 Supernova event on August 25, 2011 | |
| Event type | Supernova  |
|---|---|
| Ia[1] | |
| Date | 24 August 2011[1] |
| Constellation | Ursa Major,Big Dipper[1] |
| Right ascension | 14h 03m 05.8s[2] |
| Declination | +54° 16′ 25″[2] |
| Epoch | J2000[2] |
| Distance | 21Mly[3] |
| Redshift | 0.001208 ±5e-06 |
| Host | Pinwheel Galaxy (M101)[1] |
| Peakapparent magnitude | 9.9[4] |
| Other designations | SN 2011fe |
 Related media on Commons | |
SN 2011fe, initially designatedPTF 11kly, was aType Ia supernova discovered by thePalomar Transient Factory (PTF) survey on 24 August 2011 during an automated review of images of theMessier 101 from the nights of 22 and 23 August 2011. It was located in Messier 101, thePinwheel Galaxy, 21 millionlight years from Earth.[3] It was observed by the PTF survey very near the beginning of its supernova event, when it was approximately 1 million times too dim to be visible to the naked eye. It is the youngest type Ia ever discovered.[5] About 13 September 2011, it reached its maximum brightness ofapparent magnitude +9.9[6] which equals anabsolute magnitude of about -19, equal to 2.5 billion Suns. At +10 apparent magnitude around 5 September, SN 2011fe was visible in small telescopes. As of 30 September the supernova was at +11 apparent magnitude in the early evening sky after sunset above the northwest horizon. It had dropped to +13.7 as of 26 November 2011.[7]
The Palomar Transient Factory is an automated telescopic survey that scans the sky for transient and variable astronomical events. Information is fed to theNational Energy Research Scientific Computing Center (NERSC) atLawrence Berkeley National Lab, which computes the information to identify new star events. After the initial observation of the SN 2011fe event, telescopes were used in theCanary Islands (Spain) to identify theemission spectrum of light emitted at various stages of the event. Following this, theHubble Space Telescope, theLick Observatory in California, and theKeck Observatory in Hawaii were used to observe the event in greater detail.
Although SN 2011fe was initially very faint, it brightened rapidly. On the day it was first imaged, 24 August 2011, it was 1 million times too dim to be visible to the unaided eye. One day later, it was 10 thousand times too dim. The next day it was 6 times brighter than that. On 25 August, theEVLA radio telescope failed to detect radio emissions from SN 2011fe. While such emissions are common for other types of supernovae, they have never been observed for Type Ia's.[8]
Two possible candidates were proposed for the precursor system;[9] however, subsequent analysis appears to rule them out.[10]
Type Ia supernova events occur when awhite dwarf star accretes enough additional matter to exceed theChandrasekhar limit and collapses, triggering runaway fusion and a supernova explosion. Because this collapse happens at a consistent mass, the resulting explosions have very uniform characteristics, and are used as "standard candles" to measure the distance to their host galaxies. The exact brightness and behavior of a Type Ia supernova depends on themetallicity of its parent star (the fraction of the star composed of elements heavier thanhydrogen andhelium before its evolution into a white dwarf). Because the SN 2011fe event was detected so early, astronomers can gain a more accurate measurement of its initial composition and of its evolution during the supernova explosion, and so refine their models of Type Ia supernova events, resulting in more precise distance estimates for other Type Ia supernova observations.1
Type Ia supernova standard candles may help provide evidence to support the hypothesis ofdark energy and the acceleratingexpansion of the universe.[11] A better understanding of type Ia supernova behavior may in turn allow theoretical models of dark energy to be improved.
[The ]detection limit is still not deep enough to place restrictive limits on the binary companion to the white dwarf. Low-mass red giants and main-sequence stars below about 5 solar masses would remain undetected.
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