ESO089-G018 and ESO089-G019: long-slit spectroscopy of emission-line galaxies

Details ESO089-G018 and ESO089-G019: long-slit spectroscopy of emission-line galaxies ESO089-G018 and ESO089-G019: long-slit spectroscopy of emission-line galaxies

Mar 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010mnras.402.1480d&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 402, Issue 3, pp. 1480-1488.

Astronomy and Astrophysics

Astronomy

Methods: Data Analysis, Methods: Observational, Techniques: Spectroscopic, Galaxies: Fundamental Parameters, Galaxies: Peculiar

Scientific paper

We present the first spectroscopic observations for the galaxies ESO089-G018 (hereafter G18, an Sb(?)-type galaxy seen nearly edge-on) and ESO089-G019 (hereafter G19, an SA(s): a peculiar galaxy), extracted from the sample of ring-shaped galaxies compiled in Faúndez-Abans & de Oliveira-Abans. The main goal of this work is to investigate the spectral classification using the three line-ratio diagrams, called diagnostic diagrams, of Veilleux & Osterbrock. However, in order to separate the different types of galaxies [HII galaxies, Seyfert 2 galaxies and low-ionization nuclear emission-line region galaxies (LINERs)] we have to used empirical boundaries between them. Based on the observed spectra, we suggest G18 is a `weak-[OI] LINER' or even a `transition object' or LINER/HII. In the case of G19, we see Hβ in absorption and no [OIII] lines, impeding the [OIII]/Hβ ratio to be estimated. However, other lines ratios have been evaluated for the discussion. We classify the nature of G19 as ambiguous, because of the difficulty in determining its ionizing source (narrow-line active galactic nuclei or HII galaxies) in different diagnostic diagrams. The errors in the fluxes were mostly caused by uncertainties in the placement of the continuum level. We have estimated nuclear redshift of z = 0.034 (G18) and z = 0.039 (G19), corresponding to a heliocentric velocity of 10246 and 11734kms-1, respectively. Some other physical parameters have been derived whenever possible. All spectra were reduced and analysed in a homogeneous way with the standard IRAF procedures.
Based on observations carried out at Observatório do Pico dos Dias (OPD), which operated by the LNA/MCT, Brazil-MG.
E-mail: paulopoppe@gmail.com

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