Starbursts in the Irregular Galaxy VV 523

Hecquet, J.; Augarde, R.; Coupinot, G.; Aurière, M.

doi:10.1017/cbo9780511600159.056

Cited by 4 publications

(10 citation statements)

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“…Compelling evidence of interaction-induced disturbances in VV 523 may include the abovementioned solid-body rotation curve for at least a half of the visible disk extent and also the clearly seen optical disk warps. Hecquet et al (1995) come to similar conclusion on the interaction-induced SF in this galaxy.…”

Section: Environment and Interactionssupporting

confidence: 74%

“…A strong high excitation emission-line spectrum and unusually blue colour of VV 523: (U − B = −0. m 33), along with high FIR luminosity, far exceeding the optical one (Hecquet et al 1995), reveal very intense star formation all over the galaxy. Its blue luminosity is unusually high for Irr galaxies (M B ≈ −21.…”

Section: Environment and Interactionmentioning

confidence: 97%

“…The most detailed investigations were presented by Hecquet et al (1995, see also references there to earlier works). These authors carried out BRI-photometry (including photometry of individual clumps) and long-slit spectroscopy to study kinematics, physical conditions in ionized gas and its oxygen abundance.…”

Section: Environment and Interactionmentioning

confidence: 99%

“…Hecquet et al (1995) give for knot "d" (their region "C"), based on the empirical method of Edmunds Pagel (1984), the value of 12 + log (O/H) = 8.43 ± 0.20. Our estimate of this value by the classic method is of very low accuracy: 8.33 ± 0.30.…”

Section: Spectral Observationsmentioning

confidence: 99%

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Possibly interacting Vorontsov-Velyaminov galaxies

Pustilnik

Засов

Kniazev

et al. 2003

A&A

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Abstract. 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 ] λ4363 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 Hα-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 Z for VV 499 to ∼1/2 Z 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 Hα-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.

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Section: Environment and Interactionssupporting

confidence: 74%

Section: Environment and Interactionmentioning

confidence: 97%

Section: Environment and Interactionmentioning

confidence: 99%

Section: Spectral Observationsmentioning

confidence: 99%

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Possibly interacting Vorontsov-Velyaminov galaxies

Pustilnik

Засов

Kniazev

et al. 2003

A&A

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“…-Gamma-ray burst: GRB detection (Kolaczyk, 1997;Norris et al, 1994) and GRB analysis (Greene et al, 1997;Walker et al, 2000). -Black hole: periodic oscillation detection (Steiman-Cameron et al, 1997;Scargle, 1997) -Galaxies: starburst detection (Hecquet et al, 1995), galaxy counts (Aussel et al, 1999;Damiani et al, 1998), morphology of galaxies (Weistrop et al, 1996;Kriessler et al, 1998), multifractal character of the galaxy distribution (Martinez et al, 1993). -Galaxy cluster: sub-structure detection (Pierre and Krywult et al, 1999;Arnaud et al, 2000), hierarchical clustering (Pando et al, 1998a), distribution of superclusters of galaxies (Kalinkov et al, 1998).…”

Section: Introductionmentioning

confidence: 99%

Astronomical Image and Data Analysis

Starck

Murtagh

2002

Astronomy and Astrophysics Library

185

162

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Cover picture: Five-minute exposure (five 60-second dithered and stacked images), R filter, taken with CFH12K wide-field camera (100 million pixels) at the primary focus ofthe CFHT in July 2000. The image is from an extremely rich zone of our Galaxy, containing star formation regions, dark nebulae (molecular c10uds and dust regions), emission nebulae (Ha regions), and evolved stars which are scattered throughout the field in their two-dimensiona1 projection effect. This zone is in the constellation of Sagittarius. (©Canada-France-Hawaii Telescope, J.-C. Cuillandre,

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Panchromatic Study of Nearby Ultraviolet-bright Starburst Galaxies: Implications for Massive Star Formation and High-Redshift Galaxies

Conselice¹,

Gallagher²,

Calzetti³

et al. 2000

The Astronomical Journal

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We present a panchromatic study of nearby starburst galaxies from the ultraviolet to the visible, including narrow band Hα using WIYN and HST data, to determine how star formation processes affect the morphology and integrated fluxes of nearby starbursts. We find the UV/Hα morphology of starbursts tend to differ, although not in a standard or predictable manner. From our sample of six nearby starbursts, three systems show a good correlation between UV and Hα fluxes, but we find differences in UV and Hα morphology between the other three. Occasionally we find systems with well defined H II regions without the corresponding brightness in the UV, and vice-versa. We discuss the likely mechanisms behind these differences which include: starburst ages, dust absorption, stellar energy ejecta through SNe and winds, as well as leakage of UV photons from stellar clusters. We conclude that the large scale morphological features in starbursts are primarily due to both age and absorption from a 'picket fence' dust distribution.We further demonstrate the similarity and differences between these nearby starbursts and high redshift star forming galaxies. The overall morphology of our sample of starbursts changes little between UV and visible wavelengths. If high redshift galaxies are similar to these starbursts, their morphologies should change little between rest-frame UV and optical. We also show that FIR and UV spectral energy distributions and slopes can be used to determine large scale morphological features for extreme starbursts, with the steepest FIR slopes correlating with the most disturbed galaxies.

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Starbursts in the Irregular Galaxy VV 523

Cited by 4 publications

References 0 publications

Possibly interacting Vorontsov-Velyaminov galaxies

Possibly interacting Vorontsov-Velyaminov galaxies

Astronomical Image and Data Analysis

Panchromatic Study of Nearby Ultraviolet-bright Starburst Galaxies: Implications for Massive Star Formation and High-Redshift Galaxies

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