242 research outputs found
SCALABLE AR FOR BIM ON TELECOMMUNICATION NETWORK SITES
A growing number of research works, experiments and applications is investigating the potential at the intersection of augmented
reality (AR) and the architecture, engineering, and construction (AEC) industry. Project management, project communication,
collaborative design, maintenance and construction progress documentation, construction site safety, and training are some of the cases
that can benefit from blending real and virtual views through mobile devices. In recent years, research also highlighted how mixed
reality and building information modeling (BIM) could cooperate to provide effective communication between multiple agents and
closer interaction between digital information and the building site. Nevertheless, consolidated applications in these fields are still
limited, especially when compared to other areas of AR adoption. This paper presents the development of an AR-based mobile app for
exploring telecommunications tower sites and interacting with a related BIM database. The project aims to provide easy-to-use tools
to maintain both the physical assets and an up-to-date model. We discuss critical issues in developing a scalable and interoperable
application, supporting the feasibility study of similar solutions in the AEC sector
The rest-frame UV-to-optical spectroscopy of APM 08279+5255 - BAL classification and black hole mass estimates
We present the analysis of the rest-frame optical-to-UV spectrum of APM
08279+5255, a well-known lensed broad absorption line (BAL) quasar at . The spectroscopic data are taken with the optical DOLoRes and near-IR
NICS instruments at TNG, and include the previously unexplored range between C
III] 1910 and [O III] 4959,5007. We investigate the
possible presence of multiple BALs by computing "balnicity" and absorption
indexes (i.e. BI, BI and AI) for the transitions Si IV 1400, C IV
1549, Al III 1860 and Mg II 2800. No clear evidence
for the presence of absorption features is found in addition to the already
known, prominent BAL associated to C IV, which supports a high-ionization BAL
classification for APM 08279+5255. We also study the properties of the [O III],
H and Mg II emission lines. We find that [O III] is intrinsically weak
(), as it is typically found in
luminous quasars with a strongly blueshifted C IV emission line (2500 km
s for APM 08279+5255). We compute the single-epoch black hole mass based
on Mg II and H broad emission lines, finding M, with the magnification factor that can
vary between 4 and 100 according to CO and rest-frame UV-to-mid-IR imaging
respectively. Using a Mg II equivalent width (EW)-to-Eddington ratio relation,
the EW \AA\ measured for APM 08279+5255 translates into an
Eddington ratio of 0.4, which is more consistent with . This
magnification factor also provides a value of that is consistent
with recent reverberation-mapping measurements derived from C IV and Si IV.Comment: 10 pages, 4 figures, 4 tables, accepted for publication in A&
Evidence for a clumpy disc-wind in the star forming Seyfert\,2 galaxy MCG--03--58--007
We report the results of a detailed analysis of a deep simultaneous \textit{XMM-Newton & NuSTAR} observation of the nearby () and
bright () starburst-AGN
Seyfert\,2 system: MCG--03--58--007. From the broadband fitting we show that
most of the obscuration needs to be modeled with a toroidal type reprocessor
such as \texttt{MYTorus} \citep{MurphyYaqoob09}. Nonetheless the signature of a
powerful disc-wind is still apparent at higher energies and the observed rapid
short-term X-ray spectral variability is more likely caused by a variable zone
of highly ionized fast wind rather than by a neutral clumpy medium. We also
detect X-ray emission from larger scale gas as seen from the presence of
several soft narrow emission lines in the RGS, originating from a contribution
of a weak star forming activity together with a dominant photoionized component
from the AGN.Comment: 16 pages, 9 figures, accepted for publication in MNRA
The MAGNUM survey: Positive feedback in the nuclear region of NGC 5643 suggested by MUSE
We study the ionization and kinematics of the ionized gas in the nuclear
region of the barred Seyfert 2 galaxy NGC~5643 using MUSE integral field
observations in the framework of the MAGNUM (Measuring Active Galactic Nuclei
Under MUSE Microscope) survey. The data were used to identify regions with
different ionization conditions and to map the gas density and the dust
extinction. We find evidence for a double sided ionization cone, possibly
collimated by a dusty structure surrounding the nucleus. At the center of the
ionization cone, outflowing ionized gas is revealed as a blueshifted,
asymmetric wing of the [OIII] emission line, up to projected velocity
v(10)~-450 km/s. The outflow is also seen as a diffuse, low luminosity radio
and X-ray jet, with similar extension. The outflowing material points in the
direction of two clumps characterized by prominent line emission with spectra
typical of HII regions, located at the edge of the dust lane of the bar. We
propose that the star formation in the clumps is due to `positive feedback'
induced by gas compression by the nuclear outflow, providing the first
candidate for outflow induced star formation in a Seyfert-like radio quiet AGN.
