Query: The modelling and simulation of Bi2Te3 thermoelectric generators in synopsys tcad

Candidate papers:

abstract: This paper demonstrates the modelling and simulation of thermoelectric generators using Synopsys Technology Computer Aided Design (TCAD) semiconductor design and simulation software. A single Bi2Te3 thermoelectric couple, and a seven couple Bi2Te3 thermoelectric module, have been modelled in Synopsys TCAD and simulated for thermoelectric power generation. The simulation results correctly demonstrate that when a thermoelectric couple or module is subjected to a temperature gradient, electrical power is generated at the load, with higher power levels output as the temperature gradient increases, or as the number of thermoelectric couples contained within the device increases. The simulation results obtained in TCAD, which uses in built semiconductor physics equations, have been compared to results obtained through numerical calculation using a different set of thermoelectric equations, and the two results are in close agreement. The Synopsys TCAD models can be developed further to investigate novel device structures, and will enable new thermoelectric materials to be investigated within the framework of the simulation environment in an attempt to improve the performance, efficiency, and cost of thermoelectric devices
author_names: Christopher Gould

Noel Y A Shammas
title: The Modelling and Simulation of Bi2Te3 Thermoelectric Generators in Synopsys TCAD
year: 2015

abstract: A patient specific fluid structure interaction (FSI) model of a phase contrast magnetic resonance angiography (PC MRA) imaged arteriovenous fistula is presented. The numerical model is developed and simulated using a commercial multiphysics simulation package where a semi implicit FSI coupling scheme combines a finite volume method blood flow model and a finite element method vessel wall model. A pulsatile mass flow boundary condition is prescribed at the artery inlet of the model, and a three element Windkessel model at the artery and vein outlets. The FSI model is freely available for analysis and extension. This work shows the effectiveness of combining a number of stabilisation techniques to simultaneously overcome the added mass effect and optimise the efficiency of the overall model. The PC MRA data, fluid model, and FSI model results show almost identical flow features in the fistula; this applies in particular to a flow recirculation region in the vein that could potentially lead to fistula failure.
author_names: Winston Guess

B Dheeraj Reddy

Andrew T McBride

Bruce S Spottiswoode

J Downs

T Franz Centre for Research in Computational

Applied Mechanics

University of Cape Town

South Africa

Department of Electrical Engineering

Faculty of Electrical Engineering

the Environment

South Africa Department of Mathematics

Applied Mathematics

South Africa Infrastructure

School of Electrical Engineering

The University of Glasgow

Scotland Division of Biomedical Engineering

Department of Biology

Faculty of Nuclear Sciences

South Africa Siemens Medical Solutions Usa Inc

Usa Division of General Surgery

Department of Surgery

Groote Schuur Hospital

Cape Town

South Africa Bioengineering Science Research Group

Engineering Sciences

University of Southampton
title: Fluid structure interaction modelling and stabilisation of a patient specific arteriovenous access fistula
year: 2017

abstract: In this letter, we consider the concept of mobile crowd machine learning (MCML) for a federated learning model. The MCML enables mobile devices in a mobile network to collaboratively train neural network models required by a server while keeping data on the mobile devices. The MCML thus addresses data privacy issues of traditional machine learning. However, the mobile devices are constrained by energy, CPU, and wireless bandwidth. Thus, to minimize the energy consumption, training time, and communication cost, the server needs to determine proper amounts of data and energy that the mobile devices use for training. However, under the dynamics and uncertainty of the mobile environment, it is challenging for the server to determine the optimal decisions on mobile device resource management. In this letter, we propose to adopt a deep $Q$ learning algorithm that allows the server to learn and find optimal decisions without any a priori knowledge of network dynamics. Simulation results show that the proposed algorithm outperforms the static algorithms in terms of energy consumption and training latency.
author_names: Tran The Anh

