Credit: ESA - C. Carreau
Astronomers looking at the radioactive
afterglow of supernovae with ESA's INTEGRAL mission have revealed that
the remains of stellar explosions move through the Milky Way much
faster, on average, than stars and most of the Galaxy's gas. This
stellar debris is most likely ejected by winds and supernova explosions
in large groups of massive stars located primarily on the leading edges
of the Galaxy's spiral arms.
While the night sky delivers a peaceful and almost immutable cosmic
view, the picture belies a Universe alive with ceaseless motion from the
smallest to the largest scales. All structures in the Milky Way, both
the stars and the diffuse interstellar medium, swirl around the centre
of the Galaxy at velocities as high as hundreds of kilometres per
second, taking about one hundred million years to complete a revolution.
By studying how these objects move, astronomers can figure out the
structure of the Milky Way at large and, in particular, of the spiral
arms – a prominent characteristic of our Galaxy. These investigations
are key in the challenge of understanding the history of the Milky Way's
evolution.
Using data from ESA's INTEGRAL mission, a team of astronomers has
mapped out galactic motions, exploiting a new tracer that follows
stellar debris both through space and time. With this new method, they
revealed that the remains of stellar explosions move, on average, much
faster than stars and most of the gas in the Milky Way.
"The stellar winds blown by a massive star, and the supernova
explosions at the end of its life, are powerful agents. They release
large amounts of matter and energy into interstellar space, and we
managed to trace some of this matter during its very long journey,"
explains Karsten Kretschmer from the Laboratoire APC in Paris, France.
Kretschmer is the lead author of the paper reporting on the new results,
published in Astronomy & Astrophysics.
The astronomers traced the path of the supernova debris by tracking its
velocity relative to us through the Galaxy. They sought the light
emitted at a specific gamma-ray wavelength by the radioactive decay of
aluminium-26 (26Al), an isotope produced in the supernova
explosions. Matter ejected by a supernova is richer in heavy elements
than the raw material from which the parent star formed, because many
new atomic nuclei are created in the star's interior as well as during
the explosion.
Part of the ejected material is in the form of nuclei of radioactive
isotopes, and the majority of them decay over short timescales – ranging
between a few days and several years. But not 26Al. With a half-life of about 700 000 years, 26Al
nuclei can travel very long distances before they decay. When they do
so, astronomers can exploit the gamma rays emitted during the decay to
trace the long-term reach of stellar explosions.
"Looking at the radioactive afterglow of supernovae about a million
years after the explosions, we followed how their debris has spread
across the Galaxy. This is not possible with observations at other
wavelengths, which only show the remnants of more recent supernovae," adds Kretschmer.
Kretschmer and his collaborators used the SPectrometer on INTEGRAL
(SPI) instrument to search for the emission from the radioactive decay
of 26Al. With these data, they could map the distribution and velocity of this isotope across the Milky Way.
"Surprisingly, during the first million years of their journey, the
ejecta from supernovae seem to move, on average, twice as fast as stars
and the diffuse gas we see at other wavelengths in the Galaxy," comments co-author Roland Diehl from the Max-Planck Institut für Extraterrestrische Physik in Munich, Germany.
"We expected such high velocities in the initial phase after the
explosion, but not after a million years. Our measurements are unique as
they can detect the motion of the debris on such a long time scale, but
still before it is slowed down as it ploughs through the surrounding
gas that moves with the general flow."
The astronomers also found that supernovae tend to be more abundant in
the inner parts of the Milky Way, where the spiral arms stem from the
central regions of the Galaxy, rather than at the periphery.
"We conclude that the ejecta from supernovae are mainly
concentrated towards the leading edges of the arms, while most of the
gas and dust from which stars take shape are located in the core of the
arms," he adds.
This offset in velocity and location between the cradles of star
formation and the graveyard of stellar remains suggests the existence of
strong asymmetries in the outflows from massive stars and supernovae
within the Galaxy.
