Αποκαλύπτωντας τα μυστήρια των μεγαλύτερων μελανών οπών του Σύμπαντος

Ηλίας Κουλουρίδης

ΙΑΑΔΕΤ Εθνικό Αστεροσκοπείο Αθηνών

Service d' Astrophysique

Laboratoire AIM CEA Saclay, Paris

Ενεργοί Γαλαξιακοί Πυρήνες

Ενεργοί Γαλαξιακοί Πυρήνες

Παρατηρήσεις στο οπτικό

Παρατηρήσεις στο ραδιοφωνικό

Παρατηρήσεις στο υπέρυθρο

Παρατηρήσεις στις Ακτίνες-Χ

Παρατηρήσεις στις Ακτίνες-Χ

Ερωτήματα

Πώς δημιουργούνται οι Υπερ-μαζικές μαύρες τρύπες; Πότε δημιουργούνται; Πώς ενεργοποιούνται σαν Ενεργοί Γαλαξιακοι Πυρήνες;

Γιατί μας ενδιαφέρουν;

1.Ταυτόχρονη εξέλιξη με τον Γαλαξία που τους φιλοξενεί ή ακόμα και στο ευρύτερο περιβάλλον.

Γιατί μας ενδιαφέρουν;

1.Ταυτόχρονη εξέλιξη με τον Γαλαξία που τους φιλοξενεί ή ακόμα και στο ευρύτερο περιβάλλον.

AGN outflows

Γιατί μας ενδιαφέρουν;

1. Λόγω της έντονης ακτινοβολίας τους μπορούν να ανιχνευθούν σε μεγάλες αποστάσεις και να χρησιμοποιηθούν στη μελέτη της μεγάλης δομής του Σύμπαντος

Talk Outline

AGN in galaxy clusters (large scale environment)

The close environment of AGN

Unabsorbed Type 2 AGN (Exotic AGN)

Evolution of AGN

Compton thick AGN

Active Galactic Nuclei

AGN in galaxy clusters Koulouridis & Plionis (2010)

Sample of 16 Abell clusters in the SDSS area (>10Ksec).

Search for X-ray point sources within 3rc < r < 1 Mpc and Lx>10⁴²erg/s at the redshift of the cluster.

rc was calculated by adjusting a king’s profile to the diffuse emission of each cluster.

Expected number of sources was estimated using the logN-logS of Kim et al. 2007.

Koulouridis & Plionis 2010

AGN in galaxy clusters

Search in the SDSS for galaxies with mr

*-0.5<mr<mr*+0.5

Where mr* is the r-band magnitude corresponding to Mr* of the Blanton et al. (2003) luminosity function at the redshift of the cluster.

Expected number of galaxies was calculated from a 20 deg² region near the equatorial coordinate equator.

AGN in galaxy clusters

Higher optical than X-ray overdensities.

AGN phenomenon is suppressed in the dense environment of rich clusters.

Only 6 out of 88 detected X-ray sources are clearly associated with the clusters.

AGN in galaxy clusters

Higher optical than X-ray overdensities.

AGN phenomenon is suppressed in the dense environment of rich clusters.

Only 6 out of 88 detected X-ray sources are clearly associated with the clusters.

Possible reasons for the suppression of activity

Cold gas deficiency because of : Ram pressure and/or evaporation caused by the

in-fall through the hot ICM. Gas stripping by grazing encounters.

Lack of merging because of High velocity dispersions

Recent Results Confirmation of AGN suppression in rich clusters

Hwang et al. 2012 (Abell clusters,

SDSS spectroscopy): Investigating morphologies they found that AGN activity is triggered by interactions and merging when the gas supply is available.

Ehlert et al. (2013; 2014;) argue

that the X-ray AGN fraction in the central regions of 42 of the most massive clusters known to date is about three times lower than the field value.

Taylor et al. : No X-ray point source has verified redshift within the merging cluster DLSCL J0522.2-4820.