Nguyen Cong Luong

Dusit Tao Niyato

Dong In Kim

Li-Chun Wang
title: Efficient Training Management for Mobile Crowd Machine Learning: A Deep Reinforcement Learning Approach
venue: IEEE Wireless Communications Letters
year: 2019

abstract: We explore the high spectral resolution X ray data towards the quasar 3C273 to search for signals of hot \sim10^{6 7} K) X ray absorbing gas co located with two established intergalactic FUV OVI absorbers. We analyze the soft X ray band grating data of all XMM Newton and Chandra instruments to search for the hot phase absorption lines at the FUV predicted redshifts. The viability of potential line detections is examined by adopting the constraints of a physically justified absorption model. The WHIM hypothesis is investigated with a complementary 3D galaxy distribution analysis, and by comparison of the measurement results to the WHIM properties in the EAGLE cosmological, hydrodynamical simulation. At FUV redshift z=0.09017, we measured signals of two hot ion species, OVIII and NeIX, with a $3.9\sigma$ combined significance level. Considering the line features in all instruments collectively and assuming collisional equilibrium for absorbing gas, we were able to constrain the temperature $kT=0.26\pm0.03$ keV) and the column density $N_H\times{Z_\odot/Z}=1.3_{ 0.5}+0.6}\times10^{19} cm$ 2} of the absorber. Thermal analysis indicates that FUV and X ray absorption relate to different phases, with estimated temperatures $T_{FUV}\approx3\times10^5$ and $T_{X ray}\approx3\times10^6$ K, which match the EAGLE predictions for WHIM at the FUV/X ray measured $N_{ion} ranges. We detected a large scale galactic filament crossing the sightline at the redshift of the absorption, linking the absorption to this structure. This study provides insights into co existing warm and hot gas within a WHIM filament and estimates the ratio of the hot and warm phases. Because the hot phase is thermally distinct from the OVI gas, the estimated baryon content of the absorber is increased, conveying the promise of X ray follow up studies of FUV detected WHIM in refining the picture of the missing baryons.
author_names: Jussi Ahoranta

Jukka Nevalainen

Nastasha A Wijers

Alexis Finoguenov

Massimiliano Bonamente

Elmo Tempel

Evan M Tilton

Joop Schaye

J S Kaastra

Ghassem Gozaliasl Department of Physics

University of Helsinki

Department of Engineering Physics

University of Alabama in Huntsville

Tartu Observatory

University of Tartu

Leiden Observatory

Leiden University

The Netherlands

Nasa National Space Science

Technology Center

Leibniz-Institut fur Astrophysik Potsdam

Deparment of PhysicsAstronomy

Regis University

Sron Netherlands Institute for Space Research

Finnish Magic Consortium Finnish Centre of Astronomy with Eso
title: Hot WHIM counterparts of FUV O VI absorbers: Evidence in the line of sight towards quasar 3C 273
year: 2019

abstract: When monitoring a reactor site for nuclear nonproliferation purposes, the presence of an unknown or hidden nuclear reactor could be obscured by the activities of a known reactor of much greater power nearby. Thus when monitoring reactor activities by the observation of antineutrino emissions, one must discriminate known background reactor fluxes from possible unknown reactor signals under investigation. To quantify this discrimination, we find the confidence to reject the (null) hypothesis of a single proximal reactor, by exploiting directional antineutrino signals in the presence of a second, unknown reactor. In particular, we simulate the inverse beta decay (IBD) response of a detector filled with a 1 kT fiducial mass of Gadolinium doped liquid scintillator in mineral oil. We base the detector geometry on that of WATCHMAN, an upcoming antineutrino monitoring experiment soon to be deployed at the Boulby mine in the United Kingdom whose design and deployment will be detailed in a forthcoming white paper. From this simulation, we construct an analytical model of the IBD event distribution for the case of one $4\mathrm{ GWt}\pm2\ reactor 25 km away from the detector site, and for an additional, unknown, 35 MWt reactor 3 to 5 km away. The effects of natural background rejection cuts are approximated. Applying the model, we predict $3\sigma$ confidence to detect the presence of an unknown reactor within five weeks, at standoffs of 3 km or nearer. For more distant unknown reactors, the $3\sigma$ detection time increases significantly. However, the relative significance of directional sensitivity also increases, providing up to an eight week speedup to detect an unknown reactor at 5 km away. Therefore, directionally sensitive antineutrino monitoring can accelerate the mid field detection of unknown reactors whose operation might otherwise be masked by more powerful reactors in the vicinity.
author_names: D L Danielson

