A new set of gratings with medium resolution (R ∼ 7500) has been mounted on the LAMOST spectrographs, and the wavelength windows range in 490 ∼ 540nm and 640 ∼ 690 nm respectively for blue and red spectrograph arm. Commissioning observation has been conducted to test the survey based on 16 spectrographs and 4000 fibers. Meanwhile, a spectral analysis pipeline has been developing to get more precise stellar parameters, radial velocities and abundance of chemical elements. Instrument profiles are calculated for each fiber at each exposure according to emission lines both from arc lamp. A template grid spectra with R ∼ 7500 for fundamental parameter (Teff, logg, and [Fe/H] ) are selected from Elodie. During the commissioning observation, each star have been visited for several times, and a fraction targets include APOGEE, Kepler and PASTEL objects which have high precisely measured parameters. With the commissioning spectra, we can understand instrument performance, intrinsic precision of repeat observations, and the accuracy of the pipeline.
The large sky area multi-object fiber spectroscopic telescope (LAMOST) is an innovative reflecting schmidt telescope,
promising a very high spectrum acquiring rate of several ten-thousands of spectra per night. By using the parallel
controllable fiber positioning technique, LAMOST makes reconfiguration of fibers accurately according to the positions
of objects in minutes and fine adjusting the fibers. During telescope observation period, each optical fiber unit positional
accuracy directly determines the quality of subsequent spectrum acqusition, yet for real-time optical fiber positional
accuracy, there only exists an internal information feedback which focus on the corresponding stepper motor driving
conditions, however, this available information is not comprehensive, it can not offer the actual positional information
for each fiber unit. Considering the LAMOST on-site environment, a novel real-time optical fiber positional accuracy
detection system which can be integrated in the existing observation and control system need to be developed to solve
this problem. During the observation interval, this system can offer a comprehensive and effective information feedback
about the focal optical fiber positional accuracy. Based on this feedback, the observation assistants can properly adjust
the observation strategies to ensure the effectiveness and accuracy of acquired spectrum. Furthermore, this fiber
positional accuracy feedback can provide prior spectral quality information to the spectral processing personnel and
optimal the spectrum processing efficiency.
LAMOST is a 4m reflecting Schmidt telescope special designed for conducting multifiber spectroscopic survey with 4000 fibers. Fiber position errors greatly impact spectral data SNR. There are three groups of sources that contribute to fiber position errors: errors orthogonal to the optical axis of telescope, errors parallel to the optical axis, and the fiber tilt from the telescope optical axis. It is difficult to measure these errors, especially during the observation. In this poster, we propose an indirect method to calculate the total and systematic position errors for each individual fiber from spectra data by constructing a model of magnitude loss due to the fiber position error for the point source.
A new method to calculate the optical vignetting of LAMOST (Large Sky Area Muti-Object Fiber Spectroscopic
Telescope) is presented. With the pilot survey of LAMOST, it is necessary to have thorough and quantitative estimation
and analysis on the observing efficiency which is affected by various factors: the optical system of the telescope and the
spectrograph that is vignetting, the focal instrument, and the site condition. The wide field and large pupil of LAMOST
fed by a Schmidt reflecting mirror, with a fixed optical axis coinciding with the local polar axis, lead to significant
telescope vignetting, caused by the effective light-collecting area of the corrector, the light obstruction of the focal-plate,
and the size of the primary mirror. A calculation of the vignetting has been presented by Xue et al. (2007), which
considered 4 meter circle limitation and based on ray-tracking. In fact, there is no effect of the 4 meter circle limitation,
so that we compute the vignetting again by means of obtaining the ratio of effective projected area of the corrector. All
the results are derived by AUTOCAD. Moreover, the vignetting functions and vignetting variations with declination at
which the telescope is pointed and the position considered in the focal surface are presented and analysed. Finally,
compared with the ray-tracing method to obtain the vignetting before, the validity and availability of the proposed
method are illustrated.
The LAMOST1,2 telescope is expected to have its first light in later of 2007. The 4-meter aperture and 4000-fiber feeding ablility will make it a powerful spectra sky survey instrument, as well a challenge to the mission of data processing and analysis. So far several statistical methods, mainly based on PCA, have been developed for spectra automatic classification and red shift measurement by a team of LAMOST3. Statistical methods of Hidden Markov Modelling have become popular in many area since 1990s, which are rich in mathematical structure and can form the theoretical basis for use in a wide range of applications, e.g. speech recognition and pattern recognition. No doubt they are prospective implements for automatic spectra processing and analysis. In this paper, I attempt to briefly introduce the theoretical aspects of this type of statistical modelling and show the possible applications in automatic spectra data processing and analysis.
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