10 JUN 2010
Credits: E. Kuulkers (ISOC)
Count rate lightcurve of the Crab calibration source since the beginning of the INTEGRAL mission (7.5 years ago) in the 18-40 keV range. The long-term variations are corrected for by the use of different ARF responses for different epochs.
|
10 JUN 2010
Credits: E. Kuulkers (ISOC)
Count rate lightcurve of the Crab calibration source since the beginning of the INTEGRAL mission (7.5 years ago) in the 40-100 keV range. The long-term variations are corrected for by the use of different ARF responses for different epochs.
|
9 JUN 2010
Credits: ISDC
A 3-D plot of the shadowgram of the spectrometer SPI showing the counts received
in each of the 19 hexagonal detectors of this instrument during one pointed
observation of the INTEGRAL spacecraft. Since the most recent failure of 27 May 2010, there are now four dead detectors with zero counts.
|
18 AUG 2009
Credits: ISDC/V. Beckmann
| .ps
IBIS/ISGRI lightcurve of GRB 090817 detected near the centre of the INTEGRAL field of view.
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18 AUG 2009
Credits: ISDC/V. Beckmann
| .ps
JEM-X 1 lightcurve of GRB 090817 detected near the centre of the INTEGRAL field of view.
|
3 MAR 2007
Credits: ISDC/M. Türler
IBIS/ISGRI lightcurve of a bright outburst of XTE J1739-302 / IGR J17391-3021
observed by INTEGRAL on March 2, 2007.
Publication: Turler et al., 2007, ATel #1019
|
27 MAY 2005
Credits: ISDC/V. Beckmann
Example of a bad science window (ScW) in a mosaic image. This can be due to a low exposure time or a strong background noise. The latter can happen near the perigee of the orbit due to the radiation belts of the Earth or during a solar flare.
|
28 APR 2005
Credits: J. Rodriguez (CEA Saclay & ISDC)
| .eps.gz
RXTE/PCA spectra of IGR J19140+0951 from 3 observations taken in 2002, 2003,
and 2004. Although the source is in a low luminosity state (as compared to the
time when it is detected by INTEGRAL) differences in spectral shape are
obvious. In particular the spectral fits show significant evolution of the
power law photon index, the absorption column density and the iron line
intensity.
|
28 APR 2005
Credits: J. Rodriguez (CEA Saclay & ISDC)
| .eps.gz
RXTE light curve and spectra of the 2004 observation of IGR J19140+0951,
showing two distincts period from which PCA spectra were extracted and fitted.
Major differences are seen between both intervals: besides variation of the
flux, a cut-off is detected at ~12 keV in the bright one, and significant
evolution of the absorption column density NH is seen.
|
19 APR 2005
Credits: P. Kretschmar (ISOC at ESAC, Madrid)
IBIS, JEM-X and SPI common spectra in different states of the outburst of IGR
J17464-3213. Numbers on the top of each spectrum indicate the revolution number
of the corresponding INTEGRAL observation.
Reference: Capitanio et al. 2005, ApJ 622, 503
|
18 APR 2005
Credits: ISDC/N. Mowlavi/M. Türler
INTEGRAL exposure map (IBIS fully coded field-of-view) of the whole sky in
galactic coordinates for the 300 first revolutions. The integration time is
color coded according to the scale on the right. The main targets are labeled.
|
18 APR 2005 updated on 27 APR 2005
Credits: ISDC/N. Mowlavi/M. Türler
INTEGRAL exposure map (IBIS fully coded field-of-view) of the whole sky in
galactic coordinates for all publicly available data on 15 April 2005. The
integration time is color coded according to the scale on the right. The main
targets are labeled.
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23 MAR 2005
Credits: J. Rodriguez (CEA Saclay & ISDC)
| .eps.gz
Deconvolved JEM-X 2, ISGRI and SPI spectra of the high and low parts of the
pulses visible on the light curve (previous image). The dashed and continuous
line represent the best fit model to the observed and unabsorbed spectra,
respectively. The best fit model is an hybrid thermal/non-thermal
Comptonisation model.
