The Simons Observatory (SO) is a ground-based cosmic microwave background (CMB) experiment sited on Cerro Toco in the Atacama Desert in Chile that promises to provide breakthrough discoveries in fundamental physics, cosmology, and astrophysics. Supported by the Simons Foundation, the Heising-Simons Foundation, and with contributions from collaborating institutions, SO will see first light in 2021 and start a five year survey in 2022. SO has 287 collaborators from 12 countries and 53 institutions, including 85 students and 90 postdocs. The SO experiment in its currently funded form ('SO-Nominal') consists of three 0.4 m Small Aperture Telescopes (SATs) and one 6 m Large Aperture Telescope (LAT). Optimized for minimizing systematic errors in polarization measurements at large angular scales, the SATs will perform a deep, degree-scale survey of 10% of the sky to search for the signature of primordial gravitational waves. The LAT will survey 40% of the sky with arc-minute resolution. These observations will measure (or limit) the sum of neutrino masses, search for light relics, measure the early behavior of Dark Energy, and refine our understanding of the intergalactic medium, clusters and the role of feedback in galaxy formation. With up to ten times the sensitivity and five times the angular resolution of the Planck satellite, and roughly an order of magnitude increase in mapping speed over currently operating ("Stage 3") experiments, SO will measure the CMB temperature and polarization fluctuations to exquisite precision in six frequency bands from 27 to 280 GHz. SO will rapidly advance CMB science while informing the design of future observatories such as CMB-S4.

The Simons Observatory Collaboration Maximilian H. Abitbol Shunsuke Adachi Peter Ade James Aguirre Zeeshan Ahmed Simone Aiola Aamir Ali David Alonso Marcelo A. Alvarez Kam Arnold Peter Ashton Zachary Atkins Jason Austermann Humna Awan Carlo Baccigalupi Taylor Baildon Anton Baleato Lizancos Darcy Barron Nick Battaglia Richard Battye Eric Baxter Andrew Bazarko James A. Beall Rachel Bean Dominic Beck Shawn Beckman Benjamin Beringue Tanay Bhandarkar Sanah Bhimani Federico Bianchini Steven Boada David Boettger Boris Bolliet J. Richard Bond Julian Borrill Michael L. Brown Sarah Marie Bruno Sean Bryan Erminia Calabrese Victoria Calafut Paolo Calisse Julien Carron Fred. M Carl Juan Cayuso Anthony Challinor Grace Chesmore Yuji Chinone Jens Chluba Hsiao-Mei Sherry Cho Steve Choi Susan Clark Philip Clarke Carlo Contaldi Gabriele Coppi Nicholas F. Cothard Kevin Coughlin Will Coulton Devin Crichton Kevin D. Crowley Kevin T. Crowley Ari Cukierman John M. D'Ewart Rolando Dünner Tijmen de Haan Mark Devlin Simon Dicker Bradley Dober Cody J. Duell Shannon Duff Adri Duivenvoorden Jo Dunkley Hamza El Bouhargani Josquin Errard Giulio Fabbian Stephen Feeney James Fergusson Simone Ferraro Pedro Fluxà Katherine Freese Josef C. Frisch Andrei Frolov George Fuller Nicholas Galitzki Patricio A. Gallardo Jose Tomas Galvez Ghersi Jiansong Gao Eric Gawiser Martina Gerbino Vera Gluscevic Neil Goeckner-Wald Joseph Golec Sam Gordon Megan Gralla Daniel Green Arpi Grigorian John Groh Chris Groppi Yilun Guan Jon E. Gudmundsson Mark Halpern Dongwon Han Peter Hargrave Kathleen Harrington Masaya Hasegawa Matthew Hasselfield Makoto Hattori Victor Haynes Masashi Hazumi Erin Healy Shawn W. Henderson Brandon Hensley Carlos Hervias-Caimapo Charles A. Hill J. Colin Hill Gene Hilton Matt Hilton Adam D. Hincks Gary Hinshaw Renée Hložek Shirley Ho Shuay-Pwu Patty Ho Thuong D. Hoang Jonathan Hoh Selim C. Hotinli Zhiqi Huang Johannes Hubmayr Kevin Huffenberger John P. Hughes Anna Ijjas Margaret Ikape Kent Irwin Andrew H. Jaffe Bhuvnesh Jain Oliver Jeong Matthew Johnson Daisuke Kaneko Ethan D. Karpel Nobuhiko Katayama Brian Keating Reijo Keskitalo Theodore Kisner Kenji Kiuchi Jeff Klein Kenda Knowles Anna Kofman Brian Koopman Arthur Kosowsky Nicoletta Krachmalnicoff Akito Kusaka Phil LaPlante Jacob Lashner Adrian Lee Eunseong Lee Antony Lewis Yaqiong Li Zack Li Michele Limon Eric Linder Jia Liu Carlos Lopez-Caraballo Thibaut Louis Marius Lungu Mathew Madhavacheril Daisy Mak Felipe Maldonado Hamdi Mani Ben Mates Frederick Matsuda Loïc Maurin Phil Mauskopf Andrew May Nialh McCallum Heather McCarrick Chris McKenney Jeff McMahon P. Daniel Meerburg James Mertens Joel Meyers Amber Miller Mark Mirmelstein Kavilan Moodley Jenna Moore Moritz Munchmeyer Charles Munson Masaaki Murata Sigurd Naess Toshiya Namikawa Federico Nati Martin Navaroli Laura Newburgh Ho Nam Nguyen Andrina Nicola Mike Niemack Haruki Nishino Yume Nishinomiya John Orlowski-Scherer Luca Pagano Bruce Partridge Francesca Perrotta Phumlani Phakathi Lucio Piccirillo Elena Pierpaoli Giampaolo Pisano Davide Poletti Roberto Puddu Giuseppe Puglisi Chris Raum Christian L. Reichardt Mathieu Remazeilles Yoel Rephaeli Dominik Riechers Felipe Rojas Aditya Rotti Anirban Roy Sharon Sadeh Yuki Sakurai Maria Salatino Mayuri Sathyanarayana Rao Lauren Saunders Emmanuel Schaan Marcel Schmittfull Neelima Sehgal Joseph Seibert Uros Seljak Paul Shellard Blake Sherwin Meir Shimon Carlos Sierra Jonathan Sievers Cristobal Sifon Precious Sikhosana Maximiliano Silva-Feaver Sara M. Simon Adrian Sinclair Kendrick Smith Wuhyun Sohn Rita Sonka David Spergel Jacob Spisak Suzanne T. Staggs George Stein Jason R. Stevens Radek Stompor Aritoki Suzuki Osamu Tajima Satoru Takakura Grant Teply Daniel B. Thomas Ben Thorne Robert Thornton Hy Trac Jesse Treu Calvin Tsai Carole Tucker Joel Ullom Sunny Vagnozzi Alexander van Engelen Jeff Van Lanen Daniel D. Van Winkle Eve M. Vavagiakis Clara Vergès Michael Vissers Kasey Wagoner Samantha Walker Yuhan Wang Jon Ward Ben Westbrook Nathan Whitehorn Jason Williams Joel Williams Edward Wollack Zhilei Xu Siavash Yasini Edward Young Byeonghee Yu Cyndia Yu Fernando Zago Mario Zannoni Hezi Zhang Kaiwen Zheng Ningfeng Zhu Andrea Zonca

