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4 edition of Spectra of high-ionization Seyfert 1 galaxies found in the catalog.

Spectra of high-ionization Seyfert 1 galaxies

Spectra of high-ionization Seyfert 1 galaxies

implications for the narrow-line region

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Published by National Aeronautics and Space Administration in [Washington, D.C .
Written in English

    Subjects:
  • Seyfert galaxies,
  • Atmospheric ionization

  • Edition Notes

    Other titlesSpectra of high ionization Seyfert 1 galaxies., Astrophysical journal. 0004-637X.
    StatementDavid Moore, Ross D. Cohen and Geoffrey W. Marcy.
    SeriesNASA-CR -- 204810., NASA contractor report -- NASA CR-204810.
    ContributionsCohen, Ross D., Marcy, Geoffrey W.
    The Physical Object
    FormatMicroform
    Pagination1 microfiche (24 fr.)
    Number of Pages24
    ID Numbers
    Open LibraryOL17604922M
    OCLC/WorldCa47440566

    line Spectra of the Orion Nebula, NGC , and Other Seyfert Galaxies”, Ap. J., , – 8. Veilleux, S. , “A Study of the Structure and Kinematics of the Narrow-Line Region of Seyfert Galaxies. I. Atlas of Line Profiles ”, Ap. J. Suppl., 75, – 9. Veilleux, S. , “A Study of the Structure and Kinematics of the. If the Unification Scheme is strictly applicable to all seyfert galaxies, and if the galaxy's HI disk is aligned with the accretion disk, then Sy-1 HI spectra should have the narrower velocity widths, while total derived HI masses and surface densities should be comparable for the .

    Abstract. Here we present an overview of some of the most significant observational and theoretical studies of the broad Fe K α spectral line, which is believed to originate from the innermost regions of relativistic accretion disks around central supermassive black holes of galaxies. The most important results of our investigations in this field are also vassilyk.com by: Active Galactic Nuclei “Mrk” means from the catalog of E. B. Markarian () who produced a catalog of Seyfert galaxies in Galaxies known to emit strongly in X-rays are Seyferts (type I’s have more X-rays than type II’s). Other types of Active Galaxies include radio .

    In November , the 2nd annual Spitzer Science Center international conference was held in Pasadena, California, USA. The purpose of this conference was to provide an overview of the role that infrared imaging and spectroscopy play in revealing the nature of astrophysical environments. I was fortunate also in having three other postdocs work with me at Lick. The first, Steve Grandi, worked on the optical spectra of broad-line radio galaxies (Grandi & Osterbrock ) and on the highest-ionization Seyfert 1 galaxies (Grandi ). Later, Jim Shuder worked on the broad-line profiles in Seyfert 1 galaxies and QSOs.


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Spectra of high-ionization Seyfert 1 galaxies Download PDF EPUB FB2

Add tags for "Spectra of high-ionization Seyfert 1 galaxies: implications for the narrow-line region". Be the first. of high-ionization mid-infrared lines as an indicator of AGN power.

They found a tight correlation, with a dispersion of ~ dex, in Seyfert 1 galaxies, between the [0 IV) and the X-ray keY continuum luminosities.

A weaker correlation was found for Seyfert. Seyfert galaxies are named for Carl K. Seyfert who indescribed them as their central regions having peculiar spectra with notable emission lines.

"Normal" (spiral) galaxies often have emission nebulae in their spiral arms, as have irregulars throughout; these regions, of course, show the corresponding emission lines in their spectra.

Sep 19,  · The correlation also holds for these high-ionization emission lines and the [Ne III] um (41 eV) emission line, although only for active galaxies. We used these correlations to calculate the [Ne III] excess due to star formation in Seyfert galaxies.

Nov 01,  · Much atomic data have already been calculated to analyze X-ray spectra of solar corona or laboratory plasmas. The well-known He-like ion diagnostics, have been extended from solar to non-solar coronae and also to photoionized plasmas.Besides these K-lines, Fe-L lines have also been observed in X-ray spectra for Seyfert 1, () and for Seyfert 2 () vassilyk.com by: 3.

A low-ionization nuclear emission-line region (LINER) is a type of galactic nucleus that is defined by its spectral line emission. The spectra typically include line emission from weakly ionized or neutral atoms, such as O, O +, N +, and S +. Seyfert Galaxies.

Seyfert galaxies are lower-luminosity active galactic nuclei, with M B > + 5 log h 0 for the active nucleus the generally accepted criterion, due originally to Schmidt & Green (), for distinguishing Seyfert galaxies from quasars.

