8,330 research outputs found
A Herschel [C II] Galactic plane survey II: CO-dark H2 in clouds
ABRIDGED: Context: HI and CO large scale surveys of the Milky Way trace the
diffuse atomic clouds and the dense shielded regions of molecular hydrogen
clouds. However, until recently, we have not had spectrally resolved C+ surveys
to characterize the photon dominated interstellar medium, including, the H2 gas
without C, the CO-dark H2, in a large sample of clouds. Aims: To use a sparse
Galactic plane survey of the 1.9 THz [C II] spectral line from the Herschel
Open Time Key Programme, Galactic Observations of Terahertz C+ (GOT C+), to
characterize the H2 gas without CO in a statistically significant sample of
clouds. Methods: We identify individual clouds in the inner Galaxy by fitting
[CII] and CO isotopologue spectra along each line of sight. We combine these
with HI spectra, along with excitation models and cloud models of C+, to
determine the column densities and fractional mass of CO-dark H2 clouds.
Results: We identify 1804 narrow velocity [CII] interstellar cloud components
in different categories. About 840 are diffuse molecular clouds with no CO, 510
are transition clouds containing [CII] and 12CO, but no 13CO, and the remainder
are dense molecular clouds containing 13CO emission. The CO-dark H2 clouds are
concentrated between Galactic radii 3.5 to 7.5 kpc and the column density of
the CO-dark H2 layer varies significantly from cloud-to-cloud with an average
9X10^(20) cm-2. These clouds contain a significant fraction of CO-dark H2 mass,
varying from ~75% for diffuse molecular clouds to ~20% for dense molecular
clouds. Conclusions: We find a significant fraction of the warm molecular ISM
gas is invisible in HI and CO, but is detected in [CII]. The fraction of
CO-dark H2 is greatest in the diffuse clouds and decreases with increasing
total column density, and is lowest in the massive clouds.Comment: 21 pages, 19 figures, accepted for publication in A&A (2014
La educación por competencias en ciencias naturales
Si bien existen programas de actualización docente, en el ámbito de las Ciencias Naturales dentro de la “Educación por Competencias”, la mayoría de las instituciones que ofrecen capacitación, lo hacen sólo desde el “saber” -conocimiento-, dejando de lado el “saber hacer” y el “saber ser”. El hecho de dejar fuera dos componentes fundamentales de las competencias produce una visión distorsionada en los docentes, la cual hace crisis cuando llegan al aula ha implementar la enseñanza por competencias, pero sobre todo al momento de evaluarlas
Ionized gas at the edge of the Central Molecular Zone
To determine the properties of the ionized gas at the edge of the CMZ near
Sgr E we observed a small portion of the edge of the CMZ near Sgr E with
spectrally resolved [C II] 158 micron and [N II] 205 micron fine structure
lines at six positions with the GREAT instrument on SOFIA and in [C II] using
Herschel HIFI on-the-fly strip maps. We use the [N II] spectra along with a
radiative transfer model to calculate the electron density of the gas and the
[C II] maps to illuminate the morphology of the ionized gas and model the
column density of CO-dark H2. We detect two [C II] and [N II] velocity
components, one along the line of sight to a CO molecular cloud at -207 km/s
associated with Sgr E and the other at -174 km/s outside the edge of another CO
cloud. From the [N II] emission we find that the average electron density is in
the range of about 5 to 25 cm{-3} for these features. This electron density is
much higher than that of the warm ionized medium in the disk. The column
density of the CO-dark H layer in the -207 km/s cloud is about 1-2X10{21}
cm{-2} in agreement with theoretical models. The CMZ extends further out in
Galactic radius by 7 to 14 pc in ionized gas than it does in molecular gas
traced by CO. The edge of the CMZ likely contains dense hot ionized gas
surrounding the neutral molecular material. The high fractional abundance of N+
and high electron density require an intense EUV field with a photon flux of
order 1e6 to 1e7 photons cm{-2} s{-1}, and/or efficient proton charge exchange
with nitrogen, at temperatures of order 1e4 K, and/or a large flux of X-rays.
Sgr E is a region of massive star formation which are a potential sources of
the EUV radiation that can ionize the gas. In addition X-ray sources and the
diffuse X-ray emission in the CMZ are candidates for ionizing nitrogen.Comment: 12 pages, 9 figure
L1599B: Cloud Envelope and C+ Emission in a Region of Moderately Enhanced Radiation Field
We study the effects of an asymmetric radiation field on the properties of a
molecular cloud envelope. We employ observations of carbon monoxide (12CO and
13CO), atomic carbon, ionized carbon, and atomic hydrogen to analyze the
chemical and physical properties of the core and envelope of L1599B, a
molecular cloud forming a portion of the ring at approximately 27 pc from the
star Lambda Ori. The O III star provides an asymmetric radiation field that
produces a moderate enhancement of the external radiation field. Observations
of the [CII] fine structure line with the GREAT instrument on SOFIA indicate a
significant enhanced emission on the side of the cloud facing the star, while
the [Ci], 12CO and 13CO J = 1-0 and 2-1, and 12CO J = 3-2 data from the PMO and
APEX telescopes suggest a relatively typical cloud interior. The atomic, ionic,
and molecular line centroid velocities track each other very closely, and
indicate that the cloud may be undergoing differential radial motion. The HI
data from the Arecibo GALFA survey and the SOFIA/GREAT [CII] data do not
suggest any systematic motion of the halo gas, relative to the dense central
portion of the cloud traced by 12CO and 13CO.Comment: 9 Figure
Soft, collinear and non-relativistic modes in radiative decays of very heavy quarkonium
We analyze the end-point region of the photon spectrum in semi-inclusive
radiative decays of very heavy quarkonium (m alpha_s^2 >> Lambda_QCD). We
discuss the interplay of the scales arising in the Soft-Collinear Effective
Theory, m, m(1-z)^{1/2} and m(1-z) for z close to 1, with the scales of heavy
quarkonium systems in the weak coupling regime, m, m alpha_s and m alpha_s^2.
For 1-z \sim alpha_s^2 only collinear and (ultra)soft modes are seen to be
relevant, but the recently discovered soft-collinear modes show up for 1-z <<
alpha_s^2. The S- and P-wave octet shape functions are calculated. When they
are included in the analysis of the photon spectrum of the Upsilon (1S) system,
the agreement with data in the end-point region becomes excellent. The NRQCD
matrix elements and
are also obtained.Comment: Revtex, 11 pages, 6 figures. Minor improvements and references added.
Journal versio
Summer rainfall variability in European Mediterranean mountains from the sixteenth to the twentieth century reconstructed from tree rings.
En este trabajo se utilizan dendrocronologías para reconstruir la precipitación estival
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