The orientation parameters and rotation curves of 15 spiral galaxies

Fridman, A. M.; Afanasiev, V. L.; Додонов, С. Н.; Khoruzhii, O. V.; Моисеев, А. В.; Сильченко, О. К.; Засов, А. В.

doi:10.1051/0004-6361:200400087

Cited by 32 publications

(19 citation statements)

References 54 publications

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“…from circular rotation. This is discussed in Fridman et al (2005) together with different possible reasons for small scale anomalies (e.g. nuclear activity, gas outflow from a star formation burst region, a shock excitation mechanism, etc.).…”

Section: Discussionmentioning

confidence: 99%

Internal kinematics of spiral galaxies in distant clusters

Kutdemir¹,

Ziegler

Peletier³

et al. 2008

A&A

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Context. We continue our investigation on how the cluster environment affects the evolution of galaxies. Aims. By examining both galaxy structure and internal kinematics of cluster galaxies at lookback times of ∼5 Gyr we study the nature and impact of possible interactions at the peak epoch of cluster assembly. Methods. Going beyond our previous measurements of two-dimensional rotation curves, we here observe the whole velocity field of the galaxies of the sample. We achieve a complete coverage and optimal spatial sampling of galaxy sizes by placing three adjacent and parallel FORS2 MXU (Mask eXchange Unit) slits onto each object yielding simultaneously several emission and absorption lines. We reconstruct the gas velocity field and decompose it into circular rotation and irregular motions using a harmonic decomposition method called kinemetry. To measure the irregularity in the gas kinematics, we define 3 parameters: σ PA (the standard deviation of the kinematic position angle within a galaxy), ∆φ (the average misalignment between kinematic and photometric position angles) and k 3,5 (squared sum of the higher order Fourier terms).Results. We present the analysis of the velocity fields and morphology of 22 distant galaxies in the MS 0451.6−0305 field with 11 members at z = 0.54 and a local sample from SINGS. Using local, undistorted galaxies the three parameters σ PA , ∆φ and k 3,5 can be used to establish the regularity of the gas velocity fields. Among the galaxies for which we could measure these parameters, we find both field ones (4 of 8) and cluster members (3 of 4), which have a velocity field that we consider both irregular and asymmetric. We show that these fractions are underestimates of the total number of objects with irregular velocity fields. The values of the irregularity parameters for cluster galaxies are not very different from those of the field galaxies, implying that there are isolated field galaxies that are as distorted as the cluster members. None of the deviations in our small sample correlate with photometric/structural properties like luminosity or disk scale length in a significant way. Conclusions. We have demonstrated that our 3D-spectroscopic method successfully maps the velocity field of distant galaxies. Together with a structural analysis the importance and efficiency of cluster specific interactions can be assessed quantitatively.

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Section: Discussionmentioning

confidence: 99%

Internal kinematics of spiral galaxies in distant clusters

Kutdemir¹,

Ziegler

Peletier³

et al. 2008

A&A

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“…The degree of symmetry of a velocity field may also be affected by the presence of dust lanes, spiral arms, bars, warps, outflows/inflows, shocks or nuclear activity, minor mergers or even interactions with difuse objects (see, e.g., Fridman et al 2005;Fathi et al 2005;Wong et al 2004;López-Sánchez 2010). Their kinematics imprints could range from ∼10 km s −1 (see Wong et al 2004, for radial inflows) to a few hundred of km s −1 (for outflows from an AGN, see, e.g., Arribas et al 1996).…”

Section: Kinematic Internal Misalignmentmentioning

confidence: 99%

Ionized gas kinematics of galaxies in the CALIFA survey

García-Lorenzo

Márquez

Barrera-Ballesteros

et al. 2014

A&A

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Context. Ionized gas kinematics provide important clues to the dynamical structure of galaxies and hold constraints to the processes driving their evolution. Aims. The motivation of this work is to provide an overall characterization of the kinematic behavior of the ionized gas of the galaxies included in the Calar Alto Legacy Integral field Area (CALIFA), offering kinematic clues to potential users of the CALIFA survey for including kinematical criteria in their selection of targets for specific studies. From the first 200 galaxies observed by CALIFA survey in its two configurations, we present the two-dimensional kinematic view of the 177 galaxies satisfaying a gas content/detection threshold. Methods. After removing the stellar contribution, we used the cross-correlation technique to obtain the radial velocity of the dominant gaseous Results. At the velocity resolution of CALIFA, most objects in the sample show regular velocity fields, although the ionized-gas kinematics are rarely consistent with simple coplanar circular motions. Thirty-five percent of the objects present evidence of a displacement between the photometric and kinematic centers larger than the original spaxel radii. Only 17% of the objects in the sample exhibit kinematic lopsidedness when comparing receding and approaching sides of the velocity fields, but most of them are interacting galaxies exhibiting nuclear activity (AGN or LINER). Early-type (E+S0) galaxies in the sample present clear photometric-kinematic misaligments. There is evidence of asymmetries in the emission line profiles in 117 out of the 177 analyzed galaxies, suggesting the presence of kinematically distinct gaseous components located at different distances from the optical nucleus. The kinematic decoupling between the dominant and secondary component/s suggested by the observed asymmetries in the profiles can be characterized by a limited set of parameters. Conclusions. This work constitutes the first determination of the ionized gas kinematics of the galaxies observed in the CALIFA survey. The derived velocity fields, the reported kinematic distortions/peculiarities and the identification of the presence of several gaseous components in different regions of the objects might be used as additional criteria for selecting galaxies for specific studies.

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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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The orientation parameters and rotation curves of 15 spiral galaxies

Cited by 32 publications

References 54 publications

Internal kinematics of spiral galaxies in distant clusters

Internal kinematics of spiral galaxies in distant clusters

Ionized gas kinematics of galaxies in the CALIFA survey

Orbital Dependence of Galaxy Properties in Satellite Systems of Galaxies

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