Context. The physical conditions of the gas forming the narrow-line regions (NLR) in active galactic nuclei (AGN) have been exten- sively studied in the optical band. Recently detailed X-ray studies have shown how the emission in the 0.1–2 keV band detected in Seyfert 2 galaxies is associated to gas lying close to or associated with the NLR. Aims. We take advantage of the spectacular extension (∼15′′) of the NLR in the type II Seyfert galaxy NGC 5252 and of the comple- mentary characteristics of XMM-Newton and Chandra to investigate the physical conditions of the gas in this galaxy. Methods. The X-ray data from XMM-Newton are used to define the spectral properties of the ionising nuclear source. The Chandra data are used to trace the spatial characteristics of the soft X-ray emission. This information is then compared to the optical HST characteristics of the NLR in NGC 5252. Results. The X-ray spectrum of the nucleus of NGC 5252 is intrinsically flat (Γ ∼ 1.4–1.5) and absorbed by neutral gas with a column density NH ∼ 1022 cm−2. Below ∼1 keV a soft excess is detected. The high-resolution spectrum obtained with the XMM-Newton RGS shows emission lines in the 0.2–1.5 keV range which strongly indicate that the soft X-ray component is essentially due to ionised gas. Moreover, the soft X-ray emission is spatially resolved around the nucleus and well overlaps the images obtained in narrow optical bands centred around the [Oiii] emission line at 5007 Å. The [Oiii]/soft-X flux ratios along the ionisation cones are basically constant. This indicates that the electron density does not significantly deviate from the r−2 law (constant ionisation parameter) moving outward from the nucleus. Conclusions. This result combined with previous optical studies suggests two plausible but different scenarios in the reconstruction of the last ∼30 000 years of history of the central AGN. The most promising one is that the source is indeed a “quasar relic” with a steady and inefficient energy release from the accretion of matter onto the central super-massive black-hole. This scenario is suggested also by the flat nuclear X-ray spectrum that evokes an advection dominated accretion flow (ADAF) like emission mechanism.
X-ray imaging of the ionisation cones in NGC 5252
VIGNALI, CRISTIAN;
2010
Abstract
Context. The physical conditions of the gas forming the narrow-line regions (NLR) in active galactic nuclei (AGN) have been exten- sively studied in the optical band. Recently detailed X-ray studies have shown how the emission in the 0.1–2 keV band detected in Seyfert 2 galaxies is associated to gas lying close to or associated with the NLR. Aims. We take advantage of the spectacular extension (∼15′′) of the NLR in the type II Seyfert galaxy NGC 5252 and of the comple- mentary characteristics of XMM-Newton and Chandra to investigate the physical conditions of the gas in this galaxy. Methods. The X-ray data from XMM-Newton are used to define the spectral properties of the ionising nuclear source. The Chandra data are used to trace the spatial characteristics of the soft X-ray emission. This information is then compared to the optical HST characteristics of the NLR in NGC 5252. Results. The X-ray spectrum of the nucleus of NGC 5252 is intrinsically flat (Γ ∼ 1.4–1.5) and absorbed by neutral gas with a column density NH ∼ 1022 cm−2. Below ∼1 keV a soft excess is detected. The high-resolution spectrum obtained with the XMM-Newton RGS shows emission lines in the 0.2–1.5 keV range which strongly indicate that the soft X-ray component is essentially due to ionised gas. Moreover, the soft X-ray emission is spatially resolved around the nucleus and well overlaps the images obtained in narrow optical bands centred around the [Oiii] emission line at 5007 Å. The [Oiii]/soft-X flux ratios along the ionisation cones are basically constant. This indicates that the electron density does not significantly deviate from the r−2 law (constant ionisation parameter) moving outward from the nucleus. Conclusions. This result combined with previous optical studies suggests two plausible but different scenarios in the reconstruction of the last ∼30 000 years of history of the central AGN. The most promising one is that the source is indeed a “quasar relic” with a steady and inefficient energy release from the accretion of matter onto the central super-massive black-hole. This scenario is suggested also by the flat nuclear X-ray spectrum that evokes an advection dominated accretion flow (ADAF) like emission mechanism.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
