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Figure 2. Sibling pouch young thylacines. A, NMV C5754 in Microscopic analysis of the developing dentition in the pouch young of the extinct marsupial Thylacinus cynocephalus, with an assessment of other developmental stages and eruption
Figure 2. Sibling pouch young thylacines. A, NMV C5754, male specimen sectioned for histology images; B, NMV C 5757, female specimen, used by Feigin et al. (2018) for genomic analysis.
Figure 14 in Microscopic analysis of the developing dentition in the pouch young of the extinct marsupial Thylacinus cynocephalus, with an assessment of other developmental stages and eruption
Figure 14. Images of the head, skull, and dentition of the thylacine pouch young from the Australian Museum (AM P 762). A, X-ray of the skull, showing deciduous and successional teeth in varying stages of development and early eruption; B, Head and upper body of the pouch young, prior to X-ray analysis; C, Higher magnification of a portion of the X-ray shown in figure A, with emphasis on the erupted lower dp3, and the unerupted but larger successional p3 immediately anterior to it.
Calibration-free reaction yield quantification by HPLC with a machine-learning model of extinction coefficients
<p>This repository contains all the data and code associated with the manuscript "Calibration-free reaction yield quantification by HPLC with a machine-learning model of extinction coefficients"</p> <p>Mass spec and absorption chromatogram data are in reaction_set_1.zip, reaction_set_2.zip, and simulated_reaction_set.zip. The chemprop model trained on the Deep4Chem dataset is in Deep4Chem_chemprop.zip.</p>
Figure 4. Longitudinal section through I4 and transverse section through smaller I3. e in Microscopic analysis of the developing dentition in the pouch young of the extinct marsupial Thylacinus cynocephalus, with an assessment of other developmental stages and eruption
Figure 4. Longitudinal section through I4 and transverse section through smaller I3. e, disrupted enamel.
Figure 5 in Population biology of the freshwater shrimp Atya scabra (Leach, 1816) (Crustacea: Decapoda) in São Francisco River, Brazil: evidence from a population at risk of extinction
Figure 5. Atya scabra (Leach, 1816). (A) Relationship between sampling month and number of individuals; (B) monthly variation in the number of individuals (average ± SD) and mean flow (m3/s) and (C) monthly variation in number of ovigerous females (average ± SD) and mean rainfall (mm) during the sampling period.
Figure 4 in Population biology of the freshwater shrimp Atya scabra (Leach, 1816) (Crustacea: Decapoda) in São Francisco River, Brazil: evidence from a population at risk of extinction
Figure 4. Atya scabra (Leach, 1816). (A) Proportion of adult ovigerous and non-ovigerous females and (B) sex ratio (estimate ± SE) during the months sampled. In (B), the black square indicates a deviation from a 1:1 sex ratio.
Figure 1 in Population biology of the freshwater shrimp Atya scabra (Leach, 1816) (Crustacea: Decapoda) in São Francisco River, Brazil: evidence from a population at risk of extinction
Figure 1. (A) Dorsal and (B) lateral view of Atya scabra (Leach, 1816) captured on the São Francisco River, Sergipe, Brazil (Photo: Alves, DFR).
Figure 3 in Population biology of the freshwater shrimp Atya scabra (Leach, 1816) (Crustacea: Decapoda) in São Francisco River, Brazil: evidence from a population at risk of extinction
Figure 3. Atya scabra (Leach, 1816). Size-frequency distribution of carapace length (mm) of the male and female shrimp sampled in São Francisco River, Sergipe, Brazil.
Figure 2 in Population biology of the freshwater shrimp Atya scabra (Leach, 1816) (Crustacea: Decapoda) in São Francisco River, Brazil: evidence from a population at risk of extinction
Figure 2. Map of Brazil indicating the São Francisco River watershed. Inset: sampling site (black circle) and the region of the Xingó Reservoirs (white circle). Legend: MG–Minas Gerais; BA–Bahia; SE–Sergipe; AL–Alagoas; PE–Pernambuco.
