Magnitudes of central stars in optically thick planetary nebulae

Details Magnitudes of central stars in optically thick planetary nebulae Magnitudes of central stars in optically thick planetary nebulae

Nov 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989aj.....98.1662j&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 98, Nov. 1989, p. 1662-1671.

Astronomy and Astrophysics

Astronomy

49

H Beta Line, Optical Thickness, Planetary Nebulae, Stellar Magnitude, Stellar Temperature, Emission Spectra, Hot Stars, Line Spectra, Stellar Luminosity

Scientific paper

Twenty planetary nebula central stars are observed with the goal of measuring accurate V magnitudes. These values are compared with the 'crossover' magnitudes predicted by Kaler and Jacoby (1989), which are computed from the nebular emission-line fluxes of He II 4686 A and H-beta. Many of these nebulae are dense and compact, and generate a strong nebular continuum that masks their nuclei. For ten of these, it is necessary to use nebular subtraction techniques developed by Jacoby (1988) and Heap and Hintzen (1990). In total, magnitudes are derived for 18 of these stars, and lower limits are set for the remaining two. For 14 nuclei, the magnitudes are measured with accuracies better than 0.25 mag, which appear to be superior to those generally available in the literature. In the remaining four cases, identifications and magnitude measurements are made at the detection limit and suffer from errors approaching 0.5 mag. It is found that the agreement between the predicted 'crossover' and observed magnitudes is very good for central stars in nebulae that are optically thick; the dispersion is only 0.5 mag. Thus, the use of the 'crossover' method to estimate the magnitudes and temperatures of obscured central stars is confirmed. This result implies that, at least for these hot stars, there is little evidence for a Zanstra discrepancy. Moreover, it justifies the use of the crossover technique for central stars of extra-galactic nebulae that are spatially unresolved, or to extremely faint central stars where conventional photometric methods become unreliable.

Affiliated with

Also associated with

No associations

Rating

Magnitudes of central stars in optically thick planetary nebulae does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Magnitudes of central stars in optically thick planetary nebulae, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Magnitudes of central stars in optically thick planetary nebulae will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1612732