Oluwatomi A Akindele

Morgan Askins

Marc Bergevin

Adam Bernstein

Jonathan Burns

A Carroll

J P Coleman

R Collins

Chris Connor

Douglas Cowen

Ferenc Dalnoki-Veress

Steven A Dazeley

Milind Vaman Diwan

Juanita Aguilar Duron

Stephen T Dye

Jonathan Eisch

Anthony C Ezeribe

Vincent Fischer

Richard F Foster

Katarzyna Frankiewicz

Christopher Grant

John Gribble

J He

Christopher Holligan

G Holt

W Huang

Igor Jovanovic

Liz Kneale

L Korkeila

V A Kudryavtsev

P Kunkle

R Lap Keung Mak

John G Learned

P M Lewis

Viacheslav A Li

Xiao-ming Liu

Magdalena Malek

J Maricic

Christopher Michael Mauger

Neil McCauley

C J Metelko

Robert W Mills

Franz Muheim

A St J Murphy

M D Needham

Kurtis Alan Nishimura

Gabriel D Orebi Gann

Sean Paling

Teal Pershing

L Pickard

B Pinheiro

Steve Quillin

Stephen Rogers

A Scarff

Yan Jie Schnellbach

Paul Scovell

Theresa Shaw

V E Shebalin

G D Smith

Michael Burghard Smy

N J C Spooner

Felicia Sutanto

Robert C Svoboda

Lee F Thompson

C Toth

Mark Robert Vagins

S Ventura

Matthew J Wetstein

Minerva Group

Lawrence Berkeley National Laboratory

Department of Engineering Physics

University of California Davis

Theoretical Physics Division

Los Alamos National Laboratory

University of California Berkeley

Atomic Weapons Establishment

University of Liverpool

Boston University

Pennsylvania State University

Department of Astronomy

Middlebury Institute of International Studies at Monterey

James Martin Center for Nonproliferation Studies

Brookhaven National Laboratory

University of Hawai'i at Manoa

Iowa State University

The University of Sheffield

University of Pennsylvania

Univ of Michigan in Ann Arbor

The University of Edinburgh

Boulby Underground Laboratory

University of California Irvine
title: Directionally Accelerated Detection of an Unknown Second Reactor with Antineutrinos for Mid Field Nonproliferation Monitoring
year: 2019

abstract: This document summarizes how far the Nancy Grace Roman Space Telescope Coronagraph Instrument (Roman CGI) will go toward demonstrating high contrast imaging and spectroscopic requirements for potential future exoplanet direct imaging missions, illustrated by the HabEx and LUVOIR concepts. The assessment is made for two levels of assumed CGI performance: (i) current best estimate (CBE) as of August 2020, based on laboratory results and realistic end to end simulations with JPL standard Model Uncertainty Factors (MUFs) (ii) CGI design specifications inherited from Phase B requirements. We find that the predicted performance (CBE) of many CGI subsystems compares favorably with the needs of future missions, despite providing more modest point source detection limits than future missions. This is essentially due to the challenging pupil of the Roman Space Telescope; this pupil pushes the coronagraph masks sensitivities to misalignments to be commensurate with future missions. In particular, CGI will demonstrate active low order wavefront control and photon counting capabilities at levels of performance either higher than, or comparable to, the needs of future missions.
author_names: Bertrand Mennesson

