An Xray view of the Nature of LINERs

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An X-ray view of the Nature of LINERs
Omaira González-Martín

• 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
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Sample
Omaira González-Martín

• Multiwavelength catalogue of LINERs (Carrillo et
  al. 1999) 476 objects.
• Chandra available 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 (gt10)
• 82 LINERs 68 with Chandra, 54 with XMM-Newton
  and 40 in common.

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Image analysis
Omaira González-Martín

• 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
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NGC4594
CGCG 162-010
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Spectroscopic analysis
Omaira González-Martín

• Chandra data if available and XMM-Newton data
  otherwise (60/82)
• Models
• (ME) absNH1(MEKALkT) 6
• (PL) absNH1(power-law?) 9
• (MEPL) absNH1(MEKALkT)
  absNH2(power-law?) 24 70
• (ME2PL) absNH1(power-law?MEKALkT)
  absNH2(power-law?) 18
• (2PL) absNH1(power-law?)
  absNH2(power-law?) 3
• Iron emission lines Gaussian at 6.4 keV, 6.7 keV
  and 6.95 keV 13

?2.110.52
Log(NH2) 21.931.36
kT0.540.30
Log(NH1) 21.320.71
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Compton-thickness Lx/OIII
Omaira González-Martín

• Log(Flux(Lum(2-10keV))/ Flux(OIII)) lt 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)

r0.92
Compton-thicks
Seyferts 1
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Compton-thickness FeKa
Omaira González-Martín

• 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(FeKa) in
  Compton-thick sources need to be done.

Seyfert 1
500 eV
200 eV
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Accretion Rates
Omaira González-Martín

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

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Multiwavelength Information
Omaira González-Martín

• Stellar populations (HMXBs) 21/82
  Gonzalez-Delgado 2004 Cid Fernandes 2004
• Young stellar populations (lt10e9 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 Ha 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
Omaira González-Martín

• 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. ? ? 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

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Thanks!