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Cited by 311

The DOI matches its Crossref record; 150 of the 150 references it cites were found in a registry or an index.

FORMING COMPACT MASSIVE GALAXIES

Open access
van Dokkum, Pieter G., Nelson, Erica June, Franx, Marijn, Oesch, Pascal, Momcheva, Ivelina, Brammer, Gabriel, Schreiber, Natascha M. Förster, Skelton, Rosalind E., Whitaker, Katherine E., Wel, Arjen van der, Bezanson, Rachel, Fumagalli, Mattia, Illingworth, Garth D., Kriek, Mariska, Leja, Joel, Wuyts, Stijn·2015·The Astrophysical Journal
DOI 10.1088/0004-637x/813/1/23
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Abstract

In this paper we study a key phase in the formation of massive galaxies: the transition of star-forming galaxies into massive ( M stars ∼ 10 11 M ⊙ ), compact ( r e ∼ 1 kpc) quiescent galaxies, which takes place from z ∼ 3 to z ∼ 1.5. We use HST grism redshifts and extensive photometry in all five 3D- HST /CANDELS fields, more than doubling the area used previously for such studies, and combine these data with Keck MOSFIRE and NIRSPEC spectroscopy. We first confirm that a population of massive, compact, star-forming galaxies exists at z ≳ 2, using K -band spectroscopy of 25 of these objects at 2.0 < z < 2.5. They have a median [N ii ]/H α ratio of 0.6, are highly obscured with SFR(tot)/SFR(H α ) ∼10, and have a large range of observed line widths. We infer from the kinematics and spatial distribution of H α that the galaxies have rotating disks of ionized gas that are a factor of ∼2 more extended than the stellar distribution. By combining measurements of individual galaxies, we find that the kinematics are consistent with a nearly Keplerian fall-off from V rot ∼ 500 km s −1 at 1 kpc to V rot ∼ 250 km s −1 at 7 kpc, and that the total mass out to this radius is dominated by the dense stellar component. Next, we study the size and mass evolution of the progenitors of compact massive galaxies. Even though individual galaxies may have had complex histories with periods of compaction and mergers, we show that the population of progenitors likely followed a simple inside-out growth track in the size–mass plane of This mode of growth gradually increases the stellar mass within a fixed physical radius, and galaxies quench when they reach a stellar density or velocity dispersion threshold. As shown in other studies, the mode of growth changes after quenching, as dry mergers take the galaxies on a relatively steep track in the size–mass plane.

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Metadata

Authors
van Dokkum, P. G., Nelson, E. J., Franx, M., Oesch, P., Momcheva, I., Brammer, G., Schreiber, N. M. F., Skelton, R. E., Whitaker, K. E., Wel, A. V. D., Bezanson, R., Fumagalli, M., Illingworth, G. D., Kriek, M., Leja, J., & Wuyts, S.
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2015-10-22
Volume
813
Issue
1
Pages
23
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
DOI
10.1088/0004-637x/813/1/23
OpenAlex
W1946967981
Cited by
311
References
150
FWCI
17.94
Type
journal article
Language
en
Open access
bronze

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CoChat. (2026). Citation check: FORMING COMPACT MASSIVE GALAXIES. https://app.cochat.ai/papers/10.1088/0004-637x/813/1/23
The paper
van Dokkum, P. G., Nelson, E. J., Franx, M., Oesch, P., Momcheva, I., Brammer, G., Schreiber, N. M. F., Skelton, R. E., Whitaker, K. E., Wel, A. V. D., Bezanson, R., Fumagalli, M., Illingworth, G. D., Kriek, M., Leja, J., & Wuyts, S. (2015). FORMING COMPACT MASSIVE GALAXIES. The Astrophysical Journal. https://doi.org/10.1088/0004-637x/813/1/23

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Contains information from the Semantic Scholar Academic Graph Datasets, made available under the ODC Attribution License (ODC-BY 1.0).

Semantic Scholar’s data is described in: Kinney, R., et al. (2023). The Semantic Scholar Open Data Platform. arXiv:2301.10140.