On Effective Field Theory of Dark Matter
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Big Halpha Kinematical Sample of Barred Spiral Galaxies - I
BhaBAR: Big Halpha kinematical sample of BARred spiral galaxies - I. Fabry-Perot Observations of 21 galaxies O. Hernandez, C. Carignan, P. Amram, L. Chemin, O. Daigle To cite this version: O. Hernandez, C. Carignan, P. Amram, L. Chemin, O. Daigle. BhaBAR: Big Halpha kinematical sample of BARred spiral galaxies - I. Fabry-Perot Observations of 21 galaxies. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2005, 360 Issue 4, pp.1201. 10.1111/j.1365-2966.2005.09125.x. hal-00014446 HAL Id: hal-00014446 https://hal.archives-ouvertes.fr/hal-00014446 Submitted on 26 Jan 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Mon. Not. R. Astron. Soc. 360, 1201–1230 (2005) doi:10.1111/j.1365-2966.2005.09125.x BHαBAR: big Hα kinematical sample of barred spiral galaxies – I. Fabry–Perot observations of 21 galaxies O. Hernandez,1,2 † C. Carignan,1 P. Amram,2 L. Chemin1 and O. Daigle1 1Observatoire du mont Megantic,´ LAE, Universitede´ Montreal,´ CP 6128 succ. centre ville, Montreal,´ Quebec,´ Canada H3C 3J7 2Observatoire Astronomique de Marseille Provence et LAM, 2 pl. -
On the Nature of GRB 050509B: a Disguised Short GRB
A&A 529, A130 (2011) Astronomy DOI: 10.1051/0004-6361/201116659 & c ESO 2011 Astrophysics On the nature of GRB 050509b: a disguised short GRB G. De Barros1,2,L.Amati2,3,M.G.Bernardini4,1,2,C.L.Bianco1,2, L. Caito1,2,L.Izzo1,2, B. Patricelli1,2, and R. Ruffini1,2,5 1 Dipartimento di Fisica and ICRA, Università di Roma “La Sapienza”, Piazzale Aldo Moro 5, 00185 Roma, Italy e-mail: [maria.bernardini;bianco;letizia.caito;luca.izzo;ruffini]@icra.it 2 ICRANet, Piazzale della Repubblica 10, 65122 Pescara, Italy e-mail: [gustavo.debarros;barbara.patricelli]@icranet.org 3 Italian National Institute for Astrophysics (INAF) – IASF Bologna, via P. Gobetti 101, 40129 Bologna, Italy e-mail: [email protected] 4 Italian National Institute for Astrophysics (INAF) – Osservatorio Astronomico di Brera, via Emilio Bianchi 46, 23807 Merate (LC), Italy 5 ICRANet, Université de Nice Sophia Antipolis, Grand Château, BP 2135, 28 avenue de Valrose, 06103 Nice Cedex 2, France Received 4 February 2011 / Accepted 7 March 2011 ABSTRACT Context. GRB 050509b, detected by the Swift satellite, is the first case where an X-ray afterglow has been observed associated with a short gamma-ray burst (GRB). Within the fireshell model, the canonical GRB light curve presents two different components: the proper-GRB (P-GRB) and the extended afterglow. Their relative intensity is a function of the fireshell baryon loading parameter B and of the CircumBurst Medium (CBM) density (nCBM). In particular, the traditionally called short GRBs can be either “genuine” short GRBs (with B 10−5, where the P-GRB is energetically predominant) or “disguised” short GRBs (with B 3.0 × 10−4 and nCBM 1, where the extended afterglow is energetically predominant). -
Spiral Galaxy HI Models, Rotation Curves and Kinematic Classifications
Spiral galaxy HI models, rotation curves and kinematic classifications Theresa B. V. Wiegert A thesis submitted to the Faculty of Graduate Studies of The University of Manitoba in partial fulfillment of the requirements of the degree of Doctor of Philosophy Department of Physics & Astronomy University of Manitoba Winnipeg, Canada 2010 Copyright (c) 2010 by Theresa B. V. Wiegert Abstract Although galaxy interactions cause dramatic changes, galaxies also continue to form stars and evolve when they are isolated. The dark matter (DM) halo may influence this evolu- tion since it generates the rotational behaviour of galactic disks which could affect local conditions in the gas. Therefore we study neutral hydrogen kinematics of non-interacting, nearby spiral galaxies, characterising their rotation curves (RC) which probe the DM halo; delineating kinematic classes of galaxies; and investigating relations between these classes and galaxy properties such as disk size and star formation rate (SFR). To generate the RCs, we use GalAPAGOS (by J. Fiege). My role was to test and help drive the development of this software, which