Spavone, M., Iodice, E., van de Ven, G., Falcón-Barroso, J., Raj, M. A., Hilker, M., Peletier, R. P., Capaccioli, M., Mieske, S., Venhola, A., Napolitano, N. R., Cantiello, M., Paolillo, M., & Schipani, P. (2020). The Fornax Deep Survey with VST. Astronomy & Astrophysics, 639, A14. https://doi.org/10.1051/0004-6361/202038015
The Fornax Deep Survey with VST : VIII. Connecting the accretion history with the cluster density
|Author:||Spavone, M.1; Iodice, E.1,2; van de Ven, G.3;|
1INAF-Astronomical Observatory of Capodimonte, Salita Moiariello 16, 80131 Naples, Italy
2European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei Muenchen, Germany
3Department of Astrophysics, University of Vienna, Tuerkenschanzstrasse 17, 1180 Vienna, Austria
4Instituto de Astrofísica de Canarias, C/Vía Láctea, s/n, 38205 La Laguna, Tenerife, Spain
5Departamento de Astrofísica, Universidad de La Laguna, 8200 La Laguna, Tenerife, Spain
6Kapteyn Astronomical Institute, University of Groningen, PO Box 72, 9700 Groningen, AV, The Netherlands
7University of Naples “Federico II”, C.U. Monte Sant’Angelo, Via Cinthia, 80126 Naples, Italy
8European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile
9Division of Astronomy, Department of Physics, University of Oulu, Oulu, Finland
10School of Physics and Astronomy, Sun Yat-sen University Zhuhai Campus, Daxue Road 2, 519082 Tangjia, Zhuhai,Guangdong, PR China
11INAF-Astronomical Abruzzo Observatory, Via Maggini, 64100 Teramo, Italy
12INFN, Sezione di Napoli, Napoli 80126, Italy
|Online Access:||PDF Full Text (PDF, 7.9 MB)|
|Persistent link:|| http://urn.fi/urn:nbn:fi-fe2020092475694
|Publish Date:|| 2020-09-24
Context: This work is based on deep multi-band (g, r, i) data from the Fornax Deep Survey with the VLT Survey Telescope (VST). We analyse the surface brightness profiles of the 19 bright early-type galaxies (ETGs; mB ≤ 15 mag) inside the virial radius of the Fornax cluster (Rvir ∼ 0.7 Mpc), in the mass range 8 × 10⁸ ≤ M* ≤ 1.2 × 10¹¹ M⊙.
Aims: The main aim of this work is to identify signatures of accretion onto galaxies by studying the presence of outer stellar haloes and to understand their nature and occurrence. Our analysis also provides a new and accurate estimate of the intra-cluster light inside the virial radius of Fornax.
Methods: We performed multi-component fits to the azimuthally averaged surface brightness profiles available for all sample galaxies. This allows us to quantify the relative weight of all components in the galaxy structure that contribute to the total light. In addition, we derived the average g − i colours in each component identified by the fit, as well as the azimuthally averaged g − i colour profiles, to correlate them with the stellar mass of each galaxy and the location inside the cluster.
Results: We find that in the most massive (10¹⁰ ≤ M ≤ 10¹¹ M⊙) and reddest ETGs the fraction of light in, probably accreted, haloes (50%–90%) is much larger than in the other galaxies. All of these are located in the high-density region of the cluster (≤0.4Rvir ∼ 0.3 Mpc), belonging to the north-south clump (NS clump). Less massive galaxies (10⁹ ≤ M ≤ 10¹⁰ M⊙) have an accreted mass fraction that is lower than 30%, have bluer colours, and reside in the low-density regions of the cluster. The colour profiles of the ETGs with the largest accreted mass fraction tend to flatten in the outskirts of the galaxy, that is beyond the transition radius from the central in situ to the ex situ accreted component. Inside the virial radius of the cluster (∼0.7 Mpc), the total luminosity of the intra-cluster light, compared with the total luminosity of all cluster members (bright galaxies and dwarfs), is about 34%.
Conclusions: Inside the Fornax cluster there is a clear correlation between the amount of accreted material in the stellar haloes of galaxies and the density of the environment in which those galaxies reside. By comparing this quantity with theoretical predictions and previous observational estimates, there is a clear indication that the driving factor for the accretion process is the total stellar mass of the galaxy, which agrees with the hierarchical accretion scenario. Massive galaxies in the NS clump, with the largest accreted mass fractions, went through pre-processing in a group environment before this group merged with the main cluster early on. At the present epoch of the Fornax assembly history, these galaxies are the major contribution to the stellar density in the core of the cluster.
Astronomy and astrophysics
|Type of Publication:||
A1 Journal article – refereed
|Field of Science:||
115 Astronomy and space science
MS andEI acknowledge financial support from the VST project (P. I. P. Schipani). Authors wish to thank ESO for thefinancial contribution given for the visitor mode runs at the ESO La Silla ParanalObservatory. EI, MAR, RP, NRN and AV acknowledge financial support fromthe European Union Horizon 2020 research and innovation programme underthe Marie Skodowska-Curie grant agreement n. 721463 to the SUNDIAL ITNnetwork. NRN acknowledges financial support from the “One hundred top talentprogram of Sun Yat-sen University” Grant N. 71000-18841229. GvdV acknowl-edges funding from the European Research Council (ERC) under the EuropeanUnion’s Horizon 2020 research and innovation programme under grant agree-ment No 724857 (Consolidator Grant ArcheoDyn). J.F-B acknowledges sup-port through the RAVET project by the grant AYA2016-77237-C3-1-P from theSpanish Ministry of Science, Innovation and Universities (MCIU) and throughthe IAC project TRACES which is partially supported through the state budget and the regional budget of the Consejería de Economía, Industria, Comercio yConocimiento of the Canary Islands Autonomous Community. AV thanks theEemil Aaltonen foundation for the financial support. GvdV acknowledges fund-ing from the European Research Council (ERC) under the European Union’sHorizon 2020 research and innovation programme under grant agreement No724857 (Consolidator Grant ArcheoDyn).
|EU Grant Number:||
(721463) SUNDIAL - SUrvey Network for Deep Imaging Analysis and Learning
© ESO 2020.