392 research outputs found
Pictor A (PKS 0518-45) - From Nucleus to Lobes
We present radio and optical imaging and kinematic data for the radio galaxy
Pictor A, including HST continuum and [OIII], emission-line images (at a
resolution of 25 - 100 mas) and ground-based imaging and spectroscopy (at a
resolution of ~ 1.5". The radio data include 3 cm Australia Telescope images of
the core, at a resolution comparable to that of the optical, ground-based
images, and a VLBI image of a jet in the compact core (at a resolution of 2 -
25 mas), which seems to align with a continuum ``jet'' found in the HST images.
The core radio jet, the HST optical continuum ``jet'', and the NW H-alpha
filaments all appear to point toward the optical-synchrotron hot-spot in the NW
lobe of this object and are associated with a disrupted velocity field in the
extended ionized gas. The ground-based spectra which cover this trajectory also
yield line ratios for the ionized gas which have anomalously low [NII] (6564),
suggesting either a complex, clumpy structure in the gas with a higher
cloud-covering factor at larger radii and with denser clouds than is found in
the nuclear regions of most NLRG and Seyfert 2 galaxies, or some other,
unmodeled, mechanism for the emergent spectrum from this region. The H-alpha
emission-line filaments to the N appear to be associated with a 3 cm radio
continuum knot which lies in a gap in the filaments ~ 4" from the nucleus.
Altogether, the data in this paper provide good circumstantial evidence for
non-disruptive redirection of a radio jet by interstellar gas clouds in the
host galaxy.Comment: 19 pages, 6 ps.gz fig pages, to appear in the Ap.J. Supp
PSRCHIVE and PSRFITS: Definition of the Stokes Parameters and Instrumental Basis Conventions
This paper defines the mathematical convention adopted to describe an
electromagnetic wave and its polarisation state, as implemented in the PSRCHIVE
software and represented in the PSRFITS definition. Contrast is made between
the convention that has been widely accepted by pulsar astronomers and the
IAU/IEEE definitions of the Stokes parameters. The former is adopted as the
PSR/IEEE convention, and a set of useful parameters are presented for
describing the differences between the PSR/IEEE standard and the conventions
(either implicit or explicit) that form part of the design of observatory
instrumentation. To aid in the empirical determination of instrumental
convention parameters, well-calibrated average polarisation profiles of PSR
J0304+1932 and PSR J0742-2822 are presented at radio wavelengths of
approximately 10, 20, and 40 cm.Comment: 7 pages, 2 figures, to be published in PAS
MERLIN/VLA imaging of the gravitational lens system B0218+357
Gravitational lenses offer the possibility of accurately determining the
Hubble parameter (H_0) over cosmological distances, and B0218+357 is one of the
most promising systems for an application of this technique. In particular this
system has an accurately measured time delay (10.5+/-0.4 d; Biggs et al. 1999)
and preliminary mass modelling has given a value for H_0 of 69 +13/-19
km/s/Mpc. The error on this estimate is now dominated by the uncertainty in the
mass modelling. As this system contains an Einstein ring it should be possible
to constrain the model better by imaging the ring at high resolution. To
achieve this we have combined data from MERLIN and the VLA at a frequency of 5
GHz. In particular MERLIN has been used in multi-frequency mode in order to
improve substantially the aperture coverage of the combined data set. The
resulting map is the best that has been made of the ring and contains many new
and interesting features. Efforts are currently underway to exploit the new
data for lensing constraints using the LensClean algorithm (Kochanek & Narayan
1992).Comment: Accepted for publication in MNRAS. 6 pages, 4 included PostScript
figure
Testing the Mutually Enhanced Magicity Effect in Nuclear Incompressibility via the Giant Monopole Resonance in the Pb Isotopes
Using inelastic -scattering at extremely forward angles, including
, the strength distributions of the isoscalar giant monopole resonance
(ISGMR) have been measured in the Pb isotopes in order to