Roser Juanola-Parramon

B Nemati

Garreth J Ruane

Vanessa P Bailey

Matthew R Bolcar

S Martin

Neil T Zimmerman

Christopher C Stark

Laurent Pueyo

Dominic J Benford

Eric J Cady

Brendan P Crill

Ewan S Douglas

B Scott Gaudi

Jeremy N Kasdin

Brian D Kern

John E Krist

Jeffrey W Kruk

Thomas S Luchik

Bruce A Macintosh

Avi M Mandell

D Mawet

Ilya Y Poberezhskiy

Jason D Rhodes

A J Eldorado Riggs

Margaret C Turnbull

Aki Roberge

Fang Shi

Nick Siegler

Karl R Stapelfeldt

Marie Ygouf

Robert T Zellem

Fire Laboratory

California Institute of Technology

NASA's Goddard Space Flight Center

The University of Alabama in Huntsville

Space Telescope Sceince Institute

Nasa Headquarters

University of Arizona

Ohio State University

University of San Francisco

Stanford University

Seti Institute

Caltech Ipac
title: Paving the Way to Future Missions: the Roman Space Telescope Coronagraph Technology Demonstration
year: 2020

abstract: The paper presents new high angular resolution ALMA 1.3 mm dust continuum observations of the protoplanetary system AS 209 in the Ophiuchus star forming region. The dust continuum emission is characterized by a main central core and two prominent rings at $r 75\$au and $r 130\$au intervaled by two gaps at at $r 62\$au and $r 103\$au. The two gaps have different widths and depths, with the inner one being narrower and shallower. We determined the surface density of the millimeter dust grains using the 3D radiative transfer disk code \textsc{dali} According to our fiducial model the inner gap is partially filled with millimeter grains while the outer gap is largely devoid of dust. The inferred surface density is compared to 3D hydrodynamical simulations (FARGO 3D) of planet disk interaction. The outer dust gap is consistent with the presence of a giant planet $M_{\rm planet} \sim 0.8\,M_{\rm Staturn} the planet is responsible for the gap opening and for the pile up of dust at the outer edge of the planet orbit. The simulations also show that the same planet can give origin to the inner gap at $r 62\$au. The relative position of the two dust gaps is close to the 2:1 resonance and we have investigated the possibility of a second planet inside the inner gap. The resulting surface density (including location, width and depth of the two dust gaps) are in agreement with the observations. The properties of the inner gap pose a strong constraint to the mass of the inner planet $M_{\rm planet} 0.1\,M_{\rm J} In both scenarios (single or pair of planets) the hydrodynamical simulations suggest a very low disk viscosity \alpha 10^ 4} Given the young age of the system (0.5 1 Myr) this result implies that the formation of giant planets occurs on a timescale of \lesssim$ 1\,Myr.
author_names: D Fedele

Marco Tazzari

R A Booth

Leonardo Testi

Cathie J Clarke

Ilaria Pascucci

Agnes Kospal

Simon Bruderer

Th Henning

R Teague INAF-Osservatorio Astrofisico di Arcetri

Institute of Radio Astronomy

University of Cambridge

European Southern Observatory

Planetary Laboratory

The University of Arizona

Konkoly Observatory

Research Centre in Astronomy

Earth Sciences

Hungarian Academy of Sciences

Max Planck Institute for Radio Astronomy
title: ALMA continuum observations of the protoplanetary disk AS 209. Evidence of multiple gaps opened by a single planet
year: 2017

