The IBISCO survey. I. Multiphase discs and winds in the Seyfert galaxy Markarian 509

AbstractThe role of starburst winds versus active galactic nuclei (AGN) jets/winds in the formation of the kiloparsec scale radio emission seen in Seyferts is not yet well understood. In order to be able to disentangle the role of various components, we have observed a sample of Seyfert galaxies exhibiting kpc-scale radio emission suggesting outflows, along with a comparison sample of starburst galaxies, with the EVLA B-array in polarimetric mode at 1.4 GHz and 5 GHz. The Seyfert galaxy NGC 2639, shows highly polarized secondary radio lobes, not observed before, which are aligned perpendicular to the known pair of radio lobes. The additional pair of lobes represent an older epoch of emission. A multi-epoch multi-frequency study of the starburst-Seyfert composite galaxy NGC 3079, reveals that the jet together with the starburst superwind and the galactic magnetic fields might be responsible for the well-known 8-shaped radio lobes observed in this galaxy. We find that many of the Seyfert galaxies in our sample show bubble-shaped lobes, which are absent in the starburst galaxies that do not host an AGN.

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Classification of Compact Objects: QSS, QSOs, N-Type and Compact Galaxies, Seyfert and Galactic Nuclei

Symposium - International Astronomical Union ◽

10.1017/s0074180900005386 ◽

1972 ◽

Vol 44 ◽

pp. 97-103

Author(s):

W. W. Morgan

Keyword(s):

Galactic Nuclei ◽

Seyfert Galaxy ◽

Classification Criteria ◽

Compact Objects ◽

Stellar Objects ◽

Quasi Stellar Objects ◽

Compact Galaxies

Some methods currently in use for the classification of the optical forms of the ‘compact’ galaxies and quasi-stellar objects are reviewed. It is shown that the category ‘Seyfert Galaxy’ is basically a spectroscopic (rather than a form) classification.An optical form-classification is described which is, in principle, identical with published classification criteria for QSO, N-type, and compact objects. The importance of maintaining rigid form-standards is emphasized.

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Aperture Synthesis CO(J=1—0) Observations and Near-Infrared Photometry of the Non-Barred Seyfert Galaxy NGC 5033

Publications of the Astronomical Society of Japan ◽

10.1093/pasj/55.1.103 ◽

2003 ◽

Vol 55 (1) ◽

pp. 103-119 ◽

Cited By ~ 10

Author(s):

Kotaro Kohno ◽

Baltasar Vila-Vilaró ◽

Seiichi Sakamoto ◽

Ryohei Kawabe ◽

Sumio Ishizuki ◽

...

Keyword(s):

Near Infrared ◽

Seyfert Galaxy ◽

Aperture Synthesis ◽

Infrared Photometry

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Hour-timescale profile variations in the broad Balmer lines of the Seyfert galaxy Hour-timescale profile variations in the broad Balmer lines of the Seyfert galaxy Markarian 6

Proceedings of the International Astronomical Union ◽

10.1017/s1743921314004426 ◽

2013 ◽

Vol 9 (S304) ◽

pp. 407-408

Author(s):

Norayr S. Asatrian

Keyword(s):

Fine Structure ◽

Emission Line ◽

Sampling Rate ◽

Seyfert Galaxy ◽

Special Astrophysical Observatory ◽

Balmer Line ◽

Line Profiles ◽

Balmer Lines ◽

Profile Changes ◽

Hydrogen Emission Line

AbstractPart of results of the multi-epoch intranight optical spectroscopic monitoring of the Markarian 6 nucleus carried out at the telescopes of 6-m of the Special Astrophysical Observatory (Russia), 2.6-m of the Byurakan Astrophysical Observatory (Armenia) and 2-m of the Tautenburg Observatory (Germany) is presented.Observations were made in 1979, 1986, 1988-1991 and 2007-2009 during a total of 33 nights with an average sampling rate of 4 spectra per night. TV-scanner and long-slit spectrographs equipped with Image Tube and CCD detector arrays were used. Altogether we analyzed 110 Hβ and 58 Hα region spectra to search for intranight variability in the broad hydrogen emission line profiles. The typical spectral resolutions were 4 Å for scanner spectra, 6 Å for photographic spectra, and 5 Å and 10 Å for CCD spectra. The S/N ratio at the continuum level near the Hβ and Hα lines was in the range 15–50.The purpose of the search was to look for the characteristic variability signatures of different kinematical models of the broad emission-line region. We considered the centering and guiding errors which can result in differences between spectra.We found variations in the broad Balmer line difference profiles on time scale of hour with the level of significance of 3.6 σ to 5.0 σ. Variations take the form of narrow, small bumps located at the blue and red sides or only at the blue side of the lines. In the intermediate level of broad line flux, the Hβ and Hα profiles show fine structure. Detected profile changes occurred at the same radial velocity shifts as the details in the fine structure.The variability is at least 2 orders of magnitude more rapid than any observed for broad Balmer line profiles in AGNs that we are aware of in the literature.Discovered extremely rapid line-profile variability may be associated with reverberation effects. Two-sided profile changes may indicate the response of circularly rotating hydrogen clouds in the BLR to a light pulse from a central source. One-sided profile variations may be attributed to a response of a non-disk component: the subarcsec scale region of the jet.

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