Mock Santiago. Abstract Book. Preparing for the Next Generation Surveys April Santiago, Chile.

Transcription

1 Abstract Book Mock Santiago Preparing for the Next Generation Surveys Santiago, Chile April Image credit: Eagle simulations

2 Rationale: The goal of this workshop is to bring together leading researchers in clustering and galaxy formation studies and key representatives from major future galaxy surveys to promote discussions and collaborations on how to produce realistic and useful mock galaxy catalogues needed to fully exploit the scientific outcome of those surveys. Scientific Organising Committee Nelson Padilla (Chair, Universidad Catolica de Chile) Carlton Baugh (Institute for Computational Cosmology, Durham University) Peder Norberg (Institute for Computational Cosmology, Durham University) Sergio Contreras (Universidad Catolica de Chile) Local Organising Committee Nelson Padilla (Chair) Joaquín Armijo Matías Bravo Roberto Gonzalez Esteban Jimenez Andrea Kulier Iván Lacerna Alejandra Muñoz Arancibia Enrique Paillas Paulina Troncoso Madusha Gunawardhana Host Centro de Astro-Ingeniería, Universidad Catolica de Chile Instituto de Astrofísica, Universidad Catolica de Chile This workshop is sponsored by the Newton-CONICYT fund, by BASAL Centro de Astronomía y Tecnologías Afines PFB-06, VRI-PUC, and Fondecyt Regular Abstract Book www2.astro.puc.cl/mocksantiago/ 2

3 List of Participants María Celeste Artale (IAFE) Carlton Baugh (ICC) Lucas Bignone (IAFE) Guillermo Blanc (U. de Chile) Matías Bravo (PUC) Yanchuan Cai (University of Edinburgh) Francisco Castander (ICE) Shaun Cole (ICC) Johan Comparat (UAM) Andy Connolly (UW) Sergio Contreras (PUC) Sofia Cora (IALP) Carlos Correa (IATE) Darren Croton (Swinburne) Joe DeRose (Stanford) Mariano Domínguez (IATE) Francisco Förster (University de Chile) Jaime Forero-Romero (Universidad de los Andes) Gaspar Galaz (PUC) Eric Gawiser (Rutgers University) Roberto Gonzalez (PUC) Violeta Gonzalez-Perez (ICG) Gian Luigi Granato (INAF) Shirley Ho (CMU) Esteban Jimenez (PUC) Antonios Katsianis (U. de Chile) Iván Lacerna (PUC) Claudia Lagos (ICRAR) Diego Lambas (IATE) Sebastián López (U. de Chile) Nuala McCullagh (ICC) Julian Mejia-Restrepo (U. de Chile) Andrés Meza (UNAB) Nicolás Meza (PUC) Ben Moster (Ludwig-Maximilians-University, Munich) Martín Moyano (UNC) Tomas Muller (PUC) Roberto Muñoz (PUC) Alejandra Muñoz Arancibia (PUC) David Murphy (Cambridge) Peder Norberg (ICC) Álvaro Orsi (CEFCA) Nelson Padilla (PUC) Enrique Paillas (PUC) Dante Paz (IATE) Susana Pedrosa (IAFE) Joaquín Prieto (U. de Chile) Facundo Rodríguez (IATE) Silvio Rodríguez (IATE) Yetli Rosas-Guevara (U. de Chile) Andrés Ruiz (IATE) Salvador Salazar (MPE) Ariel Sanchez (MPE) Matthieu Schaller (ICC) Claudia Scoccola (IAFE) Mario Sgro (IAFE) Adam Stevens (Swinburne) Jeremy Tinker (NYU) Patricia Tissera (UNAB) Ezequiel Treister (PUC) Paulina Troncoso (PUC) Cristian Vega (IALP) Carolina Villalón (IATE) Idit Zehavi (Case Western Reserve University) Zheng Zheng (University of Utah) Zhenya Zheng (PUC) Abstract Book www2.astro.puc.cl/mocksantiago/ 3

4 Scientific Programme Monday 18 April Session-I: Surveys Time: 9:30am 11:10am Chair: Name Please Time Speaker Title Abstract 09:30 10:10 Shaun Cole The rise of galaxy surveys and mocks (with DESI progress and challenges) 10:10 10:30 Álvaro Orsi The J-PAS Survey: Probing the Universe in 59 colours p.11 10:30 10:50 Zhenya Zheng Ly-Alpha Galaxies at the End of Reionization, the LAGER project p.11 10:50 11:10 Peder Norberg WAVES and MOONS: the next large and faint spectroscopic surveys p.11 p.12 11:10 11:40 Coffee Break Session-II: Statistics Time: 11:40am 13:20pm Chair: Name Please 11:40 12:20 Ariel Sanchez Cosmological implications of anisotropic clustering measurements 12:20 12:40 Silvio Rodríguez in the final BOSS p.12 The real shape of galaxies: Intrinsic and environmental factors p.12 12:40 13:00 Andrés Ruiz Calibration of Semi-Analytical Models using Particle Swarm 13:00 13:20 Enrique Paillas Optimization p.13 Baryon effects on void statistics p.13 13:20 14:50 Lunch at Clementina Session-III: Mocks with SAMs and HOD Time: 14:50pm 16:30pm Chair: Name Please 14:50 15:30 Zheng Zheng Redshift-Space Galaxy Clustering: Accurate Mocks from Accurate Modeling 15:30 15:50 Idit Zehavi The evolving relation between galaxies and dark matter halos p.14 p.13 Abstract Book www2.astro.puc.cl/mocksantiago/ 4

5 15:50 16:10 Claudia Scoccola 16:10 16:30 Nuala McCullagh MultiDark PATCHY Mocks p.14 Testing the assumptions of SHAM and HOD models with Galform p.14 16:30 17:00 Coffee Break Time: 17:00pm 18:00pm Session-IV: Discussions Led by: Andy Connolly, Shaun Cole and Idit Zehavi Abstract Book www2.astro.puc.cl/mocksantiago/ 5

