Detalles de publicación
PP 017126
STELLAR POPULATION SYNTHESIS OF STAR FORMING CLUMPS IN GALAXY PAIRS AND NON-INTERACTING SPIRAL GALAXIES
(1)Instituto de Astronomía,Universidad Nacional Autónoma de México,
04510, D. F., México (2)Department of Physics & Astronomy,East Tennessee State University,(3)Instituto de Astrofísica de Canarias,C/ Vía Láctea s/n,38200 La Laguna, Tenerife, Spain(4)Departamento de Astrofísica,
Universidad de La Laguna,Tenerife, Spain(5)Consejo Superior de
Investigaciones Científi cas,Spain 6CONACYT Research Fellow - Instituto de Radioastronomía y Astrofísica,Universidad Nacional Autónoma de México,58190 Morelia, México (7) Instituto de Ciencias Nucleares,
Universidad Nacional Autónoma de México,04510, D. F., México
We have identi ed 1027 star forming complexes in a sample of 46 galaxies from the Spirals, Bridges, and Tails
(SB&T) sample of interacting galaxies, and 693 star forming complexes in a sample of 38 non-interacting spiral (NIS)
galaxies in 8m observations from the Spitzer Infrared Array Camera. We have used archival multi-wavelength UV-to
IR observations to t the observed spectral energy distribution (SED) of our clumps with the Code Investigating
GALaxy Emission (CIGALE) using a double exponentially declined star formation history (SFH). We derive SFRs,
stellar masses, ages and fractions of the most recent burst, dust attenuation, and fractional emission due to an AGN
for these clumps. The resolved star formation main sequence holds on 2.5kpc scales, although it does not hold on
1kpc scales. We analyzed the relation between SFR, stellar mass, and age of the recent burst in the SB&T and NIS
samples, and we found that the SFR per stellar mass is higher in the SB&T galaxies, and the clumps are younger in
the galaxy pairs. We analyzed the SFR radial pro le and found that SFR is enhanced through the disk and in the
tidal features relative to normal spirals
(SB&T) sample of interacting galaxies, and 693 star forming complexes in a sample of 38 non-interacting spiral (NIS)
galaxies in 8m observations from the Spitzer Infrared Array Camera. We have used archival multi-wavelength UV-to
IR observations to t the observed spectral energy distribution (SED) of our clumps with the Code Investigating
GALaxy Emission (CIGALE) using a double exponentially declined star formation history (SFH). We derive SFRs,
stellar masses, ages and fractions of the most recent burst, dust attenuation, and fractional emission due to an AGN
for these clumps. The resolved star formation main sequence holds on 2.5kpc scales, although it does not hold on
1kpc scales. We analyzed the relation between SFR, stellar mass, and age of the recent burst in the SB&T and NIS
samples, and we found that the SFR per stellar mass is higher in the SB&T galaxies, and the clumps are younger in
the galaxy pairs. We analyzed the SFR radial pro le and found that SFR is enhanced through the disk and in the
tidal features relative to normal spirals