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993 results for “T Dwarfs”
F I G U R E 5 in Turcinoemacheilus ekmekciae, a new dwarf loach from upper Tigris and Euphrates (Teleostei: Nemacheilidae)
F I G U R E 5 Sampling sites where Turcinoemacheilus specimens found in upper Tigris-Euphrates: Habitat of T. kosswigi, (a) Eziki stream: Habitats of T. minimus, (b) Göksu River, (c) Kahta stream: Habitats of T. ekmekciae, (d) Çıratan stream, (e) Destumi stream, (f) Nerduş stream, (g) Sason stream, (h) Kesan stream, and (i) Kaynarca stream.
F I G U R E 4 in Turcinoemacheilus ekmekciae, a new dwarf loach from upper Tigris and Euphrates (Teleostei: Nemacheilidae)
F I G U R E 4 Turcinoemacheilus ekmekciae, paratypes; FFR 3616, from the top, 45 mm standard length (SL); 39 mm SL, Nerduş stream: FFR 3618, 30 mm SL; 30 mm SL; Sason stream.
F I G U R E 6 in Turcinoemacheilus ekmekciae, a new dwarf loach from upper Tigris and Euphrates (Teleostei: Nemacheilidae)
F I G U R E 6 The distribution range of Turcinoemacheilus spp. in Western Asia (top). Maximum likelihood (ML) estimation of the phylogenetic relationships (bottom) based on the mitochondrial cytochrome c oxidase subunit 1 (COI) barcode region (Kimura 2-parameter (K2P) model, discrete gamma distribution for rate differences with five categories +G parameter = 0.1859). Nucleotide positions with less than 98% site coverage were eliminated, resulting in 540 analysed positions. Numbers of major nodes indicate bootstrap values of 1000 pseudoreplicates from the ML, MP, and NJ methods. "X" indicates the highest possible support from all three methods (>95). Blue bars to the right of the specimen labels indicate species boundary outcomes from the Poisson tree processes (PTP) followed by the results of the multi-rate PTP (mPTP) approach and the assemble species by automatic partitioning (ASAP) method at the rightmost.
F I G U R E 3 Turcinoemacheilus ekmekciae, FFR 3603 in Turcinoemacheilus ekmekciae, a new dwarf loach from upper Tigris and Euphrates (Teleostei: Nemacheilidae)
F I G U R E 3 Turcinoemacheilus ekmekciae, FFR 3603, paratypes, from the top, 54 mm standard length (SL); 51 mm SL; 51 mm SL; 48 mm SL; Çıratan stream.
Figs 33-44 in A mysterious dwarf: Suthepiidae nov. fam., a new harvestman family from mountains of northern Thailand (Arachnida: Opiliones: Laniatores)
Figs 33-44. Suthepia inermis sp. nov., male holotype (33-38), female paratype (39-44). (33) Penis in dorsal view. (34) Same in ventral view. (35-36) Same in lateral view. (37, 39) Right chelicera, prolateral view. (38, 40) Same in retrolateral view. (41) Whole ovipositor, ventral view. (42) Distal part of ovipositor, ventral view. (43-44). (43) Single claw of leg I of female, retrolateral view. (44) Double claw of leg IV of female, retrolateral view. Scale lines: 0.3 mm (33-36; 37-41), 0.05 mm (42), 0.07 mm (43-44).
Figs 3-8 in A mysterious dwarf: Suthepiidae nov. fam., a new harvestman family from mountains of northern Thailand (Arachnida: Opiliones: Laniatores)
Figs 3-8. Suthepia inermis sp. nov, male holotype (3, 5-6), female paratype. (4, 7-8). (3-4) Habitus, lateral view. (5, 7) Habitus, dorsal view, (6, 8) Habitus, ventral view. Scale line 0.5 mm.
Figs 17-32 in A mysterious dwarf: Suthepiidae nov. fam., a new harvestman family from mountains of northern Thailand (Arachnida: Opiliones: Laniatores)
Figs 17-32. Suthepia inermis sp. nov., male paratype (17-20, 25-28), female paratype (21-24, 29-32). (17-24) Femora I-IV, retrolateral view. (25-32) Tarsi I-IV, retrolateral view. Scale lines 0.3 mm.
Figs 9-16 in A mysterious dwarf: Suthepiidae nov. fam., a new harvestman family from mountains of northern Thailand (Arachnida: Opiliones: Laniatores)
Figs 9-16. Suthepia inermis sp. nov., pedipalps of male holotype (9-12) and of female paratype (13-16). (9, 13) Right pedipalp, retrolateral view. (10, 14) Same, prolateral view. (11, 15) Right pedipalpal tarsus, retrolateral view. (12, 16) Same, prolateral view. Scale lines 0.3 mm.
