2,372 research outputs found
The broad-band radio spectrum of LSI+61303 in outburst
Aims: Our aim is to explore the broad-band radio continuum spectrum of
LSI+61303 during its outbursts by employing the available set of secondary
focus receivers of the Effelsberg 100 m telescope. Methods: The clear
periodicity of the system LSI+61303 allowed observations to be scheduled
covering the large radio outburst in March-April 2012. We observed LSI+61303 on
14 consecutive days at 2.6, 4.85, 8.35, 10.45, 14.3, 23, and 32 GHz with a
cadence of about 12 hours followed by two additional observations several days
later. Based on these observations we obtained a total of 24 quasi-simultaneous
broad-band radio spectra. Results: During onset, the main flare shows an almost
flat broad-band spectrum, most prominently seen on March 27, 2012, where - for
the first time - a flat spectrum (alpha=0.00+/-0.07, S nu^alpha) is observed up
to 32 GHz (9 mm wavelength). The flare decay phase shows superimposed
'sub-flares' with the spectral index oscillating between -0.4 and -0.1 in a
quasi-regular fashion. Finally, the spectral index steepens during the decay
phase, showing optically thin emission with values alpha -0.5 to -0.7.
Conclusions: The radio characteristics of LSI+61303 compare well with those of
the microquasars XTE J1752-223 and Cygnus X-3. In these systems the flaring
phase is actually also composed of a sequence of outbursts with clearly
different spectral characteristics: a first outburst with a flat/inverted
spectrum followed by a bursting phase of optically thin emission.Comment: 4 pages, 3 figures, accepted for publication in A&
The Gamma-Ray Detected Narrow-Line Seyfert 1 Galaxy 1H 0323+342: Swift Monitoring and Suzaku Spectroscopy
As a radio-loud narrow-line Seyfert 1 galaxy (NLS1) detected by Fermi/LAT in
GeV -rays, 1H 0323+342 is a remarkable Active Galactic Nucleus (AGN)
showing properties characteristic of both NLS1s and blazars. Here we present
results of simultaneous X-ray and UV/optical monitoring observations on 1H
0323+342 taken with the UV/Optical Telescope (UVOT) and X-ray Telescope (XRT)
onboard the Swift satellite over six years from 2006. Overall, the object
showed statistically correlated variations in both the UV and X-ray bands on
timescales of years as well as on timescales of days. A deep Suzaku observation
reveals X-ray variability on timescales as short as a few tens of thousand
seconds, and an X-ray spectrum typical of Seyfert galaxies. The broad-band
spectral energy distribution, for which the data of UV and X-ray observations
taken on 2009 July 26-27 were used, can be well modeled with a simple one-zone
leptonic jet model plus accretion disk/corona emission. The latter is
predominantly responsible for the UV/optical and X-ray (0.3-10 keV) emission
and their observed variations. The correlated UV-X-ray variability on the
timescale of days is consistent with reprocessing of the X-ray radiation by the
accretion disk. The shortest timescale and large normalized excess variance of
the X-ray variability detected with Suzaku suggest a relatively small black
hole mass of the order of , consistent with the estimation based
on the broad H line in the optical.Comment: 38 pages, 12 figures, in press, accepted by AJ (first submitted on
2014 July 7th
S5 0716+714 : GeV variability study
The GeV observations by Fermi-LAT give us the opportunity to characterize the
high-energy emission (100 MeV - 300 GeV) variability properties of the BL Lac
object S5 0716+714. In this study, we performed flux and spectral analysis of
more than 3 year long (August 2008 to April 2012) Fermi-LAT data of the source.
During this period, the source exhibits two different modes of flux variability
with characteristic timescales of ~75 and ~140 days, respectively. We also
notice that the flux variations are characterized by a weak spectral hardening.
