Spectroscopy of planetary nebulae in M33

Details Spectroscopy of planetary nebulae in M33 Spectroscopy of planetary nebulae in M33

2003-01-08

arxiv.org/abs/astro-ph/0301129v1

Astron.Astrophys.400:511-520,2003

Astronomy and Astrophysics

Astrophysics

18 pages, 1 JPEG figure and 3 Postscript figures, Accepted for publication in A&A

Scientific paper

10.1051/0004-6361:20030031

Spectroscopic observations of 48 emission-line objects of M33 have been obtained with the multi-object, wide field, fibre spectrograph AF2/WYFFOS at the 4.2m WHT telescope (La Palma, Spain). Line intensities and logarithmic extinction, cbeta, are presented for 42 objects. Their location in the Sabbadin & D'Odorico diagnostic diagram (Halpha/[SII] vs Hlapha/[NII]) suggests that >70% of the candidates are Planetary Nebulae (PNe). Chemical abundances and nebular physical parameters have been derived for the three of the six PNe where the 4363A [OIII] emission line was measurable. These are disc PNe, located within a galactocentric distance of 4.1 kpc, and, to date, they are the farthest PNe with a direct chemical abundance determination. No discrepancy in the Helium, Oxygen and Argon abundances has been found in comparison with corresponding abundances of PNe in our Galaxy. Only a lower limit to the sulphur abundance has been obtained since we could not detect any [SIII] line. N/H appears to be lower than the Galactic value; some possible explanations for this under-abundance are discussed.

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