1,586 research outputs found
Planck Observations of M33
We have performed a comprehensive investigation of the global integrated flux
density of M33 from radio to ultraviolet wavelengths, finding that the data
between 100 GHz and 3 THz are accurately described by a single modified
blackbody curve with a dust temperature of = 21.670.30 K
and an effective dust emissivity index of = 1.350.10,
with no indication of an excess of emission at millimeter/sub-millimeter
wavelengths. However, sub-dividing M33 into three radial annuli, we found that
the global emission curve is highly degenerate with the constituent curves
representing the sub-regions of M33. We also found gradients in
and across the disk of M33, with both
quantities decreasing with increasing radius. Comparing the M33 dust emissivity
with that of other Local Group members, we find that M33 resembles the
Magellanic Clouds rather than the larger galaxies, i.e., the Milky Way and M31.
In the Local Group sample, we find a clear correlation between global dust
emissivity and metallicity, with dust emissivity increasing with metallicity. A
major aspect of this analysis is the investigation into the impact of
fluctuations in the Cosmic Microwave Background (CMB) on the integrated flux
density spectrum of M33. We found that failing to account for these CMB
fluctuations would result in a significant over-estimate of
by 5 K and an under-estimate of by 0.4.Comment: Accepted for publication in MNRA
Atomic Carbon in Galaxies
We present new measurements of the ground state fine-structure line of atomic
carbon at 492 GHz in a variety of nearby external galaxies, ranging from spiral
to irregular, interacting and merging types. In comparison with CO(1-0), the
CI(1-0) intensity stays fairly comparable in the different environments, with
an average value of the ratio of the line integrated areas in Kkm/s of
CI(1-0)/CO(1-0) = 0.2 +/- 0.2. However, some variations can be found within
galaxies, or between galaxies. Relative to CO lines, CI(1-0) is weaker in
galactic nuclei, but stronger in disks, particularly outside star forming
regions. Also, in NGC 891, the CI(1-0) emission follows the dust continuum at
1.3mm extremely well along the full length of the major axis where molecular
gas is more abundant than atomic gas. Atomic carbon therefore appears to be a
good tracer of molecular gas in external galaxies, possibly more reliable than
CO. Atomic carbon can contribute significantly to the thermal budget of
interstellar gas. Cooling due to C and CO amounts typically to 2 x 10^{-5} of
the FIR continuum or 5% of the CII line. However, C and CO cooling reaches 30%
of the gas total, in Ultra Luminous InfraRed Galaxies, where CII is abnormally
faint. Together with CII/FIR, the emissivity ratio CI(1-0)/FIR can be used as a
measure of the non-ionizing UV radiation field in galaxies.Comment: 26 pages, 8 figure
Power Asymmetries in the Cosmic Microwave Background Temperature and Polarization patterns
We test the asymmetry of the Cosmic Microwave Background anisotropy jointly
in temperature and polarization. We study the hemispherical asymmetry,
previously found only in the temperature field, with respect to the axis
identified by Hansen et al. (2009). To this extent, we make use of the low
resolution WMAP 5 year temperature and polarization Nside=16 maps and the
optimal angular power spectrum estimator BolPol (Gruppuso et al. 2009). We
consider two simple estimators for the power asymmetry and we compare our
findings with Monte Carlo simulations which take into account the full noise
covariance matrix. We confirm an excess of power in temperature angular power
spectrum in the Southern hemisphere at a significant level, between 3 sigma and
4 sigma depending on the exact range of multipoles considered. We do not find
significant power asymmetry in the gradient (curl) component EE (BB) of
polarized angular spectra. Also cross-correlation power spectra, i.e. TE, TB,
EB, show no significant hemispherical asymmetry. We also show that the Cold
Spot found by Vielva et al. (2004) in the Southern Galactic hemisphere does not
alter the significance of the hemispherical asymmetries on multipoles which can
be probed by maps at resolution Nside=16. Although the origin of the
hemispherical asymmetry in temperature remains unclear, the study of the
polarization patter could add useful information on its explanation. We
therefore forecast by Monte Carlo the Planck capabilities in probing
polarization asymmetries.Comment: 6 pages, 7 figure
Planck-LFI: Design and Performance of the 4 Kelvin Reference Load Unit
The LFI radiometers use a pseudo-correlation design where the signal from the
sky is continuously compared with a stable reference signal, provided by a
cryogenic reference load system. The reference unit is composed by small
pyramidal horns, one for each radiometer, 22 in total, facing small absorbing
targets, made of a commercial resin ECCOSORB CR (TM), cooled to approximately
4.5 K. Horns and targets are separated by a small gap to allow thermal
decoupling. Target and horn design is optimized for each of the LFI bands,
centered at 70, 44 and 30 GHz. Pyramidal horns are either machined inside the
radiometer 20K module or connected via external electro-formed bended
waveguides. The requirement of high stability of the reference signal imposed a
careful design for the radiometric and thermal properties of the loads.
