Analisi dati di archivio e Analisi dati di archivio e multifrequenza per multifrequenza per

l’Astrofisica delle Alte l’Astrofisica delle Alte Energie Energie

                      GiorgioGiorgio MattMatt(Dipartimento di Fisica, Università Roma Tre, Italy)(Dipartimento di Fisica, Università Roma Tre, Italy)

Six different fields:

Stars and Supernova RemnantsX-ray Binaries and Isolated Pulsars

Active Galactic NucleiGamma-ray Bursts

Clusters of GalaxiesCosmic Rays/Astroparticles (see Aloisio’s

talk)

Due to limited funds, not all proposals could be financed.

It is important to remark that the reports of the referees It is important to remark that the reports of the referees were positive also for many of the rejected proposals. were positive also for many of the rejected proposals.

Population studies (mean X-ray or γ-ray properties of classes of objects)

Multiwavelength observations of single objects or small samples (to study

specific problems)

Surveys (selection of sources, SEDs, etc.)

Follow-ups (to identify andcharacterize high energy sources)

“… saranno finanziati progetti di analisi di dati di archivio ottenuti da missioni spaziali UV, X,

Gamma o di Raggi Cosmici, ed analisi multifrequenza in cui i dati di alta energia siano

parte qualificante. “

Population studies Population studies

X-ray properties of young stars and protostars (Chandra, XMM, Maggio)

Type II Supernovae (UV Swift, Pian)

Timing properties of X-ray Binaries (Multi-Sat., Israel)

Mean spectral and timing properties of AGN (XMM, Cappi)

XLF of AGN and obscured AGN (XMM, Della Ceca)

T, z, A for Clusters of Galaxies (Swift, Tagliaferri)

Cool cores and T-profiles (Chandra, XMM, Ettori)

Comparison between long & short GRB (Multi-Sat., Ghirlanda, Piro)

Properties of X-ray Flashes (BeppoSAX, HETE2, Swift, Piro)

AGN population studiesAGN population studies

The CAIXA catalog and the Iwasawa-Taniguchi effect

The X-ray Luminosity Function of AGNThe X-ray Luminosity Function of AGN

The nature of X-ray selected BAL QSOsThe nature of X-ray selected BAL QSOs

CAIXACAIXA (a (a CCatalogue of atalogue of AAGN GN IIn the n the XXMM-Newton MM-Newton AArchiverchive

All Radio-Quiet AGN in targeted XMM-Newton p-n observations in the public archive (up to March 07) with:

> 200 counts in both 0.5-2 and 2-10 keV (rest frame) bands

< 1% pileup NH < 2x1022 cm-2

log(R)<1 (quasar) – log(R)<2.4 and log(RX)<-2.755 (Seyfert)

157 sources157 sources

All spectra reanalysed - If more than one obs. per source is available, the longest is chosen

- 6 and 20 cm fluxes for the whole sample- BH mass for 52% of the sources

- L-dependent bolometric correction adopted (Marconi et al. 2004)

Bianchi et al. 2009

The IT effect is highly significant157 data points (81 measures,

76 upper limits)ρ=-0.33 - P=4x10-5

Interpretation: decreasing of the covering Interpretation: decreasing of the covering factor of the torus with luminosityfactor of the torus with luminosity

log(EWFe)=(1.73±0.03) + (-0.17±0.03) log(LX,44)

Bianchi et al. 2007

Narrow core only !!

AGN population studiesAGN population studies

The CAIXA catalog and the The CAIXA catalog and the Iwasawa-Taniguchi effect Iwasawa-Taniguchi effect

The X-ray Luminosity Function of AGN

The nature of X-ray selected BAL QSOsThe nature of X-ray selected BAL QSOs

Using the XMM-Hard Bright Survey

Serendipitous Source (XMM-HBSS) AGN sample

the XLF of Absorbed and

Unabsorbed AGN has been derived

X-ray luminosity functions (XLF) of X-ray luminosity functions (XLF) of AGNAGN

4x1021<NH<1024

NH<4x1021Comparing the XMM-HBSS

Absorbed (4x1021<NH<1024)

AGN sample with an optical sample of Narrow

Line AGN including all absorbed AGN with

NH> 4x1021 cm-2 the XLF of Compton-thick

(NH>1024 cm-2) AGNhas been obtained

XLF of Compton-thick

(NH>1024 cm-2) AGN

Della Ceca et al. 2008

Compton Thin AGN vs. Compton Thick Compton Thin AGN vs. Compton Thick AGNAGN

Compton-Thick AGN NH>1024 cm-

2

----------------------------------------

Compton-Thin AGN NH<1024 cm-2

1.08±0.44

0.57±0.22

0.23±0.15

The fraction of Compton-Thick AGN decreases with Lx.

