INTEGRAL Blazars
Catching Blazars in their ordinary life
A. De Rosa, S. Gianni’, L. Bassani, P. Ubertini
On behalf of the INTEGRAL AGN survey team
Outline
 Hard X-rays selected Blazars: ordinary vs
out of ordinary life
 Blazars in the INTEGRAL survey
 Characterizing the X-ray spectra:
broadband study
 Absorption properties in RL QSOs
 Finding peculiar objects: blue FSRQs/bulk
Compton emission
 X vs Gamma-rays properties: population
study with INTEGRAL, AGILE & Fermi
A. De Rosa - 7th AGILE workshop
 The future and
work
in progress
29 Sept 2009
Observing blazars in hard-X rays
Giommivariable
07
Blazars are extremely
rare believed that
it is- widely
objects (<5% all AGNs) that the
can
beenergy peak is
low
detected in hard-X (>10 keV)due
through
to
large area surveys: Because of the rarity and
the Synchrotron
low space density of blazars, "pencil
beam"
of relativistic
surveys (..) are poorly suitedradiation
for finding
blazars.. (Perlman 1998). electrons in a jet, while
the high
Two different waysenergy one is due to
• Long monitoring: average Inverse
flux states
Compton
scattering
(IC) of the
• ToO pointed observation: flaring
activity
same electrons
A. De Rosa - 7th AGILE workshop
29 Sept 2009
with a photon field
Out of ordinary vs ordinary life
3c454.3 Lucky ToO
Unlucky ToO..
Lucky detection
300 rev - 1000 days
Unlucky detection
Vercellone et al 2009
Pian et al. 2006
A. De Rosa - 7th AGILE workshop
29 Sept 2009
The sample
source
F20-40KeV F40-100keV
1ES 0033+59.5
RX J0137.7+5814
SWIFT j0218.0+7348
IGR J03532-6820
QSO B0836+710
MKN 421
4C 04.42
3C 273
3C 279
H 1426+428
MKN 501
SWIFT 1656.3-3302
PKS J1830-211
1RXS J192450.8-291437
QSO B1933-400
PKS 2149-306
Bl Lac
IGR J22517+2218
3C 454.3
1.3
0.4
1.2
1.3
2.4
25.6
0.8
10.4
1.1
1.0
3.1
1.4
2.4
0.9
0.5
1.2
1.3
1.3
9.4
0.9
<0.4
1.9
<0.8
4.2
19.4
1.8
12.3
1.4
1.1
2.1
2.1
3.2
0.8
1.0
1.7
1.5
2.3
12.8
z
0.086
2.367
type
HBL
BLlac
BLLac
2.172
FSRQ
0.03
HBL
0.965
FSRQ
0.158
FSRQ
0.5362 FSRQ
0.129
HBL
0.03366 HBL
2.40
FSRQ
2.705
FSRQ
0.352
FSRQ
0.965
FSRQ?
2.345
FSRQ
0.0686 BLLac
3.668
FSRQ
0.859
FSRQ
Characterising the X-ray spectra
 2-10 keV observations with XMM, Chandra, XRT
 We built a broadband spectrum 0.1-200 keV for 9
sources (more are coming)
Main Results
 Flattening wrt a power-law in the soft X-rays
range : If due tointrinsic absorption -> Nh vs
redshift evolution
 Finding peculiar sources: blue quasar candidate
IGR J22517+2218 - possible bulk Compton motion
in 4C 04.42
A. De Rosa - 7th AGILE workshop
29 Sept 2009
Characterising the X-ray spectra
Evidence of flattening below 2 keV (rest
frame) has been found in several high-z QSO
up to z=4.4 (Yuan et al. 2006)
Intrinsic curvature - absorption (cold/warm)
Clear trend NH vs z has been measured
Excess of emission has be found in very few
cases (Sambruna et al. 2006, Kataoka et al. 2007, De Rosa et al. 2008)
A. De Rosa - 7th AGILE workshop
29 Sept 2009
Characterising the X-ray spectra:
absorption
Ratio
Page et al. 05
data/continuum
power-law fit to
the energy band
above 2 keV
(observer
frame)
extrapolated
over the low
energy range
Statistical warning!!