Figs 1-2 in A mysterious dwarf: Suthepiidae nov. fam., a new harvestman family from mountains of northern Thailand (Arachnida: Opiliones: Laniatores)
Figs 1-2. Suthepia inermis sp. nov., body in dorsal view. (1) Female paratype. (2) Male holotype. Scale line 0.5 mm. Photograph by J. Severin.
FIG. 1 in A new dwarf pseudosquillid of the genus Raoulserenea from French Polynesia (Crustacea, Stomatopoda)
FIG. 1. — Raoulserenea pygmaea, n. sp. Female holotype, tl 33 mm; A, anterior part of body and raptorial claw; B, sixth abdominal somite, telson, and uropod; C, endopod of first pleopod of male paratype, tl 25 mm. Scale bar: A, B,1 mm; C, 0.5 mm.
An extended stellar halo discovered in Fornax dwarf spheroidal using Gaia EDR3
<p>We provide the catalog of Fornax member candidate, including the three final samples, as well as the data of surface density profiles, see the example python code of loading the data, as well as the explanation of each quantity.</p>
Data from: Applied phenomics and genomics for improving barley yellow dwarf resistance in winter wheat
<div> <div> <p>Barley yellow dwarf is one of the major viral diseases of cereals. Phenotyping barley yellow dwarf in wheat is extremely challenging due to similarities to other biotic and abiotic stresses. Breeding for resistance is additionally challenging as the wheat primary germplasm pool lacks genetic resistance, with most of the few resistance genes named to date originating from a wild relative species. The objectives of this study were to (1) evaluate the use of high-throughput phenotyping to improve barley yellow dwarf assessment; (2) identify genomic regions associated with barley yellow dwarf resistance, and (3) evaluate the ability of genomic selection models to predict barley yellow dwarf resistance. Up to 107 wheat lines were phenotyped during each of 5 field seasons under both insecticide treated and untreated plots. Across all seasons, barley yellow dwarf severity was lower within the insecticide treatment along with increased plant height and grain yield compared with untreated entries. Only 9.2% of the lines were positive for the presence of the translocated segment carrying the resis- tance gene Bdv2. Despite the low frequency, this region was identified through association mapping. Furthermore, we mapped a poten- tially novel genomic region for barley yellow dwarf resistance on chromosome 5AS. Given the variable heritability of the trait (0.211–0.806), we obtained a predictive ability for barley yellow dwarf severity ranging between 0.06 and 0.26. Including the presence or absence of Bdv2 as a covariate in the genomic selection models had a large effect for predicting barley yellow dwarf but almost no effect for other ob- served traits. This study was the first attempt to characterize barley yellow dwarf using field-high-throughput phenotyping and apply geno- mic selection to predict disease severity. These methods have the potential to improve barley yellow dwarf characterization, additionally identifying new sources of resistance will be crucial for delivering barley yellow dwarf resistant germplasm.</p> </div> </div>
A gap in the double white dwarf separation distribution caused by the common-envelope evolution: astrometric evidence from Gaia
<p>Here we provide a supplementary dataset to our publication <em>A gap in the double white dwarf separation distribution caused by the common-envelope evolution: astrometric evidence from Gaia,</em> <a href="https://arxiv.org/abs/2203.03659">arXiv:2203.03659</a>. The dataset consists of 119 double white dwarf candidates selected in the Gaia Early Data Release 3 (EDR3) based on the sources' astrometric wobble amplitude. For each candidate we provide sky coordinates (RA, DEC), Gaia EDR3 ID, position on the HR diagram (G, BP-RP) and estimated astrometric wobble amplitude (delta a). Note that the astrometric wobble amplitude (delta a) is directly related to the binary’s orbital separation, as detailed in our paper.</p>
SED templates for "Dwarf AGNs from Variability for the Origins of Seeds (DAVOS): Intermediate-mass black hole demographics from optical synoptic surveys"
<p>FITS file containing the pre-computed grid of Done or Nemmen model SEDs. See Table 2 in the publication for details.</p>
Probing the Extent of Vertical Mixing in Brown Dwarf Atmospheres with Disequilibrium Chemistry
<p><strong>OVERVIEW</strong></p> <p>The substellar atmospheric models described in <a href="https://ui.adsabs.harvard.edu/abs/2022arXiv220814317M/abstract">Mukherjee et al. (2022)</a> are presented here. The grid of these 1D radiative-convective atmospheric models was computed using the newly released open-source climate code PICASO 3.0 (<a href="https://ui.adsabs.harvard.edu/abs/2022arXiv220807836M/abstract">Mukherjee et al. (2022)</a>, <a href="https://ui.adsabs.harvard.edu/abs/2019ApJ...878...70B/abstract">Batalha et al. (2019)</a>). The grid consists of four parameters – the effective temperature (T<sub>eff</sub>), gravity (log(g)), K<sub>zz</sub> in the radiative zones, and mixing length in the convective zones. Models with T<sub>eff </sub> between 400-1000 K with an increment of 25 K are included. log(g) has been varied from 4.5 to 5.5 with an increment of 0.25 dex. The K<sub>zz</sub> in the radiative zone has been varied between 1x, 0.01x, and 100x the parametrization presented in <a href="https://ui.adsabs.harvard.edu/abs/2022ExA....53..279M/abstract">Moses et al. (2021)</a>, whereas the convective mixing length has been between the atmospheric pressure scale height and 0.1x the scale height.