Stars form deep within the spiral arms, but may migrate outwards during
their lifetime. The most massive of them blow intense winds during
their lifetime and eventually die as supernovae. The material ejected
during these events proceeds faster towards the regions of the Milky Way
between the arms, creating gigantic bubbles that expand more easily in
those directions where interstellar material is less dense.
"From the images of nearby spiral galaxies at optical and
ultraviolet wavelengths, previous studies had already suggested that
massive stars and supernovae may be preferentially located on the edges
of spiral arms. Now, we have obtained direct proof," says Kretschmer.
The result will help astronomers piece together the turbulent journey
of matter across the Galaxy, from one generation of stars to the next.
It is also a valuable clue to investigate how the complex structure of
arms arises in spiral galaxies.
Many observations were needed in this study to gain optimal control
over the spectral resolution of the SPI instrument, which varies over
time.
"We had to collect data over almost ten years to achieve the spectral resolution required for this study," notes Diehl.
"This velocity measurement is an unprecedented technical result at
these wavelengths: with such a high spectral resolution, SPI is and will
remain a unique instrument for years to come."
The motion of 26Al nuclei rotating in the Galaxy was already
evident in the results from an earlier study, based on INTEGRAL data
and published in 2006. But longer monitoring and improved spectral
resolution were crucial to pinpoint the velocity of these nuclei to
great precision.
"The goal of this study was very ambitious: looking at stellar
aftermaths that only INTEGRAL can see. And we've succeeded, revealing
that they move much faster than we could imagine," concludes Erik Kuulkers, ESA's INTEGRAL Project Scientist.
Background information
The results described in this article are reported in "Kinematics of massive star ejecta in the Milky Way as traced by 26Al",
by K. Kretschmer et al., published in Astronomy & Astrophysics,
559, A99, 2013; 10.1051/0004-6361/201322563. The study is based on data
collected with the SPI (Spectrometer on INTEGRAL) instrument on board
ESA's INTEGRAL mission. The data were collected between February 2003
and February 2012.
The International Gamma-ray Astrophysics Laboratory (INTEGRAL) was launched on 17 October 2002. It is an ESA project with the instruments and a science data centre funded by ESA Member States (especially the Principal Investigator countries: Denmark, France, Germany, Italy, Spain, Switzerland) and Poland, and with the participation of Russia and the USA. The mission is dedicated to the fine spectroscopy (E/∆E = 500) and fine imaging (angular resolution: 12 arcmin FWHM) of celestial gamma-ray sources in the energy range 15 keV to 10 MeV with concurrent source monitoring in the X-ray (4-35 keV) and optical (V-band, 550 nm) energy ranges.
The International Gamma-ray Astrophysics Laboratory (INTEGRAL) was launched on 17 October 2002. It is an ESA project with the instruments and a science data centre funded by ESA Member States (especially the Principal Investigator countries: Denmark, France, Germany, Italy, Spain, Switzerland) and Poland, and with the participation of Russia and the USA. The mission is dedicated to the fine spectroscopy (E/∆E = 500) and fine imaging (angular resolution: 12 arcmin FWHM) of celestial gamma-ray sources in the energy range 15 keV to 10 MeV with concurrent source monitoring in the X-ray (4-35 keV) and optical (V-band, 550 nm) energy ranges.
Contacts
Karsten KretschmerLaboratoire APC - AstroParticule et Cosmologie
Université Paris Diderot
Paris, France
Email: kkretsch@apc.univ-paris7.fr
Phone: +33-1572-79376
Roland Diehl
Max-Planck Institute for Extraterrestrial Physics
Garching, Germany
Email: rod@mpe.mpg.de
Phone: +49-89-30000-3850
Erik Kuulkers
INTEGRAL Project Scientist
Directorate of Science and Robotic Exploration
European Space Agency
Email: Erik.Kuulkers@sciops.esa.int
Phone: +34-91-8131-358
Source: ESA
