1. An X-ray view of the Nature of LINERs Omaira González-Martín Instituto de Astrofísica de Andalucía Cols: J. Masegosa (IAA, SPAIN) I. Márquez (IAA, SPAIN) E. Jiménez Bailón (UNAM, MEXICO) M. Guainazzi (ESAC, SPAIN) D. Dultzin (UNAM, MEXICO) M. Guerrero (IAA, SPAIN) 30 May 2008 Omaira González-Martín

2. Sample: Multiwavelength catalogue of LINERs (Carrillo et al. 1999) 476 objects. Chandra Chandra available data in the archive till 2007-06-30: 108 LINERs. XMM-Newton XMM-Newton available data in the archive till 2007-04-30: 107 LINERs. Reidentification using optical emission lines diagnostics (Baldwin, Philips and Terlevich 1981; Veilleux et al. 1987): 83 LINERs MCG-5-23-16 was affected be pileup (>10%) 82 LINERs: 82 LINERs: 68 with Chandra, 54 with XMM-Newton and 40 in common. Omaira González-Martín 30 May 2008

3. Image analysis: 7 Bands AGN candidate: AGN candidate: With a point-like source at 4.5-8.0keV SB candidate: SB candidate: Without point-like source at 4.5-8.0keV 30 May 2008 48/82 (60%) 34/82 (40%) Chandra 43/68 (63%) Chandra 25/68 (37%) Omaira González-Martín NGC4594CGCG 162-010 0.9-1.21.6-2.04.5-8. 6.-7.KsHST

4. Spectroscopic analysis: Chandra data if available and XMM-Newton data otherwise (60/82) Models: (ME): abs[NH1](MEKAL[kT]) 6 (PL): abs[NH1](power-law[Г]) 9 (MEPL): abs[NH1](MEKAL[kT]) + abs[NH2](power-law[Г]) 24 70% (ME2PL): abs[NH1](power-law[Г]+MEKAL[kT]) + abs[NH2](power-law[Г]) 18 (2PL): abs[NH1](power-law[Г]) + abs[NH2](power-law[Г]) 3 Iron emission lines: Gaussian at 6.4 keV, 6.7 keV and 6.95 keV 13 Г=2.11±0.52 kT=0.54±0.30 Log(NH1)= 21.32±0.71 Log(NH2)=21.93±1.36 Omaira González-Martín 30 May 2008

5. Compton-thickness: Lx/[OIII] Log(Flux(Lum(2-10keV))/ Flux([OIII])) < 0.5 42/79 (53%) UGC5101, NGC3690B, NGC6240 confirmed as Compton-thick objects. No difference between AGN-like and SB-like Seyfert 2 samples: 23% (Panessa et al. 2006) Compton-thicks Seyferts 1 r=0.92 Omaira González-Martín 30 May 2008

6. Half of our sources seems to be located in the locus of Seyfert 1 objects. Compton-thick sources show lower EW. Further studies on the EW(FeKα) in Compton-thick sources need to be done. Compton-thickness: FeKα Bassani et al. (2000) Compton-thick Seyfert 1 500 eV 200 eV Omaira González-Martín 30 May 2008

7. Accretion Rates: Black-hole masses from velocity dispersions for 63/82 objects. Seyfert 2 from Panessa et al. (2006) Omaira González-Martín 30 May 2008

8. Multiwavelength Information: Stellar populations (HMXBs): 21/82 Gonzalez-Delgado 2004; Cid Fernandes 2004 NO HMXBs  Young stellar populations (<10e+9 years) only in three cases: NGC3507, NGC3998 and NGC4321. NO HMXBs HST images: 67/82 (Sharp divided method)  Compact source: 59/67 (88%).  No distinction is found between Compton-thick and Compton-thin. Inner parts? Radio data: 75/82 Nagar et al. (2005); Flohic et al. (2006)  54/75 (72%) detected.  6/54 Steep spectrum.  25/54 compatible with AGNs (8 jet structure 17 flat spectrum).  14/25 AGN candidates and 13/25 SB candidates. Broad Hα: Ho et al. 1997  15 objects.  13/15 AGN candidates (excepting NGC2639 and NGC4636) UV variability: Maoz et al. (2005)  Six objects (NGC3998, NGC4486, NGC4552, NGC4579, NGC4594 and NGC4736)  All AGN candidates and all Compton-thin All together 73/82 (89%) show evidence in favour of the AGN nature Omaira González-Martín 30 May 2008

9. Summary: X-ray Imaging: 60% nuclear compact source. 89% show indication of AGN nature, adding multiwavelength information. Compton-thickness: 53% through the F(2-10keV)/F([OIII]) ratio, higher than Seyfert 2. LINERs/Seyferts 2: Same range of properties. Eddington rates 100 time lower, expanding the same range. NH1 higher than in Seyfert 2. MEPL or ME2PL in 70%. Г ̴ 2.1, kT ̴ 0.5 keV, log(NH1) ̴ 21.3, log(NH2) ̴ 21.92, log(L(0.5-2keV)) ̴ 40.5, log(L(2-10keV)) ̴ 40.9 Omaira González-Martín 30 May 2008

10. Thanks!