2012A&A...547A..24C


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.08CET14:02:21

2012A&A...547A..24C - Astronomy and Astrophysics, volume 547A, 24-24 (2012/11-1)

Mapping luminous blue compact galaxies with VIRUS-p. Morphology, line ratios, and kinematics.

CAIROS L.M., CAON N., GARCIA LORENZO B., KELZ A., ROTH M., PAPADEROS P. and STREICHER O.

Abstract (from CDS):

Blue compact galaxies (BCG) are narrow emission-line systems that undergo a violent burst of star formation. They are compact, low-luminosity galaxies, with blue colors and low chemical abundances, which offer us a unique opportunity to investigate collective star formation and its effects on galaxy evolution in a relatively simple, dynamically unperturbed environment. Spatially resolved spectrophotometric studies of BCGs are essential for a better understanding of the role of starburst-driven feedback processes on the kinematical and chemical evolution of low-mass galaxies near and far. We carry out an integral field spectroscopy (IFS) study of a sample of luminous BCGs, with the aim to probe the morphology, kinematics, dust extinction, and excitation mechanisms of their warm interstellar medium (ISM). We obtained IFS data for five luminous BCGs with VIRUS-P, the prototype instrument for the Visible Integral Field Replicable Unit Spectrograph, attached to the 2.7 m Harlan J. Smith Telescope at the McDonald Observatory. VIRUS-P consists of a square array of 247 optical fibers, which covers a 109"x109" field of view, with a spatial sampling of 4.2" and a 0.3 filling factor. We observed in the 3550-5850Å spectral range, with a resolution of 5 Å FWHM. From these data we built two-dimensional maps of the continuum and the most prominent emission-lines ([OII] λ3727, Hγ, Hβ and [OIII] λ5007), and investigated the morphology of diagnostic emission-line ratios and the extinction patterns in the ISM as well as stellar and gas kinematics. Additionally, from integrated spectra we inferred total line fluxes and luminosity-weighted extinction coefficients and gas-phase metallicities. All galaxies exhibit an overall regular morphology in the stellar continuum, while their warm ISM morphology is more complex: in II Zw 33 and Mrk 314, the star-forming regions are aligned along a chain-structure; Haro 1, NGC 4670 and III Zw 102 display several salient features, such as extended gaseous filaments and bubbles. A significant intrinsic absorption by dust is present in all galaxies, the most extreme case being III Zw 102. Our data reveal a plethora of kinematical patterns, from overall regular gas and stellar rotation to complex velocity fields produced by structurally and kinematically distinct components.

Abstract Copyright:

Journal keyword(s): galaxies: starburst - galaxies: dwarf - galaxies: abundances - galaxies: kinematics and dynamics

Simbad objects: 16

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Number of rows : 16

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 BD+52 913 WD* 05 05 30.6182785658 +52 49 51.920797126 10.25 11.44 11.69 11.93 12.108 DA.8 961 0
2 Mrk 1094 bCG 05 10 48.1119078356 -02 40 53.660806071   14.0 14.4     ~ 82 1
3 NGC 2415 bCG 07 36 56.730 +35 14 31.04   12.5       ~ 120 1
4 UGC 3937 G 07 37 35.2198070818 +35 36 21.093706515   14.2       ~ 34 0
5 Mrk 1418 G 09 40 27.0109496636 +48 20 15.457721241   13.5       ~ 59 0
6 NGC 3011 Sy2 09 49 41.2024715868 +32 13 15.994080462   14.2       ~ 77 0
7 NAME Great Attractor SCG 10 32 -46.0           ~ 444 0
8 Feige 34 HS* 10 39 36.7377085527 +43 06 09.209752646 9.613 10.91 11.14 11.319 11.464 sdOp 593 0
9 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5667 0
10 NGC 4670 IG 12 45 17.150 +27 07 31.76   12.6       ~ 225 0
11 NAME SHAPLEY-CENTAURUS CL SCG 13 06.0 -33 04           ~ 479 0
12 BD+33 2642 pA* 15 51 59.8857490337 +32 56 54.327647794 9.806 10.61 10.73 10.884 10.961 O7p 369 0
13 HD 227900 * 20 08 24.1415999720 +41 15 03.920107895 10.14 10.75 10.62     B2III 64 0
14 BD+25 4655 HS* 21 59 41.9751489837 +26 25 57.398356446 8.27 9.39 9.68     sdO6 97 0
15 NGC 7468 bCG 23 02 59.172 +16 36 16.20   14.0       ~ 152 0
16 NGC 7625 IG 23 20 30.132 +17 13 32.16 13.31 13.23 11.98 11.25   ~ 238 0

    Equat.    Gal    SGal    Ecl

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2019.12.08-14:02:21

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