scholarly journals Echelle spectrograph at the 2.6 m Shajn telescope

2020 ◽  
Vol 1 (1) ◽  
pp. 33-38
Author(s):  
Aleksandr Lagutin ◽  
Sergei Plachinda ◽  
Dmitrii Shakhovskoi ◽  
Evgenii Nekhai ◽  
Dilyara Baklanova ◽  
...  
Keyword(s):  
High Resolution ◽  
Crimean Astrophysical Observatory ◽  
Echelle Spectrograph

The paper describes the high-resolution echelle spectrograph ESPL developed for the coude focus of the 2.6 m Shajn reflector of the Crimean Astrophysical Observatory.  The spectrograph has been regularly operated since 2013.  Efficiency of the spectrograph is estimated from observations of stars.

scholarly journals A High Resolution Spectrograph at Weihai Observatory

2012 ◽  
Vol 8 (S293) ◽  
pp. 400-402
Author(s):  
Dongyang Gao ◽  
Dayong Ren
Keyword(s):  
High Resolution ◽  
Echelle Spectrograph ◽  
Metal Abundance ◽  
And Performance

AbstractWeihai Echelle Spectrograph (WES) is the first the fiber-fed echelle spectrograph in China. WES can provide data for the studies of metal abundance of stars, exoplanets researches and asteroseismology, etc. A brief description of its design and performance is given.

scholarly journals Modelling high resolution Echelle spectrographs for calibrations: Hanle Echelle spectrograph, a case study

2015 ◽  
Vol 39 (2) ◽  
pp. 423-443 ◽  
Author(s):  
Anantha Chanumolu ◽  
Damien Jones ◽  
Sivarani Thirupathi
Keyword(s):  
High Resolution ◽  
Echelle Spectrograph

scholarly journals Precise Radial Velocity Measurements with a Cassegrain Spectrograph, I: Wavelength calibration

1999 ◽  
Vol 170 ◽  
pp. 63-67
Author(s):  
I. V. Ilyin ◽  
R. Duemmler
Keyword(s):  
High Resolution ◽  
Radial Velocity ◽  
Cross Correlation ◽  
Time Dependent ◽  
Instrumental Effects ◽  
Velocity Measurements ◽  
Echelle Spectrograph ◽  
Optical Telescope ◽  
La Palma ◽  
Observational Strategy

AbstractWe briefly describe the instrumental effects which affect the accuracy of the radial velocity measurements. We have implemented several methods to correct for the instability effects and improve the accuracy of the measurements. These include modifications of the observational strategy and a time-dependent wavelength solution as well as a discussion of the error of the offset from cross-correlation. These methods are applied to observations obtained with the high resolution échelle spectrograph SOFIN mounted at the Cassegrain focus of the alt-azimuth 2.56-m Nordic Optical Telescope, La Palma, Canary Islands.

scholarly journals High Resolution Spectroscopy of Symbiotic Stars

1990 ◽  
Vol 122 ◽  
pp. 444-445
Author(s):  
Hugo E. Schwarz ◽  
Hilmar W. Duerbeck ◽  
Waltraut C. Seitter
Keyword(s):  
High Resolution ◽  
Southern Hemisphere ◽  
Northern Hemisphere ◽  
High Resolution Spectroscopy ◽  
Symbiotic Stars ◽  
Current Interest ◽  
Echelle Spectrograph ◽  
La Palma ◽  
Recurrent Nova ◽  
The Uk

A high resolution spectroscopy survey of symbiotic stars is conducted in the southern hemisphere by the authors, using the Coudé Echelle Spectrograph (CES), equipped with a CCD at the ESO Coudé Auxiliary Telescope (CAT), and concurrently in the northern hemisphere by Bode, Evans, Meaburn and collaborators, using the UK facilities at La Palma. So far, more than 400 spectra of about 70 stars have been obtained, mostly during 1988 and 1989. The southern part of the work will be described below.The discussion of symbiotic stars in the context of novae is not far-fetched. A number of symbiotics are known to have nova-like outbursts, and several novae are not easily distinguished from symbiotic stars. A noteworthy example is the most recently recognized recurrent nova, V745 Sco, first observed by Liller on July 24, 1989. It is described here, both because in late decline it represents a link between novae and symbiotic stars, and because of its current interest.

scholarly journals Spectroscopic Observations of the Be Stars η Cen, γ Cas and φ Per

