2009A&A...507.1793N

Query : 2009A&A...507.1793N

2009A&A...507.1793N - Astronomy and Astrophysics, volume 507, 1793-1813 (2009/12-1)

Analysis of galaxy spectral energy distributions from far-UV to far-IR with CIGALE: studying a SINGS test sample.

NOLL S., BURGARELLA D., GIOVANNOLI E., BUAT V., MARCILLAC D. and MUNOZ-MATEOS J.C.

Abstract (from CDS):

Photometric data of galaxies covering the rest-frame wavelength range from far-UV to far-IR make it possible to derive galaxy properties with a high reliability by fitting the attenuated stellar emission and the related dust emission at the same time. For this purpose we wrote the code CIGALE (Code Investigating GALaxy Emission) that uses model spectra composed of the Maraston (or PEGASE) stellar population models, synthetic attenuation functions based on a modified Calzetti law, spectral line templates, the Dale & Helou dust emission models, and optional spectral templates of obscured AGN. Depending on the input redshifts, filter fluxes were computed for the model set and compared to the galaxy photometry by carrying out a Bayesian-like analysis. CIGALE was tested by analysing 39 nearby galaxies selected from SINGS. The reliability of the different model parameters was evaluated by studying the resulting expectation values and their standard deviations in relation to the input model grid. Moreover, the influence of the filter set and the quality of photometric data on the code results was estimated. For up to 17 filters with effective wavelengths between 0.15 and 160µm, we find robust results for the mass, star formation rate, effective age of the stellar population at 4000Å, bolometric luminosity, luminosity absorbed by dust, and attenuation in the far-UV. Details of the star formation history (excepting the burst fraction) and the shape of the attenuation curve are difficult to investigate with the available broad-band UV and optical photometric data. A study of the mutual relations between the reliable properties confirms the dependence of star formation activity on morphology in the local Universe and indicates a significant drop in this activity at about 1011M☉ towards higher total stellar masses. The dustiest galaxies in the SINGS sample are present in the same mass range. On the other hand, the far-UV attenuation of our sample galaxies does not appear to show a significant dependence on star formation activity. The results for our SINGS test sample demonstrate that CIGALE can be a valuable tool for studying basic properties of galaxies in the near and distant Universe if UV-to-IR data are available.

Abstract Copyright: ∼

Journal keyword(s): methods: data analysis - galaxies: fundamental parameters - galaxies: stellar content - galaxies: ISM - ultraviolet: galaxies - infrared: galaxies