This suggests that positive feedback may be a relevant mechanism in shaping the
black hole-host galaxy coevolution.Comment: 9 pages, 7 figures, accepted for publication in A&
Ionised outflows in z 2.4 quasar host galaxies
AGN-driven outflows are invoked by galaxy evolutionary models to quench star
formation and to explain the origin of the relations observed locally between
super massive black holes and their host galaxies. This work aims to detect the
presence of extended ionised outflows in luminous quasars where we expect the
maximum activity both in star formation and in black hole accretion. Currently,
there are only a few studies based on spatially resolved observations of
outflows at high redshift, . We analyse a sample of six luminous () quasars at , observed in H-band using the
near-IR integral field spectrometer SINFONI at VLT. We perform a kinematic
analysis of the [OIII] emission line at . [OIII] has a
complex gas kinematic, with blue-shifted velocities of a few hundreds of km/s
and line widths up to 1500 km/s. Using the spectroastrometric method we infer
size of the ionised outflows of up to 2 kpc. The properties of the
ionised outflows, mass outflow rate, momentum rate and kinetic power, are
correlated with the AGN luminosity. The increase in outflow rate with
increasing AGN luminosity is consistent with the idea that a luminous AGN
pushes away the surrounding gas through fast outflows driven by radiation
pressure, which depends on the emitted luminosity. We derive mass outflow rates
of about 6-700 M/yr for our sample, which are lower than those
observed in molecular outflows. Indeed physical properties of ionised outflows
show dependences on AGN luminosity which are similar to those of molecular
outflows but indicating that the mass of ionised gas is smaller than that of
the molecular one. Alternatively, this discrepancy between ionised and
molecular outflows could be explained with different acceleration mechanisms.Comment: 13 pages, 11 figures; accepted for publication in A&
Feedback and feeding in the context of galaxy evolution with SPICA: direct characterization of molecular outflows and inflows
A far-infrared observatory such as the {\it SPace Infrared telescope for
Cosmology and Astrophysics} ({\it SPICA}), with its unprecedented spectroscopic
sensitivity, would unveil the role of feedback in galaxy evolution during the
last Gyr of the Universe (), through the use of far- and
mid-infrared molecular and ionic fine structure lines that trace outflowing and
infalling gas. Outflowing gas is identified in the far-infrared through P-Cygni
line shapes and absorption blueshifted wings in molecular lines with high
dipolar moments, and through emission line wings of fine-structure lines of
ionized gas. We quantify the detectability of galaxy-scale massive molecular
and ionized outflows as a function of redshift in AGN-dominated,
starburst-dominated, and main-sequence galaxies, explore the detectability of
metal-rich inflows in the local Universe, and describe the most significant
synergies with other current and future observatories that will measure
feedback in galaxies via complementary tracers at other wavelengths.Comment: This paper belongs to the SPICA Special Issue on PASA. Accepted for
publication in PAS
Cold molecular outflows in the local Universe and their feedback effect on galaxies
We study molecular outflows in a sample of 45 local galaxies, both star
forming and AGN, primarily by using CO data from the ALMA archive and from the
literature. For a subsample we also compare the molecular outflow with the
ionized and neutral atomic phases. We infer an empirical analytical function
relating the outflow rate simultaneously to the SFR, , and galaxy
stellar mass; this relation is much tighter than the relations with the
individual quantities. The outflow kinetic power shows a larger scatter than in
previous, more biased studies, spanning from 0.1 to 5 per cent of , while the momentum rate ranges from 1 to 30 times ,
indicating that these outflows can be both energy-driven, but with a broad
range of coupling efficiencies with the ISM, and radiation pressure-driven. For
about 10 per cent of the objects the outflow energetics significantly exceed
the maximum theoretical values; we interpret these as 'fossil outflows'
resulting from activity of a past strong AGN, which has now faded. We estimate
that, in the stellar mass range probed here ( 10), less
than 5 per cent of the outflowing gas escapes the galaxy. The molecular gas
depletion time associated with the outflow can be as short as a few million
years in powerful AGN, however, the total gas (H+HI) depletion times are
much longer. Altogether, our findings suggest that even AGN-driven outflows
might be relatively ineffective in clearing galaxies of their entire gas
content, although they are likely capable of clearing and quenching the central
region
A new powerful and highly variable disk wind in an AGN-star forming galaxy, the case of MCG-03-58-007
We present the discovery of a new candidate for a fast disk wind, in the
nearby Seyfert 2 galaxy MCG-03-58-007. This wind is discovered in a deep Suzaku
observation that was performed in 2010. Overall the X-ray spectrum of
MCG-03-58-007 is highly absorbed by a neutral column density of NH~10^23 cm^-2,
in agreement with the optical classification as a type 2 AGN. In addition, this
observation unveiled the presence of two deep absorption troughs at E = 7.4 +-
0.1 keV and E = 8.5 +- 0.2 keV. If associated with blue-shifted FeXXVI, these
features can be explained with the presence of two highly ionised (log \xi/(erg
cm/s)~ 5.5) and high column density (NH~5-8 x 10^23cm^-2) outflowing absorbers
with v_out1~ -0.1c and v_out2~ -0.2c. The disk wind detected during this
observation is most likely launched from within a few hundreds gravitational
radii from the central black and has a kinetic output that matches the
prescription for significant feedback. The presence of the lower velocity
component of the disk wind is independently confirmed by the analysis of a
follow-up XMM-Newton & NuSTAR observation. A faster (v_out~ -0.35 c) component
of the wind is also seen in this second observation. During this observation we
also witnessed an occultation event lasting \Delta t ~ 120 ksec, which we
ascribe to an increase of the opacity of the disk wind (\Delta NH~1.4x10^24
cm^-2). Our interpretation is that the slow zone (v_out~ -0.1c) of the wind is
the most stable but inhomogeneous component, while the faster zones could be
associated with two different inner streamlines of the wind.Comment: 12 pages, 10 figures, 3 tables. Accepted for publication in MNRA
- …