Nuclear Rotation Curves of Galaxies in the Co-Line Emission

Sofue, Yoshiaki; Tutui, Y.; Honma, Mareki; Tomita, Akihiko

doi:10.1086/118657

Cited by 39 publications

(57 citation statements)

References 16 publications

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“…We supplemented our sample by adding host galaxies whose rotation sense was determined from the spectroscopic observations in the literature (Rubin et al 1982(Rubin et al , 1985(Rubin et al , 1999Broeils & van Woerden 1994;Han et al 1995;Taylor et al 1995;Rhee & van Albada 1996;Zaritsky et al 1997;Sofue 1997;Sofue et al 1997Sofue et al , 1998Sofue et al , 2003Héraudeau & Simien 1998;Héraudeau et al 1999;Vega Beltrán et al 2001;Garrido et al 2002Garrido et al , 2003Garrido et al , 2004Garrido et al , 2005Vogt et al 2004;Coccato et al 2004;Fridman et al 2005;Hernandez et al 2005;Noordermeer et al 2005;Chemin et al 2006;Falcón-Barroso et al 2006;Daigle et al 2006;Ganda et al 2006;Azzaro et al 2006;Herbert-Fort et al 2008;Epinat et al 2008aEpinat et al , 2008bSwaters et al 2009). We compiled 390 satellites associated with 116 hosts.…”

Section: Spin Direction Of Host Galaxiesmentioning

confidence: 99%

Orbital Dependence of Galaxy Properties in Satellite Systems of Galaxies

Hwang

Park

2010

ApJ

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We study the dependence of satellite galaxy properties on the distance to the host galaxy and the orbital motion (prograde and retrograde orbits) using the Sloan Digital Sky Survey (SDSS) data. From SDSS Data Release 7, we find 3515 isolated satellite systems of galaxies at z < 0.03 that contain 8904 satellite galaxies. Using this sample, we construct a catalog of 635 satellites associated with 215 host galaxies whose spin directions are determined by our inspection of the SDSS color images and/or by spectroscopic observations in the literature. We divide satellite galaxies into prograde and retrograde orbit subsamples depending on their orbital motion with respect to the spin direction of the host. We find that the number of galaxies in prograde orbit is nearly equal to that of retrograde orbit galaxies: the fraction of satellites in prograde orbit is 50% ± 2%. The velocity distribution of satellites with respect to their hosts is found to be almost symmetric: the median bulk rotation of satellites is −1 ± 8 km s −1 . It is found that the radial distribution of early-type satellites in prograde orbit is strongly concentrated toward the host while that of retrograde ones shows much less concentration. We also find the orbital speed of late-type satellites in prograde orbit increases as the projected distance to the host (R) decreases while the speed decreases for those in retrograde orbit. At R less than 0.1 times the host virial radius (R < 0.1r vir,host ), the orbital speed decreases in both prograde and retrograde orbit cases. Prograde satellites are on average fainter than retrograde satellites for both early and late morphological types. The u − r color becomes redder as R decreases for both prograde and retrograde orbit late-type satellites. The differences between prograde and retrograde orbit satellite galaxies may be attributed to their different origin or the different strength of physical processes that they have experienced through hydrodynamic interactions with their host galaxies.

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Section: Spin Direction Of Host Galaxiesmentioning

confidence: 99%

Orbital Dependence of Galaxy Properties in Satellite Systems of Galaxies

Hwang

Park

2010

ApJ

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“…In the derivation of the radial distance, we neglected the small inclination ( ; Sofue et al 1997), i p 18Њ since the value of the position angle is not well constrained and the effect on the result is very small. Figure 2 shows a remarkably tight dependence of the FIR/UV ratio on radius, with a monotonic decrease from values approaching 4 in the nuclear region to values approaching zero in the outermost regions.…”

Section: The Radial Dependence Of the Fir/uv Ratiomentioning

confidence: 99%

A Comparative Study of the Spatial Distribution of Ultraviolet and Far-Infrared Fluxes from M101

Popescu¹,

Tuffs²,

Madore³

et al. 2005

ApJ

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The total ultraviolet (UV) flux (from 1412 to 2718 ) of M101 is compared on a pixel-to-pixel basis with A the total far-infrared (FIR) flux (from 60 to 170 mm) using the maps of the galaxy taken by the Galaxy Evolution Explorer (GALEX) in the near-UV and far-UV and by the Infrared Space Observatory (ISO) at 60, 100, and 170 mm. The main result of this investigation is the discovery of a tight dependence of the FIR/UV ratio on radius, with values monotonically decreasing from ∼4 in the nuclear region to nearly zero toward the edge of the optical disk. Although the tightness of this dependence is in part attributable to resolution effects, the result is consistent with the presence of a large-scale distribution of diffuse dust having a face-on optical depth that decreases with radius and that dominates over the more localized variations in opacity between the arm and interarm regions. We also find a trend for the FIR/UV ratio of taking on higher values in the regions of diffuse interarm emission than in the spiral-arm regions, at a given radius. This is interpreted quantitatively in terms of the escape probability of UV photons from spiral arms and their subsequent scattering in the interarm regions, and in terms of the larger relative contribution of optical photons to the heating of the dust in the interarm regions.

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“…We have thus used high-resolution CO line data to obtain well-sampled inner rotation curves for nearby galaxies (Sofue 1996(Sofue , 1997Sofue et al 1997. Recent CCD Ha line spectroscopy has also made available to us accurate rotation curves for the inner regions, as a result of the large dynamic range and the more precise subtraction of bulge continuum light for digital images, in so far as the extinction is not very large ; the optical positionvelocity (PV) diagrams obtained often show high-velocity 1 Institute of Astronomy, University of Tokyo, Mitaka, Tokyo 181-8588, Japan.…”

Section: Introductionmentioning

confidence: 99%

Central Rotation Curves of Spiral Galaxies

Sofue

Tutui

Honma

et al. 1999

ApJ

236

251

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We present high-resolution central-to-outer rotation curves for Sb, SBb, Sc, and SBc galaxies. We discuss their general characteristics, particularly their central behavior, as well as dependencies on morphological types, activity, and peculiarity. The rotation curves generally show a steep nuclear rise and high-velocity central rotation, followed by a broad maximum in the disk and then a Ñat rotation due to the massive halo. Since the central high velocity and steep rise are common to all massive galaxies, they cannot be due to noncircular motions. Disk rotation curves of barred galaxies show larger dispersion than those of normal galaxies, probably because of noncircular motions. Interacting galaxies often show perturbed outer rotation curves, while their central rotation shows no particular peculiarity. In addition, central activities, such as starbursts and active galactic nuclei, appear to show no particular correlation with the property of rotation curves. This would suggest that the central activities are triggered by a more local e †ect than the global dynamical property.

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Nuclear Rotation Curves of Galaxies in the Co-Line Emission

Cited by 39 publications

References 16 publications

Orbital Dependence of Galaxy Properties in Satellite Systems of Galaxies

Orbital Dependence of Galaxy Properties in Satellite Systems of Galaxies

A Comparative Study of the Spatial Distribution of Ultraviolet and Far-Infrared Fluxes from M101

Central Rotation Curves of Spiral Galaxies

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