102 research outputs found
Star formation associated with a large-scale infrared bubble
Using the data from the Galactic Ring Survey (GRS) and Galactic Legacy
Infrared Mid-Plane Survey Extraordinaire (GLIMPSE), we performed a study for a
large-scale infrared bubble with a size of about 16 pc at a distance of 2.0
kpc. We present the 12CO J=1-0, 13CO J=1-0 and C18O J=1-0 observations of HII
region G53.54-0.01 (Sh2-82) obtained at the the Purple Mountain Observation
(PMO) 13.7 m radio telescope to investigate the detailed distribution of
associated molecular material. The large-scale infrared bubble shows a
half-shell morphology at 8 um. H II regions G53.54-0.01, G53.64+0.24, and
G54.09-0.06 are situated on the bubble. Comparing the radio recombination line
velocities and associated 13CO J=1-0 components of the three H II regions, we
found that the 8 um emission associated with H II region G53.54-0.01 should
belong to the foreground emission, and only overlap with the large-scale
infrared bubble in the line of sight. Three extended green objects (EGOs, the
candidate massive young stellar objects), as well as three H II regions and two
small-scale bubbles are found located in the G54.09-0.06 complex, indicating an
active massive star-forming region. C18O J=1-0 emission presents four cloud
clumps on the northeastern border of H II region G53.54-0.01. Via comparing the
spectral profiles of 12CO J=1-0, 13CO J=1-0, and C18O J=1-0 peak at each clump,
we found the collected gas in the three clumps, except for the clump coincided
with a massive YSO (IRAS 19282+1814). Using the evolutive model of H II region,
we derived that the age of H II region G53.54-0.01 is 1.5*10^6 yr. The
significant enhancement of several Class I and Class II YSOs around G53.54-0.01
indicates the presence of some recently formed stars, which may be triggered by
this H II region through the collect and collapse (CC) process.Comment: 9 pages, 6 figures, accepted for publication in A&
A search for 95 GHz class I methanol masers in molecular outflows
We have observed a sample of 288 molecular outflow sources including 123
high-mass and 165 low-mass sources to search for class I methanol masers at 95
GHz transition and to investigate relationship between outflow characteristics
and class I methanol maser emission with the PMO-13.7m radio telescope. Our
survey detected 62 sources with 95 GHz methanol masers above 3
detection limit, which include 47 high-mass sources and 15 low-mass sources.
Therefore the detection rate is 38% for high-mass outflow sources and 9% for
low-mass outflow sources, suggesting that class I methanol maser is relatively
easily excited in high-mass sources. There are 37 newly detected 95 GHz
methanol masers (including 27 high-mass and 10 low-mass sources), 19 of which
are newly identified (i.e. first identification) class I methanol masers
(including 13 high-mass and 6 low-mass sources). Statistical analysis for the
distributions of maser detections with the outflow parameters reveals that the
maser detection efficiency increases with outflow properties (e.g. mass,
momentum, kinetic energy and mechanical luminosity of outflows etc.).
Systematic investigations of relationships between the intrinsic luminosity of
methanol maser and the outflow properties (including mass, momentum, kinetic
energy, bolometric luminosity and mass loss rate of central stellar sources)
indicate a positive correlations. This further supports that class I methanol
masers are collisionally pumped and associated with shocks, where outflows
interact with the surrounding ambient medium.Comment: 32 pages, 5 figures, accepted by Ap
C2H N=1-0 and N2H+ J=1-0 observations of Planck Galactic cold clumps
A survey of C2H N=1-0 and N2H+ J=1-0 toward Planck Galactic cold clumps
(PGCCs) was performed using the Purple Mountain Observatory's 13.7 m telescope.
C2H and N2H+ were chosen to study the chemical evolutionary states of PGCCs.
