140 results on '"Yao-Yuan Mao"'
Search Results
2. Discovery and Characterization of Two Ultrafaint Dwarfs outside the Halo of the Milky Way: Leo M and Leo K
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Kristen. B. W. McQuinn, Yao-Yuan Mao, Erik J. Tollerud, Roger E. Cohen, David Shih, Matthew R. Buckley, and Andrew E. Dolphin
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Local Group ,Dwarf galaxies ,Galaxy quenching ,Reionization ,Stellar populations ,Hertzsprung Russell diagram ,Astrophysics ,QB460-466 - Abstract
We report the discovery of two ultrafaint dwarf galaxies, Leo M and Leo K, that lie outside the halo of the Milky Way (MW). Using Hubble Space Telescope imaging of the resolved stars, we create color–magnitude diagrams reaching the oldest main-sequence turnoff of each system and (i) fit for structural parameters of the galaxies; (ii) measure their distances using the luminosity of the horizontal branch stars; (iii) estimate integrated magnitudes and stellar masses; and (iv) reconstruct the star formation histories. Based on their location in the Local Group, neither galaxy is currently within the halo of the MW although Leo K is located ∼26 kpc from the low-mass galaxy Leo T and these two systems may have had a past interaction. Leo M and Leo K have stellar masses of ${1.8}_{-0.2}^{+0.3}\times {10}^{4}$ M _⊙ and 1.2 ± 0.2 × 10 ^4 M _⊙ , and were quenched ${10.6}_{-1.1}^{+2.2}$ Gyr and ${12.8}_{-4.2}^{+0.1}$ Gyr ago, respectively. Given that the galaxies are at farther distances from the MW, it is unlikely that they were quenched by environmental processing. Instead, given their low stellar masses, their early quenching timescales are consistent with the scenario that a combination of reionization and stellar feedback shut down star formation at early cosmic times.
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- 2024
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3. Forecasts for Galaxy Formation and Dark Matter Constraints from Dwarf Galaxy Surveys
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Ethan O. Nadler, Vera Gluscevic, Trey Driskell, Risa H. Wechsler, Leonidas A. Moustakas, Andrew Benson, and Yao-Yuan Mao
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Dark matter ,Dwarf galaxies ,Galaxy abundances ,Galaxy formation ,Astrophysics ,QB460-466 - Abstract
The abundance of faint dwarf galaxies is determined by the underlying population of low-mass dark matter (DM) halos and the efficiency of galaxy formation in these systems. Here, we quantify potential galaxy formation and DM constraints from future dwarf satellite galaxy surveys. We generate satellite populations using a suite of Milky Way (MW)–mass cosmological zoom-in simulations and an empirical galaxy–halo connection model, and assess sensitivity to galaxy formation and DM signals when marginalizing over galaxy–halo connection uncertainties. We find that a survey of all satellites around one MW-mass host can constrain a galaxy formation cutoff at peak virial masses of ${{ \mathcal M }}_{50}={10}^{8}\,{M}_{\odot }$ at the 1 σ level; however, a tail toward low ${{ \mathcal M }}_{50}$ prevents a 2 σ measurement. In this scenario, combining hosts with differing bright satellite abundances significantly reduces uncertainties on ${{ \mathcal M }}_{50}$ at the 1 σ level, but the 2 σ tail toward low ${{ \mathcal M }}_{50}$ persists. We project that observations of one (two) complete satellite populations can constrain warm DM models with m _WDM ≈ 10 keV (20 keV). Subhalo mass function (SHMF) suppression can be constrained to ≈70%, 60%, and 50% that in cold dark matter (CDM) at peak virial masses of 10 ^8 , 10 ^9 , and 10 ^10 M _⊙ , respectively; SHMF enhancement constraints are weaker (≈20, 4, and 2 times that in CDM, respectively) due to galaxy–halo connection degeneracies. These results motivate searches for faint dwarf galaxies beyond the MW and indicate that ongoing missions like Euclid and upcoming facilities including the Vera C. Rubin Observatory and Nancy Grace Roman Space Telescope will probe new galaxy formation and DM physics.
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- 2024
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4. SAGAbg. I. A Near-unity Mass-loading Factor in Low-mass Galaxies via Their Low-redshift Evolution in Stellar Mass, Oxygen Abundance, and Star Formation Rate
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Erin Kado-Fong, Marla Geha, Yao-Yuan Mao, Mithi A. C. de los Reyes, Risa H. Wechsler, Yasmeen Asali, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, and Benjamin Weiner
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Amorphous irregular galaxies ,Dwarf irregular galaxies ,Galaxy winds ,Galaxy chemical evolution ,Astrophysics ,QB460-466 - Abstract
Measuring the relation between star formation and galactic winds is observationally difficult. In this work we make an indirect measurement of the mass-loading factor (the ratio between the mass outflow rate and star formation rate) in low-mass galaxies using a differential approach to modeling the low-redshift evolution of the star-forming main sequence and mass–metallicity relation. We use Satellites Around Galactic Analogs (SAGA) background galaxies, i.e., spectra observed by the SAGA Survey that are not associated with the main SAGA host galaxies, to construct a sample of 11,925 spectroscopically confirmed low-mass galaxies from 0.01 ≲ z ≤ 0.21 and measure auroral line metallicities for 120 galaxies. The crux of the method is to use the lowest-redshift galaxies as the boundary condition of our model, and to infer a mass-loading factor for the sample by comparing the expected evolution of the low-redshift reference sample in stellar mass, gas-phase metallicity, and star formation rate against the observed properties of the sample at higher redshift. We infer a mass-loading factor of ${\eta }_{{\rm{m}}}={0.92}_{-0.74}^{+1.76}$ , which is in line with direct measurements of the mass-loading factor from the literature despite the drastically different sets of assumptions needed for each approach. While our estimate of the mass-loading factor is in good agreement with recent galaxy simulations that focus on resolving the dynamics of the interstellar medium, it is smaller by over an order of magnitude than the mass-loading factor produced by many contemporary cosmological simulations.
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- 2024
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5. Validating Synthetic Galaxy Catalogs for Dark Energy Science in the LSST Era
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Eve Kovacs, Yao-Yuan Mao, Michel Aguena, Anita Bahmanyar, Adam Broussard, James Butler, Duncan Campbell, Chihway Chang, Shenming Fu, Katrin Heitmann, Danila Korytov, François Lanusse, Patricia Larsen, Rachel Mandelbaum, Christopher B. Morrison, Constantin Payerne, Marina Ricci, Eli Rykoff, F. Javier Sánchez, Ignacio Sevilla-Noarbe, Melanie Simet, Chun-Hao To, Vinu Vikraman, Rongpu Zhou, Camille Avestruz, Christophe Benoist, Andrew J. Benson, Lindsey Bleem, Aleksandra Ćiprianović, Céline Combet, Eric Gawiser, Shiyuan He, Remy Joseph, Jeffrey A. Newman, Judit Prat, Samuel Schmidt, Anže Slosar, Joe Zuntz, and The LSST Dark Energy Science Collaboration
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Astronomy ,QB1-991 ,Astrophysics ,QB460-466 - Abstract
Large simulation efforts are required to provide synthetic galaxy catalogs for ongoing and upcoming cosmology surveys. These extragalactic catalogs are being used for many diverse purposes covering a wide range of scientific topics. In order to be useful, they must offer realistically complex information about the galaxies they contain. Hence, it is critical to implement a rigorous validation procedure that ensures that the simulated galaxy properties faithfully capture observations and delivers an assessment of the level of realism attained by the catalog. We present here a suite of validation tests that have been developed by the Rubin Observatory Legacy Survey of Space and Time (LSST) Dark Energy Science Collaboration (DESC). We discuss how the inclusion of each test is driven by the scientific targets for static ground-based dark energy science and by the availability of suitable validation data. The validation criteria that are used to assess the performance of a catalog are flexible and depend on the science goals. We illustrate the utility of this suite by showing examples for the validation of cosmoDC2, the extragalactic catalog recently released for the LSST DESC second Data Challenge.
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- 2022
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6. Target Selection and Sample Characterization for the DESI LOW-Z Secondary Target Program
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Elise Darragh-Ford, John F. Wu, Yao-Yuan Mao, Risa H. Wechsler, Marla Geha, Jaime E. Forero-Romero, ChangHoon Hahn, Nitya Kallivayalil, John Moustakas, Ethan O. Nadler, Marta Nowotka, J. E. G. Peek, Erik J. Tollerud, Benjamin Weiner, J. Aguilar, S. Ahlen, D. Brooks, A. P. Cooper, A. de la Macorra, A. Dey, K. Fanning, A. Font-Ribera, S. Gontcho A Gontcho, K. Honscheid, T. Kisner, Anthony Kremin, M. Landriau, Michael E. Levi, P. Martini, Aaron M. Meisner, R. Miquel, Adam D. Myers, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Schlegel, M. Schubnell, Gregory Tarlé, M. Vargas-Magaña, Zhimin Zhou, and H. Zou
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Redshift surveys ,Computational methods ,Dwarf galaxies ,Low surface brightness galaxies ,Astrophysics ,QB460-466 - Abstract
We introduce the DESI LOW- Z Secondary Target Survey, which combines the wide-area capabilities of the Dark Energy Spectroscopic Instrument (DESI) with an efficient, low-redshift target selection method. Our selection consists of a set of color and surface brightness cuts, combined with modern machine-learning methods, to target low-redshift dwarf galaxies ( z < 0.03) between 19 < r < 21 with high completeness. We employ a convolutional neural network (CNN) to select high-priority targets. The LOW- Z survey has already obtained over 22,000 redshifts of dwarf galaxies ( M _* < 10 ^9 M _⊙ ), comparable to the number of dwarf galaxies discovered in the Sloan Digital Sky Survey DR8 and GAMA. As a spare fiber survey, LOW- Z currently receives fiber allocation for just ∼50% of its targets. However, we estimate that our selection is highly complete: for galaxies at z < 0.03 within our magnitude limits, we achieve better than 95% completeness with ∼1% efficiency using catalog-level photometric cuts. We also demonstrate that our CNN selections z < 0.03 galaxies from the photometric cuts subsample at least 10 times more efficiently while maintaining high completeness. The full 5 yr DESI program will expand the LOW- Z sample, densely mapping the low-redshift Universe, providing an unprecedented sample of dwarf galaxies, and providing critical information about how to pursue effective and efficient low-redshift surveys.
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- 2023
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7. The Aemulus Project. V. Cosmological Constraint from Small-scale Clustering of BOSS Galaxies
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Zhongxu Zhai, Jeremy L. Tinker, Arka Banerjee, Joseph DeRose, Hong Guo, Yao-Yuan Mao, Sean McLaughlin, Kate Storey-Fisher, and Risa H. Wechsler
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Observational cosmology ,Cosmology ,Large-scale structure of the universe ,Astrophysics ,QB460-466 - Abstract
We analyze clustering measurements of BOSS galaxies using a simulation-based emulator of two-point statistics. We focus on the monopole and quadrupole of the redshift-space correlation function, and the projected correlation function, at scales of 0.1 ∼ 60 h ^−1 Mpc. Although our simulations are based on w CDM with general relativity (GR), we include a scaling parameter of the halo velocity field, γ _f , defined as the amplitude of the halo velocity field relative to the GR prediction. We divide the BOSS data into three redshift bins. After marginalizing over other cosmological parameters, galaxy bias parameters, and the velocity scaling parameter, we find f σ _8 ( z = 0.25) = 0.413 ± 0.031, f σ _8 ( z = 0.4) = 0.470 ± 0.026, and f σ _8 ( z = 0.55) = 0.396 ± 0.022. Compared with Planck observations using a flat Lambda cold dark matter model, our results are lower by 1.9 σ , 0.3 σ , and 3.4 σ , respectively. These results are consistent with other recent simulation-based results at nonlinear scales, including weak lensing measurements of BOSS LOWZ galaxies, two-point clustering of eBOSS LRGs, and an independent clustering analysis of BOSS LOWZ. All these results are generally consistent with a combination of ${\gamma }_{f}^{1/2}{\sigma }_{8}\approx 0.75$ . We note, however, that the BOSS data is well fit assuming GR, i.e., γ _f = 1. We cannot rule out an unknown systematic error in the galaxy bias model at nonlinear scales, but near-future data and modeling will enhance our understanding of the galaxy–halo connection, and provide a strong test of new physics beyond the standard model.
