41 research outputs found
From Merging Galaxies to Quasars: The Evolution of Nuclear Activity in Luminous and Ultraluminous Infrared Galaxies
We present the largest X-ray survey (~80 objects) of luminous and ultraluminous infrared galaxies (U/LIRGs) to date. The large infrared luminosities in these objects are thought to arise from either star formation triggered by the merging of disk galaxies or by nuclear activity. U/LIRGs have been purported to be the progenitors of some quasars. In this thesis, we utilize data from Chandra, XMM-Newton, and Suzaku X-ray observatories to quantify the contribution to the overall power of U/LIRGs by starbursts or active galactic nuclei (AGNs). A goal of this project is to statistically examine how the starburst-to-AGN ratio evolves as a function of merger stage.
We find that a majority of U/LIRGs are X-ray faint. This may be a result of high obscuration or weak nuclear activity. The dearth of detected counts makes traditional fitting difficult. As a solution, we developed a method of using hardness ratios (HR) to estimate the spectral shapes of these weak sources. Both observational evidence and simulations show that this method is effective for sources with intrinsic column densities below ~1022 cm-2 and applicable to sources with only tens of detected counts.
Applying the HR method and traditional spectral fitting to the U/LIRG data and that of 26 PG~quasars, we find a correlation of AGN dominance with dust temperature, optical spectral type, and merger stage. The probability of having a powerful AGN increases along the merger sequence. However, the AGNs can turn on at any time, as evidenced by a large number of AGNs detected in binary U/LIRGs. Starburst dominates the total power in U/LIRGs prior to the merger. Then the black hole grows rapidly during coalescence. At this time, the AGN is likely to begin driving galactic scale winds which will quench star formation, resulting in a luminous quasar. These conclusions are in general agreement with results obtained at other wavelengths and current theoretical models
A Chandra X-Ray Survey of Ultraluminous Infrared Galaxies
We present results from Chandra observations of 14 ultraluminous infrared
galaxies (ULIRGs; log(L_IR/L_Sun) >= 12) with redshifts between 0.04 and 0.16.
The goals of the observations were to investigate any correlation between
infrared color or luminosity and the properties of the X-ray emission and to
attempt to determine whether these objects are powered by starbursts or active
galactic nuclei (AGNs). The sample contains approximately the same number of
high and low luminosity objects and ``warm'' and ``cool'' ULIRGs. All 14
galaxies were detected by Chandra. Our analysis shows that the X-ray emission
of the two Seyfert 1 galaxies in our sample are dominated by AGN. The remaining
12 sources are too faint for conventional spectral fitting to be applicable.
Hardness ratios were used to estimate the spectral properties of these faint
sources. The photon indices for our sample plus the Chandra-observed sample
from Ptak et al.(2003) peak in the range of 1.0-1.5, consistent with
expectations for X-ray binaries in a starburst, an absorbed AGN, or hot
bremsstrahlung from a starburst or AGN. The values of photon index for the
objects in our sample classified as Seyferts (type 1 or 2) are larger than 2,
while those classified as HII regions or LINERs tend to be less than 2. The
hard X-ray to far-infrared ratios for the 12 weak sources are similar to those
of starbursts, but we cannot rule out the possibility of absorbed, possibly
Compton-thick, AGNs in some of these objects. Two of these faint sources were
found to have X-ray counterparts to their double optical and infrared nuclei.Comment: 40 pages, 5 tables, 14 figures, accepted by Ap
HI Absorption in Merger Remnants
It has been proposed that ultraluminous infrared galaxies (ULIRGs) pass through a luminous starburst phase, followed by a dust-enshrouded AGN phase, and finally evolve into optically bright "naked" quasars once they shed their gas/dust reservoirs through powerful wind events. We present the results of our recent 21- cm HI survey of 21 merger remnants with the Green Bank Telescope. These remnants were selected from the QUEST (Quasar/ULIRG Evolution Study) sample of ULIRGs and PG quasars; our targets are all bolometrically dominated by AGN and sample all phases of the proposed ULIRG -> IR-excess quasar -> optical quasar sequence. We explore whether there is an evolutionary connection between ULIRGs and quasars by looking for the occurrence of HI absorption tracing neutral gas outflows; our results will allow us to identify where along the sequence the majority of a merger's gas reservoir is expelled