The data catalog for Metallicity and alpha-abundance for 48 million stars in low-extinction regions in the Milky Way
<p>Stellar chemistry contains information on the environment in which the star was born. Therefore, measuring the chemical abundances of stars in the Milky Way, such as the overall metallicity [M/H] and the alpha-abundance [alpha/M], is essential in Galactic astronomy.</p> <p>We estimate ([M/H], [alpha/M]) for giants and dwarfs in low dust extinction region from the Gaia DR3 XP spectra by using tree-based machine-learning models trained on APOGEE DR17 (Abdurro’uf et al. 2022) and the metal-poor star sample of Li et al. (2022).</p> <p>Here, we upload the catalogues of ([M/H], [alpha/M]) for 182 million stars. The data are divided into 10 fits files. The i-th file (i=1,2,...,10) contains stars with E(B-V) value between 0.1*(i-1) and 0.1*i. Because our machine-learning models are trained on stars with low dust extinction (E(B-V)<0.1), we recommend using 48 million stars with low-dust extinction region with 0<E(B-V)<0.1 (table_light_mh_am_0p0ebv0p1.fits). The description for each column of the data is shown in column_description.png. </p> <p>The source paper of this catalog:</p> <ul> <li>Kohei Hatori "Metallicity and alpha-abundance for 48 million stars in low-extinction regions in the Milky Way" <br>https://iopscience.iop.org/article/10.3847/1538-4357/ad9686</li> </ul> <p>References:</p> <div> <div> <div> <ul> <li>Abdurro’uf, Accetta, K., Aerts, C., et al. 2022, ApJS, 259, 1026 35, doi: 10.3847/1538-4365/ac4414</li> </ul> </div> </div> </div> <ul> <li>Li, H., Aoki, W., Matsuno, T., et al. 2022, ApJ, 931, 147, doi: 10.3847/1538-4357/ac6514</li> </ul> <p> </p>
Figure 2 in The dentition of the extinct megamouth shark, (Lamniformes: Megachasmidae), from southern California, USA, based on geometric morphometrics
Figure 2. Homologous landmark (numbered black or white circles) and semi-homologous landmark (red circles with asterisk [*] connected by red lines) on tooth samples of Megachasma applegatei (A), M. pelagios (B), and Odontaspis ferox (C) for principal component analysis (not to scale). Seven homologous landmarks: 1, the crown apex, 2 and 3, right- and left-most extremities of the crown; 4, apical-most point around the middle of the crown base; 5 and 6, basal extremity of each of the two root lobes; and 7, apical-most point of the basal root concavity.
Figure 3. A in The dentition of the extinct megamouth shark, (Lamniformes: Megachasmidae), from southern California, USA, based on geometric morphometrics
Figure 3. A. Scatter plot diagram showing principal component analysis of 207 teeth of Megachasma applegatei (black plots) compared with all 178 teeth of extant M. pelagios (red plots), and all 78 teeth of extant Odontaspis ferox separated into tooth types using different colors (symphysial teeth = green; anterior teeth = dark blue; intermediate teeth = purple; lateral teeth = brown). B. Scatter plot diagram exclusively of M. applegatei, showing examples of actual specimens (not to scale) represented by certain plots (illustrated teeth: LACM 9883, 150907, 155340, 155348, 155357, 155373, 155393, 155424, 155434, 155456, 155563, 155622, 155630, 155651, 155653, 155694, and 155700). C. Scatter plot diagram exclusively of M. pelagios, showing examples of actual specimens (not to scale: see Fig. 1C, D) represented by certain plots. D. Scatter plot diagram exclusively of O. ferox, showing examples of actual specimens (not to scale: see Fig. 1F) represented by certain plots. Asterisk (*): on axes in B and C = PC1 and PC2 originally labeled inversely by the software (see text for detail); by photograph of teeth in C-D = Upper teeth.
