Top 5 Most Recent Articles
Top 5 Most Popular Articles
HIGHLIGHTS by Kelly Beatty
M101's Supernova Shines On
|Update: As of October 3rd the supernova in the galaxy M101 was down to about magnitude 11.1, after peaking in mid-September at 9.9. It's fading by about 0.1 magnitude every two days now, and it has changed from white to strikingly orange-red. See up-to-date light curves in three colors. Catch it right after dusk before it moves lower in the northwest.|
In 1987, when an exploding star erupted to eyeball visibility in the far-southern constellation of Dorado, northern skygazers could only wistfully imagine how it must have looked.
Right now it's fading slowly from a peak brightness of 9.9, where it remained for nearly a week. But the stellar outburst is still 10th magnitude, and, with intrusive moonlight gone from the early-evening sky, the next few nights offer your best chance to spot it.
In a light-polluted sky the star is much easier to see than M101 itself. The face-on spiral galaxy is large but dim and is easily wiped out by skyglow. If you've got a dark enough sky, M101 makes a nearly equilateral triangle in a finderscope with Alkaid and Mizar, the final two stars in the Big Dipper's handle.
If you can see the galaxy itself, the supernova is located 4.4 arcminutes south (and a bit west) of M101's center, at right ascension 14hh 3m 5.8s, declination +54° 16′ 25″.
The supernova is easy to spot in a 4- or 6-inch telescope. Although it looks like any ordinary star, it's thousands of times more distant than any other that's visible in amateur telescopes from northern latitudes. (M101 is about 23 million light-years away.) In fact, you might even pick it up through big, mounted binoculars. "I was able to clearly see SN 2011fe in M101 using mounted 16×60 Pentax binoculars on September 3rd," reports Colorado amateur Mike Prochoda.
Meanwhile, SN 2011fe's early detection and its relative nearness have drawn plenty of interest from professional astronomers. Being a Type Ia supernova (the complete thermonuclear explosion of a white-dwarf star in a binary system), this one is getting special research attention because Type Ia blasts tend to have the same intrinsic brightness and thus serve as uniform "standard candles" for telling distances all across the far universe.
Only rarely, once every couple of decades, do we get one to study in close detail right in our cosmic backyard. "A bright supernova lets you use instruments that don't ordinarily get enough photons," notes Robert Kirshner (Harvard-Smithsonian Center for Astrophysics). "Polarimetry and high-dispersion spectra (to look for gas in the vicinity, along the line of sight in the host galaxy, and in the high-latitude zones of the Milky Way) are good possibilities."
Kirshner adds, "We're especially keen to get good series of infrared spectra, because Type Ia supernovae are better standard candles in the infrared."
Caltech astronomer Richard Ellis says that the Hubble Space Telescope has been tracking the development of SN 2011fe. "We have a regular 'Target of Opportunity' program for nearby Type Ia supernovae," he explains. "We are gathering ultraviolet spectra in a sequence starting from a couple of days after explosion through maximum light and beyond."
Interestingly, no one has been able to identify the star that blew up. Careful searching of archived HST images by Weidong Li (University of California, Berkeley) and others — nor was an X-ray signature evident in before-the-blast observations from the Swift and Chandra spacecraft. So astronomers will have to dig deeper if they hope to determine whether the companion of the now-obliterated white dwarf was a red-giant star, a main-sequence star, or another white dwarf.
Posted by Kelly Beatty, September 16, 2011