6 Tuesday 19 April Session-I: Why SAMs or Hydro? Time: 9:30am 12:20pm Chair: Name Please Time Speaker Title Abstract 09:30 10:10 Claudia Lagos A discussion on semi-analytic models and hydro-simulations: 10:10 10:30 María Celeste Artale 10:30 10:50 Violeta Gonzalez- Perez 10:50 11:10 Matthieu Schaller which one, when and why p.14 Galaxy clustering in EAGLE compared to GAMA and Illustris p.15 Eagle, L-Galaxies and Galform p.15 Mock galaxy catalogue from hydrodynamical simulations. The example of EAGLE p.15 11:10 11:40 Coffee Break 11:40 12:00 Patricia Chemical Abundances of gas and stars in discs using p.16 Tissera hydrodynamical simulations 12:00 12:20 Adam Stevens Angular-momentum evolution of galaxies from semi-analytics p.16 12:20 12:40 Alejandra Modeling complex emission processes in galaxy populations p.16 Muñoz Arancibia through the Proxy+Matching technique 12:40 13:00 Nelson Padilla Nifty comparison of semi-analytic and HOD galaxy models p.17 13:00 13:20 Sergio Contreras The galaxy - dark matter halo connection p.17 13:20 14:50 Lunch Session-II: Surveys Time: 14:50pm 16:30pm Chair: Name Please 14:50 15:10 Shirley Ho How we learn to love the BOSS and planning for the future p.18 15:10 15:30 David Murphy Where s our Southern Sloan? Future prospects for spectrally mapping the southern sky p.18 Abstract Book www2.astro.puc.cl/mocksantiago/ 6

7 15:30 15:50 Guillermo The Hobby Eberly Telescope Dark Energy Experiment p.18 Blanc (HETDEX) Pilot Survey: Using LAEs for Cosmology 15:50 16:10 Francisco The MICE simulations mock catalogues p.19 Castander 16:10 16:30 Eric Gawiser Optimizing Survey Design for Galaxy Clustering with HETDEX and LSST p.19 16:30 17:00 Coffee Break Time: 17:00pm 18:00pm Session-III: Discussions Led by: Carlton Baugh, Shirley Ho and Eric Gawiser 20:00 23:00 Workshop Dinner Abstract Book www2.astro.puc.cl/mocksantiago/ 7

8 20 April Session-I: Surveys Time: 9:30am 10:50pm Chair: Name Please Time Speaker Title Abstract 09:50 10:10 Paulina Troncoso 10:10 10:30 Johan Comparat 10:30 10:50 Andy Connolly 10:50 11:10 Roberto Muñoz The evolution of Balmer jump selected galaxies in the ALHAMBRA survey p.19 Clustering properties of g-selected galaxies at z=0.8 p.20 From cosmology to pixels: an end-to-end framework for simulating data from the LSST p.20 Chasing ghost galaxies in the Fornax galaxy cluster p.21 11:10 11:40 Coffee Break Session-II: Why SAMs or Hydro? Time: 10:50am 13:20pm Chair: Name Please 11:40 12:00 Sofia Cora Semi-analytic model SAG p.21 12:00 12:20 Carlton Baugh 12:20 12:40 Susana Pedrosa Semi-analytical modelling of galaxy formation p.21 Morphological evolution and angular momentum content for galaxies in a Λ-CDM scenario 12:40 13:00 Darren Croton The TAO of SAGE and the challenge of building a virtual observatory p.22 p.22 Session-III: Statistics Time: 14:50am 15:10pm Chair: Name Please 13:00 13:20 Yanchuan Cai Simulating the Gravitational Redshift from Stacked Clusters p.22 13:20 14:50 Lunch Abstract Book www2.astro.puc.cl/mocksantiago/ 8

9 14:50 15:10 Dante Paz New tools for improving the precision of measurements on the p.23 next-generation of LSS experiments 15:10 15:30 Iván Lacerna Assembly bias in galaxies p.23 15:30 15:50 Salvador Clustering tomography on the final SDSS-III BOSS galaxy sample p.23 Salazar 15:50 16:10 Roberto Local Group Analogues p.24 Gonzalez 16:10 16:30 Gaspar Galaz Re-discovering giant low surface brightness galaxies through simulations: a pending issue p.24 16:30 17:00 Coffee Break Lucas Bignone Session-IV: Poster Presentations Time: 17:00pm 18:00pm Chair: Name Please Non-parametric morphological merger indicators in the Illustris simulation Mario Sgro Anisotropic Halo Model p.27 Joaquín Prieto The origin of spin in galaxies: clues from simulations of atomic cooling haloes Matías Bravo p.28 Antonios Katsianis The simulated SFR-M relation in hydrodynamic simulations p.28 Esteban Jimenez p.29 Yetli Rosas-Guevara Black hole Evolution in the EAGLE Universe p.29 Facundo Rodríguez Carlos Correa Álvaro Orsi Determination of halo occupation distribution: Comparison between mock and observational catalogues Feasibility study of the Alcock-Paczyński cosmological test using cosmic voids Probing the growth of structure with different galaxy selections and redshift uncertainties C. Villalón Satellite Accretion in a ΛCDM Universe p.30 Martín de los Rios The Messi (Merging Systems Identification) Algorithm p.31 p.27 p.27 p.29 p.29 p.30 Abstract Book www2.astro.puc.cl/mocksantiago/ 9

10 Thursday 21 April Session-I: Mocks with SAMs and HOD Time: 9:30am 12:00pm Chair: Name Please Time Speaker Title Abstract 09:30 09:50 Jeremy Tinker Making Mocks with the Quick Particle Mesh Method p.24 09:50 10:10 Mariano Domínguez QSOs mocks catalogues and LSS p.25 10:10 10:30 Ben Moster Galaxy Assembly in Dark Matter Haloes p.25 10:30 10:50 Joe DeRose Mocks for the Dark Energy Survey and Beyond p.25 10:50 11:10 Cristian Vega Semi-Analytic Galaxies from the MassiveBlack II simulation p.26 11:10 11:40 Coffee Break Time: 12:00pm 13:00pm Session-II: Discussions Led by: Patricia Tissera, Claudia Lagos and Ariel Sanchez Concluding Remarks Time: 12:00pm 13:00pm By: Diego Lambas 13:20 14:50 Lunch Hands on Workshops Time: 14:50pm 18:00pm 14:50 16:30 Sergio Contreras MySQL databases 16:30 17:00 Coffee Break 16:30 18:00 F. Förster LSST MAF Abstract Book www2.astro.puc.cl/mocksantiago/ 10

