Tracing the Coronal Line Region in AGN with VLT/NACO: The Very First Results

Author(s):  
Olivier Marco ◽  
Almudena Prieto

2021 ◽  
Vol 920 (1) ◽  
pp. 62
Author(s):  
James Negus ◽  
Julia M. Comerford ◽  
Francisco Müller Sánchez ◽  
Jorge K. Barrera-Ballesteros ◽  
Niv Drory ◽  
...  
Keyword(s):  


1971 ◽  
Vol 43 ◽  
pp. 580-587 ◽  
Author(s):  
P. Charvin

We present polarization measurements obtained in 1970 in the green coronal line with a new coronameter located at the Pic du Midi. The analysis of these data has been conducted with the theory given by the writer in 1964 and 1965. It appears that magnetic field orientations in the Corona can be deduced from the above measurements. First results showing large scale magnetic structures are presented.



2015 ◽  
Vol 454 (4) ◽  
pp. 3688-3696 ◽  
Author(s):  
Hermine Landt ◽  
Martin J. Ward ◽  
Katrien C. Steenbrugge ◽  
Gary J. Ferland
Keyword(s):  


1986 ◽  
Vol 62 ◽  
pp. 939
Author(s):  
G. J. Ferland ◽  
D. L. Lambert ◽  
J. H. Woodman


1994 ◽  
Vol 159 ◽  
pp. 464-464
Author(s):  
I. Yankulova ◽  
V. Golev ◽  
T. Bonev ◽  
K. Jockers

We present new narrow-band images of the Extended Emission-Line Region (EELR) in NGC 3516 in light of [O III] λ 4959, Hα + [N II] λλ 6548, 84, [O I] λ 6364, He is/c λ 6678 and [Fe VII] + [Ca V] λ 6087. The observations were carried with the 2-m reflector of the Bulgarian National Astronomical Observatory and the Focal Reducer of the Max-Plank-Institut for Aeronomy. Our [O III] and Hα + [N II] images confirm previously reported EELR features. In contrast, the image in the high-excitation [Fe VII] + [Ca V] line shows a different structure. We identify a biconical morphology over a kiloparsec scale with peak intensities 5.9 × 10−16 ergs cm−2 s−1 arcsec−2 and 3.5 × 10−16 ergs cm−2 s−1 arcsec−2 to north and south of the nucleus, respectively. The total flux of the [Fe VII] + [Ca V] emission in 5″ and 24″ circular apertures centered at the nucleus is (9.97 ± 0.38) × 10−14 ergs cm−2 s−1 and (1.53 ± 0.15) × 10−13 ergs cm−2 s−1, respectively, which is in good agreement with measurements of Boksenberg & Netzer (1977) through the 5″ aperture. The cone axis lies at PA ∼ −10°. The continuum images (Veilleux et al., 1993, Miyaji et al., 1992) indicate a “bar” aligned along PA ∼ −10°. The velocity extrema regions revealed by Veilleux et al. (1993) are coincident with the peak intensities in our [Fe VII] + [Ca V]. We suppose that our image in [Fe VII] + [Ca V] outlines a Coronal-Line Region (CLR) of NGC 3516, which extends far beyond the classical NLR of the galaxy. Korista & Ferland (1989) have recently shown theoretically that the CLR in Seyferts may be a result of a low-density interstellar medium exposed to and photoionized by a “bare” active nucleus. A typical ISM with Ne ∼ 1–5 cm−3 may produce such an extended CLR as that observed by us.



1986 ◽  
Vol 60 ◽  
pp. 375 ◽  
Author(s):  
G. J. Ferland ◽  
D. L. Lambert ◽  
J. H. Woodman


2009 ◽  
Vol 5 (S267) ◽  
pp. 122-122
Author(s):  
X. Mazzalay ◽  
A. Rodríguez-Ardila ◽  
S. Komossa

AbstractWe present a study of HST/STIS optical spectra of a sample of ten Seyfert galaxies aimed at analyzing the structure and physical properties of the coronal line region. The high spatial resolution provided by STIS (about 7 pc for the closest objects) allowed us to resolve the coronal line region and obtain key information about the kinematics of the coronal-line gas, measure directly its spatial scale, and study the mechanisms that drive the high-ionization lines.



1998 ◽  
Vol 497 (1) ◽  
pp. L9-L12 ◽  
Author(s):  
Takashi Murayama ◽  
Yoshiaki Taniguchi


1997 ◽  
Vol 159 ◽  
pp. 246-247
Author(s):  
Stefanie Komossa ◽  
Henner Fink

We have studied the warm absorbers in several Seyfert galaxies using both PI and archival ROSAT data. The parameters that govern the emissivity of the ionized material, ionization parameter U, warm-absorber column density Nwa, and the source intrinsic power-law photon index Γx, are determined from X-ray spectral fits. These are then used to predict the expected IR to UV line emission of the ionized material in the individual objects. In particular, the possibility of a warm-absorber origin of one of the known emission-line regions in AGN is assessed. Good ‘candidate components’ are, e.g., the coronal-line region, and/or the high-ionization component of the NLR, or the component responsible for broad wings in the Balmer lines. All calculations have been carried out using the code CLOUDY (Ferland 1993).



1989 ◽  
Vol 134 ◽  
pp. 320-320
Author(s):  
K. T. Korista ◽  
G. J. Ferland

Photoionization model calculations suggest the possibility that the coronal line region in Seyfert galaxies may be the result of an interstellar medium exposed to and subsequently photoionized by a “bare” Seyfert nucleus. A series of models are presented in which a “generic” AGN continuum illuminates the low-density phase of the ISM of a spiral galaxy (Korista and Ferland 1988).



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