1,465 research outputs found
The Herschel Virgo Cluster Survey. VI. The far-infrared view of M87
The origin of the far-infrared emission from the nearby radio galaxy M87 remains a matter of debate. Some studies find evidence of a far-infrared excess due to thermal dust emission, whereas others propose that the far-infrared emission can be explained by synchrotron emission without
the need for an additional dust emission component. We present Herschel PACS and SPIRE observations of M87, taken as part of the science demonstration phase observations of the Herschel Virgo Cluster Survey. We compare these data with a synchrotron model based on mid-infrared, far-infrared, submm and radio data from the literature to investigate the origin of the far-infrared emission. Both the integrated SED and the Herschel surface brightness maps are adequately explained by synchrotron emission. At odds with previous claims, we find no evidence of a diffuse dust component in M87, which is not unexpected in the harsh X-ray environment of this radio galaxy sitting at the core of the Virgo cluster
Herschel-ATLAS: The dust energy balance in the edge-on spiral galaxy UGC4754
We use Herschel PACS and SPIRE observations of the edge-on spiral galaxy UGC4754, taken as part of the H-ATLAS SDP observations, to investigate the dust energy balance in this galaxy. We build detailed SKIRT radiative models based on SDSS and UKIDSS maps and use these models to predict the far-infrared emission. We find that our radiative transfer model underestimates the observed FIR emission by a factor of two to three. Similar discrepancies have been found for other edge-on spiral galaxies based on IRAS, ISO, and SCUBA data. Thanks to the good sampling of the SED at FIR wavelengths, we can rule out an underestimation of the FIR emissivity as the cause for this discrepancy. Instead we support highly obscured star formation that contributes little to the optical extinction as a more probable explanation
Hierarchical octree and k-d tree grids for 3D radiative transfer simulations
A crucial ingredient for numerically solving the 3D radiative transfer
problem is the choice of the grid that discretizes the transfer medium. Many
modern radiative transfer codes, whether using Monte Carlo or ray tracing
techniques, are equipped with hierarchical octree-based grids to accommodate a
wide dynamic range in densities. We critically investigate two different
aspects of octree grids in the framework of Monte Carlo dust radiative
transfer. Inspired by their common use in computer graphics applications, we
test hierarchical k-d tree grids as an alternative for octree grids. On the
other hand, we investigate which node subdivision-stopping criteria are optimal
for constructing of hierarchical grids. We implemented a k-d tree grid in the
3D radiative transfer code SKIRT and compared it with the previously
implemented octree grid. We also considered three different node
subdivision-stopping criteria (based on mass, optical depth, and density
gradient thresholds). Based on a small suite of test models, we compared the
efficiency and accuracy of the different grids, according to various quality
metrics. For a given set of requirements, the k-d tree grids only require half
the number of cells of the corresponding octree. Moreover, for the same number
of grid cells, the k-d tree is characterized by higher discretization accuracy.
Concerning the subdivision stopping criteria, we find that an optical depth
criterion is not a useful alternative to the more standard mass threshold,
since the resulting grids show a poor accuracy. Both criteria can be combined;
however, in the optimal combination, for which we provide a simple approximate
recipe, this can lead to a 20% reduction in the number of cells needed to reach
a certain grid quality. An additional density gradient threshold criterion can
be added that solves the problem of poorly resolving sharp edges and...
