Ⅰ. INTRODUCTION BL Lac objects were the prototype of a new class of astrophysically interested objects with these peculiar characteristies: (ⅰ) Absence of emission lines in the core source;(ⅱ) rapid variability at ...Ⅰ. INTRODUCTION BL Lac objects were the prototype of a new class of astrophysically interested objects with these peculiar characteristies: (ⅰ) Absence of emission lines in the core source;(ⅱ) rapid variability at radio, IR and visual wavelengths; (ⅲ) non-thermal展开更多
Spectroscopic follow-up observations of newly discovered transient and variable objects(e.g.,from the LSST)are crucial for both their classification and characterization.In the case of binary and variable stars,for wh...Spectroscopic follow-up observations of newly discovered transient and variable objects(e.g.,from the LSST)are crucial for both their classification and characterization.In the case of binary and variable stars,for which many different classes are expected to be discovered,time series spectroscopy will be required,over a range of timescales,to derive radial velocities from spectral lines that are modulated on orbital,spin,pulsation or other periods.The traditional approach of employing spectrographs for this task will become increasingly demanding,both in terms of the sheer number of targets and observations,but also the amount of telescope time of sufficient aperture to achieve this.展开更多
文摘Ⅰ. INTRODUCTION BL Lac objects were the prototype of a new class of astrophysically interested objects with these peculiar characteristies: (ⅰ) Absence of emission lines in the core source;(ⅱ) rapid variability at radio, IR and visual wavelengths; (ⅲ) non-thermal
文摘Spectroscopic follow-up observations of newly discovered transient and variable objects(e.g.,from the LSST)are crucial for both their classification and characterization.In the case of binary and variable stars,for which many different classes are expected to be discovered,time series spectroscopy will be required,over a range of timescales,to derive radial velocities from spectral lines that are modulated on orbital,spin,pulsation or other periods.The traditional approach of employing spectrographs for this task will become increasingly demanding,both in terms of the sheer number of targets and observations,but also the amount of telescope time of sufficient aperture to achieve this.
