence of late energy injection

Pereyra,

Fraija,

Watson

et al. 2021

Preprint

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We present optical and near-infrared photometric observations of GRB 191016 with the COATLI, DDOTI and RATIR groundbased telescopes over the first three nights. We present the temporal evolution of the optical afterglow and describe 5 different stages that were not completely characterized in previous works, mainly due to scarcity of data points to accurately fit the different components of the optical emission. After the end of the prompt gamma-ray emission, we observed the afterglow rise slowly in the optical and near-infrared (NIR) wavelengths and peak at around 𝑇 + 1450 s in all filters. This was followed by an early decay, a clear plateau from 𝑇 + 5000 s to 𝑇 + 11000 s, and then a regular late decay. We also present evidence of the jet break at later times, with a temporal index in good agreement with the temporal slope obtained from X-ray observations. Although many of the features observed in the optical light curves of GRBs are usually well explained by a reverse shock (RS) or forward shock (FS), the shallowness of the optical rise and enhanced peak emission in the GRB191016A afterglow is not well-fitted by only a FS or a RS. We propose a theoretical model which considers both of these components and combines an evolving FS with a later embedded RS and a subsequent late energy injection from the central engine activity. We use this model to successfully explain the temporal evolution of the light curves and discuss its implications on the fireball properties.

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Understanding the nature of the optical emission in gamma-ray bursts: analysis from TAROT, COATLI, and RATIR observations

Becerra,

Klotz,

Atteia

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We collected the optical light-curve data of 227 gamma-ray bursts (GRBs) observed with the TAROT, COATLI, and RATIR telescopes. These consist of 133 detections and 94 upper limits. We constructed average light curves in the observer and rest frames in both X-rays (from Swift/X-Ray Telescope) and the optical. Our analysis focused on investigating the observational and intrinsic properties of GRBs. Specifically, we examined observational properties, such as the optical brightness function of the GRBs at T = 1000 s after the trigger, as well as the temporal slope of the afterglow. We also estimated the redshift distribution for the GRBs within our sample. Of the 227 GRBs analysed, we found that 116 had a measured redshift. Based on these data, we calculated a local rate of ρ0 = 0.2 Gpc−3 yr−1 for these events with z < 1. To explore the intrinsic properties of GRBs, we examined the average X-ray and optical light curves in the rest frame. We use the afterglowpy library to generate synthetic curves to constrain the parameters typical of the bright GRB jet, such as energy (〈E0〉 ∼ 1053.6 erg), opening angle (〈θcore〉 ∼ 0.2 rad), and density (〈n0〉 ∼ 10−2.1 cm−3). Furthermore, we analyse microphysical parameters, including the fraction of thermal energy in accelerated electrons (〈ϵe〉 ∼ 10−1.37) and in the magnetic field (〈ϵB〉 ∼ 10−2.26), and the power-law index of the population of non-thermal electrons (〈p〉 ∼ 2.2).

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COATLI: an all-sky robotic optical imager with 0.3 arcsec image quality

Cited by 6 publications

References 11 publications

DDOTI: the deca-degree optical transient imager

DDOTI: the deca-degree optical transient imager

GRB 191016A: The onset of the forward shock and evidence of late energy injection

Understanding the nature of the optical emission in gamma-ray bursts: analysis from TAROT, COATLI, and RATIR observations

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