Companions of Bright Barred Shapley-Ames Galaxies

García-Barreto, J. A.; Carrillo, R.; Vera-Villamizar, N.

doi:10.1086/378359

Cited by 14 publications

(17 citation statements)

References 37 publications

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“…Condon (1987) shows a 45 mJy north-south source at 1.4 GHz, 54 00 resolution. Single-dish observations at 5 and 11 GHz (Garcia-Barreto et al 1993) show that this source is steep spectrum. Hummel (1980) establish an upper limit of 10 mJy to any core emission at 1.4 GHz, while the 15 GHz, 4 00 , and 0>2 resolution observations of Nagar et al (2000) give an upper limit of 1.3 mJy to any radio emission.…”

Section: Comments On Individual Galaxiesmentioning

confidence: 85%

“…54 00 resolution, 1.4 GHz observations (Condon 1987) show a 21.3 mJy diffuse source. High-resolution observations at various frequencies (Heckman 1980;Hummel et al 1985;Garcia-Barreto et al 1993) show this object to harbor a flat-spectrum, et al (2000) give only upper limit of 1.3 mJy to any radio emission. NGC 4125.-There is no NVSS detection of this source.…”

Section: Comments On Individual Galaxiesmentioning

confidence: 95%

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The Radio Properties of Composite LINER/H ii Galaxies

Filho¹,

Barthel²,

2002

ASTROPHYS J SUPPL S

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Arcsecond-resolution VLA observations-newly obtained as well as published-of 40 nearby galaxies are discussed, completing a study of the radio properties of a magnitude-limited sample of nearby galaxies of the composite LINER/H ii type. Our results reveal an overall detection rate of at least 25% active galactic nucleus (AGN) candidates among these composite sources. The general properties of these AGN candidates, as compared to non-AGN composite sources and H ii galaxies, are discussed.

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Section: Comments On Individual Galaxiesmentioning

confidence: 85%

Section: Comments On Individual Galaxiesmentioning

confidence: 95%

The Radio Properties of Composite LINER/H ii Galaxies

Filho¹,

Barthel²,

2002

ASTROPHYS J SUPPL S

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“…An intuitive explanation for NGC 3367 optical asymmetric morphology and large bipolar synchrotron emission might be a recent merger with a small galaxy since NGC 3367 has no large optical companion closer than 500 kpc (García-Barreto et al 2003). A gas rich galaxy may be a suited candidate because the asymmetric SF distribution.…”

Section: Evidence For Recent Ngc 3367mentioning

confidence: 99%

“…NGC 3367 is located in the field of the Leo Group but it belongs to the background based on its optical velocity of v o = 2998 km s −1 and the mean velocity of the Leo I Group = 900 km s −1 (Ferguson & Sandage 1990;Stocke et al 1991;Tonry et al 2001). The closest candidate for a galaxy companion is NGC 3391 at a projected distance of ∼ 563 kpc or 18 optical diameters away (García-Barreto et al 2003) and a recent search for isolated galaxies in the local universe based on the SDSS has also confirmed that NGC 3367 is an isolated galaxy (Hernández-Toledo et al 2010). The optical appearance of NGC 3367 is dominated by a bright bar and an apparent large-scale asymmetry or lopsidedness to the southwest side.…”

Section: Introductionmentioning

confidence: 99%

The Bulgeless Seyfert/Liner Galaxy NGC 3367: Disk, Bar, Lopsidedness, and Environment

