publications
• A complete list of my publications over Astrophysics can be found here at NASA ADS.
• Below is a selected list of publications in reversed chronological order generated by jekyll-scholar.
2024
- arXivEPOCHS Paper X: Environmental effects on Galaxy Formation and Protocluster Galaxy candidates at 4.5<z<10 from JWST observationsQiong Li , Christopher J. Conselice, Florian Sarron, and 16 more authorsarXiv e-prints, May 2024
In this paper we describe our search for galaxy protocluster candidates at 4.5< z < 10 and explore the environmental and physical properties of their member galaxies identified through JWST wide-field surveys within the CEERS, JADES, and PEARLS NEP-TDF fields. Combining with HST data, we identify 2948 robust z>4.5 candidates within an area of 185.4 arcmin^2. We determine nearest neighbour statistics and galaxy environments. We find that high-z galaxies in overdense environments exhibit higher star formation activity compared to those in underdense regions. Galaxies in dense environments have a slightly increased SFR at a given mass compared with galaxies in the lower density environments. At the high mass end we also find a gradual flattening of the M_⋆-SFR slope. We find that galaxies in high-density regions often have redder UV slopes than those in low-density regions, suggesting more dust extinction, weaker Lyman-alpha emission and / or a higher damped Lyman-alpha absorption. We also find that the mass-size relation remains consistent and statistically similar across all environments. Furthermore, we quantitatively assess the probability of a galaxy belonging to a protocluster candidate. In total, we identified 26 overdensities at z=5-7 and estimate their dark matter halo masses. We find that all protocluster candidates could evolve into clusters with M_\rm halo > 10^14M_⊙ at z = 0, thereby supporting the theoretical and simulation predictions of cluster formation. Notably, this marks an early search for protocluster candidates in JWST wide field based on photometric data, providing valuable candidates to study cosmic structure formation at the early stages.
@article{Li2024, author = {{Li}, Qiong and {Conselice}, Christopher J. and {Sarron}, Florian and {Harvey}, Tom and {Austin}, Duncan and {Adams}, Nathan and {Trussler}, James A.~A. and {Duan}, Qiao and {Ferreira}, Leonardo and {Westcott}, Lewi and {Harris}, Honor and {Dole}, Herv{\'e} and {Grogin}, Norman A. and {Frye}, Brenda and {Koekemoer}, Anton M. and {Robertson}, Clayton and {Windhorst}, Rogier A. and {Polletta}, Maria del Carmen and {Hathi}, Nimish P.}, title = {{EPOCHS Paper X: Environmental effects on Galaxy Formation and Protocluster Galaxy candidates at $4.5<z<10$ from JWST observations}}, journal = {arXiv e-prints}, keywords = {Astrophysics - Astrophysics of Galaxies}, year = {2024}, month = may, eid = {arXiv:2405.17359}, pages = {arXiv:2405.17359}, doi = {10.48550/arXiv.2405.17359}, archiveprefix = {arXiv}, primaryclass = {astro-ph.GA}, adsurl = {https://ui.adsabs.harvard.edu/abs/2024arXiv240517359L}, adsnote = {Provided by the SAO/NASA Astrophysics Data System}, }
2023
- MNRASWhen the well runs dry: modelling environmental quenching of high-mass satellites in massive clusters at z \ensuremath≳ 1Devontae C. Baxter , M. C. Cooper , Michael L. Balogh , and 11 more authorsMonthly Notices of the Royal Astronomical Society, Dec 2023
We explore models of massive (>10^10 M_\ensuremath⊙) satellite quenching in massive clusters at z \ensuremath≳ 1 using an MCMC framework, focusing on two primary parameters: R_quench (the host-centric radius at which quenching begins) and \ensuremathτ_quench (the time-scale upon which a satellite quenches after crossing R_quench). Our MCMC analysis shows two local maxima in the 1D posterior probability distribution of R_quench at approximately 0.25 and 1.0 R_200. Analysing four distinct solutions in the \ensuremathτ_quench-R_quench parameter space, nearly all of which yield quiescent fractions consistent with observational data from the GOGREEN survey, we investigate whether these solutions represent distinct quenching pathways and find that they can be separated between ’starvation’ and ’core quenching’ scenarios. The starvation pathway is characterized by quenching time-scales that are roughly consistent with the total cold gas (H_2 + H I) depletion time-scale at intermediate z, while core quenching is characterized by satellites with relatively high line-of-sight velocities that quench on short time-scales (\raisebox-0.5ex\textasciitilde0.25 Gyr) after reaching the inner region of the cluster (<0.30 R_200). Lastly, we break the degeneracy between these solutions by comparing the observed properties of transition galaxies from the GOGREEN survey. We conclude that only the ’starvation’ pathway is consistent with the projected phase-space distribution and relative abundance of transition galaxies at z \raisebox-0.5ex~1. However, we acknowledge that ram pressure might contribute as a secondary quenching mechanism.