abstract: We present an extensive study of the BL Lac object Mrk 501 based on a data set collected during the multi instrument campaign spanning from 2009 March 15 to 2009 August 1, which includes, among other instruments, MAGIC, VERITAS, Whipple 10 m, and Fermi LAT to cover the g ray range from 0.1 GeV to 20 TeV; RXTE and Swift to cover wavelengths from UV tohard X rays; and GASP WEBT, which provides coverage of radio and optical wavelengths. Optical polarization measurements were provided for a fraction of the campaign by the Steward and St. Petersburg observatories. We evaluate the variability of the source and interband correlations, the g ray flaring activity occurring in May 2009, and interpret the results within two synchrotron self Compton (SSC) scenarios. Aims. The multiband variability observed during the full campaign is addressed in terms of the fractional variability, and the possible correlations are studied by calculating the discrete correlation function for each pair of energy bands where the significance was evaluated with dedicated Monte Carlo simulations. The space of SSC model parameters is probed following a dedicated grid scan strategy, allowing for a wide range of models to be tested and offering a study of the degeneracy of model to data agreement in the individual model parameters, hence providing a less biased interpretation than the "single curve SSC model adjustment" typically reported in the literature. Methods. We find an increase in the fractional variability with energy, while no significant interband correlations of flux changes are found on the basis of the acquired data set. The SSC model grid scan shows that the flaring activity around May 22 cannot be modeled adequately with a one zone SSC scenario (using an electron energy distribution with two breaks) while it can be suitably described within a two (independent) zone SSC scenario. Here, one zone is responsible for the quiescent emission from the averaged 4.5 month observing period, while the other one, which is spatially separated from the first, dominates the flaring emission occurring at X rays and very high energy >100 GeV, VHE) g rays. The flaring activity from May 1, which coincides with a rotation of the electric vector polarization angle (EVPA) cannot be satisfactorily reproduced by either a one zone or a two independent zone SSC model, yet this is partially affected by the lack of strictly simultaneous observations and the presence of large flux changes on sub hour timescales (detected at VHE g rays) Results. The higher variability in the VHE emission and lack of correlation with the X ray emission indicate that, at least during the 4.5 month observing campaign in 2009, the highest energy (and most variable) electrons that are responsible for the VHE g rays do not make a dominant contribution to the ~1 keV emission. Alternatively, there could be a very variable component contributing to the VHE g ray emission in addition to that coming from the SSC scenario. The studies with our dedicated SSC grid scan show that there is some degeneracy in both the one zone and the two zone SSC scenarios probed, with several combinations of model parameters yielding a similar model to data agreement, and some parameters better constrained than others. The observed g ray flaring activity, with the EVPA rotation coincident with the first g ray flare, resembles those reported previously for low frequency peaked blazars, hence suggesting that there are many similarities in the flaring mechanisms of blazars with different jet properties.
author_names: M L Ahnen

