HK NGC 6946 2 , the SIMBAD biblio

2010MNRAS.408.2234G - Mon. Not. R. Astron. Soc., 408, 2234-2255 (2010/November-2)

Integral field spectroscopy of HII region complexes: the outer disc of NGC6946.

GARCIA-BENITO R., DIAZ A., HAGELE G.F., PEREZ-MONTERO E., LOPEZ J., VILCHEZ J.M., PEREZ E., TERLEVICH E., TERLEVICH R. and ROSA-GONZALEZ D.

Abstract (from CDS):

Integral field spectroscopy obtained with the Potsdam Multi-Aperture Spectrophotometer Fiber Package (PPak) and the 3.5-m telescope at the Calar Alto Observatory has been used to study an outer HII region complex in the well-studied galaxy NGC6946. This technique provides detailed maps of the region in different emission lines, yielding spatially resolved information about the physical properties of the gas. The configuration was chosen to cover the whole spectrum from 3600 up to 10000Å, allowing the measurement of the near-infrared [Siii] lines. We selected four luminous knots to perform a detailed integrated spectroscopic analysis of these structures and of the whole PPak field of view (FOV). For all the knots the electron density has been found to be very similar and below 100/cm3. The [Oiii] electron temperature was measured in knots A, B, C and in the integrated PPak field, and was found to be around 8000K. The temperatures of [Oii] and [Siii] were estimated in the four cases. The elemental abundances computed from the `direct method' are typical of high-metallicity disc HII regions, with a mean value of 12+log(O/H) = 8.65, comparable to what has been found in this galaxy by other authors for regions at similar galactocentric distance. Therefore a remarkable abundance uniformity is found despite the different excitations found throughout the nebula. However, due to the quality of the data, the electron temperatures and metallicities obtained have associated errors comparable to the typical dispersion found in empirical calibrations.

Wolf-Rayet (WR) features have been detected in three of the knots, leading to a derived total number of WR stars of 125, 22 and 5 for knots A, C and B, respectively. The ratios of the numbers of WR to O stars are consistent with the prediction of Starburst99 for individual bursts with an age about 4Myr. Knot D, with no WR features, shows weak Hα emission, low excitation and the lowest Hβ equivalent width, all of which points to a more evolved state.

The integrated spectrum of the whole PPak FOV shows high excitation and a relatively evolved age that does not correspond to the individual knot evolutionary stages. Some effects associated with the loss of spatial resolution are also evidenced by the higher ionizing temperature that is deduced from the η' parameter measured in the integrated PPak spectrum with respect to that of the individual knots.


Abstract Copyright: © 2010 The Authors. Journal compilation © 2010 RAS

Journal keyword(s): techniques: spectroscopic - ISM: abundances - HII regions

Nomenclature: Fig. 3: [GDH2010] A (Nos A-D).

Simbad objects: 22

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