Renyue Cen

Zhejiang University

Author Statistics

Papers

Citation

H-Index

i-10 index

Research Trends

Author Order

Document Type

Co-Authors

Jeremiah P. Ostriker

Princeton University

116

Hy Trac

Carnegie Mellon University

Jordi Miralda‐Escudé

Institució Catalana de Recerca i Estudis Avançats

Kentaro Nagamine

University of Nevada, Las Vegas

Neta A. Bahcall

Princeton University

Zheng Zheng

University of Utah

Greg L. Bryan

Columbia University

Asantha Cooray

University of California, Irvine

Zoltán Haiman

Columbia University

Lars Hernquist

Center for Astrophysics Harvard & Smithsonian

Cooperative Institutions

California Institute of Technology

104

Princeton University

Centre National de la Recherche Scientifique

Max Planck Society

Center for Astrophysics Harvard & Smithsonian

The University of Tokyo

University of California, Berkeley

Max Planck Institute for Astronomy

Chinese Academy of Sciences

Johns Hopkins University

Author Statistics

Papers

Citation

H-Index

i-10 index

Research Field

On the Clustering of Lyα Clouds, High‐Redshift Galaxies, and Underlying Mass

The Astrophysical Journal (1998)

Renyue Cen Steven Phelps Jordi Miralda‐Escudé Jeremiah P. Ostriker

We examine the correlation property of Lyα forest (along the line of sight) utilizing a hydrodynamic simulation of Lyα clouds in a cold dark matter universe with a cosmological constant, and compare it to the correlation of underlying mass and galaxies. A consistent picture seems to emerge: the correlation strength for a given set of objects is positively correlated with their characteristic global density and the differences among the correlations of galaxies, Lyα clouds, and mass reflect the differences in density that each trace. We find that the galaxies are strongly biased (nearly independent of scales) over mass by a factor of ~3.0, in accord with recent observations of high-redshift galaxies. The correlation strength of Lyα clouds with column densities of 1013-1014 cm-2 is comparable to that of total mass. Positive correlations with a strength of 0.1-1.0 are found for Lyα clouds in the velocity range 50-300 km s-1. The correlation is less than 0.3 at Δv > 300 km s-1, but here our simulated box is too small to give a reliable measure.

Line-of-sight

10.1086/305418

Cite

Citations (35)

A Critical Test of Topological Defect Models: Spatial Clustering of Clusters of Galaxies

The Astrophysical Journal (1997)

Renyue Cen

Gaussian cosmological models, typified by the inflationary cold dark matter models, and non-Gaussian topological defect-based cosmological models such as the texture-seeded model, differ regarding the origin of large-scale cosmic structures. In the former it is believed that high peaks at appropriate scales in the initial density field are the sites onto which matter accretes and collapses to form galaxies and clusters of galaxies, whereas in the latter these structures form around the density perturbation seeds (which are textures in the texture model). Textures initially are randomly distributed on scales larger than their size, in sharp contrast to the initial high-density peaks in the Gaussian models, which are already strongly clustered before any gravitational evolution has occurred. One thus expects that the resultant correlation of large cosmic objects such as clusters of galaxies in the texture model should be significantly weaker than its Gaussian counterpart.

Topological defect

Texture (cosmology)

Cold dark matter

10.1086/304954

Cite

Citations (4)

Constraining Reionization with the Evolution of the Luminosity Function of Lyα Emitting Galaxies

The Astrophysical Journal (2005)

Zoltán Haiman Renyue Cen

At redshifts beyond z ≳ 6, as the mean fraction of neutral hydrogen ⟨xH i⟩ in the intergalactic medium (IGM) increases, the line flux of Lyα emitters can be significantly attenuated, which can result in a decrease in the observed number of emitters at a given Lyα flux. However, cosmological H II regions surrounding the Lyα emitting galaxies alleviate these effects. We use simple models of the Lyα line attenuation that incorporate the presence of H II regions to predict the overall effect of the Lyα absorption on the Lyα luminosity function (LF). We find, in agreement with other recent studies, that a fully neutral IGM is inconsistent with the Lyα LF remaining unchanged from z = 5.7 to z = 6.5, as suggested by recent observations. However, the presence of local H II regions prohibits placing a tight constraint on the mean neutral fraction. We find ⟨x⟩ ≲ 0.25; the presence of strong winds and/or the clustering of ionizing sources would further weaken this constraint. We conclude that the evolution of the Lyα LF is consistent with reionization occurring near this redshift, as suggested by other observations. Finally, we suggest that a measurement of observed Lyα line width as a function of the Lyα luminosity, in a future, larger sample of Lyα emitters, may serve as a robust diagnostic of the neutral fraction in the IGM.

