Fonte de Raio X

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Raios-X???
Fonte de Raio X
Chapa
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Raios-X!!!
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Subrahmanyan Chandrasekhar
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Espelhos
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Espelhos
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Espelhos
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Câmera de Alta Resolução
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Câmera de Alta Resolução
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Câmera CCD
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Câmera CCD
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Redes de Difração
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Redes de Difração
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Redes de Difração
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Sistemas de Bordo
Painéis Solares
Tampa de Proteção
Módulo de Controle
Câmera Guia
Propulsores
Antena (2)
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Parceiros

• NASA
• Grupo de Astrofísica do MSFC
• SAO (Observatório Smithsoniano de Astrofísica) -
  Câmera
• MIT (Instituto Tecnológico de Massachusets) -
  CCD/Redes
• Universidade do Estado de Pennsylvania - CCD
• Universidade de Leicester (Inglaterra) - Câmera
• SRON (Oganização Pesquisas Espaciais da Holanda)
  - Redes
• Instituto Max Planck (Alemanha) - Redes

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Lançamento

• 23 de Julho de 1999
• Cabo Canaveral (Flórida)
• Ônibus Epacial Columbia

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Em órbita!!!
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Comunicação
Deep Space Network
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Comunicação
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64h 18min - 55 h de observação sem
interromper 133 000 km - 16 000 km
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Riccardo Giacconi

• Descobriu primeiras fontes emissoras
  de raio X (1962)
• Propos e trabalhou em projetos
  de telescópios de Raio X (Uhuru, Einstein,
  Chandra)

Prêmio Nobel de Física 2002!!!
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Região Sagitarius A (Núcleo da Via Láctea)
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This false-color image shows the central region
of our Milky Way Galaxy as seen by Chandra. The
bright, point-like source at the center of the
image was produced by a huge X-ray flare that
occurred in the vicinity of the supermassive
black hole at the center of our galaxy. This
central black hole has about 2.6 million times
the mass of our sun and is associated with the
compact radio source Sagittarius A. During the
observation the X-ray source at the galactic
center brightened dramatically in a few minutes,
and after about 3 hours, rapidly declined to the
pre-flare level. The rapid variation in X-ray
intensity indicates that the flare was due to
material as close to the black hole as the Earth
is to the sun. This is the most compelling
evidence yet that matter falling toward the black
hole is fueling energetic activity in the
galactic center.
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Nebulosa Planetária Olho do Gato
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Left image The X-ray data from the Chandra X-ray
Observatory have revealed a bright central star
surrounded by a cloud of multimillion-degree gas
in the planetary nebula known as the Cat's Eye.
This Chandra image, where the intensity of the
X-ray emission is correlated to the brightness of
the orange coloring, captures the expulsion of
material from a star that is expected to collapse
into a white dwarf in a few million years. The
intensity of X rays from the central star was
unexpected, and it is the first time astronomers
have seen such X-ray emission from the central
star of a planetary nebula. The ACIS X-ray camera
aboard Chandra observed NGC 6543 on May 10-11,
1999, for a total exposure time of 46,000
seconds.
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Right image This composite image of Chandra and
Hubble Space Telescope data offers astronomers an
opportunity to compare where the hotter, X-ray
emitting gas appears in relation to the cooler
material seen in optical wavelengths. The Chandra
team found that the chemical abundances in the
region of hot gas (its X-ray intensity is shown
in purple) were like those in the wind from the
central star and different from the outer cooler
material (the red and green structures.) Although
still incredibly energetic and hot enough to
radiate X rays, Chandra shows the hot gas to be
somewhat cooler than scientists would have
expected for such a system. These results present
a puzzle since the temperature of the X-ray
emitting material suggests that mixing might have
occurred. This discrepancy means some other
process has created the "lukewarm" X-ray emission
observed by Chandra. The color composite of
optical and X-ray images was made by Zoltan G.
Levay (Space Telescope Science Institute). The
optical images were taken by J.P. Harrington and
K.J. Borkowski (University of Maryland) with the
Hubble Space Telescope
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• Credit Left X-ray (NASA/UIUC/Y.Chu et al.),
  Right X-ray/Optical Composite (X-ray
  NASA/UIUC/Y.Chu et al., Optical NASA/HST)
• Scale Images are 30 arcsec on a side
• Category Planetary Nebula
• Coordinates (J2000) RA 17h 58m 33.30s Dec 66''
  37' 59.20''
• Constellation Draco
• Observation Date (of primary image used) May
  10-11, 2000
• Observation Time (of primary image used) 12.8
  hours
• Obs. ID (of primary image used) 630
• Color Code Intensity
• Instrument ACIS

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Quasares
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The Chandra image of the twin quasars Q2345007
A, B shows that they are not identical twins.
This means that it is unlikely that they are an
optical illusion, rather, they were probably
created by merging galaxies. When galaxies
collide, the flow of gas onto the central
supermassive black holes of each of the galaxies
can be enhanced, resulting in two quasars. The
light from the quasar pair started its journey
toward Earth 11 billion years ago. Galaxies were
about three times closer together then than they
are now, so collisions were much more likely.
Quasar pairs that are seen close to one another
on the sky and are at the same distance from
Earth often turn out to be an illusion as part of
a gravitationally lensed system. In these cases,
the image of a single quasar has been split into
two or more images as its light has been bent and
focused on its way to Earth by the gravity of an
intervening massive object like a galaxy, or a
cluster of galaxies.
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The quasar pair Q2345007 A, B was thought to be
such an illusion because of the remarkably
similar patterns of the light, or spectra, from
the pair at both optical and ultraviolet
wavelengths. However no intervening galaxy or
cluster has been found for this pair, leading to
the speculation that the gravitational
light-bending might be caused by a new type of
cluster that contains hot gas and dark matter,
but no stars. Such a dark cluster would be
invisible to optical and ultraviolet telescopes,
but would be detectable in X-rays. The Chandra
X-ray images showed no evidence for a massive
dark cluster. Further, the X-ray spectra of the
two quasars were distinctly different, supporting
the idea that they are distinct objects, rather
than a mirage.
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• Credit NASA/SAO/CXC/P.Green et al.
• Scale Image is 30 arcsec per side.
• Category Quasar
• Constellation Pisces
• Observation Date May 26, 2000 and June 27, 2000
• Observation Time 18 hours total
• Color Code colors indicate X-ray energy bands -
  red (low), green (medium), and blue (high)
• Instrument ACIS
• Distance Estimate 11 billion light years

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FIM...
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Agradecimentos Cadu (capa) Equipe CDA
Referências http//chandra.harvard.edu
http//wave.xray.mpe.mpg.de/axaf/
http//www.msfc.nasa.gov/