Adults of 44 species of Dytiscidae (12 genera) were collected in typical wetland habitats of Québec Hemiarctic. The fauna is characteristic of the boreal portion of the continent with some subarctic ...and arctic elements. Colymbetes dahuricus Aubé is recorded for the first time from Québec. Distinct assemblages of species in different habitats recorded are observed and the ecological distinction of the two similar species Ilybius picipes (Kirby) and I. angustior (Gyllenhal) is documented. Ilybius angustior is typically associated with the rock pools while I. picipes is prevalent in palsa bogs pools. /// Les adultes de 44 espèces de Dytiscidae (12 genres) ont été récoltés dans les principaux types de milieux constitutifs du paysage du Québec hémiarctique. La faune recensée est composée majoritairement d'espèces boréales auxquelles s'associent quelques éléments caractéristiques de la zone subarctique et arctique. Colymbetes dahuricus Aubé est recensée pour la première fois au Québec. Différents regroupement d'espèces sont observés et la distinction écologique entre Ilybius picipes (Kirby) et I. angustior (Gyllenhal) est réalisée pour la première fois. Ilybius angustior est typiquement associée aux mares de rochers tandis que I. picipes montre un nette préférence pour les mares de tourbières à palses.
We present the performance of the Integral Field Spectrograph (IFS) of SPHERE, the high-contrast imager for the ESO VLT telescope designed to perform imaging and spectroscopy of extrasolar planets, ...obtained from tests performed at the Institute de Planétologie et d'Astrophysique de Grenoble facility during the integration phase of the instrument.} {The tests were performed using the instrument software purposely prepared for SPHERE. The output data were reduced applying the SPHERE data reduction and handling software, adding an improved spectral deconvolution procedure. To this aim, we prepared an alternative procedure for the spectral subtraction exploiting the principal components analysis algorithm. Moreover, a simulated angular differential imaging procedure was also implemented to estimate how the instrument performed once this procedure was applied at telescope. The capability of the IFS to faithfully retrieve the spectra of the detected faint companions was also considered.} {We found that the application of the updated version of the spectral deconvolution procedure alone, when the algorithm throughput is properly taken into account, gives us a \(5\sigma\) limiting contrast of the order of 5$\times$$10^{-6}\( or slightly better. The further application of the angular differential imaging procedure on these data should allow us to improve the contrast by one order of magnitude down to around 7\)\times$$10^{-7}$ at a separation of 0.3 arcsec. The application of a principal components analysis procedure that simultaneously uses spectral and angular data gives comparable results. Finally, we found that the reproducibility of the spectra of the detected faint companions is greatly improved when angular differential imaging is applied in addition to the spectral deconvolution.
For Pap tests analyzed by the laboratory of the Foothills Medical Centre in Calgary, a follow-up reminder program identifies all routine tests resulting in diagnosis of an abnormality, as well as ...technically unsatisfactory and limited normal tests. If laboratory records indicate that the woman has not returned for repeat Pap testing or tissue sampling as recommended by the pathologist,6 the laboratory information system sends a letter to the health care provider who requested the test, seeking information about the recommended follow-up. No follow-up procedure was registered in the laboratory information system for 1500 (approximately 10%) of the routine Pap tests conducted between Jan. 1 and June 30, 1997. A reminder letter was sent to the provider in all of these cases. The 991 replies (66.1% response rate) indicated that for 238 (24.0%) of the women, the recommended follow-up was in fact complete or scheduled (Table 1). Noncompliance with the pathologist's recommendation related mostly to the provider being unable to contact the women (199 women 20.1%) or the women not keeping booked appointments (154 women 15.5%). The letters triggered follow-up for 104 (10.5%) of the women. The overall cost to the laboratory was $0.80 for each letter and $11.59 for each follow-up encounter triggered by the letter. At the time of writing, Dr. Wagner was with the Department of Obstetrics and Gynecology, University of Calgary, Calgary, Alta. Dr. Duggan is with the Departments of Pathology and Laboratory Medicine and of Obstetrics and Gynecology, University of Calgary, and Calgary Laboratory Services, Calgary.
