An X-ray view of the Nature of LINERs

Omaira González-MartínOmaira González-MartínInstituto 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)

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Sample:

Multiwavelength catalogue of LINERs (Carrillo et al. 1999) 476 objects.

ChandraChandra available data in the archive till 2007-06-30: 108 LINERs.

XMM-NewtonXMM-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 LINERs82 LINERs:: 68 with Chandra, 54 with XMM-Newton and 40 in common.

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Image analysis:7 Bands

AGN candidate:AGN candidate: With a point-like source at 4.5-8.0keVSB candidate: SB candidate: Without point-like source at 4.5-8.0keV

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48/82 (60%)

34/82(40%)

Chandra43/68 (63%)

Chandra25/68(37%)

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NGC4594 CGCG 162-010

0.9-1.2 1.6-2.0 4.5-8.

6.-7. Ks HST

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±0.52kT=0.54±0.30kT=0.54±0.30 Log(NH1)=

21.32±0.71Log(NH2)=Log(NH2)=21.93±1.3621.93±1.36

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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-thicksSeyferts 1

r=0.92

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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-thickCompton-thickSeyfert 1

500 eV500 eV200 eV200 eV

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Accretion Rates:Black-hole masses from velocity dispersions for 63/82 objects. Seyfert 2 from Panessa et al. (2006)

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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 HMXBsNO 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

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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 K 2.1, kT K 0.5 keV, log(NH1) K 21.3, log(NH2) K 21.92, log(L(0.5-2keV)) K 40.5, log(L(2-10keV)) K 40.9

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Thanks!