scholarly journals Photoelectric Observations of Continuous and Emission Lines Variability in Spectra of Seyfert Galaxy NGC 1275 Nucleus

1987 ◽  
Vol 121 ◽  
pp. 195-197
Author(s):  
I. Pronik ◽  
N. Merkulova
Keyword(s):  
Time Scale ◽  
Filling Factor ◽  
Seyfert Galaxy ◽  
Emission Lines ◽  
The Galaxy ◽  
Photoelectric Observations ◽  
Ngc 1275 ◽  
Galaxy Nucleus

The spectral observations of NGC 1275 nucleus in the range of 3700-7000 AA being carried out since 1971 to 1978 showed the existance of hydrogen and forbidden emission lines variability with the time scale of 5–6 and 1–2 years (Pronik, 1980). Observations on 6-m telescope during 4 nights in January, 1977 permit to reveal the scale variability of these lines 2–3 days, too (Merkulova, Pronik, 1985). These results evidenced the necessary of close photoelectric series of spectral observations of the galaxy nucleus with the filling factor of several days and hours.

scholarly journals The NGC 1275 Galaxy Nucleus Emission Spectrum Variability at Various Stages of Activity

1989 ◽  
Vol 134 ◽  
pp. 88-89
Author(s):  
I. I. Pronik
Keyword(s):  
Emission Spectrum ◽  
Time Scale ◽  
Seyfert Galaxy ◽  
Emission Lines ◽  
Photoelectric Observations ◽  
Ngc 1275 ◽  
Galaxy Nucleus

Emission lines variability of Seyfert galaxy NGC 1275 nucleus in the scales of years and months has been observed since 1971 (I. Pronik, 1980). The photoelectric observations of I. Pronik and N. Merkulova (1987) show, that the variability in Hβ and 4959+ 5007 A [OIII] lines occurs also in the time scale of several days. Hereinafter the analysis of Hβ and [OIII] variable emission lines within months is presented according to photographic observations carried out from 1971 till 1982 by I. Pronik (1980), V. Doroshenko and V. Terebizh (1983) and K. Chuvaev (1985).

scholarly journals Variability of the Emission Line Spectrum of the Nucleus of Seyfert Galaxy NGC 1275

1974 ◽  
Vol 58 ◽  
pp. 341-345
Author(s):  
I. Pronik
Keyword(s):  
Emission Line ◽  
Seyfert Galaxy ◽  
Emission Lines ◽  
Line Spectrum ◽  
Spectroscopic Observations ◽  
Emission Line Spectrum ◽  
Ngc 1275

Recent spectroscopic observations of the nucleus of NGC 1275, together with results from earlier workers, confirm the variability of the emission lines and indicate corresponding variations in the electron temperatures and densities of different zones. These changes may be associated with the microwave outbursts from this source.

scholarly journals Spectrophotometry of Selected AGN Seyfert Galaxy AKN 564

1999 ◽  
Vol 194 ◽  
pp. 87-89
Author(s):  
L.S. Slavcheva ◽  
B.M. Mihov ◽  
G.T. Petrov ◽  
R.S. Bachev
Keyword(s):  
Electron Temperature ◽  
Electron Density ◽  
Seyfert Galaxy ◽  
Emission Lines ◽  
Narrow Line ◽  
Line Region ◽  
The Galaxy ◽  
Narrow Line Region ◽  
Image Position ◽  
Typical Temperature

Akn 564 (α1950 = 22h40m18.3s, δ1950 = 29°27′47″) is a Sy1.5G SBb type galaxy. According to Zwicky (1966) it has a photographic magnitude mp = 14.4 and a redshift of 0.025. The spectra of the galaxy were obtained at the 2.6-m telescope of the Crimean Astrophysical Observatory with a spectrograph having a dispersion of 100 A mm−1. They were processed with the help of SPEC and LONG packages integrated in MIDAS. As a result of the spectrophotometry we obtain the fluxes at λλ 4363, 4959, 5007 A: I(4363), I(4959), I(5007). The spectrum of the galaxy in λλ 4000–7000 is shown in Figure 1. We use the relation of the fluxes of those narrow forbidden emission lines: sensitive at a greater extent to the electron temperature Te than to the electron density ne. The value of R = 74.3 we got, having a typical value of ne = 5×105 cm−3 for the NLR (Narrow Line Region), leads to the estimation of a typical temperature of Te = 104 K.

scholarly journals Gas and Stellar Kinematics in the Disk and Bar of Mrk 573

1996 ◽  
Vol 157 ◽  
pp. 218-220 ◽  
Author(s):  
V. L. Afanasiev ◽  
A. N. Burenkov ◽  
A. I. Shapovalova ◽  
V. V. Vlasyuk
Keyword(s):  
Velocity Field ◽  
Complex Structure ◽  
Seyfert Galaxy ◽  
Helical Structure ◽  
Emission Lines ◽  
Stellar Kinematics ◽  
Gas Distribution ◽  
Fabry Perot ◽  
The Galaxy ◽  
Galaxy Center

AbstractResults of 3D-spectroscopy for the nearby Seyfert galaxy Mrk 573 obtained at the 6-m telescope with the scanning Fabry-Perot interferometer and the Multi-Pupil Field Spectrograph (MPFS) are presented. Emission lines images of the galaxy center demonstrate a complex structure of ENLR, coinciding with the radio data. An analysis of the velocity field shows that some gas structures do not lie in the plane of the galaxy. An explanation of the observed velocity field and gas distribution by radiation of a helical structure located inside an ionization cone is proposed.

