BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Modeling Dark Matter Halo Spin using Observations and Simulations: application to UGC 5288 DTSTART;VALUE=DATE-TIME:20230322T150300Z DTEND;VALUE=DATE-TIME:20230322T150500Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-278@meetings.aip.de DESCRIPTION:Speakers: Ansar Sioree (Indian Institute of Astrophysics\, Ben galuru)\nDark matter halo properties are well studied in cosmological simu lations but are very challenging to estimate from observations. The dark m atter halo density profile of galaxies from observations has been modeled previously using multiple probes that trace the dark matter potential\, ho wever\, the angular momentum distribution of the dark matter halos is stil l a subject of debate. In this study\, we demonstrate a method for estimat ing the halo spin and halo concentration of a low luminosity\, gas-rich dw arf galaxy by forward modeling disk properties derived from observations o f the stellar and gas surface densities\, the disk scale length\, the neut ral hydrogen rotation curve\, the bar length\, and bar ellipticity. Our me thod is a combination of semi-analytical techniques and N-body/SPH simulat ions. Here\, we apply our method to the low surface brightness (LSB) dwarf galaxy UGC 5288\, and model its dark matter halo with both a cuspy Hernqu ist profile and a flat-core pseudo-isothermal profile. We find that the be st match with observations is a pseudo-isothermal halo model with core rad ius r$_{c}$ = 0.23 kpc and a high halo spin $\\lambda$ = 0.08 at the viria l radius. These findings are consistent with previous rotation curve estim ates of the halo density profile of UGC 5288\, as well as the theoreticall y predicted high spins of dwarf LSB galaxies. We finally compare our resul ts with the halo spin distribution of barred galaxies in one of the high r esolution cosmological magneto-hydrodynamical simulations TNG-50. We find that our model predicts halo spin distribution of UGC5288 up to a ballpark value\, although\, there remain significant uncertainties due to the form ation history of the dark matter halos from the TNG50 simulations. We also find that the inner halo spin in barred galaxies is different from that o f unbarred ones\, and the halo spin shows weak correlations with bar prope rties.\n\nhttps://iaus379.aip.de/event/20/contributions/278/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/278/ END:VEVENT BEGIN:VEVENT SUMMARY:Large-scale gas flows in the Local Group DTSTART;VALUE=DATE-TIME:20230323T103000Z DTEND;VALUE=DATE-TIME:20230323T104500Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-212@meetings.aip.de DESCRIPTION:Speakers: Philipp Richter (University of Potsdam)\nIn this tal k\, I will discuss recent UV absorption-line measurements of large-scale g as flows in the Local Group with particular emphasis on the relation betwe en 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 simulatio ns .\n\nhttps://iaus379.aip.de/event/20/contributions/212/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/212/ END:VEVENT BEGIN:VEVENT SUMMARY:The dynamical mass of the Large Magellanic Cloud as measured by it s system of star clusters DTSTART;VALUE=DATE-TIME:20230323T101500Z DTEND;VALUE=DATE-TIME:20230323T103000Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-206@meetings.aip.de DESCRIPTION:Speakers: Florian Niederhofer (Leibniz-Institut für Astrophys ik Potsdam (AIP))\nThe 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 stud y the dynamics of their resolved stellar populations in unparalleled detai l. Within the last years\, high-precision proper motion measurements of st ars within the Magellanic Clouds had a tremendous impact on our understand ing of the Magellanic system and its relation to our own Galaxy. To date\, however\, the dynamics of the star cluster systems within the two dwarf g alaxies has not received much attention. \nIn this contribution\, I will i ntroduce an ongoing observational campaign conducted by our team utilising the Hubble Space Telescope (HST) to precisely measure the proper motions of star clusters within the LMC. The exquisite resolution of HST allows us to measure precise proper motions of thousands of stars within each clust er.