Anatomy of the AGN in NGC5548: Discovery of a - Cosmos

Anatomy of the AGN in NGC5548: Discovery of a fast and massive ou>low – Overview Massimo Cappi (INAF/IASF-Bologna)
and the NGC5548 collabora3on Outline
l.o.s Ø  A massive multifrequency
campaign (2013 campaign, not
2014 STORM)
Ø  An unexpected strong, mildly
ionized, variable (but long-lasting)
multilayer absorber
Ø  A new high-v UV BAL
Ø  A long-lasting event that shields the
larger scale WA
Ø  A possible model (~disc wind)
Ø  An international press release
Ø  A nice/funny cartoon movie
Overview on behalf of the NGC5548 Collabora8on 5 papers published/in press: -­‐ Kaastra et al., ‘14, Science -­‐ Mehdipour et al.. ‘15, A&A -­‐ Arav et al. , ‘15, A&A -­‐ Ursini et al. , ‘15, A&A -­‐ Di Gesu et al. , ‘15, A&A 5+ under prepara3on: -­‐ Cappi et al. -­‐ Whewell et al. -­‐ Mehdipour et al., II -­‐ Ebrero et al. -­‐ Kriss hole
et al. in NGC 5548
A fast and long-lived outflow from the supermassive black
Authors: J.S. Kaastra1,2,3*, G.A. Kriss4,5, M. Cappi6, M. Mehdipour1,7, P.-O. Petrucci8,9, K.C.
Steenbrugge10,11, N. Arav12, E. Behar13, S. Bianchi14, R. Boissay15, G. Branduardi-Raymont7, C.
Chamberlain12, E. Costantini1, J.C. Ely4, J. Ebrero1,16, L. Di Gesu1, F.A. Harrison17, S. Kaspi13, J.
Malzac18,19, B. De Marco20, G. Matt14, K. Nandra20, S. Paltani15, R. Person21, B.M. Peterson22,23,
C. Pinto24, G. Ponti20, F. Pozo Nuñez25, A. De Rosa26, H. Seta27, F. Ursini8,9, C.P. de Vries1, D.J.
Walton17, M. Whewell7.
Massive (deep) mul8frequency campaign(s) Basic Idea(s): Ø  Gain the deepest view of Seyfert ou>lows via long simultaneous UV/soW X-­‐ray observa3ons Ø  Broad band (UV-­‐to-­‐100 keV) monitoring •  ou>low variability •  con3nuum/reflec3on variability Ø  Sources: Mrk509 (past), NGC5548 (finalising now), NGC7469 (future, PI Behar). Sources must be i) variable, but not too variable; ii) Strong/clear WA in X and UV; iii) X-­‐ray brightest è
XMM-­‐Newton + HST-­‐COS driven campaign(s) A massive mul8frequency campaign on NGC5548 The 2013/14 Campaign
Chandra
INTEGRAL
NuSTAR
SWIFT
HST/COS
ents need to be
at fulfils all re-
and L are
ors of 2, 5 and
EDD
Start of STORM Rev. campaign (presented in Kriss and Edelson talks) XMM
Swift
−40
XMM−Newton
HST/COS
−20
0
20
time relative to first XMM−Newton observation (days)
40
Fig. 1: Proposed observing schedule. At time zero the core campaign
starts (40 days), with 12×50 ks XMM-Newton observations at days 0,
8, 16, 20, 24, 28, 30, 32, 34, 36, 38, 40 and 29×1.5 ks Swift obser-
Surprise! a heavy, neutral, variable absorber along the l.o.s. to NGC5548 (All) XMM Observa3ons of NGC5548 – PN spectra Archival Observations
1
0.1
