PCA of H-band IFU pixel spectra decomposes cool stellar populations in NGC 5128 and NGC 5102, identifying M-giant, long-period variable, and carbon star contributions.
Far-Ultraviolet Radiation from Elliptical Galaxies
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abstract
Far-ultraviolet radiation is a ubiquitous, if unanticipated, phenomenon in elliptical galaxies and early-type spiral bulges. It is the most variable photometric feature associated with old stellar populations. Recent observational and theoretical evidence shows that it is produced mainly by low-mass, small-envelope, helium-burning stars in extreme horizontal branch and subsequent phases of evolution. These are probably descendents of the dominant, metal rich population of the galaxies. Their lifetime UV outputs are remarkably sensitive to their physical properties and hence to the age and the helium and metal abundances of their parents. UV spectra are therefore exceptionally promising diagnostics of old stellar populations, although their calibration requires a much improved understanding of giant branch mass loss, helium enrichment, and atmospheric diffusion.
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Decomposing cool stellar populations with H-band spectral fluctuations: Long-period variable stars in NGC 5128 and carbon stars in NGC 5102
PCA of H-band IFU pixel spectra decomposes cool stellar populations in NGC 5128 and NGC 5102, identifying M-giant, long-period variable, and carbon star contributions.