Publication: Hannikainen et al. 2005, astro-ph/0502438
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23 MAR 2005
Credits: J. Rodriguez (CEA Saclay & ISDC)
| .eps.gz
JEM-X 2 3-35 keV light curve of GRS 1915+105 during Revolution 48. The time bin
is 8 sec. The line overplotted on the bottom panel represent the time of our
simultaneous RXTE observations.
Publication: Hannikainen et al. 2005, astro-ph/0502438
|
12 JAN 2005
Credits: R. Walter (ISDC)
This IBIS/ISGRI mosaic image shows the High-Mass X-ray Binary V 0332+53 (EXO
0331+530) during its 2004-2005 outburst.
|
12 JAN 2005
Credits: I. Kreykenbohm (ISDC & IAAT)
This spectrum of the High-Mass X-ray Binary V 0332+53 during its 2004-2005
outburst as observed by INTEGRAL. The combined ISGRI (red), SPI (green) and
JEM-X (white) spectrum was fitted with a simple power-law and a high energy
cut-off. The residual at the bottom clearly show 3 cyclotron lines at energies
of ~25, ~55 and ~75 keV (Soldi et al., 2005, ATel 382). This confirms the
lines discovered with RXTE by Coburn et al. (2005, ATel 381).
|
19 DEC 2004
Credits: A. Paizis (ISDC)
| .ps.gz
Within 10 hours, INTEGRAL detected two gamma-ray bursts (GRB) in it's field of
view, GRB 041218
(Mereghetti et al., GCN
2858) and GRB
041219 (Götz et al., GCN 2866). The second
burst was bright and long enough (~ 9 min.) to be clearly detected ("NEW_1"
source) in this Science Window IBIS/ISGRI hard band (60-200 keV) image obtained
with the ISDC Quick-Look Analysis (QLA) tool.
|
17 DEC 2004
Credits: D. Götz (IASF, Milano) & J.A. Zurita Heras (ISDC)
| .ps.gz
Count rate lightcurves of EXO 2030+375 in 3 energy bands from low to high
energies (from top to bottom). The time axis is in seconds. The outburst
detected by the INTEGRAL Burst Alert System (IBAS) (Götz et al. ATel 367) is best seen
in the soft band (red curve). The 42 sec pulsation of this High-Mass X-ray
Binary (HMXB) pulsar is also clearly visible.
|
9 DEC 2004
Credits: S. Shaw (ISDC & Southampton)
IBIS/ISGRI image (20-60 keV band) of Science Window number 0261 0002 001 0
taken on Dec. 2, 2004 in which a new source was discovered at a position only
about 20 arcmin off the cataclysmic variable V* V709 Cas (Eckert et al. ATel 352). The flux of
the discovered source IGR J00291+5934 was found to be about 55+/-5 mCrab in
this energy band. A follow-up X-ray observations with RXTE/PCA showed that the
source is a millisecond pulsar with a frequency record of nearly 600 Hz
(Markwardt et al. ATel
353).
For further information on this source see the list of scientific circulars.
Publication: Shaw et al., A&A 432, L13-L16 (2005)
|
11 OCT 2004
Credits: R. Walter (ISDC)
IBIS/ISGRI mosaic images (25-30 keV band) of the galactic plane centered on the
Norma-arm region with (bottom) and without (top) proper ghost removal and
background correction.
|
5 AUG 2004
Credits: ISDC/N. Mowlavi/M. Türler
INTEGRAL exposure map (IBIS fully coded field-of-view) of the whole sky in
galactic coordinates for the 200 first revolutions. The integration time is
color coded according to the scale on the right. The main targets are labeled.
|
20 JUL 2004
Credits: V. Beckmann (GSFC)
IBIS/ISGRI 40-100 keV image of the Virgo field including the Seyfert 2 galaxy
NGC 4388 and the bright quasar 3C 273. The observations used here were
performed in June/July 2003 for a total on source time of 177 ksec.