New Monitoring Campaign
0.01
normalized counts s−1 keV−1
10
1) 24/12/2000
2) 09/07/2001
3) 12/07/2001
4) 22/06/2013
5) 30/06/2013
6) 07/07/2013
7) 11/07/2013
8) 15/07/2013
9) 19/07/2013
10) 21/07/2013
0.5
11) 23/07/2013
12) 25/07/2013
13) 27/07/2013
14) 29/07/2013
15) 31/07/2013
16) 20/12/2013
17) 04/02/2014
1
2
Energy (keV)
5
10
A cold, strong, absorber 100
Hard X vs Soft X
(A)
INTEGRAL 2013
0
−10
2
1
10 10−4
RGS 2013
10−3
counts s−1 keV−1
10
pn 2013
0.1
Photons m−2 s−1 Å−1
XMM
Chandra 2002
0.01
NuSTAR
NuSTAR 2013
1
•
•
10
Energy (keV)
100
10
20
50
Energy (keV)
Low flux variability above 10 keV (~10%)
Apparent spectral curvature (See Francesco Ursini’s Talk) in Session III A soW, scanered component (NLR) M. Whewell et al.: Anatomy of the AGN in NGC 5548. ZZ
Fig. 1. The 2013-14 770 ks stacked RGS spectrum of NGC 5548 (observed frame). The strongest emission lines are labelled. The data points are
Whewell et al., in prep. RGS average spectrum 770 ks Dominated by He-­‐like triplets of OVII, CVI, and N, and RRCs Cloudy model fit à log Nw~22.9, logXi~1.4, vout~300 km/s and distance~14pc Narrow lines not affected by obscurer à small covering factor of the obscurer (as seen from accre3on disc) i.e. NLR or ENLR (and consistent with “classic” WA in NGC5548) Timing Analysis A3 M1 M2 M3
M4
M5
M6
M7 M8 M9 M10 M11 M12 M13 M14
2 1
2
5
1
10
A2
0.2 0.5 1
H/S
H(2 10 keV)
S(0.3 2 keV)
A1
0
2×105
4×105
Time (s)
6×105
8×105
SHORT-TIME SCALE VARIABILITY OF NGC 5548
FIG. 1:AFvar
on short
time scales
Timing nalysis: Frac3onal variability on long and short 3mescales en 1-2 (2-25 ks).
0.03
0.02
Fvar
0.2
0.3
0.01
0.1
Fvar
0.3
0.04
Fig. 1 shows the fractional variability of NGC
5548 on the time scales 25-2 ks (i.e. the
variability within each observation). This can be
computed integrating the power spectrum of the
source over the corresponding range of
frequencies, extracting the square root and
normalizing the result for the count rate of the
source (see Vaughan et al, 2003, MNRAS, 345,
1271).
The Fvar of the short time scales, shows low
0.5
1
2
5
10
but significant intrinsic variability over the entire
E (keV)
0.3-10 keV
noting
0.5 energy
1 band.
2 It is worth
5
10 that
the observed spectral
shape is similar to that of
E (keV)
the long
scale
FIG. 1: Fvar on short time scales
FIG. time
2: Fvar
onFvar
long (45-4000 ks, black)
(black
in Fig.ks,
2) red)
with a peak between 1-2 (2-25 ks).
anddata
on points
short (2-25
keV time
and an
approximately
scales.
constant Fvar below 1 keV, where the effects
m ① 
of the
X-rayoobscurer
on thebspectrum
thekeV (Variable cold absorp3on) Most f variability etween of1-­‐5 low② 
source
are stronger.
