The importance of preoperative elevated serum levels of CEA and CA15-3 in patients with breast cancer in predicting its histological type.

It is not known whether in patients with breast cancer the occurrence of elevated serum tumour markers depends on its histological type. The aim of the study was to assess relationship between breast cancer histological type and the presence of increased serum levels of CEA and CA 15-3. The study population was 428 patients (all women, mean age 52.5 years), treated at The Department of Surgery of Wroclaw Medical University from 2005 to 2008 due to breast cancer. All of them had their preoperative CA 15-3 and CEA serum concentrations measured. According to the TNM system, 21% of patients were in stage I, 32.5% in stage II, 46.5% in stage III of the disease. In patients with ductal type of the cancer the elevated serum levels of CEA and CA 15-3 were observed in 48.7% and 42.2%, in lobular type in 42.4% and 52.5%, and in non-ductal/tubular types in 48.1% and 40.4% (p=N/S). Stepwise logistic regression analyses showed that ductal breast cancer is related to elevated CEA and normal CA 15-3 serum levels. The histological types of breast cancer are not significantly related to elevated serum levels of CEA and/or CA 15-3

Assessing the C/O Ratio Formation Diagnostic: A Potential Trend with Companion Mass

The carbon-to-oxygen (C/O) ratio in an exoplanet atmosphere has been suggested as a potential diagnostic of planet formation. Now that a number of exoplanets have measured C/O ratios, it is possible to examine this diagnostic at a population level. Here, we present an analysis of currently measured C/O ratios of directly imaged and transit/eclipse planets. First, we derive atmospheric parameters for the substellar companion HD 284149 b using data that were taken with the OSIRIS integral field spectrograph at the W.M. Keck Observatory and report two non-detections from our ongoing imaging spectroscopy survey of exoplanetary atmospheres with Keck/OSIRIS. We find an effective temperature of $T_\mathrm{eff} = 2502$~K, with a range of 2291--2624~K, $\log g=4.52$, with a range of 4.38--4.91, and [M/H] = 0.37, with a range of 0.10--0.55. These values are in agreement with previous studies done by Bonavita et al. (2014, 2017). We derive a C/O of 0.589$^{+0.148}_{-0.295}$ for HD 284149 b. We then add this measurement to the growing list of C/O ratios for directly imaged planets from the literature, and compare them with those available from a sample of transit/eclipse planets. There is a trend in C/O ratio with companion mass (M$_{\mathrm{Jup}}$), with a break seen around 4 M$_{\mathrm{Jup}}$. We run a Kolmogorov-Smirnov and an Anderson-Darling test on planets above and below this mass boundary, and find that they are two distinct populations. This could be additional evidence of two distinct populations possibly having two different formation pathways, with companion mass as a primary indicator of most likely formation scenario.Comment: 20 pages, 12 figure

Prognostic value of CA 19-9 level in resectable pancreatic adenocarcinoma.

The prognosis in patients with pancreatic cancer is poor and some authors describe it as a lethal disease. At the time of diagnosis only 14% of patients could be surgically treated and up to 30% of them die within 12 months. Therefore, further clinical investigations on preoperative patient qualification are needed. A total of 81 patients were included into the study. The CA 19-9 concentration was measured before surgery by an automated, commercially available enzyme immunoassay in Axsym analyzer (Abott Diagnostics Laboratory). A value of 37 U/ml was used as the upper limit of normal levels. Tumors were staged according to the Union Against Cancer (UICC) of 2004 and graded during the histological evaluation according to the G0-G4 scale. All patients were monitored every three month via outpatient clinic visits. In the case of missing visit we contacted the families to establish the cause. We assessed perioperative, 12 month, 2 year and 5 year survival. Twelve moth, 2 year and 5 year survival were assessed in the whole studied population and in the group of patients with the exception of these who died during the perioperative period. The total five year survival was 6%. The median time of survival was 467 days (range: 163 - 586 days). The perioperative period was survived by 91.4% patients, 12 months were survived by 71.6% patients, 2 years were survived by 35.8% patients, 5 years were survived by 6.2% patients. The serum Ca 19-9 level was above the normal limit in 80.5% patients. ROC curve analysis revealed that CA 19-9 level of more than 106 U/ml was linked to 2 year survival with 79.3% sensitivity and 74.5% specificity. Preoperative level of CA 19-9 below 106U/ml represents a predictive factor of 2- and 5-year survival, independent of other factors, such as lower size of the tumor, absence of metastases to lymph nodes, female gender of patients. After exclusion of the patients who died in the perioperative period, no relationship could have been disclosed between preoperative CA 19-9 levels and one year survival. The observation points to the chance that patients with higher levels of CA 19-9 harbour micrometastases, the development of which is sufficiently slow to allow for a one-year survival of the patients but which increase the risk of death after two and five years