\nThe measured motions of the clusters\, combined with photometric and spectroscopic measurements\, will yield their full 6-dimensional phase spa ce information within the LMC. I will present first results of the kinemat ic structures that are described by clusters of various ages and within di fferent structural components of the galaxy. The motions of the clusters c an further act as a tracer of the gravitational potential of the LMC and I will present preliminary measurements of the mass of the LMC resulting fr om the dynamics of the star clusters. Despite its importance in the field of Magellanic Cloud kinematics and evolution\, the mass of the LMC is only vaguely known and several studies disagree on it. Our cluster-based study will provide an additional independent measurement of the LMC's mass.\n\n https://iaus379.aip.de/event/20/contributions/206/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/206/ END:VEVENT BEGIN:VEVENT SUMMARY:The stellar halo’s response as a probe of the LMC to MW mass rat io DTSTART;VALUE=DATE-TIME:20230323T082500Z DTEND;VALUE=DATE-TIME:20230323T084000Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-187@meetings.aip.de DESCRIPTION:Speakers: Simon Rozier (Observatoire Astronomique de Strasbour g)\nIn the last two decades\, some arguments have accumulated for a more i mportant 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 al.* (2021). While this merger has been p reviously reproduced using N-body simulations (see\, e.g.\, Garavito-Camar go *et al.*\, 2019)\, I will present the results of a recent study (Rozier *et al.*\, 2022) which aimed at modelling the merger via linear response theory. More specifically\, we integrated the linearized collisionless Bol tzmann-Poisson system of partial differential equations using a methodolog y known as the matrix method. Our results display the same large scale beh aviour as state-of-the-art simulations\, with a dipolar over/underdense pa ttern related to the reflex motion of the MW\, as well as an overdense wak e trailing behind the LMC. These results represent an efficient way of con straining the LMC to MW mass ratio\, since this ratio is directly proporti onal (given the linear nature of the theory) to the amplitude of the relat ive density variations of the MW stellar halo\, both in physical and in ph ase space. However\, the amplitude of these variations may also depend on some model parameters\, such as the structure of the MW potential (includi ng a possible dark matter component)\, the initial density distribution of the stellar halo\, as well as its initial internal kinematics. I will foc us on the latter source of degeneracy\, showing how the initial velocity a nisotropy of the stellar halo impacts its response to the LMC. Interesting ly enough\, it appears that the physical space density of the (dipolar) re flex motion is insensitive to the stellar halo’s initial velocity anisot ropy\, and can therefore represent an efficient probe of the LMC to MW mas s ratio.\n\nhttps://iaus379.aip.de/event/20/contributions/187/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/187/ END:VEVENT BEGIN:VEVENT SUMMARY:The Magellanic System DTSTART;VALUE=DATE-TIME:20230322T155000Z DTEND;VALUE=DATE-TIME:20230322T163000Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-290@meetings.aip.de DESCRIPTION:Speakers: Elena d’Onghia (UNIVERSITY of WISCONSIN–MADISON) \nThe Magellanic Stream is the most spectacular example of a gaseous strea m in the local Universe. In this review I will discuss the Stream's import ance for many areas of Galactic astronomy\, summarize key unanswered quest ions\, and identify future observations and simulations needed to resolve them.\n\nhttps://iaus379.aip.de/event/20/contributions/290/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/290/ END:VEVENT BEGIN:VEVENT SUMMARY:Spatio- temporal formation history and kinematics of star clusters in the Magellanic Clouds: Propagation of cluster formation and the LMC ba r DTSTART;VALUE=DATE-TIME:20230322T145900Z DTEND;VALUE=DATE-TIME:20230322T150100Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-276@meetings.aip.de DESCRIPTION:Speakers: Dhanush Sathiavals Reselammal (Senior Research fello w\, IIA)\nThe Large Magellanic cloud(LMC) and Small Magellanic cloud(SMC) are the nearest interacting dwarf galaxies in the local group. And Magell anic clouds(MCs) have had interactions with each other as well as with the Milky Way. These interactions have triggered star formation in both galax ies\, resulting in the formation of star clusters. Thus a comprehensive an alysis of cluster population in MCs could indicate the structural evolutio n due to galaxy mergers. Our aim is to understand the age dating\, spatio- temporal map of cluster formation episodes\, and trace the cluster kinemat ics as a function of age.