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 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 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 2010AJ....139.1199M)
a2 = nuclear classification obtained from Shimada et al.
(2000AJ....119.2664S 2000AJ....119.2664S)
a3 = nuclear classification obtained from Hao et al.
(2005AJ....129.1783H 2005AJ....129.1783H)
a4 = nuclear classification obtained from Veron et al.
(2006A&A...455..773V 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 2010A&A...517A..75B)
c2 = mid-IR photometry from Johnson et al. (2007AJ....134.1522J 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 2010A&A...517A..75B
(End) T. Bitsakis [Univ. of Crete, Greece], P. Vannier [CDS] 20-Jul-2011