This image is part of a NASA press release
|
19 DEC 2003
Credits: R. Walter (ISDC Geneva)
JEM-X 2 mosaic image of the Galaxy in the 2-5 keV energy band. The image
includes all Galactic Plane Scans (GPS) and all Galactic Center Deep Exposures
(GCDE) taken during roughly the first year of INTEGRAL's mission. The four
pannels are, from top to bottom, the intensity image, the variance map, the
significance image and the exposure map.
|
16 DEC 2003
Credits: A. Tiengo, D. Götz & S. Mereghetti (IASF Milano)
Thanks to the rapid and accurate IBAS localization of GRB 031203, XMM-Newton
could start an observation 6 hours after the burst. The images obtained with
the EPIC instrument show, for the first time, an X-ray afterglow (central
source) surrounded by an expanding ring. The ring is due to scattering of the
GRB X-ray emission by dust grains in our Galaxy. The apparent expansion is
due to the different light travel times of the photons scattered at various
angles. The maximum ring radius shown by these images is about 3.5 arcmin (20
hours after the burst).
The discovery of these rings was announced by S. Vaughan et al. in GCN 2489
|
17 OCT 2003
Credits: R. Walter et al.
Combined XMM-Newton and INTEGRAL/ISGRI spectrum of IGR J16318-4848. This is the
first source discovered by INTEGRAL on 29 January 2003. The X-ray spectrum is
heavily absorbed suggesting that the source is enshrouded in a very dense
cloud. Strong fluorescence emission lines are also detected.
Publication: R. Walter et al. 2003, astro-ph/0309536
|
16 OCT 2003
Credits: L. Kuiper et al.
| .ps.gz
Main pulse of the Crab profile in absolute phase as measured by IBIS/ISGRI
(20-50 keV; full line) compared to the Greenbank 812.5 MHz radio profile
(dashed line).
Publication: L. Kuiper et al. 2003, astro-ph/0309178
|
16 OCT 2003
Credits: L. Kuiper et al.
| .ps.gz
Crab profiles in absolute phase: a) radio 430 MHz (Arecibo: Moffett & Hankins
1996), b) radio 812.5 MHz (Greenbank: Lundgren 1994), c) X-rays 20-50 keV
(IBIS/ISGRI), d) gamma-rays with energies above 100 MeV (EGRET).
Publication: L. Kuiper et al. 2003, astro-ph/0309178
|
9 OCT 2003
Credits: A.J. Castro-Tirado et al.
Optical R band image of the GRB030227 field taken at the 2.5INT on 27 Feb.
2003. The position of the optical afterglow is indicated by the arrow inside
the preliminary and the final XMM-Newton error circles (6" and 4" radii,
respectively). The field is 1' x 1' with North up and East to the left.
Publication: A.J. Castro-Tirado et al. 2003, astro-ph/0309804
|
9 OCT 2003
Credits: A.J. Castro-Tirado et al.
IBIS/ISGRI image of GRB030227 detected in the Crab field during the calibration
phase on February 27, 2003 at 08:42 UT. The image has been obtained in the
15-200 keV band and was deconvolved using the IBAS software. The distance
between the Crab and the GRB is ~10°. North is up, East to the left.
Publication: A.J. Castro-Tirado et al. 2003, astro-ph/0309804
|
8 OCT 2003
Credits: A. Domingo Garau (LAEFF, Vilspa) for the OMC Team
Lightcurve of the eclipsing binary star Y Sextant folded with the known optical
period. Two clear minima are observed showing that the two stars are of similar
size and close together, shadowing the other when passing in front of it. The
lightcurve has been measured by INTEGRAL/OMC in much more detail than with
previous space missions.
|
26 AUG 2003
Credits: O. Vilhu et al.
| .eps.gz
Deconvolved spectra of Cyg X-3. The red, magenta and cyan spectra correspond to
the PCA/HEXTE data set 1, 2, 3, respectively. The HEXTE spectra have been
renormalized to the flux level implied by the PCA. The model spectrum is shown
only for the middle spectrum (data set 1) for clarity. The green, blue and
black spectra are from the JEM-X, ISGRI and SPI, respectively, with the model
spectrum shown in the black curve. The ISGRI and SPI spectra have been
renormalized to the JEM-X data. The intensity levels of the INTEGRAL spectra,
which were accumulated over several binary phases, should be close to the mean
of the RXTE data sets 2 and 3. The proportions of this figure correspond to
equal length per decade on each axis.
