Reverberation Mapping Extending the Luminosity Range

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Reverberation Mapping -Extending the Luminosity
Range

• Shai Kaspi
• Tel-Aviv University Technion Haifa
• Israel

A black hole obsessed/addict
its Hagais fault.
AGNs From Atoms to Black Holes Tel-Aviv
University, 22 February 2006
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Outline

• Introduction to reverberation mapping by B.
  Peterson- Current BLR Size Luminosity
  Relation- Broadening the luminosity range-
  Mapping low luminosity AGNs- Mapping of
  high-luminosity quasars preliminary results

Maoz D., Netzer H., Peterson B.M., Vestergaard
M., Jannuzi B. (Kaspi et al. 2005, ApJ, 629, 61)
Laor A., Maoz, D., Peterson B., Filippenko A.
Maoz D., Netzer H., Brandt W.N., Schneider D.P.,
Shemmer O. (Kaspi et al. in preparation)
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Reverberation Mapping

• Peterson et al. (2004) compiled all studies to
  date.
• 35 objects with Balmer (mainly Hb) lines time
  lag.
• Characteristic BLR size Time Lag speed of
  light.
• The BLR size luminosity relation
• Both are measured quantities.
• Luminosities in the Optical, UV, and X-rays.
• BLR size from averaging all Balmer lines time lag.

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Linear Regression
Uncertainties in both quantities And Intrinsic
scatter in the relation Two regression methods
1. FITEXY from Press et al. (1992) implemented by
Tremaine et al. (2002).
2. BCES (Bivariate Correlated Errors and
intrinsic Scatter) by Akritas Bershady (1996).
and also outlier points
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Hb RBLR Optical luminosity (5100 A)
RBLR ? lLl(5100 Å) (0.690.05)
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Hb RBLR Optical luminosity (5100 A)
RBLR ? lLl(5100 Å) (0.5180.039) (Bentz et
al. Aph/0602412)
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Hb RBLR UV luminosity (1450 A)
58 points
32 points
RBLR ? lLl(1450 Å) (0.560.05)
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RBLR X-ray luminosity (2-10 keV)
54 points
30 points
RBLR ? lLl(2-10 keV) (0.700.14)
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RBLR luminosity Relation, conclusions

• Though small differences exist between the
  different regression methods the results are
  generally consistent.
• Average slope is 0.670.05 for the optical
  continuum and broad Hß luminosity, about
  0.560.05 for the UV luminosity, and about
  0.700.14 for the X-ray luminosity.
• We find in these relations an intrinsic scatter
  of about 40 .
• In most energy bands the slope is roughly like
  the naive theoretical prediction of 0.5. This
  prediction is naively based on the assumption
  that all AGNs have the same ionization parameter,
  BLR density, column density, and ionizing SED.

0.520.04
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Broadening the Luminosity range - Hb
Current studies span 4 orders of magnitude.
There are 4 more orders of magnitude to be
explored. Extrapolation does not necessarily
give the real situation.
We need to expand the luminosity range with
reverberation mapping studies.
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Broadening the Luminosity range C IV
Up to 2004 only four AGNs with C IV BLR size
measurements
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Broadening the Luminosity range C IV
Peterson et al. (2005) added NGC4395 four
orders of magnitude in luminosity lower
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Broadening the Luminosity range C IV
Still there are the high luminosity quasars at
three orders of magnitude higher
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Higher luminosities monitoring
Photometrically monitoring 11 quasars for the
past decade. 7 of which are spectroscopically
monitored for the past 5 years. 2.1 lt z lt
3.2 1045.6 lt ?L?(5100 Å) lt 1047
erg/s Photometric observation at the 1m Wise
Observatory. Spectroscopic observation at 9m
Hobby-Eberly Telescope (HET) and at the Wise
Observatory. Lines monitored are C IV and Ly?
using the method of a comparison star
simultaneously with the quasar in the slit.
Some preliminary results (Kaspi et al. in
preparation)
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Continuum light curves
Z log L ?R ?B 2.628 46.14
0.34 0.44 3.177 46.88 0.16
0.22 2.172 46.05 0.34 0.44 2.824
46.62 0.25 0.27 3.200 46.96 0.14
0.19 2.722 47.04 0.16 0.20
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SBS 1116603
?L?(5100 Å) 1.41046 erg/s z 2.628
?R0.34 ?B0.44
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SBS 1116603 C IV Continuum CCF
No measurable time lag is found
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S4 063668
?L?(5100 Å) 7.61046 erg/s z 3.117
?R0.16 ?B0.22
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HS 17006416
?L?(5100 Å) 1047 erg/s z 2.722
?R0.16 ?B0.20
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S5 083671
?L?(5100 Å) 1.11046 erg/s z 2.172
?R0.34 ?B0.44
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S5 083671 C IV Continuum CCF
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Broadening the Luminosity range C IV
A preliminary result suggest a correlation
between the C IV size and the luminosity
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Mass Luminosity Relation
.
Peterson et al. (2005)
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Scaling C IV size to Hb size
S5 083671 CIV lag days
NGC4395 CIV lag min
? Hb lag about min
In two weeks, optical monitoring of NGC4395
spectroscopically from KPNO and photometrically
from four observatories around the world cover 22
hours a day for four days.
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Summary

• In the 1042 to 1046 erg/s luminosity range a
  firm relation exist between the BLR size and
  luminosity. Slope ranging from 0.5 to 0.7.
• Expanding the luminosity range is important and
  first steps are being taken
• Low luminosity Seyferts and LINERS to cover the
  luminosity range of 1040 to 1042 erg/sec.
• High luminosity quasars preliminary results
  are encouraging. When this long term project is
  concluded reverberation mapping studies will
  cover the luminosity range up to 1047 ergs/s, an
  additional one order of magnitude to the current
  luminosity range and 7 orders of magnitude in
  total.
• Dust Reverberation mapping (torus size?)