Conveners
SESSION 4 : The Magellanic System: the Clouds, the Stream and the Leading Arm
- Oliver Müller ()
SESSION 4 : The Magellanic System: the Clouds, the Stream and the Leading Arm
- Oliver Müller ()
SESSION 4 : The Magellanic System: the Clouds, the Stream and the Leading Arm
- Ekta Patel ()
SESSION 4 : The Magellanic System: the Clouds, the Stream and the Leading Arm
- Ekta Patel ()
Recent panoramic maps of the Magellanic system have revealed a wealth of low-surface-brightness stellar substructures surrounding both the Large and Small Magellanic Clouds (LMC/SMC); clear evidence of tidal interactions between the two Clouds, as well as with the Milky Way. However, the interaction history of the Magellanic system beyond the most recent LMC/SMC close passage remains poorly...
The Magellanic Bridge is a tidally-stripped structure located between the Magellanic Clouds and contains hundreds of stellar clusters and associations, which can help understanding the origin and evolution of the entire Magellanic Clouds-Milky Way (MW) system. Two main competing models describe the formation of the pair LMC-SMC: the LMC captured the SMC about 2 Gyr ago and they are in a bound...
Observational studies have identified several sub-structures in different regions of the Magellanic Clouds (MCs). One such interesting sub-structure in the Small Magellanic Cloud (SMC) is a dual population of intermediate-age giant stars which are spatially and kinematically distinct. Comparisons with simulations suggest that the foreground population might be tidally stripped from the SMC...
The Large Magellanic cloud(LMC) and Small Magellanic cloud(SMC) are the nearest interacting dwarf galaxies in the local group. And Magellanic clouds(MCs) have had interactions with each other as well as with the Milky Way. These interactions have triggered star formation in both galaxies, resulting in the formation of star clusters. Thus a comprehensive analysis of cluster population in MCs...
The Small Magellanic Cloud (SMC), as one of the nearest galaxies to us, provides a superb laboratory for studying its stellar populations in exquisite detail. We collected the largest sample of SMC red giant branch (RGB) stars (~6000) observed using the AAOmega spectrograph fed by the Two Degree Field (2dF) multi-object system at the Anglo-Australian Telescope of the Siding Spring Observatory...
Dark matter halo properties are well studied in cosmological simulations but are very challenging to estimate from observations. The dark matter halo density profile of galaxies from observations has been modeled previously using multiple probes that trace the dark matter potential, however, the angular momentum distribution of the dark matter halos is still a subject of debate. In this study,...
The Magellanic Stream is the most spectacular example of a gaseous stream in the local Universe. In this review I will discuss the Stream's importance for many areas of Galactic astronomy, summarize key unanswered questions, and identify future observations and simulations needed to resolve them.
The Large Magellanic Cloud (LMC) is the largest of the dwarf galaxies orbiting the Milky Way (MW). It sits in a very interesting niche within the Local Group (LG), being both sufficiently different in mass than the MW to be an interesting comparison and sufficiently massive to be a major player in the MW's recent history and present state. In particular, it is massive enough to have a...
The Magellanic Stream is unique to sample the MW potential from ~50kpc to 300
kpc, and is also unique in constraining the LMC mass, an increasingly important
question for the Local Group/Milky Way modeling. I will compare on the
strengths and weaknesses of the two types of models (tidal and ram-pressure) of
the Magellanic Stream formation. I will present our modeling for the...
The OC stream is a dwarf galaxy stream and is one of the longest and best-measured streams in the Galaxy, spanning over 200 degrees on the sky. It extends from the inner Milky Way ($\sim$15 kpc) to the outer halo ($\sim$60 kpc), giving us a great tool with which to measure our Galaxy's dark matter halo. In addition, portions of the stream pass remarkably close to the LMC ($\sim$5 kpc),...
In the last two decades, some arguments have accumulated for a more important mass ratio of the Large Magellanic Cloud (LMC) to the Milky Way (MW) than was previously thought, of about 10% or more. This implies that the LMC has a measurable influence on the dynamics in the MW stellar halo, including both stellar densities and kinematics, as observed by Conroy et al. (2021) and Petersen *et...
The ongoing interaction of the Large Magellanic Cloud (LMC) and Milky Way (MW) allows for constraint of the mass (and profile) of both. Through comparison of models of the interaction and 6d halo star data, we determined that the LMC is currently both pulling the MW stellar disc away from the barycentre of the MW at 30 km/s, as well as inducing a measurable distortion in the outer halos of...
The vast multidimensional data observed in the Local Group (LG) provide us with the unique opportunity of comparing the properties of the LG with their simulated analogs in cosmological simulations. In such a comparison it has been found that the observed kinematic properties of satellite galaxies in the LG are very unusual when compared to cosmological simulations. In both the Milky Way and...
The Small Magellanic Cloud (SMC) is one of the nearest, gas-rich interacting dwarf satellites of the Milky Way and the companion of the Large Magellanic Cloud (LMC). The interactions with the LMC and/or with the Milky Way play a significant role in the evolution of the SMC. With its widespread star formation and low metallicity, the SMC is one of the best test beds to study star formation and...
Recent measurements of a high mass for the LMC imply the LMC should host a massive Magellanic Corona, a collisionally ionized, warm-hot gaseous halo at the virial temperature $\sim10^{5.4}$ K initially extending out to the virial radius (100 - 130 kpc). Such a primordial Magellanic Corona would have shaped and fed the formation of the Magellanic Stream (e.g. Lucchini et al. 2020). Now, we have...
I present work on a spatially resolved, global star-formation history (SFH) of the Small Magellanic Cloud (SMC). I use the unprecedented deep photometric data (g~24 magnitude) from the Survey of the MAgellanic Stellar History (SMASH) survey utilising the Dark Energy Camera (DECAm) on the NOAO Blanco 4 m Telescope. The SFH is quantitatively obtained using colour-magnitude diagram (CMD) fitting...
One major source of disequilibrium in the Milky Way is its most massive satellite, the LMC. Kinematics of distant halo tracers show a velocity dipole in the Milky Way halo, which has been interpreted using N-body simulations as the LMC inducing a reflex motion in the Milky Way disk. In this talk, I discuss applying this framework to more realistic halos comprised of substructure from the...
The Large and Small Magellanic Clouds (LMC and SMC) are the largest and most luminous dwarf satellite companions of the Milky Way. Due to their close proximity, they provide a unique opportunity to study the dynamics of their resolved stellar populations in unparalleled detail. Within the last years, high-precision proper motion measurements of stars within the Magellanic Clouds had a...
In this talk, I will discuss recent UV absorption-line measurements of large-scale gas flows in the Local Group with particular emphasis on the relation between LG galaxy kinematics and CGM/IGrM gas dynamics. New results from an HST/COS all-sky survey of gas in the Milky Way's CGM and the Local Group IGrM will be presented and compared with predictions from the HESTIA simulations .
