Publications by Clotilde Laigle

The formation and evolution of low-surface-brightness galaxies


G Martin, S Kaviraj, C Laigle, JEG Devriendt, RA Jackson, S Peirani, Y Dubois, C Pichon, A Slyz

Chandra centres for COSMOS X-ray galaxy groups: differences in stellar properties between central dominant and offset brightest group galaxies


G Gozaliasl, A Finoguenov, M Tanaka, K Dolag, F Montanari, CC Kirkpatrick, E Vardoulaki, HG Khosroshahi, M Salvato, C Laigle, HJ McCracken, O Ilbert, N Cappelluti, E Daddi, G Hasinger, P Capak, NZ Scoville, S Toft, F Civano, RE Griffiths, M Balogh, Y Li, J Ahoranta, S Mei, A Iovino, BMB Henriques, G Erfanianfar

Group quenching and galactic conformity at low redshift


M Treyer, K Kraljic, S Arnouts, S de la Torre, C Pichon, Y Dubois, D Vibert, B Milliard, C Laigle, M Seibert, MJI Brown, MW Grootes, AH Wright, J Liske, MA Lara-Lopez, J Bland-Hawthorn

SPLASH-SXDF multi-wavelength photometric catalog

Astrophysical Journal Supplement Series American Astronomical Society 235 (2018) 36

V Mehta, C Scarlata, P Capak, I Davidzon, A Faisst, BC Hsieh, O Ilbert, M Jarvis, CLOTILDE Laigle, J Phillips, J Silverman, MA Strauss, M Tanaka, R Bowler, J Coupon, S Foucaud, S Hemmati, D Masters, HJ McCracken, B Mobasher, M Ouchi, T Shibuya, W-H Wang

We present a multi-wavelength catalog in the Subaru/XMM-Newton Deep Field (SXDF) as part of the Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH). We include the newly acquired optical data from the Hyper-Suprime-Cam Subaru Strategic Program, accompanied by IRAC coverage from the SPLASH survey. All available optical and near-infrared data is homogenized and resampled on a common astrometric reference frame. Source detection is done using a multi-wavelength detection image including the u-band to recover the bluest objects. We measure multi-wavelength photometry and compute photometric redshifts as well as physical properties for ~1.17 million objects over ~4.2 deg2, with ~800,000 objects in the 2.4 deg2 HSC-Ultra-Deep coverage. Using the available spectroscopic redshifts from various surveys over the range of 0 < z < 6, we verify the performance of the photometric redshifts and we find a normalized median absolute deviation of 0.023 and outlier fraction of 3.2%. The SPLASH-SXDF catalog is a valuable, publicly available resource, perfectly suited for studying galaxies in the early universe and tracing their evolution through cosmic time.

Identifying the progenitors of present-day early-type galaxies in observational surveys: Correcting 'progenitor bias' using the Horizon-AGN simulation

Monthly Notices of the Royal Astronomical Society Oxford University Press 474 (2017) 3140-3151

G Martin, S Kaviraj, J Devriendt, Y Dubois, C Pichon, C Laigle

As endpoints of the hierarchical mass-assembly process, the stellar populations of local earlytype galaxies encode the assembly history of galaxies over cosmic time. We useHorizon-AGN, a cosmological hydrodynamical simulation, to study the merger histories of local early-type galaxies and track how the morphological mix of their progenitors evolves over time. We provide a framework for alleviating 'progenitor bias' - the bias that occurs if one uses only early-type galaxies to study the progenitor population. Early types attain their final morphology at relatively early epochs - by z ~ 1, around 60 per cent of today's early types have had their last significant merger. At all redshifts, the majority of mergers have one late-type progenitor, with late-late mergers dominating at z > 1.5 and early-early mergers becoming significant only at z < 0.5. Progenitor bias is severe at all but the lowest redshifts - e.g. at z~0.6, less than 50 per cent of the stellar mass in today's early types is actually in progenitors with early-type morphology, while, at z~ 2, studying only early types misses almost all (80 per cent) of the stellar mass that eventually ends up in local early-type systems. At high redshift, almost all massive late-type galaxies, regardless of their local environment or star formation rate, are progenitors of local early-type galaxies, as are lowermass (M* < 10 10.5 M ⊙ ) late-types as long as they reside in high-density environments. In this new era of large observational surveys (e.g. LSST, JWST), this study provides a framework for studying how today's early-type galaxies have been built up over cosmic time.

