3.3. X-ray Emitting AGN in Luminous Submillimeter Galaxies
The deepest Chandra and XMM-Newton surveys have finally
provided the necessary X-ray sensitivity to complement the most
sensitive surveys at submillimeter and infrared wavelengths. One notable
instance where obtaining the highest possible X-ray sensitivity has been
essential is in studies of the AGN content of distant
submillimeter galaxies detected with the SCUBA instrument on the
James Clerk Maxwell Telescope. Most of these galaxies
are thought to contain intense starbursts with star-formation
rates of 100
M
yr-1, yet they are
not notable in optical galaxy surveys due to dust obscuration
of the corresponding starlight. The SCUBA galaxy population
is thought to be mostly at
z
1.5-3, and
such galaxies were ~ 1000 times more common at z ~ 2 than in the
local universe. The obscured starlight in submillimeter galaxies is
re-radiated in the rest-frame infrared (observed-frame submillimeter).
What fraction of submillimeter galaxies contains actively
accreting supermassive black holes? Sensitive X-ray
studies play an important role in addressing this
question, since they allow effective searching for AGN in the
majority of submillimeter galaxies that are optically faint (and
thus challenging to study in detail with optical spectroscopy).
Early comparisons between
20-150 ks
Chandra surveys and submillimeter surveys yielded little
(
10%) source
overlap. However, the latest analysis of the 2 Ms CDF-N data
reveals that seven of the 13
(
54%) bright
submillimeter
galaxies (with 850 µm flux densities of > 5 mJy)
in the CDF-N central region mapped with SCUBA have X-ray
counterparts (see Figure 8); these counterparts
have
15-200 counts in
the full Chandra bandpass.
Five of the seven X-ray detected submillimeter galaxies likely
host obscured AGN based upon their observed X-ray luminosities,
X-ray spectral shapes, and X-ray-to-submillimeter flux ratios
(see Figure 9). The remaining two have X-ray
emission properties
consistent with those expected from star formation activity,
although it is possible that they host weak AGN as well.
If the latter two sources are indeed powered mainly by star
formation, they would be the most X-ray luminous
(
4 ×
1042 erg s-1) starburst galaxies known.
![]() |
Figure 8. Map at 850 µm of the
central region of the CDF-N; the map is
|
Do the X-ray emitting AGN found in many submillimeter galaxies make
a significant contribution to these galaxies' total energy output?
Answering this question requires assessment of the amount of X-ray
absorption present since, for a given observed X-ray flux, a
Compton-thick AGN can be much more luminous than a Compton-thin AGN
(see Section 3.1). Basic X-ray spectral
fitting suggests that three of the
five submillimeter galaxies hosting AGN in the CDF-N central region
have Compton-thin absorption, while only one is likely to have
Compton-thick absorption (the final object has poor X-ray spectral
constraints). Armed with this knowledge, consideration of the
observed X-ray-to-submillimeter flux ratios (see
Figure 9) suggests
that 10% of the total
energy output from these submillimeter
galaxies is ultimately due to an AGN. Star-formation is apparently
the dominant power source for the infrared/submillimeter emission,
even when an AGN is also present.
![]() |
Figure 9. Submillimeter-to-X-ray spectral
index ( |
The results above are currently being extended, utilizing redshifts from ongoing deep optical spectroscopy. Thus far, these extended results confirm the main conclusions above.