138 research outputs found
The kinetic temperature of Barnard 68
We have observed the nearby isolated globule Barnard 68 (B68) in the
(J,K)=(1,1) and (2,2) inversion lines of ammonia. The gas kinetic temperature
derived from these is T=10+-1.2 K. The observed line-widths are almost thermal:
DV=0.181+-0.003 km/s (DVtherm=0.164+-0.010 km/s), supporting the earlier
hypothesis that B68 is in hydrostatic equilibrium. The kinetic temperature is
an input parameter to the physical cloud model put forward recently, and we
discuss the impact of the new value in this context.Comment: 4 pages, 2 figures, accepted for publication in A&A (Letters
Extending the limits of globule detection -- ISOPHOT Serendipity Survey Observations of interstellar clouds
A faint MJysr bipolar globule was discovered with the
ISOPHOT 170 m Serendipity Survey (ISOSS). ISOSS J 20246+6541 is a cold
( K) FIR source without an IRAS pointsource counterpart.
In the Digitized Sky Survey B band it is seen as a 3\arcmin size bipolar
nebulosity with an average excess surface brightness of
mag/\arcsec . The CO column density distribution determined by
multi-isotopic, multi-level CO measurements with the IRAM-30m telescope agrees
well with the optical appearance. An average hydrogen column density of
cm was derived from both the FIR and CO data. Using a
kinematic distance estimate of 400 pc the NLTE modelling of the CO, HCO,
and CS measurements gives a peak density of cm. The
multiwavelength data characterise ISOSS 20246+6541 as a representative of a
class of globules which has not been discovered so far due to their small
angular size and low 100m brightness. A significant overabundance of
CO is found . This is likely due to
isotope selective chemical processes.Comment: 5 pages, 3 figure
Solar System Objects in the ISOPHOT 170 micron Serendipity Survey
The ISOPHOT Serendipity Survey (ISOSS) covered approximately 15 % of the sky
at a wavelength of 170 micron while the ISO satellite was slewing from one
target to the next. By chance ISOSS slews went over many solar system objects
(SSOs). We identified the comets, asteroids and planets in the slews through a
fast and effective search procedure based on N-body ephemeris and flux
estimates. The detections were analysed from a calibration and scientific point
of view. Through the measurements of the well-known asteroids Ceres, Pallas,
Juno and Vesta and the planets Uranus and Neptune it was possible to improve
the photometric calibration of ISOSS and to extend it to higher flux regimes.
We were also able to establish calibration schemes for the important slew end
data. For the other asteroids we derived radiometric diameters and albedos
through a recent thermophysical model. The scientific results are discussed in
the context of our current knowledge of size, shape and albedos, derived from
IRAS observations, occultation measurements and lightcurve inversion
techniques. In all cases where IRAS observations were available we confirm the
derived diameters and albedos. For the five asteroids without IRAS detections
only one was clearly detected and the radiometric results agreed with sizes
given by occultation and HST observations. Four different comets have clearly
been detected at 170 micron and two have marginal detections. The observational
results are presented to be used by thermal comet models in the future. The
nine ISOSS slews over Hale-Bopp revealed extended and asymmetric structures
related to the dust tail. We attribute the enhanced emission in post-perihelion
observations to large particles around the nucleus. The signal patterns are
indicative of a concentration of the particles in trail direction.Comment: 15 pages, 6 figures, 6 tables; Accepted for publication in Astronomy
and Astrophysic
Dust emissivity in the Submm/Mm: SCUBA and SIMBA observations of Barnard 68
We have observed the dark cloud Barnard 68 with SCUBA at 850 um and with
SIMBA at 1.2 mm. The submillimetre and millimetre dust emission correlate well
with the extinction map of Alves, Lada and Lada (2001).The A_V/850um
correlation is clearly not linear and suggests lower temperatures for the dust
in the inner core of the cloud. Assuming a model for the temperature gradient,