astro-ph.IM

(abridged) We present the results of an extensive infrared study of the massive star-forming region G9.62+0.19. The data cover information from broad- and narrow-band filters in the wavelength range from 1 to 19 micrometer and are obtained with ESO's infrared cameras ISAAC and TIMMI2 and with SpectroCam-10 (Mt. Palomar). The high sensitivity and resolution provided by these facilities revealed intriguing new details of this star-forming region and especially about the embedded hot molecular core (HMC) - component F. We analyse the newly found infrared sub-structure of four objects in this HMC region. While one of these objects (F2) is probably a foreground field star, the nature of the brightest object in the near-infrared there (F1) remains somewhat enigmatic. Our new astrometry proves that this object is not coincident with the peak of the molecular line emission of the HMC, but displaced by 1.7 arcsecs (nearly 10000 AU on a linear scale). We estimate this object to be an additional embedded object with a dense dust shell. Very near the HMC location we find L' band emission which strongly rises in flux towards longer wavelengths. We presume that this emission (F4) arises from the envelope of the HMC which is known to be associated with a molecular outflow roughly aligned along the line of sight. Thus, the clearing effect of this outflow causes strong deviations from spherical symmetry which might allow infrared emission from the HMC to escape through the outflow cavities. This presents the first direct detection of an HMC at a wavelength as short as 3.8 micron. At 11.7 and 18.75 micron, the HMC counterpart F4 ultimately proves to be the most luminous IR source within the G9.62+0.19-F region.

