Implications of a Time-varying Galactic Potential for Determinations of the Dynamical Surface Density

Haines, Tim; D’Onghia, Elena; Famaey, Benoît; Laporte, Chervin F. P.; Hernquist, Lars

doi:10.3847/2041-8213/ab25f3

Cited by 39 publications

(40 citation statements)

References 54 publications

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“…Observations of asymmetries in the densities and velocities of stars in the disk show that the disk is likely experiencing vertical oscillations, probably because of the passage of a massive satellite (see e.g. [36,37]). In addition, the Solar System could be placed at an overdense region, compared to the surroundings, and it could also be possible that the baryonic models for gas and dust are incorrect.…”

Section: Estimated Local Dark Matter Densitymentioning

confidence: 99%

On the estimation of the local dark matter density using the rotation curve of the Milky Way

Salas

Malhan

Freese

et al. 2019

J. Cosmol. Astropart. Phys.

139

136

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The rotation curve of the Milky Way is commonly used to estimate the local dark matter density ρDM, . However, the estimates are subject to the choice of the distribution of baryons needed in this type of studies. In this work we explore several Galactic mass models that differ in the distribution of baryons and dark matter, in order to determine ρDM, . For this purpose we analyze the precise rotation curve measurements of the Milky Way up to ∼ 25 kpc from the Galactic centre obtained from Gaia DR2 [1]. We find that the estimated value of ρDM, stays robust to reasonable changes in the spherical dark matter halo. However, we show that ρDM, is affected by the choice of the model for the underlying baryonic components. In particular, we find that ρDM, is mostly sensitive to uncertainties in the disk components of the Galaxy. We also show that, when choosing one particular baryonic model, the estimate of ρDM, has an uncertainty of only about 10% of its best-fit value, but this uncertainty gets much bigger when we also consider the variation of the baryonic model. In particular, the rotation curve method does not allow to exclude the presence of an additional very thin component, that can increase ρDM, by more than a factor of 8. Therefore, we conclude that exclusively using the rotation curve of the Galaxy is not enough to provide a robust estimate of ρDM, . For all the models that we study without the presence of an additional thin component, our resulting estimates of the local dark matter density take values in the range ρDM, 0.3-0.4 GeV/cm 3 , consistent with many of the estimates in the literature.

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Section: Estimated Local Dark Matter Densitymentioning

confidence: 99%

On the estimation of the local dark matter density using the rotation curve of the Milky Way

Salas

Malhan

Freese

et al. 2019

J. Cosmol. Astropart. Phys.

139

136

View full text Add to dashboard Cite

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“…For instance, refs. [101,102] considered the effect of the passage of a heavy object-such as a dwarf galaxy-through the Galactic disc, and ref. [103] showed that vertical breathing mode perturbations can impose systematic errors of the order of 25% in the estimated ρ DM, .…”

Section: Galactic Disequilibriamentioning

confidence: 99%

Dark matter local density determination based on recent observations

Salas

2020

J. Phys.: Conf. Ser.

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The local density of dark matter is an important quantity. On the one hand, its value is needed for dark matter direct detection searches. On the other hand, a precise and robust determination of the local dark matter density would help us learn about the shape of the dark matter halo of our Galaxy, which plays an important role in dark matter indirect detection searches, as well as in many studies in astrophysics and cosmology. There are different methods available to determine the local dark matter density. Among them, it is common to study either the vertical kinematics of a selected group of tracers or the rotation curve of the Milky Way. Recent estimates of the local dark matter density have used the precise observations conducted by the ESA/Gaia mission. However, in spite of the quality of the data released by Gaia's observations, different analyses of the local dark matter density produce dissimilar results. After a brief review of the most common methods to estimate the local density of dark matter, here we argue about different explanations for the discrepancies in the results of recent analyses. We finish by presenting new approaches that have been proposed in the literature and could help us improve our knowledge of this important quantity.

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“…The second data release (DR2) of ESA's Gaia mission has provided the largest available 6D phase-space (positions and velocities) dataset for 7.2 million stars brighter than G RVS = 12 mag (Gaia Collaboration et al 2018b), making possible precise studies of the Milky Way structure and kinematics on large scales. Gaia data have already revealed signatures of nonequilibrium and ongoing vertical phase mixing in the Milky Way disc , likely induced by a previous pericentric passage of the Sagittarius dwarf galaxy Bland-Hawthorn et al 2019;Haines et al 2019) or by inter-Here be dragons, a phrase famous in medieval cartography when dragons and sea monsters used to designate uncharted and possibly dangerous regions. nally driven bending waves (Khoperskov et al 2019;Darling & Widrow 2019).…”

Section: Introductionmentioning

confidence: 99%

Hic sunt dracones: Cartography of the Milky Way spiral arms and bar resonances with Gaia Data Release 2

Khoperskov

Gerhard

Matteo

et al. 2020

A&A

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In this paper we introduce a new method for analysing Milky Way phase-space which allows us to reveal the imprint left by the Milky Way bar and spiral arms in the stars with full phase-space data in Gaia Data Release 2. The unprecedented quality and extended spatial coverage of these data enable us to discover six prominent stellar density structures in the disc to a distance of 5 kpc from the Sun. Four of these structures correspond to the spiral arms detected previously in the gas and young stars (Scutum-Centaurus, Sagittarius, Local and Perseus), while the remaining two are associated with two main resonances of the Milky Way bar. For the first time we provide evidence of the imprint left by spiral arms and resonances in the stellar densities not relying on a specific tracer, through a mean of enhancing the signatures left by these asymmetries. Our method offers new avenues for studying how the stellar populations in our Galaxy are shaped. Article number, page 2 of 10 S. Khoperskov et al.: Hic sunt dracones: Cartography of the Milky Way spiral arms and bar resonances with Gaia Data Release 2 Model I Milky Way -Gaia DR2 Model II

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Implications of a Time-varying Galactic Potential for Determinations of the Dynamical Surface Density

Cited by 39 publications

References 54 publications

On the estimation of the local dark matter density using the rotation curve of the Milky Way

On the estimation of the local dark matter density using the rotation curve of the Milky Way

Dark matter local density determination based on recent observations

Hic sunt dracones: Cartography of the Milky Way spiral arms and bar resonances with Gaia Data Release 2

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