1,869 research outputs found
Massive black hole binaries: dynamical evolution and observational signatures
The study of the dynamical evolution of massive black hole pairs in mergers
is crucial in the context of a hierarchical galaxy formation scenario. The
timescales for the formation and the coalescence of black hole binaries are
still poorly constrained, resulting in large uncertainties in the expected rate
of massive black hole binaries detectable in the electromagnetic and
gravitational wave spectra. Here we review the current theoretical
understanding of the black hole pairing in galaxy mergers, with a particular
attention to recent developments and open issues. We conclude with a review of
the expected observational signatures of massive binaries, and of the
candidates discussed in literature to date.Comment: 4 Figures. Accepted for publication in Advances in Astronom
Recommended from our members
Modal strain-based post-earthquake damage characterization of r/c frame buildings
This paper contributes a novel numerical study to assess the potential of the two most widely used modalstrain based damage indices for damage detection in structural components under flexure for post-earthquake damage characterization of reinforced concrete multi-storey planar frame buildings. To this aim, buildings are treated as transversely vibrating beam-like structures and modal strains (i.e., second derivatives of mode shapes) are computed from lateral translational mode shape ordinates known at each floor/slab level along the height of buildings before (healthy state) and after (damaged state) a damaging seismic event. In this setting, the change of modal curvature (MC) along the height of the building as well as the change of modal strain energy (MSE) are adopted as damage sensitive indices and their effectiveness to localize damage to column or to beam elements at different floors and to characterize damage severity is gauged vis-Ã -vis. This is accomplished by considering computer-generated mode shape data obtained from linear modal analyses applied to finite element models of two different 10-storey r/c planar frames, a single-bay one and a two-bay one, under healthy and several different relatively light damaged states of varying severity. The furnished numerical results demonstrate that both the MC index evaluated based on first mode shape data and the MSE index determined from the first three mode shape data are equally able for both damage localization and severity characterization for most of the damaged case scenarios considered. Further research is warranted to account for the influence of noisy field-recorded mode shape data as well as for sparse instrumentation in which acceleration sensors are not deployed on every building floor
On the cool gaseous haloes of quasars
We present optical spectroscopy of projected QSO pairs to investigate the
MgII and the CIV absorption features imprinted on the spectrum of the
background object by the gaseous halo surrounding the foreground QSO. We
observed 13 projected pairs in the redshift range 0.7<z<2.2 spanning projected
separations between 60 kpc and 120 kpc. In the spectra of the background QSOs,
we identify MgII intervening absorption systems associated to the foreground
QSOs in 7 out of 10 pairs, and 1 absorption system out of 3 is found for CIV.
The distribution of the equivalent width as a function of the impact parameter
shows that, unlike the case of normal galaxies, some strong absorption systems
(EWr > 1 Ang) are present also beyond a projected radius of ~70 kpc. If we take
into account the mass of the galaxies as an additional parameter that influence
the extent of the gaseous haloes, the distribution of the absorptions connected
to the QSOs is consistent to that of galaxies. In the spectra of the foreground
QSOs we do not detect any MgII absorption lines originated by the gas
surrounding the QSO itself, but in 2 cases these features are present for CIV.
The comparison between the absorption features observed in the transverse
direction and those along the line of sight allows us to comment on the
distribution of the absorbing gas and on the emission properties of the QSOs.
Based on observations undertaken at the European Southern Observatory (ESO)
Very Large Telescope (VLT) under Programmes 085.B-0210(A) and 086.B-0028(A).Comment: 15 pages, 3 tables, 9 figures. Accepted to be published on MNRA
Downsizing of supermassive black holes from the SDSS quasar survey (II). Extension to z~4
Starting from the quasar sample of the Sloan Digital Sky Survey (SDSS) for
which the CIV line is observed, we use an analysis scheme to derive the
z-dependence of the maximum mass of active black holes, which overcomes the
problems related to the Malmquist bias. The same procedure is applied to the
low redshift sample of SDSS quasars for which Hbeta measurements are available.
Combining with the results from the previously studied MgII sample, we find
that the maximum mass of the quasar population increases as (1+z)^(1.64+/-0.04)
in the redshift range 0.1<z<4, which includes the epoch of maximum quasar
activity.Comment: 9 pages, 8 figures. To appear in MNRA
A quasar companion to the puzzling quasar SDSS J0927+2943
We report the discovery of a quasar close to SDSS J0927+2943 (z = 0.713),
which is a massive binary / recoiling black hole candidate. The companion
quasar is at a projected distance of 125 h_70^{-1} kpc and exhibits a radial
velocity difference of ~1400 km/s with respect to the known quasar. We discuss
the nature of this peculiar quasar pair and the properties of its environment.
