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A Giant Protogalactic Disk Linked to the Cosmic Web

Martin, D. Christopher and Matuszewski, Mateusz and Morrissey, Patrick and Neill, James D. and Moore, Anna and Cantalupo, Sebastiano and Prochaska, J. Xavier and Chang, Daphne (2015) A Giant Protogalactic Disk Linked to the Cosmic Web. Nature, 524 (7564). pp. 192-195. ISSN 0028-0836. doi:10.1038/nature14616.

[img] Image (JPEG) (Extended Data Figure 1: Illustration of raw and conventionally smoothed data) - Supplemental Material
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[img] Image (JPEG) (Extended Data Figure 2: Channel maps of the UM287 data cube) - Supplemental Material
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[img] Image (JPEG) (Extended Data Figure 3: Comparison of PCWI data and Keck narrow-band and continuum images) - Supplemental Material
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[img] Image (JPEG) (Extended Data Figure 4: Channel maps of the UM287 data cube) - Supplemental Material
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[img] Image (JPEG) (Extended Data Figure 5: Channel maps of the UM287 data cube) - Supplemental Material
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[img] Image (JPEG) (Extended Data Figure 6: Spectral image and rectangular pseudo-slit slices of the UM287 data cube) - Supplemental Material
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The specifics of how galaxies form from, and are fuelled by, gas from the intergalactic medium remain uncertain. Hydrodynamic simulations suggest that ‘cold accretion flows’—relatively cool (temperatures of the order of 10^4 kelvin), unshocked gas streaming along filaments of the cosmic web into dark-matter halos—are important. These flows are thought to deposit gas and angular momentum into the circumgalactic medium, creating disk- or ring-like structures that eventually coalesce into galaxies that form at filamentary intersections. Recently, a large and luminous filament, consistent with such a cold accretion flow, was discovered near the quasi-stellar object QSO UM287 at redshift 2.279 using narrow-band imaging. Unfortunately, imaging is not sufficient to constrain the physical characteristics of the filament, to determine its kinematics, to explain how it is linked to nearby sources, or to account for its unusual brightness, more than a factor of ten above what is expected for a filament. Here we report a two-dimensional spectroscopic investigation of the emitting structure. We find that the brightest emission region is an extended rotating hydrogen disk with a velocity profile that is characteristic of gas in a dark-matter halo with a mass of 10^(13) solar masses. This giant protogalactic disk appears to be connected to a quiescent filament that may extend beyond the virial radius of the halo. The geometry is strongly suggestive of a cold accretion flow.

Item Type:Article
Related URLs:
URLURL TypeDescription ReadCube access
Martin, D. Christopher0000-0002-8650-1644
Morrissey, Patrick0000-0001-8177-1023
Neill, James D.0000-0002-0466-1119
Moore, Anna0000-0002-2894-6936
Cantalupo, Sebastiano0000-0001-5804-1428
Prochaska, J. Xavier0000-0002-7738-6875
Additional Information:© 2015 Macmillan Publishers Limited. Received 18 February; accepted 21 May 2015. Published online 5 August 2015. We thank T. Tombrello and S. Kulkarni for their support of PCWI. This work was supported by the National Science Foundation and the California Institute of Technology. Contributions: D.C.M. is the principal investigator of PCWI, led the observations and analysis of UM287, and was principal author on the paper. M.M., D.C., and P.M. designed, constructed, and operated PCWI. A.M. was the project and technical manager (2006–2010). J.D.N., M.M., and D.C.M. developed the PCWI/KCWI data pipeline and produced the final data cubes. M.M., P.M., S.C., and J.X.P. contributed Keck data and helped edit the paper. Competing financial interests: The authors declare no competing financial interests.
Group:Space Astrophysics Laboratory
Funding AgencyGrant Number
Issue or Number:7564
Record Number:CaltechAUTHORS:20150520-105840835
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Official Citation:A giant protogalactic disk linked to the cosmic web D. Christopher Martin, Mateusz Matuszewski, Patrick Morrissey, James D. Neill, Anna Moore + et al. Nature 524, 192–195 (13 August 2015) doi:10.1038/nature14616
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:57707
Deposited By: George Porter
Deposited On:05 Aug 2015 21:18
Last Modified:10 Nov 2021 21:54

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