2,164 research outputs found
First proper motions of thin dust filaments at the Galactic Center
Context: L'-band (3.8 micron) images of the Galactic Center show a large
number of thin filaments in the mini-spiral, located west of the mini-cavity
and along the inner edge of the Northern Arm. One possible mechanism that could
produce such structures is the interaction of a central wind with the
mini-spiral. Additionally, we identify similar features that appear to be
associated with stars. Aims: We present the first proper motion measurements of
the thin dust filaments observed in the central parsec around SgrA* and
investigate possible mechanisms that could be responsible for the observed
motions. Methods: The observations have been carried out using the NACO
adaptive optics system at the ESO VLT. The images have been transformed to a
common coordinate system and features of interest were extracted. Then a
cross-correlation technique could be performed in order to determine the
offsets between the features with respect to their position in the reference
epoch. Results: We derive the proper motions of a number of filaments and 2
cometary shaped dusty sources close (in projection) to SgrA*. We show that the
shape and the motion of the filaments does not agree with a purely Keplerian
motion of the gas in the potential of the supermassive black hole at the
position of SgrA*. Therefore, additional mechanisms must be responsible for
their formation and motion. We argue that the properties of the filaments are
probably related to an outflow from the disk of young mass-losing stars around
SgrA*. In part, the outflow may originate from the black hole itself. We also
present some evidence and theoretical considerations that the outflow may be
collimated.Comment: accepted for publication by A&
Galaxy evolution across the optical emission-line diagnostic diagrams?
The discovery of the M-sigma relation, the local galaxy bimodality, and the
link between black-hole and host-galaxy properties, have raised the question
whether AGN play a role in galaxy evolution. Several theoretical models
implement AGN feedback to explain the observed galaxy luminosity function, and
possibly the color and morphological transformation of spiral galaxies into
passive ellipticals. To understand the importance of AGN feedback, a study of
the AGN populations in the radio-optical domain is crucial. A mass sequence
linking star-forming galaxies and AGN has been already noted in previous works,
and it is now investigated as possible evolutionary sequence. We observed a
sample of 119 intermediate-redshift (0.04<z<0.4) SDSS-FIRST radio emitters with
the Effelsberg 100-m telescope at 4.85 and 10.45 GHz and obtained spectral
indices. We find indications of spectral index flattening in high-metallicity
star-forming galaxies, composite galaxies, and Seyferts. This "flattening
sequence" along the [NII]-based emission-line diagnostic diagram is consistent
with the hardening of galaxy ionizing field, due to nuclear activity. After
combining our data with FIRST measurements at 1.4 GHz, we find that the
three-point radio spectra of Seyferts and LINERs show substantial differences,
attributable to small radio core components and larger (arcsecond sized)
jet/lobe components, respectively. A visual inspection of FIRST images seems to
confirm this hypothesis. Galaxies along this sequence are hypothesized to be
transitioning from the active star-forming galaxies (blue cloud) to the passive
elliptical galaxies (red sequence). This supports the suggestion that AGN play
a role in shutting down star-formation, and allow the transition from one
galaxy class to the other.Comment: 20 pages, 19 figures, accepted for publication in A&
On the orientation of the Sagittarius A* system
The near-infrared emission from the black hole at the Galactic center (Sgr
A*) has unique properties. The most striking feature is a suggestive periodic
sub-structure that has been observed in a couple of flares so far. Using
near-infrared polarimetric observations and modelling the quasi-periodicity in
terms of an orbiting blob, we try to constrain the three dimensional
orientation of the Sgr A* system. We report on so far unpublished polarimetric
data from 2003. They support the observations of a roughly constant mean
polarization angle of 60 degr \pm 20 degr from 2004-2006. Prior investigations
of the 2006 data are deepened. In particular, the blob model fits are evaluated
such that constraints on the position angle of Sgr A* can be derived.
