Press & Media
A bubble in the Brick
Press release: 17/12/2021: https://www.mpia.de/news/science/2021-17-the-brick
Image credit: J. D. Henshaw/MPIA
Publication: "A wind-blown bubble in the Central Molecular Zone cloud G0.253+0.016", J. D. Henshaw, M. R. Krumholz, N. O. Butterfield, J. Mackey, A. Ginsburg, T. J. Haworth, F. Nogueras-Lara, A. T. Barnes, S. N. Longmore, J. Bally, J. M. D. Kruijssen, E. A. C. Mills, H. Beuther, D. L. Walker, C. Battersby, A. Bulatek, T. Henning, J. Ott, J. D. Soler, MNRAS, 2021, DOI: 10.1093/mnras/stab3039
Enigmatic cloud near the Galactic Centre may be richer in young stars than previously thought
A group of astronomers led by the Max Planck Institute for Astronomy found evidence for a young stellar cluster hidden inside a cloud known as “the Brick”. This cloud near the Galactic Centre so far appeared unusually quiescent regarding star formation. The new finding follows from an arc-shaped substructure whose properties are consistent with an expanding shell. The authors link it to a bubble of hot gas produced by the stellar wind of a young massive star. Since massive stars rarely form in isolation, the bubble could indicate the presence of a young stellar cluster, equivalent to several hundred solar masses.
Stars form inside dense pockets of clouds made of gas and dust. Generally, whenever a cloud is dense enough, stars will eventually form. However, this rule of thumb does not appear to hold entirely for the region around the Milky Way centre. The Central Molecular Zone (CMZ), a gas complex with a diameter between 1000 and 2000 light-years around the Galactic Centre, contains some of the densest and most massive gas clouds known in the Milky Way. However, apart from a few extraordinarily massive stellar clusters, many of those clouds show surprisingly little evidence of widespread star formation activity.
To explore this apparent contradiction, a group of astronomers led by Jonathan Henshaw from the Max Planck Institute for Astronomy (MPIA) in Heidelberg, Germany, investigated one of the most enigmatic clouds in the CMZ, called “the Brick”. It is well known for its high density and mass, equivalent to about 100,000 suns. Still, it appears to produce comparatively few stars.
“When investigating the gas motion of the Brick, we find one component that stands out,” says Jonathan Henshaw. He is the lead author of the underlying article published in the Monthly Notices of the Royal Astronomical Society. “That sub-structure, confined to a narrow range of velocities, resembles a crescent-shaped arc,” Henshaw adds.
Such arcs have been detected in regions of high-mass star formation. They can represent the material swept up by an expanding shell. High-mass stars deliver energy and momentum to their surroundings, which act as the driving force of the expansion. Based on this assumption, the research group derived a shell diameter of 8.5 light-years and an expansion velocity of approximately 5 kilometres per second. By tracing this motion back to its origin, the astronomers dated the beginning of the expansion back to a few hundred thousand years ago. This is just a wink of an eye, considering the timescales typical of cosmic phenomena.
"A wind-blown bubble in the Central Molecular Zone cloud G0.253+0.016",
J. D. Henshaw, M. R. Krumholz, N. O. Butterfield, J. Mackey, A. Ginsburg, T. J. Haworth, F. Nogueras-Lara, A. T. Barnes, S. N. Longmore, J. Bally, J. M. D. Kruijssen, E. A. C. Mills, H. Beuther, D. L. Walker, C. Battersby, A. Bulatek, T. Henning, J. Ott, J. D. Soler, MNRAS, 2021, DOI: 10.1093/mnras/stab3039
The team consists of J. D. Henshaw (Max Planck Institute for Astronomy, Heidelberg, Germany [MPIA]), M. R. Krumholz (MPIA; Australian National University, Canberra, Australia; ARC Centre of Excellence for Astronomy in Three Dimensions, Canberra, Australia; ZAH, Universität Heidelberg, Germany), N. O. Butterfield (Villanova University, USA), J. Mackey (Dublin Institute for Advanced Studies, Ireland), A. Ginsburg (University of Florida, Gainesville, USA [UFL]), T. J. Haworth (Queen Mary University of London, UK), F. Nogueras-Lara (MPIA), A. T. Barnes (Universität Bonn, Germany), S. N. Longmore (Liverpool John Moores University, UK), J. Bally (University of Colorado, USA), J. M. D. Kruijssen (ARI, Universität Heidelberg, Germany), E. A. C. Mills (University of Kansas, Lawrence, USA), H. Beuther (MPIA), D. L. Walker (University of Connecticut, Storrs, USA [UCONN]), C. Battersby (UCONN), A. Bulatek (UFL), T. Henning (MPIA), J. Ott (National Radio Astronomy Observatory, Socorro, USA; New Mexico Institute of Mining and Technology, Socorro, USA), and J. D. Soler (MPIA; Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica, Rome, Italy).
