444 research outputs found
CIV emission-line properties and systematic trends in quasar black hole mass estimates
Black-hole masses are crucial to understanding the physics of the connection
between quasars and their host galaxies and measuring cosmic black hole-growth.
At high redshift, z > 2.1, black hole masses are normally derived using the
velocity-width of the CIV broad emission line, based on the assumption that the
observed velocity-widths arise from virial-induced motions. In many quasars,
the CIV-emission line exhibits significant blue asymmetries (`blueshifts') with
the line centroid displaced by up to thousands of km/s to the blue. These
blueshifts almost certainly signal the presence of strong outflows, most likely
originating in a disc wind. We have obtained near-infrared spectra, including
the H emission line, for 19 luminous ( = 46.5-47.5 erg/s)
Sloan Digital Sky Survey quasars, at redshifts 2 < z < 2.7, with CIV emission
lines spanning the full-range of blueshifts present in the population. A strong
correlation between CIV-velocity width and blueshift is found and, at large
blueshifts, > 2000 km/s, the velocity-widths appear to be dominated by
non-virial motions. Black-hole masses, based on the full width at half maximum
of the CIV-emission line, can be overestimated by a factor of five at large
blueshifts. A larger sample of quasar spectra with both CIV and H, or
H, emission lines will allow quantitative corrections to CIV-based
black-hole masses as a function of blueshift to be derived. We find that
quasars with large CIV blueshifts possess high Eddington luminosity ratios and
that the fraction of high-blueshift quasars in a flux-limited sample is
enhanced by a factor of approximately four relative to a sample limited by
black hole mass.Science and Technology Facilities CouncilThis is the final version of the article. It first appeared from Oxford University Press via http://dx.doi.org/10.1093/mnras/stw136
BAL and non-BAL quasars: Continuum, emission, and absorption properties establish a common parent sample
Using a sample of 144,000 quasars from the Sloan Digital Sky Survey
data release 14 we investigate the outflow properties, evident both in
absorption and emission, of high-ionization Broad Absorption Line (BAL) and
non-BAL quasars with redshifts 1.6 3.5 and luminosities 45.3
48.2 erg s. Key to the investigation is a
continuum and emission-line reconstruction scheme, based on mean-field
independent component analysis, that allows the kinematic properties of the
CIV1550 emission line to be compared directly for both non-BAL and BAL
quasars. CIV-emission blueshift and equivalent-width (EW) measurements are thus
available for both populations. Comparisons of the emission-line and BAL-trough
properties reveal strong systematic correlations between the emission and
absorption properties. The dependence of quantitative outflow indicators on
physical properties such as quasar luminosity and luminosity relative to
Eddington-luminosity are also shown to be essentially identical for the BAL and
non-BAL populations. There is an absence of BALs in quasars with the hardest
spectral energy distributions (SEDs), revealed by the presence of strong
HeII1640 emission, large CIV1550-emission EW and no
measurable blueshift. In the remainder of the CIV-emission blueshift versus EW
space, BAL and non-BAL quasars are present at all locations; for every
BAL-quasar it is possible to identify non-BAL quasars with the same
emission-line outflow properties and SED-hardness. The co-location of BAL and
non-BAL quasars as a function of emission-line outflow and physical properties
is the key result of our investigation, demonstrating that (high-ionization)
BALs and non-BALs represent different views of the same underlying quasar
population
Characterizing Quasar C iv Emission-line Measurements from Time-resolved Spectroscopy
We use multi-epoch quasar spectroscopy to determine how accurately
single-epoch spectroscopy can locate quasars in emission-line parameter space
in order to inform investigations where time-resolved spectroscopy is not
available. We explore the improvements in emission-line characterization that
result from using non-parametric information from many lines as opposed to a
small number of parameters for a single line, utilizing reconstructions based
on an independent component analysis applied to the data from the Sloan Digital
Sky Survey Reverberation Mapping project. We find that most of the quasars are
well described by just two components, while more components signal a quasar
likely to yield a successful reverberation mapping analysis. In single-epoch
spectroscopy the apparent variability of equivalent width is exaggerated
because it is dependent on the continuum. Multi-epoch spectroscopy reveals that