Abridged Context. The young systems PZ Tel and HD 1160, hosting known low-mass companions, were observed during the commissioning of the new planet finder SPHERE with several imaging and ...spectroscopic modes. Aims. We aim to refine the physical properties and architecture of both systems. Methods. We use SPHERE commissioning data and REM observations, as well as literature and unpublished data from VLT/SINFONI, VLT/NaCo, Gemini/NICI, and Keck/NIRC2. Results. We derive new photometry and confirm the nearly daily photometric variability of PZ Tel A. Using literature data spanning 38 yr, we show that the star also exhibits a long-term variability trend. The 0.63-3.8 mic SED of PZ Tel B allows us to revise its properties: spectral type M7+/-1, Teff=2700+/-100 K, log(g)<4.5 dex, log(L/L_Sun)=-2.51+/-0.10 dex, and mass 38-72 MJ. The 1-3.8 mic SED of HD 1160 B suggests a massive brown dwarf or a low-mass star with spectral type M5.5-7.0, Teff=3000+/-100 K, M/H=-0.5-0.0 dex, log(L/L_Sun)=-2.81+/-0.10 dex, and mass 39-168 MJ. We confirm the deceleration and high eccentricity (e>0.66) of PZ Tel B. For e<0.9, the inclination, longitude of the ascending node, and time of periastron passage are well constrained. The system is seen close to an edge-on geometry. We reject other brown dwarf candidates outside 0.25" for both systems, and massive giant planets (>4 MJ) outside 0.5" for the PZ Tel system. We also show that K1-K2 color can be used with YJH low-resolution spectra to identify young L-type companions, provided high photometric accuracy (<0.05 mag) is achieved. Conclusions. SPHERE opens new horizons in the study of young brown dwarfs and giant exoplanets thanks to high-contrast imaging capabilities at optical and near-infrared wavelengths, as well as high signal-to-noise spectroscopy in the near-infrared from low (R~30-50) to medium resolutions (R~350).
GJ758 B is a brown dwarf companion to a nearby (15.76 pc) solar-type, metal-rich (M/H = +0.2 dex) main-sequence star (G9V) that was discovered with Subaru/HiCIAO in 2009. From previous studies, it ...has drawn attention as being the coldest (~600K) companion ever directly imaged around a neighboring star. We present new high-contrast data obtained during the commissioning of the SPHERE instrument at the VLT. The data was obtained in Y-, J-, H-, and Ks-bands with the dual-band imaging (DBI) mode of IRDIS, providing a broad coverage of the full near-infrared (near-IR) range at higher contrast and better spectral sampling than previously reported. In this new set of high-quality data, we report the re-detection of the companion, as well as the first detection of a new candidate closer-in to the star. We use the new 8 photometric points for an extended comparison of GJ758 B with empirical objects and 4 families of atmospheric models. From comparison to empirical object, we estimate a T8 spectral type, but none of the comparison object can accurately represent the observed near-IR fluxes of GJ758 B. From comparison to atmospheric models, we attribute a Teff = 600K \(\pm\) 100K, but we find that no atmospheric model can adequately fit all the fluxes of GJ758 B. The photometry of the new candidate companion is broadly consistent with L-type objects, but a second epoch with improved photometry is necessary to clarify its status. The new astrometry of GJ758 B shows a significant proper motion since the last epoch. We use this result to improve the determination of the orbital characteristics using two fitting approaches, Least-Square Monte Carlo and Markov Chain Monte Carlo. Finally, we analyze the sensitivity of our data to additional closer-in companions and reject the possibility of other massive brown dwarf companions down to 4-5 AU. abridged
The system of four planets around HR8799 offers a unique opportunity to probe the physics and chemistry at play in the atmospheres of self-luminous young (~30 Myr) planets. We recently obtained new ...photometry of the four planets and low-resolution (R~30) spectra of HR8799 d and e with the SPHERE instrument (paper III). In this paper (paper IV), we compare the available spectra and photometry of the planets to known objects and atmospheric models (BT-SETTL14, Cloud-AE60, Exo-REM) to characterize the atmospheric properties of the planets. We find that HR8799d and e properties are well reproduced by those of L6-L8 dusty dwarfs discovered in the field, among which some are candidate members of young nearby associations. No known object reproduces well the properties of planets b and c. Nevertheless, we find that the spectra and WISE photometry of peculiar and/or young early-T dwarfs reddened by submicron grains made of corundum, iron, enstatite, or forsterite successfully reproduce the SED of these two planets. Our analysis confirms that only the Exo-REM models with thick clouds fit (within 2{\sigma}) the whole set of spectrophotometric datapoints available for HR8799 d and e for Teff = 1200 K, log g in the range 3.0-4.5, and M/H=+0.5. The models still fail to reproduce the SED of HR8799c and b. The determination of the metallicity, log g, and cloud thickness are degenerate. We conclude that an enhanced content in dust and decreased CIA of H2 is certainly responsible for the deviation of the properties of the planet with respect to field dwarfs. The analysis suggests in addition that HR8799c and b have later spectral types than the two other planets, and therefore could both have lower masses.
Although controversial, diagnosis of luteal phase defect (LPD) includes the morphological assessment of endometrial development. This study was conducted to determine if refresher training in the ...histological criteria could improve the accuracy and interobserver reproducibility of endometrial dating. Seventy-eight endometrial biopsies were dated by a reference panel of two pathologists and then reviewed twice by a study panel of four pathologists. In the first review, usual practice was applied. Prior to the second review, they studied a standard document of histological criteria. Samples were dated as proliferative, secretory (post-ovulatory day, POD), menstrual, and undatable. Accuracy levels based on the reference dating and agreement levels using kappa values were calculated per review and compared. The kappa for overall dating was 0.683 in the first review and 0.696 in the second. The respective first and second review kappa values were 0.736 and 0.771 for proliferative, and 0.794 and 0.764 for secretory. Amongst those dated as secretory in the first and second reviews, respectively, 31 and 28% were assigned the same POD by any two panellists, 68 and 63% were dated to within 1 day, and 77 and 71% were dated to within 2 days. Accuracy levels per panellist for overall dating were very high in both reviews but were low for individual PODs. Accuracy and interobserver reproducibility were unaffected by refresher training, suggesting the limits of histological dating have been reached.
