2015A&A...576A.102A


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.06CEST23:38:03

2015A&A...576A.102A - Astronomy and Astrophysics, volume 576A, 102-102 (2015/4-1)

Bar pattern speeds in CALIFA galaxies. I. Fast bars across the Hubble sequence.

AGUERRI J.A.L., MENDEZ-ABREU J., FALCON-BARROSO J., AMORIN A., BARRERA-BALLESTEROS J., CID FERNANDES R., GARCIA-BENITO R., GARCIA-LORENZO B., GONZALEZ DELGADO R.M., HUSEMANN B., KALINOVA V., LYUBENOVA M., MARINO R.A., MARQUEZ I., MAST D., PEREZ E., SANCHEZ S.F., VAN DE VEN G., WALCHER C.J., BACKSMANN N., CORTIJO-FERRERO C., BLAND-HAWTHORN J., DEL OLMO A., IGLESIAS-PARAMO J., PEREZ I., SANCHEZ-BLAZQUEZ P., WISOTZKI L. and ZIEGLER B.

Abstract (from CDS):

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 (1984ApJ...282L...5T; 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. 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. 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). 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. 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.

Abstract Copyright:

Journal keyword(s): galaxies: kinematics and dynamics - galaxies: structure - galaxies: photometry - galaxies: evolution - galaxies: formation

Simbad objects: 18

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Number of rows : 18

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 36 LIN 00 11 22.2986137597 +06 23 21.626914171   14.5       ~ 71 0
2 NGC 1645 LIN 04 44 06.3955225941 -05 27 56.423998281   14   12.57   ~ 48 0
3 UGC 3253 G 05 19 41.625 +84 03 09.10   13.1       ~ 56 0
4 NGC 3300 LIN 10 36 38.434 +14 10 17.55   13.4       ~ 89 0
5 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5824 0
6 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4208 2
7 NGC 5205 LIN 13 30 03.691 +62 30 41.50   13.5       ~ 93 0
8 NGC 5378 LIN 13 56 51.0211624310 +37 47 50.045919156   13.8       ~ 88 0
9 NGC 5406 LIN 14 00 20.1216280902 +38 54 55.505973822   13.1       ~ 98 0
10 NGC 5947 AGN 15 30 36.5917232336 +42 43 01.769106580   14.8       ~ 59 0
11 NGC 6497 G 17 51 17.9720724479 +59 28 15.131465602   14.3       ~ 44 0
12 NGC 6941 G 20 36 23.4741685623 -04 37 07.443162713   13.3   13.3 12.9 ~ 61 3
13 NGC 6945 GiG 20 39 00.6020254761 -04 58 21.157712826   13.5       ~ 32 1
14 NGC 6947 G 20 41 15.0993514949 -32 29 11.260234679   14.84       ~ 27 0
15 NGC 7321 LIN 22 36 28.0163538572 +21 37 18.376079359   15.4       ~ 80 0
16 UGC 12185 LIN 22 47 25.063 +31 22 24.77   14.8       ~ 50 0
17 NGC 7563 LIN 23 15 55.950 +13 11 46.63 14.48 13.87 12.81     ~ 60 1
18 NGC 7591 SyG 23 18 16.2683208567 +06 35 09.111064142   13.8       ~ 222 0

    Equat.    Gal    SGal    Ecl

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2020.07.06-23:38:03

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