28 research outputs found
Submillimeter local oscillators for spaceborne heterodyne applications
Existing and prospective submillimeter local oscillator technologies are surveyed and compared with respect to criteria of suitability for application in spaceborne submillimeter heterodyne receivers as those proposed for the Large Deployable Reflector (LDR). Solid-state and plasma devices are considered in terms of fundamental limitations
Very Extended X-ray and H-alpha Emission in M82: Implications for the Superwind Phenomenon
We discuss the properties and implications of a 3.7x0.9 kpc region of
spatially-coincident X-ray and H-alpha emission about 11.6 kpc to the north of
the galaxy M82 previously discussed by Devine and Bally (1999). The PSPC X-ray
spectrum is fit by thermal plasma (kT=0.80+-0.17 keV) absorbed by only the
Galactic foreground column density. We evaluate the relationship of the
X-ray/H-alpha ridge to the M82 superwind. The main properties of the X-ray
emission can all be explained as being due to shock-heating driven as the
superwind encounters a massive ionized cloud in the halo of M82. This encounter
drives a slow shock into the cloud, which contributes to the excitation of the
observed H-alpha emission. At the same time, a fast bow-shock develops in the
superwind just upstream of the cloud, and this produces the observed X-ray
emission. This interpretation would imply that the superwind has an outflow
speed of roughly 800 km/s, consistent with indirect estimates based on its
general X-ray properties and the kinematics of the inner kpc-scale region of
H-alpha filaments. The gas in the M82 ridge is roughly two orders-of-magnitude
hotter than the minimum "escape temperature" at this radius, so this gas will
not be retained by M82.
(abridged)Comment: 24 pages (latex), 3 figures (2 gif files and one postscript),
accepted for publication in Part 1 of The Astrophysical Journa
ISO LWS Spectroscopy of M82: A Unified Evolutionary Model
We present the first complete far-infrared spectrum (43 to 197 um) of M82,
the brightest infrared galaxy in the sky, taken with the Long Wavelength
Spectrometer of the Infrared Space Observatory (ISO). We detected seven fine
structure emission lines, [OI] 63 and 145 um, [OIII] 52 and 88 um, [NII] 122
um, [NIII] 57 um and [CII] 158 um, and fit their ratios to a combination
starburst and photo-dissociation region (PDR) model. The best fit is obtained
with HII regions with n = 250 cm^{-3} and an ionization parameter of 10^{-3.5}
and PDRs with n = 10^{3.3} cm^{-3} and a far-ultraviolet flux of G_o =
10^{2.8}. We applied both continuous and instantaneous starburst models, with
our best fit being a 3-5 Myr old instantaneous burst model with a 100 M_o
cut-off. We also detected the ground state rotational line of OH in absorption
at 119.4 um. No excited level OH transitions are apparent, indicating that the
OH is almost entirely in its ground state with a column density ~ 4x10^{14}
cm^{-2}. The spectral energy distribution over the LWS wavelength range is well
fit with a 48 K dust temperature and an optical depth, tau_{Dust} proportional
to lambda^{-1}.Comment: 23 pages, 4 figures, accepted by ApJ, Feb. 1, 199
Carbon monoxide in the solar atmosphere I. Numerical method and two-dimensional models
The radiation hydrodynamic code CO5BOLD has been supplemented with the
time-dependent treatment of chemical reaction networks. Advection of particle
densities due to the hydrodynamic flow field is also included. The radiative
transfer is treated frequency-independently, i.e. grey, so far. The upgraded
code has been applied to two-dimensional simulations of carbon monoxide (CO) in
the non-magnetic solar photosphere and low chromosphere. For this purpose a
reaction network has been constructed, taking into account the reactions which
are most important for the formation and dissociation of CO under the physical
conditions of the solar atmosphere. The network has been strongly reduced to 27
reactions, involving the chemical species H, H2, C, O, CO, CH, OH, and a
representative metal. The resulting CO number density is highest in the cool
regions of the reversed granulation pattern at mid-photospheric heights and
decreases strongly above. There, the CO abundance stays close to a value of 8.3
on the usual logarithmic abundance scale with [H]=12 but is reduced in hot
shock waves which are a ubiquitous phenomenon of the model atmosphere. For
comparison, the corresponding equilibrium densities have been calculated, based
on the reaction network but also under assumption of instantaneous chemical
equilibrium by applying the Rybicki & Hummer (RH) code by Uitenbroek (2001).
