We have mapped Ne II (12.8 km) and S IV (10.5 km) emission from W51 IRS 2 with TEXES on Gemini North, and we compare these data to VLA free-free observations and VLT near-infrared images. With 0.5" ...spatial and 4 km s super(-1) spectral resolution, we are able to separate the ionized gas into several components: an extended H II region on the front surface of the molecular cloud, several embedded compact H II regions, and a streamer of high-velocity gas. We interpret the high-velocity streamer as a processing or fanlike jet, which has emerged from the molecular cloud into an OB star cluster where it is being ionized.
This study represents the largest compilation to date of clinical and postmortem data from decedents with coronavirus disease 2019 (COVID-19). It will augment previously published small series of ...autopsy case reports, refine clinicopathologic considerations, and improve the accuracy of future vital statistical reporting.
To accurately reflect the preexisting diseases and pathologic conditions of decedents with SARS-CoV-2 (severe acute respiratory syndrome coronavirus 2) infection through autopsy.
Comprehensive data from 135 autopsy evaluations of COVID-19-positive decedents is presented, including histologic assessment. Postmortem examinations were performed by 36 pathologists at 19 medical centers or forensic institutions in the United States and Brazil. Data from each autopsy were collected through the online submission of multiple-choice and open-ended survey responses.
Patients dying of or with COVID-19 had an average of 8.89 pathologic conditions documented at autopsy, spanning a combination of prior chronic disease and acute conditions acquired during hospitalization. Virtually all decedents were cited as having more than 1 preexisting condition, encompassing an average of 2.88 such diseases each. Clinical conditions during terminal hospitalization were cited 395 times for the 135 autopsied decedents and predominantly encompassed acute failure of multiple organ systems and/or impaired coagulation. Myocarditis was rarely cited.
Cause-of-death statements in both autopsy reports and death certificates may not encompass the severity or spectrum of comorbid conditions in those dying of or with COVID-19. If supported by additional research, this finding may have implications for public health decisions and reporting moving forward through the pandemic.
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DOBA, IZUM, KILJ, NUK, OILJ, PILJ, PNG, SAZU, SIK, UILJ, UKNU, UL, UM, UPUK, VSZLJ
► Temperature retrievals are similar to previous measurements of Neptune’s stratosphere. ► No meridional temperature variations are found within the errors. ► Meridional temperature variations are ...smaller than radiative-seasonal model predictions. ► Neptune appears to have meridionally invariant abundances of C
2H
2 and C
2H
6 in the current epoch.
Using TEXES, the Texas Echelon cross Echelle Spectrograph, mounted on the Gemini North 8-m telescope we have mapped the spatial variation of H
2, CH
4, C
2H
2 and C
2H
6 thermal-infrared emission of Neptune. These high-spectral-resolution, spatially resolved, thermal-infrared observations of Neptune offer a unique glimpse into the state of Neptune’s stratosphere in October 2007,
L
S
=
275.4° just past Neptune’s southern summer solstice (
L
S
=
270°). We use observations of the S(1) pure rotational line of molecular hydrogen and a portion of the
ν
4 band of methane to retrieve detailed information on Neptune’s stratospheric vertical and meridional thermal structure. We find global-average temperatures of 163.8
±
0.8, 155.0
±
0.9, and 123.8
±
0.8
K at the 7.0
×
10
−3-, 0.12-, and 2.1-mbar levels with no meridional variations within the errors. We then use the inferred temperatures to model the emission of C
2H
2 and C
2H
6 in order to derive stratospheric volume mixing ratios (hence forth, VMR) as a function of pressure and latitude. There is a subtle meridional variation of the C
2H
2 VMR at the 0.5-mbar level with the peak abundance found at −28° latitude, falling off to the north and south. However, the observations are consistent within error to a meridionally constant C
2H
2 VMR of
3.3
-
0.9
+
1.2
×
10
-
8
at 0.5
mbar. We find that the VMR of C
2H
6 at 1-mbar peaks at the equator and falls by a factor of 1.6 at −70° latitude. However, a meridionally constant VMR of
9.3
-
2.6
+
3.5
×
10
-
7
at the 1-mbar level for C
2H
6 is also statistically consistent with the retrievals. Temperature predictions from a radiative-seasonal climate model of Neptune that assumes the hydrocarbon abundances inferred in this paper are lower than the measured temperatures by 40
K at 7
×
10
−3
mbar, 30
K at 0.12
mbar and 25
K at 2.1
mbar. The radiative-seasonal model also predicts meridional temperature variations on the order of 10
K from equator to pole, which are not observed. Assuming higher stratospheric CH
4 abundance at the equator relative to the south pole would bring the meridional trends of the inferred temperatures and radiative-seasonal model into closer agreement.
