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  A contribution of star-forming clumps and accreting satellites to the mass assembly of z ∼ 2 galaxies

Zanella, A., Le Floc’h, E., Harrison, C. M., Daddi, E., Bernhard, E., Gobat, R., et al. (2019). A contribution of star-forming clumps and accreting satellites to the mass assembly of z ∼ 2 galaxies. Monthly Notices of the Royal Astronomical Society, 489(2), 2792-2818. doi:10.1093/mnras/stz2099.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0005-4E40-C Version Permalink: http://hdl.handle.net/21.11116/0000-0005-4E41-B
Genre: Journal Article

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Zanella, A., Author
Le Floc’h, E., Author
Harrison, C. M., Author
Daddi, E., Author
Bernhard, E., Author
Gobat, R., Author
Strazzullo, V., Author
Valentino, F., Author
Cibinel, A., Author
Almeida, J. Sánchez, Author
Kohandel, M., Author
Fensch, J., Author
Behrendt, M.1, Author              
Burkert, A.1, Author              
Onodera, M., Author
Bournaud, F., Author
Scholtz, J., Author
Affiliations:
1Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society, ou_159895              

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 Abstract: We investigate the contribution of clumps and satellites to the galaxy mass assembly. We analysed spatially resolved HubbleSpace 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 disc. 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 discs, whereas the compact components are 1.5 dex less massive and 0.4 dex younger than the discs. Furthermore, the extended blobs are typically found at larger distances from the galaxy barycentre 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 per cent and ≲80 per cent of the galaxy stellar mass, ∼30 per cent and ∼20 per cent of its star formation rate. Considering the compact blobs, we statistically estimated that massive clumps (M ≳ 109 M) have lifetimes of ∼650 Myr, and the less massive ones (108 < M < 109 M) of ∼145 Myr. This supports simulations predicting long-lived clumps (lifetime ≳ 100 Myr). Finally, ≲30 per cent (13 per cent) 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.

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 Dates: 2019-08-05
 Publication Status: Published online
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 Rev. Method: Peer
 Identifiers: DOI: 10.1093/mnras/stz2099
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Title: Monthly Notices of the Royal Astronomical Society
  Other : Mon. Not. R. Astron. Soc.
Source Genre: Journal
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Publ. Info: Oxford : Oxford University Press
Pages: - Volume / Issue: 489 (2) Sequence Number: - Start / End Page: 2792 - 2818 Identifier: ISSN: 1365-8711
CoNE: https://pure.mpg.de/cone/journals/resource/1000000000024150