The cosmic commute towards star and planet formation
Press release: 29/06/2020: https://www.mpg.de/en/mpia/2020-08-cosmic-commute
Image credit: T. Müller/J. Henshaw/MPIA
Publication: "Ubiquitous velocity fluctuations throughout the molecular interstellar medium", J. D. Henshaw, J. M. D. Kruijssen, S. N. Longmore, M. Riener, A. K. Leroy, E. Rosolowsky, A. Ginsburg, C. Battersby, M. Chevance, S. E. Meidt, S. C. O. Glover, A. Hughes, J. Kainulainen, R. S. Klessen, E. Schinnerer, A. Schruba, H. Beuther, F. Bigiel, G. A. Blanc, E. Emsellem, T. Henning, C. N. Herrera, E. W. Koch, J. Pety, S. E. Ragan, J. Sun, Nature Astronomy, in press
Interconnected gas flows reveal how star-forming gas is assembled in galaxies
The molecular gas in galaxies is organised into a hierarchy of structures. The molecular material in giant molecular gas clouds travels along intricate networks of filamentary gas lanes towards the congested centres of gas and dust where it is compressed into stars and planets, much like the millions of people commuting to cities for work around the world. To better understand this process, a team of astronomers led by Jonathan Henshaw at Max Planck Institute for Astronomy (MPIA) have measured the motion of gas flowing from galaxy scales down to the scales of the gas clumps within which individual stars form. Their results show that the gas flowing through each scale is dynamically interconnected: while star and planet formation occurs on the smallest scales, this process is controlled by a cascade of matter flows that begin on galactic scales. These results are published today in the scientific journal Nature Astronomy.
The molecular gas in galaxies is set into motion by physical mechanisms such as galactic rotation, supernova explosions, magnetic fields, turbulence, and gravity, shaping the structure of the gas. Understanding how these motions directly impact star and planet formation is difficult because it requires quantifying gas motion over a huge range in spatial scale, and then linking this motion to the physical structures we observe. Modern astrophysical facilities now routinely map huge areas of the sky, with some maps containing millions of pixels, each with hundreds to thousands of independent velocity measurements. As a result, measuring these motions is both scientifically and technologically challenging.
In order to address these challenges, an international team of researchers led by Jonathan Henshaw at the MPIA in Heidelberg set out to measure gas motions throughout a variety of different environments using observations of the gas in the Milky Way and a nearby galaxy. They detect these motions by measuring the apparent change in the frequency of light emitted by molecules caused by the relative motion between the source of the light and the observer; a phenomenon known as the Doppler effect. By applying novel software designed by Henshaw and Ph.D. student Manuel Riener (a co-author on the paper; also at MPIA), the team were able to analyse millions of measurements. “This method allowed us to visualise the interstellar medium in a new way,” says Henshaw.
The researchers found that cold molecular gas motions appear to fluctuate in velocity, reminiscent in appearance of waves on the surface of the ocean. These fluctuations represent gas motion. “The fluctuations themselves weren’t particularly surprising, we know that the gas is moving,” says Henshaw. Steve Longmore, co-author of the paper, based at Liverpool John Moores University, adds, “What surprised us was how similar the velocity structure of these different regions appeared. It didn’t matter if we were looking at an entire galaxy or an individual cloud within our own galaxy, the structure is more or less the same”.
To better understand the nature of the gas flows, the team selected several regions for close examination, using advanced statistical techniques to look for differences between the fluctuations. By combining a variety of different measurements, the researchers were able to determine how the velocity fluctuations depend on the spatial scale.
“A neat feature of our analysis techniques is that they are sensitive to periodicity,” explains Henshaw. “If there are repeating patterns in your data, such as equally spaced giant molecular clouds along a spiral arm, we can directly identify the scale on which the pattern repeats.” The team identified three filamentary gas lanes, which, despite tracing vastly different scales, all seemed to show structure that was roughly equidistantly spaced along their crests, like beads on a string, whether it was giant molecular clouds along a spiral arm or tiny “cores” forming stars along a filament.
The team discovered that the velocity fluctuations associated with equidistantly spaced structure all showed a distinctive pattern. “The fluctuations look like waves oscillating along the crests of the filaments, they have a well-defined amplitude and wavelength,” says Henshaw adding, “The periodic spacing of the giant molecular clouds on large-scales or individual star-forming cores on small-scales is probably the result of their parent filaments becoming gravitationally unstable. We believe that these oscillatory flows are the signature of gas streaming along spiral arms or converging towards the density peaks, supplying new fuel for star formation.”
In contrast, the team found that the velocity fluctuations measured throughout giant molecular clouds, on scales intermediate between entire clouds and the tiny cores within them, show no obvious characteristic scale. Diederik Kruijssen, co-author of the paper based at Heidelberg University explains: “The density and velocity structures that we see in giant molecular clouds are ‘scale-free’, because the turbulent gas flows generating these structures form a chaotic cascade, revealing ever smaller fluctuations as you zoom in – much like a Romanesco broccoli, or a snowflake. This scale-free behaviour takes place between two well-defined extremes: the large scale of the entire cloud, and the small scale of the cores forming individual stars. We now find that these extremes have well-defined characteristic sizes, but in between them chaos rules.”
