Ionised gas structure of 100 kpc in an over-dense region of the galaxy group COSMOS-Gr30 at z ~ 0.7

Benoît Epinat, Thierry Contini, Hayley Finley, Leindert Boogaard, Adrien Guérou, Jarle Brinchmann, David Carton, Léo Michel-Dansac, Roland Bacon, Sebastiano Cantalupo, Marcella Carollo, Stephen Hamer, Wolfram Kollatschny, Davor Krajnović, Raffaella Anna Marino, Johan Richard, Geneviève Soucail, Peter M. Weilbacher, Lutz Wisotzki

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Abstract

We report the discovery of a 10 4 kpc 2 gaseous structure detected in [O ii]λλ3727, 3729 in an over-dense region of the COSMOS-Gr30 galaxy group at z ∼ 0.725 with deep MUSE Guaranteed Time Observations. We estimate the total amount of diffuse ionised gas to be of the order of (∼5 ± 3) × 10 10 M - and explore its physical properties to understand its origin and the source(s) of the ionisation. The MUSE data allow the identification of a dozen group members that are embedded in this structure through emission and absorption lines. We extracted spectra from small apertures defined for both the diffuse ionised gas and the galaxies. We investigated the kinematics and ionisation properties of the various galaxies and extended gas regions through line diagnostics (R23, O32, and [O iii]/Hβ) that are available within the MUSE wavelength range. We compared these diagnostics to photo-ionisation models and shock models. The structure is divided into two kinematically distinct sub-structures. The most extended sub-structure of ionised gas is likely rotating around a massive galaxy and displays filamentary patterns that link some galaxies. The second sub-structure links another massive galaxy that hosts an active galactic nucleus (AGN) to a low-mass galaxy, but it also extends orthogonally to the AGN host disc over ∼ 35 kpc. This extent is likely ionised by the AGN itself. The location of small diffuse regions in the R23 vs. O32 diagram is compatible with photo-ionisation. However, the location of three of these regions in this diagram (low O32, high R23) can also be explained by shocks, which is supported by their high velocity dispersions. One edge-on galaxy shares the same properties and may be a source of shocks. Regardless of the hypothesis, the extended gas seems to be non-primordial. We favour a scenario where the gas has been extracted from galaxies by tidal forces and AGN triggered by interactions between at least the two sub-structures.

Original languageEnglish
Article numberA40
Pages (from-to)1-21
Number of pages21
JournalAstronomy & Astrophysics
Volume609
Early online date5 Jan 2018
DOIs
Publication statusPublished - 5 Jan 2018

Keywords

  • astro-ph.GA
  • Galaxies: evolution
  • Galaxies: kinematics and dynamics
  • Galaxies: groups: general
  • Intergalactic medium
  • Galaxies: interactions
  • Galaxies: high-redshift

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Epinat, B., Contini, T., Finley, H., Boogaard, L., Guérou, A., Brinchmann, J., Carton, D., Michel-Dansac, L., Bacon, R., Cantalupo, S., Carollo, M., Hamer, S., Kollatschny, W., Krajnović, D., Marino, R. A., Richard, J., Soucail, G., Weilbacher, P. M., & Wisotzki, L. (2018). Ionised gas structure of 100 kpc in an over-dense region of the galaxy group COSMOS-Gr30 at z ~ 0.7. Astronomy & Astrophysics, 609, 1-21. [A40]. https://doi.org/10.1051/0004-6361/201731877