On the Origin of the Southwest H alpha Regions of the Spiral Galaxy NGC 3367

García-Barreto, J. A.; Franco, J.; Carrillo, R.

doi:10.1086/177766

Cited by 12 publications

(14 citation statements)

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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%

“…Figure 5 shows a zoomed image of the central CO concentration from the high-resolution image. The unresolved peak emission is at (J2000) García-Barreto et al 1996a, 1996b. Contours are at À3, 3, 4, 5, 6, 7, 8, 9, 10, 15, and 20 ; 6 mJy beam À1 .…”

Section: The Nuclear Regg Ionmentioning

confidence: 99%

“…CO is optically thick, and the conversion factor is roughly proportional to hn H 2 i 1=2 =T ex (Downes et al 1993; Scoville et al 1997). To some extent, the density and temperature dependences are likely to offset each other, since where the gas density is high, there will be elevated star (García-Barreto et al 1996a, 1996b. 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: Molecular Gas Massmentioning

confidence: 99%

“…The optical disk of NGC 3367 is peculiar (García-Barreto et al 1996a): (1) there is a bright optical structure forming a semicircle at a radius of approximately 10-11 kpc southwest of the center-this structure is bright in the optical red continuum as well as in narrow-line H +[N ii] images; (2) it has spiral arms apparently joining this semicircular structure (to the northwest) at an angle larger than 45 ; (3) the northwest spiral arm seems to consist of two parallel structures (both in red images and in H+[N ii] images); (4) the northeast end of the stellar bar exhibits very large velocity dispersions in H (García-Barreto & Rosado 2001). Our previous analysis of the optical morphology suggested a ringlike density wave propagating outward, possibly the result of a collision of NGC 3367 with a smaller galaxy (García-Barreto et al 1996a). The perturber might have traveled approximately perpendicular to the disk of NGC 3367 in an off-center collision.…”

Section: Gas Flow To the Nucleusmentioning

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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“…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%

Section: The Nuclear Regg Ionmentioning

confidence: 99%

Section: The Nuclear Regg Ionmentioning

confidence: 99%

Section: Molecular Gas Massmentioning

confidence: 99%

Section: Gas Flow To the Nucleusmentioning

confidence: 99%

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CO in the Bipolar Radio Continuum Galaxy NGC 3367

et al. 2005

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Hα emission line morphologies in Markarian starburst galaxies

Chitre

Joshi

2001

J Astrophys Astron

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We present broad band R and narrow band Hα emission line images of a sample of optically selected starburst galaxies from the Markarian lists. The emission line morphology is studied and global properties like luminosities, equivalent widths and star formation rates are derived. The radial distribution of Hα flux and the EW are determined using concentric aperture photometry on the emission line and the continuum images. Hα flux is generally found to peak in the nuclear region and fall off outwards. The EW is found to peak off-center in most of the cases implying that though the intensity of emission is maximum at the nucleus, the star formation activity relative to the underlying continuum often peaks away from the center in Markarian starburst galaxies.

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Elusive active galactic nuclei

Maiolino

Comastri

Gilli

et al. 2003

Monthly Notices RAS

148

157

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A fraction of active galactic nuclei do not show the classical Seyfert‐type signatures in their optical spectra, i.e. they are optically ‘elusive’. X‐ray observations are an optimal tool to identify this class of objects. We combine new Chandra observations with archival X‐ray data in order to obtain a first estimate of the fraction of elusive active galactic nuclei (AGN) in local galaxies and to constrain their nature. Our results suggest that elusive AGN have a local density comparable to or even higher than optically classified Seyfert nuclei. Most elusive AGN are heavily absorbed in the X‐rays, with gas column densities exceeding 1024 cm−2, suggesting that their peculiar nature is associated with obscuration. It is likely that in elusive AGN the nuclear UV source is completely embedded and the ionizing photons cannot escape, which prevents the formation of a classical narrow‐line region. Elusive AGN may contribute significantly to the 30‐keV bump of the X‐ray background.

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On the Origin of the Southwest H alpha Regions of the Spiral Galaxy NGC 3367

Cited by 12 publications

References 0 publications

CO in the Bipolar Radio Continuum Galaxy NGC 3367

CO in the Bipolar Radio Continuum Galaxy NGC 3367

Hα emission line morphologies in Markarian starburst galaxies

Elusive active galactic nuclei

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