\nIn this study\, we used the GAIA DR3 data to ch aracterise the cluster population in the MCs. The clusters in the MCs is o btained mostly from general catalogue given by Bica et al. (2020)\, and se veral other recent literature. We classified the clusters as isolated and merged based on projected sky coordinates. Around 2000 clusters were analy zed in our study based on a certain selection criteria. We used Gaia async hronous query to bulk handle the cluster data from Gaia archive\, after ap plying proper motion-parallax cut offs and faintness magnitude limit. We d eveloped a statistical algorithm to remove filed stars from the cluster re gion. We used single to multiple comparison field regions and retrieved th e most probable cluster members. Using Padova-Parsec stellar evolutionary models\, we performed an iterative least square method to estimate the ag e and reddening of clusters that had sufficient members and a satisfactory fit of the isochrone. The spatio-temporal map of age and reddening was ob tained for clusters in both clouds. We traced the cluster formation episod es at ~ 1.6 Gyr\, 630 Myr\, 310 Myr\, and 80 Myr. The directional propagat ion of cluster formation is noted from the South to North of LMC over the time scale of 2.8 Gyr to 10 Myr. We are able to estimate the formation ti me of the LMC’s off-centered bar. Using the proper motion data of the m embers we also study the proper motion of the clusters with respect to the field population in both the Clouds.\n\nhttps://iaus379.aip.de/event/20/c ontributions/276/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/276/ END:VEVENT BEGIN:VEVENT SUMMARY:Tracing the structure and history of the Small Magellanic Cloud us ing CaII Triplet spectroscopy DTSTART;VALUE=DATE-TIME:20230322T150100Z DTEND;VALUE=DATE-TIME:20230322T150300Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-275@meetings.aip.de DESCRIPTION:Speakers: Mahdieh Navabi (The University of Surrey)\nThe Small Magellanic Cloud (SMC)\, as one of the nearest galaxies to us\, provides a superb laboratory for studying its stellar populations in exquisite deta il. 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 (Australia). The metallicities were recovered using a direct estimation of [Fe/H] from the equivalent widths of the Calcium tri plet (CaT). We discuss the potential implications of the metallicity gradi ents and compare these to previous determinations of star formation histor ies to assess the consequences of encounters between the SMC and Large Mag ellanic Cloud.\n **Finally\, we discuss our findings in the context of the correlation that exists between metallicity and dynamical mass in dwarf I rregular systems\, of which the SMC is our closest example.**\n\nhttps://i aus379.aip.de/event/20/contributions/275/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/275/ END:VEVENT BEGIN:VEVENT SUMMARY:Stromgren photometric metallicity map of the Small Magellanic Clou d using Gaia DR3-XP spectra. DTSTART;VALUE=DATE-TIME:20230322T145700Z DTEND;VALUE=DATE-TIME:20230322T145900Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-274@meetings.aip.de DESCRIPTION:Speakers: Abinaya Ondivillu Omkumar (Leibniz Institute for Ast rophysics Potsdam (AIP))\nObservational studies have identified several su b-structures in different regions of the Magellanic Clouds (MCs). One such interesting sub-structure in the Small Magellanic Cloud (SMC) is a dual p opulation of intermediate-age giant stars which are spatially and kinemati cally distinct. Comparisons with simulations suggest that the foreground p opulation might be tidally stripped from the SMC main-body\, but their ori gin is not clearly proven yet. If we have homogeneous metallicity measurem ents of the sources from these sub-structures\, we can see whether they ar e having similar values or different from the main-body population. Hence\ , metallicity measurements of these populations will help us understand th eir origin and/or their association with the