scholarly journals Ionized and hot molecular outflows in the inner 500 pc of NGC 1275

2020 ◽  
Vol 496 (4) ◽  
pp. 4857-4873
Author(s):  
Rogemar A Riffel ◽  
Thaisa Storchi-Bergmann ◽  
Nadia L Zakamska ◽  
Rogério Riffel
Keyword(s):  
Near Infrared ◽  
Line Emission ◽  
Seyfert Galaxy ◽  
Gas Phases ◽  
Gas Kinematics ◽  
The Galaxy ◽  
Stellar Velocity ◽  
Mass Outflow ◽  
Integral Field Spectrograph ◽  
Ngc 1275

ABSTRACT The role of feedback from active galactic nuclei (AGNs) in the evolution of galaxies is still not fully understood, mostly due to the lack of observational constraints in the multiphase gas kinematics on the 10–100 pc scales. We have used the Gemini Near-Infrared Integral Field Spectrograph (NIFS) to map the molecular and ionized gas kinematics in the inner 900 × 900 pc2 of the Seyfert galaxy NGC 1275 at a spatial resolution of ∼70 pc. From the fitting of the CO absorption bandheads in the K band, we derive a stellar velocity dispersion of 265 ± 26 km s−1, which implies a black hole mass of $M_{\rm SMBH}=1.1^{+0.9}_{-0.5}\times 10^9$ M⊙. We find hot (T ≳ 1000 K) molecular and ionized outflows with velocities of up to 2000 km s−1 and mass outflow rates of $2.7\times 10^{-2}$  and $1.6\, {\rm M_\odot }$ yr−1, respectively, in each of these gas phases. The kinetic power of the ionized outflows corresponds to only 0.05 per cent of the luminosity of the AGN of NGC 1275, indicating that they are not powerful enough to provide significant AGN feedback, but may be effective in redistributing the gas in the central region of the galaxy. The AGN-driven outflows seem to be responsible for the shocks necessary to produce the observed H2 and [Fe ii] line emission.

Investigation of the nuclear region of the Seyfert galaxy NGC 1275

Astrophysics ◽  
1984 ◽  
Vol 21 (2) ◽  
pp. 470-478 ◽  
Author(s):  
L. P. Metik ◽  
I. I. Pronik
Keyword(s):  
Seyfert Galaxy ◽  
Nuclear Region ◽  
Ngc 1275

scholarly journals Limits to Ionization-parameter Mapping as a Diagnostic of Hii Region Optical Depth

2021 ◽  
Vol 923 (1) ◽  
pp. 78
Author(s):  
Amit N. Sawant ◽  
Eric W. Pellegrini ◽  
M. S. Oey ◽  
Jesús López-Hernández ◽  
Genoveva Micheva
Keyword(s):  
Optical Depth ◽  
Strong Dependence ◽  
Light Flux ◽  
Emission Lines ◽  
Ionization State ◽  
Hii Region ◽  
Parameter Mapping ◽  
Ionization Structure ◽  
The Galaxy ◽  
Ionization Parameter

Abstract We employ ionization-parameter mapping (IPM) to infer the optical depth of H ii regions in the northern half of M33. We construct [O iii]λ5007/[O ii]λ3727 and [O iii]λ5007/[S ii]λ6724 ratio maps from narrowband images continuum-subtracted in this way, from which we classify the H ii regions by optical depth to ionizing radiation, based on their ionization structure. This method works relatively well in the low-metallicity regime, 12 + log ( O / H ) ≤ 8.4 , where [O iii]λ λ4959, 5007 is strong. However, at higher metallicities, the method breaks down due to the strong dependence of the [O iii]λ λ4959, 5007 emission lines on the nebular temperature. Thus, although O++ may be present in metal-rich H ii regions, these commonly used emission lines do not serve as a useful indicator of its presence, and hence the O ionization state. In addition, IPM as a diagnostic of optical depth is limited by spatial resolution. We also report a region of highly excited [O iii] extending over an area ∼1 kpc across and [O iii]λ5007 luminosity of 4.9 ± 1.5 × 1038 erg s−1, which is several times higher than the ionizing budget of any potential sources in this portion of the galaxy. Finally, this work introduces a new method for continuum subtraction of narrowband images based on the dispersion of pixels around the mode of the diffuse-light flux distribution. In addition to M33, we demonstrate the method on C iii]λ1909 imaging of Haro 11, ESO 338-IG004, and Mrk 71.

scholarly journals Integral Field Spectrography of Active Galaxies with TIGER

1997 ◽  
Vol 159 ◽  
pp. 343-346
Author(s):  
P. Ferruit ◽  
E. Pécontal ◽  
G. Adam ◽  
R. Bacon
Keyword(s):  
Seyfert Galaxy ◽  
Active Galaxies ◽  
Data Cube ◽  
Complex Object ◽  
Integral Field Spectrograph ◽  
Deconvolution Techniques ◽  
Ngc 1275 ◽  
Integral Field

AbstractThe TIGER integral field spectrograph has been used to study nearby and distant active galaxies. We first present new TIGER observations of the Seyfert galaxy NGC 1275. In this very complex object, TIGER allows us to disentangle the contributions of the numerous components. We present the first very promising results on NGC 5252 obtained with the 3-D data-cube deconvolution techniques developed by our team in Lyon.

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