2018A&A...609A..40E


C.D.S. - SIMBAD4 rel 1.7 - 2019.08.24CEST21:02:08

2018A&A...609A..40E - Astronomy and Astrophysics, volume 609A, 40-40 (2018/1-1)

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

EPINAT B., CONTINI T., FINLEY H., BOOGAARD L.A., GUEROU A., BRINCHMANN J., CARTON D., MICHEL-DANSAC L., BACON R., CANTALUPO S., CAROLLO M., HAMER S., KOLLATSCHNY W., KRAJNOVIC D., MARINO R.A., RICHARD J., SOUCAIL G., WEILBACHER P.M. and WISOTZKI L.

Abstract (from CDS):

We report the discovery of a 104kpc2 gaseous structure detected in [OII]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)x1010M 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 [OIII]/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 ∼35kpc. 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.

Abstract Copyright: © ESO, 2017

Journal keyword(s): galaxies: evolution - galaxies: kinematics and dynamics - intergalactic medium - galaxies: interactions - galaxies: groups: general - galaxies: high-redshift

Nomenclature: Fig. 3, Tables 1-3: [ECF2018] A (Nos A-I), [ECF2018] NNN N=14 among (Nos 57-228).

Status in Simbad:  being processed

Simbad objects: 9

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Number of rows : 9

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NAME Hubble Ultra Deep Field reg 03 32 39.0 -27 47 29           ~ 1199 0
2 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14211 1
3 HD 49798 HXB 06 48 04.7000758397 -44 18 58.432035331 6.758 8.017 8.287 8.391 8.543 sdO6 275 0
4 CD-32 5613 WD* 08 41 32.4293043356 -32 56 32.916852010   12.07 11.85 12.3   DA5.5 256 0
5 NAME COSMOS Field reg 10 00 28.60 +02 12 21.0           ~ 1837 0
6 [KLI2009] 44 GrG 10 00 34.0 +02 04 09           ~ 5 0
7 NAME Spiderweb Galaxy AGN 11 40 48.3 -26 29 09     22.00     ~ 241 1
8 NAME HDF-S reg 22 32 56 -60 33.0           ~ 534 0
9 NAME Stephan's Quintet CGG 22 35 57.5 +33 57 36           ~ 373 1

    Equat.    Gal    SGal    Ecl

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2019.08.24-21:02:08

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