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- 2023
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8. Pegasus W: An Ultrafaint Dwarf Galaxy Outside the Halo of M31 Not Quenched by Reionization
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Kristen B. W. McQuinn, Yao-Yuan Mao, Matthew R. Buckley, David Shih, Roger E. Cohen, and Andrew E. Dolphin
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Hertzsprung Russell diagram ,Local Group ,Astrophysics ,QB460-466 - Abstract
We report the discovery of an ultrafaint dwarf (UFD) galaxy, Pegasus W, located on the far side of the Milky Way–M31 system and outside the virial radius of M31. The distance to the galaxy is ${915}_{-91}^{+60}$ kpc, measured using the luminosity of horizontal branch stars identified in Hubble Space Telescope optical imaging. The galaxy has a half-light radius ( r _h ) ${100}_{-13}^{+11}$ pc, ${M}_{V}=-{7.20}_{-0.16}^{+0.17}$ mag, and a present-day stellar mass ${6.5}_{-1.4}^{+1.1}\times {10}^{4}$ M _⊙ . We identify sources in the color–magnitude diagram (CMD) that may be younger than ∼500 Myr, suggesting late-time star formation in the UFD galaxy, although further study is needed to confirm these are bona fide young stars in the galaxy. Based on fitting the CMD with stellar evolution libraries, Pegasus W shows an extended star formation history. Using the τ _90 metric (defined as the timescale by which the galaxy formed 90% of its stellar mass), the galaxy was quenched only ${7.4}_{-2.6}^{+2.2}$ Gyr ago, which is similar to the quenching timescale of a number of UFD satellites of M31 but significantly more recent than the UFD satellites of the Milky Way. Such late-time quenching is inconsistent with the more rapid timescale expected by reionization and suggests that, while not currently a satellite of M31, Pegasus W was nonetheless slowly quenched by environmental processes.
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- 2023
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9. Symphony: Cosmological Zoom-in Simulation Suites over Four Decades of Host Halo Mass
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Ethan O. Nadler, Philip Mansfield, Yunchong Wang, Xiaolong Du, Susmita Adhikari, Arka Banerjee, Andrew Benson, Elise Darragh-Ford, Yao-Yuan Mao, Sebastian Wagner-Carena, Risa H. Wechsler, and Hao-Yi Wu
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Dark matter ,Galaxy abundances ,N-body simulations ,Galaxy dark matter halos ,Computational methods ,Astrophysics ,QB460-466 - Abstract
We present Symphony, a compilation of 262 cosmological, cold-dark-matter-only zoom-in simulations spanning four decades of host halo mass, from 10 ^11 –10 ^15 M _⊙ . This compilation includes three existing simulation suites at the cluster and Milky Way–mass scales, and two new suites: 39 Large Magellanic Cloud-mass (10 ^11 M _⊙ ) and 49 strong-lens-analog (10 ^13 M _⊙ ) group-mass hosts. Across the entire host halo mass range, the highest-resolution regions in these simulations are resolved with a dark matter particle mass of ≈3 × 10 ^−7 times the host virial mass and a Plummer-equivalent gravitational softening length of ≈9 × 10 ^−4 times the host virial radius, on average. We measure correlations between subhalo abundance and host concentration, formation time, and maximum subhalo mass, all of which peak at the Milky Way host halo mass scale. Subhalo abundances are ≈50% higher in clusters than in lower-mass hosts at fixed sub-to-host halo mass ratios. Subhalo radial distributions are approximately self-similar as a function of host mass and are less concentrated than hosts’ underlying dark matter distributions. We compare our results to the semianalytic model Galacticus , which predicts subhalo mass functions with a higher normalization at the low-mass end and radial distributions that are slightly more concentrated than Symphony. We use UniverseMachine to model halo and subhalo star formation histories in Symphony, and we demonstrate that these predictions resolve the formation histories of the halos that host nearly all currently observable satellite galaxies in the universe. To promote open use of Symphony, data products are publicly available at http://web.stanford.edu/group/gfc/symphony .
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- 2023
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10. The LSST-DESC 3x2pt Tomography Optimization Challenge
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Joe Zuntz, François Lanusse, Alex I. Malz, Angus H. Wright, Anže Slosar, Bela Abolfathi, David Alonso, Abby Bault, Clécio R. Bom, Massimo Brescia, Adam Broussard, Jean-Eric Campagne, Stefano Cavuoti, Eduardo S. Cypriano, Bernardo M. O. Fraga, Eric Gawiser, Elizabeth J. Gonzalez, Dylan Green, Peter Hatfield, Kartheik Iyer, David Kirkby, Andrina Nicola, Erfan Nourbakhsh, Andy Park, Gabriel Teixeira, Katrin Heitmann, Eve Kovacs, Yao-Yuan Mao, and LSST Dark Energy Science Collaboration
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Astronomy ,QB1-991 ,Astrophysics ,QB460-466 - Abstract
This paper presents the results of the Rubin Observatory Dark Energy Science Collaboration (DESC) 3x2pt tomography challenge, which served as a first step toward optimizing the tomographic binning strategy for the main DESC analysis. The task of choosing an optimal tomographic binning scheme for a photometric survey is made particularly delicate in the context of a metacalibrated lensing catalogue, as only the photometry from the bands included in the metacalibration process (usually riz and potentially g) can be used in sample definition. The goal of the challenge was to collect and compare bin assignment strategies under various metrics of a standard 3x2pt cosmology analysis in a highly idealized setting to establish a baseline for realistically complex follow-up studies; in this preliminary study, we used two sets of cosmological simulations of galaxy redshifts and photometry under a simple noise model neglecting photometric outliers and variation in observing conditions, and contributed algorithms were provided with a representative and complete training set. We review and evaluate the entries to the challenge, finding that even from this limited photometry information, multiple algorithms can separate tomographic bins reasonably well, reaching figures-of-merit scores close to the attainable maximum. We further find that adding the g band to riz photometry improves metric performance by ~15% and that the optimal bin assignment strategy depends strongly on the science case: which figure-of-merit is to be optimized, and which observables (clustering, lensing, or both) are included.
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- 2021
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11. Probing the galaxy–halo connection with total satellite luminosity
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Jeremy L Tinker, Junzhi Cao, Mehmet Alpaslan, Joseph DeRose, Yao-Yuan Mao, and Risa H Wechsler
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- 2021
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12. Illuminating dark matter halo density profiles without subhaloes
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Catherine E Fielder, Yao-Yuan Mao, Andrew R Zentner, Jeffrey A Newman, Hao-Yi Wu, and Risa H Wechsler
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- 2020
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13. Concentrations of dark haloes emerge from their merger histories
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Kuan Wang, Yao-Yuan Mao, Andrew R Zentner, Johannes U Lange, Frank C van den Bosch, and Risa H Wechsler
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- 2020
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14. Constraining the scatter in the galaxy–halo connection at Milky Way masses
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Jun-zhi Cao, Jeremy L Tinker, Yao-Yuan Mao, and Risa H Wechsler
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- 2020
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15. How to optimally constrain galaxy assembly bias: supplement projected correlation functions with count-in-cells statistics
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Kuan Wang, Yao-Yuan Mao, Andrew R Zentner, Frank C van den Bosch, Johannes U Lange, Chad M Schafer, Antonia Sierra Villarreal, Andrew P Hearin, and Duncan Campbell
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- 2019
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16. Using Maximum Circular Velocity in Halo Occupation Distribution Models to Predict Galaxy Clustering
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Lorena Mezini, Kuan Wang, Yao-Yuan Mao, and Andrew R. Zentner
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- 2022
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17. Evidence of galaxy assembly bias in SDSS DR7 galaxy samples from count statistics
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Kuan Wang, Yao-Yuan Mao, Andrew R Zentner, Hong Guo, Johannes U Lange, Frank C van den Bosch, and Lorena Mezini
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present observational constraints on the galaxy-halo connection, focusing particularly on galaxy assembly bias, from a novel combination of counts-in-cylinders statistics, $P(N_{\rm{CIC}})$, with the standard measurements of the projected two-point correlation function, $w_{\rm{p}}(r_{\rm{p}})$, and number density, $n_{\rm{gal}}$, of galaxies. We measure $n_{\rm{gal}}$, $w_{\rm{p}}(r_{\rm{p}})$ and $P(N_{\rm{CIC}})$ for volume-limited, luminosity-threshold samples of galaxies selected from SDSS DR7, and use them to constrain halo occupation distribution (HOD) models, including a model in which galaxy occupation depends upon a secondary halo property, namely halo concentration. We detect significant positive central assembly bias for the $M_r, 16+5 pages, 9+3 figures, 5+2 tables, Fig. 6 shows the main result. To be submitted to MNRAS, comments welcome
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- 2022
18. Halo histories versus galaxy properties at z = 0 – III. The properties of star-forming galaxies
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Jeremy L Tinker, ChangHoon Hahn, Yao-Yuan Mao, and Andrew R Wetzel
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- 2018
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19. UniverseMachine: Predicting Galaxy Star Formation over Seven Decades of Halo Mass with Zoom-in Simulations
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Yunchong Wang, Ethan O. Nadler, Yao-Yuan Mao, Susmita Adhikari, Risa H. Wechsler, and Peter Behroozi
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- 2021
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20. Target Selection and Sample Characterization for the DESI LOW-Z Secondary Target Program
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Elise Darragh-Ford, John F. Wu, Yao-Yuan Mao, Risa H. Wechsler, Marla Geha, Jaime E. Forero-Romero, ChangHoon Hahn, Nitya Kallivayalil, John Moustakas, Ethan O. Nadler, Marta Nowotka, J. E. G. Peek, Erik J. Tollerud, Benjamin Weiner, and DESI Collaboration
- Abstract
Files to reproduce figures 
- Published
- 2022
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21. The LSST DESC DC2 Simulated Sky Survey
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Bela Abolfathi, David Alonso, Robert Armstrong, Éric Aubourg, Humna Awan, Yadu N. Babuji, Franz Erik Bauer, Rachel Bean, George Beckett, Rahul Biswas, Joanne R. Bogart, Dominique Boutigny, Kyle Chard, James Chiang, Chuck F. Claver, Johann Cohen-Tanugi, Céline Combet, Andrew J. Connolly, Scott F. Daniel, Seth W. Digel, Alex Drlica-Wagner, Richard Dubois, Emmanuel Gangler, Eric Gawiser, Thomas Glanzman, Phillipe Gris, Salman Habib, Andrew P. Hearin, Katrin Heitmann, Fabio Hernandez, Renée Hložek, Joseph Hollowed, Mustapha Ishak, Željko Ivezić, Mike Jarvis, Saurabh W. Jha, Steven M. Kahn, J. Bryce Kalmbach, Heather M. Kelly, Eve Kovacs, Danila Korytov, K. Simon Krughoff, Craig S. Lage, François Lanusse, Patricia Larsen, Laurent Le Guillou, Nan Li, Emily Phillips Longley, Robert H. Lupton, Rachel Mandelbaum, Yao-Yuan Mao, Phil Marshall, Joshua E. Meyers, Marc Moniez, Christopher B. Morrison, Andrei Nomerotski, Paul O’Connor, HyeYun Park, Ji Won Park, Julien Peloton, Daniel Perrefort, James Perry, Stéphane Plaszczynski, Adrian Pope, Andrew Rasmussen, Kevin Reil, Aaron J. Roodman, Eli S. Rykoff, F. Javier Sánchez, Samuel J. Schmidt, Daniel Scolnic, Christopher W. Stubbs, J. Anthony Tyson, Thomas D. Uram, Antonio Villarreal, Christopher W. Walter, Matthew P. Wiesner, W. Michael Wood-Vasey, and Joe Zuntz
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- 2021
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22. A composite likelihood approach for inference under photometric redshift uncertainty
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Simon P. Wilson, Markus Rau, S. J. Schmidt, Yao-Yuan Mao, Rachel Mandelbaum, and Christopher B. Morrison
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Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010308 nuclear & particles physics ,Astrophysics::Instrumentation and Methods for Astrophysics ,FOS: Physical sciences ,Astronomy and Astrophysics ,Sample (statistics) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,01 natural sciences ,Galaxy ,Redshift ,Photometry (optics) ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,Calibration ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,010303 astronomy & astrophysics ,Algorithm ,Parametrization ,Weak gravitational lensing ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Photometric redshift - Abstract