(abridged).Comment: 10 pages, 6 figures. Accepted for publication in A&
Testing baryon-induced core formation in CDM: A comparison of the DC14 and coreNFW dark matter halo models on galaxy rotation curves
Recent cosmological hydrodynamical simulations suggest that baryonic
processes, and in particular supernova feedback after bursts of star formation,
can alter the structure of dark matter haloes and transform primordial cusps
into shallower cores. To assess whether this mechanism offers a solution to the
cusp-core controversy, simulated haloes must be compared to real dark matter
haloes inferred from galaxy rotation curves. For this purpose, two new dark
matter density profiles were recently derived from simulations of galaxies in
complementary mass ranges: the DC14 halo () and the coreNFW halo (). Both models have individually been found to give good fits to
observed rotation curves. For the DC14 model, however, the agreement of the
predicted halo properties with cosmological scaling relations was confirmed by
one study, but strongly refuted by another. A next question is whether the two
models converge to the same solution in the mass range where both should be
appropriate. To investigate this, we tested the DC14 and cNFW halo models on
the rotation curves of a selection of galaxies with halo masses in the range - . We further applied the DC14
model to a set of rotation curves at higher halo masses, up to , to verify the agreement with the cosmological scaling
relations. We find that both models are generally able to reproduce the
observed rotation curves, in line with earlier results, and the predicted dark
matter haloes are consistent with the cosmological and
relations. The DC14 and cNFW models are also in fairly
good agreement with each other, even though DC14 tends to predict slightly less
extended cores and somewhat more concentrated haloes than cNFW.Comment: 19 pages, 12 figures, accepted for publication in A&
The dynamical structure of isotropic spherical galaxies with a central black hole
We discuss the kinematical structure of a two-parameter family of isotropic
models with a central black hole. The family contains the slope of the central
density cusp and the relative black hole mass as parameters. Most of the basic
kinematical quantities of these models can be expressed analytically. This
family contains three distinct models where also the distribution function,
differential energy distribution and spatial LOSVDs can be expressed completely
analytically. Each of these models show a drastically different behaviour of
the distribution function. Although the effect of a black hole on the
distribution function is very strong, in particular for models with a shallow
density cusp, the differential energy distribution is only marginally affected.
We discuss in detail the effects of a central black hole on the LOSVDs. The
projected velocity dispersion increases with black hole mass at small projected
radii, but the effect of a black hole on the shape of the LOSVDs (characterized
by the h4 parameter) is less straightforward to interpret. Too much reliance on
the wings of the LOSVDs and the value of the h4 parameter to determine black
hole masses might hence be dangerous.Comment: 12 pages, 3 figures, accepted for publication in A&
Studying the spectral properties of Active Galactic Nuclei in the JWST era
The James Webb Space Telescope (JWST), due to launch in 2014, shall provide
an unprecedented wealth of information in the near and mid-infrared
wavelengths, thanks to its high-sensitivity instruments and its 6.5 m primary
mirror, the largest ever launched into space. NIRSpec and MIRI, the two
spectrographs onboard JWST, will play a key role in the study of the spectral
features of Active Galactic Nuclei in the 0.6-28 micron wavelength range. This
talk aims at presenting an overview of the possibilities provided by these two
instruments, in order to prepare the astronomical community for the JWST era.Comment: 8 pages, 1 figure, accepted for publication in New Astronomy Reviews
(proceedings of 7th Serbian Conference on Spectral Line Shapes in
Astrophysics
Observations of apparent superslow wave propagation in solar prominences
Phase mixing of standing continuum Alfv\'en waves and/or continuum slow waves
in atmospheric magnetic structures such as coronal arcades can create the
apparent effect of a wave propagating across the magnetic field. We observe a
prominence with SDO/AIA on 2015 March 15 and find the presence of oscillatory
motion. We aim to demonstrate that interpreting this motion as a magneto
hydrodynamic (MHD) wave is faulty. We also connect the decrease of the apparent
velocity over time with the phase mixing process, which depends on the
curvature of the magnetic field lines. By measuring the displacement of the
prominence at different heights to calculate the apparent velocity, we show
that the propagation slows down over time, in accordance with the theoretical
work of Kaneko et al. We also show that this propagation speed drops below what
is to be expected for even slow MHD waves for those circumstances. We use a
modified Kippenhahn-Schl\"uter prominence model to calculate the curvature of
the magnetic field and fit our observations accordingly. Measuring three of the
apparent waves, we get apparent velocities of 14, 8, and 4 km/s. Fitting a
simple model for the magnetic field configuration, we obtain that the filament
is located 103 Mm below the magnetic centre. We also obtain that the scale of
the magnetic field strength in the vertical direction plays no role in the
concept of apparent superslow waves and that the moment of excitation of the
waves happened roughly one oscillation period before the end of the eruption
that excited the oscillation. Some of the observed phase velocities are lower
than expected for slow modes for the circumstances, showing that they rather
fit with the concept of apparent superslow propagation. A fit with our magnetic
field model allows for inferring the magnetic geometry of the prominence.Comment: 10 pages, 6 figures, 1 of which consists of 3 panel
Tale of J1328+2752 : a misaligned double-double radio galaxy hosted by a binary black-hole?
