The MUSE Hubble Ultra Deep Field Survey

Star-forming galaxies have been found to follow a relatively tight relation between stellar mass (M*) and star formation rate (SFR), dubbed the “star formation sequence”. A turnover in the sequence has been observed, where galaxies with M* <  1010 M⊙ follow a steeper relation than their higher ma...

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Published in:Astronomy and astrophysics (Berlin) 2018-11, Vol.619
Main Authors: Boogaard, Leindert A., Brinchmann, Jarle, Bouché, Nicolas, Paalvast, Mieke, Bacon, Roland, Bouwens, Rychard J., Contini, Thierry, Gunawardhana, Madusha L. P., Inami, Hanae, Marino, Raffaella A., Maseda, Michael V., Mitchell, Peter, Nanayakkara, Themiya, Richard, Johan, Schaye, Joop, Schreiber, Corentin, Tacchella, Sandro, Wisotzki, Lutz, Zabl, Johannes
Format: Article
Language:English
Subjects:
Computer simulation
Cosmic dust
Galaxies
galaxies: evolution
galaxies: formation
galaxies: ISM
galaxies: star formation
Halos
Hubble deep field
Hyperplanes
Mathematical models
methods: statistical
Normal distribution
Red shift
Scattering
Star & galaxy formation
Star formation rate
Stellar mass
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Summary:Star-forming galaxies have been found to follow a relatively tight relation between stellar mass (M*) and star formation rate (SFR), dubbed the “star formation sequence”. A turnover in the sequence has been observed, where galaxies with M* <  1010 M⊙ follow a steeper relation than their higher mass counterparts, suggesting that the low-mass slope is (nearly) linear. In this paper, we characterise the properties of the low-mass end of the star formation sequence between 7 ≤ log M*[M⊙]  ≤  10.5 at redshift 0.11 <  z  <   0.91. We use the deepest MUSE observations of the Hubble Ultra Deep Field and the Hubble Deep Field South to construct a sample of 179 star-forming galaxies with high signal-to-noise emission lines. Dust-corrected SFRs are determined from Hβ λ4861 and Hα λ6563. We model the star formation sequence with a Gaussian distribution around a hyperplane between logM*, logSFR, and log(1 + z), to simultaneously constrain the slope, redshift evolution, and intrinsic scatter. We find a sub-linear slope for the low-mass regime where log SFR [M⊙yr−1] = 0.83+0.07−0.06 log M*[M⊙]+1.74+0.66−0.68 log(1 + z) log SFR [ M ⊙ yr − 1 ] = 0 . 83 − 0.06 + 0.07 log M ∗ [ M ⊙ ] + 1 . 74 − 0.68 + 0.66 log ( 1 + z ) $ \log \text{ SFR}[M_{\odot}\,{\mathrm{yr}}^{-1}] = 0.83^{+0.07}_{-0.06}\log{M_{*}}[M_{\odot}] + {1.74^{+0.66}_{-0.68}}{\log (1+z)} $ , increasing with redshift. We recover an intrinsic scatter in the relation of σintr = 0.44+0.05−0.04 σ intr = 0 . 44 − 0.04 + 0.05 $ \sigma_{\text{ intr}}={0.44^{+0.05}_{-0.04}} $ , dex, larger than typically found at higher masses. As both hydrodynamical simulations and (semi-)analytical models typically favour a steeper slope in the low-mass regime, our results provide new constraints on the feedback processes which operate preferentially in low-mass halos.
ISSN:0004-6361
1432-0746
DOI:10.1051/0004-6361/201833136