Publication: O. Vilhu et al. 2003, astro-ph/0308395
|
26 AUG 2003
Credits: O. Vilhu et al.
| .eps.gz
The JEM-X 6-15 keV (red diamonds) and ISGRI 20-40 keV (blue squares)
lightcurves of Cyg X-3 folded over the orbital period. We also show the XTE/PCA
3-15 keV data (black asterisks) from simultaneous observations as well as the
XTE/ASM 1.5-12 keV (dashed red curve) and CGRO/BATSE 20-100 keV (blue curve)
phase dependences averaged over several years of monitoring. The count rates
are normalized to the respective maxima.
Publication: O. Vilhu et al. 2003, astro-ph/0308395
|
26 AUG 2003
Credits: O. Vilhu et al.
| .ps.gz
SPI image of the cygnus region in the 34-52 keV band. The brightest source in
the lower left corner is Cyg X-1, while Cyg X-3 is the source at the upper
right.
Publication: O. Vilhu et al. 2003, astro-ph/0308395
|
26 AUG 2003
Credits: O. Vilhu et al.
| .ps.gz
IBIS/ISGRI mosaic image of the Cygnus region in the 15-40 keV band showing
Cyg X-1 (left), Cyg X-3 (center) and SAX J2103.5+4545 (right).
Publication: O. Vilhu et al. 2003, astro-ph/0308395
|
26 AUG 2003
Credits: O. Vilhu et al.
| .ps.gz
IBIS/ISGRI mosaic image of the Cygnus region in the 40-100 keV band showing
Cyg X-1 (left), Cyg X-3 (center) and SAX J2103.5+4545 (right).
Publication: O. Vilhu et al. 2003, astro-ph/0308395
|
20 AUG 2003
Credits: A. Paizis et al.
| .ps.gz
ISGRI images of the Galactic Centre in the 20-40 keV band. The analysis of
ISGRI data is based on GCDE and GPS data from revolution 30 to 64 i.e. January
11th to April 22nd, 2003 for a total of one thousand pointings (about 2 Msec
exposure). Not all the sources are labeled for clarity. The sources labeled in
white belong to the monitoring program of the Bright LMXRB group.
Publication: A. Paizis et al. 2003, astro-ph/0308038
|
20 AUG 2003
Credits: A. Paizis et al.
| .ps.gz
ISGRI images of the Galactic Centre in the 40-60 keV band. The analysis of
ISGRI data is based on GCDE and GPS data from revolution 30 to 64 i.e. January
11th to April 22nd, 2003 for a total of one thousand pointings (about 2 Msec
exposure). Not all the sources are labeled for clarity. The sources labeled in
white belong to the monitoring program of the Bright LMXRB group.
Publication: A. Paizis et al. 2003, astro-ph/0308038
|
20 AUG 2003
Credits: A. Paizis et al.
| .ps.gz
SPI image based on GCDE data of the Galactic Centre in the 40-100 keV band from
March to April 2003 (about 1 Msec of overall exposure). The sources in white
belong to the monitoring program of the Bright LMXRB group. Other sources are
marked in yellow for orientation.
Publication: A. Paizis et al. 2003, astro-ph/0308038
|
20 AUG 2003
Credits: A. Paizis et al.
| .ps.gz
Combined JEM-X (black), ISGRI (green) and SPI (red) count spectra of the
low-mass X-ray binary (LMXRB) GX 17+2. The SPI spectrum is based on all GCDE
data from March to April 2003, while JEM-X and ISGRI spectra are extracted from
one pointing only (about 2.2 ksec). Individual normalisation has been applied
to the three instruments in order to compensate for uncertainties in the
cross-calibration.
Publication: A. Paizis et al. 2003, astro-ph/0308038
|
19 AUG 2003
Credits: K. Pottschmidt et al.
| .eps.gz
Unfolded X-ray spectra for the observations of 2002 December 2, and December 29
and the various components of the model (disk black-body, gaussian iron line,
thermal comptonization and reflection). Fluxes have been renormalized to those
measured by the PCA.