Large Magellanic Cloud (LMC). However\, spectroscopic metallicities are only available for a few thousa nd sources and also from different instruments at various spectral resolut ions\, which makes it difficult to compare their values and draw conclusio ns from the results. The third data release of Gaia has provided us with ~ 0.17 million XP spectra of the SMC sources as faint as ~ 18 mag in G-band which are spread across ~ 10° from the SMC center. Stromgren photometry is a well-established method to estimate the photometric metallicities. Ga ia BP spectra covers the u\, v\, b and y Strömgren bands. Using the estim ated Strömgren magnitudes from the Gaia BP spectra\, we calibrated the [F e/H] values. We compared a subset of the SMC sources that has [Fe/H] value s from the high-resolution (~ 22\,500) APOGEE spectrograph for the validat ion of our method. Using those metallicity measurements\, we produce a hom ogeneous metallicity map of the entire SMC also with a higher spatial reso lution and study the metallicity of different sub-structures to shed light on their possible origin and/or their associations with the LMC.\n\nhttps ://iaus379.aip.de/event/20/contributions/274/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/274/ END:VEVENT BEGIN:VEVENT SUMMARY:Ages\, metallicities and structure of stellar clusters in the Mage llanic Bridge DTSTART;VALUE=DATE-TIME:20230322T145500Z DTEND;VALUE=DATE-TIME:20230322T145700Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-233@meetings.aip.de DESCRIPTION:Speakers: Raphael A. P. Oliveira (IAG - USP)\nThe Magellanic B ridge is a tidally-stripped structure located between the Magellanic Cloud s and contains hundreds of stellar clusters and associations\, which can h elp understanding the origin and evolution of the entire Magellanic Clouds -Milky Way (MW) system. Two main competing models describe the formation o f the pair LMC-SMC: the LMC captured the SMC about 2 Gyr ago and they are in a bound orbit around the MW\, or it is an old interacting sys- tem in i ts first perigalactic passage\, falling into the MW potential ~2 Gyr ago. The Bridge should have been formed during a collision between the Clouds a round 200 Myr ago\, imply- ing kinematic signatures\, as well as age and m etallicity gradients along its extension. This work combines deep photomet ric data from VISCACHA and SMASH surveys in order to ex- plore this questi on\, by homogeneously deriving age\, metallicity\, distance\, structural p arame- ters and mass of 35 Bridge objects with modern statistical tools su ch as Markov chain Monte Carlo and machine learning. In particular\, the m ass determination corrected by completeness can help to estimate the Bridg e stellar mass and constrain the dynamical models. A spectro- scopic follo w-up in the CaII triplet region is also carried out for clusters older tha n 1 Gyr in the Bridge and other SMC regions\, to derive metallicity and ra dial velocity which\, combined with Gaia proper motions\, allow us to obta in a 6D phase-space vector. Preliminary results show a good agreement betw een VISCACHA and SMASH data and also that\, despite the presence of some o ld objects at larger distances\, the clusters in the middle of the Bridge are younger (~ 10-100 Myr) and more metal-rich than those closer to the SM C Wing. In this poster\, we will review the recent results of the VISCACHA collaboration\, present a detailed approach to age and metallicity gradie nts in the Bridge\, and discuss the evidence on the most probable for- mat ion model of the pair LMC-SMC.\n\nhttps://iaus379.aip.de/event/20/contribu tions/233/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/233/ END:VEVENT BEGIN:VEVENT SUMMARY:Exploring the kinematics of the Magellanic stellar periphery DTSTART;VALUE=DATE-TIME:20230322T143000Z DTEND;VALUE=DATE-TIME:20230322T145500Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-179@meetings.aip.de DESCRIPTION:Speakers: Lara Cullinane (JHU)\nRecent panoramic maps of the M agellanic 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 we ll as with the Milky Way. However\, the interaction history of the Magella nic system beyond the most recent LMC/SMC close passage remains poorly con strained. In order to shed light on this issue\, we have instigated a larg e-scale spectroscopic follow-up of stars in low-density features extending