Bibcode
Aguerri, J. A. L.; Méndez-Abreu, J.; Falcón-Barroso, J.; Amorin, A.; Barrera-Ballesteros, J.; Cid Fernandes, R.; García-Benito, R.; García-Lorenzo, B.; González Delgado, R. M.; Husemann, B.; Kalinova, V.; Lyubenova, M.; Marino, R. A.; Márquez, I.; Mast, D.; Pérez, E.; Sánchez, S. F.; van de Ven, G.; Walcher, C. J.; Backsmann, N.; Cortijo-Ferrero, C.; Bland-Hawthorn, J.; del Olmo, A.; Iglesias-Páramo, J.; Pérez, I.; Sánchez-Blázquez, P.; Wisotzki, L.; Ziegler, B.
Bibliographical reference
Astronomy and Astrophysics, Volume 576, id.A102, 17 pp.
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4
2015
Journal
Citations
98
Refereed citations
89
Description
Context. The bar pattern speed (Ωb) is defined as the
rotational frequency of the bar, and it determines the bar dynamics.
Several methods have been proposed for measuring Ωb.
The non-parametric method proposed by Tremaine & Weinberg (1984,
ApJ, 282, L5; TW) and based on stellar kinematics is the most accurate.
This method has been applied so far to 17 galaxies, most of them SB0 and
SBa types. Aims: We have applied the TW method to a new sample of
15 strong and bright barred galaxies, spanning a wide range of
morphological types from SB0 to SBbc. Combining our analysis with
previous studies, we investigate 32 barred galaxies with their pattern
speed measured by the TW method. The resulting total sample of barred
galaxies allows us to study the dependence of Ωb on
galaxy properties, such as the Hubble type. Methods: We measured
Ωb using the TW method on the stellar velocity maps
provided by the integral-field spectroscopy data from the CALIFA survey.
Integral-field data solve the problems that long-slit data present when
applying the TW method, resulting in the determination of more accurate
Ωb. In addition, we have also derived the ratio ℛ
of the corotation radius to the bar length of the galaxies. According to
this parameter, bars can be classified as fast (ℛ < 1.4) and
slow (ℛ > 1.4). Results: For all the galaxies, ℛ
is compatible within the errors with fast bars. We cannot rule out (at
95% level) the fast bar solution for any galaxy. We have not observed
any significant trend between ℛ and the galaxy morphological type.
Conclusions: Our results indicate that independent of the Hubble
type, bars have been formed and then evolve as fast rotators. This
observational result will constrain the scenarios of formation and
evolution of bars proposed by numerical simulations.
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