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

2005 ◽  
pp. 315-320
Author(s):  
Olivier Marco ◽  
Almudena Prieto
Keyword(s):  
Coronal Line ◽  
Line Region ◽  
First Results

The Physics of the Coronal-line Region for Galaxies in Mapping Galaxies at Apache Point Observatory

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

scholarly journals Experimental Study of the Orientation of Magnetic Fields in the Corona

1971 ◽  
Vol 43 ◽  
pp. 580-587 ◽  
Author(s):  
P. Charvin
Keyword(s):  
Magnetic Field ◽  
Experimental Study ◽  
Magnetic Fields ◽  
Large Scale ◽  
Coronal Line ◽  
Magnetic Structures ◽  
Polarization Measurements ◽  
First Results

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.

scholarly journals Strong variability of the coronal line region in NGC 5548

2015 ◽  
Vol 454 (4) ◽  
pp. 3688-3696 ◽  
Author(s):  
Hermine Landt ◽  
Martin J. Ward ◽  
Katrien C. Steenbrugge ◽  
Gary J. Ferland
Keyword(s):  
Coronal Line ◽  
Line Region ◽  
Ngc 5548

Spectroscopic Observations of Nova Cygni 1975: The Coronal Line Region Revisited: Erratum

1986 ◽  
Vol 62 ◽  
pp. 939
Author(s):  
G. J. Ferland ◽  
D. L. Lambert ◽  
J. H. Woodman
Keyword(s):  
Coronal Line ◽  
Spectroscopic Observations ◽  
Line Region

scholarly journals The Anisotropic Radiation Field in NGC 3516

1994 ◽  
Vol 159 ◽  
pp. 464-464
Author(s):  
I. Yankulova ◽  
V. Golev ◽  
T. Bonev ◽  
K. Jockers
Keyword(s):  
Narrow Band ◽  
Coronal Line ◽  
Active Nucleus ◽  
Cone Axis ◽  
Line Region ◽  
The Galaxy ◽  
North And South ◽  
Extended Emission ◽  
Good Agreement ◽  
The Continuum

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.

Spectroscopic observations of Nova Cygni 1975 - The coronal line region revisited

1986 ◽  
Vol 60 ◽  
pp. 375 ◽  
Author(s):  
G. J. Ferland ◽  
D. L. Lambert ◽  
J. H. Woodman
Keyword(s):  
Coronal Line ◽  
Spectroscopic Observations ◽  
Line Region

scholarly journals The Coronal Emission-Line Region in AGNs: A Hubble Space Telescope View

2009 ◽  
Vol 5 (S267) ◽  
pp. 122-122
Author(s):  
X. Mazzalay ◽  
A. Rodríguez-Ardila ◽  
S. Komossa
Keyword(s):  
Physical Properties ◽  
Spatial Resolution ◽  
High Spatial Resolution ◽  
Hubble Space Telescope ◽  
Seyfert Galaxies ◽  
Coronal Line ◽  
Coronal Emission ◽  
Line Region ◽  
High Ionization ◽  
Coronal Emission Line

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.

scholarly journals Where Is the Coronal Line Region in Active Galactic Nuclei?

1998 ◽  
Vol 497 (1) ◽  
pp. L9-L12 ◽  
Author(s):  
Takashi Murayama ◽  
Yoshiaki Taniguchi
Keyword(s):  
Active Galactic Nuclei ◽  
Galactic Nuclei ◽  
Coronal Line ◽  
Line Region

scholarly journals Properties of Warm Absorbers and Constraints from their Optical and UV Line Emission

1997 ◽  
Vol 159 ◽  
pp. 246-247
Author(s):  
Stefanie Komossa ◽  
Henner Fink
Keyword(s):  
Line Emission ◽  
Seyfert Galaxies ◽  
Coronal Line ◽  
X Ray ◽  
Line Region ◽  
High Ionization ◽  
Photon Index ◽  
Balmer Lines ◽  
The Individual ◽  
Ionization Parameter

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).

scholarly journals The Origin of the Coronal Lines in Seyfert Galaxies

1989 ◽  
Vol 134 ◽  
pp. 320-320
Author(s):  
K. T. Korista ◽  
G. J. Ferland
Keyword(s):  
Interstellar Medium ◽  
Spiral Galaxy ◽  
Seyfert Galaxies ◽  
Low Density ◽  
Coronal Line ◽  
Model Calculations ◽  
Line Region ◽  
Seyfert Nucleus ◽  
Photoionization Model

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).

Sign in / Sign up

Export Citation Format

Share Document