Galaxy evolution in the metric of the Cosmic Web

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

K Kraljic, S Arnouts, C Pichon, CMC Laigle, S de la Torre, D Vibert, C Cadiou, Y Dubois, M Treyer, C Schimd, S Codis, V de Lapparent, J Devriendt, HS Hwang, D Le Borgne, N Malavasi, B Milliard, M Musso, D Pogosyan, M Alpaslan, J Bland-Hawthorn, AH Wright

The role of the cosmic web in shaping galaxy properties is investigated in the GAMA spectroscopic survey in the redshift range $0.03 \leq z \leq 0.25$. The stellar mass, $u - r$ dust corrected colour and specific star formation rate (sSFR) of galaxies are analysed as a function of their distances to the 3D cosmic web features, such as nodes, filaments and walls, as reconstructed by DisPerSE. Significant mass and type/colour gradients are found for the whole population, with more massive and/or passive galaxies being located closer to the filament and wall than their less massive and/or star-forming counterparts. Mass segregation persists among the star-forming population alone. The red fraction of galaxies increases when closing in on nodes, and on filaments regardless of the distance to nodes. Similarly, the star-forming population reddens (or lowers its sSFR) at fixed mass when closing in on filament, implying that some quenching takes place. Comparable trends are also found in the state-of-the-art hydrodynamical simulation Horizon-AGN. These results suggest that on top of stellar mass and large-scale density, the traceless component of the tides from the anisotropic large-scale environment also shapes galactic properties. An extension of excursion theory accounting for filamentary tides provides a qualitative explanation in terms of anisotropic assembly bias: at a given mass, the accretion rate varies with the orientation and distance to filaments. It also explains the absence of type/colour gradients in the data on smaller, non-linear scales.

A question of separation: disentangling tracer bias and gravitational non-linearity with counts-in-cells statistics


C Uhlemann, M Feix, S Codis, C Pichon, F Bernardeau, B L'Huillier, J Kim, SE Hong, C Laigle, C Park, J Shin, D Pogosyan

Cosmic evolution of stellar quenching by AGN feedback: clues from the Horizon-AGN simulation

Monthly Notices of the Royal Astronomical Society Oxford University Press 472 (2017) 949-965

RS Beckmann, J Devriendt, AD Slyz, S Peirani, MLA Richardson, Y Dubois, C Pichon, NE Chisari, S Kaviraj, CMC Laigle, M Volonteri

The observed massive end of the local galaxy stellar mass function is steeper than its predicted dark matter (DM) halo counterpart in the standard $\Lambda $CDM paradigm. We investigate how active galactic nuclei (AGN) feedback can account for such a reduction in the stellar content of massive galaxies, through an influence on the gas content of their interstellar (ISM) and circum-galactic medium (CGM). We isolate the impact of AGNs by comparing two simulations from the HORIZON suite, which are identical except that one includes super massive black holes (SMBH) and related feedback. This allows us to cross-identify individual galaxies between these simulations and quantify the effect of AGN feedback on their properties, such as stellar mass and gas outflows. We find that the most massive galaxies ($ \rm M_{*} \geq 3 \times 10^{11} M_\odot $) are quenched to the extent that their stellar masses decrease by about 80% at $z=0$. More generally, SMBHs affect their host halo through a combination of outflows that reduce their baryonic mass, particularly for galaxies in the mass range $ \rm 10^9 M_\odot \leq M_{*} \leq 10^{11} M_\odot $, and a disruption of central gas inflows, which limits in-situ star formation, particularly massive galaxies with $ \rm M_{*} \approx10^{11} M_\odot $. As a result of these processes, net gas inflows onto massive galaxies drop by up to 70%. Finally, we measure a redshift evolution in the stellar mass ratio of twin galaxies with and without AGN feedback, with galaxies of a given stellar mass showing stronger signs of quenching earlier on. This evolution is driven by a progressive flattening of the $\rm M_{SMBH}-M_* $ relation for galaxies with $\rm M_{*} \leq 10^{10} M_\odot $ as redshift decreases, which translates into smaller SBMHs being harboured by galaxies of any fixed stellar mass, and indicates stronger AGN feedback at higher redshift.

