NGC 3081: Surface Photometry and Kinematics of a Classic Resonance Ring Barred Galaxy

Buta, Ronald J.; Purcell, Guy B.

doi:10.1086/300225

Cited by 55 publications

(57 citation statements)

References 43 publications

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“…of 70¡È80¡ and a^70A (12 kpc) major axis, while the nuclear ring has a P.A. of^120¡ and a^12A(2 kpc) major axis (see also Buta & Purcell 1998). Inside the nuclear ring, our continuum images (Fig.…”

Section: Data Reductionmentioning

confidence: 74%

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Hubble Space Telescope WFPC2 Imaging of a Sample of Early‐Type Seyfert Galaxies

Ferruit

Wilson

Mulchaey

2000

ASTROPHYS J SUPPL S

114

183

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We have deÐned a complete sample comprising all 14 Seyfert galaxies in early-type (E, S0, Sa) host galaxies with apparent magnitude mag and recessional velocity cz \ 3000 km s~1. This paper m v \ 14.5 presents Hubble Space T elescope ( We Ðnd that all the galaxies A ). in our sample display prominent nuclear dust features. In some objects, the dust strongly inÑuences the morphology of the starlight and ionized gas. Despite the restriction to early-type galaxies, Ðve (possibly six) galaxies of the 14 have a signiÐcant (if not dominant) part of their [N II] ] Ha emission originating in H II regions. This result supports the notion that the Seyfert phenomenon tends to be associated with ongoing star formation.

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Section: Data Reductionmentioning

confidence: 74%

“…5.5. NGC 3081ÈSeyfert 2 NGC 3081 is a complex galaxy with multiple rings (see Buta & Purcell 1998 and references therein) hosting a Seyfert 2 nucleus (see, e.g., Durret & Bergeron 1986). In our F547M image (Fig.…”

Section: Data Reductionmentioning

confidence: 99%

Hubble Space Telescope WFPC2 Imaging of a Sample of Early‐Type Seyfert Galaxies

Ferruit

Wilson

Mulchaey

2000

ASTROPHYS J SUPPL S

114

183

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“…This is not the case for the nuclear ring, whose intrinsic major axis is oriented 71 to the bar axis (Buta & Purcell 1998). Within the context of our analytic model, this implies that the nuclear ring has a lot of damping.…”

Section: Lindblad Resonancesmentioning

confidence: 77%

“…The inner ring is thought to occur inside CR, where ( 0 À p ) > 0 for a typical constant circular velocity rotation curve (e.g., Buta & Purcell 1998). The epicyclic frequency is defined as usual (e.g., BT eq.…”

Section: Damped Forced Motionmentioning

confidence: 99%

“…In Paper I (Buta et al 2004a), we presented an analysis of Hubble Space Telescope (HST ) UBVI images of the inner ring of NGC 3081, a classic early-type spiral with one of the most distinctive multiring morphologies among the general galaxy population. NGC 3081 is an especially good candidate for studies of star formation in rings because of several unique features (Buta & Purcell 1998). The galaxy has four well-defined, nested, and virtually closed ring features ( Fig.…”

Section: Introductionmentioning

confidence: 99%

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The Inner Resonance Ring of NGC 3081. II. Star Formation, Bar Strength, Disk Surface Mass Density, and Mass-to-Light Ratio

Byrd¹,

Freeman²,

Buta³

2006

Astron J

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We complement our Hubble Space Telescope (HST ) observations of the inner ring of the galaxy NGC 3081 using an analytical approach and n-body simulations. We find that a gas cloud inner (r) ring forms under a rotating bar perturbation with very strong azimuthal cloud crowding where the ring crosses the bar major axis. Thus, star formation results near to and ''downstream'' of the major axis. From the dust distribution and radial velocities, the disk rotates counterclockwise (CCW ) on the sky like the bar pattern speed. We explain the observed CCW color asymmetry crossing the major axis as due to the increasing age of stellar associations inside the r ring major axis. These move faster than the pattern speed. The exterior point of the r ring at the bar major axis has an orbital rate equal to the pattern speed. We show how the perturbation strength can be estimated from the ring shapes and relative spacing over the inner through outer ring regions. The bar strength (maximum tangential/radial force) appears to be constant from 6 to 15 kpc. We derive how the perturbation, the fractional long wavelength m ¼ 2 intensity, and the rotation curve can be used to calculate the disk surface mass density versus radius. The disk surface density at 7 kpc is 13 M pc À2 rising to 19 at 13 kpc. The latter is insufficient by a factor of seven to generate the observed rotation curve, implying halo domination. The surface density may have been reduced at 7 kpc due to inner ring gas cloud scattering. The surface density plus the observed surface brightness gives a disk mass-to-light (M/L) ratio which increases from 7 kpc through 13 kpc, contradicting the usual assumption in bar strength calculations. The simulation ring lifetime of several billion years is consistent with our $400 Myr HST estimates. With a sufficiently high gas cloud surface mass density, our simulations form gas cloud ''associations'' near the ends of the bar as observed. Too high a density destroys the ring.

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The Classification of Galaxies

Buta

2021

Galaxies

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NGC 3081: Surface Photometry and Kinematics of a Classic Resonance Ring Barred Galaxy

Cited by 55 publications

References 43 publications

Hubble Space Telescope WFPC2 Imaging of a Sample of Early‐Type Seyfert Galaxies

Hubble Space Telescope WFPC2 Imaging of a Sample of Early‐Type Seyfert Galaxies

The Inner Resonance Ring of NGC 3081. II. Star Formation, Bar Strength, Disk Surface Mass Density, and Mass-to-Light Ratio

The Classification of Galaxies

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