Credit: X-ray: NASA/CXC/ISDC/L.Pavan et al, Radio: CSIRO/ATNF/ATCA
Optical: 2MASS/UMass/IPAC-Caltech/NASA/NSF
An extraordinary jet trailing behind a runaway pulsar is seen in this composite image that contains data from NASA's Chandra X-ray Observatory (purple), radio data from the Australia Compact Telescope Array (green), and optical data from the 2MASS survey (red, green, and blue). The pulsar - a spinning neutron star - and its tail are found in the lower right of this image (mouse over the image for a labeled version). The tail stretches for 37 light years , making it the longest jet ever seen from an object in the Milky Way galaxy, as described in our press release.
The pulsar, originally discovered by ESA's INTEGRAL satellite, is
called IGR J1104-6103 and is moving away from the center of the supernova remnant
where it was born at a speed between 2.5 million and 5 million miles
per hour. This supersonic pace makes IGR J1104-6103 one of the fastest
moving pulsars ever observed.
A massive star ran out of fuel and collapsed to form the pulsar along
with the supernova remnant, the debris field seen as the large purple
structure in the upper left of the image. The supernova remnant (known
as SNR MSH 11-61A) is elongated along the top-right to bottom left
direction, roughly in line with the tail's direction. These features
and the high speed of the pulsar suggest that jets could have played an
important role in the supernova explosion that formed IGR J1104-6103.
In addition to its exceptional length, the tail behind IGR J1104-6103
has other interesting characteristics. For example, there is a distinct
corkscrew pattern in the jet. This pattern suggests that the pulsar is
wobbling like a top as it spins, while shooting off the jet of
particles.
Another interesting feature of this image is a structure called a
pulsar wind nebula (PWN), a cocoon of high-energy particles that
enshrouds the pulsar and produces a comet-like
tail behind it. Astronomers had seen the PWN in previous observations,
but the new Chandra and ATCA data show that the PWN is almost
perpendicular to the direction of the jet. This is intriguing because
usually the pulsar's direction of motion, its jet, and its PWN are
aligned with one another.
One possibility requires an extremely fast rotation speed for the
iron core of the star that exploded as the supernova. A problem with
this scenario is that such fast speeds are not commonly expected to be
achievable.
A paper, led by Lucia Pavan of the University of Geneva in
Switzerland, describing these results appears in the February 18th issue
of the journal Astronomy & Astrophysics and is also available online.
Other authors include Pol Bordas (University of Tuebingen in Germany),
Gerd Puehlhofer (Univ. of Tuebingen), Miroslav Filipovic (University of
Western Sydney in Australia), A. De Horta (Univ. of Western Sydney), A.
O'Brien (Univ. of Western Sydney), M. Balbo (Univ. of Geneva), R. Walter
(Univ. of Geneva), E. Bozzo (Univ. of Geneva), C. Ferrigno (Univ. of
Geneva), E. Crawford (Univ. of Western Sydney), and L. Stella (INAF).
Fast Facts for IGR J11014-6103:
Scale: Image is 22 arcmin across (about 147 light years)
Category: Supernovas & Supernova Remnants, Neutron Stars/X-ray Binaries
Coordinates (J2000): RA 11h 01m 22.08s | Dec -61° 03' 25.20"
Constellation: Carina
Observation Date: 11 Oct 2012
Observation Time: 13 hours 43 min
Obs. ID: 13787
Instrument: ACIS
References: Pavan, L. et al, 2014 A&A, in press; arXiv:1309.6792
Color Code: X-ray: (Pink) Radio: (Green); Optical (Red, Green, Blue)
Distance Estimate: About 23,000 light years
Source: NASA’s Chandra X-ray Observatory
