Next: Conclusions Up: Compensation for Read-Out Noise Previous: Implementation . ... The star cluster, shown in the left panel of Fig. 1 , consists of a field of unresolved stars at random locations and having randomly selected brightnesses. ... These are replotted in Fig. 8 to facilitate comparisons. ... The low level noise is reduced substantially in Fig. 11 , which is the average of 25 restorations of HST star cluster images, each being the result of performing 500 EM iterations. ...
... Complex astrophysical phenomena could now be studied spectroscopically: the X-ray absorption line forest intrinsic to Seyfert galaxies; the interaction between AGN jets and intracluster media; hot winds of starburst galaxies; stellar coronal plasmas; the charge -exchange emission of Mars' exosphere; the X-ray irradiation of protoplanetary disks; and the myst erious flat-topped spectral line shapes of O star winds. ... We estimate that Gen-X will be able to detect and resolve 20, 000 stars in NGC...
ST-ECF Instrument Science Report ACS-2006-02 Wavelength and Flux calibration of the ACS/SBC PR110L and PR130L prisms S. S. Larsen, February 2006 ABSTRACT Wavelength- and flux calibrations are presented for the ACS/SBC PR110L and PR130L slitless spectroscopy modes. ... Wavelength. ... Flux calibration Figure 5: Comparison of sensitivity functions for the SBC prisms derived from the inorbit calibration (solid curves) and the ground calibration from Bohlin et al. 2000 (dashed curves). ...
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