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For refcode 1995MNRAS.273..129G:
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Copyright by Royal Astronomical Society. 1995MNRAS.273..129G New narrow-band imaging of the extended emission-line region in the Seyfert galaxy NGC 3516 V. Golev, I. Yankulova, T. Bonev and K. Jockers Department of Astronomy, Faculty of Physics, St Kliment Okhridski University of Sofia, 5 James Bourchier St, BG-]l26 Sofia, Bulgaria Institute of Astronomy, Bulgarian Academy of Sciences, 72 Tsarigradsko chaussee blvd, BG-1 784 Sofia, Bulgaria Max-Planck-Institute for Astronomy D-37l89Katlenburg-Lindau, Germany Accepted 1994 October 4. Received 1994 August 8; in original form 1993 December 2 ABSTRACT We present new flux-calibrated narrow-band images of the extended emission-line region (EELR) in NGC 3516 in the light of [O III] {lambda}4959, [Fe VII] + [CaV] {lambda}6087, [OI] {lambda}6364 and H{alpha} + [NII] {lambda}{lambda}6548,6584 emission lines. Our [O III] and H{alpha} + [NII] images confirm the previously reported Z-shaped structure and other EELR features. In the extended zone (>= 4-5 arcsec and <= 24 arcsec), we measure ~1.3 x 10^-13^ erg cm^-2^ s^-1^ in [O III] {lambda}4959 and ~1.7 X 10^-12^ erg cm^-2^ s^-1^ in H{alpha}+[NII] {lambda}{lambda}6548, 6584. The outlying feature 7, found by Miyaji et al., is most conspicuous in the [OIII] {lambda}4959 image. We measure the total emission flux of this feature to be ~2.7 x 10^-15^ erg cm^-2^ s^-1^. Our image in the [Fe VII] + [Ca V] {lambda}6087 line is spatially extended to about 7-8 arcsec and its axis is aligned with both the one- sided radio jet and the extended optical emission in the H{alpha} + [N II] and [O III] {lambda}{lambda}4959,5007 lines observed north-east of the nucleus. The measured flux in [Fe VII] {lambda}6087 is ~10^-14^ erg cm^-2^ s^-1^, which yields N_e_^2^~0.35. It is clear. that the photoionized coronal-line region (CLR) in NGC 3516 is not so dense. We estimate the Q_rec_/Q_nuc_ ratio from the observed [Fe VII] + [Ca V] {lambda}6087 luminosity for the photons with energies higher than hv = 100 eV in the highly ionized structure, and we obtain (Q_rec_/Q_nuc_)_hv > 100 eV_~2.8. This number, like the estimation made by Pogge using the H{alpha} recombination line, does not present compelling evidence for a pronounced energy deficit like that observed in the EELR of the Seyfert 2 galaxies. These observations support the model of the coronal-line region proposed by Korista & Ferland. According to this model, the coronal emission in NGC 3516 may arise in a low-density (N_e_ ~ 1 cm^-3^) interstellar medium exposed to and photoionized by the bare active nucleus. Key words: galaxies: active - galaxies: individual: NGC 3516 - galaxies: ISM - galaxies: Seyfert.
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