XMM-Newton Observations
of the FR II Radio-Loud BAL
Quasar FIRST J1016+5209
Justin J. Schaefer, M. S. Brotherton
(University of Wyoming), M. D. Gregg, R.
H. Becker (UC Davis/LLNL), S. A. Laurent-
Muehleisen (UC Davis), M. Lacy (Caltech),
R. L. White (STSCI)
Abstract
We have detected FIRST J101614.3+520916 with the
XMM-Newton X-ray Observatory. FIRST J1016+5209,
one of the most extreme radio-loud broad absorption line
(BAL) quasars so far discovered, is a Fanaroff-Riley type
II (FR II) radio source. We find the X-ray flux is low in
comparison to the radio flux indicating X-ray absorption.
We have measured optical-X-ray spectral indices and X-
ray hardness ratios. FIRST J1016+5209 is relatively X-
ray bright compared to radio-quiet BAL quasars. Despite
the low counts, we have determined that a simple high-
column-density absorber does not match the soft optical-
X-ray spectral index and the HR simultaneously,
requiring a more complex model that includes a partial
covering X-ray absorber.
Introduction
The quasar FIRST J1016+5209 has an optical
spectrum that shows broad absorption features
(Figure 1), and the double-lobed radio
morphology and luminosity characteristic of a
classic FR II radio source (Figure 2). The radio
luminosity places it among the extreme end of
radio-loud quasars (Table 1). Such radio-loud
quasars normally have intrinsically more
luminous X-ray emission compared to radio-
quiet quasars, although BAL quasars in general
are typically very x-ray faint due to absorption
along the line of sight.
X-Ray Observations
• We observed FIRST J1016+5209 with XMM-Newton on
2001 November 3 with a duration of ~10 ks. Due to high
X-ray background flares only 6.1 ks of data from the
EPIC MOS 1 detector and 5.8 ks of data from the EPIC
MOS 2 detector (Figure 3), were usable.
• The x-ray flares overwhelmed the x-ray sensitive EPIC-
pn detector, and no data remained usable.
• This was the first X-ray observation of a FR II BAL
quasar.
• The time-averaged, 0.2-8 keV flux of J1016+5209 is
6.5X10-14 ergs/cm2/s. (Table 2)
• There were too few counts (46) for a detailed spectral
analysis, but the hardness ratio HR (-0.5) indicates an
excess of soft photons. (Table 2)
Conclusion
• Based on the radio-X-ray correlation (Brinkman et al. 2000) we estimate
that the intrinsic X-ray flux is ~17 times larger than observed.
• Assuming the estimated X-ray flux we calculate an intrinsic αox = -1.05 for
this object versus the observed αox = -1.51.
• First J1016+5209 is much fainter optically, but as bright in the X-rays as the
Radio-Quiet BAL Quasars of Green et al. (2001) (all αox < -1.5).
• At 2 keV and Z = 2.454 a NH = 8x1023 cm-2 would be required to account for
the faintness of the X-ray flux. The HR however is consistent only for NH ≤
1x1021.5 cm-2. This implies a more complex situation.
• A longer exposure of J1016+5209 is needed to understand the nature of the
absorber.
• CHANDRA and XMM-Newton observations of the second FR II BAL Quasar
LBQS 1138-0126 (Brotherton et al. 2002) have been taken, and analysis of
the data has begun.
• We estimate for a combined SDSS and FIRST survey search, we will
discover 100-200 FR II BAL Quasars (Brotherton et al. 2002).
References
• Brinkman et al. 2000, A&A, 356, 445-462
• Brinkman et al. 2002, A&A, 385, L31-L35
• Brotherton et al. 2002, AJ, 124, 2575-2580
• Dickey and Lockman, 1990, ARAA, 28, 215
• Gehrels 1986, ApJ, 303, 336
• Green, et al. 2000, ApJ, 558, 109-118
• Gregg, et al. 2000, ApJ, 544, 142-149
Acknowledgements
This work is funded by Wyoming NASA Space Grant Consortium, NASA Grant
#NGT-40102 and by Wyoming NASA EPSCoR NASA Grant #NCC5-578.
This work is also funded in part by NASA through the US XMM-Newton
Program with data provided by ESA.
Table 2: X-ray Properties and
Comparisons
BALQSO NH counts Soft Hard S+H HR FX αOX
cm-2 s-1 total ergs s-1cm-2
J1016+5209 7.64e+19 0.0077 36 10 46 -0.5±.08 6.5e-14 -1.51
Notes: All counts/fluxes have been background subtracted. NH is the Galactic
column density calculated using nH (Dickey and Lockman 1990). Counts are the
total counts from the 0.2-8 keV flux received by the two EPIC MOS detectors. Soft
band is 0.2-2 keV, hard band is 2-8 keV. HR= (H-S)/(H+S), with errors following
Gehrels (1986). FX is 0.2-8 keV flux, assuming a photon index = 1.7 and the
Galactic column. The optical-X-ray spectral index (αOX) is calculated using a
dereddened optical flux at 3000 Å, and a PIMMS conversion of the XMM-Newton
flux to a ROSAT bandpass (0.1-2.4 keV) for the 2 keV flux. Sν α ναox
Figure 3: MOS 2 Image
Figure 3: MOS 2 Image
Figure 1: Optical Spectrum
Low-resolution spectrum of J101614.3+520916 obtained at the Keck Observatory using LRIS. Prominent features are
labeled. There is a relatively strong intervening Mg II 2800 absorption system at an observed wavelength of 6110 Å (z =
1.182). (This caption and plot taken from Gregg et al. 2000.)
Figure 2: Radio Map
Left. FIRST Survey 20 cm image of J101614.3+520916; contour levels are -0.5, 0.5, 1.0, 5, 10.0, 20.0, 50.0, and 100.0
mJy. Right: A-array 3.6 cm image of the northwest lobe showing linear structure pointing directly back to the radio core,
evidence that the two are physically associated and not a chance arrangement of radio sources. Contour levels are
0.24, 0.5, 1.0, 1.5, 2.0, 2.5, 3.0, 3.35, 3.75, and 4.0 mJy; the map has an rms of 0.078 mJy. (The radio maps and text
for Figure 1 and Table 1 are from Gregg et al. 2000.)
Table 1: Quasar Properties
BALQSO Z E~R S20 cm Av MB log LR 5 Ghz
Log R*
Mag mJy mag mag ergs/cm2/s/Hz
J1016+5209 2.454 18.6 177 0.75 -26.2(-27.3) 34.3 3.4(2.7)
Note: “( )” indicates dereddened values.