employs a powerful genetic algorithm, con- straining 23 parameters while using the full 3D data cube as input. The RC is here simply described by a tanh-based function which adequately traces the global RC behaviour. Ex- tensive testing on artificial galaxies show that the kinematic properties of galaxies with inclination > 40 ◦, including edge-on galaxies, are found reliably. Using a hierarchical clustering algorithm on parametrised RCs from 79 galaxies culled from literature generates a preliminary scheme consisting of five classes. These are based on three parameters: maximum rotational velocity, turnover radius and outer slope of the RC. -
Kavli IPMU Annual 2014 Report
ANNUAL REPORT 2014 REPORT ANNUAL April 2014–March 2015 2014–March April Kavli IPMU Kavli Kavli IPMU Annual Report 2014 April 2014–March 2015 CONTENTS FOREWORD 2 1 INTRODUCTION 4 2 NEWS&EVENTS 8 3 ORGANIZATION 10 4 STAFF 14 5 RESEARCHHIGHLIGHTS 20 5.1 Unbiased Bases and Critical Points of a Potential ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙20 5.2 Secondary Polytopes and the Algebra of the Infrared ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙21 5.3 Moduli of Bridgeland Semistable Objects on 3- Folds and Donaldson- Thomas Invariants ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙22 5.4 Leptogenesis Via Axion Oscillations after Inflation ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙23 5.5 Searching for Matter/Antimatter Asymmetry with T2K Experiment ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ 24 5.6 Development of the Belle II Silicon Vertex Detector ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙26 5.7 Search for Physics beyond Standard Model with KamLAND-Zen ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙28 5.8 Chemical Abundance Patterns of the Most Iron-Poor Stars as Probes of the First Stars in the Universe ∙ ∙ ∙ 29 5.9 Measuring Gravitational lensing Using CMB B-mode Polarization by POLARBEAR ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ 30 5.10 The First Galaxy Maps from the SDSS-IV MaNGA Survey ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙ ∙32 5.11 Detection of the Possible Companion Star of Supernova 2011dh ∙ ∙ ∙ ∙ ∙ ∙ -
From Luminous Hot Stars to Starburst Galaxies
9780521791342pre CUP/CONT July 9, 2008 11:48 Page-i FROM LUMINOUS HOT STARS TO STARBURST GALAXIES Luminous hot stars represent the extreme upper mass end of normal stellar evolution. Before exploding as supernovae, they live out their lives of only a few million years with prodigious outputs of radiation and stellar winds which dramatically affect both their evolution and environments. A detailed introduction to the topic, this book connects the astrophysics of mas- sive stars with the extremes of galaxy evolution represented by starburst phenomena. A thorough discussion of the physical and wind parameters of massive stars is pre- sented, together with considerations of their birth, evolution, and death. Hll galaxies, their connection to starburst galaxies, and the contribution of starburst phenomena to galaxy evolution through superwinds, are explored. The book concludes with the wider cosmological implications, including Population III stars, Lyman break galaxies, and gamma-ray bursts, for each of which massive stars are believed to play a crucial role. This book is ideal for graduate students and researchers in astrophysics who are interested in massive stars and their role in the evolution of galaxies. Peter S. Conti is an Emeritus Professor at the Joint Institute for Laboratory Astro- physics (JILA) and theAstrophysics and Planetary Sciences Department at the University of Colorado. Paul A. Crowther is a Professor of Astrophysics in the Department of Physics and Astronomy at the University of Sheffield. Claus Leitherer is an Astronomer with the Space Telescope Science Institute, Baltimore. 9780521791342pre CUP/CONT July 9, 2008 11:48 Page-ii Cambridge Astrophysics Series Series editors: Andrew King, Douglas Lin, Stephen Maran, Jim Pringle and Martin Ward Titles available in the series 10. -
FBE Tez Yazim Kilavuzu