Constant narrow FeK emission (and therefore reflec3on) 0.2
Fvar
of the
observations,
which 0.3-­‐0.8 keV ~ 8-­‐10 keV (Par3al covering) ③ single
Variability between ariability
power from slonger
④  Variability hape time
on sscales
hort 3isme scale similar to longer-­‐term ⑤  Consistent with only/mostly red-­‐noise leak litude depends on the amount of intrinsic
Spectral Analysis: From an unabsorbed archetypical type-­‐1 source 10−4
10−3
Comp% -­‐ bbody Pounds et al. ‘03 Krongold et al. ‘10 Brenneman et al. ’12 10−5
10−6
keV2 (Photons cm−2 s−1 keV−1)
0.01
Archival (unobscured, just WA) spectra 0.5
1
2
Energy (keV)
5
10
10−5
Spectral Analysis: To a source absorbed by a complex mul3layer absorber 1
10
Energy (keV)
keV (Photons cm s keV )
1
XMM -­‐ PN Nustar (simultaneous, 3 obs) Par<ally covering (fcov~0.8,0.3) mildly ionized (logXi~-­‐1.5,-­‐4) mul<layer (logNw~22,23) Pexmon (R≈0.4) 10−3
Cloudy(sca%ered) 10−4
10−5
Comp% -­‐ bbody 2
−2 −1
−1
0.01
ratio
2013 campaign 10−6
1.1
0.9
1
10
Energy (keV)
A high-­‐velocity UV BAL Fig. S1.
CIV Best-fit emission model to the region surrounding the C IV emission line in the average
spectrum of NGC 5548 from summer 2013. The data (black) have been binned by four
Strong UV troughs up to 5000 km/s Fig. 2. UV absorption lines in the COS spectrum of NGC 5548. (A) The combined normalized
As presented spectra
in Jerry riss’s talk, rom STORM project, these lines EW are found from K
summer
2013
havefbeen
binned
for clarity.
For the Si IV,
C IV, and
N V doublets,
red and blue profiles are registered relative to the respective red and blue wavelengths of the
to correlate wthe
ith absorber covering factor and an3-­‐correlate with UV flux doublets. The smooth solid lines are fits to the broad absorption line profile with 1:1 ratio for the
dotted
vertical lines show
à Consistent doublets.
with bThe
eing shielding gas the locations of the narrow velocity components defined
in (20), with an additional component 6 near 0 velocity.
Fig. S4
A long-­‐las3ng obscura3on event XMM 2013/14 campaign More in Mehdipour et al., ‘15, A&A; and his poster! (F6) X-ray and UV light curves of NGC 5548 obtained with Swift between 2005 and 2014.
A shielded Warm Absorber at least 6 components
Lower ionization species in 2013
than 2002 while UV 50% larger?!?!
Arav et al., ‘15, A&A A shielded Warm Absorber Arav et al., ‘15, A&A (One) Possible model: an accre3on disc ou>lowing wind Absorber/obscurer velocity (up to 5000 km/s) + variability (within 2 days) + par3al covering (30-­‐80%) Obscurer + long-­‐las3ng event (>2.5 years) + loca3on (n sensi3ve lines + Trec prop. 1/n) + poloidal (inclina3on=30deg) à  Best consistent with origin in accre3on disc wind (btw ac3ng also as self-­‐shielding gas) (w.r.t distant torus or small BLR clouds) N.B: L
kine3c (absorber+WA) s3ll <0.5% Lbol in this source Interna3onal Press Release(s) open in browser
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Il super vento che oscura il buco nero
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:‫הפרעות אכילה של חור שחור‬
‫חוקרי הטכניון בצוות בינלאומי שגילה זרם‬
‫גז מהיר המסתיר חור שחור על מסיבי‬
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IN EMBARGO FINO ALLE ORE 20.00 DI GIOVEDI’ 19 GIUGNO 2014
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Un potente flusso di gas che si allontana dal buco nero supermassivo nel centro della galassia
NGC 5548 alla notevole velocità di 18 milioni di chilometri orari è stato individuato da un team
internazionale di ricercatori, tra cui due dell’INAF. La scoperta, pubblicata sulla rivista Science,
getta nuova luce riguardo le teorie attuali sul funzionamento dei buchi neri e l’interazione di
questi ‘mostri cosmici’ con le galassie che li ospitano.
