Ηλίας Κουλουρίδης. ΙΑΑΔΕΤ Εθνικό Αστεροσκοπείο Αθηνών. Service d' Astrophysique Laboratoire AIM CEA Saclay, Paris

Μέγεθος: px

Εμφάνιση ξεκινά από τη σελίδα:

Download "Ηλίας Κουλουρίδης. ΙΑΑΔΕΤ Εθνικό Αστεροσκοπείο Αθηνών. Service d' Astrophysique Laboratoire AIM CEA Saclay, Paris"

Ἀλεξανδρεύς Βασιλόπουλος
7 χρόνια πριν
Προβολές:

1 Αποκαλύπτωντας τα μυστήρια των μεγαλύτερων μελανών οπών του Σύμπαντος Ηλίας Κουλουρίδης ΙΑΑΔΕΤ Εθνικό Αστεροσκοπείο Αθηνών Service d' Astrophysique Laboratoire AIM CEA Saclay, Paris

2 Ενεργοί Γαλαξιακοί Πυρήνες

3 Ενεργοί Γαλαξιακοί Πυρήνες

4 Παρατηρήσεις στο οπτικό

5 Παρατηρήσεις στο ραδιοφωνικό

6 Παρατηρήσεις στο υπέρυθρο

7 Παρατηρήσεις στις Ακτίνες-Χ

8 Παρατηρήσεις στις Ακτίνες-Χ

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

10 Γιατί μας ενδιαφέρουν; 1.Ταυτόχρονη εξέλιξη με τον Γαλαξία που τους φιλοξενεί ή ακόμα και στο ευρύτερο περιβάλλον.

11 Γιατί μας ενδιαφέρουν; 1.Ταυτόχρονη εξέλιξη με τον Γαλαξία που τους φιλοξενεί ή ακόμα και στο ευρύτερο περιβάλλον.

12 AGN outflows

13 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

14 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

15 Active Galactic Nuclei

16 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 Koulouridis & Plionis 2010

17 AGN in galaxy clusters Search in the SDSS for galaxies with m r* -0.5<m r <m r* +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.

18 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.

19 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.

20 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

21 Recent Results Confirmation of AGN suppression in rich clusters Hwang et al (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 J

22 AGN in the XMM-LSS galaxy clusters Elias Koulouridis IAASARS National Observatory of Athens +XXL consortium

24 AGN in the XMM-LSS clusters Largest contiguous X-ray survey

25 AGN in the XMM-LSS clusters Koulouridis et al clusters 0.14<z<1.0 Temperatures, luminosities & r 500 available Available photometric redshifts of all point sources Available LogN-logS and area curve CFHTLS photometry for galaxies

26 Sample in the XMM-LSS Koulouridis et al C1 clusters below z = 0.33 AGN with Lx>10 42 erg/s. Poor clusters <Lx>=2.7x10 43 erg/s 14 C1 high-z (0.43<z<1.05) clusters AGN: 1.7x x erg/s Moderate luminosity clusters <Lx>=2.4x10 44 erg/s

27 Results of the low-z sample No suppression X-ray overdensity bump

28 Results of the high-z sample No suppression X-ray overdensity bump

29 3D results

30 Optical follow-up WHT multi-fibre spectroscopy William Herschell Telescope 12 Redshift nights confirmation during of galaxy clusters 160 fibres Spectroscopic confirmation 7 of r=25' a merging fields super-cluster at mz=0.43 r =19-21 (Pompei et al. submitted) 2 or 3 different configurations Discovery of another in each two field super-structures at z~ hours each configuration Spectroscopic redshift of X- 6 ray more point-like nights sources to come (hopefully) (mostly AGN) 4.2 m WHT

31 observing the birth of a massive cluster Pompei et al. (submitted) 9x3 Mpc M~10 15 M o - Mgas=~10 14 M o

32 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 superstructures.

33 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

34 Background Type II AGN Narrow permitted lines Narrow forbidden lines Type I AGN Broad permitted lines Narrow forbidden lines

35 The Unification scheme

36 Evolutionary scenario Interactions Enhanced star formation Obscured (type II) AGN unobscured (type I) AGN

37 Evolutionary scenario

38 The activity of the Seyfert neighbours Koulouridis et al Koulouridis et al 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.

39 The activity of the Seyfert neighbours

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

41 Low luminosity AGN don't have BLR? 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. Elitzur, Ho & Tramp 2014

42 Koulouridis 2014 What about the environment of hidden & non-hidden BLR Sy2s? HBLR control non-hblr control

43 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

44 Evolutionary scheme Koulouridis 2014

45 The XMM spectral catalog of SDSS optically Seyfert 2 galaxies Koulouridis et al. (in prep.) 0.05<z<0.3 Compton-thick AGN Unabsorbed Type II AGN Double power law + Fe line Single power law + Fe line

46 Αποκαλύπτωντας τα μυστήρια των μεγαλύτερων μελανών οπών του Σύμπαντος Ευχαριστώ!

47 Inverse Compton

Σχετικά έγγραφα

[1] P Q. Fig. 3.1

[1] P Q. Fig. 3.1 1 (a) Define resistance....... [1] (b) The smallest conductor within a computer processing chip can be represented as a rectangular block that is one atom high, four atoms wide and twenty atoms long. One