İSTANBUL ÜNİVERSİTESİ FEN BİLİMLERİ ENSTİTÜSÜ YÜKSEK LİSANS TEZİ SÜPERNOVALARLA İLİŞKİLİ GAMA IŞIN PATLAMALARININ (GRB), GAMA VE OPTİK-IŞIN ÖZELLİKLERİ ARASINDAKİ İLİŞKİ Astronom Özgecan ÖNAL Astronomi ve Uzay Bilimleri Bölümü 1. Danışman Doç.Dr. A. Talât SAYGAÇ 2. Danışman Doç. Dr. Massimo DELLA VALLE Haziran, 2008 İSTANBUL İSTANBUL ÜNİVERSİTESİ FEN BİLİMLERİ ENSTİTÜSÜ YÜKSEK LİSANS TEZİ SÜPERNOVALARLA İLİŞKİLİ GAMA IŞIN PATLAMALARININ (GRB), GAMA VE OPTİK -IŞIN ÖZELLİKLERİ ARASINDAKİ İLİŞKİ Astronom Özgecan ÖNAL Astronomi ve Uzay Bilimleri Bölümü 1. Danışman Doç.Dr. A. Talât SAYGAÇ 2. Danışman Doç. Dr. Massimo DELLA VALLE Haziran, 2008 İSTANBUL Bu çalışma ..../..../ 2003 tarihinde aşağıdaki jüri tarafından ....................................... Anabilim Dalı .................................. programında Doktora / Yüksek Lisans Tezi olarak kabul edilmiştir. Tez Jürisi Danışman Adı (Danışman) Jüri Adı İstanbul Üniversitesi Üniversite Mühendislik Fakültesi Fakülte Jüri Adı Jüri Adı Üniversite Üniversite Fakülte Fakülte Jüri Adı Üniversite Fakülte Bu çalışma İstanbul Üniversitesi Bilimsel Araştırma Projeleri Yürütücü Sekreterliğinin T-935/06102006 numaralı projesi ile desteklenmiştir. ÖNSÖZ Lisans ve yüksek lisans öğrenimim sırasında ve tez çalışmalarım boyunca gösterdiği her türlü destek ve yardımdan dolayı çok değerli hocam Doç. Dr. A. Talât SAYGAÇ’a en içten dileklerimle teşekkür ederim. Tezin çeşitli aşamaları boyunca durumun hassasiyetinin bilincinde olan anneme, babama ve ağabeyime nazik ve sabırlı davranışları için ayrı ayrı teşekkür ediyorum. Bu çalışmanın başladığı ilk günlerde elime ilk makaleyi tutuşturan saygıdeğer hocam Prof. Dr. Salih KARAALİ’ye, literatür taraması yaptığım dönemlerde hemen yardımıma koşan Dr. Tolga GÜVER’e ve bulduğu önemli makaleleri benimle paylaşan Araş. Gör. Sinan ALİŞ’e çok teşekkür ederim. Çalışma sürecinin çeşitli aşamalarında tartışma fırsatı bulduğum değerli astrofizikçiler Dr. Yuki KANEKO, Dr.Andrew BEARDMORE ve Dr. -
The Short Gamma-Ray Burst Revolution
Reports from Observers The Short Gamma-Ray Burst Revolution Jens Hjorth1 the afterglow light-curve properties and Afterglows – found! Andrew Levan ,3 possible high-redshift origin of some Nial Tanvir 4 short bursts suggests that more than Finally, in May 005 Swift discovered the Rhaana Starling 4 one progenitor type may be involved. first X-ray afterglow to a short GRB. Sylvio Klose5 This was made possible because of the Chryssa Kouveliotou6 rapid ability of Swift to slew across the Chloé Féron1 A decade ago studies of gamma-ray sky, pointing at the approximate location Patrizia Ferrero5 bursts (GRBs) were revolutionised by the of the burst only a minute after it hap- Andy Fruchter 7 discovery of long-lived afterglow emis- pened and pinpointing a very faint X-ray Johan Fynbo1 sion at X-ray, optical and radio wave- afterglow. The afterglow lies close to a Javier Gorosabel 8 lengths. The afterglows provided precise massive elliptical galaxy in a cluster of Páll Jakobsson positions on the sky, which in turn led galaxies at z = 0.225 (Gehrels et al. 005; David Alexander Kann5 to the discovery that GRBs originate at Pedersen et al. 005; Figure ). Many ex- Kristian Pedersen1 cosmological distances, and are thus the tremely deep observations, including Enrico Ramirez-Ruiz 9 most luminous events known in the Uni- those at the VLT, failed to locate either a Jesper Sollerman1 verse. These afterglows also provided fading optical afterglow, or a rising super- Christina Thöne1 essential information for our understand- nova component at later times (Hjorth Darach Watson1 ing of what creates these extraordinary et al. -
Classification of Galaxies Using Fractal Dimensions
