Gas Life cYcle around galaxies : oRIgin and state of Cold accretion Streams – LYRICS

Our work implies the use of state-of-the-art telescopes and receivers, among the most competitive ones worldwide (ie ALMA, VLT/MUSE). Incoming datasets are huge and high quality. They bring new and unexpected results. An important infrastructure has been set up (computation, storage) in order to deal with the data but also to produce and treat the large outputs coming from our numerical simulations and modelling codes.

- Large dataset treatment
- Production of numerous modelling output grids
- Improvement and run of RAMSES (Hydro-code) on super-computers

We usually work in small teams of 2-3 people on dedicated issues. We have regular (weekly) meetings with all the team member to discuss all together progress and new issues.
We try to keep the balance between substantial new achievements and efficient communication of the results via publications.

WP1 : Calibration of all the new ALMA data (3 sources). Extraction from the ALMA archive of 13 new sources. All these galaxies harbor molecular filaments, more or less extended. The analysis, the comparison with complementary data (MUSE for the ionised gas) and the interpretation are finished and published (Olivares et al., 2019).
WP2 : We have produced many new grids of model with CLOUDY in order to reproduce typical excitation conditions of the filaments. We managed to reproduce the state-of-the-art results as found in the literature. All the grids have been produced for tow dominant processes (i) X-rays and (ii) Cosmic Rays. Two publications are in preparation (Polles et al. a,b).
WP3 We have implemented new features in RAMSES : (i) Cosmic Rays diffusion and acceleration (ii) dust evolution (iii) stabilisation of the Black Hole (iv) re-distribution of high-resolution cells. The code is ready; The first results have been published (Beckmann et al. 2019) and discuss the filament formation via thermal instabilities.

WP1 : After the analysis of ALMA and MUSE data of the molecular filaments around BCGs (article in prep), we now focus on brigthest Group galaxies (less massive galaxies). We have finished the MUSE data reduction. The scientific analysis is on-going. We have also proposed new and complementary observations on some dedicated sources.
WP2 : The publication of the results of the new grids of models is on-going. We then plan to propose a scenario that combines several gas phases. Once this work done, we will compare those results with the predictions of shock models. These grids are ready. All thoses grids will help identify the key (discriminant) tracers to disentangle the dominant excitation mechanisms. This is a key for future observing strategies, in particular for JWST (see WP1).
WP3 : The next step will be to test more extensively (in the current simulation) the impact of some key parameters on the gas cooling and on the SFR. We also prepared a new set of simulations that include the magnetic field, the anisotropic conduction and the cosmic rays. We aim at measuring the impact of these new ingredients in the simulation vs the original one.

Beckmann, R. S. et al., 2019 2019arXiv190901329B
Olivares et al., 20192019arXiv190209164O
Hamer et al., 2019, 2019MNRAS.483.4984H
Dubois, Y. et al., 2019, 2019arXiv190704300D
Godard, B. Et al., 2019, 2019A&A...622A.100G
Russel et al., 2019, 2019arXiv190209227R
Salome, Q. et al., 2019, 2019A&A...627A...6S
Castignani et al., 2019, 2019A&A...623A..48C
Rose, T. et al., 2019, 2019MNRAS.489..349R
Rose, T. et al., 2019 2019MNRAS.485..229R
Vantyghem et al., 2019, 2019ApJ...870...57V
Beckmann et al., 2018, 2018MNRAS.478..995B
Castignani et al., 2018, 2018A&A...617A.103C
O’Sullivan et al., 2018, 2018A&A...618A.126O
Tremblay et al., 2018, 2018ApJ...863..193V
Tremblay et al., 2018, 2018ApJ...865...13T
Pulido et al., 2018, 2018ApJ...853..177P
Vantyghem et al., 2017, 2017ApJ...848..101V
Russell et al., 2017, 2017MNRAS.472.4024R
Salome, Q. et al., 2017, 2017A&A...608A..98S

Galaxies grow in mass by accreting matter flowing along streams and filaments of the cosmic web. But they would become too massive, if there was not a super-massive black hole in their nucleus to inject energy and matter back into the intergalactic medium. The details of such a feedback mechanism are however still mysterious. Giant galaxies in cluster centers (BCGs) are a unique example of Black Hole/Intergalactic gas interaction. The goal of LYRICS is to understand the life cycle of gas in the presence of AGN-feedback by studying the large filamentary network surrounding those galaxies. LYRICS builds up on i) large datasets and archival observations (MUSE, ALMA, NOEMA) ii) new implementation of physical models of gas excitation and iii) mature hydrodynamical simulations including AGN-feedback. Organised around a very complementary team, LYRICS will provide the very first comprehensive picture of the origin and state of the gas circulating around BCGs.