Among 121 observed molecular cores associated with PGCCs, 71 and 58 are
detected with C2H N=1-0 and N2H+ J=1-0, respectively. The detected lines of
most sources can be fitted with a single component with compatible Vlsr and
line widths, which confirms that these PGCC cores are very cold (with gas
temperatures 9-21 K) and quiescent while still dominanted by turbulence. The
ratio between the column densities of C2H and N2H+ (N(C2H)/N(N2H+)) is found to
be a good tracer for the evolutionary states of PGCC cores. Gas-grain chemical
model can reproduce the decreasing trend of N(C2H)/N(N2H+) as a function of
time. The cores with the lowest abundances of N2H+ (X[N2H+] < 10^{-10}) are the
youngest, and have nearly constant abundances of C2H. In evolved cores with
X[N2H+] ~ 1E-9, abundances of C2H drop quickly as the exhaustion of carbon
atoms. Although these PGCC cores are in different evolutionary states, they are
all quite young ( N(N2H+). Mapping observations are
carried out toward 20 PGCC cores. The PGCC cores in Cepheus have lower
N(C2H)/N(N2H+) and larger line widths compared with those in Taurus. This
implies that PGCC cores in Taurus are less chemically evolved than those in
Cepheus.Comment: 23 pages, 6 figures, 5 table
Gas kinematics and star formation in the filamentary molecular cloud G47.06+0.26
We performed a multi-wavelength study toward the filamentary cloud
G47.06+0.26 to investigate the gas kinematics and star formation. We present
the 12CO (J=1-0), 13CO (J=1-0) and C18O (J=1-0) observations of G47.06+0.26
obtained with the Purple Mountain Observation (PMO) 13.7 m radio telescope to
investigate the detailed kinematics of the filament. The 12CO (J=1-0) and 13CO
(J=1-0) emission of G47.06+0.26 appear to show a filamentary structure. The
filament extends about 45 arcmin (58.1 pc) along the east-west direction. The
mean width is about 6.8 pc, as traced by the 13CO (J=1-0) emission. G47.06+0.26
has a linear mass density of about 361.5 Msun/pc. The external pressure (due to
neighboring bubbles and H II regions) may help preventing the filament from
dispersing under the effects of turbulence. From the velocity-field map, we
discern a velocity gradient perpendicular to G47.06+0.26. From the Bolocam
Galactic Plane Survey (BGPS) catalog, we found nine BGPS sources in
G47.06+0.26, that appear to these sources have sufficient mass to form massive
stars. We obtained that the clump formation efficiency (CFE) is about 18% in
the filament. Four infrared bubbles were found to be located in, and adjacent
to, G47.06+0.26. Particularly, infrared bubble N98 shows a cometary structure.
CO molecular gas adjacent to N98 also shows a very intense emission. H II
regions associated with infrared bubbles can inject the energy to surrounding
gas. We calculated the kinetic energy, ionization energy, and thermal energy of
two H II regions in G47.06+0.26. From the GLIMPSE I catalog, we selected some
Class I sources with an age of about 100000 yr, which are clustered along the
filament. The feedback from the H II regions may cause the formation of a new
generation of stars in filament G47.06+0.26.Comment: 10 pages, 11 figures, accepted for publication in A&
A systematic review and meta-analysis of cohort studies on the potential association between NAFLD/MAFLD and risk of incident atrial fibrillation
Background and objectiveThe association between atrial fibrillation (AF) and non-alcoholic fatty liver disease (NAFLD) or metabolic-associated fatty liver disease (MAFLD) has been explored in recent cohort studies, however, the results have been controversial and inconclusive. This meta-analysis aimed to explore this potential association.MethodsWe systematically searched PubMed, Embase, and Web of Science databases to identify all relevant cohort studies investigating the association between NAFLD/MAFLD and AF published from database inception to October 30, 2022. Random-effects models were utilized to calculate hazard ratios (HRs) with 95% confidence intervals (CIs) for summary purposes. Additionally, subgroup and sensitivity analyses were performed.ResultsA total of 13 cohort studies with 14 272 735 participants were included. Among these, 12 cohort studies with 14 213 289 participants (median follow-up of 7.8 years) showed a significant association between NAFLD and an increased risk of incident AF (HR = 1.18, 95% CI: 1.12-1.23, P < 0.00001). Our subgroup analyses mostly yielded similar results, and the results of sensitivity analyses remained unchanged. However, meta-analysis of data from 2 cohort studies with 59 896 participants (median follow-up of 2.15 years) showed that MAFLD was not linked to incident AF (HR = 1.36, 95% CI: 0.63-2.92, P = 0.44).ConclusionCurrent evidence shows that NAFLD may be linked to a slightly higher risk of developing AF, particularly among Asian populations and those diagnosed with NAFLD using FLI criteria. Nevertheless, there is not enough evidence to support the proposed association between MAFLD and an increased risk of AF. To better understand this relationship, future studies should consider factors such as specific population, the severity of NAFLD/MAFLD, diagnostic methods of NAFLD and AF, and cardiometabolic risk factors.Systematic Review Registrationhttps://www.crd.york.ac.uk/prospero, identifier CRD42022371503
