The Fourier Transform Spectrograph (FTS) stands as a powerful tool for astronomers in characterizing the composition of celestial bodies through their emitted light. In this study, we introduce the development and initial performance evaluation of a fiber-fed FTS, specifically tailored for solar observations within the 600-1000 nm wavelength range. To improve measurement precision, we integrated a stabilized He-Ne laser as a metrology wavelength source. This setup generates a monochromatic interferogram in parallel with the scientific interferogram, allowing for adaptive correction of the instrument's non-linear scan characteristics that affect the phase information of the scientific interferogram. For wavelength calibration, we employed well-defined oxygen (O2) lines as a reference. The comparison of the solar spectrum measured with our system against a simulated model showed good agreement affirming the system's efficacy. Additionally, we discuss the wavelength calibration using O2 lines in the telluric region, offering insights into the system's repeatability. The analysis of the Fe-I absorption line within these lines further enabled us to determine the Sun's rotational velocity.
The Fourier transform spectrograph (FTS) is one important tool that has been used to analyze and characterize the radiated energy distribution of the stellar objects through an atmosphere. Most of the current spectrographs were installed at the telescope focal plane of the telescope, which required the space and complexity of alignments. The implementation of a fiber to feed the light from the telescope has been implemented to overcome those limitations. However, a small flux due to the single point field of view becomes a main challenge of this system. In this work, we report the development of the laboratory prototype of a fiber-fed FTS by using off-the-shelf components specifically designed for the Thai National Telescope (TNT). The method used to process the data relies on the cubic spline interpolation for resampling of both scientific and metrology interferograms and producing the spectrum from the raw measurements. The current maximum optical path difference is about 30 mm with an achievable spectral resolving power higher than 19,000 based on the instrument line shape of the system. The results obtained by concentrating the Sun light with the signal-to-noise-ratio (SNR) greater than 20 are presented. We also present the preliminary results of the low flux detection from a dim halogentungsten source comparable to the magnitude of a bright star in the order of a few nano-watts. The implementation of a phase-lock amplifier has been investigated to detect the signal and improve the signal-to-noise-ratio of the spectrum.
We present the design and performance verification of a fiber-fed Fourier transform spectrograph (FTS) for spectroscopy in the optical band with the ability to reach a maximum optical path difference of 15 mm and allowing for an adjustable spectral resolution (λ / Δλ) between 1 and 15,000. The designed FTS system was successfully constructed using only off-the-shelf optical components. The technique for correction of the phase distortion in the FTS using a metrology interferogram and cubic spline interpolation was investigated and discussed. The contrast performance and the instrument line shape of the FTS were measured and analyzed. To further verify the performance of the developed system, the absorption spectrum of the sunlight was measured and compared with a synthetic model with identified telluric and absorption lines. The result shows that the developed FTS can detect the absorption lines with a spectral resolution close to 15,000.
The EXOplanet high resolution SPECtrograph (EXOhSPEC) instrument is an echelle spectrograph dedicated to the detection of exoplanets by using the radial velocity method using 2m class telescopes. This spectrograph is specified to provide spectra with a spectral resolution R < 70, 000 over the spectral range from 400 to 700 nm and to reach a shortterm radial velocity precision of 3 m/s. To achieve this the separation between two adjacent spectral orders is specified to be greater than 30 pixels and to enable a wide range of targets the throughput of the instrument is specified to be higher than 4%. We present the results of the optimization of the spectrograph collimator performed and initial tests of its optical performance. First, we consider the spectrograph design and we estimate its theoretical performance. We show that the theoretical image quality is close to the diffraction limit. Second, we describe the method used to perform the tolerancing analyzes using ZEMAX software to estimate the optical performance of the instrument after manufacturing, assembly and alignment. We present the results of the performance budget and we show that the estimated image quality performance of EXOhSPEC are in line with the specifications. Third, we present the results of the stray light analysis and we show that the minimum ratio between the scientific signal and the stray light halo signal is higher than 1,000. Finally, we provide a status on the progress of the EXOhSPEC project and we show the first results obtained with a preliminary version of the prototype.
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