Publications by Clotilde Laigle


Galaxy-halo alignments in the Horizon-AGN cosmological hydrodynamical simulation

Monthly Notices of the Royal Astronomical Society Oxford University Press (2017)

NE Chisari, N Koukoufilippas, A Jindal, S Peirani, RS Beckmann, S Codis, JEG Devriendt, L Miller, Y Dubois, CMC Laigle, A Slyz, C Pichon

Intrinsic alignments of galaxies are a significant astrophysical systematic affecting cosmological constraints from weak gravitational lensing. Obtaining numerical predictions from hydrodynamical simulations of expected survey volumes is expensive, and a cheaper alternative relies on populating large dark matter-only simulations with accurate models of alignments calibrated on smaller hydrodynamical runs. This requires connecting the shapes and orientations of galaxies to those of dark matter halos and to the large-scale structure. In this paper, we characterise galaxy-halo alignments in the Horizon-AGN cosmological hydrodynamical simulation. We compare the shapes and orientations of galaxies in the redshift range $0


The Horizon-AGN simulation: evolution of galaxy properties over cosmic time

arXiv (2016)

S Kaviraj, C Laigle, T Kimm, J Devriendt, Y Dubois, C Pichon, A Slyz, E Chisari, S Peirani

We compare the predictions of Horizon-AGN, a hydro-dynamical cosmological simulation that uses an adaptive mesh refinement code, to observational data in the redshift range 0 < z > 6. We study the reproduction, by the simulation, of quantities that trace the aggregate stellar-mass growth of galaxies over cosmic time: luminosity and stellar-mass functions, the star formation main sequence, rest-frame UV-optical-near infrared colours and the cosmic star-formation history. We show that Horizon-AGN, which is not tuned to reproduce the local Universe, produces good overall agreement with these quantities, from the present day to the epoch when the Universe was 5% of its current age. By comparison to Horizon-noAGN, a twin simulation without AGN feedback, we quantify how feedback from black holes is likely to help shape galaxy stellar-mass growth in the redshift range 0 < z > 6, particularly in the most massive galaxies. Our results demonstrate that Horizon-AGN successfully captures the evolutionary trends of observed galaxies over the lifetime of the Universe, making it an excellent tool for studying the processes that drive galaxy evolution and making predictions for the next generation of galaxy surveys.


The clustering properties of radio-selected AGN and star-forming galaxies up to redshifts z similar to 3

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 464 (2017) 3271-3280

M Magliocchetti, P Popesso, M Brusa, M Salvato, C Laigle, HJ McCracken, O Ilbert


(Sub) millimetre interferometric imaging of a sample of COSMOS/AzTEC submillimetre galaxies IV. Physical properties derived from spectral energy distributions

ASTRONOMY & ASTROPHYSICS 597 (2017) ARTN A5

O Miettinen, I Delvecchio, V Smolcic, M Novak, M Aravena, A Karim, EJ Murphy, E Schinnerer, P Capak, O Ilbert, HT Intema, C Laigle, HJ McCracken


(Sub)millimetre interferometric imaging of a sample of COSMOS/AzTEC submillimetre galaxies

ASTRONOMY & ASTROPHYSICS 597 (2017) ARTN A4

V Smolcic, O Miettinen, N Tomicic, G Zamorani, A Finoguenov, BC Lemaux, M Aravena, P Capak, Y-K Chiang, F Civano, I Delvecchio, O Ilbert, N Jurlin, A Karim, C Laigle, O Le Fevre, S Marchesi, HJ McCracken, DA Riechers, M Salvato, E Schinnerer, L Tasca, S Toft


Redshift and luminosity evolution of the intrinsic alignments of galaxies in Horizon-AGN

Monthly Notices of the Royal Astronomical Society Oxford University Press 461 (2016) 2702-2721

N Chisari, C Laigle, S Codis, Y Dubois, J Devriendt, L Miller, K Benabed, A Slyz, R Gavazzi, C Pichon