we derive the cloud-averaged dust emissivities (normalised to the V-Band
extinction efficiency) at 850 um and 1.2 mm. We find k_850um/k_V = 4.0 +/- 1.0
x 10^-5 and k_1.2mm/k_V = 9.0 +/- 3.0 x 10^-6. These values are compared with
other determinations in this wavelength regime and with expectations for models
of diffuse dust and grain growth in dense clouds.Comment: 8 pages, 4 figures, A&A accepted (Letter), referee forma
The NH2D/NH3 ratio toward pre-protostellar cores around the UCHII region in IRAS 20293+3952
The deuterium fractionation, Dfrac, has been proposed as an evolutionary
indicator in pre-protostellar and protostellar cores of low-mass star-forming
regions. We investigate Dfrac, with high angular resolution, in the cluster
environment surrounding the UCHII region IRAS 20293+3952. We performed high
angular resolution observations with the IRAM Plateau de Bure Interferometer
(PdBI) of the ortho-NH2D 1_{11}-1_{01} line at 85.926 GHz and compared them
with previously reported VLA NH3 data. We detected strong NH2D emission toward
the pre-protostellar cores identified in NH3 and dust emission, all located in
the vicinity of the UCHII region IRAS 20293+3952. We found high values of
Dfrac~0.1-0.8 in all the pre-protostellar cores and low values, Dfrac<0.1,
associated with young stellar objects. The high values of Dfrac in
pre-protostellar cores could be indicative of evolution, although outflow
interactions and UV radiation could also play a role.Comment: 5 pages, 3 figures. Accepted for publication in Astronomy and
Astrophysics Letter
N2H+ depletion in the massive protostellar cluster AFGL 5142
We aim at investigating with high angular resolution the NH3/N2H+ ratio
toward the high-mass star-forming region AFGL 5142 in order to study whether
this ratio behaves similarly to the low-mass case, for which the ratio
decreases from starless cores to cores associated with YSOs. CARMA was used to
observe the 3.2 mm continuum and N2H+(1-0) emission. We used NH3(1,1) and
(2,2), HCO+(1-0) and H13CO+(1-0) data from the literature and we performed a
time-dependent chemical modeling of the region. The 3.2 mm continuum emission
reveals a dust condensation of ~23 Msun associated with the massive YSOs,
deeply embedded in the strongest NH3 core (hereafter central core). The N2H+
emission reveals two main cores, the western and eastern core, located to the
west and to the east of the mm condensation, and surrounded by a more extended
and complex structure of ~0.5 pc. Toward the central core the N2H+ emission
drops significantly, indicating a clear chemical differentiation in the region.
We found low values of the NH3/N2H+ ratio ~50-100 toward the western/eastern
cores, and high values up to 1000 in the central core. The chemical model
indicates that density, and in particular temperature, are key parameters in
determining the NH3/N2H+ ratio. The high density and temperature reached in the
central core allow molecules like CO to evaporate from grain mantles. The CO
desorption causes a significant destruction of N2H+, favoring the formation of
HCO+. This result is supported by our observations, which show that N2H+ and
HCO+ are anticorrelated in the central core. The observed values of the
NH3/N2H+ ratio in the central core can be reproduced by our model for times
t~4.5-5.3x10^5 yr (central) and t~10^4-3x10^6 yr (western/eastern). The
NH3/N2H+ ratio in AFGL 5142 does not follow the same trend as in regions of
low-mass star formation mainly due to the high temperature reached in hot
cores.Comment: Accepted for publication in A&A. 14 pages, 9 Figures, 5 Table
ISOPHOT far-infrared serendipity sky survey
