BVRI photometric analysis for the galaxy group NGC 4410

¹ Departamento de Física, CUCEI, Universidad de Guadalajara, Avenida Revolución SN, Guadalajara, Jalisco, México
² Instituto de Astronomía y Meteorología, Universidad de Guadalajara, Avenida Vallarta No. 2602, Col. Arcos Vallarta, CP 44130, Guadalajara, Jalisco, México e-mail: arturopg@astro.iam.udg.mx
³ Institute of Astronomy and Astrophysics, National Observatory of Athens, I. Metaxa & V. Paulou, Penteli, 15236 Athens, Greece
⁴ Royal Observatory of Belgium, Solar Physics, Ringlaan 3, 1180 Brussels, Belgium
⁵ Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, 04510, México DF, México
⁶ Instituto de Astronomía, Universidad Nacional Autónoma de México, CP 22800, Ensenada, Baja California, México
⁷ Jodrell Bank Observatory, School of Physics and Astronomy, University of Manchester, Macclesfield, Cheshire, SK11 9DL, UK
⁸ Astrophysics Research Institute, Liverpool John Moores University, 12 Quays House, Egerton Wharf, Birkenhead, CH41 1LD, UK

Received: 19 June 2007
Accepted: 17 March 2008

Abstract

We present a BVRI CCD (Charge Coupled Device) surface photometry analysis of the galaxy group NGC 4410, which contains four galaxies in interaction. Along with our photometric study, we show residual images (after subtracting isophotal models) and unsharp masked images to uncover any hidden structures in this system of galaxies; we have also performed a two-dimensional bulge-disk decomposition for NGC 4410C and D, and a major axis sector profile for NGC 4410A. We have calculated BVRI surface brightnesses and colors within regions such as galaxy centers, bridges, tails and optical knots in the NGC 4410 system, generating color maps and color profiles. The information obtained was used to discover the predominant stellar populations. The colors of the galaxies imply ages of ~210⁹ to ~210¹⁰ years for models using a range of metallicities. The bluer knots and H II regions have colors implying ages of a minimum of 510⁸ years, but possibly as high as 310⁹ years for stellar populations formed in the interaction. These results lead us to conclude that there is a moderate star formation rate and a tranquil evolving state of the system with a long timescale for interaction, much longer than the typical dynamical timescales of 10⁸ years. Although we note that NGC 4410D has a blue nucleus (possible nuclear starburst?), bulge, bar, and short spiral arms, and may be interacting with a H I gas cloud. Some observed structures in NGC 4410A are coincident with previously studied H II regions, a tidal arm and optical/radio knots found in this galaxy. An optical knot E coincident with a radio knot may be an optical synchrotron emission or an H II region. The galaxy NGC 4410B appears to be a boxy giant elliptical with a possible dusty disk embedded (similar to Cen A?) and NGC 4410C is confirmed as a lenticular galaxy.