Istituto di Astrofisica Spaziale e Fisica CosmicaIstituto di Fisica dello Spazio Interplanetario...

Istituto di Astrofisica Spaziale e Fisica Cosmica Istituto di Fisica dello Spazio Interplanetario

Roma, 15 Dicembre 2003Marco Feroci

Marco FerociIstituto di Astrofisica Spaziale e

Fisica Cosmica - Rome

Recent Activity at IASF/Rome on Microquasars and

Soft Gamma Repeaters



Microquasars:Galactic Jet Sources, (often) showing apparent superluminal motion of the ejecta.

Stellar-mass equivalent of the distant quasars, representing a unique laboratory to study the same Relativistic Physics, with much higher fluxes and much shorter timescales (by a factor of 10-6).

• SAX J1819.2-2525 ( =V4641 Sgr)

• GRO J1655-40

• XTE J1748-288

• GRS 1915+105



SAX J1819.2-2525the only BHC discovered by the BeppoSAX/WFC

RXTE, giant flare on 15 Sept 1999 (Wijnands & Van der Klis 2000)

BeppoSAX NFI, 13 March 1999, spectrum of quiescent emission @12 mCrab (in’t Zand et al. 2001)

The optical counterpart revealed the mass of the two objects in the

binary system: 8.7MBH 11.7 M© and 5.5M28.2 M© for the companion star (B-star)

(Orosz et al., 2001)



A total of 65 dips collected with BeppoSAX WFC, preferably at orbital phases between 0.68 and 0.92.

GRO J1655-40 in the BeppoSAX/WFC

Kuulkers et al. ,

A&A 358 (2000) 215

At the same phase but on different orbits, dips are not observed: Time-dependent structures in the absorbing material.



XTE J1748-288: BeppoSAX and XMM-Newton

BeppoSAX and XMM-Newton search for the quiescent counterpart: only Upper Limit at 10-14 erg cm-2 s-1 (assuming PL with =2 and NH=5x1022 cm-2).

1st Jet: subluminal2nd Jet: superluminal

VLA

BATSE

RXTE/ASM

Bob Hjellming, Private Communication



GRS 1915+105 – Highlights from BeppoSAX Campaigns 1996-2000Evidence for Inner Accretion Disc Disappearance

Feroci et al., A&A 351 (1999) 985

Spectral Deconvolution of X-ray Data: Multi-T BB from an Accretion Disc + PL

NO Disc !

BeppoSAX MECS

Ryle Telescope



GRS 1915+105 - Highlights from BeppoSAX Campaigns 1996-2000 The Largest Multifrequency Campaign (10 days!)

X-rays: OSSE, BATSE, ASCA, BeppoSAX

Infrared: NTT/SOFI, Calar Alto

Mm: NMA

Radio: VLA, GBI

BeppoSAX MECS

BeppoSAX PDS

NOT Detected by ASCA!

Ued

a et

al.,

Ap

J 57

1 (2

002)

918



GRS 1915+105 – Highlights from BeppoSAX Campaigns 1996-2000A Relativistic Iron Line from the Accretion Disc

Martocchia et al., A&A 387 (2002) 215

Line profile not consistent with a (symmetric) broad Gaussian line. Relativistic Disc Line Required. Emitting orbit larger than the innermost stable orbit: Schwarzschild and Kerr Metrics undistinguishable.



GRS 1915+105 – First View with INTEGRALHannikanen et al., A&A 411 (2003) L415

JEM-X2 (3-20 keV)

IBIS/ISGRI (20-450 keV)

JEM-X2 (3-20 keV)



Soft Gamma RepeatersRecurrent Transient Sources, emitting highly super-

Eddington flares of Hard-X/Gamma-rays, lasting from ms to minutes, and spanning 4-5 decades in luminosity.

They are the most convincing Magnetar candidates: isolated neutron stars, hosting the largest known Magnetic Fields in the Universe (~1014-15 Gauss).



SGRs at IASF/RM1998 Aug 27 Giant Flare from SGR 1900+14 with the

BeppoSAX Gamma Ray Burst MonitorFeroci et al., ApJ 515 (1999) L9 Feroci et al., ApJ 549 (2001) 1021

Emission from a Trapped Fireball in a Magnetar’s Magnetosphere:

Lx(t)=Lx(0) (1-t/tevap)a/(1-a)



SGRs at IASF/RMThe Intermediate Flare of 2001 Apr 18 from SGR1900+14

Woods et al., ApJ 596 (2003) 464 Guidorzi et al., A&A in press

Feroci et al., ApJ 596 (2003) 470

BeppoSAX GRBM

RXTE PCA

X-ray Afterglow (BSAX/RXTE/Chandra)



