Ionized Gas in Bright Barred Spiral Galaxies: H<i>α</i> Images

García-Barreto, J. A.; Carrillo, R.; Venegas, S.; Escalante-Ramı́rez, Boris

doi:10.1017/s0252921100049447

Cited by 24 publications

(74 citation statements)

References 8 publications

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“…In our sample, we see that the strongest bars (Q b,NGC1073 =0.63 and Q b,NGC5112 =0.62) show Hα emission, but further study is needed to see if this emission is located in the regions of high shocks/shear. (ii) García-Barreto et al (1996) found that the barred galaxies with Hubble types SBa or earlier in their sample did not show Hα emission, probably due to the low gas content available for inflow (which is not the case, for example, for NGC 4151) so the morphological type is not in principle the only reason. (iii) Martin & Friedli (1997) also found that the two highest SFRs correspond to the galaxies which present the strongest signs of recent interaction or merging (NGC 4731 and NGC 7479).…”

Section: Bar-induced Non-circular Motionsmentioning

confidence: 94%

Hα kinematics of S4G spiral galaxies – II. Data description and non-circular motions

Erroz-Ferrer¹,

Knapen²,

Leaman³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present a kinematical study of 29 spiral galaxies included in the Spitzer Survey of Stellar Structure in Galaxies, using Hα Fabry-Perot data obtained with the Galaxy Hα Fabry-Perot System instrument at the William Herschel Telescope in La Palma, complemented with images in the R band and in Hα. The primary goal is to study the evolution and properties of the main structural components of galaxies through the kinematical analysis of the FP data, complemented with studies of morphology, star formation and mass distribution. In this paper we describe how the FP data have been obtained, processed and analysed. We present the resulting moment maps, rotation curves, velocity model maps and residual maps. Images are available in FITS format through the NASA/IPAC Extragalactic Database and the Centre de Données Stellaires. With these data products we study the non-circular motions, in particular those found along the bars and spiral arms. The data indicate that the amplitude of the non-circular motions created by the bar does not correlate with the bar strength indicators. The amplitude of those non-circular motions in the spiral arms does not correlate with either arm class or star formation rate along the spiral arms. This implies that the presence and the magnitude of the streaming motions in the arms is a local phenomenon.

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Section: Bar-induced Non-circular Motionsmentioning

confidence: 94%

Hα kinematics of S4G spiral galaxies – II. Data description and non-circular motions

Erroz-Ferrer¹,

Knapen²,

Leaman³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…6) García-Barreto et al 1996a, 1996b. CO contours are at À3, 3, 5, 7, 9, 12, 14, 16, 18, 20, 22, 24, 26, 28, 30, 35, 40, 45, 50, 60, and 70 ; 150 mJy km s À1 .…”

Section: Gas Kinematics and Dynamical Massmentioning

confidence: 99%

“…Figures 3 and 4 show the total CO line flux integrated over 300 km s À1 , superposed on the H +[N ii] (continuumsubtracted) and I-band images (García- Barreto et al 1996aBarreto et al , 1996b. The strongest CO emission (65 ) arises at the compact nucleus and from a circumnuclear structure (see below).…”

Section: The Nuclear Regg Ionmentioning

confidence: 99%

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CO in the Bipolar Radio Continuum Galaxy NGC 3367

et al. 2005

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CO(1-0) emission has been imaged at 2 00 resolution in the central 10 kpc of the barred spiral galaxy NGC 3367. This galaxy has bipolar synchrotron lobes out to a radius of 6 kpc, straddling the compact nucleus. The peak molecular emission is in a source of radius 2 00 (425 pc) centered on the galaxy nucleus. The molecular gas mass is $3 ; 10 8 M in this peak and $5:9 ; 10 8 M within a radius of 4B5 (950 pc). The very large gas masses in the central source imply extinctions sufficiently high to completely obscure optical emission lines (e.g., broad-line region) associated with the nuclear radio source. The observed Balmer lines probably originate in the narrow-line region a few hundred parsecs from the nucleus. The CO emission in the central region is elongated northeastsouthwest, very similar to the position angle of the large-scale synchrotron lobes. This elongation is likely due to the nonaxisymmetric gravitational potential of the stellar bar. We infer that the northeast radio continuum lobe is on the far side of the galaxy and the southwest lobe is on the near side. The central mass of molecular gas is of sufficient mass to power the active galactic nucleus accretion luminosity for over 10 8 yr at 3 M yr À1 .

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“…Ryder & Dopita (1994) studied the relative scale lengths of Hα, V-and I-band emission from 34 S0-Sm galaxies, finding the line emission to have larger scale lengths than those of the continuum emission. García-Barreto et al (1996) investigated Hα imaging of 52 barred spiral galaxies, finding nuclear rings in 10, and emission indicating SF along the bar in 18. Dale et al (2001) analysed Hα extents of galaxies normalised by their I-band sizes, finding no strong type dependences; similar results for Hα to R-band scalelength ratios were found by Koopmann & Kenney (2004) and Koopmann et al (2006).…”

Section: Introductionmentioning

confidence: 99%

The Hαgalaxy survey

James

Bretherton

Knapen³

2009

A&A

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Aims. We analyse the current build-up of stellar mass within the disks and bulges of nearby galaxies through a comparison of the spatial distributions of forming and old stellar populations. Methods. Hα and R-band imaging are used to determine the distributions of young and old stellar populations in 313 S0a-Im field galaxies out to ∼40 Mpc. Concentration indices and mean normalised light profiles are calculated as a function of galaxy type and bar classification.Results. The mean profiles and concentration indices show a strong and smooth dependence on galaxy type. Apart from a central deficit due to bulge/bar light in some galaxy types, mean Hα and R-band profiles are very similar. Mean profiles within a given type are remarkably constant even given wide ranges in galaxy luminosity and size. SBc, SBbc, and particularly SBb galaxies have profiles that are markedly different from those of unbarred galaxies. The Hα emission from individual SBb galaxies is studied in detail; virtually all show resolved central components and concentrations of star formation at or just outside the bar-end radius. Conclusions. Galaxy type is an excellent predictor of R-band light profile. In field galaxies, star formation has the same radial distribution as R-band light, i.e. stellar mass is building at approximately constant morphology, with no strong evidence for outer truncation or inside-out disk formation. Bars have a strong impact on the radial distribution of star formation, particularly in SBb galaxies.

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Ionized Gas in Bright Barred Spiral Galaxies: Hα Images

Cited by 24 publications

References 8 publications

Hα kinematics of S4G spiral galaxies – II. Data description and non-circular motions

Hα kinematics of S4G spiral galaxies – II. Data description and non-circular motions

CO in the Bipolar Radio Continuum Galaxy NGC 3367

The Hαgalaxy survey

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