The GeV spectrum of the source shows a clear deviation from a simple power law,
and is better explained by a broken power law. Similar to other bright Fermi
blazars, the break energy does not vary with the source flux during the
different activity states. We discuss several possible scenarios to explain the
observed spectral break.Comment: 21 pages, 10 figures, Accepted for publication in Advances in Space
Research journa
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&
Metallicities of M Dwarf Planet Hosts from Spectral Synthesis
We present the first spectroscopic metallicities of three M dwarfs with known
or candidate planetary mass companions. We have analyzed high resolution, high
signal-to-noise spectra of these stars which we obtained at McDonald
Observatory. Our analysis technique is based on spectral synthesis of atomic
and molecular features using recently revised cool-star model atmospheres and
spectrum synthesis code. The technique has been shown to yield results
consistent with the analyses of solar-type stars and allows measurements of M
dwarf [M/H] values to 0.12 dex precision. From our analysis, we find [M/H] =
-0.12, -0.32, and -0.33 for GJ 876, GJ 436, and GJ 581 respectively. These
three M dwarf planet hosts have sub-solar metallicities, a surprising departure
from the trend observed in FGK-type stars. This study is the first part of our
ongoing work to determine the metallicities of the M dwarfs included in the
McDonald Observatory planet search program.Comment: 13 pages, 2 figures, accepted for publication in ApJ
Simultaneous Radio to (Sub-) mm-Monitoring of Variability and Spectral Shape Evolution of potential GLAST Blazars
The Large Area Telescope (LAT) instrument onboard GLAST offers a tremendous
opportunity for future blazar studies. In order to fully benefit from its
capabilities and to maximize the scientific return from the LAT, it is of great
importance to conduct dedicated multi-frequency monitoring campaigns that will
result comprehensive observations. Consequently, we initiated an effort to
conduct a GLAST-dedicated, quasi-simultaneous, broad-band flux-density (and
polarization) monitoring of potential GLAST blazars with the Effelsberg and
OVRO radio telescopes (11cm to 7mm wavelength). Here, we present a short
overview of these activities which will complement the multi-wavelengths
activities of the GLAST/LAT collaboration towards the 'low-energy' radio bands.
Further we will give a brief outlook including the extension of this
coordinated campaign towards higher frequencies and future scientific aims.Comment: 3 pages, to appear in the Proceedings of the First GLAST Symposium,
Stanford University, February 200
Planet-Induced Emission Enhancements in HD 179949: Results from McDonald Observations
We monitored the Ca II H and K lines of HD 179949, a notable star in the
southern hemisphere, to observe and confirm previously identified planet
induced emission (PIE) as an effect of star-planet interaction. We obtained
high resolution spectra (R ~ 53,000) with a signal-to-noise ratio S/N >~ 50 in
the Ca II H and K cores during 10 nights of observation at the McDonald
Observatory. Wide band echelle spectra were taken using the 2.7 m telescope.
Detailed statistical analysis of Ca II K revealed fluctuations in the Ca II K
core attributable to planet induced chromospheric emission. This result is
consistent with previous studies by Shkolnik et al. (2003). Additionally, we
were able to confirm the reality and temporal evolution of the phase shift of
the maximum of star-planet interaction previously found. However, no
identifiable fluctuations were detected in the Ca II H core. The Al I lambda
3944 A line was also monitored to gauge if the expected activity enhancements
are confined to the chromospheric layer. Our observations revealed some
variability, which is apparently unassociated with planet induced activity.Comment: 11 pages, 11 figures, 5 tables; Publications of the Astronomical
Society of Australia (in press
Minimal symmetric Darlington synthesis
We consider the symmetric Darlington synthesis of a p x p rational symmetric
Schur function S with the constraint that the extension is of size 2p x 2p.
Under the assumption that S is strictly contractive in at least one point of
the imaginary axis, we determine the minimal McMillan degree of the extension.
In particular, we show that it is generically given by the number of zeros of
odd multiplicity of I-SS*. A constructive characterization of all such
extensions is provided in terms of a symmetric realization of S and of the
outer spectral factor of I-SS*. The authors's motivation for the problem stems
from Surface Acoustic Wave filters where physical constraints on the
electro-acoustic scattering matrix naturally raise this mathematical issue
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