@article{Baxter2023, author = {{Baxter}, Devontae C. and {Cooper}, M.~C. and {Balogh}, Michael L. and {Rudnick}, Gregory H. and {De Lucia}, Gabriella and {Demarco}, Ricardo and {Finoguenov}, Alexis and {Forrest}, Ben and {Muzzin}, Adam and {Reeves}, Andrew M.~M. and {Sarron}, Florian and {Vulcani}, Benedetta and {Wilson}, Gillian and {Zaritsky}, Dennis}, title = {{When the well runs dry: modelling environmental quenching of high-mass satellites in massive clusters at z {\ensuremath{\gtrsim}} 1}}, journal = {Monthly Notices of the Royal Astronomical Society}, keywords = {galaxies: clusters: general, galaxies: evolution, galaxies: general, galaxies: high-redshift, galaxies: star formation, Astrophysics - Astrophysics of Galaxies}, year = {2023}, month = dec, volume = {526}, number = {3}, pages = {3716-3729}, doi = {10.1093/mnras/stad2995}, archiveprefix = {arXiv}, primaryclass = {astro-ph.GA}, adsurl = {https://ui.adsabs.harvard.edu/abs/2023MNRAS.526.3716B}, adsnote = {Provided by the SAO/NASA Astrophysics Data System}, }
2022
- A&APhysical properties of more than one thousand brightest cluster galaxies detected in the Canada-France-Hawaii Telescope Legacy SurveyA. Chu , F. Sarron , F. Durret , and 1 more authorAstronomy and Astrophysics, Oct 2022
Context. Brightest cluster galaxies (BCGs) are very massive elliptical galaxies found at the centres of clusters. Their study gives clues to the formation and evolution of the clusters in which they are embedded. \Aims: We analyse here in a homogeneous way the properties of a sample of more than 1000 BCGs in the redshift range 0.15 < z < 0.7, based on images from the Canada-France-Hawaii Telescope Legacy Survey. \Methods: Based on a recent catalogue of 1371 clusters, we applied our automatic BCG detection algorithm and successfully identified 70% of the BCGs in our sample. We analysed their 2D photometric properties with GALFIT. We also compared the position angles of the BCG major axes with those of the overall cluster to which they belong. \Results: We find no evolution of the BCG properties with redshift up to z = 0.7, in agreement with previous results by Chu et al. (2021, A&A, 649, A42), who analysed a sample an order of magnitude smaller, but reaching a redshift z = 1.8. The Kormendy relation for BCGs is tight and consistent with that of normal elliptical galaxies and BCGs measured by other authors. The position angles of the BCGs and of the cluster to which they belong agree within 30 degrees for 55% of the objects with well-defined position angles. \Conclusions: The study of this very large sample of more than 1000 BCGs shows that they were mainly formed before z = 0.7 as we find no significant growth for the luminosities and sizes of central galaxies. We discuss the importance of the intracluster light in the interpretation of these results. We highlight the role of image depth in the modelling of the luminosity profiles of BCGs, and give evidence of the presence of an inner structure which can only be resolved on deep surveys with limiting apparent magnitude at 80% completeness m_80 > 26 mag arcsec^\ensuremath-2.
