Acta Polytechnica

The recent extensive digitisation of astronomical photographic plate archives, the development of new dedicated software and the use of powerful computers have for the first time enabled effective data mining in extensive plate databases, with wide applications in various fields of recent astrophysics. As an example, analyses of supermassive binary black holes (binary blazars) require very long time intervals (50 years and more), which cannot be provided by other data sources. Examples of data obtained from data mining in plate archives are presented and briefly discussed.


BOOTES-2), w
en observing optical transients (OTs) of diverse nature.

Introduction

The majority of the sources visible in the sky have variable emission.Some of them vary in a long timescale compared to the human life.But most of them have shorter variability and, because of that, are continuously observed by telescopes both on Earth and space.The study of variability provides one of the most direct clues on the size and physical characteristics of the emitting object.In the highest energy regime (X-rays, γ-rays) the scales are related to orbits around compact objects (i.e. the result from the death of massive stars).For longer wave-lengths variability is related to larger regions and/or bigger stars.The most extreme case is the study of microwaves, that allows the study of large structures in the Universe.This shows that it is important for astrophysicists to continuously observe our changing Universe, from the smallest to the largest scales, for its understanding.

The study of variable sources in the optical regime can be performed from the Earth surface.Furthermore, it is a window for the study of many complex physical processes occurring at intermediate space/time scales (see the previous paragraph).In this regime we can study (variable) stars (e.g.erupting variables, novae, cataclysmic variables,... etc.), the most violent physical processes in the Universe (Super-Novae -hereafter SNe -and Gamma-Ray Bursts), the relatively quiet Active Galactic Nuclei (AGN) and Quasars (QSOs) and the outer discs and stellar-companions around compact objects (neutron stars and black holes).Nevertheless, the window is still open to discoveries of new types of transients.Recently, thanks to the advance of devices and detectors, new phenomena are being studied (gravita-tional lenses, binary mergers, stellar tidal disruptions by black holes).It is natural to wonder whether there are new (undiscovered) types of physical processe (sources) giving rise to new kinds of observed emission.

Observations in the optical are performed by big and medium-sized telescopes on Earth.The former are not suitable for performing the rapid follow-up needed for the study of optical transients (as we will explain hereafter).These transients events are typically of short duration (from fractions of a second to a few days), because the physical processes that originate them are of limited duration/spatial extent.Robotic smaller telescopes are very well suited for performing such studies.This is due to several factors: their observing flexibility, their rapid response and slew times and the fact that they can be located worldwide working remotely (therefore allowing continuous monitoring).Of course, additional observations might be triggered after the transient has been detected with large X-ray/Optical Observatories.In this way we can

rform deep studies on the nature of these sources.


The Burst Optical Observer
nd

Transient Exploring System and its Spectrographs BOOTES (acronym of the Burst Observer and Optical Transient Exploring System) is a world-wide network of robotic telescopes.It was originally designed from a Spanish-Czech collaboration that started in 1998 ( [1,2]).The telescopes are located at Huelva (BOOTES-1), Malaga (BOOTES-2), Granada, Auckland (BOOTES-3) and Yunnan (BOOTES-4)

located a
Spain, New Zealand and China, respec-


PREPRINT

tively.There are plans of extending this network even further (Mexico, South Africa, Chile,...).These telescopes are medium-sized (D = 30 − 60 cm), autonomous and very versatile.They are very well suited for the continuous study of the fast variability from sources of astrophysical origin (Gamma-Ray Bursts -hereafter GRBs -and Optical Transientshereafter OTs -).Currently two spectrographs are built and working properly in the network at Malaga and Granada (in the optical and infra-red, respectively).In Sec. 2 we will show preliminary results obtained so far with COLORES at BOOTES-2

n the fi
ld of OTs of astrophysical origin.


COLORES

COLORES stands for Compact Low Resolution Spectrograph ( [3]).It is a spectrograph designed to be lightweight enough to be carried by the high-speed robotic telescope 60 cm (BOOTES-2).It works in the wavelength range of (3 800 − 11 500) Å and has a spectral resolution of (15 − 60) Å.The primary scientific target of the spectrograph is a prompt GRB follow-up particularly the estimation of redshift.

COLORES is a multi-mode instrument that can switch from imaging a field (target selection and precise pointing) to spectroscopy by rotating wheelmounted grisms, slits and filters.The filters and the grisms (only one is mounted at the moment) are located in standard filter wheels and the optical design is comprised of a four-element refractive collimator and an identical four-element refractive camera.As a spectroscope, the instrument can use different slits to match the atmospheric seeing, and different grisms in order to select the spectral resolution a cording to the need of the observation.

The current detector is a 1 024×1 024 pixels device, with 13 micron pixels.The telescope is a rapid and lightweight design, and a low instrument weight was a significant constraint in the design as well as the need to be automatic and autonomous.For further details on description, operation and working with COLORES we refer to M. Jeli

k PhD thesis and
eferences therein.


Scientific goals

The BOOTES scientific goals are multifo

, and are detailed in the following.


• Obs
rvations of GRB optical counterparts:

There have been several GRBs for which the optical counterpart has been detected simultaneously to the gamma-ray event, with magnitudes in the range 5 th −10 th .These observations provide important results on the central engine of these sources.The fast slewing 0.6 cm BOOTES telescopes are providing imp rtant results in this field ( [4]).

