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          Document History for Document ID 198573

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Document Version Version Comment Date Status
198573.0 [No comment] 28.05.2018 16:41 Released

ID: 198573.0, MPI für Astronomie / Publikationen_mpia
Possibly interacting Vorontsov-Velyaminov
galaxies. II. The 6-m telescope spectroscopy of
VV 080, 131, 499, 523 and 531
Authors:Pustilnik, S.; Zasov, A.; Kniazev, A.; Pramskij, A.; Ugryumov, A.; Burenkov, A.
Date of Publication (YYYY-MM-DD):2003
Title of Journal:Astronomy and Astrophysics
Journal Abbrev.:Astronomy and Astrophysics
Volume:400
Start Page:841
End Page:857
Review Status:not specified
Audience:Not Specified
Abstract / Description:In continuation of the program formulated in
Paper I we present results of long-slit
spectroscopy with the Russian 6-m telescope of
five more objects from the Vorontsov-Velyaminov
(hereafter VV) Atlas and Catalogue of
Interacting galaxies. These are the galaxies for
which the interaction is not evident, although
all of them are classified as multiple systems
(usually as ``nests'', ``chains'' and similar
systems). The spectrophotometry data enable us
to derive for all galaxies abundances of O, and
for some of them abundances of N, Ne and S. For
two of them chemical abundances are given for
the first time. In spectra of three of the
studied galaxies [O Iii] lambda 4363 line is
measured, and T_e and oxygen abundance are
derived by the classical method. For the two
others, empirical methods are used. For all 5
galaxies, the radial velocity distribution along
the slit was obtained in the H alpha; -line.
The studied galaxies represent a rather mixed
sample: from very low luminosity irregular
galaxies, like VV 499 (DDO 053), to rather bright
VV 523 (NGC 3991). Their metallicities vary from
Z ~ 1/25 Zsun for VV 499 to ~ 1/2
Zsun for VV 523. The morphology of
these galaxies ranges between typical dIrr (VV
080) through ring-like (VV 131) to clumpy Irr
(VV 523). Position-Velocity diagrams in the
H alpha; -line along the galaxy body imply the
existence of large-scale ionized gas
outflows/supershells around the sites of intense
current and/or recent SF activity. Sizes of
supershells vary in the range of several hundred
pc to ~ 2 kpc. For all studied galaxies we
examine their local environment and indicate the
nearest neighbouring objects capable of inducing
the observed enhanced star formation.
Free Keywords:galaxies: interactions; galaxies: abundances;
; galaxies: starburst; galaxies: irregular;
; galaxies: general
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
External Affiliations:Arkhyz, Karachai-Circassia, 369167, Russia; Isaac
Newton Institute of Chile, SAO Branch),
AB(Sternberg Astronomical Institute of the Moscow
State University, Universitetsky Pr., 13, Moscow,
119899, Russia), AC(Special Astrophysical
Observatory, Nizhnij Arkhyz, Karachai-Circassia,
369167, Russia; Max Planck Institut f uuml;r
Astronomie, K ouml;nigstuhl 17, 69117,
Heidelberg, Germany; Isaac Newton Institute of
Chile, SAO Branch), AD(Special Astrophysical
Observatory, Nizhnij Arkhyz, Karachai-Circassia,
369167, Russia; Isaac Newton Institute of Chile,
SAO Branch), AE(Special Astrophysical
Observatory, Nizhnij Arkhyz, Karachai-Circassia,
369167, Russia; Isaac Newton Institute of Chile,
SAO Branch), AF(Special Astrophysical
Observatory, Nizhnij Arkhyz, Karachai-Circassia,
369167, Russia; Isaac Newton Institute of Chile,
SAO Branch)
Identifiers:URL:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bi... [ID No:1]