Obtaining accurately calibrated redshift distributions of photometric samples is one of the great challenges in photometric surveys like LSST, Euclid, HSC, KiDS, and DES. We present an inference methodology that combines the redshift information from the galaxy photometry with constraints from two-point functions, utilizing cross-correlations with spatially overlapping spectroscopic samples, and illustrate the approach on CosmoDC2 simulations. Our likelihood framework is designed to integrate directly into a typical large-scale structure and weak lensing analysis based on two-point functions. We discuss efficient and accurate inference techniques that allow us to scale the method to the large samples of galaxies to be expected in LSST. We consider statistical challenges like the parametrization of redshift systematics, discuss and evaluate techniques to regularize the sample redshift distributions, and investigate techniques that can help to detect and calibrate sources of systematic error using posterior predictive checks. We evaluate and forecast photometric redshift performance using data from the CosmoDC2 simulations, within which we mimic a DESI-like spectroscopic calibration sample for cross-correlations. Using a combination of spatial cross-correlations and photometry, we show that we can provide calibration of the mean of the sample redshift distribution to an accuracy of at least 0.002(1+z), consistent with the LSST-Y1 science requirements for weak lensing and large-scale structure probes., Comment: Updated to match the version accepted by the MNRAS, 23 pages, 9 figures, 2 tables
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- 2021
23. Symphony: Cosmological Zoom-in Simulation Suites over Four Decades of Host Halo Mass
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Ethan O. Nadler, Philip Mansfield, Yunchong Wang, Xiaolong Du, Susmita Adhikari, Arka Banerjee, Andrew Benson, Elise Darragh-Ford, Yao-Yuan Mao, Sebastian Wagner-Carena, Risa H. Wechsler, and Hao-Yi Wu
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present Symphony, a compilation of $262$ cosmological, cold-dark-matter-only zoom-in simulations spanning four decades of host halo mass, from $10^{11}$$-$$10^{15}~M_{\mathrm{\odot}}$. This compilation includes three existing simulation suites at the cluster and Milky Way$-$mass scales, and two new suites: $39$ Large Magellanic Cloud-mass ($10^{11}~M_{\mathrm{\odot}}$) and $49$ strong-lens-analog ($10^{13}~M_{\mathrm{\odot}}$) group-mass hosts. Across the entire host halo mass range, the highest-resolution regions in these simulations are resolved with a dark matter particle mass of $\approx 3\times 10^{-7}$ times the host virial mass and a Plummer-equivalent gravitational softening length of $\approx 9\times 10^{-4}$ times the host virial radius, on average. We measure correlations between subhalo abundance and host concentration, formation time, and maximum subhalo mass, all of which peak at the Milky Way host halo mass scale. Subhalo abundances are $\approx 50\%$ higher in clusters than in lower-mass hosts at fixed sub-to-host halo mass ratios. Subhalo radial distributions are approximately self-similar as a function of host mass and are less concentrated than hosts' underlying dark matter distributions. We compare our results to the semianalytic model $\mathrm{\texttt{Galacticus}}$, which predicts subhalo mass functions with a higher normalization at the low-mass end and radial distributions that are slightly more concentrated than Symphony. We use $\mathrm{\texttt{UniverseMachine}}$ to model halo and subhalo star formation histories in Symphony, and we demonstrate that these predictions resolve the formation histories of the halos that host nearly all currently observable satellite galaxies in the universe. To promote open use of Symphony, data products are publicly available at http://web.stanford.edu/group/gfc/symphony., 39 pages, 20 figures, 2 tables. Updated to published version
- Published
- 2022
24. The southern stellar stream spectroscopic survey (S5)
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Lara R. Cullinane, A. K. Vivas, E. Balbinot, Vasily Belokurov, Daniel B. Zucker, Sergey E. Koposov, Jeffrey D. Simpson, Sanjib Sharma, Alasdair Mackey, Denis Erkal, G. M. De Silva, Douglas L. Tucker, Risa H. Wechsler, J. D. Simon, Keith Bechtol, Kyler Kuehn, Alexander P. Ji, Geraint F. Lewis, Alex Drlica-Wagner, Brian Yanny, Marla Geha, Joss Bland-Hawthorn, Andrew B. Pace, S. Allam, Nora Shipp, G. S. Da Costa, Tenglin Li, Andrew R. Casey, Jeremy Mould, Zhen Wan, Yao-Yuan Mao, Sarah L. Martell, and Astronomy
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TIDAL STREAMS ,Milky Way ,media_common.quotation_subject ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,MASS ,01 natural sciences ,globular clusters: general ,Photometry (optics) ,Galactic halo ,DARK HALO ,galaxy: halo ,0103 physical sciences ,SPECTROGRAPH ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Dwarf galaxy ,media_common ,Physics ,RADIAL-VELOCITIES ,010308 nuclear & particles physics ,Astronomy ,Astronomy and Astrophysics ,galaxies: dwarf ,Astrophysics - Astrophysics of Galaxies ,GIANT STARS ,Galaxy ,EVOLUTION ,GALAXY ,Dark matter halo ,Space and Planetary Science ,Sky ,Globular cluster ,Astrophysics of Galaxies (astro-ph.GA) ,galaxy: kinematics and dynamics ,DIGITAL SKY SURVEY ,MILKY-WAY ,Astrophysics::Earth and Planetary Astrophysics - Abstract
We introduce the Southern Stellar Stream Spectroscopy Survey (${S}^5$), an on-going program to map the kinematics and chemistry of stellar streams in the Southern Hemisphere. The initial focus of ${S}^5$ has been spectroscopic observations of recently identified streams within the footprint of the Dark Energy Survey (DES), with the eventual goal of surveying streams across the entire southern sky. Stellar streams are composed of material that has been tidally striped from dwarf galaxies and globular clusters and hence are excellent dynamical probes of the gravitational potential of the Milky Way, as well as providing a detailed snapshot of its accretion history. Observing with the 3.9-m Anglo-Australian Telescope's 2-degree-Field fibre positioner and AAOmega spectrograph, and combining the precise photometry of DES DR1 with the superb proper motions from $Gaia$ DR2, allows us to conduct an efficient spectroscopic survey to map these stellar streams. So far ${S}^5$ has mapped 9 DES streams and 3 streams outside of DES; the former are the first spectroscopic observations of these recently discovered streams. In addition to the stream survey, we use spare fibres to undertake a Milky Way halo survey and a low-redshift galaxy survey. This paper presents an overview of the ${S}^5$ program, describing the scientific motivation for the survey, target selection, observation strategy, data reduction and survey validation. Finally, we describe early science results on stellar streams and Milky Way halo stars drawn from the survey. Updates on ${S}^5$, including future public data release, can be found at \url{http://s5collab.github.io}., Comment: 25 pages, 14 figures (1 in appendix), 3 tables (1 in appendix). Published on MNRAS. See also paper from Shipp et al. 2019, which measures the proper motion of the DES streams
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- 2019
25. The LSST DESC DC2 Simulated Sky Survey
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Kevin Reil, Adrian Pope, Kyle Chard, Mustapha Ishak, D. Boutigny, Humna Awan, H. Kelly, Laurent Le Guillou, W. Michael Wood-Vasey, Eli S. Rykoff, Stéphane Plaszczynski, Rahul Biswas, Richard Dubois, Saurabh Jha, Danila Korytov, C. W. Walter, J. Anthony Tyson, Katrin Heitmann, T. Glanzman, Fabio Hernandez, François Lanusse, F. Javier Sánchez, Joe Zuntz, Željko Ivezić, Marc Moniez, Yadu Babuji, HyeYun Park, Christopher W. Stubbs, Franz E. Bauer, Phillipe Gris, Chuck Claver, Paul O'Connor, J. Meyers, Christopher B. Morrison, George Beckett, Joseph Hollowed, Seth Digel, Andrew Rasmussen, Céline Combet, Phil Marshall, Éric Aubourg, Rachel Mandelbaum, J. Perry, Mike Jarvis, Thomas D. Uram, K. Simon Krughoff, Johann Cohen-Tanugi, Scott F. Daniel, Yao-Yuan Mao, Matthew P. Wiesner, James Chiang, Bela Abolfathi, Daniel Scolnic, Craig S. Lage, Ji Won Park, Steven M. Kahn, Eric Gawiser, Antonio Villarreal, A. Roodman, E. Gangler, Nan Li, Rachel Bean, David Alonso, Emily Phillips Longley, Andrei Nomerotski, Andrew P. Hearin, Salman Habib, Daniel Perrefort, Andrew J. Connolly, J. Peloton, J. Bryce Kalmbach, Eve Kovacs, Patricia Larsen, Alex Drlica-Wagner, Renée Hložek, Robert Armstrong, J.R. Bogart, Samuel Schmidt, Robert H. Lupton, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Centre de Calcul de l'IN2P3 (CC-IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), LSST Dark Energy Science, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Data products ,media_common.quotation_subject ,FOS: Physical sciences ,Image processing software ,Sky surveys ,01 natural sciences ,Field (computer science) ,Observatory ,0103 physical sciences ,N-body simulations ,[PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det] ,Deep drilling ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,010303 astronomy & astrophysics ,media_common ,Remote sensing ,Physics ,010308 nuclear & particles physics ,Testbed ,Astronomy and Astrophysics ,Cosmology ,Space and Planetary Science ,Sky ,Simulated data ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We describe the simulated sky survey underlying the second data challenge (DC2) carried out in preparation for analysis of the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) by the LSST Dark Energy Science Collaboration (LSST DESC). Significant connections across multiple science domains will be a hallmark of LSST; the DC2 program represents a unique modeling effort that stresses this interconnectivity in a way that has not been attempted before. This effort encompasses a full end-to-end approach: starting from a large N-body simulation, through setting up LSST-like observations including realistic cadences, through image simulations, and finally processing with Rubin's LSST Science Pipelines. This last step ensures that we generate data products resembling those to be delivered by the Rubin Observatory as closely as is currently possible. The simulated DC2 sky survey covers six optical bands in a wide-fast-deep (WFD) area of approximately 300 deg^2 as well as a deep drilling field (DDF) of approximately 1 deg^2. We simulate 5 years of the planned 10-year survey. The DC2 sky survey has multiple purposes. First, the LSST DESC working groups can use the dataset to develop a range of DESC analysis pipelines to prepare for the advent of actual data. Second, it serves as a realistic testbed for the image processing software under development for LSST by the Rubin Observatory. In particular, simulated data provide a controlled way to investigate certain image-level systematic effects. Finally, the DC2 sky survey enables the exploration of new scientific ideas in both static and time-domain cosmology., 39 pages, 19 figures, version accepted for publication in ApJS
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- 2021
26. How to optimally constrain galaxy assembly bias: supplement projected correlation functions with count-in-cells statistics
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Andrew R. Zentner, Johannes U. Lange, Antonio Villarreal, Kuan Wang, Frank C. van den Bosch, Duncan Campbell, Andrew Hearin, Yao-Yuan Mao, and Chad M. Schafer
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Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Degree (graph theory) ,010308 nuclear & particles physics ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Correlation function (quantum field theory) ,Redshift survey ,01 natural sciences ,Halo occupation distribution ,Galaxy ,Distribution (mathematics) ,Cover (topology) ,Space and Planetary Science ,0103 physical sciences ,Statistics ,Connection (algebraic framework) ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Most models for the connection between galaxies and their haloes ignore the possibility that galaxy properties may be correlated with halo properties other than mass, a phenomenon known as galaxy assembly bias. Yet, it is known that such correlations can lead to systematic errors in the interpretation of survey data. At present, the degree to which galaxy assembly bias may be present in the real Universe, and the best strategies for constraining it remain uncertain. We study the ability of several observables to constrain galaxy assembly bias from redshift survey data using the decorated halo occupation distribution (dHOD), an empirical model of the galaxy--halo connection that incorporates assembly bias. We cover an expansive set of observables, including the projected two-point correlation function $w_{\mathrm{p}}(r_{\mathrm{p}})$, the galaxy--galaxy lensing signal $\Delta \Sigma(r_{\mathrm{p}})$, the void probability function $\mathrm{VPF}(r)$, the distributions of counts-in-cylinders $P(N_{\mathrm{CIC}})$, and counts-in-annuli $P(N_{\mathrm{CIA}})$, and the distribution of the ratio of counts in cylinders of different sizes $P(N_2/N_5)$. We find that despite the frequent use of the combination $w_{\mathrm{p}}(r_{\mathrm{p}})+\Delta \Sigma(r_{\mathrm{p}})$ in interpreting galaxy data, the count statistics, $P(N_{\mathrm{CIC}})$ and $P(N_{\mathrm{CIA}})$, are generally more efficient in constraining galaxy assembly bias when combined with $w_{\mathrm{p}}(r_{\mathrm{p}})$. Constraints based upon $w_{\mathrm{p}}(r_{\mathrm{p}})$ and $\Delta \Sigma(r_{\mathrm{p}})$ share common degeneracy directions in the parameter space, while combinations of $w_{\mathrm{p}}(r_{\mathrm{p}})$ with the count statistics are more complementary. Therefore, we strongly suggest that count statistics should be used to complement the canonical observables in future studies of the galaxy--halo connection., Comment: Figures 3 and 4 show the main results. Published in Monthly Notices of the Royal Astronomical Society
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- 2019
27. Constraints on dark matter properties from observations of Milky Way satellite galaxies