11 Talk Abstracts Monday 09:30 10:10 The rise of galaxy surveys and mocks (with DESI progress and challenges) Shaun Cole (ICC, University of Durham) I will report on what is required for some aspects of the DESI surveys, the progress we have made and some of the challenges that remain. Monday 10:10 10:30 The J-PAS Survey: Probing the Universe in 59 colours Álvaro Orsi (CEFCA) Typical models of anisotropic clustering have achieved only partial agreement against N-body simulations and standard HOD prescriptions. As a result, clustering data used to constrain cosmological parameters is restricted to a limited range of scales. Here we explore the performance of such models when confronted against galaxies from a semi-analytical model run over a very large N-body simulation. We focus on galaxies selected by stellar mass and star-formation rate. The minimum scale that models can reproduce within a few percent depends on the target selection and the number density of the samples. Furthermore, we explore how models perform when the input real-space clustering (measured from the simulation) is used instead of a linear theory approximations. Implications for future surveys are discussed. Monday 10:30 10:50 Ly-Alpha Galaxies at the End of Reionization, the LAGER project Zhenya Zheng (PUC) High redshift Lyman-alpha galaxies (LAEs) probe the cosmic re-ionization, as the increasing IGM neutral hydrogen fraction can heavily attenuate the Lya photons, leading to apparent decline in the Lya luminosity function. Such declination likely happens at z 7 according to recent observations, implying a rapid reionization. However, due to the limited survey area, very few LAEs have been confirmed at z 7. The superb large field of view and the high throughput at red wavelengths of DECam make it a unique and one of the most powerful instruments to the search for large sample of LAEs at z 7.0. A dedicated narrowband filter at 9640A is being built, and we aim to detect several hundred of z 7.0 LAEs with a deep and large area DECam narrowband survey. In this talk we introduce our DECam NB964 survey (The Lyman-Alpha Galaxies at the End of Reionization, LAGER), make comparison with current z 7 narrowband surveys, and present how it will constrain the ionization fraction of our universe at z = 7 (with Lya luminosity function, LAE clustering, as well as the Lya line profile in the follow-up spectroscopic work). Abstract Book www2.astro.puc.cl/mocksantiago/ 11

12 Our survey may also be effective to find high-z quasars, Lyman break galaxies and low-z emission line galaxies (e.g., Ha emitters at z 0.5, O iii emitters at z 0.9, and O ii emitters at z 1.5), which will help to determine the faint end (for ELG) and bright end (for LBG and quasar) of their luminosity function. Monday 10:50 11:10 WAVES and MOONS: the next large and faint spectroscopic surveys Peder Norberg (ICC, University of Durham) No Abstract Monday 11:40 12:20 Cosmological implications of anisotropic clustering measurements in the final BOSS Ariel Sanchez (Max Planck Institute for Extraterrestrial Physics) Thanks to the combined information of BAO and RSD, anisotropic clustering measurements can probe simultaneously the expansion history of the Universe and the growth of density fluctuations, offering in this way one of the most promising routes to constrain the dark energy equation of state parameter, wde, and its possible evolution with time, or to detect possible deviations from the predictions of general relativity. The potential of LSS observations as cosmological probes has led to the construction of increasingly larger galaxy catalogues, such as the completed Baryon Oscillation Spectroscopic Survey (BOSS). In this talk, I will review some of the cosmological implications of anisotropic clustering measurements in the final BOSS. Monday 12:20 12:40 The real shape of galaxies: Intrinsic and environmental factors Silvio Rodríguez (IATE - OAC, Cordoba) By modelling the axis ratio distribution of SDSS DR8 galaxies we find the intrinsic 3D shapes of spirals and ellipticals. We use morphological information from the Galaxy Zoo project and assume a non-parametric distribution intrinsic of shapes, while taking into account dust extinction. We find that the intrinsic shapes of galaxies and their dust extinction vary with absolute magnitude, colour and physical size. We find that bright elliptical galaxies are more spherical than faint ones, a trend that is also present with galaxy size, and that there is no dependence of elliptical galaxy shape with colour. For spiral galaxies we find that the thickness of discs increases with luminosity and size, and that brighter, smaller and redder galaxies have less round discs. We also measure the effect of the environment on the intrinsic shapes of galaxies. We find that spiral galaxies in groups are very similar to field spirals with similar intrinsic properties (magnitudes, sizes and colours). But for spirals in groups, those in denser environments or closer to the centre of the group tend to have a more circular disc than similar galaxies in less dense environments or far from the group Abstract Book www2.astro.puc.cl/mocksantiago/ 12

