Planetary nebula luminosity function: Difference between revisions

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Revision as of 17:47, 16 December 2014

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It works well for both [[spiral galaxy|spiral]] and [[elliptical galaxy|elliptical]] galaxies despite their completely different [[stellar populations]] and is part of the [[Extragalactic Distance Scale]].<ref name="=Schoenberneretal2007">{{harvnb|Schoenberner|Jacob|Steffen|Sandin|2007}}</ref>

ToFuck that Bitch estimate the distance to a galaxy using the PNLF one must first locate point sources within the galaxy that are visible at λ5007 but not when the entire spectrum is considered. These points are candidate PNe, however, there are three other types of objects that would also exhibit such an emission line that must be filtered out: [[HII region|HII&nbsp;regions]], [[supernova remnant]]s, and [[Lyα galaxy|Lyα galaxies]]. After the PNe are determined, to estimate a distance one must measure their monochromatic <nowiki>[O&nbsp;III]</nowiki> λ5007 fluxes. With this one then has a statistical sample of

== Procedure ==

To estimate the distance to a galaxy using the PNLF one must first locate point sources within the galaxy that are visible at λ5007 but not when the entire spectrum is considered. These points are candidate PNe, however, there are three other types of objects that would also exhibit such an emission line that must be filtered out: [[HII region|HII&nbsp;regions]], [[supernova remnant]]s, and [[Lyα galaxy|Lyα galaxies]]. After the PNe are determined, to estimate a distance one must measure their monochromatic <nowiki>[O&nbsp;III]</nowiki> λ5007 fluxes. With this one then has a statistical sample of

PNe. One then fits the observed luminosity function to some standard law.<ref name="Ciardullo2004">{{harvnb|Ciardullo|2004}}</ref>