scholarly journals Global Astrophysical Telescope System — telescope No. 2

2013 ◽  
Vol 9 (S301) ◽  
pp. 437-438
Author(s):  
Krzysztof Kamiński ◽  
Roman Baranowski ◽  
Monika Fagas ◽  
Wojciech Borczyk ◽  
Wojciech Dimitrov ◽  
...  
Keyword(s):  
Variable Stars ◽  
Astronomical Observatory ◽  
Spectroscopic Observations ◽  
Photometric Observations ◽  
Nearly Continuous ◽  
Telescope System

AbstractWe present the new, second spectroscopic telescope of Poznań Astronomical Observatory. The telescope allows automatic simultaneous spectroscopic and photometric observations and is scheduled to begin operation from Arizona in autumn 2013. Together with the telescope located in Borowiec, Poland, it will constitute a perfect instrument for nearly continuous spectroscopic observations of variable stars. With both instruments operational, the Global Astrophysical Telescope System will be established.

scholarly journals Global Astrophysical Telescope System – GATS

2013 ◽  
Vol 9 (S301) ◽  
pp. 475-476
Author(s):  
M. Polińska ◽  
K. Kamiński ◽  
W. Dimitrov ◽  
M. Fagas ◽  
W. Borczyk ◽  
...  
Keyword(s):  
High Resolution ◽  
Astronomical Observatory ◽  
Global Network ◽  
High Resolution Spectroscopy ◽  
Spectroscopic Observations ◽  
The Usa ◽  
Robotic Telescopes ◽  
Telescope System ◽  
Adam Mickiewicz

AbstractThe Global Astronomical Telescope System is a project managed by the Astronomical Observatory Institute of Adam Mickiewicz University in Poznań (Poland) and it is primarily intended for stellar medium/high resolution spectroscopy. The system will be operating as a global network of robotic telescopes. The GATS consists of two telescopes: PST 1 in Poland (near Poznań) and PST 2 in the USA (Arizona). The GATS project is also intended to cooperate with the BRITE satellites and supplement their photometry with spectroscopic observations.

Times of maximum of KZ Hya from OACS -UNAH

2020 ◽  
Vol 8 (2) ◽  
pp. 90-93
Author(s):  
M. Meza ◽  
A. Pineda ◽  
C. Argueta ◽  
Y. Mendoza ◽  
M. C. Pereira ◽  
...  
Keyword(s):  
Variable Star ◽  
Variable Stars ◽  
Surface Layers ◽  
Maximum Light ◽  
Photometric Observations

A pulsating variable star is one whose brightness changes periodically due to the expansion and contraction of the surface layers of the star. Several times of maximum light can be obtained in brief observations of SX Phoenicis variable stars due to their short periods of pulsation (P ~ 1:0 - 1:75 h). We report three new times of maximum light of SX Phoenicis star KZ Hya obtained from photometric observations made on the night of April 5-6, 2019 from the Observatorio Astronómico Centroaméricano de Suyapa (OACS) of the Universidad Nacional Autónoma de Honduras

scholarly journals Spectroscopic Observations of the Early-Type Contact Binary AW Lacertae

1989 ◽  
Vol 107 ◽  
pp. 354-354
Author(s):  
Y. Nakamura ◽  
A. Okazaki ◽  
J. Katahira
Keyword(s):  
Spectral Type ◽  
Variable Stars ◽  
Radial Velocities ◽  
Early Type ◽  
Mass Ratio ◽  
Photometric Analysis ◽  
Spectroscopic Observations ◽  
Type Contact ◽  
Contact Binary ◽  
Photometric Solution

Abstract.Spectroscopic observations were performed of the early-type contact binary AW Lac with an image-intensified coude spectrograph of 1.9−m telescope at the Okayama Astro-physical Observatory. A total of twenty-two spectra covering blue region with a dispersion of 16 Amm−1 have been secured on Kodak IIa-O baked plates. In every spectra sharp interstellar Call H,K lines are clearly seen. The spectral type of AW Lac has been estimated as early B, which substantially confirms the one adopted in the photometric analysis by Jiang et al. (1983) and is diffrent from A0 listed in General Catalogue of Variable Stars (Kholopov et al. 1985). Contrary to the suggestion by the photometric solution of Jiang et al., no definite secondary lines could be separated, though some indications of light contamination due to the secondary component are surely observed. This would imply that the light ratio of the components should be somewhat smaller than that derived by photometric analysis. No emission features appeared either. The measurement of radial velocities of the primary component for the orbital elements was made for twenty spectra by a conventional method. It was difficult to measure the radial velocities because the lines are quite broadened and deformed. Hence the measured values for the radial velocities should be regarded as rather preliminary. The derived spectroscopic elements, combined with the photometric data, give the absolute dimensions of the system for each assumed mass ratio q. For q = 1, being the adopted photometric solution by Jiang et al., we obtain too small value for the primary’s mass, comparing with its spectral type. For the mass ratio as small as q = 0.6, we can obtain a reasonable value for the mass of the primary. However, in order to get more definite conclusion the cross-correlation method would be more appropriate for the spectroscopic analysis of this system.

scholarly journals Optical photometric variable stars towards Cygnus OB7

2019 ◽  
Vol 487 (2) ◽  
pp. 1765-1776 ◽  
Author(s):  
Somnath Dutta ◽  
Soumen Mondal ◽  
Santosh Joshi ◽  
Ramkrishna Das
Keyword(s):  
Variable Stars ◽  
T Tauri Stars ◽  
Light Curves ◽  
Main Sequence Stars ◽  
Star Forming ◽  
Rotation Rates ◽  
T Tauri ◽  
Photometric Observations ◽  
Sky Survey ◽  
Magnitude Diagram

