High-resolution Spectroscopy of the GD-1 Stellar Stream Localizes the Perturber near the Orbital Plane of Sagittarius

Bonaca, Ana; Conroy, Charlie; Hogg, David W.; Cargile, Phillip A.; Caldwell, Nelson; Naidu, Rohan P.; Price-Whelan, Adrian M.; Speagle, Joshua S.; Johnson, Benjamin D.

doi:10.3847/2041-8213/ab800c

Cited by 49 publications

(38 citation statements)

References 52 publications

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“…This has been previously established for GD-1(Malhan & Ibata 2019;Bonaca et al 2020), Fjörm(Palau & Miralda-Escudé 2019), Gjöll(Palau & Miralda-Escudé 2021), and tentatively for Sylgr(Roederer & Gnedin 2019) and Phlegethon(Ibata et al 2018). …”

supporting

confidence: 71%

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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supporting

confidence: 71%

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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“…This property makes stellar streams superb probes of the underlying gravitational potential, allowing us to constrain the mass distribution within the extent of their orbits (Johnston et al 1999). In addition, density variations and gaps within a stream can potentially provide information about past encounters with small-scale substructure and therefore an opportunity to detect the presence of dark matter subhaloes (Carlberg et al 2012;Erkal et al 2017;Bonaca et al 2019;Banik & Bovy 2019;Bonaca et al 2020).…”

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confidence: 99%

Galactic potential constraints from clustering in action space of combined stellar stream data

Reino

Rossi

Sanderson

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Stream stars removed by tides from their progenitor satellite galaxy or globular cluster act as a group of test particles on neighboring orbits, probing the gravitational field of the Milky Way. While constraints from individual streams have been shown to be susceptible to biases, combining several streams from orbits with various distances reduces these biases. We fit a common gravitational potential to multiple stellar streams simultaneously by maximizing the clustering of the stream stars in action space. We apply this technique to members of the GD-1, Pal 5, Orphan and Helmi streams, exploiting both the individual and combined data sets. We describe the Galactic potential with a Stäckel model, and vary up to five parameters simultaneously. We find that we can only constrain the enclosed mass, and that the strongest constraints come from the GD-1, Pal 5 and Orphan streams whose combined data set yields $M(< 20\ \mathrm{kpc}) = 2.96^{+0.25}_{-0.26} \times 10^{11} \ M_{\odot }$. When including the Helmi stream in the data set, the mass uncertainty increases to $M(< 20\ \mathrm{kpc}) = 3.12^{+3.21}_{-0.46} \times 10^{11} \ M_{\odot }$.

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“…Strigari et al 2007;Pieri, Bertone & Branchini 2008;Hayashi et al 2016;Hiroshima, Ando & Ishiyama 2018;Delos 2019;Facchinetti, Lavalle & Stref 2020;Rico 2020;Somalwar et al 2021), and gaps in stellar streams (e.g. Carlberg 2012; Ngan & Carlberg 2014;Erkal et al 2016;Bonaca et al 2020;Necib et al 2020), among other approaches. Since satellite galaxies are inferred to live within subhaloes, with their respective properties related via the galaxy-halo connection, DM substructure statistics are intimately connected to satellite galaxy abundances (e.g.…”

mentioning

confidence: 99%

The tidal evolution of dark matter substructure – II. The impact of artificial disruption on subhalo mass functions and radial profiles

Green

Bosch

Jiang

2021

Monthly Notices of the Royal Astronomical Society

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Several recent studies have indicated that artificial subhalo disruption (the spontaneous, non-physical disintegration of a subhalo) remains prevalent in state-of-the-art dark matter-only cosmological simulations. In order to quantify the impact of disruption on the inferred subhalo demographics, we augment the semi-analytical SatGen dynamical subhalo evolution model with an improved treatment of tidal stripping that is calibrated using the DASH database of idealized high-resolution simulations of subhalo evolution, which are free from artificial disruption. We also develop a model of artificial disruption that reproduces the statistical properties of disruption in the Bolshoi simulation. Using this framework, we predict subhalo mass functions (SHMFs), number density profiles, and substructure mass fractions and study how these quantities are impacted by artificial disruption and mass resolution limits. We find that artificial disruption affects these quantities at the $10-20\%$ level, ameliorating previous concerns that it may suppress the SHMF by as much as a factor of two. We demonstrate that semi-analytical substructure modeling must include orbit integration in order to properly account for splashback haloes, which make up roughly half of the subhalo population. We show that the resolution limit of N-body simulations, rather than artificial disruption, is the primary cause of the radial bias in subhalo number density found in dark matter-only simulations. Hence, we conclude that the mass resolution remains the primary limitation of using such simulations to study subhaloes. Our model provides a fast, flexible, and accurate alternative to studying substructure statistics in the absence of both numerical resolution limits and artificial disruption.

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High-resolution Spectroscopy of the GD-1 Stellar Stream Localizes the Perturber near the Orbital Plane of Sagittarius

Cited by 49 publications

References 52 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

Galactic potential constraints from clustering in action space of combined stellar stream data

The tidal evolution of dark matter substructure – II. The impact of artificial disruption on subhalo mass functions and radial profiles

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