</p> <p>There are three types of files released here – atmospheric composition files (TP_chemistry), thermal emission spectra files (spectra), and atmospheric Kzz profile files (TP_kz). </p> <p><strong>ATMOSPHERIC COMPOSITION</strong></p> <p>The atmospheric composition files are located in the folder TP_chemistry. These files have the temperature structure of the atmosphere as a function of pressure accompanied by the volume mixing ratio of 37 gases as a function of pressure. </p> <p>The TP_chemistry files are named following the format “profile_sc_qt_rz_[factor1]_cz_[factor2]_[Teff]_grav_[gravity]_mh_+0.0_sm_NA.dat", where [factor1] denotes the multiplier used for the radiative zone Kzz and can vary between ‘x0pt01’, ‘x1’, and ‘x100’. [factor2] denotes the multiplier for the mixing length and can vary between ‘1’ and ‘0pt1’. [Teff] and [gravity] denote the Teff and gravity of the models used. A simple code snippet to read and plot these files is presented below.</p> <p><strong>SPECTRA</strong></p> <p>The spectra files are located in the folder "spectra_highres_1", "spectra_highres_2", "spectra_highres_3", and "spectra_highres_4". These files have the thermal emission spectra between 0.3-30 microns calculated using the computed models. The native spectral resolution of these calculations is at an R = 500,000, but <strong>please be aware that these spectra should always be binned down to a resolution of R = 50,000 or less before usage</strong>. This means that these spectra should only be used to interpret datasets with a spectral resolution of 50,000 or less. Please contact the authors if higher resolution spectra are needed. The spectra have been uploaded in three different folders to make the file sizes manageable for transfer.</p> <p>The spectra files are also similarly named using the format “spectra_sc_qt_rz_[factor1]_cz_[factor2]_[Teff]_grav_[gravity]_mh_+0.0_sm_NA.tar.gz". These files can be directly read into a Python pandas dataframe using </p> <pre><code class="language-python">pd.read_csv(filename, compression='gzip')</code></pre> <p> The first column of the file is wavenumbers in cm<sup>-1, </sup>which can be converted to wavelength in microns by wavelength [microns] =10000/wavenumbers[cm<sup>-1</sup>]. The second column of the file is flux in erg/s/cm<sup>2</sup>/cm. Note that these fluxes need to be multiplied with R<sup>2</sup>/D<sup>2</sup> before comparing them with the typically observed flux of brown dwarfs/exoplanets. R is the radius of the object, and D is the distance here. A tutorial to convert these fluxes to other units is present in <a href="https://natashabatalha.github.io/picaso/notebooks/6_BrownDwarfs.html#Convert-to-F_\nu-Units-and-Regrid">this link</a>. A binned-down version (R=15,000) of these high-resolution spectra can also be found in the "spectra_lowres" folder. These can be used for datasets that have a maximum spectral resolution of 15,000.</p> <p><strong>K<sub>zz</sub> PROFILE</strong></p> <p>The K<sub>zz </sub>as a function of pressure for each model is presented in these files. The K<sub>zz</sub> is reported in cm<sup>2</sup>/s. These files are also similarly named using the format “kz_sc_qt_rz_[factor1]_cz_[factor2]_[Teff]_grav_[gravity]_mh_+0.0_sm_NA.dat". The columns of the files are pressure in bars, the temperature in K, and Kzz in cm<sup>2</sup>/s.</p> <p> </p> <p><strong>EXAMPLE PYTHON CODE TO READ AND PLOT COMPOSITION FILES</strong></p> <pre><code class="language-python">import numpy as np import pandas as pd import matplotlib.pyplot as plt grav = np.array([316,562,1000,1780,3160]) Teff=np.array([400,425,450,475,500,525,550,575,600,625,650,675,700,725,750,775,800,825,850,875,900,925,950,975,1000]) factor1 = np.array(['x0pt01','x1','x100']) factor2 = np.array(['1','0pt1']) file ="profile_sc_qt_rz_"+factor1[0]+"_cz_"+factor2[0]+"_"+str(Teff[14])+"_grav_"+str(grav[14])+"_mh_+0.0_sm_NA.dat" df = pd.read_csv(file, sep="\t") # Plot T(P) profile plt.ylim(100,1e-4) plt.semilogy(df['temperature'],df['pressure']) plt.show() # Plot H2O mixing ratio profile plt.ylim(100,1e-4) plt.loglog(df['H2O'],df['pressure']) plt.show()</code></pre> <p><strong>CREDITS</strong></p> <p>If you use these tables, please cite <a href="https://ui.adsabs.harvard.edu/abs/2022arXiv220814317M/abstract">Mukherjee et al. (2022, Astrophysical Journal, in press.)</a></p> <p> </p>
Figure 3 in Designation of a Neotype for the Dwarf Sea Hare Aplysia concava G. B. Sowerby I, 1833, and a Review of the Status of Aplysia norfolkensis G. B. Sowerby II, 1869 (Mollusca: Heterobranchia)
Figure 3. Light microscope image of Aplysia norfolkensis shell, (a) dorsal view, (b) ventral view, specimen AMS C.55733, collected by Brazier, J., 25 June 1892, Bradleys Head, Port Jackson, Sydney, NSW, Australia. Photograph: M. Nimbs.
