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2 edition of Structure and kinematics of two nearby disc galaxies found in the catalog.

Structure and kinematics of two nearby disc galaxies

Pieter Samuel Mulder

Structure and kinematics of two nearby disc galaxies

by Pieter Samuel Mulder

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  • 2 Currently reading

Published by Rijksuniversiteit te Groningen] in [The Netherlands .
Written in English

    Subjects:
  • Spiral galaxies.

  • Edition Notes

    StatementPieter Samuel Mulder.
    The Physical Object
    Pagination195 p. :
    Number of Pages195
    ID Numbers
    Open LibraryOL17253915M

    kinematics of halo stars (Majewski et al ), and the discovery of an elongated dwarf galaxy in Sagittarius (Ibata et al ). In addition most of the Milky Way satellites appear to be located near two great circles in the sky (Lynden-Bell ). The corona extends out to approximately kpc and may account for as much as (3–6) × M. Disk extends to at least 15 kpc from the Galactic center. Density of stars in the disk falls off exponentially, both radially and vertically: € n(R)∝e−RhR disk scale length hR ~ 3 kpc Most of the stars (95%) lie in a thin disk, with a vertical scale height ~ pc. Rest form a thick disk with a vertical scale height ~ 1 kpc. Thin disk.

    We present deep optical long-slit spectra of 17 edge-on spiral galaxies of intermediate to late morphological type, mostly parallel to their major axes and in a few cases parallel to the minor line-of-sight stellar kinematics are obtained from the stellar absorption lines using the improvedc ross-correlation technique. A large fraction of disk galaxies have bars: narrow linear structures crossing the face of the galaxy. In barred S0 galaxies the bar is often the only structure visible in the disk. In types Sa and later the bar often connects to a spiral pattern extending to larger radii (e.g. ).

    We present a catalog of the neutral atomic hydrogen structures (H I holes) and the analysis of their properties in nearby (≤ Mpc) gas-rich dwarf galaxies of the LITTLE THINGS (Local Irregulars That Trace Luminosity Extremes, The H I Nearby Galaxy Survey) group. We used high sensitivity (≤ mJy beam-1 channel-1), high velocity resolution ( km s-1 to km s-1) and high linear Author: Nau Raj Pokhrel. The Atlas of Peculiar Galaxies is a catalog of peculiar galaxies produced by Halton Arp in A total of galaxies are presented in the atlas, which was originally published in by the California Institute of primary goal of the catalog was to present photographs of examples of the different kinds of peculiar structures found among zation: California Institute of Technology.


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Structure and kinematics of two nearby disc galaxies by Pieter Samuel Mulder Download PDF EPUB FB2

This book addresses the structure and kinematics. A word of explanation: kinematics is the study of motion without reference to the forces which cause the motion -- dynamics addresses that, and that is not included in this text, but rather left for a second by: University of Groningen Structure and kinematics of two nearby disc galaxies Mulder, P.

Structure and kinematics of two nearby disc galaxies book NOTE: You are advised to consult the publisher's version (publisher Author: P.

Mulder. Structure and kinematics of two nearby disc galaxies () Pagina-navigatie: Main; Save publication. Save as MODS; Export to Mendeley; Save as EndNoteAuthor: P. Mulder. Wiggles in the rotation curve of the galaxies are clearly connected to the observed two-disk structure.

They are not caused by intrinsically peculiar kinematics of the objects, but simply by the superposition of the (hot) bulge component and the two (cold) disk by: 4.

The morphology and kinematics of interstellar gas in the nearby disc galaxies NGC (= Messier 94) and NGC (= Arp ), derived from observations in the 21 cm line of neutral hydrogen and in the H alpha line, are compared to the results of simulations of the dynamics of an ensemble of gas clouds in an external by: 1.

The two basic classes of galaxies are the ellipticals and the disk galaxies. Disk galaxies generally possess a nuclear bulge, which is similar to ellipticals in many respects, and a disk in which.

Spectroscopic observations of three lenticular (S0) galaxies (NGCNGCand NGC ) and one SBa galaxy (NGC ) have been taken with the 6-m telescope of the Special Astrophysical. Disks of Galaxies: Kinematics, Dynamics and Perturbations Volume: Year: View this Volume on ADS: Editors: Athanassoula, E.; Bosma, A.; Mujica, R.