UNLV Retrospective Theses & Dissertations 1-1-1999 Classification of galaxies using fractal dimensions Sandip G Thanki University of Nevada, Las Vegas Follow this and additional works at: https://digitalscholarship.unlv.edu/rtds Repository Citation Thanki, Sandip G, "Classification of galaxies using fractal dimensions" (1999). UNLV Retrospective Theses & Dissertations. 1050. http://dx.doi.org/10.25669/8msa-x9b8 This Thesis is protected by copyright and/or related rights. It has been brought to you by Digital Scholarship@UNLV with permission from the rights-holder(s). You are free to use this Thesis in any way that is permitted by the copyright and related rights legislation that applies to your use. For other uses you need to obtain permission from the rights-holder(s) directly, unless additional rights are indicated by a Creative Commons license in the record and/ or on the work itself. This Thesis has been accepted for inclusion in UNLV Retrospective Theses & Dissertations by an authorized administrator of Digital Scholarship@UNLV. For more information, please contact [email protected]. INFORMATION TO USERS This manuscript has been reproduced from the microfilm master. UMI films the text directly from the original or copy submitted. Thus, some thesis and dissertation copies are in typewriter face, while others may be from any type of computer printer. The quality of this reproduction is dependent upon the quality of the copy submitted. Broken or indistinct print, colored or poor quality illustrations and photographs, print bleedthrough, substandard margins, and improper alignment can adversely affect reproduction. In the unlikely event that the author did not send UMI a complete manuscript and there are missing pages, these will be noted. -
MC^ 2: Galaxy Imaging and Redshift Analysis of the Merging Cluster CIZA J2242. 8+ 5301
LLNL-DOC-661846-DRAFT A Preprint typeset using LTEX style emulateapj v. 8/13/10 MC2: GALAXY IMAGING AND REDSHIFT ANALYSIS OF THE MERGING CLUSTER CIZA J2242.8+5301 William A. Dawson1, M. James Jee2, Andra Stroe3, Y. Karen Ng2, Nathan Golovich2, David Wittman2, David Sobral3,4,5, M. Bruggen¨ 6, H. J. A. Rottgering¨ 3, R. J. van Weeren7 (Dated: Draft June 21, 2021) LLNL-DOC-661846-DRAFT ABSTRACT X-ray and radio observations of CIZA J2242.8+5301 suggest that it is a major cluster merger. Despite being well studied in the X-ray, and radio, little has been presented on the cluster structure and dynamics inferred from its galaxy population. We carried out a deep (i< 25) broad band imaging survey of the system with Subaru SuprimeCam (g & i bands) and the Canada France Hawaii Telescope (r band) as well as a comprehensive spectroscopic survey of the cluster area (505 redshifts) using Keck DEIMOS. We use this data to perform a comprehensive galaxy/redshift analysis of the system, which is the first step to a proper understanding the geometry and dynamics of the merger, as well as using the merger to constrain self-interacting dark matter. We find that the system is dominated by two ′+0.7 +0.13 subclusters of comparable richness with a projected separation of6.9 −0.5 (1.3−0.10 Mpc). We find that the north and south subclusters have similar redshifts of z 0.188 with a relative line-of-sight velocity difference of 69 190kms−1. We also find that north and south≈ subclusters have velocity dispersions of +100 −±1 +100 −1 +4.6 14 1160−90 kms and 1080−70 kms , respectively. -
Identifying the Host Galaxy of the Short GRB 100628A⋆
A&A 583, A88 (2015) Astronomy DOI: 10.1051/0004-6361/201425160 & c ESO 2015 Astrophysics Identifying the host galaxy of the short GRB 100628A A. Nicuesa Guelbenzu1,S.Klose1, E. Palazzi2,J.Greiner3,M.J.Michałowski4,D.A.Kann1,L.K.Hunt5, D. Malesani6, A. Rossi1,2,S.Savaglio7,S.Schulze8,9,D.Xu7,P.M.J.Afonso10, J. Elliott3, P. Ferrero11, R. Filgas12, D. H. Hartmann13, T. Krühler14, F. Knust3, N. Masetti2,15,F.OlivaresE.15,A.Rau3, P. Schady3,S.Schmidl1, M. Tanga3,A.C.Updike16, and K. Varela3 1 Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany e-mail: [email protected] 2 INAF-IASF Bologna, via Gobetti 101, 40129 Bologna, Italy 3 Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstraße 1, 85748 Garching, Germany 4 Scottish Universities Physics Alliance for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, EH9 3HJ, UK 5 INAF-Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy 6 Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen, Denmark 7 Physics Department, University of Calabria, via P. Bucci, 87036 Arcavacata di Rende, Italy 8 Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, 306, Santiago 22, Chile 9 Millennium Institute of Astrophysics, Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile 10 American River College, Physics and Astronomy Dpt., 4700 College Oak Drive, Sacramento, CA 95841, USA 11 Instituto de Astrofísica de Andalucía, Consejo Superior de Investigaciones Científicas (IAA-CSIC), Glorieta de la Astronomía s/n, 18008 Granada, Spain 12 Institute of Experimental and Applied Physics, Czech Technical University in Prague, Horská 3a/22, 12800 Prague, Czech Republic 13 Department of Physics and Astronomy, Clemson University, Clemson, SC 29634, USA 14 European Southern Observatory, Alonso de Córdova 3107, 19001 Vitacura Casilla, Santiago 19, Chile 15 Departamento de Ciencias Fisicas, Universidad Andres Bello, Avda. -