Deep exploration of the planets HR 8799 b, c, and d with moderate-resolution spectroscopy

Funding: J.-B.R. acknowledges support from the David and Ellen Lee Prize Postdoctoral Fellowship. The research was supported by grants from NSF, including AST-1411868 (J.-B.R., B.M.) and 1614492 (T.S.B.). Material presented in this work is supported by the National Aeronautics and Space Administration under Grants/Contracts/Agreements No. NNX17AB63G (Q.M.K., T.S.B., and K.K.W.) issued through the Astrophysics Division of the Science Mission Directorate and NNX15AD95G (J.-B.R., R.J.D.R.).The four directly imaged planets orbiting the star HR 8799 are an ideal laboratory to probe atmospheric physics and formation models. We present more than a decade's worth of Keck/OSIRIS observations of these planets, which represent the most detailed look at their atmospheres to date by its resolution and signal-to-noise ratio. We present the first direct detection of HR 8799 d, the second-closest known planet to the star, at moderate spectral resolution with Keck/OSIRIS (K band; R ≈ 4000). Additionally, we uniformly analyze new and archival OSIRIS data (H and K band) of HR 8799 b, c, and d. First, we show detections of water (H2O) and carbon monoxide (CO) in the three planets and discuss the ambiguous case of methane (CH4) in the atmosphere of HR 8799 b. Then, we report radial-velocity (RV) measurements for each of the three planets. The RV measurement of HR 8799 d is consistent with predictions made assuming coplanarity and orbital stability of the HR 8799 planetary system. Finally, we perform a uniform atmospheric analysis on the OSIRIS data, published photometric points, and low-resolution spectra. We do not infer any significant deviation from the stellar value of the carbon-to-oxygen ratio (C/O) of the three planets, which therefore does not yet yield definitive information about the location or method of formation. However, constraining the C/O for all the HR 8799 planets is a milestone for any multiplanet system, and particularly important for large, widely separated gas giants with uncertain formation processes.Publisher PDFPeer reviewe

The only known cyclopygid–‘atheloptic’ trilobite fauna from North America: the upper Ordovician fauna of the Pyle Mountain Argillite and its palaeoenvironmental significance

The trilobite fauna of the upper Ordovician (middle Katian) Pyle Mountain Argillite comprises a mixture of abundant mesopelagic cyclopygids and other pelagic taxa and a benthic fauna dominated by trilobites lacking eyes. Such faunas were widespread in deep water environments around Gondwana and terranes derived from that continent throughout Ordovician time but this is the only known record of such a fauna from North America and thus from Laurentia. It probably reflects a major sea level rise (the ‘Linearis drowning events’) as does the development of coeval cyclopygid-dominated deep water trilobite faunas in terranes that were marginal to Laurentia and are now preserved in Ireland and Scotland. The Pyle Mountain Argillite trilobite fauna occurs with a deep water Foliomena brachiopod fauna and comprises 22 species. Pelagic trilobites (mostly cyclopygids) constitute 36% of the preserved sclerites, and 45% of the fauna is the remains of trilobites lacking eyes, including one new species, Dindymene whittingtoni sp. nov. Three species of cyclopygid are present, belonging in Cyclopyge, Symphysops and Microparia (Heterocyclopyge). Cyclopygids are widely thought to have been stratified in the water column in life and thus their taxonomic diversity reflects the relative depths of the sea-beds on which their remains accumulated. A tabulation of middle and upper Katian cyclopygid-bearing faunas from several palaeoplates and terranes arranged on the basis of increasing numbers of cyclopygid genera allows an assessment of the relative depth ranges of the associated benthic taxa. The Pyle Mountain Argillite fauna lies towards the deeper end of this depth spectrum