Possible interpretationas for the IT

effect !!!

Della Ceca et al. 2008

AGN population studiesAGN population studies

The CAIXA catalog and the The CAIXA catalog and the Iwasawa-Taniguchi effect Iwasawa-Taniguchi effect

The X-ray Luminosity Function of AGNThe X-ray Luminosity Function of AGN

The nature of X-ray selected BAL QSOs

Previous results

Optically­selsamples

New results

X-ray selected BALQSOs (at <z>=2) show lower X-ray absorption than purely optically selected ones, and soft X-ray weakness does not hold for any of them (Giustini et al. 2008).

⇒ outflows launched with different mechanism, or tail of the population?

27/03/09 HEAD 2004  ­ New Orleans  September 9, 2004

STUDY OF PERIODIC AND APERIODIC VARIABILITY STUDY OF PERIODIC AND APERIODIC VARIABILITY OF COSMIC X-RAY SOURCES OF COSMIC X-RAY SOURCES

 SATANASS & CATS @ BARSwift Automatic Timing ANAlysis of Serendipitous Sources & Chandra 

Archival Timing Survey @ Brera And Roma (Astronomical Observatories)

Systematic search and characterization of periodic signals in the new generation X-ray telescopes (XMM-Newton, Chandra, Swift, Suzaku) archives. Aim: Identification of intrinsically fainter and/or harder X-ray pulsators (including accreting and isolated objects)

(Nichelli et al. 09)

Swift XRT → 5 new candidaepulsators

Santos et al. 08

sample at z=0.1-0.3

sample at z=0.7-1.4

Searching for Cool Cores at high-zSearching for Cool Cores at high-z

A concentration parameter has been introduced to characterize the strength of the Cool Cores where the proper cooling time cannot be measured because a detailed description of the physical properties of the ICM is not possibleCSB = Sb(<40kpc) / Sb(<400kpc)

CCs are more frequent and strong locally. The majority of high-z clusters present mild CCs.

No objects with tcool < 3 Gyr at z>0.7:mergers (Cohn & White 05)but also AGN feedback

Searching for Cool Cores at high-zSearching for Cool Cores at high-z

Ghirlanda et al. 2009

2 complete (flux limited) samples of 79 short (T<2 s) and 79 long (T>2 s) GRBs.

Peak energy (keV) of the νFν

spectrum

Low energy photon spectral index

Low energy photon spectral index

Peak energy (keV) of the νFν

spectrum

Gamma-ray burstsGamma-ray bursts

ConclusionConclusion: in short GRBs and in the first 2 sec of long GRBs a : in short GRBs and in the first 2 sec of long GRBs a common emission common emission mechanism is at work mechanism is at work QuestionQuestion: What makes long GRBs go on?: What makes long GRBs go on?

1717

XRF

GRB

X-ray FlashesX-ray Flashes

• 2 XRF localized by BSAX and followed up by Chandra (Bloom et al. 2003)

• more redshift by SWIFT at z<3 (Gendre et al. 2007)

A search of GRBs in BeppoSAX WFC/GRBM shows that about 80% of the population is made of XRF/XRR

Multiwavelength Multiwavelength observations observations

The first true Seyfert 2 galaxy (XMM + optical, Cappi)

Thermal vs non-thermal components in Thermal vs non-thermal components in Clusters of GalaxiesClusters of Galaxies

(XMM & Chandra + radio, Giovannini)(XMM & Chandra + radio, Giovannini)

The SED and variability of Blazars The SED and variability of Blazars (Multi-(Multi-λλ, Raiteri, Caraveo), Raiteri, Caraveo)

NGC 3147NGC 3147z=0.009

The XMM spectra are well fitted by a power law (Г~1.6) absorbed

by the Galactic column density, plus a neutral

iron Kα line (EW~130 eV)

NO BROAD HNO BROAD Hαα or Hor Hββ!!