Line (geometry)

Equivalent width

10.1086/428645

Cite

Citations (77)

The BUFFALO HST Survey

The Astrophysical Journal Supplement Series (2020)

Charles L. Steinhardt Mathilde Jauzac Ana Acebrón Hakim Atek P. Capak

The Beyond Ultra-deep Frontier Fields and Legacy Observations (BUFFALO) is a 101 orbit + 101 parallel Cycle 25 Hubble Space Telescope Treasury program taking data from 2018-2020. BUFFALO will expand existing coverage of the Hubble Frontier Fields (HFF) in WFC3/IR F105W, F125W, and F160W and ACS/WFC F606W and F814W around each of the six HFF clusters and flanking fields. This additional area has not been observed by HST but is already covered by deep multi-wavelength datasets, including Spitzer and Chandra. As with the original HFF program, BUFFALO is designed to take advantage of gravitational lensing from massive clusters to simultaneously find high-redshift galaxies which would otherwise lie below HST detection limits and model foreground clusters to study properties of dark matter and galaxy assembly. The expanded area will provide a first opportunity to study both cosmic variance at high redshift and galaxy assembly in the outskirts of the large HFF clusters. Five additional orbits are reserved for transient followup. BUFFALO data including mosaics, value-added catalogs and cluster mass distribution models will be released via MAST on a regular basis, as the observations and analysis are completed for the six individual clusters.

Cosmic variance

10.3847/1538-4365/ab75ed

Cite

Citations (76)

The Topology of Cosmological Reionization

The Astrophysical Journal (2008)

Khee‐Gan Lee Renyue Cen J. Richard Gott Hy Trac

Using the largest cosmological reionization simulation to date (~24 billion particles), we use the genus curve to quantify the topology of the neutral hydrogen distribution on scales ≥1 Mpc h−1 as it evolves during cosmological reionization. We find that the reionization process proceeds primarily in an inside-out fashion, in which higher density regions become ionized earlier than lower density regions. There are four distinct topological phases: (1) pre-reionization at z≳ 15, when the genus curve is consistent with a Gaussian density distribution; (2) preoverlap at 10≲ z≲ 15, during which the number of H II bubbles increases gradually with time, until percolation of H II bubbles starts to take effect (this phase is characterized by a very flat genus curve at high volume fractions); (3) overlap at 8≲ z≲ 10, when large H II bubbles rapidly merge, manifested by a precipitous drop in the amplitude of the genus curve; and (4) postoverlap at 6≲ z≲ 8, when H II bubbles have mostly overlapped, and the genus curve is consistent with a diminishing number of isolated neutral islands. After the end of reionization (z≲ 6), the genus of neutral hydrogen is consistent with Gaussian random phase, in agreement with observations.

Cold dark matter

10.1086/525520

Cite

Citations (36)

FREQUENT SPIN REORIENTATION OF GALAXIES DUE TO LOCAL INTERACTIONS

The Astrophysical Journal Letters (2014)

Renyue Cen

We study the evolution of angular momenta of ($M_*=10^{10}-10^{12}\msun$) galaxies utilizing large-scale ultra-high resolution cosmological hydrodynamic simulations and find that spin of the stellar component changes direction frequently, caused by major mergers, minor mergers, significant gas inflows and torques by nearby systems. The rate and nature of change of spin direction can not be accounted for by large-scale tidal torques, because the latter fall short in rates by orders of magnitude and because the apparent random swings of the spin direction are inconsistent with alignment by linear density field. The implications for galaxy formation as well as intrinsic alignment of galaxies are profound. Assuming the large-scale tidal field is the sole alignment agent, a new picture emerging is that intrinsic alignment of galaxies would be a balance between slow large-scale coherent torquing and fast spin reorientation by local interactions. What is still open is whether other processes, such as feeding galaxies with gas and stars along filaments or sheets, introduce coherence for spin directions of galaxies along the respective structures.

