2009ApJ...696.1668B


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.05CEST06:48:23

2009ApJ...696.1668B - Astrophys. J., 696, 1668-1682 (2009/May-2)

The internal kinematics of the H II galaxy II Zw 40.

BORDALO V., PLANA H. and TELLES E.

Abstract (from CDS):

We present a study of the kinematic properties of the ionized gas in the dominant giant H II region of the well known H II galaxy: II Zw 40. High spatial and spectral resolution spectroscopy has been obtained using the Integral Field Unit mode on the Gemini Multi-Object Spectrograph instrument at the Gemini-North7Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (USA), the Science and Technology Facilities Council (UK), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil), and CONICET (Argentina). telescope. The observations allow us to obtain the Hα intensity map, the radial velocity and velocity dispersion maps as well as estimate some physical conditions in the inner region of the starburst, such as oxygen abundance (O/H) and electron density. We have used a set of kinematics diagnostic diagrams, such as the intensity versus velocity dispersion (I-σ), intensity versus radial velocity (I-V), and V-σ, for global and individual analysis in the subregions of the nebula. We aim to separate the main line broadening mechanisms responsible for producing a smooth supersonic integrated line profile for the giant H II region. Bubbles and shells driven by stellar winds and possibly supernovae, covering a large fraction on the face of the nebula, are identified on scales larger than 50 pc. We found that unperturbed or "free from shells" regions showing the lowest σ values (∼20 km/s) should be good indicators for the σgrav component in II Zw 40. The brightest central region (R ∼ 50 pc) is responsible for σ derived from a single fit to the integrated line profile. The dominant action of gravity, and possibly unresolved winds of young (<10 Myr) massive stars, in this small region should be responsible for the characteristic Hα velocity profile of the starburst region as a whole (σ = 32-35 km/s). Our observations show that the complex structure of the interstellar medium of this galactic scale star-forming region is very similar to that of nearby extragalactic giant H II regions in the Local Group galaxies.

Abstract Copyright:

Journal keyword(s): galaxies: individual: II Zw 40 - Galaxy: kinematics and dynamics

Simbad objects: 13

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Number of rows : 13

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 588 HII 01 32 45.2 +30 38 54 14.59 14.40 14.44 14.89 15.16 ~ 116 1
2 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5134 1
3 NGC 604 HII 01 34 32.1 +30 47 01           ~ 544 0
4 NGC 1036 G 02 40 28.982 +19 17 49.48   13.5       ~ 107 0
5 NGC 1569 IG 04 30 49.186 +64 50 52.52 11.72 11.86 11.03     ~ 1147 3
6 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14826 1
7 M 42 HII 05 35 17.3 -05 23 28           ~ 3724 0
8 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1734 1
9 UGCA 116 H2G 05 55 42.645 +03 23 32.23 10.74 11.68 11.46   11.82 ~ 500 0
10 NGC 7625 IG 23 20 30.132 +17 13 32.16 13.31 13.23 11.98 11.25   ~ 242 0
11 NAME Cas A SNR 23 23 24.000 +58 48 54.00           ~ 2413 1
12 Mrk 324 G 23 26 32.783 +18 16 00.07   15.5       ~ 63 0
13 NAME Local Group GrG ~ ~           ~ 6970 0

    Equat.    Gal    SGal    Ecl

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2020.07.05-06:48:23

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