ISBN: eISBN: Electronic access to books and articles is now available to purchase. Volume eAccess: $ We parametrise the structure and kinematics of four large and massive spiral galaxies in terms of a tilted-ring model of the H i disk.

Only one of the examined galaxies shows a typical warp structure, suggesting that warps are rarer towards larger masses of spiral galaxies. The galaxies show a sharp drop in the H i surface density profile at a Cited by: 3. Abstract.

Spectroscopic observations of three lenticular (S0) galaxies (NGCNGCand NGC ) and one SBa galaxy (NGC ) have been taken with the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences aimed to study the structure and kinematic properties of early-type disk by: Instead, integral-field spectroscopic can efficiently recognize the shape, dynamics and stellar population of complete samples of early-type galaxies (ETGs).

These studies showed that the two main classes, the fast and slow rotators, can be separated using stellar kinematics. We showed there is a dichotomy in the dynamics of the two by:   The stellar kinematics of 15 intermediate- to late-type edge-on spiral galaxies were modelled to study the dynamical properties of their stellar discs.

The sample covers a substantial range in both galaxy maximum rotational and deprojected face-on disc surface by: COVID Resources.

Reliable information about the coronavirus (COVID) is available from the World Health Organization (current situation, international travel).Numerous and frequently-updated resource results are available from this ’s WebJunction has pulled together information and resources to assist library staff as they consider how to handle coronavirus.

Galaxies: from Kinematics to Dynamics 3 Figure 1. Spectra of a star and a galaxy, showing how the absorption lines in the latter are shifted and broadened relative to the former. a spectrum S(u) obtained using an observation of a suitable nearby “template” star.

In practice, such unconstrained deconvolutions are hopelessly unstable. The. This places severe limits, for example, on the stellar and total M/L in these disk systems. (d) A Face-On Tully-Fisher Relation: Another side-product of this survey is the first determination of the line-wdith--luminosity relation for face-on galaxies.

This is significant for two reasons. This book contains an up-to-date review of the structure and evolution of disk galaxies from both the observational and theoretical point of view.

The book is the proceedings of the "Island Universes" conference held at the island of Terschelling, The Netherlands in Julywhich attracted about experts and students in the field. Abstract. We present stellar kinematics of 22 nearby early-type galaxies (ETGs), based on two-dimensional (2D) absorption line stellar spectroscopy out to ~ R e (effective radii), as part of the ongoing SLUGGS Survey.

The galaxies span a factor of 20 in intrinsic luminosity, as well as a full range of environment and ETG by: Internal Kinematics and Dynamics of Galaxies.

Editors: Athanassoula, E. (Ed.) Free Preview. Buy this book eB49 Gas and Star Kinematics in Elliptical Galaxies. Energy Transfer During the Tidal Encounter of Disc Galaxies. This book addresses the structure and kinematics. A word of explanation: kinematics is the study of motion without reference to the forces which cause the motion -- dynamics addresses that, and that is not included in this text, but rather left for a second volume/5.

important to have an understanding of the structure and kinematics of the LMC. This is the topic of the present review. For information on other aspects of the LMC, the reader is referred to the book by Westerlund ().The book by van den Bergh () discusses more generally how the properties of the LMC compare to those of other galaxies in the.

THE MOSDEF SURVEY: DYNAMICAL AND BARYONIC MASSES AND KINEMATIC STRUCTURES OF STAR-FORMING GALAXIES AT z Sedona H. Price1, Mariska Kriek1, Alice E. Shapley2, Naveen A. Reddy3,5, William R. Freeman3, Alison L. Coil4, Laura de Groot3, Irene Shivaei3, Brian Siana3, Mojegan Azadi4, Guillermo Barro1, Bahram Mobasher3, Ryan L.

Sanders2, and Tom Zick1.Galaxy Kinematics. Galaxy kinematics - the measurement of the motions of luminous gas and stars -- provides fundamental tools for answering basic questions about when and how disk galaxies formed. For example, these motions allow us to infer the distribution of dynamical mass within galaxies, and hence the shape of their gravitational potentials.Abstract The kinematics of the inner zones of disc galaxies have recently been shown to be much more complicated than previously thou-ght.

New instruments and more sensitive detectors have allowed us to obtain spectra of higher S/N ratio and resolution, as well as images, for a more refined study of these inner zones. Decoupled kinematic cores have been known for some time to exist in.