@article{Chu2022, author = {{Chu}, A. and {Sarron}, F. and {Durret}, F. and {M{\'a}rquez}, I.}, title = {{Physical properties of more than one thousand brightest cluster galaxies detected in the Canada-France-Hawaii Telescope Legacy Survey}}, journal = {Astronomy and Astrophysics}, keywords = {galaxies: clusters: general, galaxies: evolution, galaxies: formation, Astrophysics - Astrophysics of Galaxies}, year = {2022}, month = oct, volume = {666}, eid = {A54}, pages = {A54}, doi = {10.1051/0004-6361/202243504}, archiveprefix = {arXiv}, primaryclass = {astro-ph.GA}, adsurl = {https://ui.adsabs.harvard.edu/abs/2022A&A...666A..54C}, adsnote = {Provided by the SAO/NASA Astrophysics Data System}, }
2021
- MNRASDETECTIFz galaxy groups in the REFINE survey - I. Group detection and quenched fraction evolution at z < 2.5Florian Sarron, and Christopher J. ConseliceMonthly Notices of the Royal Astronomical Society, Sep 2021
We use a large K-selected sample of 299 961 galaxies from the REFINE survey, consisting of a combination of data from three of the deepest near-infrared surveys, UKIDSS UDS, COSMOS/UltraVISTA, and CFHTLS-D1/VIDEO, that were homogeneously reduced to obtain photometric redshifts and stellar masses. We detect 2588 candidate galaxy groups up to z = 3.15 at S/N > 1.5. We build a very pure ( 90\rm per cent) sample of 448 candidate groups up to z = 2.5 and study some of their properties. Cluster detection is done using the DElaunay TEssellation ClusTer IdentiFication with photo-z (DETECTIFz) algorithm that we describe. This new group finder algorithm uses the joint probability distribution functions of redshift and stellar-mass of galaxies to detect groups as stellar-mass overdensities in overlapping redshift slices, where density is traced using Monte Carlo realization of the Delaunay Tessellation Field Estimator. We compute the algorithm selection function using mock galaxy catalogues taken from cosmological N-body simulation lightcones. Based on these simulations, we reach a completeness of ∼\! 80\,\rm per cent for clusters (M_200 > 10^14M_\ensuremath⊙) at a purity of ∼\! 90 \rm per cent at z < 2.5. Using our 403 most massive candidate groups, we constrain the redshift evolution of the group galaxy quenched fraction at 0.12 \ensuremath≤ z < 2.32, for galaxies with 10.25 < log M_\ensuremath⋆/M_\ensuremath⊙ < 11 in 0.5 \texttimes R_200. We find that the quenched fraction in group cores is higher than in the field in the full redshift range considered, the difference growing with decreasing redshift. This indicates either more efficient quenching mechanisms in group cores at lower redshift or pre-processing by cosmic filaments.
@article{Sarron2021, author = {{Sarron}, Florian and {Conselice}, Christopher J.}, title = {{DETECTIFz galaxy groups in the REFINE survey - I. Group detection and quenched fraction evolution at z < 2.5}}, journal = {Monthly Notices of the Royal Astronomical Society}, keywords = {galaxies: clusters: general, galaxies: evolution, galaxies: groups: general, galaxies: star formation, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics}, year = {2021}, month = sep, volume = {506}, number = {2}, pages = {2136-2155}, doi = {10.1093/mnras/stab1844}, archiveprefix = {arXiv}, primaryclass = {astro-ph.GA}, adsurl = {https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2136S}, adsnote = {Provided by the SAO/NASA Astrophysics Data System}, }
2020
- A&ACandidate fossil groups in the CFHTLS: a probabilistic approachC. Adami , F. Sarron , N. Martinet , and 1 more authorAstronomy and Astrophysics, Jul 2020
@article{Adami2020, author = {{Adami}, C. and {Sarron}, F. and {Martinet}, N. and {Durret}, F.}, title = {{Candidate fossil groups in the CFHTLS: a probabilistic approach}}, journal = {Astronomy and Astrophysics}, keywords = {galaxies: clusters: general, X-rays: galaxies: clusters, large-scale structure of Universe, galaxies: groups: general, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics}, year = {2020}, month = jul, volume = {639}, eid = {A97}, pages = {A97}, doi = {10.1051/0004-6361/201936289}, archiveprefix = {arXiv}, primaryclass = {astro-ph.GA}, adsurl = {https://ui.adsabs.harvard.edu/abs/2020A&A...639A..97A}, adsnote = {Provided by the SAO/NASA Astrophysics Data System}, }
2019
- A&APre-processing of galaxies in cosmic filaments around AMASCFI clusters in the CFHTLSFlorian Sarron, C. Adami , F. Durret , and 1 more authorAstronomy and Astrophysics, Dec 2019
Context. Galaxy clusters and groups are thought to accrete material along the preferred direction of cosmic filaments. These structures have proven difficult to detect because their contrast is low, however, and only a few studies have focused on cluster infall regions. \Aims: We detect cosmic filaments around galaxy clusters using photometric redshifts in the range 0.15 < z < 0.7. We characterise galaxy populations in these structures to study the influence of pre-processing by cosmic filaments and galaxy groups on star formation quenching. \Methods: We detected cosmic filaments in the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) T0007 data, focusing on regions around clusters of the AMASCFI CFHTLS cluster sample. The filaments were reconstructed with the discrete persistent structure extractor (DISPERSE) algorithm in photometric redshift slices. We show that this reconstruction is reliable for a CFHTLS-like survey at 0.15 < z < 0.7 using a mock galaxy catalogue. We split our galaxy catalogue into two populations (passive and star forming) using the LePhare spectral energy density fitting algorithm and worked with two redshift bins (0.15 < z \ensuremath≤ 0.4 and 0.4 < z < 0.7). \Results: We showed that the AMASCFI cluster connectivity (i.e. the number of filaments that is connected to a cluster) increases with cluster mass M_200. Filament galaxies outside R_200 are found to be closer to clusters at low redshift, regardless of the galaxy type. Passive galaxies in filaments are closer to clusters than star-forming galaxies in the low redshift bin alone. The passive fraction of galaxies decreases with increasing clustercentric distance up to d \ensuremath∼ 5 cMpc. Galaxy groups and clusters that are not located at nodes of our reconstruction are mainly found inside cosmic filaments. \Conclusions: These results give clues for pre-processing in cosmic filaments that could be due to smaller galaxy groups. This trend could be further explored by applying this method to larger photometric surveys such as the Hyper Suprime-Cam Subaru Strategic Program (HSC-SPP) or Euclid.
