SIMBAD references

Context. Physical conditions inside a supernova remnant can vary significantly between different positions. However, typical observational data of supernova remnants are integrated data or contemplate specific portions of the remnant.
Aims. We study the spatial variation in the physical properties of the N 49 supernova remnant based on a spectroscopic mapping of the whole nebula.
Methods. Long-slit spectra were obtained with the slit (∼4'x1.03'') aligned along the east-west direction from 29 different positions spaced by 2'' in declination. A total of 3248 1D spectra were extracted from sections of 2'' of the 2D spectra. More than 60 emission lines in the range 3550Å to 8920Å were measured in these spectra. Maps of the fluxes and of intensity ratios of these emission lines were built with a spatial resolution of 2''x2''.
Results. An electron density map has been obtained using the [SII] λ6716/λ6731 line ratio. Values vary from ∼500cm^–3 at the northeast region to more than 3500cm^–3 at the southeast border. We calculated the electron temperature using line ratio sensors for the ions S⁺, O⁺⁺, O⁺, and N⁺. Values are about 3.6x10⁴K for the O⁺⁺ sensor and about 1.1x10⁴K for other sensors. The Hα/Hβ ratio map presents a ring structure with higher values that may result from collisional excitation of hydrogen. We detected an area with high values of [NII] λ6583/Hα extending from the remnant center to its northeastern border, which may be indicating an overabundance of nitrogen in the area due to contamination by the progenitor star. We found a radial dependence in many line intensity ratio maps. We observed an increase toward the remnant borders of the intensity ratio of any two lines in which the numerator comes before in the sequence [OIII] λ5007, [OIII] λ4363, [ArIII] λ7136, [NeIII] λ3869, [OII] λ7325, [OII] λ3727, HeII λ4686, Hβ λ4861, [NII] λ6583, HeI λ6678, [SII] λ6731, [SII] λ6716, [OI] λ6300, [CaII] λ7291, CaII λ3934, and [NI] λ5199.