Owing to the short chemical timescales, the assumption holds for a large
fraction of the atmosphere, in particular the photosphere. In contrast, the CO
number density deviates strongly from the corresponding equilibrium value in
the vicinity of chromospheric shock waves. Simulations with altered reaction
network clearly show that the formation channel via hydroxide (OH) is the most
important one under the conditions of the solar atmosphere.Comment: 15 pages, 6 figures, final version will contain online materia
First observations with CONDOR, a 1.5 THz heterodyne receiver
The THz atmospheric windows centered at roughly 1.3 and 1.5~THz, contain
numerous spectral lines of astronomical importance, including three high-J CO
lines, the N+ line at 205 microns, and the ground transition of para-H2D+. The
CO lines are tracers of hot (several 100K), dense gas; N+ is a cooling line of
diffuse, ionized gas; the H2D+ line is a non-depleting tracer of cold (~20K),
dense gas. As the THz lines benefit the study of diverse phenomena (from
high-mass star-forming regions to the WIM to cold prestellar cores), we have
built the CO N+ Deuterium Observations Receiver (CONDOR) to further explore the
THz windows by ground-based observations. CONDOR was designed to be used at the
Atacama Pathfinder EXperiment (APEX) and Stratospheric Observatory For Infrared
Astronomy (SOFIA). CONDOR was installed at the APEX telescope and test
observations were made to characterize the instrument. The combination of
CONDOR on APEX successfully detected THz radiation from astronomical sources.
CONDOR operated with typical Trec=1600K and spectral Allan variance times of
30s. CONDOR's first light observations of CO 13-12 emission from the hot core
Orion FIR4 (= OMC1 South) revealed a narrow line with T(MB) = 210K and
delta(V)=5.4km/s. A search for N+ emission from the ionization front of the
Orion Bar resulted in a non-detection. The successful deployment of CONDOR at
APEX demonstrates the potential for making observations at THz frequencies from
ground-based facilities.Comment: 4 pages + list of objects, 3 figures, to be published in A&A special
APEX issu
Carbon Recombination Lines from the Galactic Plane at 34.5 & 328 MHz
We present results of a search for carbon recombination lines in the Galaxy
at 34.5 MHz (C) made using the dipole array at Gauribidanur near
Bangalore. Observations made towards 32 directions, led to detections of lines
in absorption at nine positions. Followup observations at 328 MHz
(C) using the Ooty Radio Telescope detected these lines in emission.
A VLA D-array observation of one of the positions at 330 MHz yielded no
detection implying a lower limit of 10' for the angular size of the line
forming region.
The longitude-velocity distribution of the observed carbon lines indicate
that the line forming region are located mainly between 4 kpc and 7 kpc from
the Galactic centre. Combining our results with published carbon recombination
line data near 76 MHz (\nocite{erickson:95} Erickson \et 1995) we obtain
constraints on the physical parameters of the line forming regions. We find
that if the angular size of the line forming regions is , then
the range of parameters that fit the data are: \Te K, \ne \cm3 and pathlengths pc which may correspond to thin
photo-dissociated regions around molecular clouds. On the other hand, if the
line forming regions are in extent, then warmer gas (\Te K) with lower electron densities (\ne \cm3) extending
over several tens of parsecs along the line of sight and possibly associated
with atomic \HI gas can fit the data. Based on the range of derived parameters,
we suggest that the carbon line regions are most likely associated with
photo-dissociation regions.Comment: To appear in Journal of Astrophysics & Astronomy, March 200
Nonthermal Emission from Star-Forming Galaxies
The detections of high-energy gamma-ray emission from the nearby starburst
galaxies M82 & NGC253, and other local group galaxies, broaden our knowledge of
star-driven nonthermal processes and phenomena in non-AGN star-forming
galaxies. We review basic aspects of the related processes and their modeling
in starburst galaxies. Since these processes involve both energetic electrons
and protons accelerated by SN shocks, their respective radiative yields can be
used to explore the SN-particle-radiation connection. Specifically, the
relation between SN activity, energetic particles, and their radiative yields,
is assessed through respective measures of the particle energy density in
several star-forming galaxies. The deduced energy densities range from O(0.1)
eV/cm^3 in very quiet environments to O(100) eV/cm^3 in regions with very high
star-formation rates.Comment: 17 pages, 5 figures, to be published in Astrophysics and Space
Science Proceeding
Photon dominated regions in the spiral arms of M83 and M51
We present CI 3P1-3P0 spectra at four spiral arm positions and the nuclei of
the nearby galaxies M83 and M51 obtained at the JCMT. This data is complemented
