J/MNRAS/397/1756 Fourier-derived parameters of the CIG sample (Durbala+, 2009) ================================================================================ Fourier photometric analysis of isolated galaxies in the context of the AMIGA project. Durbala A., Buta R., Sulentic J.W., Verdes-Montenegro L. =2009MNRAS.397.1756D (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: Galaxies, photometry ; Morphology ; Colors Keywords: galaxies: evolution - galaxies: fundamental parameters - galaxies: general - galaxies: photometry - galaxies: spiral - galaxies: structure Abstract: We present here the results of a Fourier photometric decomposition of a representative sample of ~100 isolated CIG galaxies (Catalog of Isolated Galaxies) in the morphological range Sb-Sc. This study is an integral part of the AMIGA (Analysis of the Interstellar Medium of Isolated Galaxies) project. It complements the photometric analysis presented in our previous paper for the same sample of disc galaxies by allowing a description of the spiral structure morphology. We also estimate dynamical measures like torque strength for bar and spiral, and also the total non-axisymmetric torque by assuming a constant mass-to-light ratio, and explore the interplay between the spiral and bar components of galaxies. Both the length (l_bar_) and the contrast (e.g. A_2b_) of the Fourier bars decrease along the morphological sequence Sb-Sbc-Sc, with bars in earlier types being longer and showing higher contrast. The bars of Sb galaxies are ~ three times longer than the bars in Sc types, consistent with our previous study. We find that the longer bars are not necessarily stronger (as quantified by the torque Q_b_measure), but longer bars show a higher contrast A_2b_, in very good agreement with theoretical predictions. Our data suggest that bar and spiral components are rather independent in the sense that the torque strengths of the two components are not correlated. The total strength Q_g_ is a very reliable tracer of the bar strength measure Q_b_, the two quantities showing a very tight linear correlation. Comparison with a similar sample of disc galaxies (same morphological range) extracted from the OSUBGS (Ohio State University Bright Galaxy Survey) indicates that the isolated CIG/AMIGA galaxies host significantly longer Fourier bars and possibly show a different distribution of spiral torque Q_s_. The Fourier analysis also revealed a potential case of counterwinding spiral structure (KIG652/NGC5768), which deserves further kinematic study. We find that m=2 (i.e. dominating two-armed pattern) is the most common spiral arm multiplicity among the sample of Sb-Sc CIG/AMIGA galaxies (~40 per cent), m=2 and 3 and m=1 and 2 are found in ~28 and ~13 per cent of isolated galaxies, respectively. Description: Revision of the main properties for all AMIGA galaxies. Because a significant number of new data are available for the sample since the AMIGA project started, apparent magnitudes, morphological types, distances, and optical luminosities for the CIG sample have been updated. In the frame of the Wf4Ever project, the revision of these properties was partially automated by the implementation of scientific workflows that ask for and gather values of some of the properties for all AMIGA galaxies from the HyperLeda catalog. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table1.dat 75 93 Fourier-derived parameters in i band for the CIG/KIG galaxies in our sample -------------------------------------------------------------------------------- See also: J/A+A/411/391 : AMIGA project. CIG galaxies revised positions (Leon+, 2003) J/A+A/436/443 : AMIGA I Velocities of CIG galaxies (Verdes-Montenegro+, 2005) J/A+A/449/937 : AMIGA II Morphological refinement (Sulentic+, 2006) J/A+A/462/507 : AMIGA III IRAS data (Lisenfeld+, 2007) J/A+A/470/505 : AMIGA IV Neighbours around CIG galaxies (Verley+, 2007) J/A+A/472/121 : AMIGA V Isolation parameters (Verley+, 2007) J/A+A/485/475 : AMIGA VI Radio fluxes of the isolated galaxies (Leon+ 2008) J/A+A/486/73 : AMIGA VII FIR and radio study (Sabater+, 2008) J/A+A/532/A117 : AMIGA VIII Flux ratio asymmetry parameter (Espada+, 2011) J/A+A/534/A102 : AMIGA IX Molecular gas properties (Lisenfeld+, 2011) J/A+A/540/A47 : AMIGA X Isolated galaxy colors (Fernandez Lorenzo+, 2012) J/A+A/545/A15 : AMIGA XI Optical nuclear activity (Sabater+, 2012) J/MNRAS/434/325 : 452 AMIGA gal. physical parameters (Fernandez Lorenzo+ 2013) Byte-by-byte Description of file: table1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 5 I5 --- CIG CIG (VII/82) number (K73 NNNN in Simbad) 7- 9 I3 deg PA Mean orientation angle (1) 11 A1 --- met [abc] Bulge deprojection method used (2) 13- 17 F5.3 --- Qg Total strength Qg 19- 23 F5.3 --- e_Qg Total strength standard deviation (SD) 25- 29 F5.3 --- Qb ? Bar strength 31- 35 F5.3 --- e_Qb ? Bar strength standard deviation (SD) 37- 41 F5.3 --- Qs Spiral strength 43- 47 F5.3 --- e_Qs Spiral strength standard deviation (SD) 49- 53 F5.3 --- A2b ? Maximum Fourier relative amplitude A2b 55- 59 F5.3 --- A4b ? Maximum Fourier relative amplitude A4b 61- 65 F5.3 --- A6b ? Maximum Fourier relative amplitude A6b 67- 70 F4.1 arcsec lbar ? Fourier bar length 72- 75 F4.1 arcsec r(Qb) ? Radius of maximal bar torque -------------------------------------------------------------------------------- Note (1): measured as explained in Section 3.1.1 of the paper. Note (2): Methods as follows: a = in most situations, the deprojection procedure automatically leads to a circularly shaped bulge b = in some cases the bulge is already circular in the original image (prior to deprojection), in which case we subtract the bulge model given by the budda decomposition code first c = if neither before nor after deprojection the bulge appears circular -------------------------------------------------------------------------------- Acknowledgements: Lourdes Verdes-Montenegro, lourdes(at)iaa.es ================================================================================ (End) Patricia Vannier [CDS] 26-Nov-2013