X-QUEST: A Comprehensive X-ray Study of Local ULIRGs and QSOs
We present results from the X-ray portion of a multi-wavelength study of
local ULIRGs and QSOs called QUEST (Quasar-ULIRG Evolution STudy). The data
consist of new and archival X-ray data on 40 ULIRGs and 26 PG QSOs taken with
Chandra and XMM-Newton. A combination of traditional and hardness ratio
spectral fitting methods is used to characterize the X-ray properties of these
objects. The absorption-corrected 2-10 keV to bolometric luminosity ratios of
the ULIRGs and PG QSOs suggest that the likelihood for dominant nuclear
activity increases along the merger sequence from "cool" ULIRGs, "warm" ULIRGs,
infrared-bright QSOs, and infrared-faint QSOs. The starburst dominates the
total power in ULIRGs prior to the merger, and this is followed by rapid black
hole growth during and after coalescence. These results are in general
agreement with those obtained in the mid-infrared with Spitzer and recent
numerical simulations.Comment: 63 pages preprint style including 16 figures and 11 tables; accepted
by Ap
NuSTAR Reveals an Intrinsically X-Ray Weak Broad Absorption Line Quasar in the Ultraluminous Infrared Galaxy Markarian 231
We present high-energy (3-30 keV) NuSTAR observations of the nearest quasar, the ultraluminous infrared galaxy (ULIRG) Markarian 231 (Mrk 231), supplemented with new and simultaneous low-energy (0.5-8 keV) data from Chandra. The source was detected, though at much fainter levels than previously reported, likely due to contamination in the large apertures of previous non-focusing hard X-ray telescopes. The full band (0.5-30 keV) X-ray spectrum suggests the active galactic nucleus (AGN) in Mrk 231 is absorbed by a patchy and Compton-thin (N_H ~ 1.2^(+0.3)_(-0.3) x 10^(23) cm^(–2)) column. The intrinsic X-ray luminosity (L_(0.5 – 30 keV) ~ 1.0 × 10^(43) erg s^(–1)) is extremely weak relative to the bolometric luminosity where the 2-10 keV to bolometric luminosity ratio is ~0.03% compared to the typical values of 2%-15%. Additionally, Mrk 231 has a low X-ray-to-optical power law slope (α_(OX) ~ –1.7). It is a local example of a low-ionization broad absorption line quasar that is intrinsically X-ray weak. The weak ionizing continuum may explain the lack of mid-infrared [O IV], [Ne V], and [Ne VI] fine-structure emission lines which are present in sources with otherwise similar AGN properties. We argue that the intrinsic X-ray weakness may be a result of the super-Eddington accretion occurring in the nucleus of this ULIRG, and may also be naturally related to the powerful wind event seen in Mrk 231, a merger remnant escaping from its dusty cocoon
Suzaku Observations of Local Ultraluminous Infrared Galaxies
We report the results from our analysis of {\it Suzaku} XIS (0.5-10 keV) and
HXD/PIN (15-40 keV) observations of five well-known local ULIRGs: {\em IRAS}
F05189-2524, {\em IRAS} F08572+3915, Mrk 273, PKS 1345+12, and Arp 220. The XIS
observations of F05189-2524 and Mrk 273 reveal strong iron lines consistent
with Fe K and changes in spectral shapes with respect to previous {\it
Chandra} and {\it XMM-Newton} observations. Mrk 273 is also detected by the
HXD/PIN at 1.8-. For F05189-2524, modeling of the data from the
different epochs suggests that the change in spectral shape is likely due to
the central source switching off, leaving behind a residual reflection
spectrum, or an increase in the absorbing column. An increase in the covering
fraction of the absorber can describe the spectral variations seen in Mrk 273,
although a reduction in the intrinsic AGN luminosity cannot be formally ruled
out. The {\it Suzaku} spectra of Mrk 273 are well fit by a ~94% covering
fraction model with a column density of cm. The
absorption-corrected log[ / ] ratio is consistent
with those found in PG Quasars. The 0.5-10 keV spectrum of PKS 1345+12 and Arp
220 seem unchanged from previous observations and their hard X-ray emission is