The flux of any broad component of the Hα would be at most 5% of the total Hα flux

The lack of broad optical lines in NGC3147 is an

intrinsic property of the source and not an

artefact of low S/N

NGC3147 is the first 'true' type 2 Seyfert NGC3147 is the first 'true' type 2 Seyfert galaxy galaxy

without the BLR (Bianchi et al. 2008)without the BLR (Bianchi et al. 2008)

Multiwavelength Multiwavelength observations observations

The first true Seyfert 2 galaxy The first true Seyfert 2 galaxy (XMM + optical, Cappi)(XMM + optical, Cappi)

Thermal vs non-thermal components in Clusters of Galaxies

(XMM & Chandra + radio, Giovannini)

The SED and variability of Blazars The SED and variability of Blazars (Multi-(Multi-λλ, Raiteri, Caraveo), Raiteri, Caraveo)

~ 435 kpc

SE X-raysubclump

New VLA data: discovery of diffuse, extended radio emission

most distantmost distant (z=0.45) (z=0.45) radio radio mini-halomini-halo

electron reacceleration triggered by turbulence in the CC (Gitti et al. 2002) + submerger ?

RXJ1347: subcluster merger in an otherwise relaxed cluster

The most X-ray-luminous clusterThe most X-ray-luminous cluster

XMM-Newton data: “normal” X-ray properties of a relaxed, CC cluster

Gitti et al. 2007a, 2007b

Multiwavelength Multiwavelength observations observations

The first true Seyfert 2 galaxy The first true Seyfert 2 galaxy (XMM + optical, Cappi)(XMM + optical, Cappi)

Thermal vs non-thermal components in Thermal vs non-thermal components in Clusters of GalaxiesClusters of Galaxies

(XMM & Chandra + radio, Giovannini)(XMM & Chandra + radio, Giovannini)

The SED and variability of Blazars (Multi-λ, Raiteri, Caraveo)

27/03/09 HEAD 2004  ­ New Orleans  September 9, 2004

SED of 3C 454.3 (z = 0.859) at various epochs, suggesting the presence of both a little blue bump in the optical band (emission from the broad line region) and a big blue bump in the UV-soft X-rays (thermal emission from the accretion disc), both becoming more prominent as the non-thermal contribution from the jet decreases (Raiteri et al. 2008).

Broad-band multiwavelength observations of the Broad-band multiwavelength observations of the blazar 3C 454.3blazar 3C 454.3

Detection by AGILE in November 2007. Significant day-by-day variability. A correlation analysis is consistent with no time lag between the gamma-ray and the optical flux variations. The simultaneous multifrequency observations strongly indicate that the main emission mechanism between 30 MeV and 30 GeV is dominated by inverse Compton scattering of relativistic electrons in the jet on the external photons from the broad line region. (Vercellone et al. 2009)

Surveys Surveys

• Selection of AGN, SEDs, search forCompton-thick AGN, ….

(Multi-λ, mainly X-rays and IR, Polletta, Fiore)

•Swift/Bat: all sky monitor and all sky Swift/Bat: all sky monitor and all sky survey (Swift, Caraveo)survey (Swift, Caraveo)

SED Modeling (separating AGN and SED Modeling (separating AGN and Host)Host)

Input : rest-frame SED [4-13 points]

Model: - Host (26 templates: ell., spirals, starbursts) - type 1 AGN (3 templates)(Polletta et al. 2007, Silva et al. 1998, da Cunha et al. 2008)

Model parameters [5]: L(Host), Host type, L(AGN), AGN type, AGN extinction (AV)

Total: Host+AGN

ResultsResults

Star-forming like AGNAGN2

AGN1 Sey1.8

NH from X-ray spectra

Star-forming like AGN

AGN2

AGN1 Sey1.8

AV applied to AGN component

SFGAGN2 AGN1 Sey1.8

L(AGN)/L(Host) increases with LX in all types, but at different rates

The SED classification correlates with the absorption in the X-rays (NH)