A. De Rosa - 7th AGILE workshop
29 Sept 2009
Characterising the X-ray spectra:
bulk Compton emission in 4C 04.42?
PRELIMINARY! Energy Budget
AGILE
10 days
Fermi
1 month
BC= 2BLR/(1+z) ˜ 1 keV
De Rosa et al. 2008
LBC=4/3 c4UBLR2Ncold
˜ 1046 Ncold/Nrel,
LBC˜1045 erg/s
=> Ncold/Nrel ˜ 0.1
Multifrequency program:
Kataoka et al. 2007
INTEGRAL & AGILE
(quick look courtesy of L.
A. De Rosa - 7th AGILE workshop
Pacciani)+ public Fermi
29 Sept 2009
Characterising the X-ray spectra
Finding peculiar objects
Blazars spectral sequence (Fossati et. al 1998)?
The
peaks of the
Synch
A reanalysis
shows
& Bassani
IC
Shifting
thatcomp.
the
the
EC
et al.
2007
systematically
tothe
component in
higher
with
SEDfrequencies
bis well
decreasing
luminosity.
reproduced
by the XRed
(high
luminosity)
rays
data.These
peak?
and
blueSynch
(low
luminosity)
objects
are two
red
Synch peak?
blazars.
high luminosity
BL Lacs
blazars, in agreement
blue blazars
Strong
prediction:
withAthe
spectral
ROXA J081009.9+384757.0 z = 3.95
blue
powerfulNO
blue
powerful blazar…
sequence
blazar?
Maraschi et al. 2008
IGR J22517+2218, z=3.668 a gamma-ray lighthouse:
A. DeFSRQs?
Rosa - 7th AGILE workshop
•a high energy peaked
29 Sept 2009
•
FSRQsetred
Giommi
al. blazars
2007
X and Gamma-rays population
INTEGRAL
IBIS
Fermi
LBAS
AGILE
GRID
total
723
132
47
BLLac
7 (37%)
58 (56%)
4 (31%)
FSRQ
12 (63%)
42 (40%)
7 (54%)
unknown
21(AGNs?)
4
2
X and Gamma-rays population
I. photon index distribution: IBIS & LBAS
Abdo et al. 09
Ajello et al. 09
BAT 15-55 keV
FSRQs
BLlacs
X and Gamma-rays population
I. photon index distribution
BLLacs
Following the
spectral sequence,
gamma and X-ray
spectral ranges
match different
emission
processes in blue
and red blazars
FSRQs
A. De Rosa - 7th AGILE workshop
29 Sept 2009
X and Gamma-rays population
II. Luminosity vs redshift
FSRQs
BLLacs
Abdo et al. 09
F(20-100 keV)=1.2e-11 cgs
(0.8 mCrab), Crab like
spectrum
A. De
Rosa - 7th AGILE workshop
29 Sept 2009
Texp=2Ms
The future and work in progress
 Deep extragalactic fields will be observed in the 7th
INTEGRAL AO. New sources
 X-rays coverage: XMM large programme for
INTEGRAL (hard-X rays selected) AGNs is actually on
going, and we hope so for the near future.. AO9..?
 Simultaneous observations: Gamma-rays & TeV energy
ranges
 Define a complete sample of hard X-rays selected
blazars
 Populations study: are FSRQs and BLLacs two
separate classes?
 Implication on CXRB in hard X-rays and MeV energy
range
A. De Rosa - 7th AGILE workshop
29 Sept 2009
Everything unexpected…
Thanks for your attention
A. De Rosa - 7th AGILE workshop
29 Sept 2009