301. A contribution of star-forming clumps and accreting satellites to the mass assembly of z ∼ 2 galaxies
- Author
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Anna Cibinel, F. Valentino, Frederic Bournaud, Masato Onodera, A. Zanella, J. Sánchez Almeida, E. Le Floc'h, Raphael Gobat, E. Bernhard, Emanuele Daddi, Andreas Burkert, Christopher Harrison, Manuel Behrendt, Jakub Scholtz, Jérémy Fensch, V. Strazzullo, M. Kohandel, Zanella, A., Le Floc'h, E., Harrison, C. M., Daddi, E., Bernhard, E., Gobat, R., Strazzullo, V., Valentino, F., Cibinel, A., Sánchez Almeida, J., Kohandel, M., Fensch, J., Behrendt, M., Burkert, A., Onodera, M., Bournaud, F., and Scholtz, J.
- Subjects
Stellar mass ,FOS: Physical sciences ,Astrophysics ,interactions [Galaxies] ,Astrophysics::Cosmology and Extragalactic Astrophysics ,irregular [galaxies] ,01 natural sciences ,law.invention ,Telescope ,law ,0103 physical sciences ,galaxies: interactions ,Astrophysics::Solar and Stellar Astrophysics ,Emission spectrum ,Spectroscopy ,galaxies: irregular ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,evolution [galaxies] ,Physics ,ISM [galaxies] ,010308 nuclear & particles physics ,Star formation ,Spatially resolved ,galaxies: evolution ,galaxies: ISM ,galaxies: star formation ,galaxies: structure ,Astrophysics - Astrophysics of Galaxies ,Astronomy and Astrophysics ,Mass ratio ,Galaxy ,interaction [galaxies] ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,structure [galaxies] ,Astrophysics::Earth and Planetary Astrophysics ,star formation [galaxies] - Abstract
We investigate the contribution of clumps and satellites to the galaxy mass assembly. We analyzed spatially-resolved Hubble Space Telescope observations (imaging and slitless spectroscopy) of 53 star-forming galaxies at z ~ 1 - 3. We created continuum and emission line maps and pinpointed residual "blobs" detected after subtracting the galaxy disk. Those were separated into compact (unresolved) and extended (resolved) components. Extended components have sizes ~ 2 kpc and comparable stellar mass and age as the galaxy disks, whereas the compact components are 1.5 dex less massive and 0.4 dex younger than the disks. Furthermore the extended blobs are typically found at larger distances from the galaxy barycenter than the compact ones. Prompted by these observations and by the comparison with simulations, we suggest that compact blobs are in-situ formed clumps, whereas the extended ones are accreting satellites. Clumps and satellites enclose respectively ~ 20% and ~< 80% of the galaxy stellar mass, ~ 30% and ~ 20% of its star formation rate. Considering the compact blobs, we statistically estimated that massive clumps (Mstar >~ 10^9 Msun) have lifetimes of ~ 650 Myr, and the less massive ones (10^8 < Mstar < 10^9 Msun) of ~ 145 Myr. This supports simulations predicting long-lived clumps (lifetime > 100 Myr). Finally, ~< 30% (13%) of our sample galaxies are undergoing single (multiple) merger(s), they have a projected separation ~< 10 kpc, and the typical mass ratio of our satellites is 1:5 (but ranges between 1:10 and 1:1), in agreement with literature results for close pair galaxies., 20 pages (plus appendix), 8 figures, 2 tables. Accepted for publication in MNRAS
- Published
- 2019
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