Cámara CCD

Cámara CCD usada con el círculo meridiano Grubb ParsonsTranscripción: "Orbis / Spectra Source Instruments

Unidad de control de cámara CCD

Unidad de control de temperatura de funcionamiento de la cámara CCD Orbis usada con el círculo meridiano Grubb ParsonsTranscripción: "Spectra Source Instruments

Simulating the source parameter recovery capability from

We have studied the performance of global fitting applied to lowresolution X-ray spectroscopy, focusing on the retrieval of source parameters, with emphasis on the coronal metallicity. The study has been conducted by fitting large numbers of simulated spectra with known characteristics, and studying the distribution of the best-fit parameters, using the responses of the LECS detector onboard the SAX satellite and of the SIS detector onboard the ASCA satellite

Differential FeI Line Shifts as Convective Signatures in R=40,000 Échelle Spectra?

. The convection in stellar atmospheres cause spectral lines to be more or less blue-shifted. The differential wavelength shift between two groups of spectral lines could be used to characterize the convection. This paper describes such an effort using cross-correlations between Rß40,000 'echelle spectra and laboratory wavelength templates. 1. Differential line shifts Stellar surface convection causes spectral lines to become asymmetric and wavelength shifted (see Dravins (1998) for a recent review). Even if the resolution and noise of an observed spectrum would prevent measurements of asymmetries in the lines, the shift of the entire line or, more interesting, wavelength shifts between different classes of spectral lines might be measurable. Differential shifts, i.e. the difference in shift between lines or groups of lines in a spectrum, have some observational advantages, as compared to finding the global spectroscopic radial velocity and comparing it with the corresponding astromet..