Charting the Galactic Acceleration Field. I. A Search for Stellar Streams with Gaia DR2 and EDR3 with Follow-up from ESPaDOnS and UVES

Ibata, Rodrigo; Malhan, Khyati; Martín, Nicolás F.; Aubert, Dominique; Famaey, Benoît; Bianchini, P.; Monari, Giacomo; Siebert, A.; Thomas, Guillaume; Bellazzini, M.; Bonifacio, P.; Caffau, E.; Renaud, Florent

doi:10.3847/1538-4357/abfcc2

Cited by 129 publications

(191 citation statements)

References 80 publications

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“…The member stars of these streams are taken from the Ibata et al (2021) catalogue. The streams in this catalogue were detected in the Gaia EDR3 dataset using the STREAMFINDER algorithm Ibata et al 2019).…”

Section: Tangential Velocity Dispersions Of the Milky Way Streamsmentioning

confidence: 99%

“…Specifically for "GD-1", we compare our distance fit with that of its orbit solution, only to ensure that our distance solutions are reliable (the orbit solution is taken from Malhan & Ibata 2019).obtain reliable distance solutions (see below). The parallaxes are corrected for the global parallax zero-point in Gaia EDR3 usingLindegren, Lennart et al (2020) value and the photometry is already corrected for extinction in theIbata et al (2021) catalogue. These streams are shown in Figures2 and 3.To measure σ vTan of these streams, we follow a similar procedure as described in Section 2, with slight modifications in order to deal with the Gaia data.…”

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confidence: 99%

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New constraints on the dark matter density profiles of dwarf galaxies from proper motions of globular cluster streams

Malhan¹,

Valluri²,

Freese³

et al. 2022

Preprint

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The central density profiles in low-mass and dwarf galaxy halos depend strongly on the nature of dark matter. Recently, in Malhan et al. (2021), we employed N-body simulations to show that the cuspy cold dark matter (CDM) subhalos predicted by cosmological simulations can be differentiated from cored subhalos using the properties of accreted globular cluster streams -those stellar streams produced from the tidal stripping of globular clusters that initially evolved within their parent dwarf galaxies and only later merged with the Milky Way. In particular, we previously found that clusters that are accreted within cuspy CDM subhalos produce streams with larger physical widths and higher line-of-sight velocity dispersions as compared to those streams that accrete inside cored subhalos. Here, we use the same suite of simulations to demonstrate that the dispersion in the tangential velocity of streams (σ vTan ) is another parameter that is also sensitive to the central DM density profile of their parent dwarfs. We find that globular clusters that were accreted from cuspy CDM subhalos produce streams with larger σ vTan than those that were accreted inside cored subhalos. Furthermore, we use Gaia EDR3 observations of multiple GC streams to compare their σ vTan values with simulations. This comparison indicates that the five observed streams we analyze are more likely to be associated with globular clusters of 'accreted' rather than 'in situ' origin. We also find evidence that their progenitor globular clusters were probably accreted inside cored DM subhalos (with M subhalo > ∼ 10 8−9 M ).

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Section: Tangential Velocity Dispersions Of the Milky Way Streamsmentioning

confidence: 99%

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confidence: 99%

New constraints on the dark matter density profiles of dwarf galaxies from proper motions of globular cluster streams

Malhan¹,

Valluri²,

Freese³

et al. 2022

Preprint

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“…The Gaia mission (Gaia Collaboration et al 2016) with its exquisite five-dimensional kinematic data and photometric data, has made the discovery of many new streams and of many new features of known streams possible (e.g., Malhan & Ibata 2018;Price-Whelan & Bonaca 2018;Palau & Miralda-Escudé 2019;Starkman et al 2020;Ibata et al 2021). Aside from finding the archetypical cold streams of which many examples were already known before Gaia, the Gaia data in combination with auxiliary data have revealed additional structure associated with known stellar streams, in particular around the GD-1 stream (Grillmair & Dionatos 2006).…”

Section: Comparison To Observationsmentioning

confidence: 99%

The structure of accreted stellar streams

Qian,

Arshad,

Bovy

2022

Preprint

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Many of the Milky Way's globular clusters are likely accreted from satellite galaxies that have long since merged with the Milky Way. When these globular clusters are susceptible to tidal disruption, this process likely starts already inside the parent satellite leading to an early stellar stream within the satellite. When the parent satellite merges with the Milky Way, the globular cluster and its pre-merger stellar stream are accreted in a somewhat chaotic process. Here, we investigate the properties of the accreted stream after the merger as we would see it today using a suite of simulations of accretion events. We find that the accretion process leads to a wide range of behaviors, but generally scatters the accreted stream over a wide, two-dimensional area of the sky. The behavior ranges from a set of a few or more well-defined "sub-streams" extending out from the post-merger thin stream by tens of degrees, to more widely dispersed debris over much of the sky, depending on how close to the center of the Milky Way the merger happened. Using mock Gaia-like observations of the simulated streams, we demonstrate that an accreted-stream component can explain the off-track features observed in the GD-1 stream. Sub-streams can appear like thin tidal streams themselves that are seemingly unassociated with the post-merger stream, raising the possibility that some of the progenitor-less streams observed in the Milky Way are part of a single or a few accreted streams created in an ancient merger event.

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“…Observations of stellar streams (e.g. Ibata et al 2019Ibata et al , 2021Bonaca et al 2021) and of tidal tails around GCs (e.g. Shipp et al 2020) emphasize the critical role that the galactic environment plays in their disruption.…”

Section: Introductionmentioning

confidence: 99%

Introducing EMP-Pathfinder: modelling the simultaneous formation and evolution of stellar clusters in their host galaxies

Reina-Campos,

Keller,

Kruijssen

et al. 2022

Preprint

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The formation and evolution of stellar clusters is intimately linked to that of their host galaxies. To study this connection, we present the EMP-Pathfinder suite of cosmological zoom-in Milky Way-mass simulations. These simulations contain a sub-grid description for stellar cluster formation and evolution, allowing us to study the simultaneous formation and evolution of stellar clusters alongside their host galaxies across cosmic time. As a key ingredient in these simulations, we include the physics of the multi-phase nature of the interstellar medium (ISM), which enables studies of how the presence of a cold, dense ISM affects cluster formation and evolution. We consider two different star formation prescriptions: a constant star formation efficiency per free-fall time, as well as an environmentally-dependent, turbulence-based prescription. We identify two key results drawn from these simulations. Firstly, we find that tidal shock-driven disruption caused by the graininess of the cold ISM produces old (𝜏 > 10 Gyr) stellar cluster populations with properties that are in excellent agreement with the observed populations in the Milky Way and M31. Importantly, the addition of the cold ISM addresses the areas of disagreement found in previous simulations that lacked the cold gas phase. Secondly, the formation of stellar clusters is extremely sensitive to the baryonic physics that govern the properties of the cold, dense gas reservoir in the galaxy. This implies that the demographics of stellar cluster populations represent an important diagnostic tool for constraining baryonic physics models in upcoming galaxy formation simulations that also include a description of the cold ISM.

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Charting the Galactic Acceleration Field. I. A Search for Stellar Streams with Gaia DR2 and EDR3 with Follow-up from ESPaDOnS and UVES

Cited by 129 publications

References 80 publications

New constraints on the dark matter density profiles of dwarf galaxies from proper motions of globular cluster streams

New constraints on the dark matter density profiles of dwarf galaxies from proper motions of globular cluster streams

The structure of accreted stellar streams

Introducing EMP-Pathfinder: modelling the simultaneous formation and evolution of stellar clusters in their host galaxies

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