Night-Sky High-Resolution Spectral Atlas of OH Emission Lines for Echelle Spectrograph Wavelength Calibration. II.

1997 ◽  
Vol 109 ◽  
pp. 614 ◽  
Author(s):  
D. E. Osterbrock ◽  
J. P. Fulbright ◽  
T. A. Bida
Keyword(s):  
High Resolution ◽  
Emission Lines ◽  
Echelle Spectrograph ◽  
Wavelength Calibration ◽  
Night Sky

scholarly journals Night-Sky High-Resolution Spectral Atlas of OH and O2 Emission Lines for Echelle Spectrograph Wavelength Calibration

1996 ◽  
Vol 108 ◽  
pp. 277 ◽  
Author(s):  
Donald E. Osterbrock ◽  
Jon P. Fulbright ◽  
Andre R. Martel ◽  
Michael J. Keane ◽  
Scott C. Trager ◽  
...  
Keyword(s):  
High Resolution ◽  
Emission Lines ◽  
Echelle Spectrograph ◽  
Wavelength Calibration ◽  
Night Sky

scholarly journals An optical fiber feed for small telescopes

1986 ◽  
Vol 118 ◽  
pp. 115-116
Author(s):  
W. G. Weller ◽  
T. E. Ingerson
Keyword(s):  
High Resolution ◽  
Optical Fiber ◽  
Instrument Development ◽  
Spectral Response ◽  
Conservative Estimate ◽  
Echelle Spectrograph ◽  
Wavelength Calibration ◽  
Fiber Link ◽  
Development Laboratory

We have constructed an optical fiber link between the CTIO 1.5 meter telescope and the instrument development laboratory located in the 4 meter telescope building. We have successfully observed a variety of objects using the 4 meter échelle spectrograph fed with light from the 1.5 meter telescope. These first observations indicate that the system is extremely stable, both in its spectral response and in wavelength calibration. The principal aim of the project was to provide the capability of recording high resolution spectra at the 1.5 meter, using linear detectors. Even with the loss of light associated with the use of the fiber, a conservative estimate of the speed of the system indicates a factor of 20 increase in speed over the existing coudé spectrograph.

scholarly journals Spectral Line Variations of Symbiotic Stars EG And, AG Dra, and BX Mon and Its Interpretation

2012 ◽  
Vol 8 (S290) ◽  
pp. 353-354
Author(s):  
Tae Seog Yoon ◽  
Soo Hyun Kim ◽  
Hyeonwoo Moon ◽  
Kyu-Seob Kim ◽  
Hyungil Oh
Keyword(s):  
High Resolution ◽  
Spectral Line ◽  
Emission Line ◽  
Emission Lines ◽  
Symbiotic Stars ◽  
Astronomy Observatory ◽  
Echelle Spectrograph ◽  
Balmer Lines ◽  
Hα Emission ◽  
Optical Astronomy

AbstractWe present some results obtained by high resolution spectroscopic observations for symbiotic stars EG And, AG Dra, and BX Mon in recent years which were performed with 1.8-m reflector and echelle spectrograph BOES at Bohyunsan Optical Astronomy Observatory, Youngcheon, South Korea. The variations of Hα emission line during a night and the variations of H Balmer lines and He I emission lines among several analyzed lines over months and years are shown and discussed.

scholarly journals High Resolution Spectroscopy As a Tool for Luminosity Calibration

2002 ◽  
Vol 12 ◽  
pp. 676-679
Author(s):  
Ruth C. Peterson
Keyword(s):  
High Resolution ◽  
Reasonable Agreement ◽  
Empirical Relationship ◽  
Model Atmosphere ◽  
Stellar Mass ◽  
Physical Basis ◽  
Emission Lines ◽  
High Resolution Spectroscopy ◽  
Chromospheric Emission ◽  
Advance Knowledge

AbstractRecent results are reviewed for two methods of luminosity calibration based on high-resolution spectroscopy. The first relies onTeff/loggdeterminations from model-atmosphere analyses based on high-resolution spectra. This method is physically well founded but operationally demanding, and requires advance knowledge of stellar mass. The second, W-B, stems from the empirical relationship between luminosity and the width of chromospheric emission lines first established by Wilson and Bappu. Its physical basis is only partially understood, however, and the calibration depends on stellar metallicity and on the choice of lines.BothTeff/loggand W-B easily distinguish cool dwarfs from cool giants. Generally reasonable agreement is found between distances derived from Hipparcos parallaxes and those inferred from the loggvalues derived for nearby dwarfs with relatively well-known Hipparcos parallaxes, σ(π)/π < 0.2. Constraining Hipparcos parallaxes star-by-star is not possible at present. Improvements are suggested for both approaches.

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

Wavelength calibration by combining arc and night sky lines for LAMOST

2010 ◽  
Vol 28 (2-3) ◽  
pp. 195-208
Author(s):  
Sheng Wang ◽  
HanQin Qin ◽  
ZhongFu Ye
Keyword(s):  
Wavelength Calibration ◽  
Night Sky

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.

Sign in / Sign up

Export Citation Format

Share Document