Open AccessAngular diameters, fluxes and extinction of compact planetary nebulae: further evidence for steeper extinction towards the bulge
Author(s) -
Ruffle P. M. E.,
Zijlstra A. A.,
Walsh J. R.,
Gray M. D.,
Gesicki K.,
Minniti D.,
Comeron F.
Publication year - 2004
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2004.08113.x
Subject(s) - physics , bulge , extinction (optical mineralogy) , astrophysics , planetary nebula , radius , flux (metallurgy) , angular diameter , interstellar medium , galaxy , astronomy , ionization , stars , optics , ion , computer security , quantum mechanics , computer science , materials science , metallurgy
We present values for angular diameter, flux and extinction for 70 Galactic planetary nebulae observed using narrow‐band filters. Angular diameters are derived using constant emissivity shell and photoionization line emission models. The mean of the results from these two models are presented as our best estimate. Contour plots of 36 fully resolved objects are included and the low‐intensity contours often reveal an elliptical structure that is not always apparent from full width at half maximum measurements. Flux densities are determined, and for both Hα and [O iii ] there is little evidence of any systematic differences between observed and catalogued values. Observed Hα extinction values are determined using observed Hα and catalogued radio fluxes. Hα extinction values are also derived from catalogued Hα and Hβ flux values by means of an R V dependent extinction law. R V is then calculated in terms of observed extinction values and catalogued Hα and Hβ flux values. Comparing observed and catalogue extinction values for a subset of bulge objects, observed values tend to be lower than catalogue values calculated with R V = 3.1 . For the same subset we calculate 〈 R V 〉= 2.0 , confirming that toward the bulge interstellar extinction is steeper than R V = 3.1 . For the inner Galaxy, a relation with the higher supernova rate is suggested, and that the low‐density warm ionized medium is the site of the anomalous extinction. Low values of extinction are also derived using dust models with a turnover radius of 0.08 μm.