13 centres. Also we find that central spiral galaxies in their groups tend to be thinner than other similar spirals. For ellipticals, we do not find any important dependence of their shape on their position in a group or on the local density. However, we find that elliptical galaxies in groups tend to be more spherical than field ellipticals with similar intrinsic properties. Monday 12:40 13:00 Calibration of Semi-Analytical Models using Particle Swarm Optimization Andrés Ruiz (IATE - OAC) In this talk I briefly present a fast and accurate method to select an optimal set of parameters in semi-analytic models of galaxy formation. Our approach compares the results of a model against a set of observables applying a stochastic technique called Particle Swarm Optimization (PSO), a self-learning algorithm for localizing regions of maximum likelihood in multidimensional spaces that outperforms traditional sampling methods in terms of computational cost. Monday 13:00 13:20 Baryon effects on void statistics Enrique Paillas (PUC) EAGLE provides a unique opportunity to test the effects of baryons on the statistics of voids. Several works have studied the abundance of voids in numerical simulations (e.g. Cai, Padilla & Li 2014), with the aim of using these statistics to tell apart different cosmological models. However, in these simulations only the evolution of the dark matter (DM) is followed. At best, DM haloes are used to trace the density field in an attempt to simulate what happens when galaxies are used to identify voids in real catalogues. With EAGLE we can quantify the effects from baryons. These range from the change in the DM halo mass function due to feedback, the multiple galaxies that inhabit each halo, and the effect of feedback on other scales. For instance, it is possible that the walls and filaments that constitute the void boundaries are different when baryons are present. We will use the DM-only and full EAGLE simulations to test these effects, primarily on the abundance of voids, but also on their density and dynamics profiles. Monday 14:50 15:30 Redshift-Space Galaxy Clustering: Accurate Mocks from Accurate Modelling Zheng Zheng (University of Utah) With the increasing precision of galaxy clustering measurements from ongoing and forthcoming large galaxy surveys, accurate models are required to interpret the redshift-space data, to extract relevant information, and to produce reliable mock catalogs. I will first present a method based on halos identified in high-resolution N-body simulations to accurately and efficiently model the projected and redshift-space galaxy two-point correlation functions, which enables an efficient exploration of the parameter space. I then talk about the applications of such a method to model the small-to-intermediate scale redshift-space clus- Abstract Book www2.astro.puc.cl/mocksantiago/ 13

14 tering of SDSS and BOSS galaxies and discuss the inferred galaxy-halo relation and galaxy velocity bias. Finally, I will comment on constructing redshift-space mock galaxy catalogs from the modelling results. Monday 15:30 15:50 The evolving relation between galaxies and dark matter halos Idit Zehavi (Case Western Reserve University) The Halo Occupation Distribution (HOD) approach is a powerful tool for interpreting galaxy clustering measurements and constraining the galaxy-halo connection. We present new results for the redshift evolution of the HOD predicted by semi-analytic galaxy formation models. This allows to extend the HOD approach and facilitates the creation of realistic mock galaxy catalogs for upcoming surveys. Monday 15:50 16:10 MultiDark PATCHY Mocks Claudia Scoccola (FCAG-UNLP) No Abstract Monday 16:10 16:30 Testing the assumptions of SHAM and HOD models with Galform Nuala McCullagh (ICC, University of Durham) I will discuss current work on using the Galform P-Millennium galaxy catalogue to test the assumptions made in subhalo abundance matching (SHAM) and halo occupation distribution (HOD) models. While the clustering in the Galform catalogue matches the observed clustering in SDSS, the form of the halo occupation distributions are quite different from both the HODs resulting from SHAM and the standard HOD models assumed in the literature. This allows us to test the assumption of standard HODs and to explore our sensitivity to different HOD forms. Tuesday 09:30 10:10 A discussion on semi-analytic models and hydro-simulations: which one, when and why Claudia Lagos (ICRAR) Semi-analytic models and hydrodynamical simulations are two widely used tools to study the connection between the growth of structures in the Universe and how this drives the formation and evolution of galaxies. Both tools have valuable characteristics that can be very useful in different circumstances, but to be able to maximise the science coming out of both tools is critical to understand their advantages and limitations and which type of surveys would mostly benefit of each of these tools. During this talk I will discuss when and Abstract Book www2.astro.puc.cl/mocksantiago/ 14

15 why semi-analytic models are preferred over hydro-simulations and vice-versa. Tuesday 10:10 10:30 Galaxy clustering in EAGLE compared to GAMA and Illustris María Celeste Artale (Instituto de Astronomía y Física del Espacio) We measure the projected galaxy correlation function from the cosmological hydrodynamical simulation EAGLE. We compare the clustering of samples split by luminosity, stellar mass and star formation rate with results from the GAMA survey, with two semi-analytic galaxy formation models and with the hydrodynamical cosmological simulation Illustris. Our findings indicate that the galaxy clustering in EAGLE presents a good level of agreement with GAMA and that differences in the clustering between EAGLE, Illustris and the semi-analytic models provide key insight on the different galaxy formation physics implemented in the models. Tuesday 10:30 10:50 Eagle, L-Galaxies and Galform Violeta Gonzalez-Perez (ICG, University of Portsmouth) No Abstract Tuesday 10:50 11:10 Mock galaxy catalogue from hydrodynamical simulations. The example of EAGLE Matthieu Schaller (ICC, University of Durham) In this talk, I ll present the current and future content of the public database constructed from the galaxy catalogues from the EAGLE hydrodynamical simulations. Hydrodynamical simulations are run on much smaller volumes than what is doable with Semi-Analytic models. However, the more complex modelling involved allows to include the back-reaction of baryons onto the dark matter, which plays an important role for precision cosmology probes. Another benefit over Semi-Analytic Models is the possibility to generate mock images in multiple bands, mock IFU cubes or extract morphological information from the galaxies. I ll argue that information from hydrodynamical simulations combined with SAMs should be at the heart of future mock catalogue efforts. Abstract Book www2.astro.puc.cl/mocksantiago/ 15

16 Tuesday 11:40 12:00 Chemical Abundances of gas and stars in discs using hydrodynamical simulations Patricia Tissera (UNAB) No Abstract Tuesday 12:00 12:20 Angular-momentum evolution of galaxies from semi-analytics Adam Stevens (UNAB) Using "Dark SAGE", a new semi-analytic model with consideration of resolved disc structure, I will present the evolution of the mass specific angular momentum relation of galactic discs. This sequence has strong ties to Toomre disc instabilities, which I will show are mandatory for regulating the mass spin sequence. Our method of discretising discs in annuli of fixed specific angular momentum leads to the natural formation of pseudobulges in most spiral galaxies. With a simple disc pseudobulge decomposition, we find our model predicts the mass and spin of galaxies to be tightly correlated, in remarkable agreement with observations. Tuesday 12:20 12:40 Modeling complex emission processes in galaxy populations through the Proxy+Matching technique Alejandra Muñoz Arancibia (IFA-UV) We introduce a novel technique for modeling luminosities at different wavelengths in large samples of galaxies, suitable for emission processes whose complexity requires many untested assumptions or the use of sophisticated algorithms: in the "Proxy+Matching" approach, a physical galaxy property from the model is chosen as a proxy for another property whose numerical value is unknown. Both proxy and unknown are assumed to follow a monotonic relationship, assigning that unknown to the simulated galaxies in such a way that some observational statistics for it are reproduced. By comparing the predictions for further galaxy properties with observations, a good proxy can be found. We present the prospects of this technique for probing the submillimeter and Lyman alpha emission from galaxies in a cosmological framework, using a semi-analytic model of galaxy formation and evolution. Abstract Book www2.astro.puc.cl/mocksantiago/ 16