single-epoch results do not significantly change where quasars are located in
CIV parameter space and do not have a significant impact on investigations of
the global Baldwin Effect. Quasars with emission line properties indicative of
higher are less variable, consistent with models with enhanced
accretion disk density. Narrow absorption features at the systemic redshift may
be indicative of orientation (including radio-quiet quasars) and may appear in
as much as 20% of the quasar sample. Future work applying these techniques to
lower luminosity quasars will be important for understanding the nature of
accretion disk winds
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Correcting C -Based Virial Black Hole Masses
The C λλ1498,1501 broad emission line is visible in optical spectra to redshifts exceeding ∼ 5. C has long been known to exhibit significant displacements to the blue and these ‘blueshifts’ almost certainly signal the presence of strong outflows. As a consequence, single-epoch virial black hole (BH) mass estimates derived from C velocity widths are known to be systematically biased compared to masses from the hydrogen Balmer lines. Using a large sample of 230 high-luminosity ( = 10–10 erg s), redshift 1.5 < < 4.0 quasars with both C and Balmer line spectra, we have quantified the bias in C BH masses as a function of the C blueshift. C BH masses are shown to be a factor of 5 larger than the corresponding Balmer-line masses at C blueshifts of 3000 km s and are overestimated by almost an order of magnitude at the most extreme blueshifts, ≳5000 km s. Using the monotonically increasing relationship between the C blueshift and the mass ratio BH(C )/BH(H), we derive an empirical correction to all C BH masses. The scatter between the corrected C masses and the Balmer masses is 0.24 dex at low C blueshifts (∼0 km s) and just 0.10 dex at high blueshifts (∼3000 km s), compared to 0.40 dex before the correction. The correction depends only on the C line properties – i.e. full width at half-maximum and blueshift – and can therefore be applied to all quasars where C emission line properties have been measured, enabling the derivation of unbiased virial BH-mass estimates for the majority of high-luminosity, high-redshift, spectroscopically confirmed quasars in the literature.LC thanks the Science and Technology Facilities Council (STFC) for the award of a studentship. PCH acknowledges support from the STFC via a Consolidated Grant to the Institute of Astronomy, Cambridge. MB acknowledges support from STFC via an Ernest Rutherford Fellowship.
Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/.
The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory and the University of Washington.
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A Candidate Sub-Parsec Supermassive Binary Black Hole System
We identify SDSS J153636.22+044127.0, a QSO discovered in the Sloan Digital
Sky Survey, as a promising candidate for a binary black hole system. This QSO
has two broad-line emission systems separated by 3500 km/sec. The redder system
at z=0.3889 also has a typical set of narrow forbidden lines. The bluer system
(z=0.3727) shows only broad Balmer lines and UV Fe II emission, making it
highly unusual in its lack of narrow lines. A third system, which includes only
unresolved absorption lines, is seen at a redshift, z=0.3878, intermediate
between the two emission-line systems. While the observational signatures of
binary nuclear black holes remain unclear, J1536+0441 is unique among all QSOs
known in having two broad-line regions, indicative of two separate black holes
presently accreting gas. The interpretation of this as a bound binary system of
two black holes having masses of 10^8.9 and 10^7.3 solar masses, yields a
separation of ~ 0.1 parsec and an orbital period of ~100 years. The separation
implies that the two black holes are orbiting within a single narrow-line
region, consistent with the characteristics of the spectrum. This object was
identified as an extreme outlier of a Karhunen-Loeve Transform of 17,500 z <
0.7 QSO spectra from the SDSS. The probability of the spectrum resulting from a
chance superposition of two QSOs with similar redshifts is estimated at
2X10^-7, leading to the expectation of 0.003 such objects in the sample
studied; however, even in this case, the spectrum of the lower redshift QSO
remains highly unusual.Comment: 8 pages, 2 figures, Nature in pres
Cosmic Hydrogen Was Significantly Neutral a Billion Years After the Big Bang
The ionization fraction of cosmic hydrogen, left over from the big bang,
provides crucial fossil evidence for when the first stars and quasar black
holes formed in the infant universe. Spectra of the two most distant quasars
known show nearly complete absorption of photons with wavelengths shorter than