We propose that the overall system is caught in the process of ongoing
structure formation.Comment: 4 pages, 3 figures. Accepted for publication in A&
Reclassification of the nearest quasar pair candidate: SDSS J15244+3032 - RXS J15244+3032
We present optical spectroscopy of the nearest quasar pair listed in the 13th
edition of the Veron-Cetty & Veron catalogue, i.e. the two quasars SDSS
J15244+3032 and RXS J15244+3032 (redshift z~0.27, angular separation ~7 arcsec,
and line-of-sight velocity difference ~1900 km/s). This system would be an
optimal candidate to investigate the mutual interaction of the host galaxies
with ground based optical imaging and spectroscopy. However, new optical data
demonstrate that RXS J15244+3032 is indeed a star of spectral type G.
This paper includes data gathered with the Asiago 1.82m telescope (Cima Ekar
Observatory, Asiago, Italy).Comment: 5 pages, 2 figures, 1 table. Accepted for publication in APS
The optical spectrum of PKS 1222+216 and its black hole mass
We investigate the optical spectral properties of the blazar PKS 1222+216
during a period of 3 years. While the continuum is highly variable the broad
line emission is practically constant. This supports a scenario in which the
broad line region is not affected by jet continuum variations. We thus infer
the thermal component of the continuum from the line luminosity and we show
that it is comparable with the continuum level observed during the phases of
minimum optical activity. The mass of the black hole is estimated through the
virial method from the FWHM of MgII, Hbeta, and Halpha broad lines and from the
thermal continuum luminosity. This yields a consistent black hole mass value of
6x10^8 solar masses.Comment: 7 pages, 4 figures, accepted for publication in MNRA
The quasar M_bh - M_host relation through Cosmic Time I - Dataset and black hole masses
We study the M_bh - M_host relation as a function of Cosmic Time in a sample
of 96 quasars from z=3 to the present epoch. In this paper we describe the
sample, the data sources and the new spectroscopic observations. We then
illustrate how we derive M_bh from single-epoch spectra, pointing out the
uncertainties in the procedure. In a companion paper, we address the dependence
of the ratio between the black hole mass and the host galaxy luminosity and
mass on Cosmic Time.Comment: 16 pages, 6 figures, 5 tables. Accepted for publication in MNRA
The kiloparsec-scale star formation law at redshift 4: wide-spread, highly efficient star formation in the dust-obscured starburst galaxy GN20
We present high-resolution observations of the 880 m (rest-frame FIR)
continuum emission in the z4.05 submillimeter galaxy GN20 from the IRAM
Plateau de Bure Interferometer (PdBI). These data resolve the obscured star
formation in this unlensed galaxy on scales of
0.30.2 (2.11.3 kpc).
The observations reveal a bright (161 mJy) dusty starburst centered on the
cold molecular gas reservoir and showing a bar-like extension along the major
axis. The striking anti-correlation with the HST/WFC3 imaging suggests that the
copious dust surrounding the starburst heavily obscures the rest-frame
UV/optical emission. A comparison with 1.2 mm PdBI continuum data reveals no
evidence for variations in the dust properties across the source within the
uncertainties, consistent with extended star formation, and the peak star
formation rate surface density (1198 M yr kpc)
implies that the star formation in GN20 remains sub-Eddington on scales down to
3 kpc. We find that the star formation efficiency is highest in the central
regions of GN20, leading to a resolved star formation law with a power law
slope of , and that
GN20 lies above the sequence of normal star-forming disks, implying that the
dispersion in the star formation law is not due solely to morphology or choice
of conversion factor. These data extend previous evidence for a fixed star
formation efficiency per free-fall time to include the star-forming medium on
kpc-scales in a galaxy 12 Gyr ago.Comment: 6 pages, 5 figures, accepted to ApJ
Oral contraceptive use and the risk of epithelial ovarian cancer.
The relation between the use of combination oral contraceptives (OCs) and the risk of epithelial ovarian cancer was investigated in a case-control study conducted in Milan on 209 women below the age of 60 with histologically confirmed epithelial ovarian cancer, and 418 age-matched controls with a spectrum of acute conditions apparently unrelated to OC use. Combination oral contraceptives were used by 18 (9%) cases, and 59 (14%) controls, giving a relative risk estimate of 0.6 (95% confidence interval = 0.3-1.0, P less than 0.05). The risk of ovarian cancer decreased with increasing duration of use and the point estimate remained below unity long after cessation of use. These results were not accounted for by parity, infertility, or other identified potential confounding factors. Thus, the findings of the present study add further support to the evidence emerging from American data of a reduction of approximately 40% in the risk of epithelial ovarian cancer among women who had used oral contraceptives
- …