Stefano Ansoldi

Lucio Angelo Antonelli

P Antoranz

A Babic

B Banerjee

Priyadarshini Bangale

Ulisses Barres DE Almeida

J A Barrio

J Becerra Gonz'alez

W Bednarek

Elisa Bernardini

Alessio Berti

Barbara Biasuzzi

Adrian Biland

O Blanch

S Bonnefoy

G Bonnoli

F Borracci

Thomas Bretz

Sara Buson

Alessandro Carosi

Arka Chatterjee

R Clavero

Pierre Colin

E Colombo

Jose Luis Contreras

J Cortina

Stefano Covino

Paolo Da Vela

Francesco Dazzi

Alessandro De Angelis

Barbara De Lotto

Emma de Ona Wilhelmi

Federico Di Pierro

Marlene Doert

Alberto Dom'inguez

D Dominis Prester

Daniela Dorner

Michele Doro

Sabrina Einecke

D Glawion

D Elsaesser

M Engelkemeier

Vandad Fallah Ramazani

A Fern'andez-Barral

David Carreto Fidalgo

M V Fonseca

L Font

Katharina Frantzen

Christian Fruck

D Morachis Galindo

R J Garc'ia L'opez

M Garczarczyk

D Garrido Terrats

Markus Gaug

Paola Giammaria

Nikola Godinovi'c

Adiv Gonzalez Munoz

Dariusz Gora

Daniel A Guberman

D Hadasch

A Hahn

Yoshitaka Hanabata

Masaaki Hayashida

J Herrera

Juergen Hose

D Hrupec

Gareth Hughes

W Idec

Kazuhito Kodani

Yusuke Konno

H Kubo

J Kushida

Antonio La Barbera

D Lelas

E Lindfors

S Lombardi

Francesco Longo

M A L'opez

Rub'en L'opez-Coto

P Majumdar

M Makariev

K Mallot

Galina Maneva

Marina Manganaro

Karl Mannheim

Laura Maraschi

Benito Marcote

Mose Mariotti

M C Mart'inez

D Mazin

Uta Menzel

J M Miranda

R Mirzoyan

A Moralejo

E Moretti

Daisuke Nakajima

V V Neustroev

Andrzej Niedzwiecki

M Nievas Rosillo

K Nilsson

K Nishijima

K Noda

L Nogu'es

A -K Overkemping

Simona Paiano

Joaquim Palacio

M Palatiello

D Paneque

Riccardo Paoletti

Josep Maria Paredes

Xavier Paredes-Fortuny

Giovanna Pedaletti

Michele Peresano

Luca Perri

Massimo Persic

Juri Poutanen

P G Prada Moroni

E Prandini

I Puljak

Ignasi Reichardt

Wolfgang Rhode

Marc Rib'o

J Rico

J Rodriguez Garcia

T Saito

Konstancja Satalecka

S Schroder

Cornelia Schultz

Thomas Schweizer

Steven N Shore

Aimo K Sillanpaa

J Sitarek

Iva Snidaric

D Sobczynska

A Stamerra

T Steinbring

Marcel Strzys

T Suri'c

Leo O Takalo

Fabrizio Tavecchio

P Temnikov

Tomislav Terzi'c

Diego Tescaro

Masahiro Teshima

Julia Thaele

Diego F Torres

Takeshi Toyama

Aldo Treves

G Vanzo

V Verguilov

I Vovk

John E Ward

Martin Will

M H Wu

Roberta Zanin

Anushka Udara Abeysekara

Simon Archambault

Avery Archer

W Benbow

R Bird

M Buchovecky

James Henry Buckley

Viatcheslav Bugaev

Michael P Connolly

Wei Wei Cui

Hugh Dickinson

Abraham D Falcone

Qi Feng

John Park Finley

H Fleischhack

A Flinders

Lucy Fortson

G H Gillanders

Sean Griffin

Jeff Grube

Moritz Hutten

David Hanna

Jamie Holder

Thomas Brian Humensky

Philip Kaaret

Payel Kar

Nathan C Kelley-Hoskins

M P Kertzman

D Kieda

M Krause

Frank Krennrich

M J Lang

Gernot Maier

Andrew McCann

Patrick J Moriarty

Reshmi Mukherjee

Daniel Nieto

Stephan O'Brien

R A Ong

N Otte

Nahee Park

Jeremy S Perkins

Ana Pichel

Martin Pohl

Alexis Popkow

E Pueschel

Joseph F Quinn

K Ragan

Philip T Reynolds

Gordon T Richards

E Roache

Adrian C Rovero

Cameron B Rulten

Iftach H Sadeh

M Santander

Glenn H Sembroski

K Shahinyan

Igor Telezhinsky

J V Tucci

Joshua Tyler

Scott Patrick Wakely

A Weinstein

P Wilcox

Alina Wilhelm

D A Williams

Benjamin Zitzer

Stefano Villata

C M Raiteri

Hugh D Aller

M F Aller

V M Larionov

A Arkharov

Dmitry Blinov

Natalia V Efimova

Tatiana S Grishina

Vladimir A Hagen-Thorn

Evgenia N Kopatskaya

Liudmilla V Larionova

Elena G Larionova

Daria A Morozova

Ivan S Troitsky

Rolando Ligustri

Paolo Calcidese

Andrei V Berdyugin

O M Kurtanidze

M G Nikolashvili

Givi N Kimeridze

Lorand A Sigua

S O Kurtanidze

Revaz Chigladze

W P Chen

Ekaterina Koptelova

Takanori Sakamoto

Alberto Carlo Sadun

J Ward Moody

Cameron J Pace

Richard L Pearson

Yoichi Yatsu

Y A Mori

A Carraminyana

Luis Carrasco

E De la Fuente

Jay Norris

P Smith

Ann Elizabeth Wehrle

Mark A Gurwell

Alma C Zook

Claudio Pagani

Matteo Perri

M Capalbi

Andrea Cesarini

H A Krimm

Y Y Kovalev

Yu A Kovalev

Eduardo Ros

A B Pushkarev