examine the proposed mutually enhanced magicity (MEM) effect on the nuclear
incompressibility. The MEM effect had been suggested as a likely explanation of
the "softness" of nuclear incompressibility observed in the ISGMR measurements
in the Sn and Cd isotopes. Our experimental results rule out any manifestation
of the MEM effect in nuclear incompressibility and leave the question of the
softness of the open-shell nuclei unresolved still.Comment: Accepted for publication in Physics Letters B. Very minor changes in
tex
Multi-Transition Study of M51's Molecular Gas Spiral Arms
Two selected regions in the molecular gas spiral arms in M51 were mapped with
the Owens Valley Radio Observatory (OVRO) mm-interferometer in the 12CO(2-1),
13CO(1-0), C18O(1-0), HCN(1-0) and HCO+(1-0) emission lines. The CO data have
been combined with the 12CO(1-0) data from Aalto et al. (1999) covering the
central 3.5kpc to study the physical properties of the molecular gas. All CO
data cubes were short spacing corrected using IRAM 30m (12CO(1-0): NRO 45m)
single dish data. A large velocity gradient (LVG) analysis finds that the giant
molecular clouds (GMCs) are similar to Galactic GMCs when studied at 180pc
(120pc) resolution with an average kinetic temperature of T_kin = 20(16)K and
H_2 density of n(H_2) = 120(240)cm^(-3) when assuming virialized clouds (a
constant velocity gradient dv/dr. The associated conversion factor between H_2
mass and CO luminosity is close to the Galactic value for most regions
analyzed. Our findings suggest that the GMC population in the spiral arms of
M51 is similar to those of the Milky Way and therefore the strong star
formation occurring in the spiral arms has no strong impact on the molecular
gas in the spiral arms. Extinction inferred from the derived H_2 column density
is very high (A_V about 15 - 30 mag), about a factor of 5-10 higher than the
average value derived toward HII regions. Thus a significant fraction of the
ongoing star formation could be hidden inside the dust lanes of the spiral
arms. A comparison of MIPS 24um and H_alpha data, however, suggests that this
is not the case and most of the GMCs studied here are not (yet) forming stars.
We also present low (4.5") resolution OVRO maps of the HCN(1-0) and HCO+(1-0)
emission at the location of the brightest 12CO(1-0) peak.Comment: 41 pages, 12 figures, 7 tables; accepted for publication by Ap
A Multi-Wavelength High Resolution Study of the S255 Star Forming Region. General structure and kinematics
We present observational data for two main components (S255IR and S255N) of
the S255 high mass star forming region in continuum and molecular lines
obtained at 1.3 mm and 1.1 mm with the SMA, at 1.3 cm with the VLA and at 23
and 50 cm with the GMRT. The angular resolution was from ~ 2" to ~ 5" for all
instruments. With the SMA we detected a total of about 50 spectral lines of 20
different molecules (including isotopologues). About half of the lines and half
of the species (in particular N2H+, SiO, C34S, DCN, DNC, DCO+, HC3N, H2CO,
H2CS, SO2) have not been previously reported in S255IR and partly in S255N at
high angular resolution. Our data reveal several new clumps in the S255IR and
S255N areas by their millimeter wave continuum emission. Masses of these clumps
are estimated at a few solar masses. The line widths greatly exceed expected
thermal widths. These clumps have practically no association with NIR or radio
continuum sources, implying a very early stage of evolution. At the same time,
our SiO data indicate the presence of high-velocity outflows related to some of
these clumps. In some cases, strong molecular emission at velocities of the
quiescent gas has no detectable counterpart in the continuum. We discuss the
main features of the distribution of NH3, N2H+, and deuterated molecules. We
estimate properties of decimeter wave radio continuum sources and their
relationship with the molecular material.Comment: 21 pages, 26 figures, accepted for publication in Astrophysical
Journa
A Luminous Be+White Dwarf Supersoft Source in the Wing of the SMC: MAXI J0158-744
We present a multi-wavelength analysis of the very fast X-ray transient MAXI
J0158-744, which was detected by MAXI/GSC on 2011 November 11. The subsequent
exponential decline of the X-ray flux was followed with Swift observations, all
