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HL Tau

The exciting results of the highest-resolution test campaign yet attempted by the Atacama Large Millimeter/submillimeter Array (ALMA) are detailed in a recent set of four papers.

Juno

Animation (click to watch) of the asteroid Juno as seen in mm wavelengths by ALMA’s Long Baseline Campaign. Image credit: ALMA (NRAO/ESO/NAOJ)

ALMA’s array of antennas can be configured so that the baseline of the simulated telescope is as small as 150 m or as large as 15 km across. In its smaller configurations, ALMA studies the large-scale structure of cold objects in the Universe — and this is how the array has been used since it began its first operations in 2011. But now ALMA has begun to test its long-baseline configuration, in which it is able to make its highest-resolution observations and study the small-scale structure of objects in detail.

The Targets

ALMA’s Long Baseline Campaign, run in late 2014, observed five science targets using 22–36 antennas arranged with a baseline of up to the full 15 km. The targets were selected to push the limits of ALMA’s capabilities: each target has a small angular size (less than two arcseconds) with fine-scale structure that is largely unresolved in previous observations. Two of the targets, the variable star Mira and the active galaxy 3C138, were primarily used for calibration and comparisons of ALMA data to those of other telescopes. The remaining three targets not only demonstrated ALMA’s capabilities, but also resulted in new science discoveries.

SDP.81

ALMA’s highest resolution observation yet, of the gravitationally lensed galaxy SDP.81. The maximum resolution of this image is 23 milliarcseconds. Image credit: ALMA (NRAO/ESO/NAOJ); B. Saxton NRAO/AUI/NSF

  • Juno is one of the largest asteroids in our solar system’s main asteroid belt. ALMA’s observations of Juno were made when the asteroid was approximately 295 million km from Earth, and the ten images ALMA took have been stitched together into a brief animation that show the asteroid tumbling through space as it orbits the Sun. The resolution of these images — enough to study the shape and even some surface features of the asteroid! — are unprecedented for this wavelength.
  • HL Tau is a young star surrounded by a protoplanetary disk. ALMA’s detailed observations of this region revealed remarkable structure within the disk: a series of light and dark concentric rings indicative of planets caught in the act of forming. Studying this system will help us understand how multi-planet solar systems like our own form and evolve.
  • The star-forming galaxy SDP.81 — located so far away that the light we see was emitted when the Universe was only 15% of its current age — is gravitationally-lensed into a cosmic arc, due to the convenient placement of a nearby foreground galaxy. The combination of the lucky alignment and ALMA’s high resolution grant us a spectacularly detailed view of this distant galaxy, allowing us to study its actual shape and the motion within it.

The observations from ALMA’s first test of its long baseline demonstrate that ALMA is capable of doing the transformational science it promised. As we gear up for the next cycle of observations, it’s clear that exciting times are ahead!

Citation:

ALMA Partnership et al. 2015 ApJ 808 L1, L2, L3 and L4. Focus on the ALMA Long Baseline Campaign

core collapse simulation

What happens at the very end of a massive star’s life, just before its core’s collapse? A group led by Sean Couch (California Institute of Technology and Michigan State University) claim to have carried out the first three-dimensional simulations of these final few minutes — revealing new clues about the factors that can lead a massive star to explode in a catastrophic supernova at the end of its life.

A Giant Collapses

In dying massive stars, in-falling matter bounces off the of collapsed core, creating a shock wave. If the shock wave loses too much energy as it expands into the star, it can stall out — but further energy input can revive it and result in a successful explosion of the star as a core-collapse supernova.

In simulations of this process, however, theorists have trouble getting the stars to consistently explode: the shocks often stall out and fail to revive. Couch and his group suggest that one reason might be that these simulations usually start at core collapse assuming spherical symmetry of the progenitor star.

Adding Turbulence

Couch and his collaborators suspect that the key is in the final minutes just before the star collapses. Models that assume a spherically-symmetric star can’t include the effects of convection as the final shell of silicon is burned around the core — and those effects might have a significant impact!