1976 ◽  
Vol 70 ◽  
pp. 199-207 ◽  
Author(s):  
W. M. Burton ◽  
R. G. Evans
Keyword(s):  
Data Analysis ◽  
High Resolution ◽  
Main Part ◽  
Visible Region ◽  
Progress Report ◽  
Short Description ◽  
Be Stars ◽  
Royal Greenwich Observatory ◽  
Echelle Spectrograph ◽  
Shell Star

The main part of this paper is concerned with observations obtained using the Princeton ultraviolet telescope-spectrometer on the Copernicus satellite through the Princeton guest investigator programme. These observations provided high resolution ultraviolet spectra of the bright southern shell star η Cen, which are now being analysed in detail. A short description of the new η Cen spectra and a progress report on the data analysis are presented below. In the second part of the paper we describe visible-region spectra of the northern Be stars γ Cas and φ Per obtained with a cross-dispersed echelle spectrograph on the 36-inch Yapp telescope at the Royal Greenwich Observatory.

High-resolution Fourier transform spectrograph for characterization of echelle spectrograph wavelength calibrators

2012 ◽  
Author(s):  
Alexander G. Glenday ◽  
David F. Phillips ◽  
Matthew Webber ◽  
Chih-Hao Li ◽  
Gabor Furesz ◽  
...  
Keyword(s):  
Fourier Transform ◽  
High Resolution ◽  
Echelle Spectrograph

A Discussion on solar studies with special reference to space observations - A high resolution solar ultraviolet spectrum between 200 and 220 nm

1971 ◽  
Vol 270 (1202) ◽  
pp. 29-46 ◽  
Keyword(s):  
High Resolution ◽  
Solar Spectrum ◽  
Ultraviolet Spectrum ◽  
Absorption Feature ◽  
Intensity Analysis ◽  
Echelle Spectrograph ◽  
Broad Absorption ◽  
First Time ◽  
Solar Ultraviolet ◽  
The Continuum

A high resolution solar spectrum in the range 200 to 220 nm has been recorded with an echelle spectrograph launched in, a sun-pointing Skylark rocket. The data have been reduced and are presented as intensity-wavelength plots together with a wavelength list and proposed identifications. A broad absorption feature at 212.4 nm is assigned to a single source and an intensity analysis confirms this to be the non-resonance Sii line at 212.412 nm. The discontinuity in the continuum intensity near 208.7 nm is revealed with high resolution for the first time and is assigned to the photoionization edge of A11. An analysis shows that its intensity drop and wavelength position can only be explained by adjustments to the solar model in the region 0.001 < T 5000 < 0.2.

Improved Non-LTE Model Atmospheres for Subluminous O-Stars

1988 ◽  
Vol 132 ◽  
pp. 117-122
Author(s):  
U. Heber ◽  
K. Hunger ◽  
T. Rauch ◽  
K. Werner
Keyword(s):  
High Resolution ◽  
New Method ◽  
Balmer Line ◽  
Pure Hydrogen ◽  
Line Profiles ◽  
Stark Broadening ◽  
Echelle Spectrograph ◽  
Helium Spectra ◽  
Model Atom

Improved non-LTE model atmospheres designed for the analysis of very hot subluminous O stars are presented. The calculations are based on the new method of the accelerated lambda iteration (ALI) which proves capable of treating up to 100 levels of various ions. Presented here are improved calculations for (i) pure hydrogen model atmospheres including Stark broadening, (ii) for hydrogen- and helium-composed model atmospheres and (iii) first preliminary models which include in addition a detailed carbon model atom. These models remove an apparent mismatch of Balmer line profiles noted previously and fit high S/N, high-resolution hydrogen and helium spectra obtained with the ESO-Cassegrain echelle spectrograph very well.

scholarly journals HIRDES – The High-Resolution Double-Echelle Spectrograph for the World Space Observatory Ultraviolet (WSO/UV)

2008 ◽  
Vol 41 (12) ◽  
pp. 1992-1997 ◽  
Author(s):  
K. Werner ◽  
J. Barnstedt ◽  
W. Gringel ◽  
N. Kappelmann ◽  
H. Becker-Roß ◽  
...  
Keyword(s):  
High Resolution ◽  
Space Observatory ◽  
Echelle Spectrograph ◽  
The World
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