Intrinsic galaxy shape and angular momentum alignments can arise in cosmological large-scale structure due to tidal interactions or galaxy formation processes. Cosmological hydrodynamical simulations have recently come of age as a tool to study these alignments and their contamination to weak gravitational lensing. We probe the redshift and luminosity evolution of intrinsic alignments in Horizon-AGN between z=0 and z=3 for galaxies with an r-band absolute magnitude of <-20. Alignments transition from being radial at low redshifts and high luminosities, dominated by the contribution of ellipticals, to being tangential at high redshift and low luminosities, where discs dominate the signal. This cannot be explained by the evolution of the fraction of ellipticals and discs alone: intrinsic evolution in the amplitude of alignments is necessary. The alignment amplitude of elliptical galaxies alone is smaller in amplitude by a factor of ~2, but has similar luminosity and redshift evolution as in current observations and in the nonlinear tidal alignment model at projected separations of > 1 Mpc. Alignments of discs are null in projection and consistent with current low redshift observations. The combination of the two populations yields an overall amplitude a factor of ~4 lower than observed alignments of luminous red galaxies with a steeper luminosity dependence. The restriction on accurate galaxy shapes implies that the galaxy population in the simulation is complete only to an r-band absolute magnitude of <-20. Higher resolution simulations will be necessary to avoid extrapolation of the intrinsic alignment predictions to the range of luminosities probed by future surveys.


ISM MASSES AND THE STAR FORMATION LAW AT Z = 1 TO 6 ALMA OBSERVATIONS OF DUST CONTINUUM IN 145 GALAXIES IN THE COSMOS SURVEY FIELD (vol 820, 83, 2016)

ASTROPHYSICAL JOURNAL 824 (2016) ARTN 63

N Scoville, K Sheth, H Aussel, P Vanden Bout, P Capak, A Bongiorno, CM Casey, L Murchikova, J Koda, J Alvarez-Marquez, N Lee, C Laigle, HJ McCracken, O Ilbert, A Pope, D Sanders, J Chu, S Toft, RJ Ivison, S Manohar


THE COSMOS2015 CATALOG: EXPLORING THE 1 < z < 6 UNIVERSE WITH HALF A MILLION GALAXIES

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES 224 (2016) ARTN 24

C Laigle, HJ McCracken, O Ilbert, BC Hsieh, I Davidzon, P Capak, G Hasinger, JD Silverman, C Pichon, J Coupon, H Aussel, D Le Borgne, K Caputi, P Cassata, Y-Y Chang, F Civano, J Dunlop, J Fynbo, JS Kartaltepe, A Koekemoer, O Le Fevre, E Le Floc'h, A Leauthaud, S Lilly, L Lin, S Marchesi, B Milvang-Jensen, M Salvato, DB Sanders, N Scoville, V Smolcic, M Stockmann, Y Taniguchi, L Tasca, S Toft, M Vaccari, J Zabl


REST-UV ABSORPTION LINES AS METALLICITY ESTIMATOR: THE METAL CONTENT OF STAR-FORMING GALAXIES AT z similar to 5

ASTROPHYSICAL JOURNAL 822 (2016) ARTN 29

AL Faisst, PL Capak, I Davidzon, M Salvato, C Laigle, O Ilbert, M Onodera, G Hasinger, Y Kakazu, D Masters, HJ McCracken, B Mobasher, D Sanders, JD Silverman, L Yan, NZ Scoville


A COHERENT STUDY OF EMISSION LINES FROM BROADBAND PHOTOMETRY: SPECIFIC STAR FORMATION RATES AND [O III]/H beta RATIO AT 3 < z < 6

ASTROPHYSICAL JOURNAL 821 (2016) ARTN 122

AL Faisst, P Capak, BC Hsieh, C Laigle, M Salvato, L Tasca, P Cassata, I Davidzon, O Ilbert, O Le Fevre, D Masters, HJ McCracken, C Steinhardt, JD Silverman, S de Barros, G Hasinger, NZ Scoville


ISM MASSES AND THE STAR FORMATION LAW AT Z=1 TO 6: ALMA OBSERVATIONS OF DUST CONTINUUM IN 145 GALAXIES IN THE COSMOS SURVEY FIELD

