2022A&A...657A..94N


Query : 2022A&A...657A..94N

2022A&A...657A..94N - Astronomy and Astrophysics, volume 657A, 94-94 (2022/1-1)

The Fornax Cluster VLT Spectroscopic Survey. IV. Cold kinematical substructures in the Fornax core from COSTA.

NAPOLITANO N.R., GATTO M., SPINIELLO C., CANTIELLO M., HILKER M., ARNABOLDI M., TORTORA C., CHATURVEDI A., D'ABRUSCO R., LI R., PAOLILLO M., PELETIER R., SAIFOLLAHI T., SPAVONE M., VENHOLA A., CAPACCIOLI M. and LONGO G.

Abstract (from CDS):


Context. Substructures in stellar haloes are a strong prediction of galaxy formation models in ΛCDM. Cold streams such as those from small satellite galaxies are extremely difficult to detect and kinematically characterize. The COld STream finder Algorithm (COSTA) is a novel algorithm able to find streams in the phase space of planetary nebulae (PNe) and globular cluster (GC) populations. COSTA isolates groups of (N) particles with small velocity dispersion (between 10 km/s and ∼120 km/s) using an iterative (n) sigma-clipping over a defined number of (k) neighbor particles.
Aims. We applied COSTA to a catalog of PNe and GCs from the Fornax Cluster VLT Spectroscopic Survey (FVSS) within ∼200 kpc from the cluster core in order to detect cold substructures and characterize their kinematics (mean velocity and velocity dispersion).
Methods. We selected more than 2000 PNe and GCs from the FVSS catalogs and adopted a series of optimized setups of the COSTA parameters based on Montecarlo simulations of the PN and GC populations to search for realistic stream candidates. We find 13 cold substructures with velocity dispersion ranging from ∼20 to ∼100 km/s, which are likely associated either to large galaxies or to ultra-compact dwarf (UCD) galaxies in the Fornax core.
Results. The luminosities of these streams show a clear correlation with internal velocity dispersion, and their surface brightness correlates with their size and distance from the cluster center, which is compatible with the dissipative processes producing them. However, we cannot exclude that some of these substructures formed by violent relaxation of massive satellites that finally merged into the central galaxy. Among these substructures we have: (1) a stream connecting NGC 1387 to the central galaxy, NGC 1399, previously reported in the literature; (2) a new giant stream produced by the interaction of NGC 1382 with NGC 1380 and (possibly) NGC 1381; (3) a series of streams kinematically connected to nearby UCDs; and (4) clumps of tracers with no clear kinematical association to close cluster members.
Conclusions. We show evidence for a variety of cold substructures predicted in simulations. Most of the streams are kinematically connected to UCDs, supporting the scenario that they can be remnants of disrupted dwarf systems. However, we also show the presence of long coherent substructures connecting cluster members and isolated clumps of tracers possibly left behind by their parent systems before these merged into the central galaxy. Unfortunately, the estimated low-surface brightness of these streams does not allow us to find their signatures in the current imaging data and deeper observations are needed to confirm them.

Abstract Copyright: © ESO 2022

Journal keyword(s): intergalactic medium - galaxies: interactions - galaxies: formation - galaxies: kinematics and dynamics

Status at CDS : Examining the need for a new acronym.

Simbad objects: 30

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Number of rows : 30
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 NGC 1379 GiP 03 36 03.9668625792 -35 26 28.547476800 12.17 12.04 10.91 10.60   ~ 255 1
2 NGC 1380 GiP 03 36 27.590 -34 58 34.68 11.32 10.94 9.93 9.37   ~ 406 1
3 NGC 1381 GiP 03 36 31.6592184144 -35 17 42.739221912 12.90 12.47 11.50 11.02   ~ 238 1
4 NGC 1387 GiP 03 36 57.0337458600 -35 30 23.675934060 12.18 11.75 10.69 10.16   ~ 247 1
5 FLSBG 248 LSB 03 36 59.8 -35 20 36           ~ 9 1
6 NGFS J033706-352031 G 03 37 06.038 -35 20 29.37           ~ 3 0
7 NGC 1382 GiP 03 37 08.9722655064 -35 11 41.995386996 13.19 13.79 12.92 12.31   ~ 114 1
8 LEDA 74787 LSB 03 37 10.0 -35 23 11   19.3       ~ 16 0
9 NGFS J033716-352130 LSB 03 37 15.685 -35 21 29.67           ~ 5 0
10 NGFS J033720-353118 G 03 37 19.884 -35 31 17.76           ~ 3 0
11 NGFS J033738-352308 LSB 03 37 38.6 -35 23 07           ~ 6 0
12 NGFS J033750-353302 G 03 37 49.872 -35 33 01.58           ~ 3 0
13 NGFS J033751-352146 LSB 03 37 50.909 -35 21 46.37           ~ 5 0
14 NGFS J033754-353429 G 03 37 53.866 -35 34 29.23           ~ 2 0
15 NGC 1396 GiG 03 38 06.5677454520 -35 26 23.637846372   14.80       ~ 89 1
16 LEDA 74806 LSB 03 38 18.80 -35 31 49.4   17.3 17.18     ~ 31 1
17 NGC 1399 BiC 03 38 29.083 -35 27 02.67 11.05 9.74 9.59 8.12   ~ 1530 1
18 ACO S 373 ClG 03 38 30 -35 27.3           ~ 1725 0
19 NGFS J033842-352329 G 03 38 41.826 -35 23 30.41           ~ 3 0
20 FCC B1281 GiC 03 38 42.2 -35 33 08           ~ 7 0
21 NGC 1404 GiP 03 38 51.917 -35 35 39.81 11.53 10.69 10.00 9.03   ~ 725 1
22 NGFS J033922-353524 G 03 39 22.473 -35 35 24.08           ~ 3 0
23 NGFS J033929-353421 LSB 03 39 28.908 -35 34 21.30           ~ 5 0
24 NGFS J033942-352806 LSB 03 39 41.997 -35 28 06.10           ~ 5 0
25 NGFS J034002-352930 G 03 40 01.740 -35 29 29.86           ~ 2 0
26 NGFS J034003-352754 LSB 03 40 03.118 -35 27 54.26           ~ 5 0
27 NAME Hydra I Cluster ClG 10 36 36.0 -27 31 04           ~ 813 1
28 NAME Virgo Cluster ClG 12 26 32.1 +12 43 24           ~ 6379 0
29 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4599 2
30 NAME Local Group GrG ~ ~           ~ 7893 0

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2023.01.30-22:16:34

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