Abstract
We present subkiloparsec-scale mapping of the 870 μm ALMA continuum emission in six luminous (L IR ∼ 5 ×1012 L o) submillimeter galaxies (SMGs) from the ALESS survey of the Extended Chandra Deep Field South. Our high-fidelity 0.″07-resolution imaging (∼500 pc) reveals robust evidence for structures with deconvolved sizes of ≲0.5-1 kpc embedded within (dominant) exponential dust disks. The large-scale morphologies of the structures within some of the galaxies show clear curvature and/or clump-like structures bracketing elongated nuclear emission, suggestive of bars, star-forming rings, and spiral arms. In this interpretation, the ratio of the "ring" and "bar" radii (1.9 ±;0.3) agrees with that measured for such features in local galaxies. These potential spiral/ring/bar structures would be consistent with the idea of tidal disturbances, with their detailed properties implying flat inner rotation curves and Toomre-unstable disks (Q < 1). The inferred one-dimensional velocity dispersions (σ r ≲ 70-160 km s-1) are marginally consistent with the limits implied if the sizes of the largest structures are comparable to the Jeans length. We create maps of the star formation rate density (ΣSFR) on ∼500 pc scales and show that the SMGs are able to sustain a given (galaxy-averaged) ΣSFR over much larger physical scales than local (ultra)luminous infrared galaxies. However, on 500 pc scales, they do not exceed the Eddington limit set by radiation pressure on dust. If confirmed by kinematics, the potential presence of nonaxisymmetric structures would provide a means for net angular momentum loss and efficient star formation, helping to explain the very high star formation rates measured in SMGs.
| Original language | English (US) |
|---|---|
| Article number | 130 |
| Journal | Astrophysical Journal |
| Volume | 876 |
| Issue number | 2 |
| DOIs | |
| State | Published - May 10 2019 |
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
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ALMA Reveals Potential Evidence for Spiral Arms, Bars, and Rings in High-redshift Submillimeter Galaxies. / Hodge, J. A.; Smail, I.; Walter, F.; Cunha, E. Da; Swinbank, A. M.; Rybak, M.; Venemans, B.; Brandt, W. N.; Rivera, G. Calistro; Chapman, S. C.; Chen, Chian Chou; Cox, P.; Dannerbauer, H.; Decarli, R.; Greve, T. R.; Knudsen, K. K.; Menten, K. M.; Schinnerer, E.; Simpson, J. M.; Werf, P. Van Der; Wardlow, J. L.; Weiss, A.
In: Astrophysical Journal, Vol. 876, No. 2, 130, 10.05.2019.Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - ALMA Reveals Potential Evidence for Spiral Arms, Bars, and Rings in High-redshift Submillimeter Galaxies
AU - Hodge, J. A.
AU - Smail, I.
AU - Walter, F.
AU - Cunha, E. Da
AU - Swinbank, A. M.
AU - Rybak, M.
AU - Venemans, B.
AU - Brandt, W. N.
AU - Rivera, G. Calistro
AU - Chapman, S. C.
AU - Chen, Chian Chou
AU - Cox, P.
AU - Dannerbauer, H.
AU - Decarli, R.
AU - Greve, T. R.
AU - Knudsen, K. K.
AU - Menten, K. M.
AU - Schinnerer, E.
AU - Simpson, J. M.
AU - Werf, P. Van Der
AU - Wardlow, J. L.
AU - Weiss, A.
N1 - Funding Information: J. A. Hodge I. Smail F. Walter E. da Cunha A. M. Swinbank M. Rybak B. Venemans W. N. Brandt G. Calistro Rivera S. C. Chapman Chian-Chou Chen P. Cox H. Dannerbauer R. Decarli T. R. Greve K. K. Knudsen K. M. Menten E. Schinnerer J. M. Simpson P. van der Werf J. L. Wardlow A. Weiss J. A. Hodge I. Smail F. Walter E. da Cunha A. M. Swinbank M. Rybak B. Venemans W. N. Brandt G. Calistro Rivera S. C. Chapman Chian-Chou Chen P. Cox H. Dannerbauer R. Decarli T. R. Greve K. K. Knudsen K. M. Menten E. Schinnerer J. M. Simpson P. van der Werf J. L. Wardlow A. Weiss Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden, The Netherlands Centre for Extragalactic Astronomy, Department of Physics, Durham University, South Road, Durham, DH1 3LE, UK Institute for Computational Cosmology, Durham University, South Road, Durham, DH1 3LE, UK Max–Planck Institut f�r Astronomie, K�nigstuhl 17, D-69117 Heidelberg, Germany Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia Department of Astronomy & Astrophysics, 525 Davey Lab, The Pennsylvania State University, University Park, PA 16802, USA Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA Department of Physics, 104 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA Department of Physics and Atmospheric Science, Dalhousie University, 6310 Coburg Road, Halifax, NS B3H 4R2, Canada European Southern Observatory, Karl Schwarzschild Stra�e 2, Garching, Germany Institut d’Astrophysique de Paris, CNRS, UMR 7095, 98bis boulevard Arago, F-75014, Paris, France Instituto de Astrof�sica de Canarias, V�a L�ctea s/n, E-38205, La Laguna, Tenerife, Spain Universidad de La Laguna, Dpto. Astrofsica, E-38206 La Laguna, Tenerife, Spain INAF/Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via Gobetti 93/3, I-40129 Bologna, Italy Cosmic Dawn Center (DAWN), DTU-Space, Technical University of Denmark, Elektrovej 327, DK-2800 Kgs. Lyngby, Denmark Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen �, Denmark University College London, Department of Physics & Astronomy, Gower Street, London, WC1E 6BT, UK Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, SE-43992 Onsala, Sweden Max-Planck Institut f�r Radioastronomie, Auf dem H�gel 69, D-53121 Bonn, Germany Academia Sinica Institute of Astronomy and Astrophysics, No. 1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan Physics Department, Lancaster University, Lancaster, LA1 4 YB, UK J. A. Hodge, I. Smail, F. Walter, E. da Cunha, A. M. Swinbank, M. Rybak, B. Venemans, W. N. Brandt, G. Calistro Rivera, S. C. Chapman, Chian-Chou Chen, P. Cox, H. Dannerbauer, R. Decarli, T. R. Greve, K. K. Knudsen, K. M. Menten, E. Schinnerer, J. M. Simpson, P. van der Werf, J. L. Wardlow and A. Weiss 2019-05-10 2019-05-13 09:44:45 cgi/release: Article released bin/incoming: New from .zip yes We present subkiloparsec-scale mapping of the 870 μ m ALMA continuum emission in six luminous ( L IR ∼ 5�נ10 12 L ⊙ ) submillimeter galaxies (SMGs) from the ALESS survey of the Extended Chandra Deep Field South. Our high-fidelity 0.