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higher order series linesconfirm photoionization, excluding
contribution from collisional plasma
Important role of photoexcitation(resonant scattering:
Band et al. 1990, Matt 1994, Krolik & Kriss 1995)
Detection ofnarrow
Radiative Recombination Continua (RRC)
=>Low temperature gas
=>Photoionization
XMM-Newton 190 ks combined RGS spectrum
The high resolution
spectrum of Mrk3 is
unambiguously produced in a photoionized
gas:
-K lines dominant over
Fe L-RRCs
Resonant scattering is important:
-Fe L 3d-2p/3s-2p ratio
-K resonant/ forbidden ratio
Mrk3
Bianchi et al. 2006
Sako et al. 2000
Chandra HETGSSam
bru
na e
t al. 2
001 Circinus
Sch
urch
et a
l. 2004
XMM RGSNGC4151
What about the other Sy2s?
Most RGS spectra of Sy2s are dominated by emission lines with low or no continuum
Often, most of the ‘soft excess’is concentrated in single, very strong lines
which can be easily detected even insources with very low SNR spectra
Guainazzi & Bianchi, 2007
We produced the first catalogue of soft X-ray emission lines in a sample which includes all the type ≥ 1.5 AGN observed
byXMM-Newton RGS
CIELO-AGNCatalogue of Ionized Emission Line Obscured AGN
Guainazzi & Bianchi, 2007
69 objects<F0.1-2 keV> 10-13 cgs
OVIII Lyα detected in 50% of the sample OVII triplet in 40%
Many other lines from O, Fe, C, Si, Mg,
Ne, N detected in 15%
Guainazzi & Bianchi, 2007
CIELO confirms the results derived from the analysis of the brightest
sources Strong higher order lines
PhotoexcitationRRCs are:CommonCommon (detected in 40% o.t.s.)
NarrowNarrow (10 eV)
Photoionization
The stacked spectrum of
all the objects with
good SNR included in
CIELO confirms
these results
Main features (e.g. OVII and OVIII lines) are
also recovered in the stacked spectrum of
poor SNR objects
(~60% of the catalog)
NGC3393 – z=0.0125
NGC1386 – z=0.0029
Bia
nch
i et
al. 2
006
(+
6 o
ther
obje
cts)
Where is this gas located?
Circinus
Sm
ith &
Wils
on 2
00
1
NGC4151
Yang e
t al. 2
00
1
A close association between the soft X-ray emission and the NLR (traced by [OIII]) is observed both on large and small scale
The comparison between the Chandra and the HST images shows that the [OIII]/soft X-ray ratio is fairly constant along
with the radius, up to hundreds of pc. Photoionization models reproduce this behavior if ner-, with 2 (i.e. constant
ionization parameter). This is in agreement with NLR emission line ratios
(e.g. Kraemer et al. ’00, Kraemer & Crenshaw ’00, Bradley et al. ’04, Collins et al. ‘05).
Bianchi et al., 2007
What is this gas?
HST Chandra
110 pc
3 pc
In the immermost 110 pc:• low luminosity AGN: LX≈1039 erg s-1
• young stellar cluster: LX≈6×1038 erg s-1
NGC4303Jiménez-Bailón et al. 2003 NGC7130
Levenson et al. 2005
What about the starburst contribution?
Empirical diagnostic diagram based on high resolution spectroscopy
Guainazzi & Bianchi 2007
AGN
-Total LO≥1040 erg s-1
-OVII/OVIII≥1
So… AGN or starburst?
STARBURST
OVIII/OVII excess is NOT
coincident with star formation regions!Bianchi et al., 2007 NGC7582
… of course this is too simple
High-resolution spectroscopy IS fundamental to understand the physical properties of the gas in the AGN circumnuclear environment (as high-resolution imaging IS
fundamental to unveil its true location)
In obscured AGN, CIELO unveils mounting evidence for
Dominant role of AGN-photoionization,
Important role of resonant scattering,
Broadly constant ionisation parameter ...
on scales as large as a few hundreds parsec
ConclusionsConclusions
CIELO unveils a criterion to discriminate between AGN- and
starburst-dominated sources on the basis of the OVII(f)/OVIII