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INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

Laura BarragÀn. Universidad Complutense de Madrid
Tutors: Erik Kuulkers & Peter Kretschmar


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

INTEGRAL: International Gamma-Ray Astrophysics Laboratory
· The payload · The mission · The project


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

INTEGRAL payload
· IBIS (Imager on-Board the Integral Satellite)
high resolution images of celestial objects of all classes. 15keV ­ 10MeV. ISGRI // PICsIT FOV ~ 8º x 8º

· JEM-X (Join European Monitor for X-rays)
3 ­ 35 keV Images FOV: 5º radius circle

· SPI (Spectrometer on Integral) · OMC (Optical Monitoring Camera)


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

INTEGRAL
Observation of various gamma-ray phenomena by combining fine spectroscopy with imaging and accurate positioning of celestial sources of gamma-ray emission.

Science objectives:
Compact objects
(White Dwarfs, Neutron Stars, Black Hole Candidates, High Energy Transients and Gamma-Ray Bursts)

Extragalactic astronomy Stellar nucleosynthesis

(Galaxies, Clusters, AGN, Seyferts, Blazars, Cosmic Diffuse Background)

(Hydrostatic Nucleosynthesis (AGB, WR Stars), Explosive Nucleosynthesis (Supernovae, Novae)) (Cloud Complex Regions, Mapping of continuum and line emission, ISM, CR distribution) (Transrelativistic Pair

Galactic plane and centre structure Particle processes acceleration
Plasmas, Beams, Jets)

Identification of high energy sources
Gamma-Ray Objects as a Class)

(Unidentified


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

The INTEGRAL Galactic Bulge monitoring program
Observe the region frequently and regularly investigate the source variability and transient activity on time scales of days to weeks and months relatively soft and hard energies

Get the data of IBIS/ISGRI and JEM-X fit to standard models: powerlaw & cutoffpowerlaw
-Have we missed something?

plot the parameters with time (revolutions)
- Global properties of the sources - Are there spectral changes?


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

Why IBIS/ISGRI & JEM-X?
Revolutions 287-429 MJD 53419-53646, 2005/02/18-2006/04/21 IBIS/ISGRI 20-60keV Mosaic

All the sources
SPI: bad resolution (2.5º)

Galactic center
(IBIS: Angular resolution: 12arcmin)

OMC: too many stars (optical !!)


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

Obtaining the data IBIS/ISGRI
81 sources 10 hours

JEM-X
12 more significant sources 1 hour


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

Data treatment
Cleaning for IBIS/ISGRI

· Collecting the sources
·

get images, spectra & light curves

Binning for JEM-X (PROGRAM) Parameters in each revolution
Fitting IBIS/ISGRI & JEM-X independently Fitting IBIS/ISGRI & JEM-X together

· Fitting with XSPEC:


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

The models:
Powerlaw: par1 = norm= N photon index of power law (dimensionless) photons keV­1cm­2s­1 at 1 keV

Cutoffpl: power law, high energy exponential cutoff par1 = power law photon index par2 = norm = N e-folding energy of exponential rolloff (in keV) Photons keV-1cm-2s-1 at 1 keV


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

The fitting:
GRS 1758-258
IBIS/ISGRI
Normalized counts s-1 keV-1

JEM-X
Normalized counts s-1 keV-1

Rev:0298

Cutoffpl

Strong source
Cutoffpl

Rev:0298

0

Energy (keV) Rev:0298

20 Cutoffpl

IBIS/ISGRI & JEM-X
Normalize counts s-1-1 keV-1 Normalizedd counts s keV-1

JEM-X IBIS/ISGRI

22

Energy (keV)

100

0

Energy (keV)

100


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

JEM-X
Normalized counts s-1 keV-1

Rev:0298

Cutoffpl

1A 1742-294
weaker source

IBIS/ISGRI
Normalized counts s-1 keV-1

Rev:0298

Cutoffpl

0

Energy (keV)

20

IBIS/ISGRI & JEMX

Rev:0298

Cutoffpl

Normalized counts s-1 keV-1

22

Energy (keV)

JEM-X IBIS

100

0

Energy (keV)

100


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

What the program does:
Ignores the bad energies: compromise Fits the models (adding a constant when we have both detectors) Asks for the detection significance Plots the fitted spectra and saves them Saves the fittings Saves the parameters and errors for each source and model

