2015A&A...583A..55O


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST08:14:54

2015A&A...583A..55O - Astronomy and Astrophysics, volume 583A, 55-55 (2015/11-1)

Kinematics of Haro11: The miniature Antennae.

OESTLIN G., MARQUART T., CUMMING R.J., FATHI K., BERGVALL N., ADAMO A., AMRAM P. and HAYES M.

Abstract (from CDS):

Luminous blue compact galaxies are among the most active galaxies in the local Universe in terms of their star formation rate per unit mass. They are rare at the current cosmic epoch, but were more abundant in the past and may be seen as the local analogues of higher red shift Lyman break galaxies. Studies of their kinematics is key to understanding what triggers their unusually active star formation. In this work, we investigate the kinematics of stars and ionised gas in Haro11, one of the most luminous blue compact galaxies in the local Universe. Previous works have indicated that many of these galaxies may be triggered by galaxy mergers. We have employed Fabry-Perot interferometry, long-slit spectroscopy, and integral field unit (IFU) spectroscopy to explore the kinematics of Haro11. We target the near-infrared calcium triplet, and use cross-correlation and penalised pixel fitting techniques to derive the stellar velocity field and velocity dispersion. We analyse ionised gas through emission lines from hydrogen, [Oiii], and [Siii]. When spectral resolution and signal to noise allows, we investigate the line profile in detail and identify multiple velocity components when present. The spectra reveal a complex velocity field whose components, both stellar and gaseous, we attempt to disentangle. We find that to first order, the velocity field and velocity dispersions derived from stars and ionised gas agree. Hence the complexities reveal real dynamical disturbances providing further evidence for a merger in Haro11. Through decomposition of emission lines, we find evidence for kinematically distinct components, for instance, a tidal arm. The ionised gas velocity field can be traced to large galactocentric radii, and shows significant velocity dispersion even far out in the halo. If interpreted as virial motions, this indicates that Haro11 may have a mass of ∼1011M. Haro11 shows many resemblances with the famous Antennae galaxies both morphologically and kinematically, but it is much denser, which is the likely explanation for the higher star formation efficiency in Haro11.

Abstract Copyright:

Journal keyword(s): galaxies: kinematics and dynamics - galaxies: interactions - galaxies: evolution - galaxies: individual: Haro 11 - galaxies: starburst

Simbad objects: 6

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Number of rows : 6

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 ESO 350-38 AGN 00 36 52.489 -33 33 17.23   14.31 14.41 13.49   ~ 290 0
2 ESO 495-21 bCG 08 36 15.190 -26 24 33.66 12.04 11.93 11.45 11.09 12.3 ~ 501 3
3 [ZFR2002] 2 HXB 12 01 48.83 -18 54 03.6           ~ 5 0
4 NAME Antennae IG 12 01 53.170 -18 52 37.92           ~ 1556 0
5 CD-44 12736 PM* 18 36 25.9487430436 -44 18 36.919462094   10.83 10.22     G0 193 0
6 CD-30 17706 WD* 20 10 56.8485174654 -30 13 06.629141494 11.654 12.286 12.242 12.311 12.381 DA3.1 219 0

    Equat.    Gal    SGal    Ecl

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2020.07.13-08:14:54

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