to distances beyond 20 degrees from the Clouds’ centres. We use a combi nation of Gaia astrometry and spectroscopically-derived radial velocities\ , obtained with 2dF+AAOmega on the Anglo-Australian Telescope\, to determi ne 3D kinematics for thousands of stars in these features and the extended outer disks of the two Clouds. In this talk\, I will discuss new results focussed on the southern outskirts of the LMC. Several substructures in th is region\, including claw-like features extending from the southern LMC d isk\, and a long arm-like substructure wrapping around the southern LMC ou tskirts toward the eastern SMC disk\, are found to be predominantly compos ed of perturbed LMC disk material. All substructures show significant pert urbations from equilibrium disk kinematics\, with one claw-like feature di splaying out-of-plane velocities exceeding 60 km/s and apparent counter-ro tation relative to the LMC’s disk. Such complex features plausibly requi re multiple previous interactions with the SMC to fully explain the observ ed dynamical properties. This demonstrates the efficacy of our data as a b enchmark for assessing dynamical models to disentangle the origins of Mage llanic substructures\, the masses of the two Clouds\, and the evolution of the Magellanic system. I will also briefly discuss new efforts to conduct analogous kinematic mapping of M33 and its outskirts\, which aim to simil arly understand the evolution of this massive dwarf galaxy.\n\nhttps://iau s379.aip.de/event/20/contributions/179/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/179/ END:VEVENT BEGIN:VEVENT SUMMARY:The impact of massive satellites on the kinematic properties of th e Local Group satellite galaxies DTSTART;VALUE=DATE-TIME:20230323T085500Z DTEND;VALUE=DATE-TIME:20230323T091000Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-211@meetings.aip.de DESCRIPTION:Speakers: Nicolas Garavito Camargo (Flatiron Institute)\nThe v ast multidimensional data observed in the Local Group (LG) provide us with the unique opportunity of comparing the properties of the LG with their s imulated 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 bot h the Milky Way and the Andromeda galaxy\, satellite galaxies are found to be distributed and moving in flattened co-rotating systems. A configurati on that is only found in 0.3-3% of the simulated galaxies. Such disagreeme nt is known as the planes of satellites problem. More intriguing is that t he disagreement is persistent even in different dark matter models and unl ike other 'small-scale problems' it is not sensitive to the inclusion of b aryonic processes in the simulations. \n\nIn this talk\, I would provide n ew evidence of how a natural explanation of the observed co-rotation patte rns are associated with the out-of-equilibrium state of the galaxy. Recen t missions and surveys\, such as Gaia\, have revealed that the Milky Way g alaxy is not in dynamical equilibrium. The barycenter of the galaxy is mov ing due to the ongoing interaction with the Large Magellanic Cloud. Using the Latte hydrodynamical high-resolution zoom-in simulation of MW-like gal axies A massive satellite moves the reference frame of the inner halo wit h respect to the outer halo. Resulting in some cases in apparent co-rotati on motions of the outer halo when observed from the disk of the galaxies. I'll show how the orbital poles distribution of outer halo objects is stro ngly affected during the pericenter passages. I will further discuss what properties of the mergers\, mass ratios\, pericenter passages\, and eccent ricities\, would be needed to reproduce the observational co-rotations pat tern observed in the Milky Way and M31.\n\nThese results provide new insig ht into how the observed co-ration patterns can inform us about the out-of -equilibrium stare of the galaxy. Which is a natural explanation that does not depend on the nature of the Dark Matter particle and in baryonic proc esses. In the talk\, I will also discuss the importance of taking into acc ount the dynamic state of the LG when comparing it with LG analogs in cosm ological simulations.