The ISOPHOT Serendipity Survey utilizes the slew time between ISO's pointed observations with strip scanning measurements of the sky in the far-IR at 170 micrometers . The slews contain information about two fundamentally different types of objects, namely unresolved galactic and extragalactic far-IR sources as well as extended regions of galactic cirrus emission. Since the structure of the obtained data is almost unique, the development of dedicated software to extract astrophysically interesting parameters for the crossed sources is mandatory. Data analysis is currently in its early stages and concentrates on the detection of point sources. First results from an investigation of a high galactic latitude field near the North Galactic Pole indicate that the detection completeness with respect to previously known IRAS sources will be almost 100 percent for sources with f(subscript 100micrometers > 2 Jy, dropping below approximately equals 50 percent for f(subscript 100micrometers < 1.5 Jy. Nevertheless, even faint sources down to a level of f(subscript 170micrometers approximately equals 1 Jy can be detected. Since the majority of the detected point sources are galaxies, the Serendipity Survey will result in a large database of approximately equals 2000 galaxies
Searching for chameleon-like scalar fields with the ammonia method
(Abridged) The ammonia method, which has been proposed to explore the
electron-to-proton mass ratio, mu = m_e/m_p, is applied to nearby dark clouds
in the Milky Way. This ratio, which is measured in different physical
environments of high (terrestrial) and low (interstellar) densities of baryonic
matter is supposed to vary in chameleon-like scalar field models, which predict
strong dependence of both masses and coupling constant on the local matter
density. High resolution spectral observations of molecular cores in lines of
NH3 (J,K) = (1,1), HC3N J = 2-1, and N2H+ J = 1-0 were performed at three radio
telescopes to measure the radial velocity offsets, DeltaV = V_rot - V_inv,
between the inversion transition of NH3 (1,1) and the rotational transitions of
other molecules with different sensitivities to the parameter dmm = (mu_obs -
mu_lab)/mu_lab. The measured values of DeltaV exhibit a statistically
significant velocity offset of 23 +/- 4_stat +/- 3_sys m/s. When interpreted in
terms of the electron-to-proton mass ratio variation, this infers that dmm =
(2.2 +/- 0.4_stat +/- 0.3_sys)x10^{-8}. If only a conservative upper bound is
considered, then the maximum offset between ammonia and the other molecules is
|DeltaV| <= 30 m/s. This gives the most accurate reference point at z = 0 for
dmm: |dmm| <= 3x10^{-8}.Comment: 23 pages, 11 figures, 6 tables. Accepted for publication in A&A.
Title and text corrected, references update
Effect of floor type on the performance, physiological and behavioural responses of finishing beef steers
peer-reviewedBackground:The study objective was to investigate the effect of bare concrete slats (Control), two types of mats [(Easyfix mats (mat 1) and Irish Custom Extruder mats (mat 2)] fitted on top of concrete slats, and wood-chip to simulate deep bedding (wood-chip placed on top of a plastic membrane overlying the concrete slats) on performance, physiological and behavioral responses of finishing beef steers. One-hundred and forty-four finishing steers (503 kg; standard deviation 51.8 kg) were randomly assigned according to their breed (124 Continental cross and 20 Holstein–Friesian) and body weight to one of four treatments for 148 days. All steers were subjected to the same weighing, blood sampling (jugular venipuncture), dirt and hoof scoring pre study (day 0) and on days 23, 45, 65, 86, 107, 128 and 148 of the study. Cameras were fitted over each pen for 72 h recording over five periods and subsequent 10 min sampling scans were analysed.
Results: Live weight gain and carcass characteristics were similar among treatments. The number of lesions on the hooves of the animals was greater (P < 0.05) on mats 1 and 2 and wood-chip treatments compared with the animals on the slats. Dirt scores were similar for the mat and slat treatments while the wood-chip treatment had greater dirt scores. Animals housed on either slats or wood-chip had similar lying times. The percent of animals lying was greater for animals housed on mat 1 and mat 2 compared with those housed on concrete slats and wood chips. Physiological variables showed no significant difference among treatments.
Conclusions:
In this exploratory study, the performance or welfare of steers was not adversely affected by slats, differing mat types or wood-chip as underfoot material
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