17 Tuesday 12:40 13:00 Nifty comparison of semi-analytic and HOD galaxy models Nelson Padilla (Swinburne University of Technology) The nifty project compares the output of 12 semi-analytic and 2 halo occupation distribution models, all of which use the same parent simulation. Results of this comparison on the abundance of galaxies as a function of their intrinsic properties, and their clustering will be shown. Tuesday 13:00 13:20 The galaxy - dark matter halo connection Sergio Contreras (PUC) We demonstrate how the properties of a galaxy depend on the mass of its host dark matter subhalo, using two independent models of galaxy formation. For the cases of stellar mass and black hole mass, the median property value displays a monotonic dependence on subhalo mass. The slope of the relation changes for subhalo masses for which heating by active galactic nuclei becomes important. The median property values are predicted to be remarkably similar for central and satellite galaxies. The two models predict considerable scatter around the median property value, though the size of the scatter is model dependent. There is only modest evolution with redshift in the median galaxy property at a fixed subhalo mass. Properties such as cold gas mass and star formation rate, however, are predicted to have a complex dependence on subhalo mass. In these cases subhalo mass is not a good indicator of the value of the galaxy property. We illustrate how the predictions in the galaxy property - subhalo mass plane differ from the assumptions made in some empirical models of galaxy clustering by reconstructing the model output using a basic subhalo abundance matching scheme. In its simplest form, abundance matching generally does not reproduce the clustering predicted by the models, typically resulting in an overprediction of the clustering signal. Using the predictions of the galaxy formation model for the correlations between pairs of galaxy properties, the basic abundance matching scheme can be extended to reproduce the model predictions more faithfully for a wider range of galaxy properties. Our results have implications for the analysis of galaxy clustering, particularly for low abundance samples. Abstract Book www2.astro.puc.cl/mocksantiago/ 17

18 Tuesday 14:50 15:10 How we learn to love the BOSS and planning for the future Shirley Ho (Carnegie Mellon University) No Abstract Tuesday 15:10 15:30 Where s our Southern Sloan? Future prospects for spectrally mapping the southern sky David Murphy (Cambridge University) Efforts to fully explore the southern hemisphere have gained traction, with large photometric campaigns (e.g. VST-ATLAS, DES, VHS) covering vast regions with multi-band photometry spanning from 350nm to 2000nm. Nevertheless, one of the core legacy products driving Northern SDSS science is access to spectra alongside these photometric resources. I highlight the current situation in Chile for spectroscopic support of the above southern surveys, and what the future holds, particularly for LSST-era science. Tuesday 15:30 15:50 The Hobby Eberly Telescope Dark Energy Experiment (HETDEX) Pilot Survey: Using LAEs for Cosmology Guillermo Blanc (University de Chile) I will present the HETDEX Survey, an ambitious project that aims to obtain blind integral field spectroscopy over hundreds of square degrees in order to assemble a sample of 1 million Ly-alpha emitting galaxies at 1.8<z<3.5. The main goal of HETDEX is to measure the galaxy distribution power spectrum in order to study the evolution of the Dark Energy equation of state out to high redshift. Beyond the study of cosmology the "blind" nature of HETDEX will translate into a massive and diverse spectroscopic dataset that will include large numbers high redshift and local galaxies, AGNs, MW stars, planetary nebulae around nearby galaxies, and any other source falling on the survey footprint. Therefore HETDEX will provide a rich database for all kinds of studies in astrophysics. I will describe the survey strategy, present the VIRUS spectrograph which is currently being commissioned at the HET 9.2m telescope, and discuss early results from the HETDEX Pilot Survey Abstract Book www2.astro.puc.cl/mocksantiago/ 18

19 Tuesday 15:50 16:10 The MICE simulations mock catalogues Francisco Castander (ICE, IEEC-CSIC) I will present the MICE cosmological simulations and associated mock galaxy catalogues ( pic.es) that have been developed to help design and analyse current and future cosmological surveys. In particular, they contain lensing and clustering observables computed in a self-consistent way in a cosmological relevant volume. I will present how they are being used to analyse the first LSS results coming from the DES and being optimized to interpret future surveys like PAU, DESI and Euclid. Tuesday 16:10 16:30 Optimizing Survey Design for Galaxy Clustering with HETDEX and LSST Eric Gawiser (Rutgers University) To take full advantage of the statistics offered by huge galaxy samples, large-scale structure studies with current and future surveys require improved methods for reducing systematic errors. I will give examples of two approaches that are relevant to the construction of mock galaxy catalogs: 1. Choosing an LSST dither pattern that minimizes spurious galaxy clustering caused by non-uniformity in survey depth. 2. Applying Bayesian and Machine Learning techniques to HETDEX classification of emission line galaxies in redshift space. 09:50 10:10 The evolution of Balmer jump selected galaxies in the ALHAMBRA survey Paulina Troncoso (PUC) In this talk, I present a new color-selection technique, based on the Bruzual & Charlot (2003) models convolved with the ALHAMBRA bands. We use the homogeneous optical coverage of the ALHAMBRA filter system to select samples of star-forming galaxies at different epochs of the Universe and study their properties. The redshifted position of the Balmer jump in the optical bands is used to select star-forming galaxies in the redshift range 0.5 < z < 1.5, those are dubbed Balmer jump Galaxies (BJGs). Five volumelimited BJG sub-samples with different mean redshifts are found to reside in haloes of median masses ±0.2 Mo slightly increasing toward z = 0.5. This increment is similar to numerical simulations results which suggests that we are tracing the evolution of an evolving population of haloes as they grow to reach a mass of ±0.1 M at z = 0.5. The likely progenitors of our samples at z 3 are Lyman Break Galaxies, which at z 2 would evolve into star forming BzK galaxies, and their descendants in the local Universe are elliptical galaxies. Hence, this allows us to follow the putative evolution of the SFR, stellar mass and age of these galaxies. From z = 1.0 to z = 0.5, the stellar mass of the volume limited BJG samples nearly does not change with redshift, suggesting that major mergers play a minor role on the evolution of these galaxies. The SFR evolution accounts for the small variations of stellar mass, suggesting that star Abstract Book www2.astro.puc.cl/mocksantiago/ 19

