For three years, Jenny Calahan led fellow undergraduate students at the University of Arizona (UA) in research to help unravel the mystery of how the galaxy’s most massive stars are born. On 23 July 2018, just two months after Calahan graduated with a bachelor’s degree in physics and astronomy, the resulting research paper, “Searching for Inflow Towards Massive Starless Clump Candidates Identified in the Bolocam Galactic Plane Survey,” was published in the Astrophysical Journal. Her co-authors include students who assisted with the survey and research.
“There’s still a pretty open question in astronomy when it comes to massive star formation,” says Calahan. “How do stars weighing more than eight solar masses form from clouds of dust and gas?”
Astronomers understand this process for stars the size of our sun. Particles in clouds are attracted to each other and begin to clump together. Gravity takes hold and the gases flow to the centre of the cloud as it collapses. Over millions of years, the gas is put under so much pressure that it begins to burn, and the star is born when nuclear fusion finally begins in the core of the compressed gas.
Theories about how much gas and time it takes to make a star like our Sun can be proven through observations, because each stage of a Sun-like star’s life — from the collapse of gas clouds into a pre-stellar core to the star’s expansion into a red giant and collapse into a white dwarf — can be been seen throughout the galaxy.
But astronomers have yet to understand how stars more than eight times the mass of our Sun form. Stars of this size explode into supernovae at the end of their lives, leaving behind black holes or neutron stars. “There are a few theories for massive star formation that work in simulations, but we haven’t seen those initial conditions out in the wild universe,” says Calahan.
One theory is the formation of massive cores, says Yancy Shirley, associate professor in the UA’s Department of Astronomy. The massive cores are dense collections of gas several times larger than the star they create. For massive stars, the cores must be at least 30 times the mass of our Sun. “People are having trouble finding objects like that,” says Shirley.
The other theory is that multiple low-mass cores form within a gas clump. The low-mass cores grow as they compete for material in the clump, and eventually, one of the cores grows large enough to form a massive star.
“This is the debate: which of these two pictures is more correct, or is it some combination of the two?” Shirley said.
The first step in answering the question is identifying the earliest phase of star formation, so Calahan, under the advisement of Shirley, set out to find clumps showing signs of collapsing gas motion, called “inflow.”
Calahan selected 101 subjects from a list of more than 2,000 huge, cold and seemingly starless clouds of gas called starless clump candidates, or SCCs. Though astronomers have studied SCCs in the past, many of them focused on the brightest and most massive objects. Calahan’s study was unique in that it was a blind survey. Ranging in size from a few hundred times the mass of our Sun to a few thousand solar masses, the SCCs Calahan selected are a representative sample of all gas clouds that have the potential to form massive stars.
Using the Arizona Radio Observatory’s 12-metre (39-foot) radio telescope at the UA’s Steward Observatory on Kitt Peak, Calahan detected and tracked radio waves emitted by the molecular gas oxomethylium (HCO+), which emits a specific radio wavelength.
Once Shirley and the undergraduate students he advises use the telescope to identify objects of special interest, like collapsing SCCs, the clumps of interest are then further studied using the Atacama Large Millimetre/submillimetre Array (ALMA) in Chile, which can peer deeper into the gas and find stars or other objects that cannot be seen with the 12-metre telescope.
Oxomethylium, one of the more abundant ion molecules in space, is a highly reactive ion that would not survive in our Earth’s atmosphere. When oxomethylium moves towards an observer, the wavelengths are compressed; when the gas moves away from an observer, the wavelengths are stretched.
By analysing the wavelengths, Calahan identified six SCCs that showed the telltale signs of collapse, suggesting that gas collapse happens quickly, accounting for only six percent of the formation process of massive stars. “One side is falling away from us and one side is falling towards us,” says Calahan.
“The way we’re using it right now is as a pathfinder,” says Shirley. He and the undergraduate students he advises use the 12-metre telescope to conduct surveys that identify objects of special interest, like collapsing SCC’s. These clumps of interest are then further studied using ALMA, which can peer deeper into the gas and find stars or other objects that cannot be seen with the 12-metre telescope.
Surveys take many dozens of hours to complete. Calahan and Shirley spent 19 weekends over the course of eight months to study the SCCs. “I’ve now seen every part of this research,” says Calahan. “I got to be part of asking the question, observing and doing the data reduction.”
Groups of undergraduate students travelled with Calahan and Shirley to telescope, where they learned astronomical observation and data analysis techniques. “The first time we went up, I learned how to use the telescope and I learned how to analyse the data,” says Calahan. “By the third time, I could teach other students.”
Shirley has served as adviser to several students who have published the research they did at UA, but Calahan is the first student of his whose paper was accepted before graduation. “I don’t think I could have done this at any other university,” says Calahan. “We have the resources and the faculty to teach us how to reduce real-life data and observe on a real-life telescope. That’s really unique to this institution.”
Keep up to date with the latest reviews in All About Space – available every month for just £4.99. Alternatively you can subscribe here for a fraction of the price!