To test this hypothesis, the group ran fully 3D simulations of the final three minutes of the life of a 15 solar-mass star, ending with core collapse, bounce, and shock-revival. The outcome was striking: the 3D modeling introduced powerful turbulent convection (with speeds of several hundred km/s!) in the last few minutes of silicon-shell burning. As a result, the initial structure and motions in the star just before core collapse were very different from those in core-collapse simulations that use spherically-symmetric initial conditions. The turbulence was then further amplified during collapse and formation of the shock, generating pressure that aided the shock expansion — which should ultimately help the star explode!

The group cautions that their simulations are still very idealized, but these results clearly indicate that the 3D structure of massive stellar cores has an important impact on the core-collapse supernova mechanism.

Citation

Sean M. Couch et al. 2015 ApJ 808 L21 doi:10.1088/2041-8205/808/1/L21

Asteroid Itokawa

Recent observations of asteroid (335433) 2005 UW163 have added a new member to the mysterious category of “super-fast rotators” — asteroids that rotate faster than should be possible, given current theories of asteroid composition.

Asteroids come in sizes of a few meters to a few hundred kilometers, and can spin at rates from 0.1 to nearly 1000 revolutions per day. Current theories suggest that asteroids smaller than 150m are mostly monolithic (made up of a single rock), whereas asteroids larger than 150m are usually what’s known as a “rubble pile” — a collection of rock fragments from past collisions, bound together into a clump by gravity. “Rubble pile” asteroids have an important structural limitation: they can’t spin faster than once every 2.2 hours without flying apart as the centripetal force overcomes the force of gravity.

Asteroid 2005 UW163 violates this rule: its diameter is 690m, but it rotates once every 1.29 hours. This discovery was made by a team of scientists using telescopes at the Palomar Observatory in California to conduct a large survey of the rotation rates of nearby asteroids. The group, led by Chan-Kao Chang of Taiwan’s National Central University, discovered 11 super-fast rotator candidates — of which asteroid 2005 UW163 is the first to have its rotation rate confirmed by additional observations.

The category of super-fast rotators poses an interesting problem: how are they able to spin so quickly without flying apart? Either the density of these asteroids is unexpectedly high (roughly four times the density of typical “rubble pile” asteroids), or else there must be additional forces besides gravity at work to help hold the asteroid together, such as bonds between the rocks. Future observations of super-fast rotators will help us better understand the peculiar structure of these rocky neighbors.

Citation:

Chan-Kao Chang et al. 2014 ApJ 791 L35 doi:10.1088/2041-8205/791/2/L35

Protoplanetary disk

A team of scientists led by Catherine Walsh (Leiden Observatory) has found evidence of two planets orbiting a young, hot star located relatively nearby, at just 335 light years from Earth. The star, HD 100546, is surrounded by a disk of gas and dust — which is a prime environment for forming planets. Previous observations have hinted at two planets potentially hiding in this disk, but directly imaging planets in disks is very difficult. Walsh’s team took a different approach to finding these subtle planets: rather than looking for them directly, the group instead looked for gaps in the dust of the disk.

The team examined the signature of dust particles in the disk around HD 100546 using observations from the Atacama Large Millimeter/Submillimeter Array (ALMA), a telescope located in Chile. They found that rather than forming a solid disk, the dust particles have settled into two nested rings with a gap between them. That gap is telltale evidence of a planet: planets embedded in disks tend to clear out a path as they orbit, accreting the gas and dust onto themselves.

Walsh’s team followed up the discovery by using different models of planetary formation to try to reproduce ALMA’s observations. They found that the best model required there to be two planets in HD 100546’s system: one located very close to the star, and a second, newly-forming planet located within the disk gap.

This model is consistent with previous estimates of where the two suspected planets might be located, which is promising news for exoplanet enthusiasts. HD 100546 could be our first opportunity to study a planet caught in the act of forming — which is an important step toward understanding how planets are created out of disks around young stars.

Citation:

Catherine Walsh et al. 2014 ApJ 791 L6 doi:10.1088/2041-8205/791/1/L6

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