“Picture the giant molecular clouds as equally-spaced mega-cities connected by highways,” says Henshaw. “From a birds eye view, the structure of these cities, and the cars and people moving through them, appears chaotic and disordered. However, when we zoom in on individual roads, we see people who have travelled from far and wide entering their individual office buildings in an orderly fashion. The office buildings represent the dense and cold gas cores from which stars and planets are born."
"Ubiquitous velocity fluctuations throughout the molecular interstellar medium",
J. D. Henshaw, J. M. D. Kruijssen, S. N. Longmore, M. Riener, A. K. Leroy, E. Rosolowsky, A. Ginsburg, C. Battersby, M. Chevance, S. E. Meidt, S. C. O. Glover, A. Hughes, J. Kainulainen, R. S. Klessen, E. Schinnerer, A. Schruba, H. Beuther, F. Bigiel, G. A. Blanc, E. Emsellem, T. Henning, C. N. Herrera, E. W. Koch, J. Pety, S. E. Ragan, J. Sun, Nature Astronomy, in press
This study was published under the title "Ubiquitous velocity fluctuations throughout the molecular interstellar medium" in the journal Nature Astronomy. Besides the main author Jonathan D. Henshaw, 25 people from 21 research institutes from 8 countries are involved in the publication. Of these, Jonathan D. Henshaw, Manuel Riener, Eva Schinnerer, Henrik Beuther and Thomas Henning are conducting research at MPIA.
The center of our Milky Way galaxy lies about 27,000 light-years away in the direction of the constellation of Sagittarius. At its core is a black hole about four million solar masses in size. Around the black hole is a donut-shaped structure about eight light-years across that rings the inner volume of neutral gas and thousands of individual stars. Around that, stretching out to about 700 light-years, is a dense zone of activity called the Central Molecular Zone (CMZ). It contains almost eighty percent of all the dense gas in the galaxy - a reservoir of tens of millions of solar masses of material - and hosts giant molecular clouds and massive star forming clusters of luminous stars, among other regions many of which are poorly understood. For example, the CMZ contains many dense molecular clouds that would normally be expected to produce new stars, but which are instead eerily desolate. It also contains gas moving at highly supersonic velocities - hundreds of kilometers per second (hundreds of thousands of miles per hours).
Where did the CMZ come from? No place else in the Milky Way is remotely like it (although there may be analogues in other galaxies). How does it retain its structure as its molecular gas moves, and how do those rapid motions determine its evolution? One difficulty facing astronomers is that there is so much obscuring dust between us and the CMZ that visible light is extinguished by factors of over a trillion. Infrared, radio, and some X-ray radiation can penetrate the veil, however, and they have allowed astronomers to develop the picture just outlined.
CfA astronomers Cara Battersby, Dan Walker, and Qizhou Zhang, with their team of colleagues, used the Australian Mopra radio telescope to study the three molecules HNCO, N2H+, and HNC in the CMZ. These particular molecules were selected because they do a good job of tracing the wide range of conditions thought to be present in the CMZ, from shocked gas to quiescent material, and also because they suffer only minimally from cluttering and extinction effects that complicate more abundant species like carbon monoxide. The scientists developed a new computer code to analyze efficiently the large amounts of data they had.
The astronomers find, consistent with previous results, that the CMZ is not centered on the black hole, but (for reasons that are not understood) is offset; they also confirm that the gas motions throughout are supersonic. They identify two large-scale flows across the region, and suggest they represent one coherent (or at most two independent) streams of material, perhaps even spiral-like arms. They also analyze the gas in several previously identified zones of the CMZ, finding that one shell-like region thought to be the result of supernova explosions may instead be several regions that are physically unrelated, and that a giant cloud thought to be independent is actually an extension of the large-scale flows. The scientists note that this work is a first step in unraveling an intrinsically complex galactic environment, and that pending research will trace the gas motions to larger distances and try to model the CMZ gas motions with computer simulations.
"Molecular gas kinematics within the central 250 pc of the Milky Way,"
J. D. Henshaw, S. N. Longmore, J. M. D. Kruijssen, B. Davies, J. Bally,. Barnes, C. Battersby, M. Burton, M. R. Cunningham, J. E. Dale, A. Ginsburg, K. Immer, P. A. Jones, S. Kendrew, E. A. C. Mills, S. Molinari, T. J. T. Moore, J. Ott, T. Pillai, J. Rathborne, P. Schilke, A. Schmiedeke, L. Testi, D. Walker, A. Walsh and Q. Zhang, MNRAS, 2016, 457, 2675.