On behalf of the INTEGRAL Science Team · The Cat4 sources: the deepest picture of the soft gamma...

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On behalf of the INTEGRAL Science Team

INTEGRAL INTEGRAL overviewoverview

IBIS and SPI are the main instrumentsSPI optimised for spectra: 20keV-MeVIBIS ti i d f i i 17k V 10M Voverviewoverview IBIS optimised for imaging: 17keV-10MeV

IBIS is the primary surveysurvey instrumentIBISIBISIBISIBIS p y yyWide FOV (30x30 degrees) ISGRI detector mainly operates 17-600 keVSPISPISPISPI 600 keVSensitivity ~0.1mCrab for deep exposures (>10Ms)

SPISPISPISPI

JEM-X and OMC are the Monitors

Credit: ESA


IBIS: started hunting new IBIS: started hunting new γγ--rayray sources …sources …and, now monitoring weak old knownand, now monitoring weak old known, g, g

Takes advantage of the large FOV (~1000sq deg) for multiple source detection also in complex region (Galaxy Centre etc)source detection also in complex region (Galaxy Centre etc)

Unbiased search of the IBIS datasets: ~8 years of operations

Looking for weak persistent sources only visible on long timescales: spans a duration of > 2900 days 190Ms unprecedented long (no spans a duration of 2900 days 190Ms unprecedented long (no basic systematic errors ≈4.5σ limit averall)

Looking for transient sources on various timescales (ms to y)Looking for transient sources on various timescales (ms to y)

Follow-up of new sources in other waveband (25-30% are id ifi d)unidentified)

Overall analysis of all the sources: Spectra, timing, states


n y f u p , m ng,

What we get now…

What we promised in ‘93…


17-30, 30-60, 40-100 colours but also 100-300

WhyWhy so so wellwell?..?..ExposureExposure and and Endurance, Endurance, i.e.Sensitivityi.e.Sensitivitypp ,, yy

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The Cat4 sources: The Cat4 sources: the deepest picture of the soft gamma ray slythe deepest picture of the soft gamma ray slythe deepest picture of the soft gamma ray slythe deepest picture of the soft gamma ray sly

HMXBLMXBAGNAGNCVUnkn

GC


P. Ubertini, The INTEGRAL Legacy: Unveiling the soft gamma-ray skyCRIS – Catania, Italy, 13-17 September 2010

The The CatCat 4 4 sourcessources



The soft gammaThe soft gamma--ray sky according to IBIS…ray sky according to IBIS…> 700 > 700 sourcessources in the IBIS Sky (in the IBIS Sky (BirdBird et al, 2010), et al, 2010), todaytoday more more thanthan 1000…1000…


18-60 keV band

The soft gammaThe soft gamma--ray sky according to IBIS…ray sky according to IBIS…The The deepesdeepes imageimage ofof the SGR the SGR A*A* regionregion

20-40 keV band

INTEGAL view of the Galactic Centre in the 20-40 keV energy range, obtained from all IBIS observations of this region between 2003 and 2009, for a total exposure of 20 Ms. The main sources are indicated by black crosses. Most of them are X-ray binaries powered by accretion on neutron stars or stellar-mass black holes. The central source IGR J17456-2901 coincides with the position


stars or stellar mass black holes. he central source IG J 7 56 90 co nc des w th the pos t on of Sgr A*. The position of IGR J17475-2822 is compatible with that of the Sgr B2 molecular cloud (from Terrier et al., 2010, ApJ 719, 143).

INTEGRAL IBIS 20 – 60 keV images of the INTEGRAL IBIS 20 60 keV images of the Galactic Centre (7º × 2º) from 2003 until2009. Most of the sources are X-ray binaries and display strong time variability. display strong time variability.

The green circle shown in the top panel corresponds to the position of the molecular cloud Sgr B2. The p gassociated hard X-ray source, IGR J17475-2822 shows a clear decline in flux during the 7 years of monitoring (Terrier et al., 2010, ApJ 719, 143).


g p

Krivonos et al.,2010, 521 sources, 17-60 keV band

From http://hea.iki.rssi.ru/en/index.php?page=rsdc 7 years map with p p p p g y pstellar density field overlapped. The green contours are isophotes of the 4.9 micron surface brightness of the Galaxy (COBE/DIRBE) revealing the bulge/disk structure of the inner Galaxy. The near-infrared brightness of


g y gthe galaxy traces also the hard X-ray ridge emission

Comparison to previous catalogsComparison to previous catalogs



Spectral Informations: Spectral Informations: d t i 14 b dd t i 14 b daveraged spectra in 14 energy bandsaveraged spectra in 14 energy bands

17 20 kev17-20 kev

200 300 kev



200-300 kevHigher energy

Comparison of Cat 4 to previous IBIS catalogs: a substantial fraction of ‘new’ unknown sources are usually identified as a substantial fraction of new unknown sources are usually identified as

AGNs via optical, IR or X-Ray follow-up observations:

Th hi h n l f INTEGRAL nd S ift/BAT ill The high-energy survey legacy of INTEGRAL and Swift/BAT will therefore remain unique for the next decades and the "decade long" unbiased INTEGRAL survey will be of seminal importance for

l extragalactic astronomers


Figure 14: Expected number of sources catalogued by INTEGRAL until 2014

The more recently available BAT catalog (Cusumano et. al, Swiftworkshop, 2010), complementcomplement thethe IBISIBIS surveysurvey withwith 10491049 sourcessourcesIn fact the Extragalactic sources account for 62.5% of the totalwhile the galactic ones only for 22.5% being the unknown about15%. i.e. half of the IBIS unknown population.f f p p


NSs in HMXBs: NSs in HMXBs: Examples of important Examples of important unexpectedunexpected INTEGRAL discoveriesINTEGRAL discoveriespp

and possible association with Gamma ray sourceand possible association with Gamma ray source1. the highly absorbed (mostly transient) binary systems as

a new class of HMXB: slow pulsar (100 1000s period) in a new class of HMXB: slow pulsar (100-1000s period) in a giant cocoon (Nh often >23)

2. the Super-giant Fast X-ray Transients: a new (sub) class of super-giant HMXB (wind accretion in blobs?)