The nature of the minute amounts of cryoprecipitable proteins present in all normal sera has been investigated in particular relation to the physicochemical and functional properties of the ...precipitated immunoglobulins. Cryoprecipitated material from 48 normal donor sera were first analyzed for their protein, IgG and IgM content. SDS-PAGE analysis revealed many bands in a majority of samples but in about one third a very limited number of bands was observed. IgM, IgG and albumin were identified and a lower molecular weight component (16 KD) was always present. Restricted clonality was demonstrated by IEF in 25-30% of the samples. In 50% of cryoprecipitates IgG was present in higher molecular weight fractions than 7S on sucrose density gradient at neutral pH. Ultracentrifugation at acid pH lead to a dissociation of these IgG fractions in most of the samples. A positive reaction for IgM rheumatoid factor was seen in 63% of the samples and there was a specific enrichment of RF activity in cryoprecipitates as compared to the corresponding serum. These data suggest that the cryoprecipitation of immunoglobulins in normal serum reflects specific interactions between immunoglobulin molecules rather than merely a non-specific precipitation of cold-insoluble molecules.
Context. Astrometric monitoring of directly-imaged exoplanets allows the study of their orbital parameters and system architectures. Because most directly-imaged planets have long orbital periods ...(>20 AU), accurate astrometry is challenging when based on data acquired on timescales of a few years and usually with different instruments. The LMIRCam camera on the LBT is being used for the LEECH survey to search for and characterize young and adolescent exoplanets in L' band, including their system architectures. Aims. We first aim to provide a good astrometric calibration of LMIRCam. Then, we derive new astrometry, test the predictions of the orbital model of 8:4:2:1 mean motion resonance proposed by Goździewski & Migaszewski, and perform new orbital fitting of the HR 8799 bcde planets. We also present deep limits on a putative fifth planet interior to the known planets. Methods. We use observations of HR 8799 and the Theta1 Ori C field obtained during the same run in October 2013. Results. We first characterize the distortion of LMIRCam. We determine a platescale and a true north orientation for the images of 10.707 +/- 0.012 mas/pix and -0.430 +/- 0.076 deg, respectively. The errors on the platescale and true north orientation translate into astrometric accuracies at a separation of 1 of 1.1 mas and 1.3 mas, respectively. The measurements for all planets are usually in agreement within 3 sigma with the ephemeris predicted by Goździewski & Migaszewski. The orbital fitting based on the new astrometric measurements favors an architecture for the planetary system based on 8:4:2:1 mean motion resonance. The detection limits allow us to exclude a fifth planet slightly brighter/more massive than HR 8799 b at the location of the 2:1 resonance with HR 8799 e (~9.5 AU) and about twice as bright as HR 8799 cde at the location of the 3:1 resonance with HR 8799 e (~7.5 AU).
Context. High-contrast imaging is currently the only available technique for the study of the thermodynamical and compositional properties of exoplanets in long-period orbits. The SPICES project is a ...coronagraphic space telescope dedicated to the spectro-polarimetric analysis of gaseous and icy giant planets as well as super-Earths at visible wavelengths. So far, studies for high-contrast imaging instruments have mainly focused on technical feasibility because of the challenging planet/star flux ratio of 10-8-10-10 required at short separations (200 mas or so) to image cold exoplanets. However, the analysis of planet atmospheric/surface properties has remained largely unexplored. Aims. The aim of this paper is to determine which planetary properties SPICES or an equivalent direct imaging mission can measure, considering realistic reflected planet spectra and instrument limitation. Methods. We use numerical simulations of the SPICES instrument concept and theoretical planet spectra to carry out this performance study. Results. We find that the characterization of the main planetary properties (identification of molecules, effect of metallicity, presence of clouds and type of surfaces) would require a median signal-to-noise ratio of at least 30. In the case of a solar-type star \leq 10 pc, SPICES will be able to study Jupiters and Neptunes up to ~5 and ~2 AU respectively. It would also analyze cloud and surface coverage of super-Earths of radius 2.5 RE at 1 AU. Finally, we determine the potential targets in terms of planet separation, radius and distance for several stellar types. For a Sun analog, we show that SPICES could characterize Jupiters (M \geq 30 ME) as small as 0.5 Jupiter radii at ~2 AU up to 10 pc, and super-Earths at 1-2 AU for the handful of stars that exist within 4-5 pc. Potentially, SPICES could perform analysis of a hypothetical Earth-size planet around alpha Cen A and B.