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A. K. Romer, J. Carretero, Annika H. G. Peter, P. Doel, Antonella Palmese, M. A. G. Maia, Vera Gluscevic, Tenglin Li, Ethan O. Nadler, David J. James, A. R. Walker, Marcelle Soares-Santos, S. Desai, Gregory M. Green, Keith Bechtol, Josh Frieman, S. Everett, V. Scarpine, H. T. Diehl, Alex Drlica-Wagner, Dragan Huterer, W. C. Wester, B. Flaugher, Samuel Hinton, J. De Vicente, G. Gutierrez, S. Serrano, J. Annis, D. L. Burke, Douglas L. Tucker, Kyler Kuehn, J. Gschwend, I. Sevilla-Noarbe, Kimberly K. Boddy, M. Smith, Jennifer L. Marshall, Salcedo Romero de Ávila, N. Kuropatkin, L. N. da Costa, S. Allam, Robert A. Gruendl, S. Mau, T. M. C. Abbott, M. Costanzi, M. Carrasco Kind, Daniel Gruen, A. A. Plazas, E. J. Sanchez, M. McNanna, Michel Aguena, M. E. C. Swanson, K. Honscheid, Juan Garcia-Bellido, Andrew B. Pace, Yao-Yuan Mao, Felipe Menanteau, D. W. Gerdes, F. Paz-Chinchón, Elisabeth Krause, A. H. Riley, David J. Brooks, G. Tarle, Ramon Miquel, E. Suchyta, August E. Evrard, Risa H. Wechsler, Bhuvnesh Jain, Ofer Lahav, UAM. Departamento de Física Teórica, Nadler, E. O., Drlica-Wagner, A., Bechtol, K., Mau, S., Wechsler, R. H., Gluscevic, V., Boddy, K., Pace, A. B., T. S., Li, Mcnanna, M., Riley, A. H., García-Bellido, J., Mao, Y. -Y., Green, G., Burke, D. L., Peter, A., Jain, B., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Brooks, D., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Honscheid, K., Huterer, D., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Walker, A. R., Wester, W., Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), and Department of Energy (US)
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Scattering cross-section ,Milky Way ,Dark matter ,General Physics and Astronomy ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Halo ,Particle dark matter ,Dwarf Galaxies ,Astrophysics - Astrophysics of Galaxie ,0103 physical sciences ,Thermal ,Satellite galaxy ,Dark Matter ,Astrophysics - Cosmology and Nongalactic Astrophysic ,010306 general physics ,Astrophysics::Galaxy Astrophysics ,Physics ,Física ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,High Energy Physics - Phenomenology ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Matter wave - Abstract
Nadler, Ethan O, et al. DES Collaboration, We perform a comprehensive study of Milky Way (MW) satellite galaxies to constrain the fundamental properties of dark matter (DM). This analysis fully incorporates inhomogeneities in the spatial distribution and detectability of MW satellites and marginalizes over uncertainties in the mapping between galaxies and DM halos, the properties of the MW system, and the disruption of subhalos by the MW disk. Our results are consistent with the cold, collisionless DM paradigm and yield the strongest cosmological constraints to date on particle models of warm, interacting, and fuzzy dark matter. At 95% confidence, we report limits on (i) the mass of thermal relic warm DM, mWDM>6.5 keV (free-streaming length, λfs≲10h-1 kpc), (ii) the velocity-independent DM-proton scattering cross section, σ02.9×10-21 eV (de Broglie wavelength, λdB≲0.5 kpc). These constraints are complementary to other observational and laboratory constraints on DM properties., The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grant Agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq Grant No. 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
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- 2021
28. UniverseMachine: Predicting Galaxy Star Formation over Seven Decades of Halo Mass with Zoom-in Simulations
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Susmita Adhikari, Peter Behroozi, Yunchong Wang, Ethan O. Nadler, Risa H. Wechsler, and Yao-Yuan Mao
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Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Star formation ,Milky Way ,Star (game theory) ,Dark matter ,Local Group ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Satellite galaxy ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Galaxy Astrophysics ,Dwarf galaxy ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We apply the empirical galaxy--halo connection model UniverseMachine to dark matter-only zoom-in simulations of isolated Milky Way (MW)--mass halos along with their parent cosmological simulations. This application extends \textsc{UniverseMachine} predictions into the ultra-faint dwarf galaxy regime ($ 10^{2}\,\mathrm{M_{\odot}} \leqslant M_{\ast} \leqslant 10^{5}\,\mathrm{M_{\odot}}$) and yields a well-resolved stellar mass--halo mass (SMHM) relation over the peak halo mass range $10^8\,\mathrm{M_{\odot}}$ to $10^{15}\,\mathrm{M_{\odot}}$. The extensive dynamic range provided by the zoom-in simulations allows us to assess specific aspects of dwarf galaxy evolution predicted by \textsc{UniverseMachine}. In particular, although UniverseMachine is not constrained for dwarf galaxies with $M_* \lesssim 10^{8}\,\mathrm{M_{\odot}}$, our predicted SMHM relation is consistent with that inferred for MW satellite galaxies at $z=0$ using abundance matching. However, UniverseMachine predicts that nearly all galaxies are actively star forming below $M_{\ast}\sim 10^{7}\,\mathrm{M_{\odot}}$ and that these systems typically form more than half of their stars at $z\lesssim 4$, which is discrepant with the star formation histories of Local Group dwarf galaxies that favor early quenching. This indicates that the current UniverseMachine model does not fully capture galaxy quenching physics at the low-mass end. We highlight specific improvements necessary to incorporate environmental and reionization-driven quenching for dwarf galaxies, and provide a new tool to connect dark matter accretion to star formation over the full dynamic range that hosts galaxies., Accepted for publication in ApJ. 21 pages, 8 figures, 1 table. Minor edits to v1. Added discussion of reionization contribution of ultra-faint dwarfs in sections 4.4 and 5
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- 2021
29. The Effects of Dark Matter and Baryonic Physics on the Milky Way Subhalo Population in the Presence of the Large Magellanic Cloud
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Ethan O. Nadler, Arka Banerjee, Yao-Yuan Mao, Susmita Adhikari, and Risa H. Wechsler
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Physics ,education.field_of_study ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Milky Way ,Astrophysics::High Energy Astrophysical Phenomena ,Population ,Dark matter ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Warm dark matter ,Satellite galaxy ,Astrophysics::Solar and Stellar Astrophysics ,Disc ,education ,Large Magellanic Cloud ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Dwarf galaxy - Abstract
Given recent developments in our understanding of the Large Magellanic Cloud's (LMC) impact on the Milky Way's (MW) dark matter subhalo population, we compare the signatures of dark matter and baryonic physics on subhalos in MW systems with realistic LMC analogs. In particular, we study the effects of self-interacting dark matter (SIDM), warm dark matter (WDM), and the Galactic disk on the peak maximum circular velocity ($V_{\mathrm{peak}}$) function, radial distribution, and spatial distribution of MW and LMC-associated subhalos using cosmological dark matter-only zoom-in simulations of MW+LMC systems. For a fixed abundance of subhalos expected to host dwarf galaxies ($V_{\mathrm{peak}}\gtrsim 20\ \mathrm{km\ s}^{-1}$), SIDM and WDM can produce a similar mass-dependent suppression of the subhalo $V_{\mathrm{peak}}$ function, while disk disruption is mass independent. Subhalos in the inner regions of the MW are preferentially disrupted by both self-interactions and the disk, while suppression in WDM is radially independent. The relative abundance of LMC-associated subhalos is not strongly affected by disk disruption or WDM, but is significantly suppressed in SIDM due to self-interactions with the LMC at early times and with the MW during LMC infall at late times, erasing spatial anisotropy in the MW subhalo population. These results provide avenues to distinguish dark matter and baryonic physics by combining properties of the MW and LMC subhalo populations probed by upcoming observations of satellite galaxies and stellar streams., Comment: 9 pages, 2 figures, 1 table. Updated to published version
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- 2021
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30. Extending the SAGA Survey (xSAGA) I: Satellite Radial Profiles as a Function of Host Galaxy Properties
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John F. Wu, J. E. G. Peek, Erik J. Tollerud, Yao-Yuan Mao, Ethan O. Nadler, Marla Geha, Risa H. Wechsler, Nitya Kallivayalil, and Benjamin J. Weiner
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Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Astrophysics::Galaxy Astrophysics - Abstract
We present "Extending the Satellites Around Galactic Analogs Survey" (xSAGA), a method for identifying low-$z$ galaxies on the basis of optical imaging, and results on the spatial distributions of xSAGA satellites around host galaxies. Using spectroscopic redshift catalogs from the SAGA Survey as a training data set, we have optimized a convolutional neural network (CNN) to identify $z < 0.03$ galaxies from more distant objects using image cutouts from the DESI Legacy Imaging Surveys. From the sample of $> 100,000$ CNN-selected low-$z$ galaxies, we identify $>20,000$ probable satellites located between 36-300 projected kpc from NASA-Sloan Atlas central galaxies in the stellar mass range $9.5 < \log(M_\star/M_\odot) < 11$. We characterize the incompleteness and contamination for CNN-selected samples, and apply corrections in order to estimate the true number of satellites as a function of projected radial distance from their hosts. Satellite richness depends strongly on host stellar mass, such that more massive host galaxies have more satellites, and on host morphology, such that elliptical hosts have more satellites than disky hosts with comparable stellar masses. We also find a strong inverse correlation between satellite richness and the magnitude gap between a host and its brightest satellite. The normalized satellite radial distribution between 36-300 kpc does not depend strongly on host stellar mass, morphology, or magnitude gap. The satellite abundances and radial distributions we measure are in reasonable agreement with predictions from hydrodynamic simulations. Our results deliver unprecedented statistical power for studying satellite galaxy populations, and highlight the promise of using machine learning for extending galaxy samples of wide-area surveys., 27 pages, 18 figures, 1 table. Accepted to ApJ. Code available at https://github.com/jwuphysics/xsaga
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- 2021
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31. The clustering of DESI-like luminous red galaxies using photometric redshifts
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Aaron M. Meisner, Michael Levi, Francisco Prada, Abhishek Prakash, Yutong Duan, David J. Brooks, Rongpu Zhou, Yao-Yuan Mao, Martin Landriau, Andrew R. Zentner, Gregory Tarlé, Jeffrey A. Newman, John Moustakas, Adam D. Myers, Department of Energy (US), National Aeronautics and Space Administration (US), National Science Foundation (US), Science and Technology Facilities Council (UK), Gordon and Betty Moore Foundation, Ministerio de Ciencia, Innovación y Universidades (España), National Natural Science Foundation of China, and Chinese Academy of Sciences
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Research program ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Higher education ,haloes [Galaxies] ,Large-scale structure of Universe ,Library science ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,01 natural sciences ,Spitzer Space Telescope ,Galaxies: distances and redshifts ,Observatory ,0103 physical sciences ,distances and redshifts [Galaxies] ,User Facility ,Galaxies: haloes ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Physics ,010308 nuclear & particles physics ,business.industry ,Galaxies: evolution ,Astronomy and Astrophysics ,Redshift survey ,evolution [Galaxies] ,13. Climate action ,Space and Planetary Science ,astro-ph.CO ,business ,National laboratory ,Astronomical and Space Sciences ,Fermi Gamma-ray Space Telescope ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present measurements of the redshift-dependent clustering of a DESI-like luminous red galaxy (LRG) sample selected from the Legacy Survey imaging data set, and use the halo occupation distribution (HOD) framework to fit the clustering signal. The photometric LRG sample in this study contains 2.7 million objects over the redshift range of 0.4 < z < 0.9 over 5655 deg2. We have developed new photometric redshift (photo-z) estimates using the Legacy Survey DECam and WISE photometry, with σNMAD = 0.02 precision for LRGs. We compute the projected correlation function using new methods that maximize signal-to-noise ratio while incorporating redshift uncertainties. We present a novel algorithm for dividing irregular survey geometries into equal-area patches for jackknife resampling. For a five-parameter HOD model fit using the MultiDark halo catalogue, we find that there is little evolution in HOD parameters except at the highest redshifts. The inferred large-scale structure bias is largely consistent with constant clustering amplitude over time. In an appendix, we explore limitations of Markov chain Monte Carlo fitting using stochastic likelihood estimates resulting from applying HOD methods to N-body catalogues, and present a new technique for finding best-fitting parameters in this situation. Accompanying this paper, we have released the Photometric Redshifts for the Legacy Surveys catalogue of photo-z's obtained by applying the methods used in this work to the full Legacy Survey Data Release 8 data set. This catalogue provides accurate photometric redshifts for objects with z < 21 over more than 16 000 deg2 of sky. © 2020 The Author(s), Published by Oxford University Press on behalf of Royal Astronomical Society, The authors would like to thank Hee-Jong Seo, Jeremy Tinker, and Gustavo Niz for their feedback on the draft and useful discussions. RZ and JANwere supported by the U.S. Department of Energy Office of Science, Office of High Energy Physics via grant DE-SC0007914. RZalso is supported by the Director, Office of Science, Office ofHigh Energy Physics of the U.S. Department of Energy under Contract No. DE-AC02-05CH1123. Support for YYM was provided by the Pittsburgh Particle Physics, Astrophysics and Cosmology Center through the Samuel P. Langley PITT PACC Postdoctoral Fellowship, and by NASA through the NASA Hubble Fellowship grant no. HST-HF2-51441.