Simbad objects: 42

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Number of rows : 42
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 NGC 24 EmG 00 09 56.542 -24 57 47.27 12.12 12.20 11.58 11.46 11.5 ~ 249 1
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 11149 1
3 NGC 584 Sy2 01 31 20.7231919800 -06 52 04.770287472 11.93 11.44 10.48     ~ 402 2
4 NGC 925 H2G 02 27 16.913 +33 34 43.97   10.69 10.12 9.55   ~ 783 1
5 NGC 1097 LIN 02 46 19.059 -30 16 29.68 10.46 9.97 9.48 8.72 9.8 ~ 1342 3
6 NGC 1269 EmG 03 17 18.5785534752 -41 06 28.628735184 9.85 9.83 8.81 8.72   ~ 422 1
7 NGC 1316 BL? 03 22 41.789 -37 12 29.52 9.81 9.15 8.53 7.66   ~ 1387 1
8 NGC 1404 GiP 03 38 51.917 -35 35 39.81 11.53 10.69 10.00 9.03   ~ 751 1
9 NGC 1512 GiP 04 03 54.281 -43 20 55.86 11.30 11.43 10.54 10.37   ~ 396 1
10 NGC 1566 Sy1 04 20 00.3968473248 -54 56 16.624708764 10.29 10.19 9.73 9.21 10.1 ~ 912 2
11 NGC 1705 Sy2 04 54 13.4661493464 -53 21 39.471592428 12.32 12.96 12.56 12.58 12.9 ~ 662 1
12 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 17434 0
13 NGC 2798 GiP 09 17 22.9 +42 00 00 13.03 13.04 12.32     ~ 325 3
14 APG 283 PaG 09 17 26.99 +41 59 48.8   12.2       ~ 193 1
15 NGC 2841 LIN 09 22 02.6778711696 +50 58 35.737082868 10.43 10.09 9.22     ~ 1073 1
16 NGC 2976 GiP 09 47 15.458 +67 54 58.97 11.77 11.03 10.16 9.51   ~ 673 1
17 M 81 Sy2 09 55 33.1726556496 +69 03 55.062505368   7.89 6.94     ~ 4450 3
18 NGC 3189 GiP 10 18 05.643 +21 49 54.98 12.60 12.12 11.15 11.14   ~ 399 2
19 NGC 3180 GiG 10 18 16.985 +41 25 27.77   10.4       ~ 735 0
20 NGC 3198 EmG 10 19 54.990 +45 32 58.88 10.83 10.87 10.33     ~ 905 1
21 M 95 GiP 10 43 57.7313485800 +11 42 13.301191332 10.71 10.51 9.73 9.48   ~ 1122 2
22 NGC 3521 G 11 05 48.5680991376 -00 02 09.245076540 10.06 9.83 9.02 10.1 9.6 ~ 817 2
23 NGC 3621 Sy2 11 18 16.300 -32 48 45.36 10.10 9.44 9.56 8.07 10.1 ~ 590 3
24 M 66 GiP 11 20 15.0 +12 59 29 9.85 9.65 8.92     ~ 1386 4
25 NGC 4536 GiP 12 34 27.1 +02 11 18 11.14 11.16 10.55 17.393   ~ 853 3
26 NGC 4559 H2G 12 35 57.6402869976 +27 57 35.859278160   10.46 10.01     ~ 629 1
27 M 90 Sy2 12 36 49.8009839880 +13 09 46.523813040 10.56 10.26 9.54     ~ 899 1
28 M 58 Sy2 12 37 43.5 +11 49 06 10.80 10.48 9.66     ~ 1079 2
29 M 104 LIN 12 39 59.43185902 -11 37 22.9961800 9.51 9.55 8.00 8.05   ~ 1396 3
30 NGC 4625 GiP 12 41 52.7121819576 +41 16 26.115765780 12.74 12.92 12.35     ~ 364 2
31 NGC 4631 GiP 12 42 08.009 +32 32 29.44   9.78 9.19 9.10   ~ 1095 2
32 NGC 4725 Sy2 12 50 26.5716367992 +25 30 02.733090588   13.45 12.44     ~ 695 2
33 M 94 SyG 12 50 53.0737971432 +41 07 12.900884628 9.15 8.96 8.24 7.78   ~ 1386 2
34 M 64 SyG 12 56 43.696 +21 40 57.57   9.36 8.52     ~ 940 2
35 NGC 5033 Sy2 13 13 27.535 +36 35 37.14   11.01 12.03 9.73   ~ 869 3
36 M 63 LIN 13 15 49.2741893928 +42 01 45.728076108   9.34 8.59 8.35   ~ 1224 2
37 M 51 Sy2 13 29 52.698 +47 11 42.93   9.26 8.36 8.40   ~ 4330 4
38 NGC 5195 GiP 13 29 59.590 +47 15 58.06 10.76 10.45 9.55 9.31   ~ 778 3
39 NGC 5474 GiP 14 05 01.608 +53 39 43.95   11.28 10.79     ~ 443 1
40 NGC 5713 GiP 14 40 11.528 -00 17 21.16 11.88 11.84 11.20     ~ 398 2
41 M 102 SyG 15 06 29.561 +55 45 47.91 11.12 10.74 9.89     ~ 552 3
42 NGC 7331 LIN 22 37 04.0506038088 +34 24 56.800076508 10.65 10.35 9.48     ~ 1228 2

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