Hendrik Linz Bringfried Stecklum Thomas Henning Peter Hofner Bernhard Brandl

astro-ph

The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro Toco in Chile, due to begin observations in the early 2020s. We describe the scientific goals of the experiment, motivate the design, and forecast its performance. SO will measure the temperature and polarization anisotropy of the cosmic microwave background in six frequency bands: 27, 39, 93, 145, 225 and 280 GHz. The initial configuration of SO will have three small-aperture 0.5-m telescopes (SATs) and one large-aperture 6-m telescope (LAT), with a total of 60,000 cryogenic bolometers. Our key science goals are to characterize the primordial perturbations, measure the number of relativistic species and the mass of neutrinos, test for deviations from a cosmological constant, improve our understanding of galaxy evolution, and constrain the duration of reionization. The SATs will target the largest angular scales observable from Chile, mapping ~10% of the sky to a white noise level of 2 $μ$K-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, $r$, at a target level of $σ(r)=0.003$. The LAT will map ~40% of the sky at arcminute angular resolution to an expected white noise level of 6 $μ$K-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the LSST sky region and partially with DESI. With up to an order of magnitude lower polarization noise than maps from the Planck satellite, the high-resolution sky maps will constrain cosmological parameters derived from the damping tail, gravitational lensing of the microwave background, the primordial bispectrum, and the thermal and kinematic Sunyaev-Zel'dovich effects, and will aid in delensing the large-angle polarization signal to measure the tensor-to-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and more than 20,000 extragalactic sources.

The Simons Observatory Collaboration Peter Ade James Aguirre Zeeshan Ahmed Simone Aiola Aamir Ali David Alonso Marcelo A. Alvarez Kam Arnold Peter Ashton Jason Austermann Humna Awan Carlo Baccigalupi Taylor Baildon Darcy Barron Nick Battaglia Richard Battye Eric Baxter Andrew Bazarko James A. Beall Rachel Bean Dominic Beck Shawn Beckman Benjamin Beringue Federico Bianchini Steven Boada David Boettger J. Richard Bond Julian Borrill Michael L. Brown Sarah Marie Bruno Sean Bryan Erminia Calabrese Victoria Calafut Paolo Calisse Julien Carron Anthony Challinor Grace Chesmore Yuji Chinone Jens Chluba Hsiao-Mei Sherry Cho Steve Choi Gabriele Coppi Nicholas F. Cothard Kevin Coughlin Devin Crichton Kevin D. Crowley Kevin T. Crowley Ari Cukierman John M. D'Ewart Rolando Dünner Tijmen de Haan Mark Devlin Simon Dicker Joy Didier Matt Dobbs Bradley Dober Cody J. Duell Shannon Duff Adri Duivenvoorden Jo Dunkley John Dusatko Josquin Errard Giulio Fabbian Stephen Feeney Simone Ferraro Pedro Fluxà Katherine Freese Josef C. Frisch Andrei Frolov George Fuller Brittany Fuzia Nicholas Galitzki Patricio A. Gallardo Jose Tomas Galvez Ghersi Jiansong Gao Eric Gawiser Martina Gerbino Vera Gluscevic Neil Goeckner-Wald Joseph Golec Sam Gordon Megan Gralla Daniel Green Arpi Grigorian John Groh Chris Groppi Yilun Guan Jon E. Gudmundsson Dongwon Han Peter Hargrave Masaya Hasegawa Matthew Hasselfield Makoto Hattori Victor Haynes Masashi Hazumi Yizhou He Erin Healy Shawn W. Henderson Carlos Hervias-Caimapo Charles A. Hill J. Colin Hill Gene Hilton Matt Hilton Adam D. Hincks Gary Hinshaw Renée Hložek Shirley Ho Shuay-Pwu Patty Ho Logan Howe Zhiqi Huang Johannes Hubmayr Kevin Huffenberger John P. Hughes Anna Ijjas Margaret Ikape Kent Irwin Andrew H. Jaffe Bhuvnesh Jain Oliver Jeong Daisuke Kaneko Ethan D. Karpel Nobuhiko Katayama Brian Keating Sarah S. Kernasovskiy Reijo Keskitalo Theodore Kisner Kenji Kiuchi Jeff Klein Kenda Knowles Brian Koopman Arthur Kosowsky Nicoletta Krachmalnicoff Stephen E. Kuenstner Chao-Lin Kuo Akito Kusaka Jacob Lashner Adrian Lee Eunseong Lee David Leon Jason S. -Y. Leung Antony Lewis Yaqiong Li Zack Li Michele Limon Eric Linder Carlos Lopez-Caraballo Thibaut Louis Lindsay Lowry Marius Lungu Mathew Madhavacheril Daisy Mak Felipe Maldonado Hamdi Mani Ben Mates Frederick Matsuda Loïc Maurin Phil Mauskopf Andrew May Nialh McCallum Chris McKenney Jeff McMahon P. Daniel Meerburg Joel Meyers Amber Miller Mark Mirmelstein Kavilan Moodley Moritz Munchmeyer Charles Munson Sigurd Naess Federico Nati Martin Navaroli Laura Newburgh Ho Nam Nguyen Michael Niemack Haruki Nishino John Orlowski-Scherer Lyman Page Bruce Partridge Julien Peloton Francesca Perrotta Lucio Piccirillo Giampaolo Pisano Davide Poletti Roberto Puddu Giuseppe Puglisi Chris Raum Christian L. Reichardt Mathieu Remazeilles Yoel Rephaeli Dominik Riechers Felipe Rojas Anirban Roy Sharon Sadeh Yuki Sakurai Maria Salatino Mayuri Sathyanarayana Rao Emmanuel Schaan Marcel Schmittfull Neelima Sehgal Joseph Seibert Uros Seljak Blake Sherwin Meir Shimon Carlos Sierra Jonathan Sievers Precious Sikhosana Maximiliano Silva-Feaver Sara M. Simon Adrian Sinclair Praween Siritanasak Kendrick Smith Stephen R. Smith David Spergel Suzanne T. Staggs George Stein Jason R. Stevens Radek Stompor Aritoki Suzuki Osamu Tajima Satoru Takakura Grant Teply Daniel B. Thomas Ben Thorne Robert Thornton Hy Trac Calvin Tsai Carole Tucker Joel Ullom Sunny Vagnozzi Alexander van Engelen Jeff Van Lanen Daniel D. Van Winkle Eve M. Vavagiakis Clara Vergès Michael Vissers Kasey Wagoner Samantha Walker Jon Ward Ben Westbrook Nathan Whitehorn Jason Williams Joel Williams Edward J. Wollack Zhilei Xu Byeonghee Yu Cyndia Yu Fernando Zago Hezi Zhang Ningfeng Zhu