\n\nhttps://iaus379.aip.de/event/20/contributions/211 / LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/211/ END:VEVENT BEGIN:VEVENT SUMMARY:The Mass of the Large Magellanic Cloud DTSTART;VALUE=DATE-TIME:20230322T163000Z DTEND;VALUE=DATE-TIME:20230322T164500Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-205@meetings.aip.de DESCRIPTION:Speakers: Laura Watkins (AURA for ESA\, STScI)\nThe Large Mage llanic 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 interest ing comparison and sufficiently massive to be a major player in the MW's r ecent history and present state. In particular\, it is massive enough to h ave a significant and observable effect on the MW itself and on stellar st reams in the MW halo\, though the extent of its influence depends on its m ass. Its mass is also interesting as a benchmark against which we can inte rpret observations of more distant objects.\n\nBennet et al. (2022) recent ly measured proper motions (PMs) -- using HST\, Gaia or both HST and Gaia together -- for a set of globular clusters (GCs) in the LMC. Supplemented with literature distances and line-of-sight velocities\, this provides a c atalogue of 6D phase space information for 32 LMC GCs. These are ideal dyn amical tracers of the LMC’s potential.\n\nIn my talk\, I will describe h ow we have used this set of tracers to estimate the anisotropy and mass of the LMC within 13 kpc\, and then how we have used these estimates to extr apolate the LMC’s virial mass. This is the first time that this family o f mass estimation methods has been applied to the LMC\, and I will also co mpare our estimate against other estimates of the LMC’s mass via differe nt methods and discuss the broader context of our results.\n\nhttps://iaus 379.aip.de/event/20/contributions/205/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/205/ END:VEVENT BEGIN:VEVENT SUMMARY:Velocity dipoles in the halos of FIRE simulated galaxies DTSTART;VALUE=DATE-TIME:20230323T091600Z DTEND;VALUE=DATE-TIME:20230323T091800Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-273@meetings.aip.de DESCRIPTION:Speakers: Alex Riley (Durham University)\nOne major source of disequilibrium in the Milky Way is its most massive satellite\, the LMC. K inematics of distant halo tracers show a velocity dipole in the Milky Way halo\, which has been interpreted using N-body simulations as the LMC indu cing a reflex motion in the Milky Way disk. In this talk\, I discuss apply ing this framework to more realistic halos comprised of substructure from the FIRE-2 zoom-in cosmological simulations. Velocity dipoles are resolved in Milky Way-mass hosts experiencing an LMC-like interaction and evolve i n a manner consistent with a two-body interaction between the stellar disk and the LMC analog. The magnitude of this dipole can be used to constrain the mass ratio of the Milky Way and LMC. However\, satellite galaxies and stellar streams can create velocity dipoles in systems that aren't experi encing a major satellite accretion\, suggesting that care must be taken to remove substructure in the Milky Way observations.\n\nhttps://iaus379.aip .de/event/20/contributions/273/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/273/ END:VEVENT BEGIN:VEVENT SUMMARY:SMASHing the Small Magellanic Cloud: star formation history DTSTART;VALUE=DATE-TIME:20230323T091400Z DTEND;VALUE=DATE-TIME:20230323T091600Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-272@meetings.aip.de DESCRIPTION:Speakers: Sakowska Joanna (University of Surrey)\nI present wo rk on a spatially resolved\, global star-formation history (SFH) of the Sm all 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 Te lescope. The SFH is quantitatively obtained using colour-magnitude diagram (CMD) fitting techniques. For the first time\, optical depth effects alon g the SMC's line-of-sight are considered in the SFHs derived. \n\nI focus on the SFH of a shell-like structure located in the northeastern part of t he SMC. I compare this SFH to the SFHs of several SMC regions. I discuss t he results of such comparison with a focus on whether the recent and high star formation activity in the shell-like structure is correlated with the enhancements of star formation at young ages in the SMC. Finally\, I put my results in the context of the tidal interactions between the SMC and it s larger companion\, the Large Magellanic Cloud (LMC) to shed light on the origins of the shell-like feature.