ABSTRACT We present optical I-band light curves of the stars towards a star-forming region Cygnus OB7 from 17-night photometric observations. The light curves are generated from a total of 381 image frames with very good photometric precision. From the light curves of 1900 stars and their periodogram analyses, we detect 31 candidate variables including five previously identified. 14 out of 31 objects are periodic and exhibit the rotation rates in the range of 0.15–11.60 d. We characterize those candidate variables using optical/infrared colour–colour diagram and colour–magnitude diagram (CMD). From spectral indices of the candidate variables, it turns out that four are probably Classical T-Tauri stars (CTTSs), rest remain unclassified from present data, they are possibly field stars or discless pre-main-sequence stars towards the region. Based on their location on the various CMDs, the ages of two T Tauri Stars were estimated to be ∼5 Myr. The light curves indicate at least five of the periodic variables are eclipsing systems. The spatial distribution of young variable candidates on Planck 857 GHz (350 $\mu$m) and 2MASS (Two Micron All Sky Survey) Ks images suggest that at least two of the CTTSs are part of the active star-forming cloud Lynds 1003.

New Variable Stars Discovered as By-product of the Beijing Astronomical Observatory Supernova Survey

2002 ◽  
Vol 2 (5) ◽  
pp. 463-473 ◽  
Author(s):  
Min-Zhi Kong ◽  
Yu-Lei Qiu ◽  
Chuan-Jian Shen ◽  
Jin-Song Deng ◽  
Bo Zhang ◽  
...  
Keyword(s):  
Variable Stars ◽  
Astronomical Observatory

scholarly journals Observations of comets and minor planets at Kiev comets station (585)

2009 ◽  
Vol 5 (S263) ◽  
pp. 298-302
Author(s):  
Alexander R. Baransky ◽  
Klim I. Churuymov ◽  
Vasyl A. Ponomarenko
Keyword(s):  
Astronomical Observatory ◽  
Minor Planets ◽  
Photometric Observations ◽  
National University

AbstractWe present the results of astrometric and photometric observations of comets and minor planets obtained at the Kiev comet station (Code MPC 585) of the Astronomical Observatory of Kyiv Shevchenko National University in 2006-2009. The 2318 position observations of 176 comets, 302 observations of 57 numbered minor planets, and 220 observations of 30 unnumbered minor planets were obtained. The accuracy of the astrometric observations of the comets is analyzed.

scholarly journals U–SMART : SMALL APERTURE ROBOTIC TELESCOPES FOR UNIVERSITIES

2019 ◽  
Vol 51 ◽  
pp. 44-46
Author(s):  
P. Gebhardt ◽  
A. Schrimpf ◽  
C. Dersch ◽  
M. Spasovic ◽  
L. Bringmann ◽  
...  
Keyword(s):  
Variable Stars ◽  
Remote Access ◽  
Archival Data ◽  
Control Software ◽  
Small Aperture ◽  
Camera Control ◽  
Spectroscopic Observations ◽  
Photometric And Spectroscopic Observations ◽  
Robotic Telescopes ◽  
Photo Plate

A group of universities have come together with the aim of designing and developing small aperture robotic telescopes (SmART) for use by students to observe variable stars and transient follow-ups. The group is deliberating on the components of the robotic system e.g. the telescope, the mount, the back-end camera, control software etc and their integration keeping in mind the scientific objectives. The Marburg group is studying variable stars using photometric and spectroscopic observations in a small local observatory and via analysis of photo plate archival data mainly from Sonneberg observatory (Thuringa, Germany). Our goal is to setup a small, affordable observatory at Marburg University with full remote access to all components, including a spectrometer. Among others, the future measurements can be follow-ups, of variable stars, exoplanet search and spectroscopic measurements, e.g. in cooperation with the BRITE-constellation. We would like to invite other universities to join the project and cooperate in setting up a University network of small aperture robotic telescopes (U-SmART) around the globe.

scholarly journals On the periodicity of Hubble-Sandage objects in M 31

1989 ◽  
Vol 113 ◽  
pp. 275-276
Author(s):  
G. R. Ivanov
Keyword(s):  
Variable Stars ◽  
Astronomical Observatory ◽  
General Catalogue ◽  
M 31 ◽  
Η Car

The spectral and photometric characteristics of the Hubble-Sandage objects (HSO) are similar to those of the η Car and S Dor variables. They are actually referred to as S Dor-type in the General Catalogue of Variable Stars. Their light variations differ from star to star.The aim of the present paper is to discuss a possible periodicity in HSOs in M 31. We used phtometry from Hubble(1929), Sharov(1973, 1981), Rosino and Bianchini(1973), and added some observations taken during 1980-87. The latter were obtained with the 2-m Ritchey-Chretien-Coude and 0.5-m Schmidt telescopes of the Bulgarian National Astronomical Observatory – Rozhen.

scholarly journals Search for Variable Stars in the Open Cluster NGC 2539

2001 ◽  
Vol 183 ◽  
pp. 211-212
Author(s):  
K.J. Choo ◽  
S.-L. Kim ◽  
T. S. Yoon ◽  
M.-Y. Chun ◽  
H. Sung ◽  
...  
Keyword(s):  
Open Cluster ◽  
Variable Stars ◽  
Photometric Observations

AbstractWe report on the results of CCD photometric observations of the open cluster NGC 2539. Eight new variable stars have been found in the observed field of this cluster. However, no γ Doradus-type variability was found among the member stars.

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