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. JM gratefully acknowledges support from NSF grant AST-1616414 and DOE grant DE-SC0020086. ADM was supported by the U.S. Department of Energy, Office of Science, Office of High Energy Physics, under Award Number DE-SC0019022. ARZ was funded by the US National Science Foundation (NSF) through grants AST 1516266 and AST 1517563. DYT thanks Prof. Steve Ahlen for his mentorship and support and acknowledges the generous support by U.S. Department of Energy Office of Science, grant No. DE-SC0015628. This research is supported by the Director, Office of Science, Office of High Energy Physics of the U.S. Department of Energy under Contract No. DE-AC02-05CH1123, and by the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract; additional support for DESI is provided by the U.S. National Science Foundation, Division of Astronomical Sciences underContract No. AST-0950945 to the National Optical Astronomy Observatory; the Science and Technologies Facilities Council of the United Kingdom; the Gordon and Betty Moore Foundation; the Heising-Simons Foundation; the French Alternative Energies and Atomic EnergyCommission (CEA); the National Council of Science and Technology of Mexico, and by the DESI Member Institutions. The authors are honoured to be permitted to conduct astronomical research on Iolkam Du'ag (Kitt Peak), a mountain with particular significance to the Tohono O'odham Nation. The Legacy Surveys consist of three individual and complementary projects: the Dark Energy Camera Legacy Survey (DECaLS; NOAO Proposal ID #2014B-0404; PIs: David Schlegel and Arjun Dey), the Beijing-Arizona Sky Survey (BASS; NOAO Proposal ID #2015A-0801; PIs: Zhou Xu and Xiaohui Fan), and theMayall z-band Legacy Survey (MzLS; NOAOProposal ID #2016A-0453; PI: Arjun Dey). DECaLS, BASS, and MzLS together include data obtained, respectively, at the Blanco telescope, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory (NOAO); the Bok telescope, Steward Observatory, University of Arizona; and the Mayall telescope, Kitt Peak National Observatory, NOAO. The Legacy Surveys project is honoured to be permitted to conduct astronomical research on Iolkam Du'ag (Kitt Peak), a mountain with particular significance to the Tohono O'odham Nation. This project used data obtained with the Dark Energy Camera (DECam), which was constructed by the Dark Energy Survey (DES) collaboration. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at UrbanaChampaign, the Kavli Institute of Cosmological Physics at the University of Chicago, Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, the Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University. BASS is a key project of the Telescope Access Program (TAP), which has been funded by the National Astronomical Observatories of China, the Chinese Academy of Sciences (the Strategic Priority Research Program 'The Emergence of Cosmological Structures' Grant #XDB09000000), and the Special Fund for Astronomy from the Ministry of Finance. The BASS is also supported by the External Cooperation Program of Chinese Academy of Sciences (Grant #114A11KYSB20160057), and National Natural Science Foundation of China (Grant #11433005). The Legacy Survey team makes use of data products from the Near-Earth Object Wide-field Infrared Survey Explorer (NEOWISE), which is a project of the Jet Propulsion Laboratory/California Institute of Technology. NEOWISE is funded by the National Aeronautics and Space Administration. The Legacy Surveys imaging of the DESI footprint is supported by the Director, Office of Science, Office of High Energy Physics of the U.S. Department of Energy under Contract No. DE-AC02-05CH1123, by the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract; and by the U.S. National Science Foundation, Division of Astronomical Sciences under Contract No. AST-0950945 to NOAO. Funding for the DEEP2 Galaxy Redshift Survey has been provided by NSF grants AST-95-09298, AST-0071048, AST-0507428, and AST-0507483 as well as NASA LTSA grant NNG04GC89G. Funding for the DEEP3 Galaxy Redshift Survey has been provided by NSF grants AST-0808133, AST-0807630, and AST-0806732. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, theU.S. Department ofEnergy, theNational Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. Funding for the SloanDigital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO, and the participating institutions. The GAMA website is http://www.gama-survey.org/.This paper uses data from the VIMOS Public Extragalactic Redshift Survey (VIPERS). VIPERS has been performed using the ESO Very Large Telescope, under the `Large Programme' 182.A-0886. The participating institutions and funding agencies are listed at http://vipers.inaf.it.This research uses data from the VIMOS VLT Deep Survey, obtained from the VVDS database operated by Cesam, Laboratoire d'Astrophysique de Marseille, France., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.
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- 2021
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32. Illuminating Dark Matter Halo Density Profiles Without Subhaloes
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Jeffrey A. Newman, Risa H. Wechsler, Catherine E. Fielder, Hao-Yi Wu, Andrew R. Zentner, and Yao-Yuan Mao
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Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Annihilation ,Cold dark matter ,Dark matter ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Dark matter halo ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Halo ,Astrophysics::Galaxy Astrophysics ,Einasto profile ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Cold dark matter haloes consist of a relatively smooth dark matter component as well as a system of bound subhaloes. It is the prevailing practice to include all halo mass, including mass in subhaloes, in studies of halo density profiles. However, often in observational studies satellites are treated as having their own distinct dark matter density profiles in addition to the profile of the host. This difference makes comparisons between theoretical and observed results difficult. In this work we investigate density profiles of the smooth components of host haloes by excluding mass contained within subhaloes. We find that the density profiles of the smooth halo component (without subhaloes) differs substantially from the conventional halo density profile. Smooth profiles decline more rapidly at large radii and are not well characterised by the standard NFW profile. We also find that concentrations derived from smooth density profiles exhibit less scatter at fixed mass and a weaker mass dependence than standard concentrations. Both smooth and standard halo profiles can be described by a generalised Einasto profile, an Einasto profile with a modified central slope, with smaller residuals than either an NFW or Einasto profile. These results hold for both Milky Way-mass and cluster-mass haloes. This new characterisation of smooth halo profiles can be useful for many analyses, such as lensing and dark matter annihilation, in which the smooth and clumpy components of a halo should be accounted for separately., 19 pages, 9 figures, appendices, submitted to MNRAS
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- 2020
33. Concentrations of Dark Haloes Emerge from Their Merger Histories
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Andrew R. Zentner, Risa H. Wechsler, Frank C. van den Bosch, Yao-Yuan Mao, Johannes U Lange, and Kuan Wang
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Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010308 nuclear & particles physics ,media_common.quotation_subject ,Dark matter ,Small deviations ,Concentration parameter ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Astrophysics - Astrophysics of Galaxies ,Dark matter halo ,13. Climate action ,Space and Planetary Science ,Sky ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,Halo ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,media_common ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The concentration parameter is a key characteristic of a dark matter halo that conveniently connects the halo's present-day structure with its assembly history. Using 'Dark Sky', a suite of cosmological $N$-body simulations, we investigate how halo concentration evolves with time and emerges from the mass assembly history. We also explore the origin of the scatter in the relation between concentration and assembly history. We show that the evolution of halo concentration has two primary modes: (1) smooth increase due to pseudo-evolution; and (2) intense responses to physical merger events. Merger events induce lasting and substantial changes in halo structures, and we observe a universal response in the concentration parameter. We argue that merger events are a major contributor to the uncertainty in halo concentration at fixed halo mass and formation time. In fact, even haloes that are typically classified as having quiescent formation histories experience multiple minor mergers. These minor mergers drive small deviations from pseudo-evolution, which cause fluctuations in the concentration parameters and result in effectively irreducible scatter in the relation between concentration and assembly history. Hence, caution should be taken when using present-day halo concentration parameter as a proxy for the halo assembly history, especially if the recent merger history is unknown., 15 pages, 7 + 1 figures, accepted for publication in MNRAS, comments welcome
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- 2020
34. Signatures of Velocity-Dependent Dark Matter Self-Interactions in Milky Way-mass Halos
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Arka Banerjee, Susmita Adhikari, Yao-Yuan Mao, Risa H. Wechsler, and Ethan O. Nadler
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Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010504 meteorology & atmospheric sciences ,Milky Way ,Momentum transfer ,Dark matter ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Ram pressure ,Momentum ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,Halo ,Anisotropy ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We explore the impact of elastic, anisotropic, velocity-dependent dark matter (DM) self-interactions on the host halo and subhalos of Milky Way (MW)--mass systems. We consider a generic self-interacting dark matter (SIDM) model parameterized by the masses of a light mediator and the DM particle. The ratio of these masses, $w$, sets the velocity scale above which momentum transfer due to DM self-interactions becomes inefficient. We perform high-resolution zoom-in simulations of an MW-mass halo for values of $w$ that span scenarios in which self-interactions either between the host and its subhalos or only within subhalos efficiently transfer momentum, and we study the effects of self-interactions on the host halo and on the abundance, radial distribution, orbital dynamics, and density profiles of subhalos in each case. The abundance and properties of surviving subhalos are consistent with being determined primarily by subhalo--host halo interactions. In particular, subhalos on radial orbits in models with larger values of the cross section at the host halo velocity scale are more susceptible to tidal disruption owing to mass loss from ram pressure stripping caused by self-interactions with the host. This mechanism suppresses the abundance of surviving subhalos relative to collisionless DM simulations, with stronger suppression for larger values of $w$. Thus, probes of subhalo abundance around MW-mass hosts can be used to place upper limits on the self-interaction cross section at velocity scales of $\sim 200\ \rm{km\ s}^{-1}$, and combining these measurements with the orbital properties and internal dynamics of subhalos may break degeneracies among velocity-dependent SIDM models., 19 pages, 10 figures, 1 table. Updated to published version
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- 2020
35. The SAGA Survey. II. Building a Statistical Sample of Satellite Systems around Milky Way-like Galaxies
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Nitya Kallivayalil, Risa H. Wechsler, Erik Tollerud, Benjamin J. Weiner, Ethan O. Nadler, Marla Geha, and Yao-Yuan Mao
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Physics ,Cold dark matter ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010504 meteorology & atmospheric sciences ,Milky Way ,Local Group ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,01 natural sciences ,Galaxy ,Luminosity ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,Satellite galaxy ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics ,0105 earth and related environmental sciences ,Dwarf galaxy ,Luminosity function (astronomy) - Abstract
We present the Stage II results from the ongoing Satellites Around Galactic Analogs (SAGA) Survey. Upon completion, the SAGA Survey will spectroscopically identify satellite galaxies brighter than $ M_{r,o} = -12.3 $ around 100 Milky Way (MW) analogs at $ z \sim 0.01 $. In Stage II, we have more than quadrupled the sample size of Stage I, delivering results from 127 satellites around 36 MW analogs with an improved target selection strategy and deep photometric imaging catalogs from the Dark Energy Survey and the Legacy Surveys. We have obtained 25,372 galaxy redshifts, peaking around $ z = 0.2 $. These data significantly increase spectroscopic coverage for very low redshift objects in $ 17 < r_o < 20.75 $ around SAGA hosts, creating a unique data set that places the Local Group in a wider context. The number of confirmed satellites per system ranges from zero to nine, and correlates with host galaxy and brightest satellite luminosities. We find that the number and the luminosities of MW satellites are consistent with being drawn from the same underlying distribution as SAGA systems. The majority of confirmed SAGA satellites are star forming, and the quenched fraction increases as satellite stellar mass and projected radius from the host galaxy decrease. Overall, the satellite quenched fraction among SAGA systems is lower than that in the Local Group. We compare the luminosity functions and radial distributions of SAGA satellites with theoretical predictions based on cold dark matter simulations and an empirical galaxy-halo connection model and find that the results are broadly in agreement., 42 pages, 22 figures, 3 tables. See Sec. 9 (p.28) for summary and figure index. Main results are shown in Sec. 6-8 (Fig. 8-18). Accepted by ApJ. Data available on survey website: https://sagasurvey.org