AGN in the XMM-LSS galaxy clusters Elias Koulouridis

IAASARS National Observatory of Athens

+XXL consortium

AGN in the XMM-LSS clusters

Largest contiguous X-ray survey

AGN in the XMM-LSS clusters Koulouridis et al. 2014

33 clusters 0.14<z<1.0

Temperatures, luminosities & r500 available

Available photometric redshifts of all point sources

Available LogN-logS and area curve

CFHTLS photometry for galaxies

Sample in the XMM-LSS Koulouridis et al. 2014

19 C1 clusters below z = 0.33 AGN with Lx>1042 erg/s. Poor clusters <Lx>=2.7x1043

erg/s 14 C1 high-z (0.43<z<1.05)

clusters AGN: 1.7x1042- 1.4x 1043 erg/s Moderate luminosity clusters

<Lx>=2.4x1044 erg/s

Results of the low-z sample

No suppression

X-ray overdensity “bump”

Results of the high-z sample

No suppression

X-ray overdensity “bump”

3D results

Optical follow-up WHT multi-fibre spectroscopy

William Herschell Telescope

4.2 m WHT

12 nights during 2013-2014

160 fibres

7 r=25' fields

mr=19-21

2 or 3 different configurations in each field

3-4 hours each configuration

6 more nights to come (hopefully)

Redshift confirmation of galaxy clusters

Spectroscopic confirmation of a merging super-cluster at z=0.43 (Pompei et al. submitted)

Discovery of another two super-structures at z~0.3

Spectroscopic redshift of X-ray point-like sources (mostly AGN)

observing the birth of a massive cluster Pompei et al. (submitted)

9x3 Mpc

M~1015 Mo - Mgas=~1014 Mo

AGN in XXL super-structures Koulouridis et al. (in prep)

Two of the super-structures discovered at z~0.3 by WHT observations.

Top panels: Voronoi tessellation using CFHTLS photometric redshift data (0.25<z<0.35), over-plotted with the positions of the X-ray detected clusters and the point-like sources (Fx>1x10e-14 erg/s/cm^2). In field-1 one more non-X-ray detected cluster can be seen.

Middle panels: the respective X-ray maps, red circles denote sources spectroscopically confirmed by WHT observation as super-structure members.

Bottom panels: Overdensity of optical galaxies within 5' annuli centred at the geometrical centre of the super-structures.

The environment of active galactic nuclei (AGN)

The Environment of Seyfert galaxies NOA

Elias Koulouridis, M. Plionis,I. Georgantopoulos

INAOE

V. Chamvushyan

IAUNAM

D. Dultzin, Y. Krongold

Background

Type I AGN Broad permitted lines Narrow forbidden lines

Type II AGN Narrow permitted lines Narrow forbidden lines

The Unification scheme

Evolutionary scenario

Interactions → Enhanced star formation → Obscured (type II) AGN →unobscured (type I) AGN

Evolutionary scenario

The activity of the Seyfert neighbours Koulouridis et al. 2013

Koulouridis et al. 2013 The neighbours of Sy2s are

systematically more ionized than the neighbours of Sy1s and their EW(Hα) values tend also to be higher.

Most of the non-SFN neighbours of Sy2 galaxies show a recent starburst event (<30 Myr), while the corresponding age for most of the Sy1's neighbours is >100 Myr.

The previous two results indicate differences in the star formation history of the neighbours of different types of AGN as well as in the age of the most recent interaction.

The activity of the Seyfert neighbours

Nuclear Activity in Isolated Galaxies Hernandez-Ibarra et al. 2013

513 Isolated galaxies (Karachentseva 1973; Varela et al. 2004)

70% of Isolated galaxies have AGN-->70% LINERS

3% have broad lines

No Sy1...

Secular evolution for low luminosity AGN but interactions is a necessary condition for high luminosity AGN.

Low luminosity AGN don't have BLR?

Elitzur, Ho & Tramp 2014

Ho et al. (2012) and Miniutti et al. (2013) report AGNs with very high Eddington ratios, but very low black hole masses and no broad lines.

What about the environment of hidden & non-hidden BLR Sy2s?

HBLR control non-HBLR control

Koulouridis 2014

What about hidden & non-hidden BLR Sy2s?

Non-HBLR Sy2s reside in more dense environments, have close neighbours and are merging more frequently.

Non-HBLR Sy2s are probably intrinsically different from HBLR Sy2s, which in turn are probably obscured Sy1s.

Non-detection of their BLR can be explained by the intrinsic lack of it, because of the low accretion rate of gas and dust onto the super-massive black hole, or alternatively, by heavy obscuration that can successfully cloak the BLR.

The existence of true Sy2 can be fitted nicely within an evolutionary scheme, where low accretion rate is predicted at the beginning and the end of the Seyfert's duty cycle.

Koulouridis 2014

Evolutionary scheme

Koulouridis 2014

The XMM spectral catalog of SDSS optically Seyfert 2 galaxies

Koulouridis et al. (in prep.)

Compton-thick AGN Unabsorbed Type II AGN

0.05<z<0.3

Double power law + Fe line Single power law + Fe line

Αποκαλύπτωντας τα μυστήρια των μεγαλύτερων μελανών οπών του Σύμπαντος

Ευχαριστώ!

Inverse Compton