Materials used for the manufacturing have been characterized for thermal, RF
and mechanical properties. We describe in this paper the design and the
performance of the reference system.Comment: This is an author-created, un-copyedited version of an article
accepted for publication in JINST. IOP Publishing Ltd is not responsible for
any errors or omissions in this version of the manuscript or any version
derived from it. The definitive publisher authenticated version is available
online at [10.1088/1748-0221/4/12/T12006]. 14 pages, 34 figure
On the Conformal forms of the Robertson-Walker metric
All possible transformations from the Robertson-Walker metric to those
conformal to the Lorentz-Minkowski form are derived. It is demonstrated that
the commonly known family of transformations and associated conformal factors
are not exhaustive and that there exists another relatively less well known
family of transformations with a different conformal factor in the particular
case that K = -1. Simplified conformal factors are derived for the special case
of maximally-symmetric spacetimes. The full set of all possible
cosmologically-compatible conformal forms is presented as a comprehensive
table. A product of the analysis is the determination of the set-theoretical
relationships between the maximally symmetric spacetimes, the Robertson-Walker
spacetimes, and functionally more general spacetimes. The analysis is preceded
by a short historical review of the application of conformal metrics to
Cosmology.Comment: Historical review added. Accepted by J. Math. Phy
Atomic Carbon Emission from Individual Molecular Clouds in M33
We present observations of the 492 GHz [CI] emission for four individual
giant molecular clouds in the Local Group galaxy M33 obtained with the James
Clerk Maxwell Telescope. The average [CI] to CO J=1-0 integrated intensity
ratio of 0.10+/-0.03 is similar to what is observed in Galactic molecular
clouds but smaller than what is seen in starburst galaxies. Similarly, the
column density ratio N(C)/N(CO) is similar to that observed in the Orion Bar,
but smaller than values obtained for starburst galaxies. The [CI] line is found
to be a more important coolant than the lowest three rotational transitions of
CO for all the clouds in the sample. The [CI] luminosity does not appear to be
enhanced significantly in two low-metallicity clouds, which may be due to the
unusual ionization environment of the clouds.Comment: 12 pages, aastex, 1 postscript figure; accepted for publication in
ApJ Letters; also available at
http://www.physics.mcmaster.ca/Wilson_Preprints
Functional morphology of the forelimb of Early Miocene caviomorph rodents from Patagonia
Caviomorph rodents (New World Hystricognathi) are represented in the Santa Cruz Formation of Patagonia (Early Miocene, Santacrucian) by four superfamilies. From this unit, excellent cranial and associated postcranial remains of Neoreomys, Eocardia, Schistomys (Cavioidea), Perimys (Chinchilloidea) and Steiromys (Erethizontoidea) are known. To interpret their use of substrate, a comparative description of limb bones (scapula, humerus, radius and ulna) of the five genera was performed within a taxonomic and ecologically diverse sample of extant rodents. Using palaeobiological inferences based on the habits and functional morphology of members of the extant sample, hypotheses were generated for the use of substrate by the Santacrucian taxa. Neoreomys would have had a marked flexo-extension capacity of the humerus and a moderate flexion of the manus. This genus and Eocardia would have had a complete and stabilized forearm extension, with wide stride and moderate extension of the forearm for the latter. Schistomys presents features similar to Eocardia. Perimys would have had strong external rotation of the humerus, moderate flexion of the manus and moderate, complete and stabilized extension of the forearm. Steiromys would have had good pronation/supination capacity, strong internal rotation of the humerus and flexion of the forearm and manus. Neoreomys