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- 2020
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36. Halo histories versus galaxy properties at z = 0 – III. The properties of star-forming galaxies
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ChangHoon Hahn, Yao-Yuan Mao, Jeremy L. Tinker, and Andrew Wetzel
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astro-ph.GA ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,Galaxy merger ,01 natural sciences ,Galactic halo ,Galaxy group ,0103 physical sciences ,Brightest cluster galaxy ,010303 astronomy & astrophysics ,Lenticular galaxy ,evolution [galaxies] ,Astrophysics::Galaxy Astrophysics ,Galaxy rotation curve ,Physics ,010308 nuclear & particles physics ,Astronomy ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,observations [cosmology] ,Dark matter halo ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Elliptical galaxy ,Astronomical and Space Sciences - Abstract
We measure how the properties of star-forming central galaxies correlate with large-scale environment, $\delta$, measured on $10$Mpc/h scales. We use group catalogs to isolate a robust sample of central galaxies with high purity and completeness. The properties we investigate are star formation rate (SFR), exponential disk scale length $R_{\rm exp}$, and Sersic index of the light profile, $n$. We find that, at all stellar masses, there is an inverse correlation between SFR and $\delta$, meaning that above-average star forming centrals live in underdense regions. For $n$ and $R_{\rm exp}$, there is no correlation with $\delta$ at $M_{\rm star}\lesssim 10^{10.5}$ $M_\odot$, but at higher masses there are positive correlations; a weak correlation with $R_{\rm exp}$ and a strong correlation with $n$. These data are evidence of assembly bias within the star-forming population. The results for SFR are consistent with a model in which SFR correlates with present-day halo accretion rate, $\dot{M}_h$. In this model, galaxies are assigned to halos using the abundance matching ansatz, which maps galaxy stellar mass onto halo mass. At fixed halo mass, SFR is assigned to galaxies using the same approach,but $\dot{M}_h$ is used to map onto SFR. The best-fit model requires some scatter in the $\dot{M}_h$-SFR relation. The $R_{\rm exp}$ and $n$ measurements are consistent with a model in which these quantities are correlated with the spin parameter of the halo, $\lambda$. Halo spin does not correlate with $\delta$ at low halo masses, but for higher mass halos, high-spin halos live in higher density environments at fixed $M_h$. Put together with the earlier installments of this series, these data demonstrate that quenching processes have limited correlation with halo formation history, but the growth of active galaxies, as well as other detailed properties, are influenced by the details of halo assembly., Comment: 13 pages, submitted to MNRAS
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- 2018
37. Halo histories versus Galaxy properties at z = 0 – I. The quenching of star formation
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Charlie Conroy, Yao-Yuan Mao, Jeremy L. Tinker, and Andrew Wetzel
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Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010308 nuclear & particles physics ,Dark matter ,FOS: Physical sciences ,Astronomy ,Astronomy and Astrophysics ,Type-cD galaxy ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Astrophysics - Astrophysics of Galaxies ,01 natural sciences ,Galaxy ,Galactic halo ,Dark matter halo ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Galaxy group ,0103 physical sciences ,Halo ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Galaxy rotation curve ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We test whether halo age and galaxy age are correlated at fixed halo and galaxy mass. The formation histories, and thus ages, of dark matter halos correlate with their large-scale density $\rho$, an effect known as assembly bias. We test whether this correlation extends to galaxies by measuring the dependence of galaxy stellar age on $\rho$. To clarify the comparison between theory and observation, and to remove the strong environmental effects on satellites, we use galaxy group catalogs to identify central galaxies and measure their quenched fraction, $f_Q$, as a function of large-scale environment. Models that match halo age to central galaxy age predict a strong positive correlation between $f_Q$ and $\rho$. However, we show that the amplitude of this effect depends on the definition of halo age: assembly bias is significantly reduced when removing the effects of splashback halos---those halos that are central but have passed through a larger halo or experienced strong tidal encounters. Defining age using halo mass at its peak value rather than current mass removes these effects. In SDSS data, at M$_{\rm gal}\gtrsim 10^{10.0}$ M_sol/h$^2$, there is a $\sim 5\%$ increase in $f_Q$ from low to high densities, which is in agreement with predictions of dark matter halos using peak halo mass. At lower stellar mass there is little to no correlation of $f_Q$ with $\rho$. For these galaxies, age-matching is inconsistent with the data across the wide range the halo formation metrics that we tested. This implies that halo formation history has a small but statistically significant impact on quenching of star formation at high masses, while the quenching process in low-mass central galaxies is uncorrelated with halo formation history., Comment: 13 pages, 12 figures, submitted to MNRAS
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- 2017
38. Probing the galaxy-halo connection with total satellite luminosity
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J. DeRose, Jeremy L. Tinker, Junzhi Cao, Yao-Yuan Mao, Mehmet Alpaslan, and Risa H. Wechsler
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Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Stellar mass ,010308 nuclear & particles physics ,media_common.quotation_subject ,Dark matter ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Luminosity ,Space and Planetary Science ,Sky ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,Satellite galaxy ,Halo ,010303 astronomy & astrophysics ,Weak gravitational lensing ,Astrophysics::Galaxy Astrophysics ,media_common ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We demonstrate how the total luminosity in satellite galaxies is a powerful probe of dark matter halos around central galaxies. The method cross-correlates central galaxies in spectroscopic galaxy samples with fainter galaxies detected in photometric surveys. After background subtraction, the excess galaxies around the central galaxies represent faint satellite galaxies within the dark matter halo. Using abundance matching models, we show that the the total galaxy luminosity, L_sat, scales linearly with host halo mass, making L_sat an excellent proxy for M_h. L_sat is also sensitive to the formation time of the halo, as younger halos have more substructure at fixed M_h. We demonstrate that probes of galaxy large-scale environment can break this degeneracy. Although this is an indirect probe of the halo, it can yield a high-S/N measurement for galaxies expected to occupy halos at $, 21 pages, submitted to MNRAS
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- 2019
39. Constraining the scatter in the galaxy-halo connection at Milky Way masses
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Jeremy L. Tinker, Yao-Yuan Mao, Risa H. Wechsler, and Junzhi Cao
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Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Stellar mass ,Milky Way ,Dark matter ,Sigma ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Space and Planetary Science ,Galaxy group ,Astrophysics of Galaxies (astro-ph.GA) ,Halo ,Connection (algebraic framework) ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We develop and implement two new methods for constraining the scatter in the relationship between galaxies and dark matter halos. These new techniques are sensitive to the scatter at low halo masses, making them complementary to previous constraints that are dependent on clustering amplitudes or rich galaxy groups, both of which are only sensitive to more massive halos. In both of our methods, we use a galaxy group finder to locate central galaxies in the SDSS main galaxy sample. Our first technique uses the small-scale cross-correlation of central galaxies with all lower mass galaxies. This quantity is sensitive to the satellite fraction of low-mass galaxies, which is in turn driven by the scatter between halos and galaxies. The second technique uses the kurtosis of the distribution of line-of-sight velocities between central galaxies and neighboring galaxies. This quantity is sensitive to the distribution of halo masses that contain the central galaxies at fixed stellar mass. Theoretical models are constructed using peak halo circular velocity, $V_{\rm peak}$, as our property to connect galaxies to halos. The cross-correlation technique yields a constraint of $\sigma[ M_\ast|V_{\rm peak}]=0.27\pm 0.05$ dex, corresponding to a scatter in $\log M_\ast$ at fixed $M_h$ of $\sigma[ M_\ast|M_h]=0.38\pm 0.06$ dex at $M_h=10^{11.8}$ Msun. The kurtosis technique yields $\sigma[ M_\ast|V_{\rm peak}]=0.30\pm0.03$, corresponding to $\sigma[ M_\ast|M_h]=0.34\pm 0.04$ at $M_h=10^{12.2}$ Msun. The values of $\sigma[ M_\ast|M_h]$ are significantly larger than the constraints at higher masses, in agreement with the results of hydrodynamic simulations. This increase is only partly due to the scatter between $V_{\rm peak}$ and $M_h$, and it represents an increase of nearly a factor of two relative to the values inferred from clustering and group studies at high masses., Comment: 14 pages, 13 figures, submitted to MNRAS
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- 2019
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40. Probing the Fundamental Nature of Dark Matter with the Large Synoptic Survey Telescope
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Alex Drlica-Wagner, Yao-Yuan Mao, Susmita Adhikari, Robert Armstrong, Arka Banerjee, Nilanjan Banik, Keith Bechtol, Simeon Bird, Kimberly Boddy, Ana Bonaca, Jo Bovy, Buckley, Matthew R., Esra Bulbul, Chihway Chang, George Chapline, Johann Cohen-Tanugi, Alessandro Cuoco, Francis-Yan Cyr-Racine, Dawson, William A., Ana Díaz Rivero, Cora Dvorkin, Denis Erkal, Fassnacht, Christopher D., Juan García-Bellido, Maurizio Giannotti, Vera Gluscevic, Nathan Golovich, David Hendel, Hezaveh, Yashar D., Shunsaku Horiuchi, James Jee, M., Manoj Kaplinghat, Keeton, Charles R., Koposov, Sergey E., Li, Ting S., Rachel Mandelbaum, Mcdermott, Samuel D., Mitch Mcnanna, Michael Medford, Manuel Meyer, Moniez Marc, Simona Murgia, Nadler, Ethan O., Lina Necib, Eric Nuss, Pace, Andrew B., Peter, Annika H. G., Polin, Daniel A., Chanda Prescod-Weinstein, Read, Justin I., Rogerio Rosenfeld, Nora Shipp, Simon, Joshua D., Slatyer, Tracy R., Oscar Straniero, Strigari, Louis E., Erik Tollerud, Anthony Tyson, J., Mei-Yu Wang, Wechsler, Risa H., David Wittman, Hai-Bo Yu, Gabrijela Zaharijas, Yacine Ali-Haïmoud, James Annis, Simon Birrer, Rahul Biswas, Jonathan Blazek, Brooks, Alyson M., Elizabeth Buckley-Geer, Regina Caputo, Eric Charles, Seth Digel, Scott Dodelson, Brenna Flaugher, Joshua Frieman, Eric Gawiser, Hearin, Andrew P., Renee Hložek, Bhuvnesh Jain, Jeltema, Tesla E., Koushiappas, Savvas M., Mariangela Lisanti, Marilena Loverde, Siddharth Mishra-Sharma, Newman, Jeffrey A., Brian Nord, Erfan Nourbakhsh, Steven Ritz, Robertson, Brant E., Sánchez-Conde, Miguel A., Anže Slosar, Tait, Tim M. P., Aprajita Verma, Ricardo Vilalta, Walter, Christopher W., Brian Yanny, Zentner, Andrew R., Marine Sciences Research Center (MSRC), Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Ohio State University [Columbus] (OSU), Abdus Salam International Centre for Theoretical Physics [Trieste] (ICTP), SLAC National Accelerator Laboratory (SLAC), Stanford University, Department of Physics and Astronomy [Pittsburgh], University of Pittsburgh (PITT), Pennsylvania Commonwealth System of Higher Education (PCSHE)-Pennsylvania Commonwealth System of Higher Education (PCSHE), California Institute of Technology (CALTECH), LSST Dark Energy Collaboration, and Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2)
- Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics - Abstract
94 pages, 22 figures, 1 table; Astrophysical and cosmological observations currently provide the only robust, empirical measurements of dark matter. Future observations with Large Synoptic Survey Telescope (LSST) will provide necessary guidance for the experimental dark matter program. This white paper represents a community effort to summarize the science case for studying the fundamental physics of dark matter with LSST. We discuss how LSST will inform our understanding of the fundamental properties of dark matter, such as particle mass, self-interaction strength, non-gravitational couplings to the Standard Model, and compact object abundances. Additionally, we discuss the ways that LSST will complement other experiments to strengthen our understanding of the fundamental characteristics of dark matter. More information on the LSST dark matter effort can be found at https://lsstdarkmatter.github.io/ .