M L Lister

Kirill V Sokolovsky

Matthias Kadler

Glenn Piner

Anne Lahteenmaki

Merja Tornikoski

Emmanouil Angelakis

Thomas P Krichbaum

Ioannis Nestoras

Lars Fuhrmann

J Anton Zensus

Pietro Cassaro

Andrea Orlati

Giuseppe Maccaferri

P Leto

Marcello Giroletti

Joseph L Richards

W Max-Moerbeck

Applied Biosciences Eth Zurich

Universita' di Udine

Infn Trieste

Inaf - National Institute for Astrophysics

Universit'a di Siena

Infn sez di Pisa

Croatian Magic Consortium

Rudjer Boskovic Institute

University of Rijeka

University of Split

University of Zagreb

Saha Institute of Nuclear Physics

Max-Planck-Institut fur extraterrestrische Physik

Universidad Complutense

Instituto de Astrof'isica de Canarias

Universidad de la Laguna

Dpto Astrof'isica

University of L'od'z

Deutsches Elektronen-Synchrotron

Institut de F'isica d'Altes Energies

The Barcelona Institute of Science

Universitat Wurzburg

Universita di Padova

Institute for Space Sciences

Technische Universitat Dortmund

Finnish Magic Consortium

Tuorla Astronomical Observatory

University of Turku

Astronomy Division

University of Oulu

Unitat de F'isica de les Radiacions

Departament de F'isica

Universitat Aut'onoma de Barcelona

Japanese Magic Consortium

The University of Tokyo

Department of Engineering Physics

Hakubi Center

Kyoto University

Tokai University

The University of Tokushima

Inst for Nucl Research

Nucl Energy

Universita' di Pisa

Now at Centro Brasileiro de Pesquisas F'isicas

Rio de Janeiro

Nasa Goddard Space Flight Center

Humboldt University of Berlin

Institut fur theoretische Physik

Berlin Germany

also at University of Trieste

now at Ecole polytechnique f'ed'erale de Lausanne

now at Max-Planck-Institut fur Kernphysik

also at Japanese Magic Consortium

now at Finnish Centre for Astronomy with Eso

also at INAF-Trieste

Dept of Physics Astronomy

University of Bologna

also at Isdc - Science Data Center for Astrophysics

A Misaki Department of Physics

Department of Physics Astronomy

University of Maryland

College Park

University of Utah

Salt lake City

Physics Department

M L Sukhadia University

Washington State University

St Louis

Fred Lawrence Whipple Observatory

Harvard--Smithsonian Center for Astrophysics

School of Cosmic Physics

University College Dublin

University of Southern California

Los P Angeles

National University of Ireland Galway

Purdue University

West Lafayette

Center for Computational Astrophysics

Tsinghua University

Iowa State University

525 Davey Lab

Pennsylvania State University

University Park

University of Minnesota

Astronomy Department

Adler Planetarium

Astronomy Museum

the Bartol Research Institute

University of Delaware

Columbia University

New York

University of Iowa

Van Allen Hall

Iowa City

DePauw University

Barnard College

Enrico Fermi Institute

University of Chicago

Instituto de Astronomia y Fisica del Espacio

Ciudad de Buenos Aires

Institute of Metal Physics

University of Potsdam

Department of Astrophysical Sciences

Cork Institute of Technology

Georgia Institute of Technology

Santa Cruz Institute for Particle Physics

Santa Cruz

Argonne National Laboratory

University of Johannesburg

South Africa

INAF-Osservatorio Astrofisico di Torino

University of Michigan

Ann Arbor

Astronomical Institute

St Petersburg State University

St Petersburg

Pulkovo Astronomical Observatory

Institute for Particle Physics

University of Crete

Foundation for Research

Circolo Astrofili Talmassons

Osservatorio Astrofisico della Regione Autonoma Valle d'Aosta

Abastumani Astrophysical Observatory

Engelhardt Astronomical Observatory

Kazan Federal University

Guangzhou University

Graduate Institute of Astronomy

National Central University

College of Materials Science

952 Engineering

Aoyama Gakuin University

Sagamihara Kanagawa

University of Colorado Denver

Brigham Young University

Tokyo Institute of Technology

Meguro City

Instituto Nacional de Astrof'isica

'optica y Electr'onica

Instututo de Astronomia y Meteorologia

Dpto de Fisica

Universidad de Guadalajara

Steward Observatory