Figure 2 in Designation of a Neotype for the Dwarf Sea Hare Aplysia concava G. B. Sowerby I, 1833, and a Review of the Status of Aplysia norfolkensis G. B. Sowerby II, 1869 (Mollusca: Heterobranchia)
Figure 2. Original descriptions and figure illustrations of shells for Aplysia concava G. B. Sowerby I, 1833: vol. 2, p. 243, pl. 235, figs 24a,b; and Aplysia norfolkensis G. B. Sowerby II, 1869: vol. 17, p. 216, pl. 10, figs 42a,b. Sourced from Biodiversity Heritage Library, (see Sowerby I, 1833; Sowerby II, 1869).
Figure 1 in Designation of a Neotype for the Dwarf Sea Hare Aplysia concava G. B. Sowerby I, 1833, and a Review of the Status of Aplysia norfolkensis G. B. Sowerby II, 1869 (Mollusca: Heterobranchia)
Figure 1. Photograph of living neotype of Aplysia concava, specimen AMS C.574820, Newcastle, NSW, Australia, collected 14 December 2016, by Stephen D. A. Smith. Photograph: M. Nimbs.
Near-Infrared Spectral Templates of L Dwarfs
<p>As described in <em>Meeting the Cool Neighbors XII: An Optically-Anchored Analysis of the Near-Infrared Spectra of L Dwarfs</em> (Cruz et. al.), we have combined the NIR spectra of objects of the same optical spectral type to make NIR spectral average templates for field and low-gravity L dwarfs at each integer spectral type, in the range L0–L8. As more optical and/or NIR data are collected for L dwarfs, the templates could potentially be updated. In anticipation of this, we dub the templates presented here version 1.0.</p> <p>The naming convention of the ascii files is the following:</p> <p>Spectral type + Band + Gravity<br> <br> Gravity can be <br> 'f' (field objects) or <br> 'b' ({beta}-type low-gravity objects) or <br> 'g' ({gamma}-type very low-gravity objects)<br> <br> Example: L1H_f.txt is the template for the H band of the field L1 objects.<br> <br> Columns are:<br> 1. Wavelength in microns<br> 2. Average normalized flux<br> 3. Normalized flux standard deviation<br> 4. Min normalized flux<br> 5. Max normalized flux <br> The last two columns define the range of the strip at each wavelength.<br> <br> The files are formatted according to the machine readable format used by the AAS Journals and CDS/VizieR. The files can be read in python using the astropy package:<br> <br> from astropy.table import Table<br> data = Table.read("L1H_f.dat", format="ascii.cds")</p>
Light Curve and Target Data for "M-Dwarf Flare Candidates Simultaneously Observed by K2 and TESS"
<p>This repository contains light curves and data from the study conducted in the research note titled "M-Dwarf Flare Candidates Simultaneously Observed by K2 and TESS".</p> <p>Each file contains a light curve (produced outputs from PyVAN (<a href="https://ui.adsabs.harvard.edu/abs/2019AJ....158..119L/abstract" rel="nofollow">https://ui.adsabs.harvard.edu/abs/2019AJ....158..119L/abstract</a>, <a href="https://github.com/kdlawson/pyvan">https://github.com/kdlawson/pyvan</a>), modfied to easily distinguish between K2/TESS data) for each target flagged with a flaring event. Files titled #T indicate TESS data and #K indicates K2 data. </p> <p>Overlap plots are included (titled Shape#) for those which were clearly defined by TESS, but not seen by K2.</p> <p>See Table 1 for specific target identification and measurements.</p> <p>Targets 11, 20, 27, and 28 saw K2 detections that we believe to be false positives based on lack of structure and substanstial supporting evidence from TESS.</p> <p>Finally a .csv is included with the information for all targets observed in this study.</p>
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Allen Brain Atlas
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International Brain Laboratory public data
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OpenNeuro
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