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J/A+A/533/A142    UV-to-IR fluxes of Hickson compact groups    (Bitsakis+, 2011)

Examining the UV-to-IR properties of Hickson compact groups of galaxies. II. Multiwavelength analysis of the complete GALEX-Spitzer sample. Bitsakis T., Charmandaris V., da Cunha E., Diaz-Santos T., le Floc'h E., Magdis G. <Astron. Astrophys. 533, A142 (2011)> =2011A&A...533A.142B
ADC_Keywords: Galaxies, IR ; Photometry, infrared ; Photometry, SDSS ; Ultraviolet ; Photometry, UBVRI Keywords: infrared: galaxies - galaxies: evolution - galaxies: interactions - galaxies: star formation Abstract: We present a comprehensive study on the impact of the environment of compact galaxy groups on the evolution of their members using a multi-wavelength analysis, from the UV to the infrared, for a sample of 32 Hickson compact groups (HCGs) containing 135 galaxies. Fitting the SEDs of all galaxies with the state-of-the-art model of da Cunha (2008MNRAS.388.1595D) we can accurately calculate their mass, SFR, and extinction, as well as estimate their infrared luminosity and dust content. We compare our findings with samples of field galaxies, early-stage interacting pairs, and cluster galaxies with similar data. We find that classifying the groups as dynamically "old" or "young", depending on whether or not at least one quarter of their members are early-type systems, is physical and consistent with past classifications of HCGs based on their atomic gas content. Dynamically "old" groups are more compact and display higher velocity dispersions than "young" groups. Late-type galaxies in dynamically "young" groups have specific star formation rates (sSFRs), NUV-r, and mid-infrared colors which are similar to those of field and early stage interacting pair spirals. Late-type galaxies in dynamically "old" groups have redder NUV-r colors, as they have likely experienced several tidal encounters in the past building up their stellar mass, and display lower sSFRs. We identify several late-type galaxies which have sSFRs and colors similar to those of elliptical galaxies, since they lost part of their gas due to numerous interactions with other group members. Also, 25% of the elliptical galaxies in these groups have bluer UV/optical colors than normal ellipticals in the field, probably due to star formation as they accreted gas from other galaxies of the group, or via merging of dwarf companions. Finally, our SED modeling suggests that in 13 groups, 10 of which are dynamically "old", there is diffuse cold dust in the intragroup medium. All this evidence point to an evolutionary scenario in which the effects of the group environment and the properties of the galaxy members are not instantaneous. Early on, the influence of close companions to group galaxies is similar to the one of galaxy pairs in the field. However, as the time progresses, the effects of tidal torques and minor merging, shape the morphology and star formation history of the group galaxies, leading to an increase of the fraction of early-type members and a rapid built up of the stellar mass in the remaining late-type galaxies. Description: The UV to IR photometry of 135 galaxies contained in 32 Hickson Compact Groups (HCGs) of galaxies. The sample is GALEX-Spitzer selected. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 319 135 UV-to-IR fluxes for the galaxies in the sample table4.dat 59 135 The morphological type and derived physical parameters based on the SED modeling of the HCG galaxies table6.dat 25 135 Distance to, virial radius, and morphology of the nearest neighbor, as well as "strength" of interaction for the HCG galaxies
See also: VII/213 : Hickson's Compact groups of Galaxies (Hickson+ 1982-1994) VII/248 : Quasars and Active Galactic Nuclei (12th Ed.) (Veron+ 2006) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 3 A3 --- --- [HCG] 4- 7 A4 --- HCG Galaxy name 9- 13 A5 --- MType Galaxy morphology 16- 21 A6 --- Nuc Nuclear classification (2) 23- 27 F5.1 Mpc Dist Galaxy distance 29- 32 F4.2 mJy FFUV GALEX FUV flux 35- 38 F4.2 mJy e_FFUV GALEX FUV flux error 41- 44 F4.2 mJy FNUV GALEX NUV flux 47- 50 F4.2 mJy e_FNUV GALEX NUV flux error 53- 57 F5.2 mJy FB B flux 59- 62 F4.2 mJy e_FB B flux error 65- 70 F6.2 mJy FR R flux 73- 76 F4.2 mJy e_FR R flux error 79- 83 F5.2 mJy Fu SDSS u flux 85- 88 F4.2 mJy e_Fu SDSS u flux error 90- 94 F5.2 mJy Fg