Context : The HR 1614 is an overdensity in velocity space and has for a long time been known as an old ( \sim 2 Gyr ) and metal-rich ( [ Fe / H ] \approx + 0.2 ) nearby moving group that has a dissolving open cluster origin .
The existence of such old and metal-rich groups in the solar vicinity is quite unexpected since the vast majority of nearby moving groups are known to be young .

Aims : In the light of new and significantly larger data sets than ever before ( astrometric , photometric , and spectroscopic ) , we aim to re-investigate the properties and origin of the HR 1614 moving group .
If the HR 1614 overdensity is a dissolving cluster , its stars should represent a single-age and single-elemental abundance population .

Methods : To identify and characterise the HR 1614 moving group we use astrometric data from Gaia DR2 ; distances , extinction , and reddening corrections from the StarHorse code ; elemental abundances from the GALAH and APOGEE spectroscopic surveys ; and photometric metallicities from the SkyMapper survey .
Bayesian ages were estimated for the SkyMapper stars .
Since the Hercules stream is the closest kinematical structure to the HR 1614 moving group in velocity space and as its origin is believed to be well-understood , we use the Hercules stream for comparison purposes .
Stars that are likely to be members of the two groups were selected based on their space velocities .

Results : The HR 1614 moving group is located mainly at negative U velocities , does not form an arch of constant energy in the U - V space , and is tilted in V .
We find that the HR 1614 overdensity is not chemically homogeneous , but that its stars exist at a wide range of metallicities , ages , and elemental abundance ratios .
They are essentially similar to what is observed in the Galactic thin and thick discs , a younger population ( around 3 Gyr ) that is metal-rich ( -0.2 \leq [ Fe/H ] \leq 0.4 ) and alpha-poor .
These findings are very similar to what is seen for the Hercules stream , which is believed to have a dynamical origin and consists of regular stars from the Galactic discs .

Conclusions : The HR 1614 overdensity has a wide spread in metallicity , [ Mg/Fe ] , and age distributions resembling the general properties of the Galactic disc .
It should therefore not be considered a dissolving open cluster , or an accreted population .
Based on the kinematic and chemical properties of the HR 1614 overdensity we suggest that it has a complex origin that could be explained by combining several different mechanisms such as resonances with the Galactic bar and spiral structure , phase mixing of dissolving spiral structure , and phase mixing due to an external perturbation .