• The detection of OTs of cosmic origin: These events could be unrelated to GRBs and could constitute a new type of astrophysical phenomenon (perhaps associated to QSOs/AGN).If some of them are related to GRBs, the most recent GRB models predict that here should be a large number of bursting sources in which only transient Xray/optical emission should be observed, but no gamma-ray emission.The latter would be confined a jet-like structure and pointi g towards us only in a few cases.

• Monitoring a range of astronomical objects: These are astrophysical objects ranging from galactic sources such as comets, cataclysmic variables, recurrent novae, compact objects in X-ray binaries to extragalactic sources such as distant SNe and AGN.In the latter case, there are hints th

sudden and rapid flares occur.


Scientif
c results using BOOTES-2/COLORES

In the following we present some important scientific results obtained using BOOTES-2 and its lowresolution spectrograph COLORES, since the beginning o

its operatio
(Summer of 2012).


GRB 130606A

Since the first light on 1998, more than a hundred of GRBs have been observed with BOOTES, some of them only ≈30 s after the onset of the gamma-ray event.The majority of the results have been published in circulars and refereed journals1 .Here we focus on the recent event occurred on 6 th June (2013).A ≈275 s cosmic gamma-ray burst (GRB 130606A) was recorded by Swift and KONUS-Wind on 6 th June 2013, 21:04:34 U.T. (T0) ( [5,6]) displaying a bright afterglow (the emission at other wavelengths following the gamma-rays) in X-rays, but no apparent optical transient emission ( [7]) in the range of the UVOT telescope aboard Swift.BOOTES-2 station automatically responded to the alert and an optical counterpart was identified ( [8]), thanks to the spectral response of the detector up to 1 µm, longer than that of Swift/UVOT (0.17-0.65 µm).We refer to [9] for details on th

observations and results.


TCP J17154683-3
28303 = NOVA SCORPIUS 2014

Following the discovery on 26 th March (2014) of a 10 th mag new source in Scorpius dubbed TCP J17154683-3128303 by [10] also detected by Swift on Mar 27 ( [11]), [12] report that an optical spectrum was obtained with the COLORES spectrograph at the 0.6 m robotic telescope at the BOOTES-2 astronomical station (see Figure 1).


Optical spectra from red-dwarf flaring stars

The Swift team reported on the detection of a
superflare from one of the stars in the close visual dM4e+dM4e flare star binary system DG CVn.The Burst Alert Telescope (BAT) triggered on DG CVn the 23 rd April (2014) at 21:07:08 UT = T0 ( [14]).BOOTES-2/COLORES has been observing DG CVn since the beginning of the superflare and new interesting optical spectral variability following the X-ray superflare evolution has been observed (we refer to [15] for further details).Additionally, following the detection and subsequent monitoring of the new outburst from the RS CVn UX Ari by SWIFT and MAXI ( [17,18]), the 0.6 m robotic telescope at the BOOTES-2 astronomical station, obtained optical (4 000-9 000) Å spectra starting at 19 th July (2014), 01:32:24.382UT and ending at 04:25:55.652UT. [16] report that the optical spectra contain broad molecular TiO, CaI, MgI, NaI lines plus a red continuum (see Figure 2).These spectra lack of any significant Balmer lines in emission.These spectral features are indicative of a late-type star spectrum (as previously reported).Nevertheless, there are no indications of important chromospheric activity, that might have been disappeared by the time of our observations.


Discussion and conclusions

The era of OTs is about

start.Since the beginning
f the modern times the big telescopes have been the only resource for astronomers to study astrophysical sources.In spite of constituting the best tool for deep studies of individual targets, they are not properly suited for the discovery of optical transient sources.Their big size limits the speed they can cover the entire sky and the time for overheads might be longer than that for medium-sized telescopes.Many factors make them difficult to fully automatize and indeed currently none is completely robotic and autonomous.Medium-sized telescopes (i.e.D≤1 m) can be much quicker moving from target to target and time overheads are usually very small.Therefore, robotic medium-sized telescopes are currently the best ones for the follow-up and studies of the longterm variability of the astrophysical transient sources.

BOOTES-2 constitutes one step forward with respect to any ro otic telescope on Earth that has existed so far.This is because it is the first robotic telescope with a spectrograph mounted on it which has demonstrated to work properly.This does not allow only to perform early follow-up and to measure the redshift of GRBs, with cosmic origin, but also to perform early follow-up (both photometric and spectroscopic) of transient sources, often located much more nearby.These OTs might have been reported at other wave-lengths (typically at X-and γ-rays), which would create an alert to the scientific community (often through an Astronomer Telegram).In such a case the observer (remotely) sends the telecommands to start the observation with BOOTES-2, that re-observes the target every time it is visible during the following nights.

Apart from the intensive campaign of follow-up of GRBs performed by the BOOTES network (≈100 GRBs have been observed so far), BOOTES-2 and its spectrograph (COLORES) are providing excellent results in the field of OTs, too.In this paper we mention a few of them, obtained during the last 1.5 year (since the spectrograph was mounted on the telescope).But this is only the beginning and we look forward to follow many OTs for understanding better their physical properties and may be also to discover and follow-up new kinds of OTs.This will prepare us for the advent of the Large Synoptic Survey Telescope (LSST), the biggest telescope ever built on Earth for the study of the entire sky, that will allow the discovery of many kinds of new astrophysical sources (if they exist) and follow-up of OTs, planned to start operations on 2023.


PREPRINT

Figure 1 .
1
Figure 1.Optical spectrum in the range (3 8