Confidence contours in the position-inclination angle plane are derived. On a
3sigma level the position angle of the equatorial plane normal is in the range
60 degr - 108 degr (east of north) in combination with a large inclination
angle. This agrees well with recent independent work in which radio
spectral/morphological properties of Sgr A* and X-ray observations,
respectively, have been used. However, the quality of the presently available
data and the uncertainties in our model bring some ambiguity to our
conclusions.Comment: 10 pages, 4 figures; Research Note accepted by A&A for publicatio
Simultaneous NIR/sub-mm observation of flare emission from SgrA*
We report on a successful, simultaneous observation and modeling of the
sub-millimeter to near-infrared flare emission of the Sgr A* counterpart
associated with the super-massive black hole at the Galactic center. Our
modeling is based on simultaneous observations that have been carried out on 03
June, 2008 using the NACO adaptive optics (AO) instrument at the ESO VLT and
the LABOCA bolometer at the APEX telescope. Inspection and modeling of the
light curves show that the sub-mm follows the NIR emission with a delay of
1.5+/-0.5 hours. We explain the flare emission delay by an adiabatic expansion
of the source components.Comment: 12 pages, 9 figures, 3 tables, in press with A&
Resolving the Host Galaxy of the Nearby QSO I Zw 1 with Sub-Arcsecond Multi-Transition Molecular Line Observations
We present the first sub-kpc 0.7" (~ 850 pc) resolution 12CO(1-0) molecular
line observations of the ISM in the host galaxy of the QSO I Zw 1. The
observations were obtained with the BIMA mm-interferometer in its compact A
configuration. The BIMA data are complemented by new observations of the
12CO(2-1) and 13CO(1-0) line with IRAM Plateau de Bure mm-interferometer (PdBI)
at 0.9" and 1.9" resolution, respectively. These measurements, which are part
of a multi-wavelength study of the host galaxy of I Zw 1, are aimed at
comparing the ISM properties of a QSO host with those of nearby galaxies as
well as to obtain constraints on galaxy formation/evolution models. Our images
of the 12CO(1-0) line emission show a ring-like structure in the circumnuclear
molecular gas distribution with an inner radius of about 1.2 kpc. The presence
of such a molecular gas ring was predicted from earlier lower angular
resolution PdBI 12CO(1-0) observations. A comparison of the BIMA data with IRAM
PdBI 12CO(2-1) observations shows variations in the excitation conditions of
the molecular gas in the innermost 1.5" comprising the nuclear region of I Zw
1. The observed properties of the molecular cloud complexes in the disk of the
host galaxy suggest that they can be the sites of massive circumnuclear star
formation, and show no indications of excitation by the nuclear AGN. This all
indicates that the molecular gas in a QSO host galaxy has similar properties to
the gas observed in nearby low luminosity AGNs.Comment: to be published in ApJ 1 July 2004 issu
The mean infrared emission of SagittariusA*
(abridged) The massive black hole at the center of the Milky Way,
SagittariusA* is, in relative terms, the weakest accreting black hole
accessible to observations. At the moment, the mean SED of SgrA* is only known
reliably in the radio to mm regimes. The goal of this paper is to provide
constraints on the mean emission from SgrA* in the near-to-mid infrared.
Excellent imaging quality was reached in the MIR by using speckle imaging
combined with holographic image reconstruction, a novel technique for this kind
of data. No counterpart of SgrA* is detected at 8.6 microns. At this
wavelength, SgrA* is located atop a dust ridge, which considerably complicates
the search for a potential point source. An observed 3 sigma upper limit of ~10
mJy is estimated for the emission of SgrA* at 8.6 microns, a tighter limit at
this wavelength than in previous work. The de-reddened 3 sigma upper limit,
including the uncertainty of the extinction correction, is ~84 mJy . Based on
the available data, it is argued that, with currently available instruments,
SgrA* cannot be detected in the MIR, not even during flares. At 4.8 and 3.8
microns, on the other hand, SgrA* is detected at all times, at least when
considering timescales of a few up to 13 min. We derive well-defined
time-averaged, de-reddened flux densities of 3.8+-1.3 mJy at 4.8 microns and
5.0+-0.6 mJy at 3.8 microns. Observations with NIRC2/Keck and NaCo/VLT from the
literature provide good evidence that SgrA* also has a fairly well-defined
de-reddened mean flux of 0.5-2.5 mJy at wavelengths of 2.1-2.2 microns. We
present well-constrained anchor points for the SED of SgrA* on the
high-frequency side of the Terahertz peak. The new data are in general
agreement with published theoretical SEDs of the mean emission from SgrA*, but
we expect them to have an appreciable impact on the model parameters in future
theoretical work.Comment: accepted for publication by Astronomy & Astrophysics on 20 June 201
K-band polarimetry of an Sgr A* flare with a clear sub-flare structure
Context: The supermassive black hole at the Galactic center, SgrA*, shows
frequent radiation outbursts, often called 'flares'. In the near-infrared some
of these flares were reported as showing intrinsic quasi-periodicities. The
flux peaks associated with the quasi-periodic behavior were found to be highly
polarized. Aims: The aim of this work is to present new evidence to support
previous findings of the properties of the polarized radiation from SgrA* and
to again provide strong support for the quasi-periodicity of ~18+-3 min
reported earlier. Methods: Observations were carried out at the European
Southern Observatory's Very Large Telescope on Paranal, Chile. We used the
NAOS/CONICA adaptive optics/near-infrared camera instrument. By fitting the
polarimetric lightcurves with a hot-spot model, we addressed the question of
whether the data are consistent with this model. To fit the observed data we
used a general relativistic ray-tracing code in combination with a simple
hot-spot/ring model. Results: We report on new polarization measurements of a
K-band flare from the supermassive black hole at the Galactic center. The data
provide very strong support for a quasi-periodicity of 15.5+-2 min. The mean
polarization of the flare is consistent with the direction of the electric
field vector that was reported in previous observations. The data can be
modeled successfully with a combined blob/ring model. The inclination i of the
blob orbit must be i > 20 deg on a 3sigma level, and the dimensionless spin
parameter of the black hole is derived to be a > 0.5.Comment: accepted by A&A Letters for publication; 5 pages, 9 figure
Coordinated NIR/mm observations of flare emission from Sagittarius A*
We report on a successful, simultaneous observation and modelling of the
millimeter (mm) to near-infrared (NIR) flare emission of the Sgr A* counterpart
associated with the supermassive black hole at the Galactic centre (GC). We
present a mm/sub-mm light curve of Sgr A* with one of the highest quality
continuous time coverages and study and model the physical processes giving
rise to the variable emission of Sgr A*.Comment: 14 pages, 16 figure
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