J/AJ/158/95 V348 And and V572 Per: heliocentric minima and RVs (Zasche+, 2019)
V348 And and V572 Per: bright triple systems with eccentric eclipsing binaries.
Zasche P., Uhlar R., Svoboda P., Jurysek J., Korcakova D., Wolf M.,
Slechta M., Kotkova L.
<Astron. J., 158, 95-95 (2019)>
=2019AJ....158...95Z 2019AJ....158...95Z (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing ; Stars, bright ; Photometry ; Optical ;
Radial velocities
Keywords: binaries: eclipsing - binaries: spectroscopic - binaries: visual -
stars: fundamental parameters - stars: individual (V348 And, V572 Per)
Abstract:
The eclipsing binaries are still important objects for our understanding
of the universe. Especially these ones located within the more complex
multiple systems can help us solving the problem of their origin and
subsequent evolution of these higher order multiples. Photometry and
spectroscopy spanning over more than 25 yr were used for the first complete
analysis of the two bright triple systems, namely V348 And and V572 Per.
The light curves in photometric filters were combined together with the
radial velocities and analyzed simultaneously, yielding the precise
physical parameters of the eclipsing components of these multiple systems.
The system V348 And consists of two eclipsing components with its orbital
period of about 27.7 days. The system is a very detached one, and both
eclipses are rather narrow, lasting only about 0.016 of its period. The
visual orbit of the wide pair has the period of about 87 yr. All three
components of the system are probably of B8-9 spectral type, and the
parallax of the system was slightly shifted to the value of 2.92 mas.
On the other hand, the system V572 Per shows apsidal motion of its inner
orbit, the orbital period being of about 1.2 days, while the apsidal motion
of about 48 yr. The components are of A and F spectral types, while the
motion with the third component around a common barycenter is only
negligible. According to our modeling, this system is not a member of
open cluster Alpha Persei.
Description:
All of our new spectroscopic observations were secured in the Ondrejov
observatory in Czech Republic, using the 2 m telescope. The classical
slit spectrograph has a resolution of R∼12500. The individual exposure
times were chosen according to the quality of the particular night,
typically 800-3600 s. All of the spectrograms were reduced in a standard
way, the wavelength calibration was made via a ThAr comparison spectra
obtained before and after the stellar ones. The flat fields were taken
in the beginning and end of the night and their averages were then used
for the reduction. After that, the radial velocities (RV) were derived
with the program SPEFO (Horn et al. 1996, J/A+A/309/521, or Skoda
1996ASPC..101..187S 1996ASPC..101..187S), on several absorption lines in the measured spectral
region around Hα (usually Fe, Ca, or Si lines), with using the
zero-point correction via measuring the telluric lines.
Owing to the relatively high brightness of these stars, only rather small
telescopes were used for the photometric observations. The system V348 And
was observed (by P. Svoboda) with only the 34 mm refractor at his private
observatory in Brno, Czech Republic, using the SBIG ST-7 CCD camera.
The second star V572 Per was monitored with the similar instrument at
the private observatory (by R. Uhlar) in Jilove u Prahy, Czech Republic,
using a G2-0402 CCD camera. All of the measurements were reduced in a
standard way using the program C-MUNIPACK, which is based on aperture
photometry and uses the standard DAOPHOT procedures (Tody
1993ASPC...52..173T 1993ASPC...52..173T). The photometric data were obtained during the time
span of 2007-2018. Nevertheless, some of the older data were only used
for the minima times derivation. All of these data were secured in the
Johnson-Cousins photometric system (Bessell 1990PASP..102.1181B 1990PASP..102.1181B),
particularly the system V348 And was observed in BVR, while the system
V572 Per in BVRI filters.
Objects:
-------------------------------------------------------------------
RA (ICRS) DE Designation(s) (Period)
-------------------------------------------------------------------
00 15 17.83 +44 12 12.2 V348 And = V* V348 And (P=27.703514)
03 15 48.68 +50 57 21.2 V572 Per = V* V572 Per (P=1.2131789)
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 48 69 Heliocentric minima of the systems used for
our analysis
table4.dat 45 44 Radial velocities of the systems used for
our analysis
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See also:
J/A+A/309/521 : 55 UMa spectroscopic orbit (Horn+, 1996)
J/A+A/617/A32 : MASCARA bright variable stars light curves (Burggraaff+, 2018)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Star Star name (V348 And or V572 Per)
10- 20 F11.5 d HJD [48046.8/58498.4] Heliocentric Julian Date
(HJD-2400000)
22- 28 F7.5 d e_HJD [0.00016/0.04519] Error on HJD
30 A1 --- Type [P/S] Primary (P) or secondary (S) component
32- 35 A4 --- Filt Filter(s)
37- 48 A12 --- Obs Source of observation (1)
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Note (1): Source of observation as follows:
Hipparcos = Hipparcos (Perryman & ESA 2009A&A...500..501P 2009A&A...500..501P);
MASCARA = Multi-site All-Sky CAmeRA (MASCARA; Burggraaff et al. 2018,
J/A+A/617/A32);
OMC/INTEGRAL = International Gamma-Ray Astrophysics Laboratory (INTEGRAL) and
its optical monitoring camera (OMC) instrument
(Mas-Hesse et al. 2003A&A...411L.261M 2003A&A...411L.261M).
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Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Star Star name (V348 And or V572 Per)
10- 19 F10.4 d HJD [56041.5/57954.6] Heliocentric Julian Date
(HJD-2400000)
21- 27 F7.2 km/s RV1 [-127.74/130.68] Primary radial velocity
29- 32 F4.2 km/s e_RV1 [0.38/7.34] Error on RV1
34- 40 F7.2 km/s RV2 [-165.72/159.44]? Secondary radial velocity
42- 45 F4.2 km/s e_RV2 [0.39/8.75]? Error on RV2
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History:
From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 10-Oct-2019