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- 2019
41. Sussing merger trees: stability and convergence
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Frazer R. Pearce, Jiaxin Han, Alexander Knebe, Yipeng Jing, Dylan Tweed, Weipeng Lin, Vicente Rodriguez-Gomez, Julian Onions, Pascal J. Elahi, Chaichalit Srisawat, Aurel Schneider, Intae Jung, John C. Helly, Yao-Yuan Mao, Peter A. Thomas, Yang Wang, Peter Behroozi, and Sukyoung K. Yi
- Subjects
Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Structure formation ,COSMIC cancer database ,010308 nuclear & particles physics ,Dark matter ,ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,01 natural sciences ,Stability (probability) ,Tree (graph theory) ,Space and Planetary Science ,0103 physical sciences ,Range (statistics) ,Galaxy formation and evolution ,methods: numerical, galaxies: haloes– galaxies: evolution, dark matter ,Halo ,010303 astronomy & astrophysics ,QB ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Merger trees are routinely used to follow the growth and merging history of dark matter haloes and subhaloes in simulations of cosmic structure formation. Srisawat et al. (2013) compared a wide range of merger-tree-building codes. Here we test the influence of output strategies and mass resolution on tree-building. We find that, somewhat surprisingly, building the tree from more snapshots does not generally produce more complete trees; instead, it tends to short- en them. Significant improvements are seen for patching schemes which attempt to bridge over occasional dropouts in the underlying halo catalogues or schemes which combine the halo-finding and tree-building steps seamlessly. The adopted output strategy does not affec- t the average number of branches (bushiness) of the resultant merger trees. However, mass resolution has an influence on both main branch length and the bushiness. As the resolution increases, a halo with the same mass can be traced back further in time and will encounter more small progenitors during its evolutionary history. Given these results, we recommend that, for simulations intended as precursors for galaxy formation models where of order 100 or more snapshots are analysed, the tree-building routine should be integrated with the halo finder, or at the very least be able to patch over multiple adjacent snapshots., 16 pages, 14 figures, accepted by MNRAS
- Published
- 2016
42. Two Ultra-faint Milky Way Stellar Systems Discovered in Early Data from the DECam Local Volume Exploration Survey
- Author
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Erik Tollerud, L. C. Johnson, D. Hernandez-Lang, Steven R. Majewski, Guy S. Stringfellow, David J. Sand, M. McNanna, Keith Bechtol, J. D. Simon, C. E. Martínez-Vázquez, Yao-Yuan Mao, N. P. Kuropatkin, Alistair R. Walker, David James, Eric H. Neilsen, Prashin Jethwa, Marcelle Soares-Santos, Brian Yanny, Risa H. Wechsler, Andrew B. Pace, R. P. van der Marel, Y. Choi, Adriano Pieres, Sahar S. Allam, Allison K. Hughes, Pol Massana, Eric F. Bell, Denis Erkal, S. Mau, Jeffrey L. Carlin, F. Paz-Chinchón, Wayne A. Barkhouse, Knut Olsen, P. S. Ferguson, Burçin Mutlu-Pakdil, Monika Adamów, Tenglin Li, David L. Nidever, A. Zenteno, P. Balaji, Eric Morganson, K. Tavangar, Carme Gallart, Ethan O. Nadler, Kyler Kuehn, Noelia E. D. Noël, Alex Drlica-Wagner, Javier Sanchez, Denija Crnojević, L. Santana-Silva, A. H. Riley, W. Cerny, Antonella Palmese, Douglas L. Tucker, Nora Shipp, Antonela Monachesi, A. K. Vivas, J. Esteves, and Robert A. Gruendl
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Physics ,education.field_of_study ,Proper motion ,010504 meteorology & atmospheric sciences ,Metallicity ,Milky Way ,Population ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Horizontal branch ,Astrophysics - Astrophysics of Galaxies ,01 natural sciences ,Stars ,Star cluster ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,education ,Large Magellanic Cloud ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences - Abstract
We report the discovery of two ultra-faint stellar systems found in early data from the DECam Local Volume Exploration survey (DELVE). The first system, Centaurus I (DELVE J1238-4054), is identified as a resolved overdensity of old and metal-poor stars with a heliocentric distance of ${\rm D}_{\odot} = 116.3_{-0.6}^{+0.6}$ kpc, a half-light radius of $r_h = 2.3_{-0.3}^{+0.4}$ arcmin, an age of $\tau > 12.85$ Gyr, a metallicity of $Z = 0.0002_{-0.0002}^{+0.0001}$, and an absolute magnitude of $M_V = -5.55_{-0.11}^{+0.11}$ mag. This characterization is consistent with the population of ultra-faint satellites, and confirmation of this system would make Centaurus I one of the brightest recently discovered ultra-faint dwarf galaxies. Centaurus I is detected in Gaia DR2 with a clear and distinct proper motion signal, confirming that it is a real association of stars distinct from the Milky Way foreground; this is further supported by the clustering of blue horizontal branch stars near the centroid of the system. The second system, DELVE 1 (DELVE J1630-0058), is identified as a resolved overdensity of stars with a heliocentric distance of ${\rm D}_{\odot} = 19.0_{-0.6}^{+0.5} kpc$, a half-light radius of $r_h = 0.97_{-0.17}^{+0.24}$ arcmin, an age of $\tau = 12.5_{-0.7}^{+1.0}$ Gyr, a metallicity of $Z = 0.0005_{-0.0001}^{+0.0002}$, and an absolute magnitude of $M_V = -0.2_{-0.6}^{+0.8}$ mag, consistent with the known population of faint halo star clusters. Given the low number of probable member stars at magnitudes accessible with Gaia DR2, a proper motion signal for DELVE 1 is only marginally detected. We compare the spatial position and proper motion of both Centaurus I and DELVE 1 with simulations of the accreted satellite population of the Large Magellanic Cloud (LMC) and find that neither is likely to be associated with the LMC., Comment: 17 pages, 6 figures, 1 table; updated to match published version; updated to address erratum
- Published
- 2020
43. CosmoDC2: A Synthetic Sky Catalog for Dark Energy Science with LSST
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François Lanusse, Adrian Pope, Katrin Heitmann, Eve Kovacs, Christopher B. Morrison, Anita Bahmanyar, Rachel Mandelbaum, Benjamin Joachimi, Melanie Simet, Hal Finkel, Martin White, Chun-Hao To, Esteban Rangel, Andrew J. Benson, Yao-Yuan Mao, Jeffrey A. Newman, Chihway Chang, Andrew P. Hearin, Danila Korytov, Nan Li, Joseph Hollowed, Patricia Larsen, Eli S. Rykoff, Joseph DeRose, Salman Habib, Duncan Campbell, Risa H. Wechsler, Eric Gawiser, Vinu Vikraman, and Nicholas Frontiere
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Stellar mass ,astro-ph.GA ,media_common.quotation_subject ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Large Synoptic Survey Telescope ,Astronomy & Astrophysics ,Atomic ,01 natural sciences ,Cosmology ,Particle and Plasma Physics ,Affordable and Clean Energy ,0103 physical sciences ,Nuclear ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Weak gravitational lensing ,media_common ,Physics ,010308 nuclear & particles physics ,Astrophysics::Instrumentation and Methods for Astrophysics ,Molecular ,Astronomy ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Redshift ,Galaxy ,13. Climate action ,Space and Planetary Science ,Sky ,Astrophysics of Galaxies (astro-ph.GA) ,astro-ph.CO ,Dark energy ,Astronomical and Space Sciences ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Physical Chemistry (incl. Structural) - Abstract
This paper introduces cosmoDC2, a large synthetic galaxy catalog designed to support precision dark energy science with the Large Synoptic Survey Telescope (LSST). CosmoDC2 is the starting point for the second data challenge (DC2) carried out by the LSST Dark Energy Science Collaboration (LSST DESC). The catalog is based on a trillion-particle, 4.225 Gpc^3 box cosmological N-body simulation, the `Outer Rim' run. It covers 440 deg^2 of sky area to a redshift of z=3 and is complete to a magnitude depth of 28 in the r-band. Each galaxy is characterized by a multitude of properties including stellar mass, morphology, spectral energy distributions, broadband filter magnitudes, host halo information and weak lensing shear. The size and complexity of cosmoDC2 requires an efficient catalog generation methodology; our approach is based on a new hybrid technique that combines data-driven empirical approaches with semi-analytic galaxy modeling. A wide range of observation-based validation tests has been implemented to ensure that cosmoDC2 enables the science goals of the planned LSST DESC DC2 analyses. This paper also represents the official release of the cosmoDC2 data set, including an efficient reader that facilitates interaction with the data., Comment: 27 pages, 17 figures, submitted to APJS
- Published
- 2019
44. Predictably Missing Satellites: Subhalo Abundance in Milky Way-like Halos
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Yao-Yuan Mao, Catherine E. Fielder, Jeffrey A. Newman, Timothy C. Licquia, and Andrew R. Zentner
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Physics ,Cold dark matter ,010308 nuclear & particles physics ,Milky Way ,Dark matter ,Dwarf galaxy problem ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,01 natural sciences ,Galaxy ,Space and Planetary Science ,Abundance (ecology) ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,Halo ,010303 astronomy & astrophysics ,Scale factor (cosmology) ,Astrophysics::Galaxy Astrophysics - Abstract
On small scales there have been a number of claims of discrepancies between the standard Cold Dark Matter (CDM) model and observations. The 'missing satellites problem' infamously describes the overabundance of subhalos from CDM simulations compared to the number of satellites observed in the Milky Way. A variety of solutions to this discrepancy have been proposed; however, the impact of the specific properties of the Milky Way halo relative to the typical halo of its mass have yet to be explored. Motivated by recent studies that identified ways in which the Milky Way is atypical (e.g., Licquia et al. 2015), we investigate how the properties of dark matter halos with mass comparable to our Galaxy's --- including concentration, spin, shape, and scale factor of the last major merger --- correlate with the subhalo abundance. Using zoom-in simulations of Milky Way-like halos, we build two models of subhalo abundance as functions of host halo properties and conclude that the Milky Way should be expected to have 22%-44% fewer subhalos with low maximum rotation velocities ($V_{\rm max}^{\rm sat} \sim 10$kms$^{-1}$) at the 95% confidence level and up to 72% fewer than average subhalos with high rotation velocities ($V_{\rm max}^{\rm sat} \gtrsim 30$kms$^{-1}$, comparable to the Magellanic Clouds) than would be expected for a typical halo of the Milky Way's mass. Concentration is the most informative single parameter for predicting subhalo abundance. Our results imply that models tuned to explain the missing satellites problem assuming typical subhalo abundances for our Galaxy will be over-correcting., Comment: 21 pages, 11 figures, submitted to Monthly Notices of the Royal Astronomical Society
- Published
- 2018
- Full Text
- View/download PDF
45. The Aemulus Project II: Emulating the Halo Mass Function
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Matthew R. Becker, J. DeRose, Thomas McClintock, Zhongxu Zhai, Sean McLaughlin, Risa H. Wechsler, Eduardo Rozo, Yao-Yuan Mao, and Jeremy L. Tinker
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Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010504 meteorology & atmospheric sciences ,Halo mass function ,Foundation (engineering) ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,01 natural sciences ,Nuclear physics ,Methods statistical ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,Astrophysics - Instrumentation and Methods for Astrophysics ,010303 astronomy & astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Astrophysics - Cosmology and Nongalactic Astrophysics ,0105 earth and related environmental sciences - Abstract
Existing models for the dependence of the halo mass function on cosmological parameters will become a limiting source of systematic uncertainty for cluster cosmology in the near future. We present a halo mass function emulator and demonstrate improved accuracy relative to state-of-the-art analytic models. In this work, mass is defined using an overdensity criteria of 200 relative to the mean background density. Our emulator is constructed from the AEMULUS simulations, a suite of 40 N-body simulations with snapshots from z=3 to z=0. These simulations cover the flat wCDM parameter space allowed by recent Cosmic Microwave Background, Baryon Acoustic Oscillation and Type Ia Supernovae results, varying the parameters w, Omega_m, Omega_b, sigma_8, N_{eff}, n_s, and H_0. We validate our emulator using five realizations of seven different cosmologies, for a total of 35 test simulations. These test simulations were not used in constructing the emulator, and were run with fully independent initial conditions. We use our test simulations to characterize the modeling uncertainty of the emulator, and introduce a novel way of marginalizing over the associated systematic uncertainty. We confirm non-universality in our halo mass function emulator as a function of both cosmological parameters and redshift. Our emulator achieves better than 1% precision over much of the relevant parameter space, and we demonstrate that the systematic uncertainty in our emulator will remain a negligible source of error for cluster abundance studies through at least the LSST Year 1 data set., Comment: https://aemulusproject.github.io/