the Ly-alpha transition of neutral hydrogen, indicating that hydrogen in the
intergalactic medium (IGM) had not been completely ionized at a redshift z~6.3,
about a billion years after the big bang. Here we show that the radii of
influence of ionizing radiation from these quasars imply that the surrounding
IGM had a neutral hydrogen fraction of tens of percent prior to the quasar
activity, much higher than previous lower limits of ~0.1%. When combined with
the recent inference of a large cumulative optical depth to electron scattering
after cosmological recombination from the WMAP data, our result suggests the
existence of a second peak in the mean ionization history, potentially due to
an early formation episode of the first stars.Comment: 14 Pages, 2 Figures. Accepted for publication in Nature. Press
embargo until publishe
Dust-free quasars in the early Universe
The most distant quasars known, at redshifts z=6, generally have properties
indistinguishable from those of lower-redshift quasars in the rest-frame
ultraviolet/optical and X-ray bands. This puzzling result suggests that these
distant quasars are evolved objects even though the Universe was only seven per
cent of its current age at these redshifts. Recently one z=6 quasar was shown
not to have any detectable emission from hot dust, but it was unclear whether
that indicated different hot-dust properties at high redshift or if it is
simply an outlier. Here we report the discovery of a second quasar without
hot-dust emission in a sample of 21 z=6 quasars. Such apparently hot-dust-free
quasars have no counterparts at low redshift. Moreover, we demonstrate that the
hot-dust abundance in the 21 quasars builds up in tandem with the growth of the
central black hole, whereas at low redshift it is almost independent of the
black hole mass. Thus z=6 quasars are indeed at an early evolutionary stage,
with rapid mass accretion and dust formation. The two hot-dust-free quasars are
likely to be first-generation quasars born in dust-free environments and are
too young to have formed a detectable amount of hot dust around them.Comment: To be published in Nature on the 18 March 2010
Molecular Gas in the Host Galaxy of a Quasar at Redshift z=6.42
Observations of the molecular gas phase in quasar host galaxies provide
fundamental constraints on galaxy evolution at the highest redshifts. Molecular
gas is the material out of which stars form; it can be traced by spectral line
emission of carbon--monoxide (CO). To date, CO emission has been detected in
more than a dozen quasar host galaxies with redshifts (z) larger 2, the record
holder being at z=4.69. At these distances the CO lines are shifted to longer
wavelengths, enabling their observation with sensitive radio and millimetre
interferometers. Here we present the discovery of CO emission toward the quasar
SDSS J114816.64+525150.3 (hereafter J1148+5251) at a redshift of z=6.42, when
the universe was only 1/16 of its present age. This is the first detection of
molecular gas at the end of cosmic reionization. The presence of large amounts
of molecular gas (M(H_2)=2.2e10 M_sun) in an object at this time demonstrates
that heavy element enriched molecular gas can be generated rapidly in the
earliest galaxies.Comment: 12 pages, 2 figures. To appear in Nature, July, 200
Getting into hot water:sick guppies frequent warmer thermal conditions
Ectotherms depend on the environmental temperature for thermoregulation and exploit thermal regimes that optimise physiological functioning. They may also frequent warmer conditions to up-regulate their immune response against parasite infection and/or impede parasite development. This adaptive response, known as ‘behavioural fever’, has been documented in various taxa including insects, reptiles and fish, but only in response to endoparasite infections. Here, a choice chamber experiment was used to investigate the thermal preferences of a tropical freshwater fish, the Trinidadian guppy (Poecilia reticulata), when infected with a common helminth ectoparasite Gyrodactylus turnbulli, in female-only and mixed-sex shoals. The temperature tolerance of G. turnbulli was also investigated by monitoring parasite population trajectories on guppies maintained at a continuous 18, 24 or 32 °C. Regardless of shoal composition, infected fish frequented the 32 °C choice chamber more often than when uninfected, significantly increasing their mean temperature preference. Parasites maintained continuously at 32 °C decreased to extinction within 3 days, whereas mean parasite abundance increased on hosts incubated at 18 and 24 °C. We show for the first time that gyrodactylid-infected fish have a preference for warmer waters and speculate that sick fish exploit the upper thermal tolerances of their parasites to self medicate
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