E
E. K. S. Hicks
Researcher at University of Alaska Anchorage
Publications - 31
Citations - 1734
E. K. S. Hicks is an academic researcher from University of Alaska Anchorage. The author has contributed to research in topics: Galaxy & Active galactic nucleus. The author has an hindex of 17, co-authored 31 publications receiving 1460 citations. Previous affiliations of E. K. S. Hicks include University of Florence.
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Journal ArticleDOI
The SINS/zC-SINF survey of z~2 galaxy kinematics: Evidence for powerful AGN-driven nuclear outflows in massive star-forming galaxies
N. M. Förster Schreiber,Reinhard Genzel,S. Newman,J. D. Kurk,Dieter Lutz,Linda J. Tacconi,Stijn Wuyts,K. Bandara,A. Burkert,Peter Buschkamp,C. M. Carollo,Giovanni Cresci,E. Daddi,R. D. Davies,Frank Eisenhauer,E. K. S. Hicks,Philipp Lang,S. J. Lilly,Vincenzo Mainieri,Chiara Mancini,T. Naab,Y. Peng,Alvio Renzini,David J. Rosario,K. Shapiro Griffin,Alice E. Shapley,Amiel Sternberg,Sandro Tacchella,D. Vergani,Emily Wisnioski,E. Wuyts,G. Zamorani +31 more
TL;DR: In this paper, the authors reported the detection of ubiquitous powerful nuclear outflows in massive (> 10^11 Msun) z~2 star-forming galaxies (SFGs), which are plausibly driven by an Active Galactic Nucleus (AGN).
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Mergers and Mass Accretion Rates in Galaxy Assembly: The Millennium Simulation Compared to Observations of z~2 Galaxies
Shy Genel,Reinhard Genzel,Nicolas Bouché,Amiel Sternberg,T. Naab,N. M. Förster Schreiber,K. Shapiro,Linda J. Tacconi,Dieter Lutz,Giovanni Cresci,Peter Buschkamp,Ric Davies,E. K. S. Hicks +12 more
TL;DR: In this paper, the authors use the Millennium Simulation to build new halo merger trees and extract halo merge fractions and mass accretion rates, and show that even for halos not undergoing major mergers, mass accuration rates are plausibly sufficient to account for the high star formation rates observed in z~2 disks.
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Molecular gas streamers feeding and obscuring the active nucleus of NGC1068
F. Mueller Sanchez,Ric Davies,R. Genzel,Linda J. Tacconi,Frank Eisenhauer,E. K. S. Hicks,S. Friedrich,Amiel Sternberg +7 more
TL;DR: The first direct observations of neutral, molecular gas streaming in the nucleus of NGC1068 on scales of <30 pc using SINFONI near-infrared integral field spectroscopy were reported in this article.
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High-Redshift Star-Forming Galaxies: Angular Momentum and Baryon Fraction, Turbulent Pressure Effects and the Origin of Turbulence
Andreas Burkert,Reinhard Genzel,Nicolas Bouché,Giovanni Cresci,Sadegh Khochfar,Jesper Sommer-Larsen,Amiel Sternberg,T. Naab,N. Foerster-Schreiber,Linda J. Tacconi,K. Shapiro,E. K. S. Hicks,Dieter Lutz,R. D. Davies,Peter Buschkamp,Shy Genel +15 more
Abstract: The structure of a sample of high-redshift (z=2), rotating galaxies with high star formation rates and turbulent gas velocities of sigma=40-80 km/s is investigated. Fitting the observed disk rotational velocities and radii with a Mo, Mao, White (1998) (MMW) model requires unusually large disk spin parameters lambda_d>0.1 and disk-to-dark halo mass fraction m_d=0.2, close to the cosmic baryon fraction. The galaxies segregate into dispersion-dominated systems with 1 200 km/s, vmax/sigma>3 and rd=4-8 kpc. For the dispersion-dominated sample, radial pressure gradients partly compensate the gravitational force, reducing the rotational velocities. Including this pressure effect in the MMW model, dispersion-dominated galaxies can be fitted well with spin parameters lf lambda_d=0.03-0.05 for high disk mass fractions of m_d=0.2 and with lambda_d=0.01-0.03 for m_d=0.05. These values are in good agreement with cosmological expectations. For the rotation-dominated sample however pressure effects are small and better agreement with theoretically expected disk spin parameters can only be achieved if the dark halo mass contribution in the visible disk regime (2-3*rd) is smaller than predicted by the MMW model. We argue that these galaxies can still be embedded in standard cold dark matter halos if the halos did not contract adiabatically in response to disk formation. It is shown that the observed high turbulent gas motions of the galaxies are consistent with a Toomre instability parameter Q=1 which is equal to the critical value, expected for gravitational disk instability to be the major driver of turbulence. The dominant energy source of turbulence is then the potential energy of the gas in the disk.
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Stellar and Molecular Gas Kinematics of NGC1097: Inflow Driven by a Nuclear Spiral
TL;DR: In this article, the authors present spatially resolved distributions and kinematics of the stars and molecular gas in the central 320pc of NGC1097, and estimate the inflow rate along the arms.