- Express Letter
- Open Access
Autonomous spectrographic system to analyse the main elements of fireballs and meteors
© The Author(s) 2018
- Received: 11 March 2017
- Accepted: 19 December 2017
- Published: 3 January 2018
Meteor spectra studies started in the 1860s by means of the observations taken by A.S. Herschel (Millman 1963). Photographic techniques have been used to study meteor spectra since the end of the nineteen century (Millman 1980), and transmission gratings started to replace prisms in meteor spectrographs since the 1950s. Broad spectroscopy programmes were carried out in USA, Canada, the former USSR and Czechoslovakia (Ceplecha et al. 1988). New video techniques to study meteor spectra started to be used in the early 1970s (Hemenway et al. 1971), as well as new methods and TV processes for data reduction, described by Millman and Clifton (1975), Borovicka and Bocek (1995) and Zender et al. (2004). Meteor spectroscopy is based on the emission of atomic lines (emission spectra), along with other molecular bands and continuous radiation. Early on, Halliday (1961), Ceplecha (1971) and Borovička (1994a) provided significant identification lists of lines in high-dispersion photographic spectra. Meteor emission lines can be divided into two components according to their temperature (high and low) (Borovička 1994b).
Video techniques allow the recording of relatively faint meteors (Espartero and Madiedo 2016 and references therein) in comparison with photographic images, so only certain emission lines can be detected, such as Na, Mg, Ca and Fe, in addition to the O, N and N2 atmospheric emissions (obtained by low-resolution spectroscopy). With our video systems, we can capture meteors with apparent visual magnitude as faint as 3 ± 1 (Madiedo et al. 2016), but the spectrographic equipment is limited to the spectral study of fireballs with visual apparent magnitude of − 4 and brighter.
Light emitted by meteors during the ablation process in the terrestrial atmosphere allows us to study, by means of spectrographs, the chemical nature of their parent bodies. Thus, the analysis of the spectrum of a given meteor can provide distinct information about the plasm, the ablation process and the chemical composition of the meteoroid (Borovička 1993, 1994a; Trigo-Rodríguez et al. 2003) and even relevant information about its parent body.
This new system for capturing spectroscopic images has been designed in order to obtain more detailed and complete emission spectra from bright bolides and meteors with higher spectral resolution when compared to video techniques. This system is the first in a series of three stations that are foreseen to be located at a minimum distance of 100 km from each other, in order to be able to calculate the atmospheric trajectory, radiant of origin and orbit of its progenitor in the solar system (Ceplecha 1987) from at least two stations, in addition to analysing the corresponding meteor spectra.
The existing spectrographic equipment we have developed is located at the Andalusian Astronomical Observatory (37°24′54″N, 3º57′12″W), a dark location at 1030 m above the sea level, in south Spain (close to the Alcalá la Real village). The equipment has been connected to a weather station that regulates the proper functioning of the spectrographs. The station allows the equipment to automatically start operating at sunset and being disconnected at sunrise on a daily basis.
We use two different spectrographs, with different optical configurations and CCD cameras, to attempt to get images with different fields of view and sensitivity for the same fireball. The combination of these images allows to capture the complete fireball phenomenon and obtain precise details thereof.
To assemble all the elements that form the spectrograph, firstly, all elements were adjusted manually to obtain a precise optical focus and its stability. For each of the two spectrographs, the resulting block (CCD case + adapter + objective + grating) was then inserted inside two concentric polyvinyl chloride (PVC) tubes. These tubes are covered at their upper end with a special glass, perfectly sealed with a silicone elastomer, which allows both waterproofing and preventing temperature differences from impairing the connection joint (Fig. 1).
The equipment is connected to two computers in which the recorded images are saved to the hard drive. Moreover, all the devices that form this system can be controlled at distance and programmed in advance.
The main elements of the spectrographs (CCD cameras, wide-field objectives and diffraction gratings, support and protection) are described below.
Description of main features of the two CCDs used in the spectrographs
1392 × 1040
10.2 × 8.3
Kodak KAI 11002
4008 × 2672
37.25 × 25.7
Wide-field objectives and diffraction gratings
Two different photographic lenses are used. On the one hand, a Sigma 4.5 mm f/2.8 EX DC HSM objective is attached to the Atik 314L + CCD, which provides a 120º field of view and is adapted by a male/female aluminium adapter to achieve a good focus. On the other hand, a 50 mm f/1.2 Nikon objective that provides a field of view of 15° is also attached to the Atik 11000 CCD via an adapter cap.
Facing each objective and with only a 0.67 mm maximum separation, the 1000 lines per mm holographic grating are connected over a filter adaptor, which varies in each device depending on its size. This allows for a quick and easy handling for its maintenance, given that every 6 months the grating must be replaced by a new one to obtain optimum results and prevent its deterioration (as solar radiation and temperature changes deteriorate the joint between the grating and the objective, causing its detachment).