ASTROPHYSICAL JOURNAL 820 (2016) ARTN 83

N Scoville, K Sheth, H Aussel, P Vanden Bout, P Capak, A Bongiorno, CM Casey, L Murchikova, J Koda, J Alvarez-Marquez, N Lee, C Laigle, HJ McCracken, O Ilbert, A Pope, D Sanders, J Chu, S Toft, RJ Ivison, S Manohar


THE SPLASH SURVEY: QUIESCENT GALAXIES ARE MORE STRONGLY CLUSTERED BUT ARE NOT NECESSARILY LOCATED IN HIGH-DENSITY ENVIRONMENTS

ASTROPHYSICAL JOURNAL 817 (2016) ARTN 97

L Lin, PL Capak, C Laigle, O Ilbert, B-C Hsieh, H-Y Jian, BC Lemaux, JD Silverman, J Coupon, HJ McCracken, G Hasinger, O Le Fevre, N Scoville


THE CHANDRA COSMOS LEGACY SURVEY: OPTICAL/IR IDENTIFICATIONS

ASTROPHYSICAL JOURNAL 817 (2016) ARTN 34

S Marchesi, F Civano, M Elvis, M Salvato, M Brusa, A Comastri, R Gilli, G Hasinger, G Lanzuisi, T Miyaji, E Treister, CM Urry, C Vignali, G Zamorani, V Allevato, N Cappelluti, C Cardamone, A Finoguenov, RE Griffiths, A Karim, C Laigle, SM LaMassa, K Jahnke, P Ranalli, K Schawinski, E Schinnerer, JD Silverman, V Smolcic, H Suh, B Trakhtenbrot


Intrinsic alignments of galaxies in the Horizon-AGN cosmological hydrodynamical simulation

Monthly Notices of the Royal Astronomical Society Oxford University Press 454 (2015) 2736-2753

N Chisari, S Codis, C Laigle, Y Dubois, C Pichon, J Devriendt, A Slyz, L Miller, R Gavazzi, K Benabed

The intrinsic alignments of galaxies are recognised as a contaminant to weak gravitational lensing measurements. In this work, we study the alignment of galaxy shapes and spins at low redshift ($z\sim 0.5$) in Horizon-AGN, an adaptive-mesh-refinement hydrodynamical cosmological simulation box of 100 Mpc/h a side with AGN feedback implementation. We find that spheroidal galaxies in the simulation show a tendency to be aligned radially towards over-densities in the dark matter density field and other spheroidals. This trend is in agreement with observations, but the amplitude of the signal depends strongly on how shapes are measured and how galaxies are selected in the simulation. Disc galaxies show a tendency to be oriented tangentially around spheroidals in three-dimensions. While this signal seems suppressed in projection, this does not guarantee that disc alignments can be safely ignored in future weak lensing surveys. The shape alignments of luminous galaxies in Horizon-AGN are in agreement with observations and other simulation works, but we find less alignment for lower luminosity populations. We also characterize the systematics of galaxy shapes in the simulation and show that they can be safely neglected when measuring the correlation of the density field and galaxy ellipticities.


SPITZER BRIGHT, ULTRAVISTA FAINT SOURCES IN COSMOS: THE CONTRIBUTION TO THE OVERALL POPULATION OF MASSIVE GALAXIES AT z=3-7

ASTROPHYSICAL JOURNAL 810 (2015) ARTN 73

KI Caputi, O Ilbert, C Laigle, HJ McCracken, O Le Fevre, J Fynbo, B Milvang-Jensen, P Capak, M Salvato, Y Taniguchi


Can we use weak lensing to measure total mass profiles of galaxies on 20 kpc scales?