Do tables per source or per revolution


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

Tables
1A1742-294_______ _________________ _________________ _________________ _________________ _________________ _________________ _________________ _________________ _________________ _________________ 4U1722-30________ _________________ _________________ _________________ _________________ _________________ _________________ _________________ _________________ _________________ _________________ 0287_ _____ _____ _____ _____ _____ _____ _____ _____ _____ _____ 0287_ _____ _____ _____ _____ _____ _____ _____ _____ _____ _____ ibis=>1.893674 jemx=>6.366455 ______________ ______________ ______________ ______________ ______________ ______________ ______________ ______________ ______________ ibis=>11.94899 jemx=>5.31 ______________ ______________ ______________ ______________ ______________ ______________ ______________ ______________ ______________ cutoffpl____ __________ __________ __________ __________ powerlaw__ __________ __________ __________ 1.01384583333___ 48__ ________________ ____ ________________ ____ ________________ ____ ________________ ____ 1.6486877551____ 49__ ________________ ____ ________________ ____ ________________ ____ HighECut___ 3.04827_____ 2.46647_____ PhoIndex___ 0.339208____ -1.03229_____ norm______ 0.0440495___ 0.0204574____ factor______ 177.163_____ 0___________ 3.76889_____ 0.202403___ 0.0848622__ 665.753____

PhoIndex__ 2.60637_____ 2.52898_____ 2.68574______ norm______ 1.30568_____ 1.10451_____ 1.54277______ factor______ 45.9245______0__________ 94.7367_____

cutoffpl____ __________ __________ __________ __________ powerlaw__ __________ __________ __________

0.855120833333__ 48__ ________________ ____ ________________ ____ ________________ ____ ________________ ____ 0.835812244898__ 49__ ________________ ____ ________________ ____ ________________ ____

HighECut__ 497.52______ 0.0103426____ 500________ PhoIndex__ 1.99015_____ 1.60583______ 2.2178______ norm______ 0.0957875___ 0.0432066___ 0.159581____ factor_____ 1106.95______ 802.575_____ 1337.23_____ PhoIndex__ 2.08794_____ 1.88883_____ 2.30079_____ norm______ 0.116182____ 0.0720688___ 0.189047____ factor______ 1194.37_____ 865.344_____ 1681.61_____

Easy access to the data

COMPARISON

Combine the data in order to plot the parameters


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

FIRST SCIENTIFIC RESULTS
Plotting the parameters
(function of time)

GRS 1758-258
IBIS/ISGRI
HEC NCUT CUT HEC
CUT

JEM-X

NCUT

2 CUT

R_

PL



NPL

2 PL

D.S.

D.S. R_

R_

2

PL

NPL



PL

R_

2 CUT

0287

0295 0297 Revolutions

0299

0287

0295 0297 Revolutions

0299


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

Both IBIS/ISGRI & JEM-X

D.S.J.

D.S.I. R_

2 PL

F

PL

NPL

PL

R_

2 CUT

F

CUT

NCUT



CUT

GRS 1758-258

HEC

0287

0295 Revolutions

0297

0299


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

1A 1742-294
HEC
CUT

NCUT

2 CUT

R_



PL

NPL

R_

D.S.

D.S.

R_

2 PL

2 PL

NPL



PL

R_

2 CUT

NCUT

CUT

HEC

0287

0295 0297 Revolutions

0299

0287

0295 0297 Revolutions

0299

IBIS/ISGRI

JEM-X


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

D.S.J.

D.S.I. R_

2 PL

F

PL

NPL

PL

R_

Both IBIS/ISGRI & JEM-X

2 CUT

F

CUT

NCUT



CUT

1A 1742-294

HEC

0287

0295 Revolutions

0297

0299


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

Future work:
Improve modeling
IBIS/ISGRI & JEM-X Rev:0298 Cutoffpl
Normalized counts s-1 keV-1

Ex: Red

2 CUT

~6

0

Energy (keV)

100


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

Future work:
Fit all the revolutions Plot the parameters we obtain Compare the different types of sources
(X-ray bursters, BH-binaries, etc)


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

CODED MASK TECHNIQUE
NO MIRRORS IN GAMMA RAYS NO OPTICAL-LIKE IMAGES

SLIDE

CODED MASK:
· · · Mask the opening of the telescope Measure its shadow on the detector orientation of the satellite & analysis of data from the detector determine position & intensity of sources

EXTRA

image of the observed sky:

a. b. c.

Coded mask Detector Field of view


INTEGRAL spectra of Galactic Bulge sources.

Laura BarragÀn

ANTI-COINCIDENCE SYSTEM
Blocked photon

SLIDE

Valid photon

MASK
Vetoed photon or particle

EXTRA

ANTI-COINCIDENCE