University of Arizona

Space Telescope Science Institute

Pomona College

University of Leicester

Asi Science Data Center

Via del Politecnico

I-00133 Roma

University of Trento

Center for Space Research

Exploration in Space Science

Universities Space Research Association

Astro Space Center of the Lebedev Physical Institute

Max--Planck--Institut fur Radioastronomie

Observatori Astronomic

Universitat Politecnica de Valencia

Departament d'Astronomia i Astrof'isica

Crimean Astrophysical Observatory

Sternberg Astronomical Institute

Mcgill University

Institute of Radio Astronomy

Space Applications

Remote Sensing

National Observatory of Athens

Whittier College

Aalto University Metsahovi Radio Observatory

Inaf Istituto di Radioastronomia

Sezione di Noto

Stazione Radioastronomica di Medicina

M Guainazzi Iasfinaf Bologna

Inaf - Osservatorio Astrofisico di Catania

Cahill Center for Astronomy

California Institute of Technology
title: Multiband variability studies and novel broadband SED modeling of Mrk 501 in 2009
year: 2016

abstract: Using N body simulations, we have modeled the production and evolution of diffuse, low surface brightness intracluster light (ICL) in three simulated galaxy clusters. Using an observational definition of ICL to be luminosity at a surface brightness uV> 26.5 mag/arcsec 2 we have found that the fraction of cluster luminosity contained in ICL generally increases as clusters evolve, although there are large deviations from this trend over short timescales, including sustained periods of decreasing ICL luminosity. Most ICL luminosity increases come in short, discrete events which are highly correlated with group accretion events within the cluster. In evolved clusters we find that 10 15% of the clusters' luminosity is at ICL surface brightness. The morphological structure of the ICL changes with time, evolving from a complex of filaments and smallscale, relatively high surface brightness features early in a cluster's history, to a more diffuse and amorphous cluster scale ICL envelope at later times. Finally, we also see a correlation between the evolution of ICL at different surface brightnesses, including a time delay between the evolution of faint and extremely faint surface brightness features which is traced to the differing dynamical timescales in the group and cluster environment. Subject headings: galaxies: clusters: general galaxies: evolution galaxies interactions galaxies: kinematics and dynamics methods: N body simulations
author_names: Craig S Rudick

J Christopher Mihos

Cameron McBride Department of Astronomy

Case Western Reserve Univesity

Now in the Department of Physics

University of Pittsburgh
title: The Formation and Evolution of Intracluster Light
year: 2006

abstract: We present a theoretical model to predict the properties of an observed $z 5.72 Lyman \alpha$ emitter galaxy CIV absorption pair separated by 1384 comoving kpc/h. We use the separation of the pair and an outflow velocity/time travelling argument to demonstrate that the observed galaxy cannot be the source of metals for the CIV absorber. We find a plausible explanation for the metal enrichment in the context of our simulations: a dwarf galaxy with $M_{\star} 1.87 \times$ 10${9} M_{\odot} located 119 comoving kpc/h away with a wind velocity of \sim$ 100 km/s launched at $z \sim$ 7. Such a dwarf $M_{\text{UV} 20.5) is fainter than the detection limit of the observed example. In a general analysis of galaxy CIV absorbers, we find galaxies with 20.5 M_{\text{UV} 18.8 are responsible for the observed metal signatures. In addition, we find no correlation between the mass of the closest galaxy to the absorber and the distance between them, but a weak anti correlation between the strength of the absorption and the separation of galaxy absorber pairs.
author_names: Luz 'Angela Garc'ia

Edoardo Tescari

Emma V Ryan-Weber

J S B Wyithe Centre for Astrophysics

Swinburne University of Technology

Arc Centre of Excellence for All-Sky Astrophysics in 3 Physics

The University of Melbourne
title: Theoretical study of an LAE C IV absorption pair at z 5.7
year: 2017