with maps of CO 1-0, 2-1, and 3-2, and ISO/LWS far-infrared data of CII (158
micron), OI (63 micron), and NII (122 micron) allowing for the investigation of
a complete set of all major gas cooling lines. From the intensity of the NII
line, we estimate that between 15% and 30% of the observed CII emission
originate from the dense ionized phase of the ISM. The analysis indicates that
emission from the diffuse ionized medium is negligible. In combination with the
FIR dust continuum, we find gas heating efficiencies below ~0.21% in the
nuclei, and between 0.25 and 0.36% at the outer positions. Comparison with
models of photon-dominated regions (PDRs) of Kaufman et al. (1999) with the
standard ratios OI(63)/CII_PDR and (OI(63)+CII_PDR) vs. TIR, the total infrared
intensity, yields two solutions. The physically most plausible solution
exhibits slightly lower densities and higher FUV fields than found when using a
full set of line ratios, CII_PDR/CI(1-0), CI(1-0)/CO(3-2), CO(3-2)/CO(1-0),
CII/CO(3-2), and, OI(63)/CII_PDR. The best fits to the latter ratios yield
densities of 10^4 cm^-3 and FUV fields of ~G_0=20-30 times the average
interstellar field without much variation. At the outer positions, the observed
total infrared intensities are in perfect agreement with the derived best
fitting FUV intensities. The ratio of the two intensities lies at 4-5 at the
nuclei, indicating the presence of other mechanisms heating the dust
A spatially resolved study of photoelectric heating and [CII] cooling in the LMC
(abridged) We study photoelectric heating throughout the Large Magellanic
Cloud. We quantify the importance of the [CII] cooling line and the
photoelectric heating process of various environments in the LMC and
investigate which parameters control the extent of photoelectric heating. We
use the BICE [CII] map and the Spitzer/SAGE infrared maps. We examine the
spatial variations in the efficiency of photoelectric heating: photoelectric
heating rate over power absorbed by grains. We correlate the photoelectric
heating efficiency and the emission from various dust constituents and study
the variations as a function of H\alpha emission, dust temperatures, and the
total infrared luminosity. From this we estimate radiation field, gas
temperature, and electron density. We find systematic variations in
photoelectric efficiency. The highest efficiencies are found in the diffuse
medium, while the lowest coincide with bright star-forming regions (~1.4 times
lower). The [CII] line emission constitutes 1.32% of the far infrared
luminosity across the whole of the LMC. We find correlations between the [CII]
emission and ratios of the mid infrared and far infrared bands, which comprise
various dust constituents. The correlations are interpreted in light of the
spatial variations of the dust abundance and by the local environmental
conditions that affect the dust emission properties. As a function of the total
infrared surface brightness, S_{TIR}, the [CII] surface brightness can be
described as: S_{[CII]}=1.25 S_{TIR}^{0.69} [10^{-3} erg s^{-1} cm^{-2}
sr^{-1}]. The [CII] emission is well-correlation with the 8 micrometer
emission, suggesting that the polycyclic aromatic hydrocarbons play a dominant
role in the photoelectric heating process.Comment: Accepted for publication in A&A, 16 pages, 17 figure
Extensive optical and near-infrared observations of the nearby, narrow-lined type Ic SN 2007gr: days 5 to 415
We present photometric and spectroscopic observations at optical and
near-infrared wavelengths of the nearby type Ic SN 2007gr. These represent the
most extensive data-set to date of any supernova of this sub-type, with
frequent coverage from shortly after discovery to more than one year
post-explosion. We deduce a rise time to B-band maximum of 11.5 \pm 2.7 days.
We find a peak B-band magnitude of M_B=-16.8, and light curves which are
remarkably similar to the so-called 'hypernova' SN 2002ap. In contrast, the
spectra of SNe 2007gr and 2002ap show marked differences, not least in their
respective expansion velocities. We attribute these differences primarily to
the density profiles of their progenitor stars at the time of explosion i.e. a
more compact star for SN 2007gr compared to SN 2002ap. From the
quasi-bolometric light curve of SN 2007gr, we estimate that 0.076 0.010
Msun of 56Ni was produced in the explosion. Our near-infrared (IR) spectra
clearly show the onset and disappearance of the first overtone of carbon
monoxide (CO) between ~70 to 175 days relative to B-band maximum. The detection
of the CO molecule implies that ionised He was not microscopically mixed within
the carbon/oxygen layers. From the optical spectra, near-IR light curves, and
colour evolution, we find no evidence for dust condensation in the ejecta out
to about 400 days. Given the combination of unprecedented temporal coverage,
and high signal-to-noise data, we suggest that SN 2007gr could be used as a
template object for supernovae of this sub-class.Comment: A&A accepted; 26 pages & 16 figure