″07-resolution imaging (∼500 pc) reveals robust evidence for structures with deconvolved sizes of ≲0.5–1 kpc embedded within (dominant) exponential dust disks. The large-scale morphologies of the structures within some of the galaxies show clear curvature and/or clump-like structures bracketing elongated nuclear emission, suggestive of bars, star-forming rings, and spiral arms. In this interpretation, the ratio of the “ring” and “bar” radii (1.9���0.3) agrees with that measured for such features in local galaxies. These potential spiral/ring/bar structures would be consistent with the idea of tidal disturbances, with their detailed properties implying flat inner rotation curves and Toomre-unstable disks ( Q < 1). The inferred one-dimensional velocity dispersions ( σ r �≲�70–160 km s −1 ) are marginally consistent with the limits implied if the sizes of the largest structures are comparable to the Jeans length. We create maps of the star formation rate density (Σ SFR ) on ∼500 pc scales and show that the SMGs are able to sustain a given (galaxy-averaged) Σ SFR over much larger physical scales than local (ultra)luminous infrared galaxies. However, on 500 pc scales, they do not exceed the Eddington limit set by radiation pressure on dust. 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PY - 2019/5/10
Y1 - 2019/5/10
N2 - We present subkiloparsec-scale mapping of the 870 μm ALMA continuum emission in six luminous (L IR ∼ 5 ×1012 L o) submillimeter galaxies (SMGs) from the ALESS survey of the Extended Chandra Deep Field South. Our high-fidelity 0.″07-resolution imaging (∼500 pc) reveals robust evidence for structures with deconvolved sizes of ≲0.5-1 kpc embedded within (dominant) exponential dust disks. The large-scale morphologies of the structures within some of the galaxies show clear curvature and/or clump-like structures bracketing elongated nuclear emission, suggestive of bars, star-forming rings, and spiral arms. In this interpretation, the ratio of the "ring" and "bar" radii (1.9 ±;0.3) agrees with that measured for such features in local galaxies. These potential spiral/ring/bar structures would be consistent with the idea of tidal disturbances, with their detailed properties implying flat inner rotation curves and Toomre-unstable disks (Q < 1). The inferred one-dimensional velocity dispersions (σ r ≲ 70-160 km s-1) are marginally consistent with the limits implied if the sizes of the largest structures are comparable to the Jeans length. We create maps of the star formation rate density (ΣSFR) on ∼500 pc scales and show that the SMGs are able to sustain a given (galaxy-averaged) ΣSFR over much larger physical scales than local (ultra)luminous infrared galaxies. However, on 500 pc scales, they do not exceed the Eddington limit set by radiation pressure on dust. If confirmed by kinematics, the potential presence of nonaxisymmetric structures would provide a means for net angular momentum loss and efficient star formation, helping to explain the very high star formation rates measured in SMGs.
AB - We present subkiloparsec-scale mapping of the 870 μm ALMA continuum emission in six luminous (L IR ∼ 5 ×1012 L o) submillimeter galaxies (SMGs) from the ALESS survey of the Extended Chandra Deep Field South. Our high-fidelity 0.″07-resolution imaging (∼500 pc) reveals robust evidence for structures with deconvolved sizes of ≲0.5-1 kpc embedded within (dominant) exponential dust disks. The large-scale morphologies of the structures within some of the galaxies show clear curvature and/or clump-like structures bracketing elongated nuclear emission, suggestive of bars, star-forming rings, and spiral arms. In this interpretation, the ratio of the "ring" and "bar" radii (1.9 ±;0.3) agrees with that measured for such features in local galaxies. These potential spiral/ring/bar structures would be consistent with the idea of tidal disturbances, with their detailed properties implying flat inner rotation curves and Toomre-unstable disks (Q < 1). The inferred one-dimensional velocity dispersions (σ r ≲ 70-160 km s-1) are marginally consistent with the limits implied if the sizes of the largest structures are comparable to the Jeans length. We create maps of the star formation rate density (ΣSFR) on ∼500 pc scales and show that the SMGs are able to sustain a given (galaxy-averaged) ΣSFR over much larger physical scales than local (ultra)luminous infrared galaxies. However, on 500 pc scales, they do not exceed the Eddington limit set by radiation pressure on dust. If confirmed by kinematics, the potential presence of nonaxisymmetric structures would provide a means for net angular momentum loss and efficient star formation, helping to explain the very high star formation rates measured in SMGs.
UR - http://www.scopus.com/inward/record.url?scp=85067290254&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85067290254&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ab1846
DO - 10.3847/1538-4357/ab1846
M3 - Article
AN - SCOPUS:85067290254
VL - 876
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 130
ER -