Support and protection
Protection systems for the spectrographs have been specifically designed and created for this set of elements, as per the dimensions and needs of each device. The individual PVC protection consists of two concentric tubes whose dimensions fit the CCD and other elements that shape our device. The PVC tubes only have a 8-mm difference in diameter between them, in the case of spectrograph #1 (96/88 mm) and a 6-mm difference in spectrograph #2 (130/124 mm) as Fig. 1a shows. This lets both tubes fit inside each other and move relative to one another. They serve as fastening and anchoring for the cameras and optical systems. In the first experimental and test phase, adaptors with different height overlapping rings threaded between the CCD detector and the objective were placed to obtain the adequate focal length that would allow us to get sharp images. These elements were inserted inside two PVC tubes, which allow the whole set to be handled and moved without any relevant optical disturbances. The upper part of the tube is covered by 1-mm-thick float glass and with the same diameter as the tube, in order to correctly fit and being sealed with a special silicon cord for glass and exterior.
The last element that comprises this system is the regulated heating tape, which is connected to the upper part of the tube, surrounding the protection glass. This tape prevents frost formation as well as the condensation of water vapour (mist), both inside and outside. It has been built with a printed flexible circuit and surface mounted device (SMD) resistance, isolated with silicone and thick fabric to avoid heat loss.
For the spectrographs to be operated in a reliable and durable way, an AES (Fig. 2) has been designed and built, which can be manipulated remotely via the Internet. The automatic module is built with a structure of 10 × 10 mm square section steel bars with electrowelded joints, which allows us to place the necessary trays and supports for the mechanical elements that give mobility to the leaning roof. As outer coating, panels of 2-mm-thick galvanized sheet have been placed in both walls and the sliding roof. The roof of the observatory has been designed with a double leaning slope whose opening and closing are done in an opposed and synchronized way (Fig. 2).
Inside, the spectrographs are placed on the supports, as well as the various devices that allow for the opening and closing of the roof. The activation of the roof of this small observatory is achieved by two 24-V electric engines, which are activated through two relays, current intensity transformers and a programmer. These electronic devices are programmed and regulated through the control computer and allow us to move the roof accordingly. This ensemble is connected to the 220 V electric current through a system of uninterrupted power source, which also allows us to control the possible oscillations in voltage and amperage that may damage the equipment. The AES controller is based on the astronomical weather station input.
Astronomical weather station
A weather station for astronomy (dubbed EMA) weather station was specifically designed to control and measure the atmospheric and sky quality parameters in order to guarantee that observations are performed in safe conditions.
The EMA weather station measures, among other parameters, the sky brightness (using a Sky Quality Meter), the speed of air (by means of an anemometer) or the cloud index (thanks to a Peltier system that measures the difference in infrared radiation between the ground and the sky), the latter being the most relevant indicator for our protection system, as we choose to close the protection if it surpasses the 70% fraction of clouds in the sky. At this point, the EMA sends a signal to the AES to close its sliding roof, while the CCDs are switched to ‘standby’ mode until the cloud cover value decreases below the threshold and the system resumes operation again.
The process that allows the correct functioning of the system (protection module, spectrographs and computers) is the following one. The ensemble is connected to the EMA of the Andalusian Astronomy Observatory, which activates the system at sunset and deactivates it at sunrise, thus allowing it to stay disconnected and the protection module to remain closed during the daytime hours. The switching on/off depends on the magnitude of sky brightness, and it is not necessary to update an astronomical clock or timer with the passage of days, since its autoregulation is autonomous (Trueblood and Russel 1985).
Daily operations begin with the aperture of the AES soon after twilight, provided the sky’s brightness value is < 12 mag/arcsec2, as these lower values would saturate the images obtained. This value drops again shortly before the sunrise, at which time the systems stop functioning and the AES closes. The computers remain on hibernation mode every day and are activated automatically at twilight, continuing to store the images into the corresponding hard drives.
The spectrographs obtain different types of images depending on their optical lens and CCDs combinations. With spectrograph #1 (the wide-field spectrograph), images of up to 250 kB providing a field of view of 120° are obtained, and with spectrograph #2 (the narrow field spectrograph), images of up to 2.2 MB providing a field of 15° are gathered, reaching limiting magnitudes of 9 and 11, respectively (when comparing to the stellar catalogue USNO-B1.0), if atmospheric conditions and seeing are optimal. Download time is 2 and 5.2 s for spectrographs #1 and #2, respectively, with optimal exposure times being 60 s for spectrograph #1 and 90 s for spectrograph #2. These times are halved during the previous and following days around the full moon phase, thus avoiding the saturation of the images to a great extent.
The data are stored in the hard drives of two computers (one for each spectrograph), so when a fireball alert is received (by e-mail) through the Spanish Meteor Network (SPMN), the images can be pinpointed by date and time. Capturing images is done with the original ARTEMI software provided by the Atik CCD manufacturer, and the data are saved in FITS format.
The image reduction process is done by subtracting the previous or following image to the image containing the fireball, with the dark and bias being subtracted with the MAXIM DL software.
