[go: up one dir, main page]
More Web Proxy on the site http://driver.im/
Skip to main content
We gratefully acknowledge support from the Simons Foundation, member institutions, and all contributors. Donate
arXiv logo
Cornell University Logo

Astrophysics

arXiv:astro-ph/0011146 (astro-ph)
[Submitted on 7 Nov 2000 (v1), last revised 19 Nov 2000 (this version, v2)]

Title:Modelling gaseous and stellar kinematics in the disc galaxies NGC 772, NGC 3898, and NGC 7782

Authors:E. Pignatelli (1), E. M. Corsini (2), J. C. Vega Beltran (3), C. Scarlata (4)A. Pizzella (2), J. G. Funes, S.J. (5), W. W. Zeilinger (6), J. E. Beckman (3), F. Bertola (4) ((1) SISSA, Italy, (2) Osservatorio di Asiago, Italy, (3) IAC, Spain, (4) Universita' di Padova, Italy, (5) Vatican Observatory, Arizona, USA, (6) Universitat Wien, Austria)
View PDF
Abstract: We present V-band surface photometry and major-axis kinematics of stars and ionized gas of three early-type spiral galaxies, namely NGC 772, NGC 3898 and NGC 7782. For each galaxy we present a self-consistent Jeans model for the stellar kinematics, adopting the light distribution of bulge and disc derived by means of a two-dimensional parametric photometric decomposition. This allowed us to investigate the presence of non-circular gas motions, and derive the mass distribution of luminous and dark matter in these objects.
NGC 772 and NGC 7782 have apparently normal kinematics with the ionized gas tracing the gravitational equilibrium circular speed. This is not true in the innermost region (r < 8'') of NGC 3898 where the ionized gas is rotating more slowly than the circular velocity predicted by dynamical modelling. This phenomenon is common in the bulge-dominated galaxies for which dynamical modelling enables us to make the direct comparison between the gas velocity and the circular speed, and it poses questions about the reliability of galaxy mass distributions derived by the direct decomposition of the observed ionized-gas rotation curve into the contributions of luminous and dark matter.
Comments: 21 pages, 18 low resolution encapsulated postscript figures. For high resolution figures, see this http URL . Accepted for publications in MNRAS. Replaced with accepted version, with only minor changes. Tables with original data will be made available at CDS
Subjects: Astrophysics (astro-ph)
Cite as: arXiv:astro-ph/0011146
  (or arXiv:astro-ph/0011146v2 for this version)
  https://doi.org/10.48550/arXiv.astro-ph/0011146
Journal reference: Mon.Not.Roy.Astron.Soc. 323 (2001) 188
Related DOI: https://doi.org/10.1046/j.1365-8711.2001.04207.x

Submission history

From: Ezio Pignatelli [view email]
[v1] Tue, 7 Nov 2000 14:47:12 UTC (636 KB)
[v2] Sun, 19 Nov 2000 13:28:28 UTC (636 KB)
Full-text links:

Access Paper:

  • View PDF
  • TeX Source
  • Other Formats
view license
Current browse context:
astro-ph
< prev   |   next >
new | recent | 2000-11

References & Citations

export BibTeX citation

Bookmark

BibSonomy logo Reddit logo

Bibliographic and Citation Tools

Bibliographic Explorer (What is the Explorer?)
Connected Papers (What is Connected Papers?)
Litmaps (What is Litmaps?)
scite Smart Citations (What are Smart Citations?)

Code, Data and Media Associated with this Article

alphaXiv (What is alphaXiv?)
CatalyzeX Code Finder for Papers (What is CatalyzeX?)
DagsHub (What is DagsHub?)
Gotit.pub (What is GotitPub?)
Hugging Face (What is Huggingface?)
Papers with Code (What is Papers with Code?)
ScienceCast (What is ScienceCast?)

Demos

Replicate (What is Replicate?)
Hugging Face Spaces (What is Spaces?)
TXYZ.AI (What is TXYZ.AI?)

Recommenders and Search Tools

Influence Flower (What are Influence Flowers?)
CORE Recommender (What is CORE?)
IArxiv Recommender (What is IArxiv?)

arXivLabs: experimental projects with community collaborators

arXivLabs is a framework that allows collaborators to develop and share new arXiv features directly on our website.

Both individuals and organizations that work with arXivLabs have embraced and accepted our values of openness, community, excellence, and user data privacy. arXiv is committed to these values and only works with partners that adhere to them.

Have an idea for a project that will add value for arXiv's community? Learn more about arXivLabs.

Which authors of this paper are endorsers? | Disable MathJax (What is MathJax?)