\n\nhttps://iaus379.aip.de/event/20/con tributions/272/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/272/ END:VEVENT BEGIN:VEVENT SUMMARY:Direct Observations of the Primordial Magellanic Corona DTSTART;VALUE=DATE-TIME:20230323T091200Z DTEND;VALUE=DATE-TIME:20230323T091400Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-271@meetings.aip.de DESCRIPTION:Speakers: Dhanesh Krishnarao (Colorado College)\nRecent measur ements of a high mass for the LMC imply the LMC should host a massive Mage llanic Corona\, a collisionally ionized\, warm-hot gaseous halo at the vir ial temperature $\\sim10^{5.4}$ K initially extending out to the virial ra dius (100 - 130 kpc). Such a primordial Magellanic Corona would have shape d and fed the formation of the Magellanic Stream (e.g. Lucchini et al. 202 0). Now\, we have discovered direct observational evidence for this Magell anic Corona via highly ionized oxygen (O VI)\, and indirect detections via C IV and Si IV\, seen in UV absorption toward background quasars using da ta from HST and FUSE (Krishnarao et al. 2022\, Nature)\, We find the Magel lanic Corona is part of a pervasive multiphase Magellanic CGM seen in many ionization states with a declining projected radial profile out to at lea st 35 kpc from the LMC and a total ionized CGM mass of $10^{(9.1 +/- 0.2)} M_\\odot$. This independently confirms the large mass of the LMC as dynami cally predicted. The evidence for the Magellanic Corona is a crucial step forward in characterizing the Magellanic Group and its nested evolution wi th the Local Group and will help us diagnose the impact of galactic scale winds emerging from star formation feedback in the LMC. In future work fro m an accepted HST Legacy Archival Program (PI: Kat Barger)\, we will direc tly measure and map this galactic scale outflow and the Magellanic Corona using hundreds of sightlines towards stars in the LMC from the ULYSSES pro gram (Roman-Duval et al. 2020).\n\nhttps://iaus379.aip.de/event/20/contrib utions/271/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/271/ END:VEVENT BEGIN:VEVENT SUMMARY:Multiband study of Shell region in the North-Eastern Small Magella nic Cloud using UVIT/AstroSat and Gaia DTSTART;VALUE=DATE-TIME:20230323T091000Z DTEND;VALUE=DATE-TIME:20230323T091200Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-232@meetings.aip.de DESCRIPTION:Speakers: Sipra Hota (Indian Institute of Astrophysics)\nThe S mall Magellanic Cloud (SMC) is one of the nearest\, gas-rich interacting d warf 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 st udy star formation and evolution in a tidally driven environment. The shel l region located in the North-East outskirt of SMC is a tidally affected r egion where there has been recent star formation. Our aim is to understand the spatial distribution\, age dating\, and kinematics of the young popul ation in this part of the tidally affected SMC disk.\nWe obtained far-UV ( FUV) images of eleven fields in the North-East SMC Shell region using the UltraViolet Imaging Telescope (UVIT) on AstroSat. We created science-ready images and performed PSF photometry. We cross-matched the detected FUV st ars with the Gaia EDR3 data and eliminated foreground stars to create an F UV catalog of a few thousand stars. We created FUV-optical color-magnitude diagrams and estimated the ages of the stellar population using isochrone s to map the morphology\, density\, and tidal features of stars younger th an ∼ 600 Myr. The identified episodes of star formation are used to cons train the details of the recent interaction of the SMC with the LMC. We al so estimated the dispersion in the proper motion of the young and old star s to explore the kinematics of the North-East part of the outer SMC disk.\ n\nhttps://iaus379.aip.de/event/20/contributions/232/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/232/ END:VEVENT BEGIN:VEVENT SUMMARY:The Formation of Magellanic System and the total mass of Large Mag ellanic Cloud DTSTART;VALUE=DATE-TIME:20230322T164500Z DTEND;VALUE=DATE-TIME:20230322T170000Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-208@meetings.aip.de DESCRIPTION:Speakers: Jianling WANG (National Astronomical Observatories\, Chinese Academy of Sciences)\nThe Magellanic Stream is unique to sample t he MW potential from ~50kpc to 300\nkpc\, and is also unique in constraini ng the LMC mass\, an increasingly important\nquestion for the Local Group/ Milky Way modeling. I will compare on the\nstrengths and weaknesses of th e two types of models (tidal and ram-pressure) of\nthe Magellanic Stream formation. I will present our modeling for the formation\nof the Magellan ic System\, including those of the most recent discoveries in the\nStream\ , in the Bridge and at the outskirts of Magellanic Clouds. This model has\ nbeen successful in predicting most recent observations in both properties of\nstellar and gas phase. It appears that it is an over-constrained mode l and\nprovides a good path to investigate the Stream properties. In part icular\, this\nmodel requires LMC mass significantly smaller than 10^11 Ms un.