would have been ambulatory and an occasional runner. Eocardia and Schistomys would have been good runners. Perimys would have been a digger and Steiromys a climber. This morphological disparity reflects a high ecological diversity, compatible with differential use of space during the Santacrucian.Fil: Muñoz, Nahuel Antu. Universidad Nacional de La Plata. Facultad de Ciencias Naturales y Museo. División PaleontologÃa Vertebrados; Argentina. Consejo Nacional de Investigaciones CientÃficas y Técnicas. Centro CientÃfico Tecnológico Conicet - La Plata; ArgentinaFil: Toledo, Néstor. Universidad Nacional de La Plata. Facultad de Ciencias Naturales y Museo. División PaleontologÃa Vertebrados; Argentina. Consejo Nacional de Investigaciones CientÃficas y Técnicas. Centro CientÃfico Tecnológico Conicet - La Plata; ArgentinaFil: Candela, Adriana Magdalena. Universidad Nacional de La Plata. Facultad de Ciencias Naturales y Museo. División PaleontologÃa Vertebrados; Argentina. Consejo Nacional de Investigaciones CientÃficas y Técnicas. Centro CientÃfico Tecnológico Conicet - La Plata; ArgentinaFil: VizcaÃno, Sergio Fabián. Universidad Nacional de La Plata. Facultad de Ciencias Naturales y Museo. División PaleontologÃa Vertebrados; Argentina. Consejo Nacional de Investigaciones CientÃficas y Técnicas. Centro CientÃfico Tecnológico Conicet - La Plata; Argentin
Advanced modelling of the Planck-LFI radiometers
The Low Frequency Instrument (LFI) is a radiometer array covering the 30-70
GHz spectral range on-board the ESA Planck satellite, launched on May 14th,
2009 to observe the cosmic microwave background (CMB) with unprecedented
precision. In this paper we describe the development and validation of a
software model of the LFI pseudo-correlation receivers which enables to
reproduce and predict all the main system parameters of interest as measured at
each of the 44 LFI detectors. These include system total gain, noise
temperature, band-pass response, non-linear response. The LFI Advanced RF Model
(LARFM) has been constructed by using commercial software tools and data of
each radiometer component as measured at single unit level. The LARFM has been
successfully used to reproduce the LFI behavior observed during the LFI
ground-test campaign. The model is an essential element in the database of LFI
data processing center and will be available for any detailed study of
radiometer behaviour during the survey.Comment: 21 pages, 15 figures, this paper is part of the Prelaunch status LFI
papers published on JINST:
http://www.iop.org/EJ/journal/-page=extra.proc5/jins
Planck-LFI radiometers' spectral response
The Low Frequency Instrument (LFI) is an array of pseudo-correlation
radiometers on board the Planck satellite, the ESA mission dedicated to
precision measurements of the Cosmic Microwave Background. The LFI covers three
bands centred at 30, 44 and 70 GHz, with a goal bandwidth of 20% of the central
frequency.
The characterization of the broadband frequency response of each radiometer
is necessary to understand and correct for systematic effects, particularly
those related to foreground residuals and polarization measurements. In this
paper we present the measured band shape of all the LFI channels and discuss
the methods adopted for their estimation. The spectral characterization of each
radiometer was obtained by combining the measured spectral response of
individual units through a dedicated RF model of the LFI receiver scheme.
As a consistency check, we also attempted end-to-end spectral measurements of
the integrated radiometer chain in a cryogenic chamber. However, due to
systematic effects in the measurement setup, only qualitative results were
obtained from these tests. The measured LFI bandpasses exhibit a moderate level
of ripple, compatible with the instrument scientific requirements.Comment: 16 pages, 9 figures, this paper is part of the Prelaunch status LFI
papers published on JINST:
http://www.iop.org/EJ/journal/-page=extra.proc5/jins
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