The Morphologies of Massive Galaxies at 1<z<3 in the CANDELS-UDS Field: Compact Bulges, and the Rise and Fall of Massive Disks

By V. Bruce, J. Dunlop, M. Cirasuolo, R. McLure, Thomas Targett, E. Bell, Darren Croton, A. Dekel, S. Faber, H. Ferguson and 9 more. Proceedings of the International Astronomical Union, 2012

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Abstract We have used high-resolution, HST WFC3/IR, near-infrared imaging to conduct a detailed bulge-disk decomposition of the morphologies of ≃ 200 of the most massive (M* > 1011 M⊙) galaxies at 1 < z < 3 in the CANDELS-UDS field. We find that, while such massive galaxies at low redshift are generally bulge-dominated, at redshifts 1 2 they are mostly disk-dominated. Interestingly, we find that while most of the quiescent galaxies are bulge-dominated, a significant fraction (25–40%) of the most quiescent galaxies, have disk-dominated morphologies. Thus, our results suggest that the physical mechanisms which quench star-formation activity are not simply connected to those responsible for the morphological transformation of massive galaxies.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/05423bacedeac3b1c571392ebef8c5a641ed2182

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Citations in the corpus

The Evolution of Galaxy Structure Over Cosmic Time (2014, background): “…same selection (e.g., Buitrago et al. 2013). this has been interpreted by some to imply that these galaxies are more ’disk-like’ at high redshifts (Bruce et al. 2012), although the morphologies of these systems by visual inspection, and their internal structures and The Structural Evolution of…”
Evolution of density profiles in high-z galaxies: compaction and quenching inside-out (2015, background): “On the other hand, quenched disc galaxies have also been found (McGrath et al. 2008; van Dokkum et al. 2008; Bundy et al. 2010; Salim et al. 2012; Bruce et al. 2012; Carollo et al. 2014).”
Galaxy And Mass Assembly (GAMA): mass–size relations of z < 0.1 galaxies subdivided by Sérsic index, colour and morphology (2014, background): “…continue to identify a clear disconnect between the M∗−Re relation of nearby galaxies and those at intermediate to high redshift (McIntosh et al. 2005; Trujillo et al. 2007; Buitrago et al. 2008; van der Wel et al. 2008; Damjanov et al. 2009; Williams, Bureau & Cappellari 2010; Bruce et al. 2012).”
The sizes, masses and specific star formation rates of massive galaxies at 1.3 < z < 1.5: strong evidence in favour of evolution via minor mergers (2012, methodology): “Based on the photometric redshift catalogue of Bruce et al. (2012), there are 22 galaxies within the CANDELS/UDS area with Ktot ≤ 21.5 and photometric redshifts in the range 1.3 ≤ z ≤ 1.5.”
A CANDELS–3D-HST SYNERGY: RESOLVED STAR FORMATION PATTERNS AT 0.7 < z < 1.5 (2013, background): “…initial subsets of the CANDELS legacy data set, several works have 2 contrasted monochromatic structural measurements to galaxy-integrated stellar population properties (Wuyts et al. 2011b; Szomoru et al. 2011; Bell et al. 2012; Wang et al. 2012; Kartaltepe et al. 2012; Bruce et al. 2012).”
Introducing the Illustris Project: the evolution of galaxy populations across cosmic time (2014, background): “Such correlations are found at all redshifts where data are available, z 3; however, they are complicated, include significant scatter, and not yet satisfactorily understood (Mignoli et al. 2009; Mendez et al. 2011; Bruce et al. 2012; Kaviraj et al. 2013; Talia et al. 2014).”
Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies (2015, background): “This is consistent with SFGs having more settled, disk-like morphologies, larger sizes, and progressively denser cores (see also, Bruce et al. 2012; Lang et al. 2014; Tacchella et al. 2015).”
BULGE GROWTH AND QUENCHING SINCE z = 2.5 IN CANDELS/3D-HST (2014, methodology): “Additionally, Bruce et al. (2012) show that the majority of star-forming galaxies have disk-dominated light profiles and passive galaxies have bulge-dominated profiles directly from decomposed bulge+disk light-profile fitting of M > 1011M⊙ galaxies at 1 < z < 3.”
3D-HST+CANDELS: THE EVOLUTION OF THE GALAXY SIZE–MASS DISTRIBUTION SINCE z = 3 (2014, unknown): “…and is arguably required to explain, the disappearance from z ∼ 2 to the present of disk-like structures among L ∗ early types (van der Wel et al. 2011; Bruce et al. 2012; Chang et al. 2013), and the observation that the most massive galaxies in the present-day universe do not have a disk-like…”