\n\nhttps://iaus379.aip.de/event/20/contributions/208/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/208/ END:VEVENT BEGIN:VEVENT SUMMARY:The LMC-induced distortion of the Milky Way (and vice versa) DTSTART;VALUE=DATE-TIME:20230323T084000Z DTEND;VALUE=DATE-TIME:20230323T085500Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-209@meetings.aip.de DESCRIPTION:Speakers: Michael Petersen (University of Edinburgh)\nThe ongo ing interaction of the Large Magellanic Cloud (LMC) and Milky Way (MW) all ows for constraint of the mass (and profile) of both. Through comparison o f 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 barycentr e of the MW at 30 km/s\, as well as inducing a measurable distortion in th e outer halos of both the MW and LMC. These effects emphasise the need to move away from equilibrium models when attempting to measure the mass dist ributions of either. Models for the M33-M31 interaction -- a similar mass ratio -- reveal a markedly different interaction\, with significantly smal ler effects owing to the orbital history.\n\nhttps://iaus379.aip.de/event/ 20/contributions/209/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/209/ END:VEVENT BEGIN:VEVENT SUMMARY:The OC stream's evolution in the dark matter haloes of the Milky W ay and the LMC DTSTART;VALUE=DATE-TIME:20230323T080000Z DTEND;VALUE=DATE-TIME:20230323T082500Z DTSTAMP;VALUE=DATE-TIME:20241114T092403Z UID:indico-contribution-56-178@meetings.aip.de DESCRIPTION:Speakers: Denis Erkal (University of Surrey)\nThe 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$60 kpc)\, givin g us a great tool with which to measure our Galaxy's dark matter halo. In addition\, portions of the stream pass remarkably close to the LMC ($\\sim $5 kpc)\, allowing us to simultaneously measure the properties of our Gala xy and the LMC. By combining data from Gaia DR3 with the S5 survey\, LAMOS T\, SDSS\, and APOGEE\, I will present a 6D view of the stream. In light o f this powerful data\, we fit the OC stream using a flexible model of the Milky Way halo and the LMC. In particular\, we measure the Milky Way's mas s to a precision of 4% in the middle of the stream's radial extent\, $\\si m$2.85$\\times10^{11}M_\\odot$ at $\\sim$32.4 kpc. We also infer a highly flattened dark matter halo of the Milky Way\, with the data preferring an oblate (q = $\\sim$0.55) and prolate (q = $\\sim$1.40) halo over a spheric al one. Interestingly\, we find that both of these haloes are producing a similar forcefield in the orbital plane of the OC stream\, suggesting they may be attempting to mimic a forcefield which cannot be described with by a flattened halo. We also measure the LMC's dark matter halo. In particul ar\, we find the LMC has a mass of $\\sim1.3\\times10^{11} M_\\odot$\, whi ch is one-sixth the Milky Way's virial mass. Our fits also suggest that th e LMC's dark matter halo must extend out to at least $\\sim$53 kpc from th e LMC\, consistent with the LMC being on first approach to the Milky Way. Finally\, we find that the OC stream's close passage with the LMC occurs $ \\sim$300 Myr ago. Since the OC stream is very sensitive to the LMC's loca tion at this time\, this allows us to better constrain the LMC's past orbi t up to that time. For the first time\, we constrain the amount of dynamic al friction the LMC has experienced and find that it is consistent with wh at is expected given the LMC's substantial dark matter halo. I will end wi th the future directions of this work and how these results can be used to constrain alternative gravity and alternative dark matter models.\n\nhttp s://iaus379.aip.de/event/20/contributions/178/ LOCATION:Haus H\, Telegrafenberg URL:https://iaus379.aip.de/event/20/contributions/178/ END:VEVENT END:VCALENDAR