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Performances and capabilities
J. Miguel Mas-Hesse
CAB (CSIC-INTA)
on behalf of the OMC Team
Real and Virtual Instruments - JENAM
Granada, September 17th, 2004
INTEGRAL: The International Gamma-ray
Astrophysical Laboratory
• INTEGRAL was launched in October 2002
and provides fine spectroscopy and imaging
in the hard X-ray / soft gamma-ray band
(15 kev - 10 MeV)
Real and Virtual Observatories - JENAM
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Imager IBIS
15 keV – 10 MeV
The INTEGRAL instruments
Monitor Jem-X
12’ FWHM imaging
4-35 keV
<1’ source location
Source ID &
monitoring
Broad lines
Continuum
Monitor OMC
Spectrometer SPI
500 – 600 nm
20 keV – 8 MeV
Source ID &
monitoring
E/∆E ~500
1.3o source location
Narrow lines
Diffuse emission
Continuum
Real and Virtual Observatories - JENAM
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Exposure map after 9 months of operation
Nov 02 – Aug 03
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Some scientific results
Diffuse gamma-ray emission from the Galactic center
resolved in individual sources
Real and Virtual Observatories - JENAM
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10
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Detailed map of the Galactic Center Region
2O
0
__
-10
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Highly absorbed X-ray binaries
INTEGRAL/IBIS
XMM
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-1
3.5 10
-1
3.0 10
Assuming a Gaussian distribution of 8deg FWHM
~20σ
σ
o
511 keV line
observations
10-3 photons s-1 cm-2 keV-
2.5 10-1
2.0 10-1
1.5 10-1
1.0 10-1
5.0 10-2
0.0 100
-5.0 10-2
500
505
510
515
Energy (keV)
520
•Bulge component only (8 ± 3o Φ). Single
point source excluded
•Deeper exposures are needed to see any
+3
-2
disk component
•Origin of positrons remains a mystery.
Yields from supernovae and novae
insufficient.
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525
The Optical Monitoring Camera: OMC
• OMC provides simultaneous optical
photometry of the high energy sources
being observed by IBIS, SPI and JEM-X
Real and Virtual Observatories - JENAM
• It monitors also up to 100 potentially
variable sources within its FoV in
each pointing
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OMC principal characteristics
Field of view
Aperture
Focal length
Optical throughput
System point spread function
CCD pixels
Angular pixel size
CCD quantum efficiency
Time resolution
Typical integration times
Wavelength range
Limiting magnitude
Sensitivity to variations
5°×5°
50 mm
153.7 mm (f/3.1)
> 70 % at 550 nm
Gaussian with FWHM ≈ 1.4 pix
1056 x 2061 (1024 x 1024 image area)
17”.5 x 17”.5
88 % at 550 nm
> 3s
10 – 100 s
V filter (centered at 550 nm)
< 17 (V) (10×100 s, 3σ)
∆V = 0.005 (V=9) to ∆V = 0.15 (V=16)
(depending on crowding)
More information on poster 7-10
Real and Virtual Observatories - JENAM
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Large Magellanic
Cloud region
5º×5º
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OMC capabilities
3 examples illustrate the capabilities and limitations of
the OMC:
• Cygnus X1
• X-ray selected optical sources
• Serendipitous science
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Cyg X-1
• Bright non-eclipsing binary system (V = 8.8).
• Another star is at a distance < 60” (< ~3 pix),
contaminating the photometry.
• The photometric extraction is further affected by the
rotation of the field.
• OMC can nevertheless provide a well sampled optical
light curve of the system.
Real and Virtual Observatories - JENAM
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Real and Virtual Observatories - JENAM
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Optical period: 5.6 d,
associated to the geometrical
cross section of the
companion star.
Real and Virtual Observatories - JENAM
20-30 kev data courtesy of A. Bazzano and the IBIS team
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X-ray selected sources
• In addition to the prime γ-ray target OMC monitors the
sources included in its Input Catalogue.
• The Input Catalogue contains, among others targets, the
complete ROSAT Bright and Faint Sources catalogues.
• We have identified at least 5 new variable objects within
the error boxes of these ROSAT sources.
• In all cases, the variability is very rapid (< 1 day).
• Follow up observations will be performed to confirm the
association between the X and optical objects.
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Period: 0.46 d
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Period: 0.42 d
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Period: 0.99 d
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0.5 d
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1.0 d
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Serendipitous science
• The OMC Input Catalogue contains also all known
optically variable, or suspectedly variable, sources.
• As a by-product, OMC will provide an Output
Catalogue with calibrated light curves for thousands of
objects.
• New variable sources are also being detected.
More information on poster 3-22
Real and Virtual Observatories - JENAM
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β Lyrae type eclipsing binary
Period: 0.93 d
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RR Lyrae type variable star
Period: 1.02 d
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Previously unknown variable star
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