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Fig. 2.


Comparison of certain observed lines in F5 stars (orange curves) with average flux inferred from whole spectral class (blue curves). The lighter bands surrounding the fluxes show their associated uncertainties, while the green colored areas identify the integrated flux differences that we attribute to lines from Eu. Panel a: F5 star (specobjID = 3719984370237415424) that shows a substantial flux deficit compared to the mean in the 4127–4131 Å wavelength range that encompasses an important line of Eu II (see Table 1). Panel b: another F5 star (specobjID = 2786716958031191040) also showing a significant flux deficiency in the 4659–4663 Å range, which is the interval of wavelengths where one expects to find a strong Eu I line. In both cases the stars have been identified as positive detections. In contrast, panel c shows a third F5 star (specobjID = 3002850987342928896) that does not show evidence for the existence of this latter line in absorption, which classifies it as a non-detection.

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