astro-ph.CO

It has recently been shown that the NP-hard problem of calculating the minimum number of hybridization events that is needed to explain a set of rooted binary phylogenetic trees by means of a hybridization network is fixed-parameter tractable if an instance of the problem consists of precisely two such trees. In this paper, we show that this problem remains fixed-parameter tractable for an arbitrarily large set of rooted binary phylogenetic trees. In particular, we present a quadratic kernel.

Leo van Iersel Simone Linz

q-bio.PE

In the near future, the overlap of the Rubin Observatory Legacy Survey of Space and Time (LSST) and the Simons Observatory (SO) will present an ideal opportunity for joint cosmological dataset analyses. In this paper we simulate the joint likelihood analysis of these two experiments using six two-point functions derived from galaxy position, galaxy shear, and CMB lensing convergence fields. Our analysis focuses on realistic noise and systematics models and we find that the dark energy Figure-of-Merit (FoM) increases by 53% (92%) from LSST-only to LSST+SO in Year 1 (Year 6). We also investigate the benefits of using the same galaxy sample for both clustering and lensing analyses, and find the choice improves the overall signal-to-noise by ~30-40%, which significantly improves the photo-z calibration and mildly improves the cosmological constraints. Finally, we explore the effects of catastrophic photo-z outliers finding that they cause significant parameter biases when ignored. We develop a new mitigation approach termed "island model", which corrects a large fraction of the biases with only a few parameters while preserving the constraining power.

Xiao Fang Tim Eifler Emmanuel Schaan Hung-Jin Huang Elisabeth Krause Simone Ferraro

astro-ph.CO

Recently, considerable effort has been put into developing fast algorithms to reconstruct a rooted phylogenetic network that explains two rooted phylogenetic trees and has a minimum number of hybridization vertices. With the standard approach to tackle this problem being combinatorial, the reconstructed network is rarely unique. From a biological point of view, it is therefore of importance to not only compute one network, but all possible networks. In this paper, we make a first step towards approaching this goal by presenting the first algorithm---called allMAAFs---that calculates all maximum-acyclic-agreement forests for two rooted binary phylogenetic trees on the same set of taxa.

