Three-dimensional Spectroscopy of Blue Compact Galaxies: Diagnostic Diagrams

Martínez-Delgado, I.; Tenorio-Tagle, G.; Muñoz–Tuñón, C.; Моисеев, А. В.; Cairós, L. M.

doi:10.1086/515438

Cited by 30 publications

(33 citation statements)

References 18 publications

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“…A clear lower limit to the width of c1 observed in some studies of similar environments (Muñoz-Tuñón et al 1996;Martínez-Delgado et al 2007;Westmoquette et al 2007aWestmoquette et al , 2007b) supports this explanation. The only two broadening mechanisms that can work on a global scale are gravitationally induced virial motions and the stirring effects of wide-scale, intense star formation on the ambient ISM.…”

mentioning

confidence: 75%

Hubble Space TelescopeSpace Telescope Imaging Spectrograph Spectroscopy of the Environment in the Starburst Core of M82

Westmoquette

Smith

Gallagher

et al. 2007

ApJ

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We present optical HST STIS observations made with two slits crossing four of the optically brightest starburst clumps near the nucleus of M82. These provide H kinematics, extinction, electron density, and emission measures. From the radial velocity curves derived from both slits we confirm the presence of a stellar bar. We derive a new model for the orientation of the bar and disk with respect to the main starburst clumps and the cluster M82-A1. We propose that clump A has formed within the bar region as a result of gas interactions between the bar orbits, whereas region C lies at the edge of the bar and regions D and E are located farther out from the nucleus but heavily obscured. We derive extremely high interstellar densities of 500Y900 cm À3 , corresponding to ISM pressures of P/k % (0:5Y1:0) ; 10 7 cm À3 K, and discuss the implications of the measured gas properties on the production and evolution of the galactic wind. Despite varying pressures, the ionization parameter is uniform down to parsec scales, and we discuss why this might be so. Where the signal-to-noise ratios of our spectra are high enough, we identify multiple emission-line components. Through detailed Gaussian line fitting, we identify a ubiquitous broad (200Y300 km s À1 ) underlying component to the bright H line and discuss the physical mechanism(s) that could be responsible for such widths. We conclude that evaporation and/or ablation of material from interstellar gas clouds caused by the impact of highenergy photons and fast flowing cluster winds produce a highly turbulent layer on the surface of the clouds from which the emission arises.

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mentioning

confidence: 75%

Hubble Space TelescopeSpace Telescope Imaging Spectrograph Spectroscopy of the Environment in the Starburst Core of M82

Westmoquette

Smith

Gallagher

et al. 2007

ApJ

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“…Such high densities could be explained by collisions between molecular clouds of the interstellar medium, or by gas inflow events. R4 and R5 have also the largest equivalent widths ( Martínez-Delgado et al 2008), implying that they are very young starbursts, probably ignited by the galaxy collision. Oxygen abundances are slightly larger in the nucleus and in R3; this abundance difference is consistent with the merger hypothesis.…”

Section: Mrk 297mentioning

confidence: 99%

Integral Field Spectroscopy of Blue Compact Dwarf Galaxies

García-Lorenzo

Cairós

Caon

et al. 2008

ApJ

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We present results of integral field optical spectroscopy of five luminous blue compact dwarf galaxies. The data were obtained using the fiber system INTEGRAL attached to the William Herschel Telescope. region with a resolution of 0.9 00 spaxel À1 . We use high-resolution optical images to isolate the star-forming knots in the objects; line ratios, electron densities, and oxygen abundances in each of these regions are computed. We build continuum and emission-line intensity maps, as well as maps of the most relevant line ratios:/H, and H/H, which allow us to obtain spatial information on the ionization structure and mechanisms. We also derive the gas velocity field from the H and [O iii] k5007 emission lines. We find that all five galaxies are in the high end of the metallicity range of blue compact dwarfs with oxygen abundances varying from Z ' 0:3 to 1.5 Z . The objects show H iiYlike ionization in the whole field of view, except the outer regions of III Zw 102, whose large [N ii] k6584/H values suggest the presence of shocks. The five galaxies display inhomogeneous extinction patterns, and three of them have high H/H ratios, indicative of a large dust content; all of the galaxies display complex, irregular velocity fields in their inner regions.

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“…This difference may be due to asymmetric drift, i.e., to different velocity dispersions of the components studied. Indeed the velocity dispersion of ionized gas outside r > 10 ′′ exceeds 50 km/s, and such a behavior is indicative of the additional increase of chaotic motions caused by a powerful burst of star formation (Martínez-Delgado, 2007).…”

Section: Inner Diskmentioning

confidence: 99%

Warped polar ring in the Arp 212 galaxy

Моисеев

2008

Astrophys. Bull.

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Abstract. The Fabry-Perot scanning interferometer mounted on the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences is used to study the distribution and kinematics of ionized gas in the peculiar galaxy Arp 212 (NGC 7625, III Zw 102). Two kinematically distinct subsystems-the inner disk and outer emission filaments-are found within the optical radius of the galaxy. The first subsystem, at galactocentric distances r < 3.5 kpc, rotates in the plane of the stellar disk. The inner part of the ionized-gas disk (r < 1.5-2 kpc) exactly coincides with the previously known disk consisting of molecular gas. The second subsystem of ionized gas is located at galactocentric distances 2-6 kpc. This subsystem rotates in a plane tilted by a significant angle to the stellar disk. The angle of orbital inclination in the outer disk increases with galactocentric distance and reaches 50• at r ≈ 6 kpc. The ionized fraction of the gaseous disk does not show up beyond this galactocentric distance, but we believe that the HI disk continues to warp and approaches the plane that is polar with respect to the inner disk of the galaxy. Hence Arp 212 can be classified as a galaxy with a polar ring (or a polar disk). The observed kinematics of the ionized and neutral gas can be explained assuming that the distribution of gravitational potential in the galaxy is not spherically symmetric. Most probably, the polar ring have formed via accretion of gas from the dwarf satellite galaxy UGC 12549.

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Three-dimensional Spectroscopy of Blue Compact Galaxies: Diagnostic Diagrams

Cited by 30 publications

References 18 publications

Hubble Space TelescopeSpace Telescope Imaging Spectrograph Spectroscopy of the Environment in the Starburst Core of M82

Hubble Space TelescopeSpace Telescope Imaging Spectrograph Spectroscopy of the Environment in the Starburst Core of M82

Integral Field Spectroscopy of Blue Compact Dwarf Galaxies

Warped polar ring in the Arp 212 galaxy

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