not convincingly detected by the HXD/PIN. The large column density derived from
CO observations and the large equivalent width of an ionized Fe line in Arp 220
can be reconciled by an ionized reflection model. F08572+3915 is undetected in
both the XIS and HXD/PIN, but the analysis of unpublished {\em Chandra} data
provides a new measurement at low energies.Comment: 37 pages including 4 tables and 10 figures. Accepted for publication
in ApJ. It is tentatively scheduled to appear in the January 20, 2009 issue
of Ap
Chandra Observations of Galaxy Zoo Mergers: Frequency of Binary Active Nuclei in Massive Mergers
We present the results from a Chandra pilot study of 12 massive galaxy
mergers selected from Galaxy Zoo. The sample includes major mergers down to a
host galaxy mass of 10 that already have optical AGN
signatures in at least one of the progenitors. We find that the coincidences of
optically selected active nuclei with mildly obscured ( cm) X-ray nuclei are relatively common (8/12), but the
detections are too faint ( counts per nucleus; erg s cm) to reliably separate starburst and
nuclear activity as the origin of the X-ray emission. Only one merger is found
to have confirmed binary X-ray nuclei, though the X-ray emission from its
southern nucleus could be due solely to star formation. Thus, the occurrences
of binary AGN in these mergers are rare (0-8%), unless most merger-induced
active nuclei are very heavily obscured or Compton thick.Comment: 8 pages, including 5 figures and 1 table. Accepted by Ap
XMM-Newton Detection of a Compton-thick AGN in the 1-Jy ULIRG/LINER F04103-2838
We report on the detection of Fe Kalpha emission in F041032838, an
ultraluminous infrared galaxy (ULIRG; log[L/L] 12)
that is optically classified as a LINER. Previous {\it Chandra} observations
suggested the presence of both a starburst and an AGN in this source. A deeper
(20 ksec) {\it XMM-Newton} spectrum reveals an Fe Kalpha line at rest
frame energy 6.4 keV, consistent with cold neutral iron. The best-fit
spectral model indicates the Fe Kalpha line has an equivalent width of
1.6 keV. The hard X-ray emission is dominated by a Compton-thick AGN with
intrinsic 0.2--10 keV luminosity ergs s, while the soft
X-ray emission is from 0.1 keV gas attributed to the starburst. The X-ray
spectrum of this source bears a striking resemblance to that of the archetypal
luminous infrared galaxy NGC 6240 despite differences in merger state and
infrared properties.Comment: 23 pre-print pages including 5 figures and 1 table. Accepted by Ap
Wide-field Imaging Interferometry Testbed II: Implementation, Performance, and Plans
The Wide-Field Imaging Interferometry Testbed (WIIT) will provide valuable
information for the development of space-based interferometers. This laboratory
instrument operates at optical wavelengths and provides the ability to test
operational algorithms and techniques for data reduction of interferometric
data. Here we present some details of the system design and implementation,
discuss the overall performance of the system to date, and present our plans
for future development of WIIT. In order to make best use of the
interferometric data obtained with this system, it is critical to limit
uncertainties within the system and to accurately understand possible sources
of error. The WIIT design addresses these criteria through a number of
ancillary systems. The use of redundant metrology systems is one of the most
important features of WIIT, and provides knowledge of the delay line position
to better than 10 nm. A light power detector is used to monitor the brightness
of our light sources to ensure that small fluctuations in brightness do not
affect overall performance. We have placed temperature sensors on critical
components of the instrument, and on the optical table, in order to assess
environmental effects on the system. The use of these systems provides us with
estimates of the overall system uncertainty, and allows an overall
characterization of the results to date. These estimates allow us to proceed
forward with WIIT, adding rotation stages for 2-D interferometry. In addition,
they suggest possible avenues for system improvement. Funding for WIIT is
provided by NASA Headquarters through the ROSS/SARA Program and by the Goddard
Space Flight Center through the IR&D Program.Comment: 11 pages, 9 figure