Publication: K. Pottschmidt et al. 2003, astro-ph/0309203
|
19 AUG 2003
Credits: K. Pottschmidt et al.
| .eps.gz
Count spectra, best fit model, and residuals for the Cyg X-1 observations of
2002 December 2, and December 29 (PCA, 3-25 keV, light blue; JEM-X, 10-40 keV,
green; HEXTE, 20-200 keV, red; IBIS, 40-250 keV, dark blue; SPI, 50-300 keV,
olive green). The model includes a disk black-body, a gaussian iron line,
thermal comptonization and reflection.
Publication: K. Pottschmidt et al. 2003, astro-ph/0309203
|
18 AUG 2003
Credits: ISDC/N. Mowlavi/M. Türler
INTEGRAL exposure map (IBIS fully coded field-of-view) of the whole sky in
galactic coordinates for the 100 first revolutions. The integration time is
color coded according to the scale on the right. The main targets are labeled.
|
18 AUG 2003
Credits: ISDC/N. Mowlavi
INTEGRAL exposure map (IBIS fully coded field-of-view) of the whole sky in
galactic coordinates for the 100 first revolutions. The integration time is
color coded according to the scale on the right. The bottom histogram shows the
exposure time per revolution number.
|
18 AUG 2003
Credits: ISDC/N. Mowlavi
INTEGRAL exposure map (IBIS partially coded field-of-view) of the whole sky in
galactic coordinates for the 100 first revolutions. The integration time is
color coded according to the scale on the right. The bottom histogram shows the
exposure time per revolution number.
|
22 MAY 2003
Credits: K. Ebisawa (ISDC)
INTEGRAL exposure map (IBIS partialy coded field-of-view) of the whole sky in
galactic coordinates from Launch (Octobre 17, 2002) up to May 20, 2003. The
integration time is color coded according to the scale at the bottom.
|
12 MAY 2003
Credits: R. Walter (ISDC)
IBIS/ISGRI mosaic image of the Galaxy in the 15-40 keV energy band. The image
includes all Galactic Plane Scans (GPS) and all Galactic Center Deep Exposures
(GCDE) from launch up to revolution 67 (May 4, 2003).
|
12 MAY 2003
Credits: R. Walter (ISDC)
IBIS exposure map of the Galaxy based on all Galactic Plane Scans (GPS) and
all Galactic Center Deep Exposures (GCDE) from launch up to revolution 67
(May 4, 2003).
|
3 MAR 2003
Credits: A. Domingo Garau for the OMC Team
First OMC light curve of a variable star, the Algol type eclipsing binary
DY Aqr, with a period of 2.16 days.
|
27 FEB 2003
Credits: V. Beckmann (ISDC) for the SPI Team
SPI image in the 20-200 keV energy band showing both the Crab nebula and the
4th Gamma-Ray Burst (GRB) seen in the INTEGRAL field-of-view on February 27,
2003 at 08:42 UT. It was obtained with the SPIROS software for a time interval
of 18 sec (including the burst), using detectors 0-18 (single + PSD events)
and with an empty field observation as a background model.
|
27 FEB 2003
Credits: V. Beckmann (ISDC) for the SPI Team
SPI spectrum of the 4th Gamma-Ray Burst (GRB) seen in the INTEGRAL
field-of-view on February 27, 2003 at 08:42 UT. The full Science Window
was used here as a background, but excluding the 18 sec time interval of the
GRB (this removes the Crab and other sources from the counts). The spectrum
makes use of the single + PSD + multiple events (pseudo detectors 0-84) in the
18 sec as used for the image above. The fifth data point is consistent with
zero.
|
18 DEC 2002
Credits: K. Pottschmidt (ISDC) for the ISDC team, the INTEGRAL instrument teams and the RXTE Cyg X-1 monitoring campaign
| .eps.gz
Comparison of the Cyg X-1 spectrum obtained by INTEGRAL and by the X-ray
satellite RXTE. The very small residuals of the spectral fit show that the
INTEGRAL IBIS and SPI data are already very well interpreted by the analysis
software.
|
17 DEC 2002
Credits: S. Mereghetti & D. Götz (IASF/ISDC) for the IBIS/IBAS Team
IBIS image of the first Gamma-Ray Burst (GRB) in the field-of-view of the
INTEGRAL instruments. The coordinates are superposed on the image.
