1,863 research outputs found
VLBA images of the precessing jet of LSI+61303
Context: In 2004, changes in the radio morphology of the Be/X-ray binary
system LSI+61303 suggested that it is a precessing microquasar. In 2006, a set
of VLBA observations performed throughout the entire orbit of the system were
not used to study its precession because the changes in radio morphology could
tentatively be explained by the alternative pulsar model. However, a recent
radio spectral index data analysis has confirmed the predictions of the
two-peak microquasar model, which therefore does apply in LSI+61303. Aims: We
revisit the set of VLBA observations performed throughout the orbit to
determine the precession period and improve our understanding of the physical
mechanism behind the precession. Methods: By reanalyzing the VLBA data set, we
improve the dynamic range of images by a factor of four, using
self-calibration. Different fitting techniques are used and compared to
determine the peak positions in phase-referenced maps. Results: The improved
dynamic range shows that in addition to the images with a one-sided structure,
there are several images with a double-sided structure. The astrometry
indicates that the peak in consecutive images for the whole set of observations
describes a well-defined ellipse, 6-7 times larger than the orbit, with a
period of about 28 d. Conclusions: A double-sided structure is not expected to
be formed from the expanding shocked wind predicted in the pulsar scenario. In
contrast, a precessing microquasar model can explain the double- and one-sided
structures in terms of variable Doppler boosting. The ellipse defined by the
astrometry could be the cross-section of the precession cone, at the distance
of the 8.4 GHz-core of the steady jet, and 28d the precession period.Comment: 7 pages, 5 figures, Accepted for publication in Astronomy and
Astrophysics, added references for sect.
Long-term periodicity in LSI+61303 as beat frequency between orbital and precessional rate
Context: In the binary system LSI+61303 the peak flux density of the radio
outburst, which is related to the orbital period of 26.4960 +/- 0.0028d,
exibits a modulation of 1667 +/- 8 d. The radio emission at high spatial
resolution appears structured in a precessing jet with a precessional period of
27-28 d. Aims: How close is the precessional period of the radio jet to the
orbital period? Any periodicity in the radio emission should be revealed by
timing analysis. The aim of this work is to establish the accurate value of the
precessional period. Methods: We analyzed 6.7 years of the Green Bank
Interferometer database at 2.2 GHz and 8.3 GHz with the Lomb-Scargle and phase
dispersion minimization (PDM) methods and performed simulations. Results: The
periodograms show two periodicities, P1 = 26.49 +/- 0.07 d (\nu1=0.03775
d^{-1}) and P2 = 26.92 +/- 0.07 d (\nu2 = 0.03715 d^{-1}). Whereas radio
outbursts have been known to have nearly orbital occurrence P1 with timing
residuals exhibiting a puzzling sawtooth pattern, we probe in this paper that
they are actually periodical outbursts and that their period is Paverage=
(2/(\nu1 + \nu2)= 26.70 +/- 0.05 d. The period Paverage as well as the
long-term modulation Pbeat=1/(\nu1 - \nu2)=1667 +/- 393 d result from the beat
of the two close periods, the orbital P1 and the precessional P2 periods.