of which revealed spectra with low temperatures (~100eV) indicating that MAXI
J0158-744 is a new Supersoft Source (SSS). The Swift X-ray spectra near maximum
show features around 0.8 keV that we interpret as possible absorption from
OVIII, and emission from O, Fe, and Ne lines. We obtained SAAO and ESO optical
spectra of the counterpart early in the outburst and several weeks later. The
early spectrum is dominated by strong Balmer and HeI emission, together with
weaker HeII emission. The later spectrum reveals absorption features that
indicate a B1/2IIIe spectral type, and all spectral features are at velocities
consistent with the Small Magellanic Cloud. At this distance, it is a luminous
SSS (>10^37 erg/s) but whose brief peak luminosity of >10^39 erg/s in the 2-4
keV band makes it the brightest SSS yet seen at "hard" X-rays. We propose that
MAXI J0158-744 is a Be-WD binary, and the first example to possibly enter ULX
territory. The brief hard X-ray flash could possibly be a result of the
interaction of the ejected nova shell with the B star wind in which the white
dwarf (WD) is embedded. This makes MAXI J0158-744 only the third Be/WD system
in the Magellanic Clouds, but it is by far the most luminous. The properties of
MAXI J0158-744 give weight to previous suggestions that SSS in nearby galaxies
are associated with early-type stellar systems.Comment: 15 pages, 8 figures; ApJ accepte
Variability monitoring of the hydroxyl maser emission in G12.889+0.489
Through a series of observations with the Australia Telescope Compact Array
we have monitored the variability of ground-state hydroxyl maser emission from
G12.889+0.489 in all four Stokes polarisation products. These observations were
motivated by the known periodicity in the associated 6.7-GHz methanol maser
emission. A total of 27 epochs of observations were made over 16 months. No
emission was seen from either the 1612 or 1720 MHz satellite line transitions
(to a typical five sigma upper limit of 0.2 Jy). The peak flux densities of the
1665 and 1667 MHz emission were observed to vary at a level of ~20% (with the
exception of one epoch which dropped by <40%). There was no distinct flaring
activity at any epoch, but there was a weak indication of periodic variability,
with a period and phase of minimum emission similar to that of methanol. There
is no significant variation in the polarised properties of the hydroxyl, with
Stokes Q and U flux densities varying in accord with the Stokes I intensity
(linear polarisation, P, varying by <20%) and the right and left circularly
polarised components varying by <33% at 1665-MHz and <38% at 1667-MHz. These
observations are the first monitoring observations of the hydroxyl maser
emission from G12.889+0.489.Comment: 7 pages, 6 figures, accepted for publication in MNRA
A Survey of Extragalactic Faraday Rotation at High Galactic Latitude: The Vertical Magnetic Field of the Milky Way towards the Galactic Poles
We present a study of the vertical magnetic field of the Milky Way towards
the Galactic poles, determined from observations of Faraday rotation toward
more than 1000 polarized extragalactic radio sources at Galactic latitudes |b|
> 77 degs, using the Westerbork Radio Synthesis Telescope and the Australia
Telescope Compact Array. We find median rotation measures (RMs) of 0.0 +/- 0.5
rad/m^2 and +6.3 +/- 0.7 rad/m^2 toward the north and south Galactic poles,
respectively, demonstrating that there is no coherent vertical magnetic field
in the Milky Way at the Sun's position. If this is a global property of the
Milky Way's magnetism, then the lack of symmetry across the disk rules out pure
dipole or quadrupole geometries for the Galactic magnetic field. The angular
fluctuations in RM seen in our data show no preferred scale within the range ~
0.1 to 25 degs. The observed standard deviation in RM of ~ 9 rad/m^2 then
implies an upper limit of ~1microGauss on the strength of the random magnetic
field in the warm ionized medium at high Galactic latitudes.Comment: 38 pages, 7 figures, 3 tables Accepted for publication in ApJ,
Electronic versions of Tables 1 and 2 are available via email from the first
autho
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