SDSS g flux 96- 99 F4.2 mJy e_Fg SDSS g flux error 102-107 F6.2 mJy Fr SDSS r flux 109-112 F4.2 mJy e_Fr SDSS r flux error 114-119 F6.2 mJy Fi SDSS i flux 121-124 F4.2 mJy e_Fi SDSS i flux error 126-131 F6.2 mJy Fz SDSS z flux 133-136 F4.2 mJy e_Fz SDSS z flux error 138-143 F6.2 mJy FJ J flux 145-149 F5.2 mJy e_FJ J flux error 151-156 F6.2 mJy FH H flux 158-162 F5.2 mJy e_FH H flux error 164-169 F6.2 mJy FKs Ks flux 171-175 F5.2 mJy e_FKs Ks flux error 177-182 F6.2 mJy F3.6 Spitzer/IRAC 3.6um flux 184-187 F4.2 mJy e_F3.6 Spitzer/IRAC 3.6um flux error 189-194 F6.2 mJy F4.5 Spitzer/IRAC 4.5um flux 196-199 F4.2 mJy e_F4.5 Spitzer/IRAC 4.5um flux error 201-206 F6.2 mJy F5.7 Spitzer/IRAC 5.7um flux 208-211 F4.2 mJy e_F5.7 Spitzer/IRAC 5.7um flux error 213-218 F6.2 mJy F8.0 Spitzer/IRAC 8.0um flux 220-224 F5.2 mJy e_F8.0 Spitzer/IRAC 8.0um flux error 226-232 F7.2 mJy F24 Spitzer/MIPS 24um flux 234-238 F5.2 mJy e_F24 Spitzer/MIPS 24um flux error 240-244 I5 mJy F60 IRAS 60um flux 246-250 I5 mJy e_F60 IRAS 60um flux error 252-256 I5 mJy F100 IRAS 100um flux 258-262 I5 mJy e_F100 IRAS 100um flux error 264-268 I5 mJy F65 AKARI/N60 65um flux 270-274 I5 mJy e_F65 AKARI/N60 65um flux error 276-280 I5 mJy F90 AKARI/WIDE-S 90um flux 282-286 I5 mJy e_F90 AKARI/WIDE-S 90um flux error 288-292 I5 mJy F140 AKARI/WIDE-L 140um flux 294-298 I5 mJy e_F140 AKARI/WIDE-L 140um flux error 300-304 I5 mJy F160 AKARI/N160 160um flux 306-310 I5 mJy e_F160 AKARI/N160 160um flux error 312-319 A8 --- Ref References (1)
Note (1): References code as follows: a1 = nuclear classification obtained from Martinez et al. (2010AJ....139.1199M) a2 = nuclear classification obtained from Shimada et al. (2000AJ....119.2664S) a3 = nuclear classification obtained from Hao et al. (2005AJ....129.1783H) a4 = nuclear classification obtained from Veron et al. (2006A&A...455..773V, Cat. VII/248) b1 = near-IR photometry from Palomar b2 = near-IR photometry from 2MASS b3 = near-IR photometry from Skinakas c1 = mid-IR photometry from Bitsakis et al. (2010A&A...517A..75B) c2 = mid-IR photometry from Johnson et al. (2007AJ....134.1522J) c3 = mid-IR photometry from Spitzer archive, PID 50764 c4 = mid-IR photometry from Spitzer archive, PID 159 c5 = mid-IR photometry from Spitzer archive, PID 40385 c6 = mid-IR photometry from Spitzer archive, PID 198 Note (2): nuclear classifications as AGN, LLAGN (low-luminosity AGN), HII, LINER (Low-Ionization Nuclear Emission-line Region), dLINER (dwarf LINER), TO (transition object), pec(uliar), unclas(sified)
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 4 A4 --- HCG HCG galaxy name 5- 7 A3 --- n_HCG [*± ] Note on galaxy (1) 8- 12 A5 --- MType Morphological type 14- 18 F5.2 --- chi2 chi2 value 20- 23 F4.2 --- tauObs Observed optical depth 25- 28 F4.2 --- tauISM Diffuse ISM optical depth V,ISM 30- 33 F4.2 --- tau Total optical depth (tauBC+tauISM) (2) 35- 40 F6.2 10+9Msun Mstar Stellar Mass 42- 46 F5.2 Msun/yr SFR Star formation rate 48- 52 F5.2 10-11yr-1 sSFR Specific star formation rate 54- 59 F6.2 10+9Lsun LIR Infrared luminosity
Note (1): Notes as follows: * = The most massive galaxy of each group, used in the calculations of the dynamical masses in Table 5 + = Galaxies with no 24um data. The SFRs, sSFRs, and LIR of these systems are not well constrained - = An AGN in their nucleus dominates their mid-IR emission Note (2): Total optical depth, tauBC+tauISM, where tauBC is the optical depth from the stellar birth clouds and tauISM is optical depth contributed from the diffuse ISM.
Byte-by-byte Description of file: table6.dat
Bytes Format Units Label Explanations
1- 4 A4 --- HCG HCG galaxy name 6- 8 I3 kpc R ? Projected distance to the nearest neighbor 10- 13 I4 kpc rvir ? Virial radius 15- 19 F5.3 --- Str ? "Strength" of interaction as described in Sect. 4.6., <R/rvir,nei>/n (1) 21- 25 A5 --- NType ? Morphological type of the nearest neighbor (early or late)
Note (1): This is estimated by averaging the ratios of the projected distances over the virial radii for all the neighbors of each galaxy and divide them by the total number of neighbors (n).
Acknowledgements: Theodoros Bitsakis, bitsakis(at)physics.uoc.gr References: Bitsakis et al., Paper I 2010A&A...517A..75B
(End) T. Bitsakis [Univ. of Crete, Greece], P. Vannier [CDS] 20-Jul-2011
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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