|
17 DEC 2002
Credits: S. Mereghetti & D. Götz (IASF/ISDC) for the IBIS/IBAS Team
IBIS image and light curve of the first Gamma-Ray Burst (GRB) in the
field-of-view of the INTEGRAL instruments. It is a single peaked burst
with a duration of about 20 seconds.
|
11 DEC 2002
Credits: P. Kretschmar for the JEM-X Team
JEM-X 1 (left) and JEM-X 2 (right) mosaic images of Cyg X-1 (lower right) and
Cyg X-3 (upper left) as obtained from 51 pointings of a 5x5 dithering, of
which only one 4x4 corner was selected here. The white circles mark the
catalog positions and have a radius of 20 arcmin. No vignetting correction
was applied to the input images. The exposure time ranges from ~5000 sec
to almost 100,000 sec in the center of the mosaic.
|
27 NOV 2002
Credits: M. Türler for the SPI Team
The SPI anticoincidence system (ACS) light curve of the first gamma-ray burst
seen in the field-of-view of the INTEGRAL gamma-ray instruments.
The burst GRB021125 reached INTEGRAL on November 25, 2002 at 17:58:24 UT.
The lightcurve shown here has been averaged into 0.5 sec time bins.
|
26 NOV 2002
Credits: V. Beckmann for the SPI Team
SPI image of Cyg X-1 (center) and Cyg X-3 (upper left) as obtained by the
SPIROS software based on single, PSD and multiple events between 15 and 40
keV. The analysis is based on 41 science windows combining 74,700 sec
(ONTIME) in hexagonal dithering mode.
|
21 NOV 2002
Credits: P. Kretschmar for the JEM-X Team
JEM-X 1 mosaic image of the Cyg X-1 region with hexagonal dithering.
The position of the main sources in the field-of-view are shown.
Note that Cyg X-1 is not exactely at the right position because the
correction for instrument misalignment was not yet applied.
|
17 NOV 2002
Credits: A. Domingo Garau for the OMC Team
The High Mass X-ray Binary Cyg X-1 appears at the centre of this OMC
sub-window obtained with an integration time of 100 s. According to GCVS(1998)
its magnitude at maximum (minimum) brightness is 8.72 (8.93). The period of
this variability is about 5.6 days. The lower right source is the variable
star V1674 Cyg of a V magnitude of 10.07 and an amplitude of 0.06 mag. On the
upper left side we could have a detection of a star with apparent visual
magnitude of 14.79.
|
17 NOV 2002
Credits: P. Kretschmar for the JEM-X Team
JEM-X 1 exposure map corresponding to the mosaic image of the Cyg X-1 region
obtained across 16 Science Windows with hexagonal dithering.
An uniform exposure has been assumed for the map of each individual Science
Window.
|
17 NOV 2002
Credits: P. Kretschmar for the JEM-X Team
JEM-X 1 mosaic image of the Cyg X-1 region obtained across
16 Science Windows with hexagonal dithering.
The individual images have been vignetting corrected and data used up to
10% transmission. One clearly sees the amplified noise structure around
the centre.
|
17 NOV 2002
Credits: S. Mereghetti & D. Götz for the IBIS/IBAS Team
First IBIS source as seen with the IBAS (INTEGRAL Burst Alert System) software.
The coordinate grid is based on the predicted attitude.
Cyg X-1 is detected about 9 arcmin from its true position.
The eight apparent sources seen symmetrically around the central source
(Cyg X-1) are so called ghosts.
|
17 NOV 2002
Credits: P. Kretschmar for the JEM-X Team
| .ps.gz
First JEM-X images (JEM-X 1 above; JEM-X 2 below) for ScW 001130000100 with
Cyg X-1 on axis. The images were produced with the standard tools in the
JEM-X integration environment choosing no vignetting correction and excluding
the outer zones of the detector shadowgrams.
|
17 NOV 2002
Credits: The SPI Team
First image of the Cyg X-1 region taken by SPI during the first
pointing on November 16, 2002. The integration time is aprroximatively 1 hour
and the energy range is ~25-45 keV.