- Published
- 2018
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46. The Galaxy Clustering Crisis in Abundance Matching
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Fangzhou Jiang, Antonio Villarreal, Yao-Yuan Mao, Andrew R. Zentner, Duncan Campbell, Frank C. van den Bosch, Johannes U. Lange, and Nikhil Padmanabhan
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Physics ,education.field_of_study ,Stellar mass ,Accretion (meteorology) ,010308 nuclear & particles physics ,Dark matter ,Population ,Astronomy ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,Satellite galaxy ,Halo ,Cluster analysis ,education ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
Galaxy clustering on small scales is significantly under-predicted by sub-halo abundance matching (SHAM) models that populate (sub-)haloes with galaxies based on peak halo mass, $M_{\rm peak}$. SHAM models based on the peak maximum circular velocity, $V_{\rm peak}$, have had much better success. The primary reason $M_{\rm peak}$ based models fail is the relatively low abundance of satellite galaxies produced in these models compared to those based on $V_{\rm peak}$. Despite success in predicting clustering, a simple $V_{\rm peak}$ based SHAM model results in predictions for galaxy growth that are at odds with observations. We evaluate three possible remedies that could "save" mass-based SHAM: (1) SHAM models require a significant population of "orphan" galaxies as a result of artificial disruption/merging of sub-haloes in modern high resolution dark matter simulations; (2) satellites must grow significantly after their accretion; and (3) stellar mass is significantly affected by halo assembly history. No solution is entirely satisfactory. However, regardless of the particulars, we show that popular SHAM models based on $M_{\rm peak}$ cannot be complete physical models as presented. Either $V_{\rm peak}$ truly is a better predictor of stellar mass at $z\sim 0$ and it remains to be seen how the correlation between stellar mass and $V_{\rm peak}$ comes about, or SHAM models are missing vital component(s) that significantly affect galaxy clustering., 25 pages, 22 figures, submitted to MNRAS, comments welcome
- Published
- 2017
47. The Radial Acceleration Relation in Disk Galaxies in the MassiveBlack-II Simulation
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Rupert A. C. Croft, Andrew R. Zentner, Tiziana Di Matteo, Fernando Zago, Ananth Tenneti, Arthur Kosowsky, and Yao-Yuan Mao
- Subjects
Physics ,Surface brightness fluctuation ,Dark matter ,Astronomy ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Disc galaxy ,Astrophysics - Astrophysics of Galaxies ,01 natural sciences ,Galaxy ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,Elliptical galaxy ,Galaxy formation and evolution ,Surface brightness ,010306 general physics ,010303 astronomy & astrophysics ,Galaxy rotation curve ,Astrophysics::Galaxy Astrophysics - Abstract
A strong correlation has been measured between the observed centripetal accelerations in galaxies and the accelerations implied by the baryonic components of galaxies. This empirical radial acceleration relation must be accounted for in any viable model of galaxy formation. We measure and compare the radial accelerations contributed by baryons and by dark matter in disk galaxies in the MassiveBlack-II hydrodynamic galaxy formation simulation. The sample of 1594 galaxies spans three orders of magnitude in luminosity and four in surface brightness, comparable to the observed sample from the Spitzer Photometry & Accurate Rotation Curves (SPARC) dataset used by McGaugh et al. (2016). We find that radial accelerations contributed by baryonic matter only and by total matter are highly correlated, with only small scatter around their mean or median relation, despite the wide ranges of galaxy luminosity and surface brightness. We further find that the radial acceleration relation in this simulation differs from that of the SPARC sample, and can be described by a simple power law in the acceleration range we are probing., 7 pages, 4 figures
- Published
- 2017
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48. DESCQA: An Automated Validation Framework for Synthetic Sky Catalogs
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K. Simon Krughoff, Rachel Mandelbaum, Yao-Yuan Mao, Salman Habib, Risa H. Wechsler, François Lanusse, Duncan Campbell, Thomas D. Uram, Andrés N. Ruiz, Andrew J. Benson, E. Paillas, Zarija Lukić, Tiziana Di Matteo, Rongpu Zhou, Adrian Pope, Ananth Tenneti, Cristian A Vega-Martínez, Sofía A. Cora, Nelson Padilla, Paul M. Ricker, Katrin Heitmann, Jeffrey A. Newman, Ying Zu, Andrew P. Hearin, Eve Kovacs, J. Bryce Kalmbach, and Joseph DeRose
- Subjects
Ciencias Astronómicas ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Interface (Java) ,Ciencias Físicas ,NUMERICAL [METHODS] ,media_common.quotation_subject ,Large-scale structure of universe ,FOS: Physical sciences ,Large Synoptic Survey Telescope ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,Physical Chemistry ,Atomic ,01 natural sciences ,010305 fluids & plasmas ,purl.org/becyt/ford/1 [https] ,Set (abstract data type) ,Particle and Plasma Physics ,0103 physical sciences ,Nuclear ,Quality (business) ,Astronomical And Space Sciences ,010303 astronomy & astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,media_common ,Physics ,Information retrieval ,Organic Chemistry ,Astrophysics::Instrumentation and Methods for Astrophysics ,Molecular ,Astronomy and Astrophysics ,purl.org/becyt/ford/1.3 [https] ,Pipeline (software) ,Astronomía ,Space and Planetary Science ,Sky ,Fundamental physics ,astro-ph.CO ,LARGE-SCALE STRUCTURE OF UNIVERSE ,Astrophysics - Instrumentation and Methods for Astrophysics ,CIENCIAS NATURALES Y EXACTAS ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Numerical analysis ,astro-ph.IM ,Physical Chemistry (incl. Structural) - Abstract
The use of high-quality simulated sky catalogs is essential for the success of cosmological surveys. The catalogs have diverse applications, such as investigating signatures of fundamental physics in cosmological observables, understanding the effect of systematic uncertainties on measured signals and testing mitigation strategies for reducing these uncertainties, aiding analysis pipeline development and testing, and survey strategy optimization. The list of applications is growing with improvements in the quality of the catalogs and the details that they can provide. Given the importance of simulated catalogs, it is critical to provide rigorous validation protocols that enable both catalog providers and users to assess the quality of the catalogs in a straightforward and comprehensive way. For this purpose, we have developed the DESCQA framework for the Large Synoptic Survey Telescope Dark Energy Science Collaboration as well as for the broader community. The goal of DESCQA is to enable the inspection, validation, and comparison of an inhomogeneous set of synthetic catalogs via the provision of a common interface within an automated framework. In this paper, we present the design concept and first implementation of DESCQA. In order to establish and demonstrate its full functionality we use a set of interim catalogs and validation tests. We highlight several important aspects, both technical and scientific, that require thoughtful consideration when designing a validation framework, including validation metrics and how these metrics impose requirements on the synthetic sky catalogs., La lista completa de autores se encuentra en el documento., Instituto de Astrofísica de La Plata, Facultad de Ciencias Astronómicas y Geofísicas
- Published
- 2017
- Full Text
- View/download PDF
49. Beyond Assembly Bias: Exploring Secondary Halo Biases for Cluster-size Haloes
- Author
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Andrew R. Zentner, Risa H. Wechsler, and Yao-Yuan Mao
- Subjects
Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010308 nuclear & particles physics ,Dark matter ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Radial distribution ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Cosmology ,Galaxy ,Space and Planetary Science ,0103 physical sciences ,Halo effect ,Cluster size ,Halo ,Proxy (statistics) ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Secondary halo bias, commonly known as 'assembly bias,' is the dependence of halo clustering on a halo property other than mass. This prediction of the Lambda-Cold Dark Matter cosmology is essential to modelling the galaxy distribution to high precision and interpreting clustering measurements. As the name suggests, different manifestations of secondary halo bias have been thought to originate from halo assembly histories. We show conclusively that this is incorrect for cluster-size haloes. We present an up-to-date summary of secondary halo biases of high-mass haloes due to various halo properties including concentration, spin, several proxies of assembly history, and subhalo properties. While concentration, spin, and the abundance and radial distribution of subhaloes exhibit significant secondary biases, properties that directly quantify halo assembly history do not. In fact, the entire assembly histories of haloes in pairs are nearly identical to those of isolated haloes. In general, a global correlation between two halo properties does not predict whether or not these two properties exhibit similar secondary biases. For example, assembly history and concentration (or subhalo abundance) are correlated for both paired and isolated haloes, but follow slightly different conditional distributions in these two cases. This results in a secondary halo bias due to concentration (or subhalo abundance), despite the lack of assembly bias in the strict sense for cluster-size haloes. Due to this complexity, caution must be exercised in using any one halo property as a proxy to study the secondary bias due to another property., Comment: 14+1 pages, 9+1 figures. Figures 2 and 8 highlight the main results. Accepted by MNRAS. Fig 9 updated; main result unchanged
- Published
- 2017
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50. SUSSING MERGER TREES: the influence of the halo finder
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Julian Onions, Santiago Avila, Pascal J. Elahi, Chaichalit Srisawat, Alexander Knebe, Jiaxin Han, Frazer R. Pearce, Aurel Schneider, Yao-Yuan Mao, Dylan Tweed, Vicente Rodriguez-Gomez, Peter A. Thomas, and Peter Behroozi
- Subjects
Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Structure formation ,COSMIC cancer database ,Dark matter ,FOS: Physical sciences ,Astronomy ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Tree (graph theory) ,Prime (order theory) ,methods: numerical, galaxies: evolution, galaxies: haloes, dark matter ,Dark matter halo ,Space and Planetary Science ,Halo ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics ,QB - Abstract
Merger tree codes are routinely used to follow the growth and merger of dark matter haloes in simulations of cosmic structure formation. Whereas in Srisawat et. al. we compared the trees built using a wide variety of such codes here we study the influence of the underlying halo catalogue upon the resulting trees. We observe that the specifics of halo finding itself greatly influences the constructed merger trees. We find that the choices made to define the halo mass are of prime importance. For instance, amongst many potential options different finders select self-bound objects or spherical regions of defined overdensity, decide whether or not to include substructures within the mass returned and vary in their initial particle selection. The impact of these decisions is seen in tree length (the period of time a particularly halo can be traced back through the simulation), branching ratio (essentially the merger rate of \subhalos) and mass evolution. We therefore conclude that the choice of the underlying halo finder is more relevant to the process of building merger trees than the tree builder itself. We also report on some built-in features of specific merger tree codes that (sometimes) help to improve the quality of the merger trees produced., Accepted in MNRAS. 15 pages, 10 figures, 1 table
- Published
- 2014
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