TY - GEN
T1 - Kpg 390
T2 - A pair of trailing spirals.
AU - Repetto, P.
AU - Rosado, M.
AU - Gabbasov, R.
AU - Fuentes-Carrera, I.
PY - 2010/6
Y1 - 2010/6
N2 - In this study we present scanning Fabry-Perot H observations of the isolated interacting galaxy pair NGC 5278/79. We derived velocity fields, various kinematic parameters and rotation curves for both galaxies. These kinematical results together with the fact that dust lanes have been detected in both galaxies, as well as the analysis of surface brightness profiles along the minor axis, allowed us to determine univocally that both components of the interacting pair are trailing spirals. We have also estimated the mass of NGC 5278 fitting its rotation curve with a disk-halo component. We have tested three different types of halo (pseudo-isothermal, Hernquist and Navarro Frenk White) and we have obtained that the rotation curve can be fitted either with a pseudo-isothermal, an Hernquist halo or a Navarro Frenk White halo component, although in the first case the amount of dark matter required is about ten times smaller than for the other two halo distributions.
AB - In this study we present scanning Fabry-Perot H observations of the isolated interacting galaxy pair NGC 5278/79. We derived velocity fields, various kinematic parameters and rotation curves for both galaxies. These kinematical results together with the fact that dust lanes have been detected in both galaxies, as well as the analysis of surface brightness profiles along the minor axis, allowed us to determine univocally that both components of the interacting pair are trailing spirals. We have also estimated the mass of NGC 5278 fitting its rotation curve with a disk-halo component. We have tested three different types of halo (pseudo-isothermal, Hernquist and Navarro Frenk White) and we have obtained that the rotation curve can be fitted either with a pseudo-isothermal, an Hernquist halo or a Navarro Frenk White halo component, although in the first case the amount of dark matter required is about ten times smaller than for the other two halo distributions.
KW - (cosmology): dark matter
KW - Astrometry
KW - Galaxies: interactions
KW - Galaxies: kinematics and dynamics
KW - Galaxies: spiral
KW - Instrumentation: interferometers
KW - Methods: data analysis
KW - Techniques: image processing
KW - Techniques: interferometric
KW - Techniques: radial velocities
UR - http://www.scopus.com/inward/record.url?scp=84882762484&partnerID=8YFLogxK
U2 - 10.1017/S1743921311017534
DO - 10.1017/S1743921311017534
M3 - Contribución a la conferencia
SN - 9780521197397
T3 - Proceedings of the International Astronomical Union
SP - 127
EP - 134
BT - Astrophysical Dynamics
A2 - Brummell, Nicholas
A2 - Brun, Sacha
A2 - Boulder, Mark
A2 - Ponty, Yannick
ER -