A Seyfert galaxy has a quasar-like nucleus, but the host galaxy is clearly detectable. Ultraviolet and optical spectra are presented for three unusual Seyfert galaxies (MrkMrk 42, and Mrk ) that resemble Seyfert 1 galaxies in that they have strong high-ionization lines and.

We present a study of the intrinsic absorption lines in the ultraviolet spectra of Seyfert 1 galaxies. The study is based on spectra from the Hubble Space Telescope and includes the Seyfert 1 galaxies observed with the Faint Object Spectrograph and Goddard High-Resolution Spectrograph at spectral resolutions of λ/Δλ ≈, with good signal-to-noise ratios.

2, MID-IR HIGH-IONIZATION LINES FROM AGNs AND STAR-FORMING GALAXIES 1 10 Dist (Mpc) 0 10 20 30 40 50 60 70 80 N Figure 1. Distribution of the galaxy distances of the complete sample (black), QSO (gray), Seyfert 1 and 2 galaxies (red), LINERs (blue), and Hii galaxies (orange).

The excitation of optical permitted Fe II emission in Seyfert 1 galaxies and certain QSOs is considered in light of recent spectrophotometric observations. The Fe II emission is too strong to be explained by recombination.

Collisional excitation by itself does not appear capable of. Jun 01,  · Uncovering the Spectral Energy Distribution in Active Galaxies Using High Ionization Mid-infrared Emission Lines.

and and derive a best fit of?i ~ for Seyfert 1 galaxies. Only the high-ionization Seyfert 2 galaxy TF J{plus} is highly polarized, displaying a broad-line spectrum visible in polarized light.

The other two objects, TF J{plus} and FF J{plus}, display spectra dominated by a population of young (A type) stars similar to those of {open_quotes}E{plus}A{close_quotes} galaxies.

Type 1 Seyfert galaxies have in their spectra:. Type 2 Seyfert galaxies have only the narrow line component:. Both types have high ionization, forbidden lines. (= transitions not easily observed in the lab). Types of Seyfert Galaxies.

λ (Å). Spectroscopic Diagnostics. Spectra of high-ionization Seyfert 1 galaxies [microform]: implications for the narrow-line region / Da Was 49 [microform]: mirror for a hidden Seyfert 1 galaxy: IUE observing program final technical report Detection of [Ni II] [lambda] in six seyfert galaxies [microform] / J.P.

Halpern, J.B. Oke. Research into active galactic nuclei (AGN) – the compact, luminous hearts of many galaxies – is at the forefront of modern astrophysics.

Understanding these objects requires extensive knowledge in many different areas: accretion disks, the physics of dust and ionized gas, astronomical spectroscopy, star formation, and the cosmological evolution of galaxies and black vassilyk.com by: Seyfert galaxies—the most common examples of nearby active galaxies—are separated into two classes based on their emission line widths.

Evolutionary sequence of Seyfert galaxies: We suggest that there exists an evolutionary sequence from Seyfert 2 to Seyfert 1 galaxies.

• In Seyfert identified several optical [Fe VII] lines in the spectra of the nuclei of some galaxies - to become known as Seyfert galaxies • In the s rocket borne spectrographs revealed the UV spectrum of the corona • In Oke & Sargent report observations of a Seyfert Galaxy (NGC ) showing Fe XIV λ and Fe X λ Then seventeen years later Seyfert () studied these and other galaxies, and isolated the small fraction of them which show many relatively high-ionization emission lines in their nuclear spectra.

These nuclei are invariably highly luminous, and their emission lines are wider than the lower-ionization emission lines that occur in the spectra.

the literature, such as “Seyfert 1 galaxies” and “Seyfert 2 galaxies,” in honor of Carl Seyfert, who observed the first few galaxies of this type in the late s (see Chapter 6 for a detailed discussion of the various groups), are the result of an early confusion between different sources that are now known to have similar properties.

Seyfert and radio galaxies come in flavors with all emission lines about the same width (Seyfert 2, narrow-line radio galaxy or NLRG) and with certain emission lines much broader (Seyfert 1, broad-line radio galaxy or BLRG). These pairs are similar in optical spectrum, except that BLRGs may have.Mon.

Not. R. Astron. Soc.1–11 () Printed 28 April (MN LATEX style file v) Spectroscopic detection of CIV in a galaxy at z= Implications for the ionizing spectra of reionization-era galaxiesCited by: Type I AGN are also called Seyfert 1 galaxies or a Sy1s, ditto Sy2s).

See e.g. Gene Smith’s UCSD page. Types I and II AGN: Type I refers to AGN whose nucleus is visible (the spectra has both narrow and broad emission lines), while in type II AGN, the broad line region (BLR) is .