Figure 1. A in The dentition of the extinct megamouth shark, (Lamniformes: Megachasmidae), from southern California, USA, based on geometric morphometrics
Figure 1. A. Generalized consensus tree of extant lamniform families on the basis of molecular-based phylogenetic studies, highlighting Megachasmidae in bold (see Stone and Shimada 2019, fig. 6, and references therein). B. Extant megamouth shark, Megachasma pelagios (after Compagno 1984). C, D. Right upper (C) and right lower (D) teeth of extant M. pelagios (BPBM 22730, 446 cm TL, male) in (from top row to bottom row) lingual, labial, mesial, apical, and basal views, showing strong tendency towards homodonty. E. Extant smalltooth sand tiger, Odontaspis ferox (after Compagno 1984). F. Left upper and left lower dental series of extant O. ferox (BPBM 9335, 297(?) cm TL, male(?)) showing representative 'lamnoid tooth pattern' (A or a = anterior teeth; I or i = intermediate tooth; L or l = lateral tooth; S or s = symphysial tooth). Scale bars: B and E = 50 cm; C, D, F = 5 mm
Figure 4 in The dentition of the extinct megamouth shark, (Lamniformes: Megachasmidae), from southern California, USA, based on geometric morphometrics
Figure 4. Three reconstructed dentitions of Megachasma applegatei under three different assumptions (see text for detail). A. Artificial dentition based on Odontaspis ferox as a model. B. Artificial dentition depicted as intermediate between O. ferox and M. pelagios. C. Artificial dentition based on M. pelagios as a model. Scale bar = 5 mm (note: each scale bar applies to each respective dentition consisting of teeth with digitally adjusted sizes [see text]).
How to render species comparable taxonomic units through deep time: A case study on intraspecific osteological variability in extant and extinct lacertid lizards
<p>Generally, the species is considered to be the only naturally occurring taxon. However, species recognized and defined using different species delimitation criteria cannot readily be compared, impacting studies of biodiversity through Deep Time. This comparability issue is particularly marked when comparing extant with extinct species because the only available data for species delimitation in fossils are derived from their preserved morphology, which is generally restricted to osteology in vertebrates. Here, we quantify intraspecific, intrageneric, and intergeneric osteological variability in extant species of lacertid lizards using pairwise dissimilarity scores based on a data set of 253 discrete osteological characters for 99 specimens referred to 24 species. Variability is always significantly lower intraspecifically than between individuals belonging to distinct species of a single genus, which is in turn significantly lower than intergeneric variability. Average values of intraspecific variability and associated standard deviations are consistent (with few exceptions), with an overall average within a species of 0.208 changes per character scored. Application of the same methods to six extinct lacertid species (represented by 40 fossil specimens) revealed that intraspecific osteological variability is inconsistent, which can at least in part be attributed to different researchers having unequal expectations of the skeletal dissimilarity within species units. Such a divergent interpretation of intraspecific and interspecific variability among extant and extinct species reinforces the incomparability of the species unit. Lacertidae is an example where extant species recognized and defined based on a number of delimitation criteria show comparable and consistent intraspecific osteological variability. Here, as well as in equivalent cases, application of those skeletal dissimilarity values to paleontological species delimitation potentially provides a way to ameliorate inconsistencies created by the use of morphology to define species.</p>
Figure 1 in A revision of the extinct Mesozoic family Prochydoridae Smirnov, 1992 (Crustacea: Cladocera) with a discussion of its phylogenetic position
Figure 1. Drawings of Upper Mesozoic Prochydoridae based on SEM photographs. A, Prochydorus rotundus from Khotont, reconstruction based on a series of specimens. B, antenna II of holotype, PIN 4307/2040. C, specimen PIN 4307/2031 from Khotont, antenna II. D, Archeoxus mirabilis from Khotont, reconstruction based on a series of specimens. E, antenna II of specimen PIN 4307/2018. F, 'Archeoxus' vetrosus from Khotont, antenna II of holotype PIN 4307/2027. G, Palaeorak scherbakovi gen. nov., sp. nov. from Khasurty, holotype 5026/178. H, reconstruction of general view based on series of specimens. I, postabdominal claw, 5026/177. J, antenna II, 5026/179. Scale bars: 1 mm.