We present a radio and optical study of the double-double radio galaxy J1328+2752 based on new low-frequency Giant Metrewave Radio Telescope observations and Sloan Digital Sky Survey (SDSS) data. The radio data were used to investigate the morphology and to perform a spectral index analysis. In this source, we find that the inner double is misaligned by similar to 30 degrees from the axis of the outer diffuse structure. The SDSS spectrum shows that the central component has double-peaked line profiles with different emission strengths. The average velocity offset of the two components is 235 +/- 10.5 kms(-1). The misaligned radio morphology along with the double-peaked emission lines indicate that this source is a potential candidate binary supermassive black hole. This study further supports mergers as a possible explanation for repeated jet activity in radio sources
Dynamical models with a general anisotropy profile
Both numerical simulations and observational evidence indicate that the outer
regions of galaxies and dark matter haloes are typically mildly to
significantly radially anisotropic. The inner regions can be significantly
non-isotropic, depending on the dynamical formation and evolution processes. In
an attempt to break the lack of simple dynamical models that can reproduce this
behaviour, we explore a technique to construct dynamical models with an
arbitrary density and an arbitrary anisotropy profile. We outline a general
construction method and propose a more practical approach based on a
parameterized anisotropy profile. This approach consists of fitting the density
of the model with a set of dynamical components, each of which have the same
anisotropy profile. Using this approach we avoid the delicate fine-tuning
difficulties other fitting techniques typically encounter when constructing
radially anisotropic models. We present a model anisotropy profile that
generalizes the Osipkov-Merritt profile, and that can represent any smooth
monotonic anisotropy profile. Based on this model anisotropy profile, we
construct a very general seven-parameter set of dynamical components for which
the most important dynamical properties can be calculated analytically. We use
the results to look for simple one-component dynamical models that generate
simple potential-density pairs while still supporting a flexible anisotropy
profile. We present families of Plummer and Hernquist models in which the
anisotropy at small and large radii can be chosen as free parameters. We also
generalize these two families to a three-parameter family that
self-consistently generates the set of Veltmann potential-density pairs.
(Abridged...)Comment: 18 pages, accepted for publication in A&
New HErschel Multi-wavelength Extragalactic Survey of Edge-on Spirals (NHEMESES)
Edge-on spiral galaxies offer a unique perspective on the vertical structure
of spiral disks, both stars and the iconic dark dustlanes. The thickness of
these dustlanes can now be resolved for the first time with Herschel in
far-infrared and sub-mm emission. We present NHEMESES, an ongoing project that
targets 12 edge-on spiral galaxies with the PACS and SPIRE instruments on
Herschel. These vertically resolved observations of edge-on spirals will impact
on several current topics.
First and foremost, these Herschel observations will settle whether or not
there is a phase change in the vertical structure of the ISM with disk mass.
Previously, a dramatic change in dustlane morphology was observed as in massive
disks the dust collapses into a thin lane. If this is the case, the vertical
balance between turbulence and gravity dictates the ISM structure and
consequently star-formation and related phenomena (spiral arms, bars etc.). We
specifically target lower mass nearby edge-ons to complement existing Herschel
observations of high-mass edge-on spirals (the HEROES project).
Secondly, the combined data-set, together with existing Spitzer observations,
will drive a new generation of spiral disk Spectral Energy Distribution models.
These model how dust reprocesses starlight to thermal emission but the dust
geometry remains the critical unknown.
And thirdly, the observations will provide an accurate and unbiased census of
the cold dusty structures occasionally seen extending out of the plane of the
disk, when backlit by the stellar disk. To illustrate the NHEMESES project, we
present early results on NGC 4244 and NGC 891, two well studies examples of a
low and high-mass edge-on spiral.Comment: 3 pages, 4 figures, to appear in the proceedings of IAU 284, "The
Spectral Energy Distribution of Galaxies", (SED2011), 5-9 September 2011,
Preston, UK, editors, R.J. Tuffs & C.C.Popescu (v2 updated metadata
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