Biases in the perceived timing of perisaccadic perceptual and motor events

Subjects typically experience the temporal interval immediately following a saccade as longer than a comparable control interval. One explanation of this effect is that the brain antedates the perceptual onset of a saccade target to around the time of saccade initiation. This could explain the apparent continuity of visual perception across eye movements. Thisantedating account was tested in three experiments in which subjects made saccades of differing extents and then judged either the duration or the temporal order of key events. Postsaccadic stimuli underwent subjective temporal lengthening and had early perceived onsets. A temporally advanced awareness of saccade completion was also found, independently of antedating effects. These results provide convergent evidence supporting antedating and differentiating it from other temporal biases

Detecting Exoplanets Closer to Stars with Moderate Spectral Resolution Integral-Field Spectroscopy

While radial velocity surveys have demonstrated that the population of gas giants peaks around $3~\text{au}$, the most recent high-contrast imaging surveys have only been sensitive to planets beyond $\sim~10~\text{au}$. Sensitivity at small angular separations from stars is currently limited by the variability of the point spread function. We demonstrate how moderate-resolution integral field spectrographs can detect planets at smaller separations ($\lesssim~0.3$ arcseconds) by detecting the distinct spectral signature of planets compared to the host star. Using OSIRIS ($R$ $\approx$ 4000) at the W. M. Keck Observatory, we present the results of a planet search via this methodology around 20 young targets in the Ophiuchus and Taurus star-forming regions. We show that OSIRIS can outperform high-contrast coronagraphic instruments equipped with extreme adaptive optics and non-redundant masking in the $0.05-0.3$ arcsecond regime. As a proof of concept, we present the $34\sigma$ detection of a high-contrast M dwarf companion at $\approx0.1$" with a flux ratio of $\approx0.92\%$ around the field F2 star HD 148352. We developed an open-source Python package, breads, for the analysis of moderate-resolution integral field spectroscopy data in which the planet and the host star signal are jointly modeled. The diffracted starlight continuum is forward-modeled using a spline model, which removes the need for prior high-pass filtering or continuum normalization. The code allows for analytic marginalization of linear hyperparameters, simplifying posterior sampling of other parameters (e.g., radial velocity, effective temperature). This technique could prove very powerful when applied to integral field spectrographs like NIRSpec on the JWST and other upcoming first-light instruments on the future Extremely Large Telescopes.Comment: Accepted for publication in the Astronomical Journal on May 12, 202

Phylogenetic placement of Adalatherium hui (Mammalia, Gondwanatheria) from the Late Cretaceous of Madagascar : implications for allotherian relationships

The phylogenetic position of Gondwanatheria within Mammaliaformes has historically been controversial. The well-preserved skeleton of Adalatherium hui from the Late Cretaceous of Madagascar offers a unique opportunity to address this issue, based on morphological data from the whole skeleton. Gondwanatheria were, until recently, known only from fragmentary dental and mandibular material, as well as a single cranium. The holotype of A. hui provides the first postcranial skeleton for gondwanatherians and substantially increases the amount of character data available to score. We sampled 530 characters and 84 cynodonts (including 34 taxa historically affiliated with Allotheria) to test the phylogenetic relationships of Gondwanatheria and Allotheria using parsimony, undated Bayesian, and tip-dated Bayesian methods. We tested three lower dental formulae for Adalatherium, because its postcanines are distinctly different from those of other mammaliaforms and cannot readily be homologized with any known dental pattern. In all analyses, Adalatherium is recovered within Gondwanatheria, most frequently outside of Sudamericidae or Ferugliotheriidae, which is congruent with establishment of the family Adalatheriidae. The different dental coding schemes do not greatly impact the position of Adalatherium, although there are differences in character optimization. In all analyses, Gondwanatheria are placed within Allotheria, either as sister to Multituberculata, nested within Multituberculata, or as sister to Cifelliodon (and Euharamiyida), or in a polytomy with other allotherians. The composition of Allotheria varies in our analyses. The haramiyidans Haramiyavia and Thomasia are placed outside of Allotheria in the parsimony and tip-dated Bayesian analyses, but in a polytomy with other allotherians in the undated Bayesian analyses