Gas emissions in Planck cold dust clumps---A Survey of the J=1-0 Transitions of CO, CO, and CO
A survey toward 674 Planck cold clumps of the Early Cold Core Catalogue (ECC)
in the J=1-0 transitions of CO, CO and CO has been carried
out using the PMO 13.7 m telescope. 673 clumps were detected with the CO
and CO, and 68% of the samples have CO emission. Additional
velocity components were also identified.A close consistency of the three line
peak velocities was revealed for the first time. Kinematic distances are given
out for all the velocity components and half of the clumps are located within
0.5 and 1.5 kpc. Excitation temperatures range from 4 to 27 K, slightly larger
than those of . Line width analysis shows that the majority of ECC clumps
are low mass clumps. Column densities N span from 10 to
4.5 cm with an average value of
(4.43.6) cm. N cumulative fraction
distribution deviates from the lognormal distribution, which is attributed to
optical depth. The average abundance ratio of the CO to CO in
these clumps is 7.03.8, higher than the terrestrial value. Dust and gas
are well coupled in 95% of the clumps. Blue profile, red profile and line
asymmetry in total was found in less than 10% of the clumps, generally
indicating star formation is not developed yet. Ten clumps were mapped. Twelve
velocity components and 22 cores were obtained. Their morphologies include
extended diffuse, dense isolated, cometary and filament, of which the last is
the majority. 20 cores are starless.Only 7 cores seem to be in gravitationally
bound state. Planck cold clumps are the most quiescent among the samples of
weak-red IRAS, infrared dark clouds, UC H{\sc ii} region candidates, EGOs and
methanol maser sources, suggesting that Planck cold clumps have expanded the
horizon of cold Astronomy.Comment: Accepted to Ap
A 95 GHz Class I Methanol Maser Survey Toward A Sample of GLIMPSE Point Sources Associated with BGPS Clumps
We report a survey with the Purple Mountain Observatory (PMO) 13.7-m radio
telescope for class I methanol masers from the 95 GHz (8_0 - 7_1 A^+)
transition. The 214 target sources were selected by combining information from
both the Spitzer GLIMPSE and 1.1 mm BGPS survey catalogs. The observed sources
satisfy both the GLIMPSE mid-IR criteria of [3.6]-[4.5]>1.3, [3.6]-[5.8]>2.5,
[3.6]-[8.0]>2.5 and 8.0 um magnitude less than 10, and also have an associated
1.1 mm BGPS source. Class I methanol maser emission was detected in 63 sources,
corresponding to a detection rate of 29% for this survey. For the majority of
detections (43), this is the first identification of a class I methanol maser
associated with these sources. We show that the intensity of the class I
methanol maser emission is not closely related to mid-IR intensity or the
colors of the GLIMPSE point sources, however, it is closely correlated with
properties (mass and beam-averaged column density) of the BGPS sources.
Comparison of measures of star formation activity for the BGPS sources with and
without class I methanol masers indicate that the sources with class I methanol
masers usually have higher column density and larger flux density than those
without them. Our results predict that the criteria
log(S_{int})22.1,
which utilizes both the integrated flux density (S_{int}) and beam-averaged
column density (N_{H_{2}}^{beam}) of the BGPS sources, are very efficient for
selecting sources likely to have an associated class I methanol maser. Our
expectation is that searches using these criteria will detect 90% of the
predicted number of class I methanol masers from the full BGPS catalog (~
1000), and do so with a high detection efficiency (~75%).Comment: Accepted for publication in ApJ Supplement. 58 pages, 12 figures, 7
table
Genetic polymorphisms of CYP2A13 and its relationship to nasopharyngeal carcinoma in the Cantonese population
Nasopharyngeal carcinoma (NPC) is characterized by a high prevalence in Southern China, especially among Cantonese individuals of the Guangdong Province. Epidemiological studies have suggested that frequent exposure to high levels of nitrosamine from preserved foods such as salted fish could be a risk factor for NPC. Cytochrome P450 encompasses a family of enzymes that metabolize carcinogens and CYP2A13, a member of this family, is expressed predominantly in the respiratory tract with the highest levels in the nasal mucosa. In an effort to test whether a correlation exists between CYP2A13 genetic polymorphism and the risk of developing NPC, we sequenced all nine exons and the exon-intron junctions of the CYP2A13 gene in 45 NPC patients. We identified a total of 21 single nucleotide polymorphism (SNPs), including 7 novel SNPs. The most frequent functional variant allele was 74A-1757G-3375T-7233G with a haplotype frequency of 7.8% in the 45 NPC cases. In addition, a stop codon mutation was detected in one case. We then selected the 3 most frequent SNPs and one stop codon mutation to expand our study to a case-control analysis within the Cantonese population. A novel haplotype consisting 8 SNPs in introns, and four additional novel SNPs were identified; but no correlation between CYP2A13 genetic polymorphism and individual susceptibility to NPC was observed
- …