Unsolved Mysteries of High-velocity Clouds

Benjamin, Robert A.

doi:10.1007/1-4020-2579-3_17

Cited by 3 publications

(1 citation statement)

References 90 publications

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“…The thick navy posterior labeled "All" is the same as the navy posterior in Figures 8 and 9. metals, such as Mg II and Fe II, into clouds should also inject dust (Wakker 2001;Benjamin 2005). Constraints on the dust content of the Magellanic Stream can thus have important implications for dust survival and destruction in the Stream environment.…”

Section: Polarized Dust In Magellanic Stream Imentioning

confidence: 99%

BICEP/Keck. XVI. Characterizing Dust Polarization through Correlations with Neutral Hydrogen

Ade

Ahmed

Amiri

et al. 2023

ApJ

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We characterize Galactic dust filaments by correlating BICEP/Keck and Planck data with polarization templates based on neutral hydrogen (H i) observations. Dust polarization is important for both our understanding of astrophysical processes in the interstellar medium (ISM) and the search for primordial gravitational waves in the cosmic microwave background (CMB). In the diffuse ISM, H i is strongly correlated with the dust and partly organized into filaments that are aligned with the local magnetic field. We analyze the deep BICEP/Keck data at 95, 150, and 220 GHz, over the low-column-density region of sky where BICEP/Keck has set the best limits on primordial gravitational waves. We separate the H i emission into distinct velocity components and detect dust polarization correlated with the local Galactic H i but not with the H i associated with Magellanic Stream i. We present a robust, multifrequency detection of polarized dust emission correlated with the filamentary H i morphology template down to 95 GHz. For assessing its utility for foreground cleaning, we report that the Hi morphology template correlates in B modes at a ∼10%–65% level over the multipole range 20 < ℓ < 200 with the BICEP/Keck maps, which contain contributions from dust, CMB, and noise components. We measure the spectral index of the filamentary dust component spectral energy distribution to be β = 1.54 ± 0.13. We find no evidence for decorrelation in this region between the filaments and the rest of the dust field or from the inclusion of dust associated with the intermediate velocity H i. Finally, we explore the morphological parameter space in the H i-based filamentary model.

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Section: Polarized Dust In Magellanic Stream Imentioning

confidence: 99%

BICEP/Keck. XVI. Characterizing Dust Polarization through Correlations with Neutral Hydrogen

Ade

Ahmed

Amiri

et al. 2023

ApJ

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High-Velocity Clouds

Wakker

Woerden

2013

Planets, Stars and Stellar Systems

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The Smith Cloud: A High-Velocity Cloud Colliding with the Milky Way

Lockman¹,

Benjamin²,

Heroux³

et al. 2008

ApJ

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101

163

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New 21cm H I observations made with the Green Bank Telescope show that the high-velocity cloud known as Smith's Cloud has a striking cometary appearance and many indications of interaction with the Galactic ISM. The velocities of interaction give a kinematic distance of 12.4 ± 1.3 kpc, consistent with the distance derived from other methods. The Cloud is > 3 × 1 kpc in size and its tip at (ℓ, b) ≈ 39 • − 13 • is 7.6 kpc from the Galactic center and 2.9 kpc below the Galactic plane. It has > 10 6 M ⊙ in H I. Its leading section has a total space velocity near 300 km s −1 , is moving toward the Galactic plane with a velocity of 73 ± 26 km s −1 , and is shedding material to the Galaxy. In the absence of drag the Cloud will cross the plane in about 27 Myr. Smith's Cloud may be an example of the accretion of gas by the Milky Way needed to explain certain persistant anomalies in Galactic chemical evolution.

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Unsolved Mysteries of High-velocity Clouds

Cited by 3 publications

References 90 publications

BICEP/Keck. XVI. Characterizing Dust Polarization through Correlations with Neutral Hydrogen

BICEP/Keck. XVI. Characterizing Dust Polarization through Correlations with Neutral Hydrogen

High-Velocity Clouds

The Smith Cloud: A High-Velocity Cloud Colliding with the Milky Way

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