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 449 (2015) 2128-2143

MIN Kobayashi, A Leauthaud, S More, N Okabe, C Laigle, J Rhodes, TT Takeuchi


Physical properties of z > 4 submillimeter galaxies in the COSMOS field

ASTRONOMY & ASTROPHYSICS 576 (2015) ARTN A127

V Smolcic, A Karim, O Miettinen, M Novak, B Magnelli, DA Riechers, E Schinnerer, P Capak, M Bondi, P Ciliegi, M Aravena, F Bertoldi, S Bourke, J Banfield, CL Carilli, F Civano, O Ilbert, HT Intema, O Le Fevre, A Finoguenov, G Hallinan, H-R Kloeckner, A Koekemoer, C Laigle, D Masters, HJ McCracken, K Mooley, E Murphy, F Navarette, M Salvato, M Sargent, K Sheth, S Toft, G Zamorani


CFHTLenS: a weak lensing shear analysis of the 3D-Matched-Filter galaxy clusters

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 447 (2015) 1304-1318

J Ford, L Van Waerbeke, M Milkeraitis, C Laigle, H Hildebrandt, T Erben, C Heymans, H Hoekstra, T Kitching, Y Mellier, L Miller, A Choi, J Coupon, L Fu, MJ Hudson, K Kuijken, N Robertson, B Rowe, T Schrabback, M Velander


Swirling around filaments: are large-scale structure vortices spinning up dark haloes?

Monthly Notices of the Royal Astronomical Society Oxford University Press 446 (2014) 2744-2759

C Laigle, C Pichon, S Codis, Y Dubois, D Le Borgne, D Pogosyan, J Devriendt, S Peirani, S Prunet, S Rouberol, A Slyz, T Sousbie

The kinematic analysis of dark matter and hydrodynamical simulations suggests that the vorticity in large-scale structure is mostly confined to, and predominantly aligned with, their filaments, with an excess of probability of 20 per cent to have the angle between vorticity and filaments direction lower than 60° relative to random orientations. The cross-sections of these filaments are typically partitioned into four quadrantswith opposite vorticity sign, arising frommultiple flows, originating from neighbouringwalls. The spins of haloes embedded within these filaments are consistently aligned with this vorticity for any halo mass, with a stronger alignment for the most massive structures up to an excess of probability of 165 per cent. The global geometry of the flow within the cosmic web is therefore qualitatively consistent with a spin acquisition for smaller haloes induced by this large-scale coherence, as argued in Codis et al. In effect, secondary anisotropic infall (originating from the vortex-rich filament within which these lower-mass haloes form) dominates the angular momentum budget of these haloes. The transition mass from alignment to orthogonality is related to the size of a given multi-flow region with a given polarity. This transition may be reconciled with the standard tidal torque theory if the latter is augmented so as to account for the larger scale anisotropic environment of walls and filaments.


Dancing in the dark: galactic properties trace spin swings along the cosmic web

Monthly Notices of the Royal Astronomical Society Oxford University Press 444 (2014) 1453-1468

Y Dubois, C Pichon, C Welker, DL Borgne, J Devriendt, C Laigle, S Codis, D Pogosyan, S Arnouts, K Benabed, E Bertin, J Blaizot, F Bouchet, J-F Cardoso, S Colombi, VD Lapparent, V Desjacques, R Gavazzi, A Slyz, T Sousbie, R Teyssier, L Tresse, M Treyer, D Vibert, M Volonteri

<p>A large-scale hydrodynamical cosmological simulation, Horizon-AGN, is used to investigate the alignment between the spin of galaxies and the cosmic filaments above redshift 1.2. The analysis of more than 150 000 galaxies per time step in the redshift range 1.2 &lt; <em>z</em> &lt; 1.8 with morphological diversity shows that the spin of low-mass blue galaxies is preferentially aligned with their neighbouring filaments, while high-mass red galaxies tend to have a perpendicular spin. The reorientation of the spin of massive galaxies is provided by galaxy mergers, which are significant in their mass build-up. We find that the stellar mass transition from alignment to misalignment happens around 3 × 10<sup>10</sup> M<sub>⊙</sub>. Galaxies form in the vorticity-rich neighbourhood of filaments, and migrate towards the nodes of the cosmic web as they convert their orbital angular momentum into spin. The signature of this process can be traced to the properties of galaxies, as measured relative to the cosmic web. We argue that a strong source of feedback such as active galactic nuclei is mandatory to quench <em>in situ</em> star formation in massive galaxies and promote various morphologies. It allows mergers to play their key role by reducing post-merger gas inflows and, therefore, keeping spins misaligned with cosmic filaments.</p>

Pages