Un team internazionale di astronomi, tra cui i ricercatori INAF Massimo Cappi e Alessandra De
Rosa, ha scoperto un potente flusso di gas che fuoriesce ad alta velocità dalle regioni prossime
al buco nero supermassivo nel cuore della galassia NGC 5548, che si trova in direzione della
costellazione di Boote, a 240 milioni di anni luce da noi. La presenza di questo violento ‘soffio’,
che si propaga a 18 milioni di chilometri orari, oscura gran parte della regione dove il buco
nero emette la radiazione più energetica, arrivando a bloccare il 90 per cento dei raggi X
prodotti e buona parte di quelli ultravioletti. Arriva così da questo studio, ottenuto utilizzando i
telescopi spaziali di ESA e NASA XMM-Newton, Hubble Space Telescope, Swift, NuSTAR,
Chandra, INTEGRAL, e telescopi da terra, ovvero la migliore strumentazione oggi disponibile
per questo tipo di indagini, una convincente conferma osservativa alle teorie che prevedono
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l’espulsione
diAPIpotenti venti di gas e polveri ad alta velocità da parte
delle zone centrali dei
nuclei galattici attivi. Oltre ad essere di interesse per comprendere meglio i meccanismi di
funzionamento dei buchi neri, questi processi potrebbero anche avere un ruolo determinante
nella complessa interazione tra i buchi neri supermassivi e le galassie che li ospitano.
‫החוקרים זיהו זרם גז סמיך הנע במהירות כלפי חוץ וחוסם‬
‫ שמפיץ החור השחור העל מסיבי שבמרכז‬X ‫ מקרני ה‬90%
‫הגלקסיה‬
‫ ראש מכון אשר לחקר החלל וד"ר שי‬,‫ ובהם פרופסור אהוד בכר‬,‫צוות ביינלאומי של אסטרונומים‬
NGC!5548! ‫ גילו כי בחור השחור העל מסיבי שנמצא בלב גלקסיה‬,‫כספי מהפקולטה לפיזיקה בטכניון‬
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‫ המתרחש רק לעיתים רחוקות מאוד בלִבה של גלקסיה‬,‫שינוי מוזר ובלתי צפוי‬open
‫לאחרונה‬
‫התחולל‬
‫ שמפיץ החור‬X ‫ מקרני ה‬90% ‫ החוקרים זיהו זרם גז סמיך הנע במהירות כלפי חוץ וחוסם‬.‫פעילה‬
.‫השחור העל מסיבי שבמרכז הגלקסיה‬
La materia che precipita in un buco nero si surriscalda a tal punto da emettere raggi X e
radiazione ultravioletta. Quest’ultima può produrre getti di gas in uscita dalle zone interne del
buco nero con velocità molto alte. “Tali ‘venti’ possono essere così intensi da spazzare via
parte del gas circostante il buco nero, che altrimenti vi sarebbe precipitato” dice Cappi.
“Affinché il vento si formi, il gas che viene espulso non deve essere troppo caldo, ed è quindi
necessario che qualcosa lo protegga dai raggi X emessi dalle zone prossime al nucleo della
galassia attiva. Queste osservazioni ci permettono di capire meglio come funzionano I buchi
neri che, paradossalmente e misteriosamente, non solo attraggono la materia che li circonda,
ma ne accelerano ed espellano una parte, anche ad alte velocità”.
-
-
L’identificazione di questi venti è stata ottenuta nell’ambito di una articolata campagna
osservativa tra il 2013 e il 2014 guidata da Jelle Kaastra, dello SRON, l’Istituto olandese per le
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ricerche spaziali. I dati raccolti, come quelli dai telescopi spaziali XMM-Newton ed Hubble,
hanno messo in evidenza alcuni profondi cambiamenti nel nucleo attivo della galassia rispetto
a quelli che gli stessi telescopi avevano raccolto nel 2011. I ricercatori hanno notato infatti che
nella zona centrale della galassia sono ora presenti tracce di gas più freddo rispetto a quello
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A nice cartoon movie to (strongly) support our press releases Assassin’s Creed World Director Renaud Person pdfcrowd.com
Thank you for your anen3on