A Caltech Library Service

Multi-Filament Inflows Fueling Young Star Forming Galaxies

Martin, D. Christopher and O'Sullivan, Donal and Matuszweski, Mateusz and Hamden, Erika and Dekel, Avishai and Lapiner, Sharon and Morrissey, Patrick and Neill, James D. and Cantalupo, Sebastiano and Prochaska, J. Xavier and Steidel, Charles and Trainor, Ryan and Moore, Anna and Ceverino, Daniel and Primack, Joel and Rizzi, Luca (2019) Multi-Filament Inflows Fueling Young Star Forming Galaxies. . (Unpublished)

[img] PDF - Submitted Version
See Usage Policy.


Use this Persistent URL to link to this item:


Theory suggests that there are two primary modes of accretion through which dark matter halos acquire the gas to form and fuel galaxies, hot and cold mode accretion. In cold mode accretion, gas streams along cosmic web filaments to the center of the halo, allowing for the efficient delivery of star-forming fuel. Recently, two QSO-illuminated HI Lyman alpha (Ly{\alpha}) emitting objects were reported to have properties of cold, rotating structures (Martin et al. 2015, Martin et al. 2016). However, the spatial and spectral resolution available was insufficient to constrain radial flows associated with connecting filaments. With the Keck Cosmic Web Imager (KCWI) we now have eight times the spatial resolution, permitting the detection of these in-spiraling flows. In order to detect these inflows, we introduce a suite of models which incorporate zonal radial flows, demonstrate their performance on a numerical simulation that exhibits coldflow accretion, and show that they are an excellent match to KCWI velocity maps of two Ly{\alpha} emitters observed around high-redshift quasars. These Multi-Filament Inflow models kinematically isolate zones of radial inflow that correspond to extended filamentary emission. The derived gas flux and inflow path is sufficient to fuel the inferred central galaxy star formation rate and angular momentum. Thus, our kinematic emission maps provide strong evidence for the inflow of gas from the cosmic web building galaxies at the peak of star formation.

Item Type:Report or Paper (Discussion Paper)
Related URLs:
URLURL TypeDescription Paper
Martin, D. Christopher0000-0002-8650-1644
O'Sullivan, Donal0000-0002-4959-9179
Hamden, Erika0000-0002-3131-7372
Dekel, Avishai0000-0003-4174-0374
Morrissey, Patrick0000-0001-8177-1023
Neill, James D.0000-0002-0466-1119
Cantalupo, Sebastiano0000-0001-5804-1428
Prochaska, J. Xavier0000-0002-7738-6875
Steidel, Charles0000-0002-4834-7260
Trainor, Ryan0000-0002-6967-7322
Moore, Anna0000-0002-2894-6936
Ceverino, Daniel0000-0002-8680-248X
Primack, Joel0000-0001-5091-5098
Rizzi, Luca0000-0003-0882-2327
Additional Information:This work was supported by the National Science Foundation, the W. M Keck Observatory and the California Institute of Technology. The VELA simulations were performed at NASA Advanced Supercomputing (NAS) at NASA Ames Research Center. D.C. is funded by the ERC Advanced Grant, STARLIGHT: Formation of the First Stars (project number 339177). Author Contributions: D.C.M. is the Principal Investigator of KCWI, performed the analysis of the simulated galaxy, data and MFI models, and was principal author on the paper. D.O. and D.C.M led the observations of UM287 and CSO 38. D.O., M.M. reduced the data. D. O., M. M., and E. H. contributed to the paper writing. P.M., M.M., D.C.M., D.N., D.O., and A.M. designed, constructed, and operated KCWI. D.N., M.M. and D.C.M. developed the KCWI data pipeline and produced the final data cubes. D. C. developed the VELA simulations. A.D. and S. L. provided the simulated galaxy VELA07 and contributed to the paper. D.C. and J.P. contributed the cosmological simulation. C.S, R.T., S.C., and J.X.P. contributed to the development of KCWI, Keck data for the two protogalaxies, and to the editing of the paper. L. R. made major contributions to KCWI commissioning and participated in the observations of CSO 38. Code and Data Availability: KCWI pipeline code is available on the W. M. Keck Observatory website. KCWI data on CSO38 and UM287 is publically available. Data on UM287 will be available 18 months after the observation in Oct 2017. The data that support the plots within this paper and other findings of this study are available from the corresponding author upon reasonable request.
Group:Space Radiation Laboratory, Astronomy Department
Funding AgencyGrant Number
W. M. Keck ObservatoryUNSPECIFIED
European Research Council (ERC)339177
Record Number:CaltechAUTHORS:20191218-101527501
Persistent URL:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:100345
Deposited By: Tony Diaz
Deposited On:18 Dec 2019 18:27
Last Modified:02 Jun 2023 00:57

Repository Staff Only: item control page