## Thompson, Troland & Heiles (2019) – A Survey of Magnetic Field Strengths in the Envelopes of Molecular Clouds via the 18 cm OH Zeeman Effect

We present the results of an extensive Arecibo observational survey of magnetic field strengths in the inter-core regions of molecular clouds to determine their role in the evolution and collapse

## Green et al. (2019) – A 3D Dust Map Based on Gaia, Pan-STARRS 1 and 2MASS

We present a new three-dimensional map of dust reddening, based on Gaia parallaxes and stellar photometry from Pan-STARRS 1 and 2MASS. This map covers the sky north of a declination

## Peek & Burkhart (2019) – Do Androids Dream of Magnetic Fields? Using Neural Networks to Interpret the Turbulent Interstellar Medium

The interstellar medium (ISM) of galaxies is composed of a turbulent magnetized plasma. In order to quantitatively measure relevant turbulent parameters of the ISM, a wide variety of statistical techniques

## Marchal et al. (2019) – ROHSA: Regularized Optimization for Hyper-Spectral Analysis – Application to phase separation of 21 cm data

Extracting the multiphase structure of the neutral interstellar medium (ISM) is key to understand the star formation in galaxies. The radiative condensation of the diffuse warm neutral medium producing a

## Clark, Peek & Miville-Deschênes (2019) – The Physical Nature of Neutral Hydrogen Intensity Structure

We investigate the physical properties of structures seen in channel map observations of 21 cm neutral hydrogen (H I) emission. H I intensity maps display prominent linear structures that are

## Panopoulou et al. (2019) – Extreme starlight polarization in a region with highly polarized dust emission

Context. Galactic dust emission is polarized at unexpectedly high levels, as revealed by Planck. Aims: The origin of the observed ~=20% polarization fractions can be identified by characterizing the properties

## Zucker et al. (2019) – A Large Catalog of Accurate Distances to Local Molecular Clouds: The Gaia DR2 Edition

We present a uniform catalog of accurate distances to local molecular clouds informed by the Gaia DR2 data release. Our methodology builds on that of Schlafly et al. (2014). First,

## Heiles et al. (2019) – The interstellar medium: the key component in galactic evolution and modern cosmology

The gases of the interstellar medium (ISM) possess orders of magnitude more mass than those of all the stars combined and are thus the prime component of the baryonic Universe.

## González-Casanova, Lazarian & Burkhart (2019) – Velocity centroid gradients for absorbing media

We explore how the velocity gradient technique (VGT) can be applied to absorbing media in the case of 13CO 2-1 emission. The VGT is a new way to trace magnetic

## Körtgen, Federrath & Banerjee (2019) – On the shape and completeness of the column density probability distribution function of molecular clouds

Both observational and theoretical research over the past decade has demonstrated that the probability distribution function (PDF) of the gas density in turbulent molecular clouds is a key ingredient for

## Hanany et al. (2019) – PICO: Probe of Inflation and Cosmic Origins

The Probe of Inflation and Cosmic Origins (PICO) is an imaging polarimeter that will scan the sky for 5 years in 21 frequency bands spread between 21 and 799 GHz.

## Tchernyshyov, Peek & Zasowski (2018) – Kinetic Tomography. II. A Second Method for Mapping the Velocity Field of the Milky Way Interstellar Medium and a Comparison with Spiral Structure Models

In this work, we derive a spatially resolved map of the line-of-sight velocity of the interstellar medium and use it, along with a second map of line-of-sight velocity from Paper

## Mocz & Burkhart (2018) – Star formation from dense shocked regions in supersonic isothermal magnetoturbulence

Supersonic isothermal turbulence establishes a network of transient dense shocks that sweep up material and have a density profile described by balance between ram pressure of the background fluid versus

## Körtgen et al. (2018) – The Origin of Filamentary Star Forming Clouds in Magnetised Galaxies

Observations show that galaxies and their interstellar media are pervaded by strong magnetic fields with energies in the diffuse component being at least comparable to the thermal and even as

## Murray et al. (2018) – Optically Thick H I Does Not Dominate Dark Gas in the Local ISM

The local interstellar medium (ISM) is suffused with “dark” gas, identified by excess infrared and gamma-ray emission, yet undetected by standard ISM tracers such as neutral hydrogen (H I) or

## Nguyen et al. (2018) – Dust-Gas Scaling Relations and OH Abundance in the Galactic ISM

Observations of interstellar dust are often used as a proxy for total gas column density N H. By comparing Planck thermal dust data (Release 1.2) and new dust reddening maps

## Planck Collaboration et al. (2018) – Planck 2018 results. XII. Galactic astrophysics using polarized dust emission

We present 353 GHz full-sky maps of the polarization fraction $p$, angle $\psi$, and dispersion of angles $S$ of Galactic dust thermal emission produced from the 2018 release of Planck

## Clark (2018) – A New Probe of Line-of-sight Magnetic Field Tangling

The Galactic neutral hydrogen (H I ) sky at high Galactic latitudes is suffused with linear structure. Particularly prominent in narrow spectral intervals, these linear H I features are well

## Fissel et al. (2018) – Relative Alignment Between the Magnetic Field and Molecular Gas Structure in the Vela C Giant Molecular Cloud using Low and High Density Tracers

We compare the magnetic field orientation for the young giant molecular cloud Vela C inferred from 500-$\mu$m polarization maps made with the BLASTPol balloon-borne polarimeter to the orientation of structures

## Li et al. (2018) – Where is OH and Does It Trace the Dark Molecular Gas (DMG)?

Hydroxyl (OH) is expected to be abundant in diffuse interstellar molecular gas because it forms along with H2 under similar conditions and forms within a similar extinction range. We have

## Körtgen, Federrath & Banerjee (2017) – The driving of turbulence in simulations of molecular cloud formation and evolution

Molecular clouds are to a great extent influenced by turbulent motions in the gas. Numerical and observational studies indicate that the star formation rate and efficiency crucially depend on the