The limited role of galaxy mergers in driving stellar mass growth over cosmic time

Monthly Notices of the Royal Astronomical Society Letters Oxford University Press 472 (2017) L50-L54

G Martin, S Kaviraj, JEG Devriendt, Y Dubois, CMC Laigle, C Pichon

A key unresolved question is the role that galaxy mergers play in driving stellar mass growth over cosmic time. Recent observational work hints at the possibility that the overall contribution of `major' mergers (mass ratios $\gtrsim$1:4) to cosmic stellar mass growth may be small, because they enhance star formation rates by relatively small amounts at high redshift, when much of today's stellar mass was assembled. However, the heterogeneity and relatively small size of today's datasets, coupled with the difficulty in identifying genuine mergers, makes it challenging to $\textit{empirically}$ quantify the merger contribution to stellar mass growth. Here, we use Horizon-AGN, a cosmological hydrodynamical simulation, to comprehensively quantify the contribution of mergers to the star formation budget over the lifetime of the Universe. We show that: (1) both major and minor mergers enhance star formation to similar amounts, (2) the fraction of star formation directly attributable to merging is small at all redshifts (e.g. $\sim$35 and $\sim$20 per cent at z$\sim$3 and z$\sim$1 respectively) and (3) only $\sim$25 per cent of today's stellar mass is directly attributable to galaxy mergers over cosmic time. Our results suggest that smooth accretion, not merging, is the dominant driver of stellar mass growth over the lifetime of the Universe.

The COSMOS2015 galaxy stellar mass function Thirteen billion years of stellar mass assembly in ten snapshots


I Davidzon, O Ilbert, C Laigle, J Coupon, HJ McCracken, I Delvecchio, D Masters, P Capak, BC Hsieh, O Le Fevre, L Tresse, M Bethermin, Y-Y Chang, AL Faisst, E Le Floc'h, C Steinhardt, S Toft, H Aussel, C Dubois, G Hasinger, M Salvato, DB Sanders, N Scoville, JD Silverman

The VLA-COSMOS 3 GHz Large Project: Multiwavelength counterparts and the composition of the faint radio population


V Smolcic, I Delvecchio, G Zamorani, N Baran, M Novak, J Delhaize, E Schinnerer, S Berta, M Bondi, P Ciliegi, P Capak, F Civano, A Karim, O Le Fevre, O Ilbert, C Laigle, S Marchesi, HJ McCracken, L Tasca, M Salvato, E Vardoulaki

The VLA-COSMOS 3 GHz Large Project: The infrared-radio correlation of star- forming galaxies and AGN to z less than or similar to 6


J Delhaize, V Smolcic, I Delvecchio, M Novak, M Sargent, N Baran, B Magnelli, G Zamorani, E Schinnerer, EJ Murphy, M Aravena, S Berta, M Bondi, P Capak, C Carilli, P Ciliegi, F Civano, O Ilbert, A Karim, C Laigle, O Le Fevre, S Marchesi, HJ McCracken, M Salvato, N Seymour, L Tasca

The VLA-COSMOS 3 GHz Large Project: Cosmic star formation history since z similar to 5


M Novak, V Smolcic, J Delhaize, I Delvecchio, G Zamorani, N Baran, M Bondi, P Capak, CL Carilli, P Ciliegi, F Civano, O Ilbert, A Karim, C Laigle, O Le Fevre, S Marchesi, H McCracken, O Miettinen, M Salvato, M Sargent, E Schinnerer, L Tasca

The VLA-COSMOS 3 GHz Large Project: AGN and host-galaxy properties out to z less than or similar to 6