Hernández-Toledo

Cano-Díaz

Valenzuela

et al. 2011

The Astronomical Journal

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NGC 3367 is a nearby isolated active galaxy that shows a radio jet, a strong bar, and evidence of lopsidedness. We present a quantitative analysis of the stellar and gaseous structure of the galaxy disk and search for evidence of recent interaction. Our study is based on new UBVRI Hα and JHK images and on archive Hα Fabry-Perot and H i Very Large Array data. From a coupled one-dimensional/two-dimensional GALFIT bulge/bar/disk decomposition a (B/D ∼ 0.07-0.1) exponential pseudobulge is inferred in all the observed bands. A near-infrared (NIR) estimate of the bar strength Q max T (R) = 0.44 places NGC 3367 bar among the strongest ones. The asymmetry properties were studied using (1) the optical and NIR concentration-asymmetry-clumpiness indices, (2) the stellar (NIR) and gaseous (Hα, H i) A 1 Fourier mode amplitudes, and (3) the H i-integrated profile and H i mean intensity distribution.While the average stellar component shows asymmetry values close to the average found in the local universe for isolated galaxies, the young stellar component and gas values are largely decoupled showing significantly larger A 1 mode amplitudes suggesting that the gas has been recently perturbed and placing NGC 3367 in a global starburst phase. NGC 3367 is devoid of H i gas in the central regions where a significant amount of molecular CO gas exists instead. Our search for (1) faint stellar structures in the outer regions (up to μ R ∼ 26 mag arcsec −2 ), (2) (Hα) star-forming satellite galaxies, and (3) regions with different colors (stellar populations) along the disk all failed. Such an absence is interpreted by using results from recent numerical simulations to constrain either a possible tidal event with an LMC like galaxy to some dynamical times in the past or a very low mass but perhaps gas rich recent encounter. We conclude that a cold flow accretion mode (gas and small/dark galaxies) may be responsible for the nuclear activity and peculiar (young stars and gas) morphology regardless of the highly isolated environment. Black hole growth in bulgeless galaxies may be triggered by smooth mass accretion.

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“…The angular resolution of the maps in Condon's (1987) atlas was insufficient to distinguish emission from the bar, the spiral arms and the halo. Another survey of barred galaxies in radio continuum by García-Barreto et al (1993) had even lower angular resolution; neither survey included polarization. The first high-resolution References: (1) Sandage & Tammann (1981); (2) de Vaucouleurs et al (1991); (3) Fullmer & Lonsdale (1989); (4) Condon (1987).…”

Section: Introductionmentioning

confidence: 99%

Magnetic fields in barred galaxies

Beck

Shoutenkov

Ehle

et al. 2002

A&A

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Abstract. The total and polarized radio continuum emission of 20 barred galaxies was observed with the Very Large Array (VLA) at λ3, 6, 18 and 22 cm and with the Australia Telescope Compact Array (ATCA) at λ6 cm and 13 cm. Maps at 30 angular resolution are presented here. Polarized emission (and therefore a large-scale regular magnetic field) was detected in 17 galaxies. Most galaxies of our sample are similar to non-barred galaxies with respect to the radio/far-infrared flux correlation and equipartition strength of the total magnetic field. Galaxies with highly elongated bars are not always radio-bright. We discuss the correlation of radio properties with the aspect ratio of the bar and other measures of the bar strength. We introduce a new measure of the bar strength, Λ, related to the quadrupole moment of the bar's gravitational potential. The radio surface brightness I of the barred galaxies in our sample is correlated with Λ, I ∝ Λ 0.4±0.1 , and thus is highest in galaxies with a long bar where the velocity field is distorted by the bar over a large fraction of the disc. In these galaxies, the pattern of the regular field is significantly different from that in non-barred galaxies. In particular, field enhancements occur upstream of the dust lanes where the field lines are oriented at large angles to the bar's major axis. Polarized radio emission seems to be a good indicator of large-scale non-axisymmetric motions.

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Companions of Bright Barred Shapley-Ames Galaxies

Cited by 14 publications

References 37 publications

The Radio Properties of Composite LINER/H ii Galaxies

The Radio Properties of Composite LINER/H ii Galaxies

The Bulgeless Seyfert/Liner Galaxy NGC 3367: Disk, Bar, Lopsidedness, and Environment

Magnetic fields in barred galaxies

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