The Effects of Metallicity on the Cepheid PL Relation and The
Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 30 October 2018 (MN LATEX style file v1.4) The Effects of Metallicity on the Cepheid P-L Relation and the Consequences for the Extragalactic Distance Scale Paul D. Allen1,2 and Tom Shanks1 1 Department of Physics, Science Laboratories, South Road, Durham DH1 3LE. 2 Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH. 30 October 2018 ABSTRACT If a Cepheid luminosity at given period depends on metallicity, then the P-L relation in galaxies with higher metallicities may show a higher dispersion if these galaxies also sample a wider range of intrinsic metallicities. Using published HST Cepheid data from 25 galaxies, we have found such a correlation between the the P-L dispersion and host galaxy metallicity which is significant at the ≈ 3σ level in the V band. In the I band the correlation is less significant, although the tighter intrinsic dispersion of the P-L relation in I makes it harder to detect such a correlation in the HST sample. We find that these results are unlikely to be explained by increased dust absorption in high metallicity galaxies. The data support the suggestion of Hoyle et al. that the metallicity dependence of the Cepheid P-L relation may be stronger than expected, with ∆M/[O/H] ≈−0.66 mag dex−1 at fixed period. The high observed dispersions in the HST Cepheid P-L relations have the further consequence that the bias due to incompleteness in the P-L relation at faint magnitudes is more significant than previously thought. -
Arxiv:1705.02358V2 [Hep-Ph] 24 Nov 2017
Dark Matter Self-interactions and Small Scale Structure Sean Tulin1, ∗ and Hai-Bo Yu2, y 1Department of Physics and Astronomy, York University, Toronto, Ontario M3J 1P3, Canada 2Department of Physics and Astronomy, University of California, Riverside, California 92521, USA (Dated: November 28, 2017) Abstract We review theories of dark matter (DM) beyond the collisionless paradigm, known as self-interacting dark matter (SIDM), and their observable implications for astrophysical structure in the Universe. Self- interactions are motivated, in part, due to the potential to explain long-standing (and more recent) small scale structure observations that are in tension with collisionless cold DM (CDM) predictions. Simple particle physics models for SIDM can provide a universal explanation for these observations across a wide range of mass scales spanning dwarf galaxies, low and high surface brightness spiral galaxies, and clusters of galaxies. At the same time, SIDM leaves intact the success of ΛCDM cosmology on large scales. This report covers the following topics: (1) small scale structure issues, including the core-cusp problem, the diversity problem for rotation curves, the missing satellites problem, and the too-big-to-fail problem, as well as recent progress in hydrodynamical simulations of galaxy formation; (2) N-body simulations for SIDM, including implications for density profiles, halo shapes, substructure, and the interplay between baryons and self- interactions; (3) semi-analytic Jeans-based methods that provide a complementary approach for connecting particle models with observations; (4) merging systems, such as cluster mergers (e.g., the Bullet Cluster) and minor infalls, along with recent simulation results for mergers; (5) particle physics models, including light mediator models and composite DM models; and (6) complementary probes for SIDM, including indirect and direct detection experiments, particle collider searches, and cosmological observations.