|
17 NOV 2002
Credits: The IBIS Team
First image of the Cyg X-1 region taken by IBIS/ISGRI during the first
pointing on November 16, 2002 (ScW 001130000100). The energy range of this
image is 40-100 keV and Cyg X-1 is detected at a level of ~13 sigma.
|
17 NOV 2002
Credits: The IBIS Team
First image of the Cyg X-1 region taken by IBIS/ISGRI during the first
pointing on November 16, 2002 (ScW 001130000100). The energy range of this
image is 14-40 keV and Cyg X-1 is detected at a level of ~23.6 sigma.
|
14 NOV 2002
Credits: Niels Jřrgen Westergaard (DSRI Copenhagen)
First detection of LMC X-3 (at the center) and LMC X-4 (2 deg below slightly
right) in the Large Magellanic Cloud (LMC).
|
8 NOV 2002
Credits: Laurent Lerusse for the IBIS Team
ISGRI detector shadowgram showing several bright pixels. An on-board
system is handling those noisy pixels by switching them off for a while.
The number of noisy pixels is not greater than expected (less than 10%).
In this lego plot the brightest pixels have been cut by choosing a reduced
range of the vertical axis.
|
7 NOV 2002
Credits: SPI Team
This is the first spectrum extracted from the data by the SPIROS analysis
software.
|
7 NOV 2002
Credits: SPI Team
This detector spectrum is based on one science window, summed for all 19
Germanium detectors of SPI.
|
6 NOV 2002
Credits: IBIS Team
PICsIT detector shadowgrams for single (left) and multiple (right) events.
Only 3 out of the 8 modules have their VETO system working. The image shows
how the VETO system reduces efficiently the background noise by suppressing
the events entering the detector from behind.
|
6 NOV 2002
Credits: JEM-X Team (N.J. Westergaard, DSRI Copenhagen)
Deconvolved image of the Cen X-3 region with a source visible close to
the position of Cen X-3.
|
6 NOV 2002
Credits: Volker Beckmann for the SPI Team
First processed gamma-ray data of the background sky as obtained
by SPI and using the SPIROS analysis software. The apparent source
(lower right) found by the iterative procedure of the SPIROS (v. 3.6)
analysis software is not significant.
|
5 NOV 2002
Credits: Volker Beckmann for the SPI Team
First processed gamma-ray data of the background sky as obtained
by SPI and using the SPISKYMAX analysis software.
The three symmetric features are spurious.
|
29 OCT 2002
Credits: Andreas von Kienlin for the SPI Team
The SPI anticoincidence system (ACS) detects it's first gamma-ray burst on
October 27, 2002 around 8:34 UT.
The burst is revealed already in the overall counting rates of the SPI ACS
with 50 ms time resolution (upper figure). Calculating the
average over 10 time bins the burst becomes clearly visible (lower figure).
The time of the rise of the GRB is identical to the time of
the burst GRB 011027 reported by the GCN.
|
28 OCT 2002
Credits: Peter Kretschmar for the JEM-X Team
Binned detector spectra for the first three science windows seen by
JEM-X 2, all with a default PHA-to-PI conversion. These plots just show
the evolution of the spectra with increasing high voltage.
|
28 OCT 2002
Credits: Peter Kretschmar for the JEM-X Team
Shadowgram based on the corrected positions of the second stretch
of data taking. This essentially shows the expected smooth shape with
a rim brightening and gaps where the calibration source events have
been taken out by on-board processing.
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25 OCT 2002
Credits: Miguel Mas Hesse (LAEFF-INTA Madrid) for the OMC Team
The second complete field of view (5x5 degree) sky image of the OMC, in the
area of the Large Magellanic Cloud. This image has been obtained combining
three 10 sec and three 16 sec exposures.
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22 OCT 2002
Credits: Miguel Mas Hesse (LAEFF-INTA Madrid) for the OMC Team
Sharp optical image taken by the optical monitoring camera (OMC) just after
the opening of the instrument cover.
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21 OCT 2002
Credits: IBIS Team
ISDC operation status monitoring (OSM) display of the first data
collected by the PICsIT detector layer of IBIS. At the top left is a lego plot
of all single events, on the right a single event detector spectrum and the
corresponding shadowgram images at low, medium and high energy are shown below
(from left to right, respectively).
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