20 formation and possible minor mergers are the main channels of mass assembly. 10:10 10:30 Clustering properties of g-selected galaxies at z = 0.8 Johan Comparat (IFT/CSIC UAM Madrid Spain) Current and future large redshift surveys, as the Sloan Digital Sky Survey IV extended Baryon Oscillation Spectroscopic Survey (SDSS-IV/eBOSS) or the Dark Energy Spectroscopic Instrument (DESI), will use Emission-Line Galaxies (ELG) to probe cosmological models by mapping the large-scale structure of the Universe in the redshift range 0.6 < z < 1.7. With current data, we explore the halo-galaxy connection by measuring three clustering properties of g-selected ELGs as matter tracers in the redshift range 0.6 < z < 1: (i) the redshift-space two-point correlation function using spectroscopic redshifts from the BOSS ELG sample and VIPERS; (ii) the angular two-point correlation function on the footprint of the CFHT-LS; (iii) the galaxy-galaxy lensing signal around the ELGs using the CFHTLenS. We interpret these observations by mapping them onto the latest high-resolution MultiDark Planck N-body simulation, using a novel (Sub)Halo-Abundance Matching technique that accounts for the ELG incompleteness. ELGs at z 0.8 live in halos of (1 ± 0.5) h 1 M and 22.5±2.5% of them are satellites belonging to a larger halo. The halo occupation distribution of ELGs indicates that we are sampling the galaxies in which stars form in the most efficient way, according to their stellar-to-halo mass ratio. 10:30 10:50 From cosmology to pixels: an end-to-end framework for simulating data from the LSST Andy Connolly (University of Washington) The LSST will, over a 10-year period, produce a multi-color, multi-epoch survey of more than square degrees of the southern sky. The end product of the LSST will be an archive of images and catalogs from which a wide variety of high-precision statistical studies can be undertaken. To accomplish this, the LSST project has developed a multi-facetted suite of modeling and simulation tools for use in developing the system requirements and architecture, and validating that the system design and the as-delivered components will yield data products with the required statistical properties. I will describe the development, validation, and use of the LSST simulation framework, including the generation of simulated catalogs and images for targeted trade studies, the creation of large-scale simulations that test the procedures for data calibration, and use of end-to-end image simulations to evaluate the performance of the system as a whole. I will also show how new cosmological models can be integrated within this framework to develop a simulated digital view of the universe. Abstract Book www2.astro.puc.cl/mocksantiago/ 20

21 10:50 11:10 Chasing ghost galaxies in the Fornax galaxy cluster Roberto Muñoz (PUC) The Fornax galaxy cluster is the second richest cluster within 100 million light years from Earth. Because of its proximity, which ensures optimal spatial resolution in comparison with more distant clusters, Fornax is an excellent laboratory to study the physical properties of galaxies and dense stellar systems, such as globular clusters (GCs) and ultra-compact dwarf galaxies (UCDs). We have embarked on a multi-wavelength study (DECam/ optical, VISTA/ NIR, VIMOS/ spectroscopy) of the Fornax galaxy cluster over the central 1.5 Mpc 2 central region, which will allows us to image about 10,000 GCs at previously not covered wavelengths and provide accurate photometric diagnostics for more than 100 massive galaxies down to M V =-12 mag. 11:40 12:00 Semi-analytic model SAG Sofia Cora (Instituto de Astrofísica de La Plata, Argentina) Semi-analytic models of galaxy formation and evolution (SAMs) are a powerful method to study how galaxies form and evolve within individual dark matter halos in a CDM cosmogony provided by N-body simulations. SAMs incorporates the physical processes that affect the baryonic component, with the advantage of reaching a larger dynamic range than fully selfconsistent hydro-simulations at a far smaller computational cost. We present the state-of-art of the semi-analytic model SAG. This model follows the formation and evolution of galaxies including gas cooling, star formation, SNe explosions and AGN feedback. Bulge formation and black hole growth take place through starbursts driven by mergers and disc instabilities. SAG has a detailed implementation of metal enrichment of stars and interstellar medium which involves yields from supernovae type II and Ia taking into account the corresponding lifetimes of their progenitors. It also considers the effect of gradual star formation during starbursts, of accretion with misaligned angular momenta on the properties of galactic disks, and of environmental processes such as tidal stripping and ram pressure stripping. A special feature of SAG is the possibility of estimating nebular emission of star-forming galaxies. In this presentation, we show the main achievements of this model, which is able to reproduce observed properties of both local and high redshift galaxies. 12:00 12:20 Semi-analytical modelling of galaxy formation Carlton Baugh (ICC, University of Durham) I will give an overview of the semi-analytical approach to modelling galaxy formation and explain how it can be used to build mock catalogues. Abstract Book www2.astro.puc.cl/mocksantiago/ 21

