An X-ray view of the Nature of LINERs

1. Omaira González-Martín 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

2. Omaira González-Martín Sample: • Multiwavelength catalogue of LINERs (Carrillo et al. 1999) 476 objects. • Chandraavailable data in the archive till 2007-06-30: 108 LINERs. • 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: 68 with Chandra, 54 with XMM-Newton and 40 in common. 30 May 2008

3. Omaira González-Martín Image analysis: 7 Bands AGN candidate:With a point-like source at 4.5-8.0keV SB candidate: Without point-like source at 4.5-8.0keV Chandra 43/68 (63%) Chandra 25/68 (37%) 48/82 (60%) 34/82 (40%) 0.9-1.2 1.6-2.0 4.5-8. 6.-7. Ks HST 30 May 2008 NGC4594 CGCG 162-010

4. Omaira González-Martín 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 keV13 Г=2.11±0.52 Log(NH2)= 21.93±1.36 kT=0.54±0.30 Log(NH1)= 21.32±0.71 30 May 2008

5. Omaira González-Martín 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) r=0.92 Compton-thicks Seyferts 1 30 May 2008

6. Compton-thick Bassani et al. (2000) Omaira González-Martín Compton-thickness: FeKα • 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. Seyfert 1 500 eV 200 eV 30 May 2008

7. Omaira González-Martín Accretion Rates: Black-hole masses from velocity dispersions for63/82objects. Seyfert 2 from Panessa et al. (2006) 30 May 2008

8. Omaira González-Martín Multiwavelength Information: • Stellar populations (HMXBs): 21/82 Gonzalez-Delgado 2004; Cid Fernandes 2004 • 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 30 May 2008

9. Omaira González-Martín 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 30 May 2008

10. Thanks!