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 - 2023	#notes
1	NGC 24	GiG	00 09 56.542	-24 57 47.27	12.12	12.20	11.58	11.46	11.5	~	241	1
2	NAME SMC	G	00 52 38.0	-72 48 01		2.79	2.2			~	10840	1
3	NGC 584	GiP	01 31 20.7231919800	-06 52 04.770287472	11.93	11.44	10.48			~	396	2
4	NGC 925	H2G	02 27 16.913	+33 34 43.97		10.69	10.12	9.55		~	764	1
5	NGC 1097	LIN	02 46 19.059	-30 16 29.68	10.46	9.97	9.48	8.72	9.8	~	1312	3
6	NGC 1269	GiG	03 17 18.5785534752	-41 06 28.628735184	9.85	9.83	8.81	8.72		~	413	1
7	NGC 1316	GiP	03 22 41.789	-37 12 29.52	9.81	9.15	8.53	7.66		~	1354	1
8	NGC 1404	GiP	03 38 51.917	-35 35 39.81	11.53	10.69	10.00	9.03		~	737	1
9	NGC 1512	GiP	04 03 54.281	-43 20 55.86	11.30	11.43	10.54	10.37		~	378	1
10	NGC 1566	Sy1	04 20 00.3968473248	-54 56 16.624708764	10.29	10.19	9.73	9.21	10.1	~	867	2
11	NGC 1705	SBG	04 54 13.4661493464	-53 21 39.471592428	12.32	12.96	12.56	12.58	12.9	~	647	1
12	NAME LMC	G	05 23 34.6	-69 45 22			0.4			~	16973	1
13	NGC 2798	GiP	09 17 22.9	+42 00 00	13.03	13.04	12.32			~	320	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			~	1052	1
16	NGC 2976	GiP	09 47 15.458	+67 54 58.97	11.77	11.03	10.16	9.51		~	657	1
17	M 81	Sy2	09 55 33.1726556496	+69 03 55.062505368		7.89	6.94			~	4358	3
18	NGC 3189	GiP	10 18 05.643	+21 49 54.98	12.60	12.12	11.15	11.14		~	388	2
19	NGC 3180	GiG	10 18 16.985	+41 25 27.77		10.4				~	709	0
20	NGC 3198	EmG	10 19 54.990	+45 32 58.88	10.83	10.87	10.33			~	891	1
21	M 95	GiP	10 43 57.7313485800	+11 42 13.301191332	10.71	10.51	9.73	9.48		~	1084	2
22	NGC 3521	LSB	11 05 48.5680991376	-00 02 09.245076540	10.06	9.83	9.02	10.1	9.6	~	791	2
23	NGC 3621	AGN	11 18 16.300	-32 48 45.36	10.10	9.44	9.56	8.07	10.1	~	567	3
24	M 66	GiP	11 20 15.0	+12 59 29	9.85	9.65	8.92			~	1342	4
25	NGC 4536	GiP	12 34 27.1	+02 11 18	11.14	11.16	10.55	17.393		~	833	3
26	NGC 4559	H2G	12 35 57.6402869976	+27 57 35.859278160		10.46	10.01			~	609	1
27	M 90	Sy2	12 36 49.8009839880	+13 09 46.523813040	10.56	10.26	9.54			~	880	1
28	M 58	SyG	12 37 43.5	+11 49 06	10.80	10.48	9.66			~	1054	2
29	M 104	LIN	12 39 59.43185902	-11 37 22.9961800	9.51	9.55	8.00	8.05		~	1379	3
30	NGC 4625	GiP	12 41 52.7121819576	+41 16 26.115765780	12.74	12.92	12.35			~	354	2
31	NGC 4631	GiP	12 42 08.009	+32 32 29.44		9.78	9.19	9.10		~	1079	2
32	NGC 4725	Sy2	12 50 26.5716367992	+25 30 02.733090588		13.45	12.44			~	675	2
33	M 94	SyG	12 50 53.0737971432	+41 07 12.900884628	9.15	8.96	8.24	7.78		~	1357	2
34	M 64	SyG	12 56 43.696	+21 40 57.57		9.36	8.52			~	915	2
35	NGC 5033	Sy1	13 13 27.535	+36 35 37.14		11.01	12.03	9.73		~	851	3
36	M 63	LIN	13 15 49.2741893928	+42 01 45.728076108		9.34	8.59	8.35		~	1197	2
37	M 51	GiP	13 29 52.698	+47 11 42.93		9.26	8.36	8.40		~	4247	4
38	NGC 5195	GiP	13 29 59.590	+47 15 58.06	10.76	10.45	9.55	9.31		~	763	3
39	NGC 5474	GiP	14 05 01.608	+53 39 43.95		11.28	10.79			~	432	1
40	NGC 5713	GiP	14 40 11.528	-00 17 21.16	11.88	11.84	11.20			~	391	2
41	M 102	SyG	15 06 29.561	+55 45 47.91	11.12	10.74	9.89			~	543	3
42	NGC 7331	LIN	22 37 04.0506038088	+34 24 56.800076508	10.65	10.35	9.48			~	1206	2

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