22 12:20 12:40 Morphological evolution and angular momentum content for galaxies in a Λ-CDM scenario Susana Pedrosa (IAFE) Galaxy formation in the current cosmological paradigm is a very complex process where inflows, outlfows, interactions and mergers are common events. These processes can redistribute the angular momentum content of baryons. Recent observational results suggest that disc formed conserving angular momentum while elliptical galaxies, albeit losing angular momentum, determine a correlation between the specific angular momentum of the galaxy and the stellar mass. These observations provide stringent constrain for galaxy formation models in a hierarchical clustering scenario. We use cosmological hydrodynamical simulations that include an effective, physically-motivated Supernova feedback to analyse the properties and formation history of a sample of galaxies of a cosmological simulation by performing a bulge-disc decomposition of the analysed systems and their progenitor systems. 12:40 13:00 The TAO of SAGE and the challenge of building a virtual observatory Darren Croton (Swinburne University of Technology) In this talk I will discuss the use of new technologies to build and deliver cosmological-scale galaxy formation simulations to the astronomy community. Combining high performance computing, a "web 2.0" front-end architecture, and cloud-based processing and storage, the Australian Government funded "Theoretical Astrophysical Observatory" (TAO; allows astronomers construct their own mock universes from a range of different simulations, filter the output through virtual telescopes, and download the results for their own scientific use. TAO is of value to both large survey teams and individuals, and serves a wide range of scientific needs. 13:00 13:20 Simulating the Gravitational Redshift from Stacked Clusters Yanchuan Cai (University of Edinburgh) Photons from central galaxies sitting at the bottom of the potential well of galaxy clusters are expected to be gravitationally shifted by a larger amount than satellites and other neighbouring galaxies. The difference of the gravitational redshift signal with respect to the cluster centre is small but can in principle be detected by stacking a large sample of clusters. A robust detection of the gravitational redshift signal using near future galaxy redshift surveys may provide a constraint on theories of gravity. This requires an accurate prediction of the observed redshift and a thorough understanding of systematics. Using N-body simulations, I will make predictions for such a signal and show how it may be affected by systematics such as the assumption that individual clusters are spherical symmetric. Abstract Book www2.astro.puc.cl/mocksantiago/ 22

23 14:50 15:10 New tools for improving the precision of measurements on the next-generation of LSS experiments Dante Paz (Instituto de Astronomía Teórica y Experimental - IATE) The estimation of cosmological constraints from observations of the large-scale structure of the Universe, such as the power spectrum or the correlation function, requires the knowledge of the inverse of the associated covariance matrix, namely the precision matrix, Ψ. In most analysis, Ψ is estimated from a limited set of mock catalogs. Depending on how many mocks are used, this estimation has an associated error which must be propagated into the final cosmological constraints. For future surveys such as Euclid and Dark Energy Spectroscopic Instrument, the control of this additional uncertainty requires a prohibitively large number of mock catalogs. In a recent work our group have presented a novel technique for the estimation of the precision matrix, the covariance tapering method, which has a promising future in BAO or Cosmic Voids based measurements. In this talk I will review some of these results in the context of the community efforts for improving the accuracy in the precision cosmology field. 15:10 15:30 Assembly bias in galaxies Iván Lacerna (PUC) In the last decade, results from N-body simulations have shown that the clustering of dark matter haloes at large scales depends on the assembly history in addition to the halo mass. This effect in haloes was termed assembly bias. By means of semi-analytic models and hydrodynamical simulations of galaxy formation, it has been found that galaxy clustering on large scales is also affected by the correlation of halo environment with halo assembly history. However, on the observational side, the existence of the assembly bias is still debated. In this talk, I will present theoretical and observational results related to the assembly bias in galaxies. This is a relevant issue that could affect the ability of the next generation of galaxy surveys to infer accurate cosmological parameters. 15:30 15:50 Clustering tomography on the final SDSS-III BOSS galaxy sample Salvador Salazar (MPE) We test the cosmological implications of studying galaxy clustering using a tomographic approach applied to the final BOSS DR12 galaxy sample, including both auto- and cross-correlation functions between redshift shells. We model the signal of the full shape of the angular correlation function, ω(θ), in redshift bins using state-of-the-art modelling of non-linearities, bias and redshift-space distortions. We present results on the redshift evolution of the linear bias of BOSS galaxies, which cannot be obtained with traditional methods for galaxy-clustering analysis. We also obtain constraints on cosmological parameters in several different parameter-spaces, combining this tomographic analysis with measurements of the CMB and type Abstract Book www2.astro.puc.cl/mocksantiago/ 23

24 Ia supernova (SNIa). 15:50 16:10 Local Group Analogues Roberto Gonzalez (PUC) We can search for MW-M31 like systems(lg analogues) in observational or mock catalogs to study how common is the LG in a cosmological context and their properties. I show some results on LG mass, satellite distribution/accretion history, and the environment where LGs are located. 16:10 16:30 Re-discovering giant low surface brightness galaxies through simulations: a pending issue Gaspar Galaz (PUC) In this talk we summarize some efforts to reproduce through simulations the appearance of giant low surface brightness galaxies (GLSBs) in the universe. In spite of the small number of these kind of galaxies discovered so far, very recent discoveries of milky way sized LSB galaxies in the Coma cluster by van Dokkum et al. (2015), and recent deep optical observations of the structure of Malin 1, are boosting the research on these kind of galaxies. Therefore, it is of great importance to reproduce (e.g. understand) under which conditions, when in the history of the universe, and where in the cosmic web, these galaxies are formed and how they evolve. We explore these issues through mock catalogues generated by semi-analytical models. Thursday 09:30 09:50 Making Mocks with the Quick Particle Mesh Method Jeremy Tinker (New York University) I will demonstrate the power and flexibility of the Quick Particle Mesh technique (QPM) for making realistic mock galaxy catalogs. QPM can create halo catalogs of arbitrarily low halo masses without changing the resolution of the PM simulation on which it is based. Using QPM, we have created mock catalogs with halos down to M in simulation volumes 5 Gpc per side, with minimal computational effort. Current QPM mocks can fit the entire DESI survey within them, as well as the eboss QSO sample, which extends from z=0.8 to z=2.3. Abstract Book www2.astro.puc.cl/mocksantiago/ 24

