2024A&A...688A.153P


Query : 2024A&A...688A.153P

2024A&A...688A.153P - Astronomy and Astrophysics, volume 688A153 (2024/8-1)

The satellite galaxy plane of NGC 4490 in light of ΛCDM Sparsity of similarly extreme analogs and a possible role of satellite pairs.

PAWLOWSKI M.S., MULLER O., TAIBI S., JULIO M.P., KANEHISA K.J. and HEESTERS N.

Abstract (from CDS):

Context. The system of galaxies around NGC 4490 was recently highlighted to display a flattened, kinematically correlated structure reminiscent of planes of satellite galaxies around other hosts.
Aims. Since known satellite planes are in tension with expectations from cosmological simulations in the Λ cold dark matter (ΛCDM) model, we aim to quantitatively assess for the first time the tension posed by the NGC 4490 system.
Methods. We measured the on-sky flattening as the major-to-minor axis ratio b/a of the satellite distribution and their line-of-sight kinematic correlation. Analogs to the system were selected in the TNG50 simulation and their flattening and correlation were similarly measured.
Results. We confirm the strong kinematic coherence of all 12 observed satellite objects with available line-of-sight velocities (of 14 in total): the northern ones approach and the southern ones recede relative to the host. The spatial distribution of all 14 objects is substantially flattened with b/a = 0.38 (0.26 considering only the 12 objects with available velocities). Such extreme arrangements are rare in the ΛCDM simulation, at a level of 0.21 to 0.35%. This fraction of analogs would drop further if at least one of the two satellite objects without velocities is confirmed to follow the kinematic trend, and would become zero if both are rejected as non-members. We also identify a likely galaxy pair in the observed system, and find a similar pair in the best-matching simulated analog.
Conclusions. Our measurements establish NGC 4490 as another strong example of a satellite plane in the Local Volume. This emphasizes that planes of satellites are a more general issue faced by ΛCDM also beyond the Local Group. The tension with typical systems drawn from simulations suggests that the observed one requires a specific formation scenario, potentially connected to the larger-scale galaxy alignment in its vicinity. The presence of galaxy pairs in the observed and a simulated system hints at the importance such groupings may have to understand satellite planes.

Abstract Copyright: © The Authors 2024

Journal keyword(s): galaxies: dwarf - galaxies: groups: individual: NGC 4490 - galaxies: kinematics and dynamics - dark matter

Simbad objects: 19

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Number of rows : 19
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 M 31 AGN 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 13622 1
2 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 3588 2
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 19090 0
4 NGC 2750 GiP 09 05 47.893 +25 26 14.51   12.7       ~ 121 0
5 M 81 Sy2 09 55 33.1726556496 +69 03 55.062505368   7.89 6.94     ~ 4725 3
6 M 106 Sy2 12 18 57.620 +47 18 13.39   9.14 8.41 8.11   ~ 2512 4
7 SMDG J1224352+393812 LSB 12 24 35.19 +39 38 12.1           ~ 5 0
8 NGC 4369 AGN 12 24 36.204 +39 22 58.73   12.3       ~ 210 1
9 SMDG J1229432+410943 LSB 12 29 43.24 +41 09 42.7           ~ 6 0
10 NGC 4485 GiP 12 30 31.113 +41 42 04.22 12.10 12.42 11.93 11.93   ~ 305 2
11 NGC 4490 GiG 12 30 34.5 +41 38 26 10.03 10.22 9.79     ~ 616 3
12 Z 216-11 GiG 12 34 00.54952 +39 01 09.3052   15.4       ~ 65 0
13 LEDA 2178478 AG? 12 34 38.222 +41 16 36.11           ~ 8 0
14 MCG+07-26-029 LSB 12 35 11.596 +41 03 34.69   16.5       ~ 36 0
15 NAME Centaurus A BLL 13 25 27.61521044 -43 01 08.8050291   8.18 6.84 6.66   ~ 4774 3
16 M 83 SBG 13 37 00.91920 -29 51 56.7400 8.85 8.11 7.52 7.21   ~ 2778 2
17 M 101 GiP 14 03 12.583 +54 20 55.50   8.46 7.86 7.76   ~ 3138 2
18 NGC 7751 AG? 23 46 58.3588462776 +06 51 42.726478248   13.9       ~ 41 0
19 NAME Local Group GrG ~ ~           ~ 9325 0

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