Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue - X. Three high-contrast systems with secondaries detected with IR spectroscopy

We present results of the combined photometric and spectroscopic analysis of three detached eclipsing binaries, which secondary components are not visible or very hard to identify in the optical spectra - ASAS J052743-0359.7, ASAS J065134-2211.5, and ASAS J073507-0905.7. The first one is a known visual binary ADS 4022, and we found that it is a quadruple system, composed of two spectroscopic binaries, one of which shows eclipses. None of the systems was previously recognized as a spectroscopic binary. We collected a number of high-resolution optical and IR spectra to calculate the radial velocities (RVs) and later combined them with MITSuME and ASAS photometry. The IR spectra were crucial for secure identification of the cooler components' lines. RV measurements were done with the TODCOR technique, and RV curves modelled with our own procedure V2FIT. Light curve modelling was performed with JKTEBOP and PHOEBE codes. Temperatures and metallicities of two systems were estimated from spectra. For the ADS 4022 system we also used the archival WDS data and new SOAR observations in order to derive the orbit of the visual pair for the first time. Ages were estimated by comparing our results with PARSEC isochrones. The eclipsing pair A052743 A ($P=5.27$ d) is composed of a 1.03(6) M$_\odot$, 1.03(2) R$_\odot$ primary and a 0.60(2) M$_\odot$, 0.59(2) R$_\odot$ secondary. The components of the $P=21.57$ d non-eclipsing pair B likely have masses in between the two eclipsing components, and both pairs are on a $\sim$188 yr orbit around their common centre of mass. The system A065134 ($P=8.22$ d) consists of a 0.956(12) M$_\odot$, 0.997(4) R$_\odot$ primary and a 0.674(5) M$_\odot$, 0.690(7) R$_\odot$ secondary. Finally, A073507 ($P=1.45$ d), which consists of a 1.452(34) M$_\odot$, 1.635(12) R$_\odot$ primary and a 0.808(13) M$_\odot$, 0.819(11) R$_\odot$ secondary, is likely a PMS system.Comment: 22 pages, 13 figures, 8 tables, accepted for publication in A&A, abstract modified for arXi

Orbital and physical parameters of eclipsing binaries from the ASAS catalogue – XI. CHIRON investigation of long-period binaries*

We present the results of a spectroscopic campaign on eclipsing binaries with long orbital period (P = 20 − 75 d) carried out with the CHIRON spectrograph. Physical and orbital solutions for seven systems were derived from the V-band, and I-band ASAS, WASP, and TESS photometry, while radial velocities were calculated from high quality optical spectra using a two-dimensional cross-correlation technique. The atmospheric parameters of the stars have been determined from the separated spectra. Most of our targets are composed of evolved stars (sub-giants or red giants) but two systems show components in different phases of evolution and one possible merger. For four binaries the masses and radii of the components were obtained with precision better than $3$. These objects provide very valuable information on stellar evolution

Orbital and physical parameters of eclipsing binaries from the ASAS catalogue - XI. CHIRON investigation of long-period binaries

We present the results of a spectroscopic campaign on eclipsing binaries with long orbital period (P = 20 - 75 d) carried out with the CHIRON spectrograph. Physical and orbital solutions for seven systems were derived from the V-band, and I-band ASAS, WASP, and TESS photometry, while radial velocities were calculated from high quality optical spectra using a two-dimensional cross-correlation technique. The atmospheric parameters of the stars have been determined from the separated spectra. Most of our targets are composed of evolved stars (sub-giants or red giants) but two systems show components in different phases of evolution and one possible merger. For four binaries the masses and radii of the components were obtained with precision better than 3% . These objects provide very valuable information on stellar evolution

Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue. X. Three high-contrast systems with secondaries detected with IR spectroscopy

Aims: We present results of the combined photometric and spectroscopic analysis of three detached eclipsing binaries, the secondary components of which are not visible or are very hard to identify in the optical spectra - ASAS J052743-0359.7, ASAS J065134-2211.5, and ASAS J073507-0905.7. The first one is the known visual binary ADS 4022, and we found that it is a quadruple system composed of two spectroscopic binaries, one of which shows eclipses. None of the systems have previously been recognized as a spectroscopic binary. Methods: We used the following telescopes/spectrographs to collect a number of high-resolution optical and IR spectra: Subaru/IRCS, CTIO-1.5 m/CHIRON, Euler/CORALIE, MPG-2.2 m/FEROS, OAO-188/HIDES, and TNG/HARPS-N. We used these data to calculate radial velocities (RVs) and later combined them with MITSuME and ASAS photometry. The Subaru/IRCS IR spectra were crucial for secure identification of the lines of the cooler components. Radial velocity measurements were made with the TODCOR technique, and RV curves were modelled with our own procedure V2FIT. Light-curve modelling was performed with JKTEBOP and PHOEBE codes. Temperatures and metallicities of two systems were estimated from spectra. For the ADS 4022 system we also used the archival WDS data and new SOAR observations in order to derive the orbit of the visual pair for the first time. Ages were estimated by comparing our results with PARSEC isochrones. Results: The eclipsing pair ASAS J052743-0359.7 A (P = 5.27 d) is composed of a 1.03(6) M☉, 1.03(2) R☉ primary and a 0.60(2) M☉, 0.59(2) R☉ secondary. The components of the P = 21.57 d non-eclipsing pair B likely have masses in between the two eclipsing components, and both pairs are on a ̃188 yr orbit around their common centre of mass. The system ASAS J065134-2211.5 (P = 8.22 d) consists of a 0.956(12) M☉, 0.997(4) R☉ primary and a 0.674(5) M☉, 0.690(7) R☉ secondary. Finally, ASAS J073507-0905.7 (P = 1.45 d), which consists of a 1.452(34) M☉, 1.635(12) R☉ primary and a 0.808(13) M☉, 0.819(11) R☉ secondary, is likely a pre-main sequence system. In all cases secondary eclipses are total. Time series photometry is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/622/A114</A

Polish and European SST Assets: the Solaris-Panoptes Global Network of Robotic Telescopes and the Borowiec Satellite Laser Ranging System

Contains fulltext : 166018.pdf (publisher's version ) (Open Access)Advanced Maui Optical and Space Surveillance Technologies Conference, , Wailea, Maui, Hawaii, September 20-23, 201