arXiv subjects

Istiak Akib

Publications and source records attributed to Istiak Akib.

3 recordsLinked to original sources

arXiv2026

The accretion history of the Milky Way V. The kinematics of most globular clusters trace the merger epochs

Several studies have associated globular clusters (GCs) with former Galactic accretion events by comparing their positions in the energy-angular momentum ($E$-$L_z$) plane, an approach further supported by similarities in their age-metallicity relations. However, recent merger simulations suggest that GCs initially associated with the Gaia-Sausage-Enceladus (GSE) disc may have lost their orbital energy and thus may not reliably trace this accretion event. We extend this framework by considering three N-body simulations of the Milky Way-GSE merger with different initial masses, mass ratios, and gas content. In addition to GCs belonging to the GSE disc progenitor, we accounted for GCs in its halo and, in gas-rich models, a population of GCs formed during the Milky Way-GSE merger. We confirm that most GCs originating in the disc have lost a significant part of their orbital energy during repeated passages through the dense disc medium, and we conjecture that associated tidal shocks may have destroyed many of them. In contrast, GCs from the halo and GCs formed during the merger have largely retained their orbital energy, which remains comparable to that of GSE stars even up to 9 Gyr after the completion of the merger. By using a more realistic GC population and GSE modelling, we find that most GCs linked to GSE can be associated with Milky Way accretion events in the $E$-$L_z$ plane, which supports previous observational associations based on a combination of energy-angular momentum and age-metallicity relations.

astro-ph.GA↗

arXiv2025

Impact of merger histories on the timing argument estimate of the Local Group mass

The timing argument (TA) aims to find the total mass of the Local Group (LG) from the relative motions of the Milky Way (MW) and Andromeda Galaxy (M31). However, the classical TA always overestimates the LG mass, presumably because it does not account for the hierarchical scenario and other interactions such as that with the Large Magellanic Cloud (LMC). We focus on the impact of the recent major merger at M31 by using three merger models to find the peculiar motion of M31 within the simple two-body and point-mass scenario of TA. We found that the merger correction may affect the TA mass by either plus or minus 10-15% depending on the M31 tangential motion, which has very large uncertainties. If we consider a M31 merger configuration that reduces the TA mass by 10-15% to which we add the impact due to the LMC infall into the MW as reported in the literature, the TA mass would be found consistent with the LG mass from Hubble-Lemaitre flow. Galaxies are expected to experience about 16 major mergers each since z=11.5. Assuming all these mergers have similar impact on the TA mass as the most recent M31 merger, the ratio of LG mass to TA mass would be $0.85^{+0.65}_{-0.37}$ and such a TA mass is consistent with all the LG mass estimates. Our result also agrees with the findings using LG analogues in the cosmological simulations. We find that the TA mass estimate is limited by the hierarchical scenario, since it not possible to track the progenitors of both MW and M31 through so many mergers. We conclude that the MW-M31 dynamical system is far too complex to be modelled as a simple two-body point mass system.

astro-ph.GA↗

arXiv2025

An intriguing coincidence between the majority of vast polar structure dwarfs and a recent major merger at the M31 position

A significant part of the Milky Way (MW) dwarf galaxies orbit within a Vast POlar Structure (VPOS), which is perpendicular to the Galactic disc and whose origin has not yet been identified. It includes the Large Magellanic Cloud (LMC) and its six dynamically associated dwarf galaxies. Andromeda Galaxy (M31) experienced a major merger two to three billion years ago, and its accurate modelling predicts that an associated tidal tail is pointing towards the Galaxy. Here, we tested a possible association between M31 tidal tail particles and MW dwarf galaxies, focusing first on the LMC and its associated dwarfs since they are less affected by ram pressure. We traced back these dwarf galaxy orbits by one billion years and calculated their association with the tidal tail particles in the 6D phase space, based on their proper motion from \textit{Gaia} DR3. We find that for low-mass MW models (total mass less than 5 $\times 10^{11} M_{\odot}$), the separation in the 6D space can be less than 1$σ$ for most of the M31 modelling, albeit with a significant degree of freedom due to the still unknown proper motion of M31. We further discover that many other dwarfs could also be associated with the M31 tidal tails if their motions had been radially slowed, as expected from the ram pressure exerted by the MW corona. This intriguing coincidence could explain the origin of the VPOS, which resulted from a matter exchange between M31 and MW.

astro-ph.GA↗