From intracluster planetary nebulae to high-redshift Lyα emitters.

Details From intracluster planetary nebulae to high-redshift Lyα emitters. From intracluster planetary nebulae to high-redshift Lyα emitters.

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999msngr..98...50k&link_type=abstract

The Messenger, vol. 98, p. 50-52

Other

Lyman-Alpha Forest: Planetary Nebulae, Lyman-Alpha Forest: Observations, Planetary Nebulae: Intracluster Gas

Scientific paper

The fact that the spectra of planetary nebulae (PNs) are dominated by strong emission lines, with a very weak continuum, has two interesting consequences for extragalactic work. First, PNs in other galaxies are easily detectable: we need two images of a galaxy, one taken through a narrow-band filter transmitting a strong nebular emission (e.g. [O III] 5007) and another taken through an off-band filter which does not transmit any strong nebular line. In the on-band image the PN appears as a point source. Since the nebular continuum is so weak, the point source should be invisible in the off-band image. By blinking the two images, and provided that the off-band image is deep enough, it is easy to identify the PNs. Second, for each detected PN we can measure an accurate radial velocity, because all the flux we have detected is concentrated at the redshifted wavelength of the emission line. Thus we can take a good spectrogram in an exposure time not much longer than what we need for the imaging. Since PNs are preferentially discovered in the outskirts of galaxies, where the surface brightness is lower, this means that PNs are ideal test particles for studies of rotation and mass distribution in the halos of the corresponding galaxies. Typical examples of such studies are Hui et al. (1995) on NGC 5128, and Arnaboldi et al. (1996) on the Virgo cluster galaxy NGC 4406. Here begins an unusual chain of unexpected results.

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