Figure 3 in A revision of the extinct Mesozoic family Prochydoridae Smirnov, 1992 (Crustacea: Cladocera) with a discussion of its phylogenetic position
Figure 3. SEM micrographs of Upper Mesozoic Prochydoridae from Khotont. A, B, Prochydorus rotundus, PIN 4307/ 2013, general view and head. C, PIN 4307/2041, antenna II and mandible. D–F, specimen PIN 4307/2031, general view, anterior body portion and antenna II. G, H, Archeoxus ventrosus, holotype PIN 4307/2027, general view and antenna II. Scale bars: A, C–E, G, 1 mm; B, F, H, 0.1 mm.
Figure 2 in A revision of the extinct Mesozoic family Prochydoridae Smirnov, 1992 (Crustacea: Cladocera) with a discussion of its phylogenetic position
Figure 2. SEM micrographs of Prochydorus rotundus from Khotont, Mongolia. A–D, holotype PIN 4307/2024, general view, postabdominal claws, antenna II and apical segment of its exopod. E, holotype PIN 4307/2040 (counter-impression). F, G, paratype PIN 4307/2019, general view and mandibles. H, paratype PIN 4307/2020. Scale bars: A, F, H, 1 mm; B–E, G, 0.1 mm.
Too hot for the devil? Did climate change cause the mid-Holocene extinction of the Tasmanian devil (Sarcophilus harrisii) from mainland Australia?
<p>The possible role of climate change in late Quaternary animal extinctions is hotly debated, yet few studies have investigated its direct effects on animal physiology to assess whether past climate changes might have had significant impacts on now-extinct species. Here we test whether climate change could have imposed physiological stress on the Tasmanian devil (Sarcophilus harrisii) during the mid-Holocene, when the species went extinct on mainland Australia. Physiological values for the devil were quantified using mechanistic niche models of energy and water requirements for thermoregulation, and soil-moisture-based indices of plant stress from drought to indirectly represent food and water availability. The spatial pervasiveness, extremity, and frequency of physiological stresses were compared between a period of known climatic and presumed demographic stability (8000-6010 BP) and the extinction period (5000-3010 BP). We found no evidence of widespread negative effects of climate on physiological parameters for the devil on the mainland during its extinction window. This leaves cultural and demographic changes in the human population or competition from the dingo (Canis dingo) as the main contending hypotheses to explain mainland loss of the devil in the mid-Holocene.</p>
Dust extinction curves: Ferrara (1999) original resolution
<p>These datasets are based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>, and are intended to closely match the models run by <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a> - they use the same dust grain properties and galactic geometry. Additionally, they are tabulated at the same inclinations, optical depths, wavelengths, and morphologies as in <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a>.</p> <p><strong>Dust Properties</strong></p> <p>Dust grain albedos, scattering asymmetries, and opacities to extinction are taken from <a href="http://adsabs.harvard.edu/abs/1997ApJ...487..625G">Gordon et al. (1997)</a>, for either their Milky Way, “MW”, or Small Magellanic Cloud, “SMC”, models (as encoded in each file name), and assume Henyey-Greenstein scattering.</p> <p> </p> <p><strong>Stellar Geometry</strong></p> <p>Galactic disks follow exponential profiles in both radial and vertical directions, with the vertical scale height equal to 0.0875 times the radial scale length. Spheroids follow spherical <a href="http://adsabs.harvard.edu/abs/1983MNRAS.202..995J">Jaffe (1983)</a> profiles. Note that spheroid radii in this work are listed as the scale radius, <em>r</em><sub>s</sub>, while <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a> listed the corresponding effective radius, <em>r</em><sub>e</sub>=<em>r</em><sub>s</sub>/1.16.</p> <p><strong>Dust Geometry</strong></p> <p>Dust is distributed in the disk, and follows exponential profiles in both radial and vertical directions. The vertical scale height is set to a multiple, <em>h</em><sub>z</sub>, of the stellar disk scale height. The value of <em>h</em><sub>z</sub> is encoded in each file name.</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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