The high-resolution spectrograph of the 6-m Large Azimuthal Telescope (BTA)

Панчук, В. Е.; Клочкова, В. Г.; Yushkin, M. V.; Naidenov, I. D.

doi:10.1364/jot.76.000087

Cited by 68 publications

(48 citation statements)

References 2 publications

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“…The observing dates and data spectral ranges are listed in the first two columns of Table 1. Most spectra were obtained with theéchelle spectrograph NES with spectral resolution R = 60000 [19,20]. Our first spectrum obtained on 2001 August 9 was taken with the spectrograph LYNX 1K×1K CCD, R ∼ 25000 [21].…”

Section: Observational Datamentioning

confidence: 99%

High-resolution optical spectroscopy of the yellow hypergiant V1302 Aql (=IRC+10420) in 2001–2014

Клочкова

Ченцов

Мирошниченко

et al. 2016

Mon. Not. R. Astron. Soc.

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We present the results of a study of spectral features and the velocity field in the atmosphere and the circumstellar envelope of the hypergiant V1302 Aql, the optical counterpart of the IR source IRC+10420, based on high-resolution spectroscopic observations obtained in 2001-2014. We measured radial velocities of the following types of lines: forbidden and permitted pure emissions, absorption and emission components of lines of ions, pure absorptions (e.g., He i, Si ii), and interstellar components of the Na i D-lines, K i, and DIBs. The heliocentric radial velocity measured for pure absorptions as well as for the forbidden and permitted pure emissions is close to the systemic radial velocity and equal to V r = 63.7±0.3, 65.2±0.3, and 62.0±0.4 km s −1 , respectively. Positions of the absorption components of the lines with inverse P Cyg profiles are stable and indicate the presence of clumps moving toward the star with a velocity of ∼20 km s −1 . The average radial velocity of the DIBs is V r (DIB) = 4.6±0.2 km s −1 . Comparison of the absorption lines observed in [2001][2002][2003][2004][2005][2006][2007][2008][2009][2010][2011][2012][2013][2014] and those in earlier data shows no noticeable variations. We conclude that the hypergiant reached a phase of slowing down (or termination) of the effective temperature growth and is currently located near the high-temperature boundary of the Yellow Void in the Hertszprung-Russell diagramme.

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Section: Observational Datamentioning

confidence: 99%

High-resolution optical spectroscopy of the yellow hypergiant V1302 Aql (=IRC+10420) in 2001–2014

Клочкова

Ченцов

Мирошниченко

et al. 2016

Mon. Not. R. Astron. Soc.

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“…These observational data are also used to search for peculiarities in the PPN spectra, to analyze the velocity fields in the atmospheres and envelopes of these stars with mass loss, and to search for the likely long-term spectral and velocity-field variations. Here we use the data acquired in the Nasmyth focus with the NES [59,60] and Lynx [61] echelle spectrographs. The NES spectrograph, equipped with a 2048×2048 CCD and an image slicer [62], produces a spectroscopic resolution of R≈ 60 000.…”

Section: Observational Datamentioning

confidence: 99%

Circumstellar envelope manifestations in the optical spectra of evolved stars

Клочкова

2014

Astrophys. Bull.

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We consider the peculiarities of the optical spectra of far evolved stars with circumstellar gaseous-dusty envelopes: the time variability of the absorptionemission profiles of the Hα line, the presence of stationary emission and absorption molecular bands, multicomponent complex profiles of the Na I D-doublet lines. We show that the peculiarities of the line profiles (the presence of an emission component in the Na I D doublet lines, the specific type of the molecular features, the asymmetry or splitting of the profiles of strongest absorptions with low excitation potential of the low level) can be associated with the kinematic and chemical properties of the circumstellar envelope and its morphological type.

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“…Observations at the 6-m BTA telescope of the SAO RAS with the NES spectrograph [7] were held in 2007 and 2009. In October 2007, we obtained one spectrum with a 1-h exposure in the region of λλ 5210-6690Å, and five spectra were obtained in November 2009 with a 1-h exposure each in the region of λλ 4000-5450Å.…”

Section: Observations At Sao Ras 6-m Bta Telescopementioning

confidence: 99%

Orbital and physical parameters of the spectroscopic binary HD37737

et al. 2013

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d 84705) and the orbital elements of the binary system. We obtained an estimate of the mass function f (m) = 0.23 ± 0.02 M . The best agreement between the synthetic and observed spectra is achieved at T eff = 30 000 K and log g = 3.50 according to the observations on both instruments. The obtained parameters correspond to a star of spectral type O9.5 III, with mass estimated at 26 ± 2 M . The minimum mass estimate of the secondary component of the binary is 6.2 ± 0.5 M . We have discovered a fact that the velocities, obtained from different spectral lines, differ, which is typical for giant stars. Engaging additional spectra, obtained in 2005 with the 2.1-m KPNO telescope, we investigated the effect of this fact on the estimate of the speed of the system's center of mass. The difference in the velocities of various lines is approximately the same in the spectra, obtained at all the three instruments. The obtained ratios suggest that the deeper layers of the atmosphere of the star are moving with a greater velocity than the outer layers. Depending on the line, the estimate of the heliocentric velocity of the binary's center of mass varies in the range from −11 to 1 km/s.

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The high-resolution spectrograph of the 6-m Large Azimuthal Telescope (BTA)

Cited by 68 publications

References 2 publications

High-resolution optical spectroscopy of the yellow hypergiant V1302 Aql (=IRC+10420) in 2001–2014

High-resolution optical spectroscopy of the yellow hypergiant V1302 Aql (=IRC+10420) in 2001–2014

Circumstellar envelope manifestations in the optical spectra of evolved stars

Orbital and physical parameters of the spectroscopic binary HD37737

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