124 research outputs found
Discovery of the Pigtail Molecular Cloud in the Galactic Center
This paper reports the discovery of a helical molecular cloud in the central
molecular zone (CMZ) of our Galaxy. This "pigtail" molecular cloud appears at
(l, b, V_LSR) ~ (-0.7deg, +0.0deg, -70 to -30 km/s), with a spatial size of ~
(20 pc)^2 and a mass of (2-6) 10^5 solar masses. This is the third helical
gaseous nebula found in the Galactic center region to date. Line intensity
ratios indicate that the pigtail molecular cloud has slightly higher
temperature and/or density than the other normal clouds in the CMZ. We also
found a high-velocity wing emission near the footpoint of this cloud. We
propose a formation model of the pigtail molecular cloud. It might be
associated with a magnetic tube that is twisted and coiled because of the
interaction between clouds in the innermost x_1 orbit and ones in the outermost
x_2 orbit.Comment: 15 pages, 6 figures, accepted for publication in Astrophysical
Journa
Dense Molecular Clumps associated with the LMC Supergiant Shells LMC 4 \& LMC 5
We investigate the effects of Supergiant Shells (SGSs) and their interaction
on dense molecular clumps by observing the Large Magellanic Cloud (LMC) star
forming regions N48 and N49, which are located between two SGSs, LMC 4 and LMC
5. CO (=3-2, 1-0) and CO (=1-0) observations with the ASTE
and Mopra telescopes have been carried out towards these regions. A clumpy
distribution of dense molecular clumps is revealed with 7 pc spatial
resolution. Large velocity gradient analysis shows that the molecular hydrogen
densities () of the clumps are distributed from low to high
density (- cm) and their kinetic temperatures () are typically high (greater than K). These clumps seem to be in the
early stages of star formation, as also indicated from the distribution of
H, young stellar object candidates, and IR emission. We found that the
N48 region is located in the high column density HI envelope at the interface
of the two SGSs and the star formation is relatively evolved, whereas the N49
region is associated with LMC 5 alone and the star formation is quiet. The
clumps in the N48 region typically show high and ,
which are as dense and warm as the clumps in LMC massive cluster-forming areas
(30 Dor, N159). These results suggest that the large-scale structure of the
SGSs, especially the interaction of two SGSs, works efficiently on the
formation of dense molecular clumps and stars.Comment: 26 pages, 7 tables, 16 figure
Dense Clumps in Giant Molecular Clouds in the Large Magellanic Cloud: Density and Temperature Derived from CO() Observations
In order to precisely determine temperature and density of molecular gas in
the Large Magellanic Cloud, we made observations of optically thin
CO() transition by using the ASTE 10m telescope toward 9 peaks
where CO() clumps were previously detected with the same
telescope. The molecular clumps include those in giant molecular cloud (GMC)
Types I (with no signs of massive star formation), II (with HII regions only),
and III (with HII regions and young star clusters). We detected
CO() emission toward all the peaks and found that their
intensities are 3 -- 12 times lower than those of CO(). We
determined the intensity ratios of CO() to CO(),
, and CO() to CO(),
, at 45\arcsec resolution. These ratios were used for
radiative transfer calculations in order to estimate temperature and density of
the clumps. The parameters of these clumps range kinetic temperature
= 15 -- 200 K, and molecular hydrogen gas density
= 8 -- 7 cm. We confirmed
that the higher density clumps show higher kinetic temperature and that the
lower density clumps lower kinetic temperature at a better accuracy than in the
previous work. The kinetic temperature and density increase generally from a
Type I GMC to a Type III GMC. We interpret that this difference reflects an
evolutionary trend of star formation in molecular clumps. The
and kinetic temperature of the clumps are well correlated
with H flux, suggesting that the heating of molecular gas
= -- cm can be explained by stellar FUV
photons.Comment: 39 pages, 7 figures, 4 tables. Accepted for publication in The
Astronomical Journa
SLPI is a critical mediator that controls PTH-induced bone formation
Osteoclastic bone resorption and osteoblastic bone formation/replenishment are closely coupled in bone metabolism. Anabolic parathyroid hormone (PTH), which is commonly used for treating osteoporosis, shifts the balance from osteoclastic to osteoblastic, although it is unclear how these cells are coordinately regulated by PTH. Here, we identify a serine protease inhibitor, secretory leukocyte protease inhibitor (SLPI), as a critical mediator that is involved in the PTH-mediated shift to the osteoblastic phase. Slpi is highly upregulated in osteoblasts by PTH, while genetic ablation of Slpi severely impairs PTH-induced bone formation. Slpi induction in osteoblasts enhances its differentiation, and increases osteoblast–osteoclast contact, thereby suppressing osteoclastic function. Intravital bone imaging reveals that the PTH-mediated association between osteoblasts and osteoclasts is disrupted in the absence of SLPI. Collectively, these results demonstrate that SLPI regulates the communication between osteoblasts and osteoclasts to promote PTH-induced bone anabolism.Morimoto A., Kikuta J., Nishikawa K., et al. SLPI is a critical mediator that controls PTH-induced bone formation. Nature Communications 12, 2136 (2021); https://doi.org/10.1038/s41467-021-22402-x
- …