I Delvecchio, V Smolcic, G Zamorani, CDP Lagos, S Berta, J Delhaize, N Baran, DM Alexander, DJ Rosario, V Gonzalez-Perez, O Ilbert, CG Lacey, O Le Fevre, O Miettinen, M Aravena, M Bondi, C Carilli, P Ciliegi, K Mooley, M Novak, E Schinnerer, P Capak, F Civano, N Fanidakis, NH Ruiz, A Karim, C Laigle, S Marchesi, HJ McCracken, E Middleberg, M Salvato, L Tasca

The VLA-COSMOS 3 GHz Large Project: Continuum data and source catalog release


V Smolcic, M Novak, M Bondi, P Ciliegi, KP Mooley, E Schinnerer, G Zamorani, F Navarrete, S Bourke, A Karim, E Vardoulaki, S Leslie, J Delhaize, CL Carilli, ST Myers, N Baran, I Delvecchio, O Miettinen, J Banfield, M Balokovic, F Bertoldi, P Capak, DA Frail, G Hallinan, H Hao, NH Ruiz, A Horesh, O Ilbert, H Intema, V Jelic, H-R Kloeckner, J Krpan, SR Kulkarni, H McCracken, C Laigle, E Middleberg, EJ Murphy, M Sargent, NZ Scoville, K Sheth

An ALMA survey of submillimetre galaxies in the COSMOS field: The extent of the radio-emitting region revealed by 3 GHz imaging with the Very Large Array


O Miettinen, M Novak, V Smolcic, I Delvecchio, M Aravena, D Brisbin, A Karim, EJ Murphy, E Schinnerer, M Albrecht, H Aussel, F Bertoldi, PL Capak, CM Casey, F Civano, CC Hayward, NH Ruiz, O Ilbert, C Jiang, C Laigle, O Le Fevre, B Magnelli, S Marchesi, HJ McCracken, E Middelberg, AM Munoz Arancibia, F Navarrete, ND Padilla, DA Riechers, M Salvato, KS Scott, K Sheth, LAM Tasca, M Bondi, G Zamorani

Type 2 AGN Host Galaxies in the Chandra-COSMOS Legacy Survey: No Evidence of AGN-driven Quenching


H Suh, F Civano, G Hasinger, E Lusso, G Lanzuisi, S Marchesi, B Trakhtenbrot, V Allevato, N Cappelluti, PL Capak, M Elvis, RE Griffiths, C Laigle, P Lira, L Riguccini, DJ Rosario, M Salvato, K Schawinski, C Vignali

Obscured active galactic nuclei triggered in compact star-forming galaxies


Y-Y Chang, E Le Floc'h, S Juneau, E da Cunha, M Salvato, F Civano, S Marchesi, JM Gabor, O Ilbert, C Laigle, HJ McCracken, B-C Hsieh, P Capak

Evolution of Interstellar Medium, Star Formation, and Accretion at High Redshift


N Scoville, N Lee, PV Bout, T Diaz-Santos, D Sanders, B Darvish, A Bongiorno, CM Casey, L Murchikova, J Koda, P Capak, C Vlahakis, O Ilbert, K Sheth, K Morokuma-Matsui, RJ Ivison, H Aussel, C Laigle, HJ McCracken, L Armus, A Pope, S Toft, D Masters

The VIMOS Public Extragalactic Redshift Survey (VIPERS): galaxy segregation inside filaments at z similar or equal to 0.7


N Malavasi, S Arnouts, D Vibert, S de la Torre, T Moutard, C Pichon, I Davidzon, K Kraljic, M Bolzonella, L Guzzo, B Garilli, M Scodeggio, BR Granett, U Abbas, C Adami, D Bottini, A Cappi, O Cucciati, P Franzetti, A Fritz, A Iovino, J Krywult, V Le Brun, O Le Fevre, D Maccagni, K Malek, F Marulli, M Polletta, A Pollo, L Tasca, R Tojeiro, D Vergani, A Zanichelli, J Bel, E Branchini, J Coupon, G De Lucia, Y Dubois, A Hawken, O Ilbert, C Laigle, L Moscardini, T Sousbie, M Treyer, G Zamorani