Conclusions: The precessional period, indicated by the astrometry to be of
27--28 d, is P2=26.92 d. The system \lsi seems to be one more case in astronomy
of beat, i.e., a phenomenon occurring when two physical processes create stable
variations of nearly equal frequencies. The very small difference in frequency
creates a long-term variation of period 1/(\nu1-\nu2). The long-term modulation
of 1667 d results from the beat of the two close orbital and precessional
rates.Comment: 8 pages, 4 figures, accepted for publication in A&
The Black Hole Candidate LSI+61303
In recent years, fundamental relationships for the black hole X-ray binaries
have been established between their X-ray luminosity and the photon index
of their X-ray spectrum. For the moderate-luminosity regime, an
anti-correlation between and has been observed. In this article,
aimed to verify if the moderate luminous X-ray binary system LSI +61303 is a
black hole, we analyse observations of LSI +61303. We compare the
derived vs distribution, first with the statistical trend for
black hole X-ray binaries, then with the trend of the pulsar PSR B1259-63, and
finally with the individual trends of the black hole X-ray binaries Swift
J1357.2-0933 and V404 Cygni. We find that the system PSR B1259-63 shows a
positive correlation between and , whereas in contrast LSI +61303
shows the same anti-correlation as for black hole X-ray binaries. Moreover, the
trend of LSI +61303 in the / plane overlaps with
that of the two black holes Swift J1357.2-0933 and V404 Cygni. All three
systems, Swift J1357.2-0933, V404 Cygni and LSI +61303 well trace the last part
of the evolution of accreting black holes at moderate-luminosity until their
drop to quiescence.Comment: 5 pages, 4 figures, MNRAS accepte
Long-term OVRO monitoring of LSI+61303: confirmation of the two close periodicities
Context: The gamma-ray binary LSI+61303 shows multiple periodicities. The
timing analysis of 6.7 yr of GBI radio data and of 6 yr of Fermi-LAT GeV
gamma-ray data both have found two close periodicities P1(GBI) = 26.49 \pm 0.07
d, P2(GBI)=26.92 \pm 0.07 d and P1(gamma)=26.48 \pm 0.08 d, P2(gamma) = 26.99
\pm 0.08 d. Aims: The system LSI+61303 is the object of several continuous
monitoring programs at low and high energies. The frequency difference between
f1 and f2 of only 0.0006 d(-1) requires long-term monitoring because the
frequency resolution in timing analysis is related to the inverse of the
overall time interval. The Owens Valley Radio Observatory (OVRO) 40 m telescope
has been monitoring the source at 15 GHz for five years and overlaps with
Fermi-LAT monitoring. The aim of this work is to establish whether the two
frequencies are also resolved in the OVRO monitoring. Methods: We analysed OVRO
data with the Lomb-Scargle method. We also updated the timing analysis of
Fermi-LAT observations. Results: The periodograms of OVRO data confirm the two
periodicities P1(OVRO) = 26.5 \pm 0.1 d and P2(OVRO) = 26.9 \pm 0.1 d.
Conclusions: The three indipendent measurements of P1 and P2 with GBI, OVRO,
and Fermi-LAT observations confirm that the periodicities are permanent
features of the system LSI+61303. The similar behaviours of the emission at
high (GeV) and low (radio) energy when the compact object in LSI+61303 is
toward apastron suggest that the emission is caused by the same periodically
(P1) ejected population of electrons in a precessing (P2) jet.Comment: 4 pages, 7 figures, A&A Letters in pres
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&
Near- and Far-Infrared Counterparts of Millimeter Dust Cores in the Vela Molecular Ridge Cloud D
The aim of this paper is to identify the young protostellar counterparts
associated to dust millimeter cores of the Vela Molecular Ridge Cloud D through
new IR observations (H_2 narrow-band at 2.12 micron and N broad band at 10.4
micron) along with an investigation performed on the existing IR catalogues.
The association of mm continuum emission with infrared sources from catalogues
(IRAS, MSX, 2MASS), JHK data from the literature and new observations, has been
established according to spatial coincidence, infrared colours and spectral
energy distributions. Only 7 out of 29 resolved mm cores (and 16 out of the 26
unresolved ones) do not exhibit signposts of star formation activity. The other
ones are clearly associated with: far-IR sources, H_2 jets or near-IR objects
showing a high intrinsic colour excess. The distribution of the spectral
indices pertaining to the associated sources is peaked at values typical of
Class I objects, while three objects are signalled as candidates Class 0
sources. We remark the high detection rate (30%) of H_2 jets driven by sources
located inside the mm-cores. They appear not driven by the most luminous
objects in the field, but rather by less luminous objects in young clusters,
testifying the co-existence of both low- and intermediate-mass star formation.
The presented results reliably describe the young population of VMR-D. However,
the statistical evaluation of activity vs inactivity of the investigated cores,
even in good agreement with results found for other star forming regions, seems
to reflect the limiting sensitivity of the available facilities rather than any
property intrinsic to the mm-condensations.Comment: 38 pages. To be published to Astronomy & Astrophysic
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