TY - JOUR

T1 - Polar-ring galaxies: the SDSS view on the symbiotic galaxies

AU - Reshetnikov, V.

AU - Combes, F.

PY - 2015

Y1 - 2015

N2 - Polar-ring galaxies (PRGs) are multispin systems, showing star formation in a blue latetype component, perpendicular to a red early-type one, revealing how galaxy formation can sometimes occur in successive steps. We perform two-dimensional decomposition in the g, r, i bandpasses of 50 PRGs from the Sloan Digital Sky Survey. Each object was fit with a S´ersic host galaxy and a S´ersic ring. Our general results are: (i) the central (host) galaxies of the PRGs are non-dwarf sub-L∗ galaxies with colours typical for early-type galaxies. (ii) Polar structures in our sample are, on average, fainter and bluer than their host galaxies. (iii) In most galaxies, the stellarmassM∗ of the polar component is not negligible in comparison with that of the host. (iv) The distributions of the host galaxies on the size – luminosity and Kormendy diagrams are shifted by ∼1 mag to fainter magnitudes in comparison with E/S0 galaxies. It means that the PRGs hosts are more similar to quenched discs than to ordinary early-type galaxie

AB - Polar-ring galaxies (PRGs) are multispin systems, showing star formation in a blue latetype component, perpendicular to a red early-type one, revealing how galaxy formation can sometimes occur in successive steps. We perform two-dimensional decomposition in the g, r, i bandpasses of 50 PRGs from the Sloan Digital Sky Survey. Each object was fit with a S´ersic host galaxy and a S´ersic ring. Our general results are: (i) the central (host) galaxies of the PRGs are non-dwarf sub-L∗ galaxies with colours typical for early-type galaxies. (ii) Polar structures in our sample are, on average, fainter and bluer than their host galaxies. (iii) In most galaxies, the stellarmassM∗ of the polar component is not negligible in comparison with that of the host. (iv) The distributions of the host galaxies on the size – luminosity and Kormendy diagrams are shifted by ∼1 mag to fainter magnitudes in comparison with E/S0 galaxies. It means that the PRGs hosts are more similar to quenched discs than to ordinary early-type galaxie

KW - galaxies

KW - interactions

KW - photometry

KW - statistics

KW - structure

U2 - 10.1093/mnras/stu2604

DO - 10.1093/mnras/stu2604

M3 - Article

VL - 447

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 3

ER -