25 Thursday 09:50 10:10 QSOs mocks catalogues and LSS Mariano Domínguez (IATE) A high redshift universe QSOs mock is build up based on SAM results on the Millennium simulation and its results are compared with an all sky sample of QSO selected from allwise catalog using machine learning techniques. We study the QSO halo mass distribution using halo occupation methods and correlations with weak lensing distorsions on the CMB Planck data. Our results show strong evolutive dependences that should be taken into account for future mock catalogues and AGN understanding. Thursday 10:10 10:30 Galaxy Assembly in Dark Matter Haloes Ben Moster (Ludwig-Maximilians-University, Munich) Semi-empirical galaxy formation models (such as abundance matching) provide a unique and direct link between galaxies and dark matter haloes, and do not depend on model assumptions on unresolved physics. I will present the next generation of semi-empirical galaxy formation models that take into account the assembly history of the dark matter haloes. To this end the SFR of a galaxy is computed from the growth rate of a simulated DM halo using a mass and redshift dependent conversion efficiency which is constrained by requiring several observations (SMFs, ssfrs, clustering, quenched fractions) be reproduced. While previous models determined galaxy quantities only as an average for a given halo mass, the new models can predict stellar mass, star formation rate, gas mass, and colour for individual systems based on their formation history. Using this new technique I will present star formation and accretion histories for quenched and starforming galaxies, and the evolution of the star formation main sequence. I will also show how other high redshift quantities that will be probed in future surveys can be predicted, such as gas fractions and galaxy merger rates, and how mock observations based on the model look like. Furthermore I will demonstrate how modelled quantities depend on the environment and the galaxy?s location within the cosmic web. Thursday 10:30 10:50 Mocks for the Dark Energy Survey and Beyond Joe DeRose (Stanford University) The interpretation of the vast amount of data that current and future photometric galaxy surveys collect will require the use of mock galaxy catalogs implementing a broad range of physics in many times the volume of the surveys themselves. I will present new methods that build upon the successes of Subhalo Abundance Matching while enabling the generation of realistic mocks on the scales necessary for surveys such as the Dark Energy Survey. Abstract Book www2.astro.puc.cl/mocksantiago/ 25

26 Thursday 10:50 11:10 Semi-Analytic Galaxies from the MassiveBlack II simulation Cristian Vega (Instituto de Astrofísica de La Plata) The construction of mock galaxy catalogs by applying the semi-analytical model of galaxy formation and evolution SAG in the Dark Matter Only MassiveBlack II simulation is explained here, including details on the output properties of the galaxies and discussing the advantages of the technique. General benchmarks and the first statistical results of the galaxy population are also shown. Abstract Book www2.astro.puc.cl/mocksantiago/ 26

27 Poster Abstracts 17:00 18:00 Non-parametric morphological merger indicators in the Illustris simulation Lucas Bignone (IAFE) Non-parametric morphological statistics of galaxy images are commonly used to classify galaxy morphologies and to identify mergers signatures. Morphological indicators of merger events are a key part of understanding the galaxy merger rate, a fundamental yet poorly constraint quantity. Given that merger indicators may be apparent only during a limited time and only under certain conditions, we study the non-parametric morphological statistics (C, M20 and Gini) of z=0 galaxies in the Illustris simulation and determine the fraction of major merger, minor mergers and close pairs that automatic morphological classification are able to correctly identify, and the timescales during which such identification is possible. The correct understanding of the information provided by automatic classification of mergers events are very important in light of future large sample surveys such as LSST that will posses the depth, volume, and wavelength coverage to greatly improve our knowledge of merger events and rates. 17:00 18:00 Anisotropic Halo Model Mario Sgro (IAFE) We present an extension of the classical halo model which take into account the triaxial shape of the dark matter halos. It also provides a easy way to quantify the halo-halo alignment. 17:00 18:00 The origin of spin in galaxies: clues from simulations of atomic cooling haloes Joaquín Prieto (Universidad de Chile) No Abstract Abstract Book www2.astro.puc.cl/mocksantiago/ 27

28 17:00 18:00 No Title Matías Bravo (PUC) No Abstract 17:00 18:00 The simulated SFR-M relation in hydrodynamic simulations Antonios Katsianis (University of Chile) The relation between the Star Formation Rate (SFR) and stellar mass (M ) of galaxies represents a fundamental constraint on galaxy formation, and has been studied extensively both in observations and cosmological hydrodynamic simulations. However, the observed amplitude has not been successfully reproduced in simulations, indicating either that the halo accretion history and baryonic physics are poorly understood/modeled or that observations contain biases. In this talk, I present the evolution of the simulated and observed SFR-M relations of z 1 4 galaxies. Simulations from various groups (e.g. EAGLES, Illustris, ANGUS) produce relations that have remarkable agreement despite the fact that they have employed different cosmological codes and run simulations with different resolutions. This is interesting for two reasons. A) simulations can produce realistic populations of galaxies within representative cosmological volumes even at relatively modest resolutions. B) It is likely that current numerical codes that rely on similar subgrid multiphase Inter-Stellar Medium (ISM) models and are tuned to reproduce statistical properties of galaxies, produce similar results for the SFR-M relation by construction, regardless of resolution, box size and, to some extent, the adopted feedback prescriptions. In addition, I display the inconsistency between observed relations that are obtained using different techniques. Numerical results are consistent with observations that use Spectral Energy Distribution (SED) techniques to estimate star formation rates, dust corrections and stellar masses. On the contrary, simulations are not able to reproduce results that were obtained by combining only UV and IR luminosities (UV+IR). These imply SFRs at a fixed stellar mass that are larger almost by a factor of 5 than those of SED measurements for z For z < 1.5, the results from simulations, SED fitting techniques and IR+UV conversion agree well. We find that surveys that preferably select star forming galaxies (e.g. by adopting Lyman-break, Hα or blue selection) typically predict a larger median/average star formation rate at a fixed stellar mass especially for high mass objects, with respect to mass selected samples and hydrodynamic simulations. It has been reported in the literature that simulations produce steeper SFR-M relations than observations. Interestingly, we find that updated observed star formation rate - stellar mass relations that are able to take into account faint small mass objects with low star formation rates tend to be steeper than previous estimates and actually in agreement with the predictions from cosmological simulations. Abstract Book www2.astro.puc.cl/mocksantiago/ 28