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Finding and characterizing the afterglow of a long gamma-ray burst (GRB) is like digging a needle out of a haystack, says Leo Singer. Long GRBs, which are the brightest known electromagnetic events in the universe, are also connected with the deaths of rapidly spinning, massive stars. (Credit: NASA/GSFC/Dana Berry)


Sky survey detects rare supernova

Since February, researchers have been searching the skies for certain types of stars and have made some significant early discoveries.

The first is the progenitor of a rare type of supernova in a nearby galaxy; the other is the afterglow of a gamma-ray burst.

The survey project, known as the intermediate Palomar Transient Factory (iPTF), is focused on finding transients—astronomical objects whose brightness changes over timescales ranging from hours to days.


The survey is led by the California Institute of Technology (Caltech) and builds on the legacy of the Palomar Transient Factory (PTF), designed in 2008 to systematically chart the transient sky by using a robotic observing system mounted on the 48-inch Samuel Oschin Telescope on Palomar Mountain near San Diego, California.

“The first results from iPTF bode well for the discovery of many more supernovae in their infancy and many more afterglows from the Fermi satellite”, says Shrinivas Kulkarni, a professor of astronomy and planetary science at Caltech and principal investigator for both the PTF and iPTF.

Finding a rare supernova

Supernovae—massive exploding stars at the end of their life span—make up one important type of transient. A new paper published in Astrophysical Journal Letters describes the detection of a so-called Type Ib supernova.

Type Ib supernovae are rare explosions where the progenitor star lacks an outer layer of hydrogen, the most abundant element in the universe, hence the “stripped envelope” moniker. It has proven difficult to pin down which kinds of stars give rise to Type Ib supernovae.

One of the most promising ideas, says Caltech graduate student and lead author Yi Cao, is that they originate from Wolf-Rayet stars. These objects are 10 times more massive and thousands of times brighter than the sun and have lost their hydrogen envelope by means of very strong stellar winds.

Until recently, no solid evidence existed to support this theory. Cao and colleagues believe that a young supernova that they discovered, iPTF13bvn, occurred at a location formerly occupied by a likely Wolf-Rayet star.

Supernova iPTF13bvn was spotted on June 16, less than a day after the onset of its explosion. With the aid of the adaptive optics system used by the 10-meter Keck telescopes in Hawaii—which reduces the blurring effects of Earth’s atmosphere—the team obtained a high-resolution image of this supernova to determine its precise position.

Then they compared the Keck image to a series of pictures of the same galaxy (NGC 5806) taken by the Hubble Space Telescope in 2005, and found one starlike source spatially coincident to the supernova. Its intrinsic brightness, color, and size—as well as its mass-loss history, inferred from supernova radio emissions—were characteristic of a Wolf-Rayet star.

“All evidence is consistent with the theoretical expectation that the progenitor of this Type Ib supernova is a Wolf-Rayet star,” says Cao. “Our next step is to check for the disappearance of this progenitor star after the supernova fades away. We expect that it will have been destroyed in the supernova explosion.”

Though Wolf-Rayet progenitors have long been predicted for Type Ib supernova, the new work represents the first time researchers have been able to fill the gap between theory and observation, according to study coauthor and Caltech alumna Mansi Kasliwal. “This is a big step in our understanding of the evolution of massive stars and their relation to supernovae,” she says.

Gamma-ray burst

Leo Singer, a Caltech grad student and lead author of second paper in Astrophysical Journal Letters, describes finding and characterizing the afterglow of a long gamma-ray burst (GRB) as being similar to digging a needle out of a haystack.

Long GRBs, which are the brightest known electromagnetic events in the universe, are also connected with the deaths of rapidly spinning, massive stars.

Although such GRBs initially are detected by their high-energy radiation—GRB 130702A, for example, was first located by NASA’s Fermi Gamma-ray Space Telescope—an X-ray or visible-light afterglow must also be found to narrow down a GRB’s position enough so that its location can be pinpointed to one particular galaxy and to determine if it is associated with a supernova.

After Fermi’s initial detection of GRB 130702A, iPTF was able to narrow down the GRB’s location by scanning an area of the sky over 360 times larger than the face of the moon and sifting through hundreds of images using sophisticated machine-learning software; it also revealed the visible-light counterpart of the burst, designated iPTF13bxl. This is the first time that a GRB’s position has been determined precisely using optical telescopes alone.

After making the initial correlation between the GRB and the afterglow, Singer and colleagues corroborated their results and gained additional information using a host of other instruments, including optical, X-ray, and radio telescopes. In addition, ground-based telescopes around the world monitored the afterglow for days as it faded away, and recorded the emergence of a supernova five days later.

According to Singer, GRB130702A / iPTF13bxl turned out to be special in many ways.

“First, by measuring its redshift, we learned that it was pretty nearby as far as GRBs go,” he says. “It was pretty wimpy compared to most GRBs, liberating only about a thousandth as much energy as the most energetic ones. But we did see it eventually turn into a supernova.

“Typically we only detect supernovae in connection with nearby, subluminous GRBs, so we can’t be certain that cosmologically distant GRBs are caused by the same kinds of explosions.”

The iPTF project is a scientific collaboration between Caltech; Los Alamos National Laboratory; the University of Wisconsin, Milwaukee; the Oskar Klein Centre in Sweden; the Weizmann Institute of Science in Israel; the TANGO Program of the University System of Taiwan; and the Kavli Institute for the Physics and Mathematics of the Universe in Japan.

Source: Caltech

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