No or little obscuration in AGN1 and Sey1.8, high obscuration in AGNs, wide range of obscuration in SFGs

Polletta et al. 2008

Unveiling Obscured QSO in SWIRE surveyUnveiling Obscured QSO in SWIRE survey

44 Extreme Dust Obscured Galaxies (E-DOGs) in the SWIRE survey

Selection Criteria: X-ray Coverage, MIR/O>2000 and F(24μm)>1.3 mJy

Goal: Probe their nature of obscured AGN through direct X-ray spectral analysis

Source Breakdown:

- 23 sources detected in X-ray

- Obscured (NH>1022) 50-95%

- QSO2s ~50%

- 18% are promising C-thick QSO2s candidates

From the L(5.8μm) – L(X) relation:

NH estimation for 15 undetected

sources with IR AGN spectra:

- 40% QSO2s

- 20% CTQSO candidates

Conclusions: the selection based on high MIR/O and high F(24μm) applied to a large area survey like SWIRE is very efficient in finding out a large number of X-ray

obscured QSOs and CT candidates. Deepest observation are needed to confirm the nature of several CT

candidates (Chandra and XMM proposals)

Lanzuisi et al. 2009

Surveys Surveys

• Selection of AGN, SEDs, search forSelection of AGN, SEDs, search forCompton-thick AGN, …. Compton-thick AGN, ….

(Multi-(Multi-λλ, mainly X-rays and IR, Polletta, , mainly X-rays and IR, Polletta, Fiore)Fiore)

•Swift/Bat: all sky monitor and all sky survey (Swift, Caraveo)

BAT all-sky survey at IASF-BAT all-sky survey at IASF-PalermoPalermo

970 sources

Flux limit ~0.8 mCrab

748 identified sources

491 extragalactic objects

39 months of BAT data

Identification and characterization of INTEGRAL sources

(INTEGRAL + X-rays, Bassani)

Follow-ups Follow-ups

(1) Source Identification and (2) (1) Source Identification and (2) Classification Classification

Around 23% of the INTEGRAL detections are NEW HIGH ENERGY SOURCES which need:

IDENTIFICATIONFrom arcmin to arcsec localization

CLASSIFICATIONOptical/IR spectroscopy follow-up

to do this we need X-ray observations

ARCHIVAL DATA SWIFT/XRT DATA

an example: IGR J07597-3842

INTEGRAL/IBIS 18-60 keV image with 2.3’ error box superimposed

SWIFT/XRT 2-10 keV image with 3.5” error box superimposed

Optical spectrum : the source is a Sey 1.2

Using this method so far ~130 sources identified and classified

(http://www.iasfbo.inaf.it/extras/IGR/main.html)

AGN studies Objective: investigate the continuum

shape and the properties of the absorbing/reflecting medium

RESULTS: • Characterization of NH in a complete

sample of 88 AGNs (Malizia, in preparation)

- discovery of 2 Compton thick AGN (Malizia et al. 2009, Bassani et al.

2009)

• First broad band study of a sample of NLS1 galaxies hard X-ray

selected (Malizia et al. 2008)

3) Γ, Ec, R distribution in a complete sample of AGN of: Sey 1 (complete) and Sey 2 (uncomplete)

(Molina, in preparation)

Seyfert 1s

AGNAGN

27/03/09 HEAD 2004  ­ New Orleans  September 9, 2004

Example of Swift/XRT monitoring (0.2-10 keV) of 5 SFXTs during bright flares and ISGRI long term monitoring (20-60 keV) of a SFXT source. It is evident the different timescale flaring behaviour, significantly longer as observed by Swift/XRT (several days) with respect to IBIS (less than a day).

Sidoli et al. 2008a, 2009b, 2009c; Romano et al. 2008a, 2009b, 2009c

Supergiant Fast X-Ray Transients (SFXT)Supergiant Fast X-Ray Transients (SFXT)

ConclusionsConclusions

The quantity and quality of the projects demonstrate that the High

Energy Astrophysics Italian community is lively and enterprising.