Celine Scornavacca Simone Linz Benjamin Albrecht

q-bio.PE

Chern-Simons gauge theories coupled to massless fundamental scalars or fermions define interesting non-supersymmetric 3d CFTs that possess approximate higher-spin symmetries at large N. In this paper, we compute the scaling dimensions of the higher-spin operators in these models, to leading order in the 1/N expansion and exactly in the 't Hooft coupling. We obtain these results in two independent ways: by using conformal symmetry and the classical equations of motion to fix the structure of the current non-conservation, and by a direct Feynman diagram calculation. The full dependence on the 't Hooft coupling can be restored by using results that follow from the weakly broken higher-spin symmetry. This analysis also allows us to obtain some explicit results for the non-conserved, parity-breaking structures that appear in planar three-point functions of the higher-spin operators. At large spin, we find that the anomalous dimensions grow logarithmically with the spin, in agreement with general expectations. This logarithmic behavior disappears in the strong coupling limit, where the anomalous dimensions turn into those of the critical O(N) or Gross-Neveu models, in agreement with the conjectured 3d bosonization duality.

S. Giombi V. Gurucharan V. Kirilin S. Prakash E. Skvortsov

hep-th

Throughout the last decade, we have seen much progress towards characterising and computing the minimum hybridisation number for a set P of rooted phylogenetic trees. Roughly speaking, this minimum quantifies the number of hybridisation events needed to explain a set of phylogenetic trees by simultaneously embedding them into a phylogenetic network. From a mathematical viewpoint, the notion of agreement forests is the underpinning concept for almost all results that are related to calculating the minimum hybridisation number for when |P|=2. However, despite various attempts, characterising this number in terms of agreement forests for |P|>2 remains elusive. In this paper, we characterise the minimum hybridisation number for when P is of arbitrary size and consists of not necessarily binary trees. Building on our previous work on cherry-picking sequences, we first establish a new characterisation to compute the minimum hybridisation number in the space of tree-child networks. Subsequently, we show how this characterisation extends to the space of all rooted phylogenetic networks. Moreover, we establish a particular hardness result that gives new insight into some of the limitations of agreement forests.

Simone Linz Charles Semple

q-bio.PE cs.DS math.CO

Semi-directed phylogenetic networks have recently emerged as a class of phylogenetic networks sitting between rooted (directed) and unrooted (undirected) phylogenetic networks as they contain both directed as well as undirected edges. While the spaces of rooted phylogenetic networks and unrooted phylogenetic networks have been analyzed in recent years and various rearrangement moves to traverse these spaces have been introduced, the results do not immediately carry over to semi-directed phylogenetic networks. Here, we propose a simple rearrangement move for semi-directed phylogenetic networks, called cut edge transfer (CET), and show that the space of semi-directed level-$1$ networks with precisely $k$ reticulations is connected under CET. This level-$1$ space is currently the predominantly used search space for most algorithms that reconstruct semi-directed phylogenetic networks. Hence, every semi-directed level-$1$ network with a fixed number of reticulations and leaf set can be reached from any other such network by a sequence of CETs. By introducing two additional moves, CET$^+$ and CET$^-$, that allow for the addition or deletion of reticulations, we then establish connectedness for the space of all semi-directed phylogenetic networks on a fixed leaf set. As a byproduct of our results for semi-directed phylogenetic networks, we also show that the space of rooted level-$1$ networks with a fixed number of reticulations and leaf set is connected under CET, when translated into the rooted setting.

Simone Linz Kristina Wicke

math.CO q-bio.PE

In the study of rooted phylogenetic networks, analyzing the set of rooted phylogenetic trees that are embedded in such a network is a recurring task. From an algorithmic viewpoint, this analysis almost always requires an exhaustive search of a particular multiset $S$ of rooted phylogenetic trees that are embedded in a rooted phylogenetic network $\mathcal{N}$. Since the size of $S$ is exponential in the number of reticulations of $\mathcal{N}$, it is consequently of interest to keep this number as small as possible but without loosing any element of $S$. In this paper, we take a first step towards this goal by introducing the notion of a non-essential arc of $\mathcal{N}$, which is an arc whose deletion from $\mathcal{N}$ results in a rooted phylogenetic network $\mathcal{N}'$ such that the sets of rooted phylogenetic trees that are embedded in $\mathcal{N}$ and $\mathcal{N}'$ are the same. We investigate the popular class of tree-child networks and characterize which arcs are non-essential. This characterization is based on a family of directed graphs. Using this novel characterization, we show that identifying and deleting all non-essential arcs in a tree-child network takes time that is cubic in the number of leaves of the network. Moreover, we show that deciding if a given arc of an arbitrary phylogenetic network is non-essential is $Π_2^P$-complete.

Simone Linz Charles Semple

math.CO q-bio.PE