Peculiar galaxy

10.1088/2041-8205/785/1/l15

Cite

Citations (12)

Steps toward the Power Spectrum of Matter. III. The Primordial Spectrum

The Astrophysical Journal (1999)

J. Einasto M. Einasto E. Tago Alexei A. Starobinsky F. Atrio‐Barandela

We compare the observed power spectrum of matter found in our earlier papers with analytical power spectra. We extrapolate the observed power spectra on small scales to find the linear power spectrum of matter. We consider spatially flat cold and mixed dark matter models with the cosmological constant as well as open models. We fix the Hubble constant and the baryon density in the middle of the allowed range and vary the density parameter and the cosmological constant. We determine the primordial power spectrum of matter using the power spectrum of matter and the transfer functions of analytical models. We take two different spectra suggested by observations: one with a sharp maximum at 120 h-1 Mpc and a second one with a broader maximum, as found for regions with rich and medium-rich superclusters of galaxies, respectively. For both models, the primordial power spectra have a break in amplitude; in the case of the spectrum with a sharp maximum the break is sharp. We conclude that a scale-free primordial power spectrum is excluded if presently available data on the distribution of clusters and galaxies represent the true mass distribution of the universe.

Matter power spectrum

Cold dark matter

Mass distribution

10.1086/307386

Cite

Citations (8)

Dependence of Star Formation Rate on Overdensity

arXiv (Cornell University) (1999)

Kentaro Nagamine Renyue Cen Jeremiah P. Ostriker

We use a large-scale Lambda-CDM hydrodynamical simulation to assess the dependence of the cosmic Star Formation Rate (SFR) on overdensity of luminosity. The `morphology-density relation' is qualitatively captured when the SFR is plotted as a function of redshift, divided into the quartiles of the overdensity distribution.

Star (game theory)

Quartile

10.48550/arxiv.astro-ph/9912023

Cite

Citations (0)

Testing Cosmological Models by Gravitational Lensing. I. Method and First Applications

The Astrophysical Journal (1998)

J. Wambsganß Renyue Cen Jeremiah P. Ostriker

Gravitational lensing directly measures mass density fluctuations along the lines of sight to very distant objects. No assumptions need to be made concerning bias, the ratio of fluctuations in galaxy density to mass density. Hence, lensing is a very useful tool for studying the universe at low to moderate redshifts.

Strong gravitational lensing

Gravitational lensing formalism

10.1086/305174

Cite

Citations (96)

Detecting Preheating in Protoclusters with Lyα Forest Tomography

The Astrophysical Journal (2022)

Robin Kooistra Shigeki Inoue Khee‐Gan Lee Renyue Cen Naoki Yoshida

Studies of low redshift galaxy clusters suggest the intra-cluster medium (ICM) has experienced non-gravitational heating during the formation phase of the clusters. Using simple phenomenological heating prescriptions, we simulate the effect of this preheating of the nascent ICM in galaxy proto-clusters and examine its effect on Lyman-$\alpha$ (Ly$\alpha$) forest tomographic maps. We analyse a series of cosmological zoom-in simulations of proto-clusters within the framework of the Ly$\alpha$ transmission-dark matter (DM) density distribution. We find that the more energy is injected into the proto-ICM at $z$ = 3, the more the distribution at high DM density tilts towards higher Ly$\alpha$ transmission. This effect has been confirmed in both low-resolution simulations adopting a preheating scheme based on entropy floors, as well as in higher-resolution simulations with another scheme based on energy floors. The evolution of the slope of this distribution is shown to vary with redshift. The methodology developed here can be applied to current and upcoming Ly$\alpha$ forest tomographic survey data to help constrain feedback models in galaxy proto-clusters.

10.3847/1538-4357/ac4cb1

Cite

Citations (7)