We have also retrieved observations of C
2H
4 emission from Neptune’s stratosphere using TEXES on the NASA Infrared Telescope Facility (IRTF) in June 2003,
L
S
=
266°. Using the observations from the middle of the planet and an average of the middle three latitude temperature profiles from the 2007 observations (9.5° of
L
S later, the seasonal equivalent of 9.5 Earth days within Earth’s seasonal cycle), we infer a C
2H
4 VMR of
5.9
-
0.8
+
1.0
×
10
-
7
at 1.5
×
10
−3
mbar, a value that is 3.25 times that predicted by global-average photochemical models.
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GEOZS, IJS, IMTLJ, KILJ, KISLJ, NUK, OILJ, PNG, SAZU, SBCE, SBJE, UL, UM, UPCLJ, UPUK
We present a data cube of the NeII (12.8 μm) emission from the inner 2 pc of Sgr A West with 1″ and 4 km s−1 resolution, and with substantially better SNR and velocity resolution than previous ...observations of the ionized gas. We compare the observations to two proposed models of the gas motions and distribution: flows along tidally stretched streamers, and more nearly circular motions with density wave compression. The density wave model provides a considerably better fit to the kinematics of the northern arm and western arc. Neither model fits the eastern arm and bar kinematics well. To help understand the origin of the spiral pattern we calculated orbits in the potential of a black hole in a star cluster and find that the orbits naturally evolve to set up a one-armed spiral wave very similar to that observed, both spatially and kinematically. Magnetic or other perturbing forces may influence the formation of the spiral wave, but self gravity is not required. Because a density wave evolves on the orbit precession timescale, rather than the orbital timescale, a wave pattern should persist for several 105 yr. No net inward motion of the gas is required by the model. If there is inflow, it is much smaller than is suggested by the infalling streamer model.
Hydrogen peroxide (H
2O
2) has been suggested as a possible oxidizer of the martian surface. Photochemical models predict a mean column density in the range of 10
15–10
16 cm
−2. However, a stringent ...upper limit of the H
2O
2 abundance on Mars (9×10
14 cm
−2) was derived in February 2001 from ground-based infrared spectroscopy, at a time corresponding to a maximum water vapor abundance in the northern summer (30 pr.
μm,
Ls=112°). Here we report the detection of H
2O
2 on Mars in June 2003, and its mapping over the martian disk using the same technique, during the southern spring (
Ls=206°) when the global water vapor abundance was ∼10 pr.
μm. The spatial distribution of H
2O
2 shows a maximum in the morning around the sub-solar latitude. The mean H
2O
2 column density (6×10
15 cm
−2) is significantly greater than our previous upper limit, pointing to seasonal variations. Our new result is globally consistent with the predictions of photochemical models, and also with submillimeter ground-based measurements obtained in September 2003 (
Ls=254°), averaged over the martian disk (Clancy et al., 2004, Icarus 168, 116–121).
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GEOZS, IJS, IMTLJ, KILJ, KISLJ, NUK, OILJ, PNG, SAZU, SBCE, SBJE, UL, UM, UPCLJ, UPUK
High spectral and spatial resolution, mid-infrared fine-structure line observations toward two ultracompact H II (UC H II) regions (G29.96-0.02 and Mon R2) allow us to study the structure and ...kinematics of cometary UC H II regions. In our earlier study of Mon R2, we showed that highly organized mass motions accounted for most of the velocity structure in that UC H II region. In this work, we show that the kinematics in both Mon R2 and G29.96 are consistent with motion along an approximately paraboloidal shell. We model the velocity structure seen in our mapping data and test the stellar wind bow shock model for such paraboloidal-like flows. The observations and the simulation indicate that the ram pressures of the stellar wind and ambient interstellar medium cause the accumulated mass in the bow shock to flow along the surface of the shock. A relaxation code reproduces the mass flow's velocity structure as derived by the analytical solution. It further predicts that the pressure gradient along the flow can accelerate ionized gas to a speed higher than that of the moving star. In the original bow shock model, the star speed relative to the ambient medium was considered to be the exit speed of ionized gas in the shell.
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