@article{Sarron2019, author = {{Sarron}, Florian and {Adami}, C. and {Durret}, F. and {Laigle}, C.}, title = {{Pre-processing of galaxies in cosmic filaments around AMASCFI clusters in the CFHTLS}}, journal = {Astronomy and Astrophysics}, keywords = {galaxies: clusters: general, large-scale structure of Universe, galaxies: evolution, galaxies: statistics, methods: data analysis, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics}, year = {2019}, month = dec, volume = {632}, eid = {A49}, pages = {A49}, doi = {10.1051/0004-6361/201935394}, archiveprefix = {arXiv}, primaryclass = {astro-ph.GA}, adsurl = {https://ui.adsabs.harvard.edu/abs/2019A&A...632A..49S}, adsnote = {Provided by the SAO/NASA Astrophysics Data System}, }
2018
- A&AEvolution of the cluster optical galaxy luminosity function in the CFHTLS: breaking the degeneracy between mass and redshiftFlorian Sarron, N. Martinet , F. Durret , and 1 more authorAstronomy and Astrophysics, May 2018
Obtaining large samples of galaxy clusters is important for cosmology: cluster counts as a function of redshift and mass can constrain the parameters of our Universe. They are also useful in order to understand the formation and evolution of clusters. We develop an improved version of the Adami & MAzure Cluster FInder (AMACFI), now the Adami, MAzure & Sarron Cluster FInder (AMASCFI), and apply it to the 154 deg^2 of the Canada- France-Hawaii Telescope Legacy Survey (CFHTLS) to obtain a large catalogue of 1371 cluster candidates with mass M_200 > 10^14 M_\ensuremath⊙ and redshift z \ensuremath≤ 0.7. We derive the selection function of the algorithm from the Millennium simulation, and cluster masses from a richness-mass scaling relation built from matching our candidates with X-ray detections. We study the evolution of these clusters with mass and redshift by computing the i’-band galaxy luminosity functions (GLFs) for the early-type (ETGs) and late-type galaxies (LTGs). This sample is 90% pure and 70% complete, and therefore our results are representative of a large fraction of the cluster population in these redshift and mass ranges. We find an increase in both the ETG and LTG faint populations with decreasing redshift (with Schechter slopes \ensuremathα_ETG = -0.65 \ensuremath\pm 0.03 and \ensuremathα_LTG = -0.95 \ensuremath\pm 0.04 at z = 0.6, and \ensuremathα_ETG = -0.79 \ensuremath\pm 0.02 and \ensuremathα_LTG = -1.26 \ensuremath\pm 0.03 at z = 0.2) and also a decrease in the LTG (but not the ETG) bright end. Our large sample allows us to break the degeneracy between mass and redshift, finding that the redshift evolution is more pronounced in high-mass clusters, but that there is no significant dependence of the faint end on mass for a given redshift. These results show that the cluster red sequence is mainly formed at redshift z > 0.7, and that faint ETGs continue to enrich the red sequence through quenching of brighter LTGs at z \ensuremath≤ 0.7. The efficiency of this quenching is higher in large-mass clusters, while the accretion rate of faint LTGs is lower as the more massive clusters have already emptied most of their environment at higher redshifts. \\textbackslashBased on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at Terapix available at the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. \\textbackslashThe candidate cluster catalog is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/613/A67
@article{Sarron2018, author = {{Sarron}, Florian and {Martinet}, N. and {Durret}, F. and {Adami}, C.}, title = {{Evolution of the cluster optical galaxy luminosity function in the CFHTLS: breaking the degeneracy between mass and redshift}}, journal = {Astronomy and Astrophysics}, keywords = {galaxies: clusters: general, galaxies: evolution, galaxies: luminosity function, mass function, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics}, year = {2018}, month = may, volume = {613}, eid = {A67}, pages = {A67}, doi = {10.1051/0004-6361/201731981}, archiveprefix = {arXiv}, primaryclass = {astro-ph.GA}, adsurl = {https://ui.adsabs.harvard.edu/abs/2018A&A...613A..67S}, adsnote = {Provided by the SAO/NASA Astrophysics Data System}, }