XMM

IGR J16318-4848

IGR J174544-2619 2 hr flare

XMM

INTEGRAL/IBIS

R Walter et al A&A 411 L427 2003


R. Walter et al., A&A 411, L427, 2003

V. Sguera et al., ApJ 646, 453 2006

HighHigh--energy sources appear on all timeenergy sources appear on all time--scalesscales

Sources can appear in ~ 1000sSources can appear in ~ 1000s

Or in a few daysOr in a few days



Or in a few weeks

Pietro Ubertini, SAIT, Napoli, May 6th 2010, Page 19

For this INTEGRAL result last month..

the COSPAR Bureau, with the consent of the Russian A d f S i h d d th Z ld i h M d l tAcademy of Sciences, has awarded the Zeldovich Medal to:

D Vit S (It l )Dr. Vito Sguera (Italy)b f th I t l/IBIS T member of the Integral/IBIS Team

“for his research on the new class of soft gamma-ray for his research on the new class of soft gamma-ray sources, namely Super Giant Fast X-Ray Transient, of seminal importance for high energy astrophysics studies”p g gy p y


Electron-Positron Annihilation in MW

508 514 keV5

2 10700002.1 −±=E

508-514 keV

Knoedelseder; Jean; Bouchet; Teegarden; Weidenspointner

2cme


Knoedelseder; Jean; Bouchet; Teegarden; Weidenspointner..ChurazovChurazov et al, 2005, 2010 et al, 2005, 2010 + present viewgraphs+ present viewgraphs

Diversity of positron sourcesy f p

Nucleosynthesis:yMassive stars (SN II, WR: e.g., 26Al) ◄Low mass stars (SNIa - 56Co, Novae - 13N)G B ( h h i C l & K k 2010)Gamma ray Burst (recent hypothesis Calvez & Kusenko, 2010)Cosmic rays + ISM (π+) ◄

Jets (microquasars, pulsars, ms pulsars)

Supermassive black hole (Sgr A*), episodic accretion(Cheng et al 2006, 2007)

Dark matter annihilation ?(Boehm et al ; Hooper et al 150 papers)


(Boehm et al.; Hooper et al., …. 150 papers)

Diversity of positron sourcesy f p

Nucleosynthesis:yMassive stars (SN II, WR: e.g., 26Al)Low mass stars (SNIa - 56Co, Novae - 13N) ◄G b ( h h i C l & K k 2010Gamma ray bursts (recent hypothesis Calvez & Kusenko, 2010Cosmic rays + ISM (π+)

Jets (microquasars, pulsars, ms pulsars)

Supermassive black hole (Sgr A*), episodic accretion(e.g. Cheng et al.)

Dark matter annihilation ?Impossibile v isualizzare l'immagine. La memoria del computer potrebbe essere insufficiente per aprire l'immagine oppure l'immagine potrebbe essere danneggiata. Riavviare il computer e aprire di nuovo il file. Se v iene visualizzata di nuovo la x rossa, potrebbe essere necessario eliminare l'immagine e inserirla di nuovo.

(Boehm et al.; Hooper et al., …. 150 papers)

INTEGRAL spectra from the central galactic radian. Black: total emission of resolved point sources; Blue: total

INTEGRAL spectrafrom the central galactic radian po nt sources; Blue total

diffuse emission; Magenta: 511 keV annihilation radiation (positroniumcontinuum and line emission); Accreting magnetic with Dwarf

from the central galactic radian

total emission of resolved point sources

uum m );Green: emission from the galactic ridge resulting from interstellar particle interaction; Red: accreting

emission from galactic ridge resulting from interstellar particle interaction

total diffuse emission

g g f

; gmagnetic white dwarfs (Bouchet et al., 2010, to be submitted). The vertical dotted lines indicate the

511 keV annihilation: positroniumcontinuum and line emission

narrow lines.


Inserts show the fine l i spectroscopy analysis

of selected lines (from Jean et al., 2006, A&A 445 579 W A&A 445, 579; Wang et al., 2007, A&A 469, 1005; Wang et al., 2009 A&A 496 713)2009, A&A 496, 713)


Doppler shift of the 26Al gamma-ray line at 1.8 MeV due to large-scale galactic rotation. First indicated in 26Al INTEGRAL data from the first 2 years of observations (Diehl et al., 2006, Nature 439, 45), now, as shown in the figure, the line shift is , ), , g ,strongly significant using data from 5.5 years of observations (Kretschmer et al., 2010, in preparation).


Work in progress: 150-300 keV all sky map: ~100 high energy sources: pulsar, PWN, microQSO, Binary Black-

Holes NS systems andHoles, NS systems…and..

the diffuse Soft-gamma ray background granularity and its possible connection with ALPs connection with ALPs ….


INTEGRAL SCIENTIFIC PUBLICATIONSINTEGRAL SCIENTIFIC PUBLICATIONS

Until June 2010, INTEGRAL observations have resulted in:

545 refereed papers..now about 100/year1318 total publicationsm re th n 74 PhD theses since l unch ndmore than 74 PhD theses since launch, andother 23 PhD on-going theses



Proposal due by 8 OctoberProposal due by 8 October…MORE to come at the next Integral Workshop in Dublin 27-30 September..7 pt m r..



ThanksThanks….



On behalf of the INTEGRAL Science Team · The Cat4 sources: the deepest picture of the soft gamma...

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