In case of a publication based on Aristarchos data please take into account the following guidelines:
Credit “Aristarchos telescope” in published papers:
Publications based wholly or in part on data obtained at the Aristarchos telescope are required to carry the following Acknowledgment, primarily as a footnote to the title but, if such footnotes are not permitted by the journal, book, etc, then in the Acknowledgments section of the paper itself:
“Based on observations made with the 2.3m Aristarchos telescope, Helmos Observatory, Greece, which is operated by the Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing of the National Observatory of Athens, Greece.”
Latest Publications
H2 molecular gas in the old planetary nebula NGC 3587
Ramos-Larios G., Guerrero M. A., Toalá J. A., Akras S., Fang X.
A Unique Low-mass-ratio Contact Eclipsing Binary System under the Period Cutoff
Papageorgiou, Athanasios ; Christopoulou, Panagiota-Eleftheria
Three Ultra-short-period Contact Eclipsing Binary Systems Mined from Massive Astronomical Surveys
Papageorgiou, A., Christopoulou, P.-E., Ferreira
Asteroid spin-states of a 4 Gyr collisional family
Athanasopoulos, D., Hanuš, J., Avdellidou,
CoBiToM Project — II: Evolution of contact binary systems close to the orbital period cut-off
Loukaidou, G. A. ; Gazeas,
Discovery of an optical cocoon tail behind the runaway HD 185806
Studies on the circumstellar structures around evolved stars provide vital information on the evolution of the parent star and the properties of the local interstellar medium. In this work, we present the discovery and characterization of an optical cocoon tail behind the star HD 185806. The cocoon apex emission is puzzling, as it is detected in the infrared but shows no signal in the optical wavelength.
Deep optical study of the mixed-morphology supernova remnant G 132.7+1.3 (HB3)
We present optical ccd images of the large supernova remnant (SNR) G132.7 + 1.3 (HB3) covering its full extent for the first time, in the emission lines of H α+ [N II], [S II] and [O III], where new and known filamentary and diffuse structures are detected. These observations are supplemented by new low-resolution long-slit spectra and higher-resolution images in the same emission lines. Both the flux-calibrated images and spectra confirm that the optical emission originates from shock-heated gas since the [S II]/H α > 0.4.