The first and second orders of the spectrum are present, and in some cases, due to the brightness of the fireball, the signal corresponding to the first order can saturate during a part of its atmospheric trajectory. The CHIMET software (Madiedo et al. 2011) has been used, as it can provide valuable information of the studied objects through a synthetic spectrum. The basic procedure has been described in Trigo-Rodríguez et al. (2003).
In the case of fireballs with apparent visual magnitude of − 4 and brighter, the system can provide their low-resolution spectra, thanks to the holographic diffraction grating. A minimum integration time of 2 s is required in order to obtain high quality. Sometimes, the result obtained may not be good enough, since it also depends on the geometric position of the diffraction grating with respect to the angle of incidence of the spectral emission. The first and second orders of the spectrum may be present depending on the time and apparent magnitude of the meteor, but in some cases and due to the intense brightness of the fireball, the signal corresponding to the first order may become saturated during part of its atmospheric trajectory. For its correct analysis, it is necessary then to resort to the second order of the spectrum.
To properly obtain the spectrum, we first determine the intensity profile by comparing the pixel brightness (in arbitrary intensities) versus the number of pixels along the given direction. The spectrum is analysed and calibrated automatically in intensity and wavelength by means of the CHIMET software mentioned above (Madiedo et al. 2011), in order to identify the main wavelengths with different chemical species, such as Na, Mg, Fe, Ca or Cr. To this end, the program uses a database containing the main frequencies and typical emissions of meteor spectra. These frequencies have been taken from the NIST Atomic Spectra Database (http://physics.nit.gov/PhysRefData/ASD/lines_form.html). Thus, the software can superimpose the theoretical spectral lines with the new lines of the observed spectrum. Then, it selects some known lines of the spectrum, such as Na and Mg, and the software automatically sets the different positions of other well-known theoretical lines.
The video cameras of the SPMN showed that its brightness reached -7. As it was not possible to identify the origin of this meteor, it was considered to be of sporadic origin. Our analysis of its spectral lines clearly indicates the most prominent emission features due to the Na I-1 (5889 Å) and Mg I-2 (5167 Å) lines together with the Fe I-15 multiplets (5269 and 5429 Å). The numbers of the multiplets are given according to Moore (1945), with the most relevant ionized species being highlighted according to the most intense lines and peaks.
On the other hand, it is worth noting the scarce presence of refractory elements such as Ca and Al, which is a common phenomenon in the case of a meteoroid with a low heliocentric velocity (Trigo-Rodríguez 2002; Trigo-Rodríguez et al. 2003). This is due to the inefficiency of providing all the available Ca or Al in its vapour phase. Thus, it was previously reported (Trigo-Rodríguez et al. 2003) that, in the chondritic meteoroids, the elements Ca and Al are associated with refractory minerals that do not complete their vaporization during the ablation phase (Trigo-Rodríguez 2002; Trigo-Rodríguez et al. 2003; Trigo-Rodríguez and Llorca 2007).
The chemical abundances of the main spectral elements of a meteor provide a more detailed information if we consider the classification of its populations (Borovička et al. 2005) and the comparison of the ratios of its chemical elements by means of ternary diagrams (Trigo-Rodríguez et al. 2003). These techniques allow us to study the nature of fireballs that are captured by our spectrographs from 2013 to 2016 and that are analysed in Espartero et al. (2017). In some cases, it has been possible to gather video images from two or more stations, which allows us to complete our work with the orbital analysis of their parent bodies, providing their radiant and most relevant parameters.
The spectra images obtained with this method allow us to analyse fireballs with apparent magnitude of − 4 and brighter and whose trajectory, with the aforementioned brightness, lasts at least 2 s.
The spectra obtained cover the range from 3700 to 10000 Å, including the first- and second-order spectra.
The chemical abundances analysed in the Alcalá la Real fireball spectrum presented in this work indicate that it could be a sporadic object with a chondritic nature.
For the future, we aim at expanding the network of spectrographs, incorporating two new stations, at > 100 km distance each other, which will allow altogether to determine the atmospheric trajectory, the apparent radiant in the sky, and the orbit of the parent object. We also plan to use fish-eye optics for the future spectrographs, in order not to lose the fireballs that happen to occur close to the horizon. The image acquisition must be also configured alternatively in order to continuously cover the visible sky. This will ensure the full performance of these devices.
Espartero performed the instrumentation set-up and data analysis and drafted the manuscript. Martínez, Frias and Montes participated in designing the instrumentation and helped draft the manuscript. Castro-Tirado participated in designing the study and interpreting the results, and helped draft the manuscript. All authors read and approved the final manuscript.
We thanks the support of the M.I. Ayuntamiento de Alcalá la Real, the Diputación de Jaén, the Spanish Meteor Network (SPMN) and the Spanish Ministry through Project AYA 2015-71718-R (including FEDER funds). We thank A. Castellón (University of Málaga) for fruitful discussions. We also acknowledge the useful comments from the referees, as they have helped to significantly improve this manuscript.
The authors declare that they have no competing interests.
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