SGRs at IASF/RMWide Band Spectra of Short Bursts from SGR 1900+14

Canonical Optically Thin Thermal Bremsstrahlung

kT=29 keV

MECS

PDS

Two-Blackbody Law

kT1=3.5 keV kT2=9.0 keV

0

50

100

150

200

250

300

0 50 100 150

flux bb1 E-8 erg/cm^2 s

flux

bb2

E-8

erg

/cm

^2 s

0

1

2

3

4

5

6

0 1 2 3 4 5 6 7 8 9 10 11 12 13 14

Temperatura keV

N°b

urst

A. Caliandro, Laurea Thesis, Paper in preparation

Distribution of kT for 10 Short Bursts

Flux BB1 vs Flux BB2



SGRs in the Present of IASF/RM: INTEGRAL

15-40 keV 2003 Sept. 4 00:53:43 40-100 keV

15-40 keV 2003 Sept. 5 07:46:15 40-100 keV

15-40 keV 2003 Sept. 4 01:15:57 40-100 keV

Time (20 ms bins)

INTEGRAL AO2

PI of an AO2 Proposal for Serendipitous

detections of SGR bursts, co-PI of a

Proposal for Follow-up

observations of active SGRs

INTEGRAL/IBIS – Bursts from SGR 1806-20



SGRs in the Future of IASF/RM: SuperAGILE



COMPORTAMENTO MULTISPETTRALE DICOMPORTAMENTO MULTISPETTRALE DISORGENTI COSMICHE DI ALTA ENERGIASORGENTI COSMICHE DI ALTA ENERGIA

Franco GiovannelliIstituto di Astrofisica Spaziale e Fisica Cosmica,

CNR



LAVORI IN CORSOLAVORI IN CORSO

• Campagne di osservazioni dall’emisfero Nord e Sud per la ricerca delle correlazioni dirette tra Pulsatori X e SNRs (Italia, Spagna, Argentina)

• Studi teorici: Produzione di gamma di alta energia da HMXRBs. Processi di Accrescimento in Sistemi Binari (Italia,Polonia,Spagna,Russia)

• Campagne per la ricerca di exo-pianeti (Italia, Spagna, Russia)

• Campagne di osservazioni multibanda di Binarie X e Candidati Black Holes (Italia, Polonia, Spagna, Argentina)

• Campagne di osservazioni di sismologia stellare: Stelle sdO e sdB (Italia, Spagna)

SIXE: Spanish Italian X-ray Experiment (Fase-A Completata) - Fase-B: inizio in funzione decisioni politiche Spagna-Italia

Serie di Workshops (Italia, Germania, Spagna, USA): Multifrequency Behaviour of High Energy Cosmic Sources Frontier Objects in Astrophysics and Particle Physics The Bridge between the Big Bang and Biology



(Spanish Italian X-ray Experiment) SIXEFASE-A conclusa con successo: finanziata dal PNIE (Plan Nacional Investigación Espacial), Spagnolo

Banda X: 3-50 KeV Banda Ottica: B-V (Camera Ottica coassiale, tipo OMC di INTEGRAL) con lo stesso campo di vista. Piattaforma: MINISAT-02 (Spagna) Lanciatore: PEGASUS

FILOSOFIA: Osservazioni multibanda (X-Ottica) di POCHE sorgenticosmiche rappresentanti classi omogenee di oggetti.

TTexposureexposure x A x Aeffectiveeffective 10 101010 s cm s cm22

ORBITA Circolare: h = 500-600 Km i = 20°-25°/155°-

160°Stazioni diTerra: Maspalomas, INTA Malindi, ASI

Coma Cluster(30 giorni di misura)

1 modulo SIXE

OMC

Piattaforma MINISAT-02

IASF, UNI-BO, UNI-CT, UNI-PA, INAF-RM, INAF-CT, ENEA (Italia), IEEC, UPC, INTA, CNM (Spagna)



Vol. 67 Ni. 1/2 -70 Ni. 3/4 - 73 No. 1 - 73 No. 4

2003,… Chinese J. A&A (in press)

Multifrequency Behaviour of High Energy Cosmic Sources [F. Giovannelli & L. Sabau-Graziati (eds.)]

Serie: 1995, 97, 99, 2001, 2003,… Mem. SAIt

Serie: 1986, 1988,…., 2000, 2002,…, SIF

Frontier Objects in Astrophysics and Particle Physics

Franco Giovannelli & Giampaolo Mannocchi (eds.)

The Bridge between the Big Bang and Biology

Serie: 1999, 2002,….

(Franco Giovannelli (ed.)

*****

*****

CNR - Ufficio del Presidente, Volume Speciale

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