141 research outputs found
Notes on the disentangling of spectra I. Enhancement in precision
Context: The technique of disentangling has been applied to numerous
high-precision studies of spectroscopic binaries and multiple stars. Although,
its possibilities have not yet been fully understood and exploited. Aims:
Theoretical background aspects of the method, its latest improvements and hints
for its use in practice are explained in this series of papers. Methods: In
this first paper of the series, we discuss spectral-resolution limitations due
to a discrete representation of the observed spectra and introduce a new method
how to achieve a precision higher than the step of input-data binning. Results:
Based on this principle, the latest version of the KOREL code for Fourier
disentangling achieves an increase in precision for an order of magnitude.Comment: 2 figure
Disentangling telluric lines in stellar spectra
The use of a method of spectra disentangling for telluric lines is explained
in detail, with a particular emphasis on high-precision radial-velocity
measurements for the search for extrasolar planets. New improvements to the
method are introduced.Comment: Accepted for publication in Astronomy and Astrophysic
Notes on disentangling of spectra II. Intrinsic line-profile variability due to Cepheid pulsations
The determination of pulsation velocities from observed spectra of Cepheids
is needed for the Baade-Wesselink calibration of these primary distance
markers. The applicability of the Fourier-disentangling technique for the
determination of pulsation velocities of Cepheids and other pulsating stars is
studied. The KOREL-code was modified to enable fitting of free parameters of a
prescribed line-profile broadening function corresponding to the radial
pulsations of the stellar atmosphere. It was applied to spectra of delta Cep in
the H-alpha region observed with the Ondrejov 2-m telescope. The telluric lines
were removed using template-constrained disentangling, phase-locked variations
of line-strengths were measured and the curves of pulsational velocities
obtained for several spectral lines. It is shown that the amplitude and phase
of the velocities and line-strength variations depend on the depth of line
formation and the excitation potential. The disentangling of pulsations in the
Cepheid spectra may be used for distance determination
CoRoT photometry and high-resolution spectroscopy of the interacting eclipsing binary AU Mon
Analyses of very accurate CoRoT space photometry, past Johnson V
photoelectric photometry and high-resolution \'echelle spectra led to the
determination of improved and consistent fundamental stellar properties of both
components of AU Mon. We derived new, accurate ephemerides for both the orbital
motion (with a period of 11.113d) and the long-term, overall brightness
variation (with a period of 416.9d) of this strongly interacting Be + G
semi-detached binary. It is shown that this long-term variation must be due to
attenuation of the total light by some variable circumbinary material. We
derived the binary mass ratio = 0.17\p0.03 based on the
assumption that the G-type secondary fills its Roche lobe and rotates
synchronously. Using this value of the mass ratio as well as the radial
velocities of the G-star, we obtained a consistent light curve model and
improved estimates of the stellar masses, radii, luminosities and effective
temperatures. We demonstrate that the observed lines of the B-type primary may
not be of photospheric origin. We also discover rapid and periodic light
changes visible in the high-quality residual CoRoT light curves. AU Mon is put
into perspective by a comparison with known binaries exhibiting long-term
cyclic light changes.Comment: Accepted for publication in MNRA
VLT multi-object spectroscopy of 33 eclipsing binaries in the Small Magellanic Cloud. New distance and depth of the SMC, and a record-breaking apsidal motion
Aim: Our purpose is to provide reliable stellar parameters for a significant
sample of eclipsing binaries, which are representative of a whole dwarf and
metal-poor galaxy. We also aim at providing a new estimate of the mean distance
to the SMC and of its depth along the line of sight for the observed field of
view. Method: We use radial velocity curves obtained with the ESO FLAMES
facility at the VLT and light curves from the OGLE-II photometric survey. The
radial velocities were obtained by least-squares fits of the observed spectra
to synthetic ones, excluding the hydrogen Balmer lines. Results: Our sample
contains 23 detached, 9 semi-detached and 1 overcontact systems. Most detached
systems have properties consistent with stellar evolution calculations from
single-star models at the standard SMC metallicity Z = 0.004, though they tend
to be slightly overluminous. The few exceptions are probably due to third light
contribution or insufficient signal-to-noise ratio. The mass ratios are
consistent with a flat distribution, both for detached and
semi-detached/contact binaries. A mass-luminosity relation valid from ~4 to ~18
Msol is derived. The uncertainties are in the +-2 to +-11% range for the
masses, in the +-2 to +-5% range for the radii and in the +-1 to +-6% range for
the effective temperatures. The average distance modulus is 19.11+-0.03
(66.4+-0.9 kpc). The moduli derived from the V and from the I data are
consistent within 0.01 mag. The 2-sigma depth of the SMC is, for our field, of
0.25 mag or 7.6 kpc under the assumption of a gaussian distribution of stars
along the line of sight. Three systems show significant apsidal motion, one of
them with an apsidal period of 7.6 years, the shortest known to date for a
detached system with main sequence stars.Comment: 61 pages, 41 figures; accepted for publication in Astronomy &
Astrophysic
- …