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Dust extinction curves: KMH94 R_V=5.5 model

This dataset is based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>. Dust Properties Dust grain properties are taken from <a href="http://adsabs.harvard.edu/abs/1994ApJ...422..164K">Kim, Martin, and Hendry (1994)</a>, specifically their model with with RV=3.1 and a full scattering calculation. Stellar Geometry Galactic disks follow exponential profiles in the radial direction, and sech2 distributions in the vertical direction. The vertical scale height is set to a multiple, hd, of the stellar disk scale length, and its value is encoded in each file name. Spheroids follow spherical <a href="http://adsabs.harvard.edu/abs/1990ApJ...356..359H">Hernquist (1990)</a> profiles. Dust Geometry 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, hz, of the stellar disk scale length, and its value is encoded in each file name.

Dust extinction curves: KMH94 HG R_V=5.5 model

This dataset is based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>. Dust Properties Dust grain properties are taken from <a href="http://adsabs.harvard.edu/abs/1994ApJ...422..164K">Kim, Martin, and Hendry (1994)</a>, specifically their model with with RV=3.1 and Henyey-Greenstein scattering. Stellar Geometry Galactic disks follow exponential profiles in the radial direction, and sech2 distributions in the vertical direction. The vertical scale height is set to a multiple, hd, of the stellar disk scale length, and its value is encoded in each file name. Spheroids follow spherical <a href="http://adsabs.harvard.edu/abs/1990ApJ...356..359H">Hernquist (1990)</a> profiles. Dust Geometry 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, hz, of the stellar disk scale length, and its value is encoded in each file name.

Dust extinction curves: Grasil-like

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 mimic the geometries used by <a href="https://adlibitum.oats.inaf.it/silva/grasil/grasil.html">Grasil</a>. Dust Properties Dust grain properties are taken from <a href="http://adsabs.harvard.edu/abs/2003ARA%26A..41..241D">Draine (2003)</a> - specifically their model with either RV=3.1 or RV=5.5 as encoded in the file name with prefix dustD03. Stellar Geometry Galactic disks follow exponential profiles in both radial and vertical directions, with the vertical scale height equal to 0.1 or 0.5 times the radial scale length as encoded in the file name with prefix hzStars. Note that spheroid radii in this work are listed as the scale radius, rs, while <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a> listed the corresponding effective radius, re=rs/1.16. Dust Geometry 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, hz, of the stellar disk scale height. The value of hz is encoded in each file name with prefix hzDust.

Dust extinction curves: Draine R_V=5.5 model

This dataset is based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>. Dust Properties Dust grain properties are taken from <a href="http://adsabs.harvard.edu/abs/2003ARA%26A..41..241D">Draine (2003)</a> - specifically their model with RV=5.5. Stellar Geometry Galactic disks follow exponential profiles in the radial direction, and sech2 distributions in the vertical direction. The vertical scale height is set to a multiple, hd, of the stellar disk scale length, and its value is encoded in each file name. Spheroids follow spherical <a href="http://adsabs.harvard.edu/abs/1990ApJ...356..359H">Hernquist (1990)</a> profiles. Dust Geometry 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, hz, of the stellar disk scale length, and its value is encoded in each file name.

Dust extinction curves: Draine R_V=3.1 model

This dataset is based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>. Dust Properties Dust grain properties are taken from <a href="http://adsabs.harvard.edu/abs/2003ARA%26A..41..241D">Draine (2003)</a> - specifically their model with RV=3.1. Stellar Geometry Galactic disks follow exponential profiles in the radial direction, and sech2 distributions in the vertical direction. The vertical scale height is set to a multiple, hd, of the stellar disk scale length, and its value is encoded in each file name. Spheroids follow spherical <a href="http://adsabs.harvard.edu/abs/1990ApJ...356..359H">Hernquist (1990)</a> profiles. Dust Geometry 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, hz, of the stellar disk scale length, and its value is encoded in each file name.

Dust extinction curves: Draine R_V=4.0 model

This dataset is based on the models described in <a href="https://ui.adsabs.harvard.edu/abs/2018RNAAS...2..188B">Benson (2018)</a>. Dust Properties Dust grain properties are taken from <a href="http://adsabs.harvard.edu/abs/2003ARA%26A..41..241D">Draine (2003)</a> - specifically their model with RV=4.0. Stellar Geometry Galactic disks follow exponential profiles in the radial direction, and sech2 distributions in the vertical direction. The vertical scale height is set to a multiple, hd, of the stellar disk scale length, and its value is encoded in each file name. Spheroids follow spherical <a href="http://adsabs.harvard.edu/abs/1990ApJ...356..359H">Hernquist (1990)</a> profiles. Dust Geometry 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, hz, of the stellar disk scale length, and its value is encoded in each file name.

Dust extinction curves: Ferrara (1999) high resolution

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. However, they are tabulated using a much higher resolution grid of inclinations, optical depths, wavelengths, and morphologies than in <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a>. Dust Properties 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.   Stellar Geometry 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, rs, while <a href="http://adsabs.harvard.edu/abs/1999ApJS..123..437F">Ferrara et al. (1999)</a> listed the corresponding effective radius, re=rs/1.16. Dust Geometry 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, hz, of the stellar disk scale height. The value of hz is encoded in each file name.

Figures 1–10. Termitodius species dorsal habitus and lateral pronotum. 1–2 in Extinct or extant? A new species of Termitodius Wasmann, 1894, (Coleoptera: Scarabaeidae: Aphodiinae: Rhyparini) with a short review of the genus

Figures 1–10. Termitodius species dorsal habitus and lateral pronotum. 1–2) T. coronatus, cotype. 3–4) T. araujoi. 5–6) T. chaki, paratype. 7–8) T. woodruffi, copal paratype. 9–10) T. woodruffi, holotype.

Figures 17–25 in Extinct or extant? A new species of Termitodius Wasmann, 1894, (Coleoptera: Scarabaeidae: Aphodiinae: Rhyparini) with a short review of the genus

Figures 17–25. Images of Termitodius and host. 17) T. woodruffi, paratype, cut open in copal processing, note genitalia inside body (arrow). After photographing, genitalia removed for study. 18–19) T. araujoi male genitalia, caudal and lateral view. 20–21) T. woodruffi male genitalia of paratype in Fig. 17, caudal and lateral view. 22) T. woodruffi with worker host termite. 23) Soldier termite with T. woodruffi. 24–25) T. woodruffi, individual paratypes.

Figures 27–32. Some smaller copal pieces containing T in Extinct or extant? A new species of Termitodius Wasmann, 1894, (Coleoptera: Scarabaeidae: Aphodiinae: Rhyparini) with a short review of the genus

Figures 27–32. Some smaller copal pieces containing T. woodruffi paratypes, host termites and other inclusions. 27) CMNC. 28) REWC. 29–30) CEMT. Scale line = 1 mm. 31) IAvH-E. 32) FSCA (ex. RLBC), arrow indicates male with genitalia extracted, see Fig. 17. Photos for Figures 29–30 by Vinícius Costa-Silva (CEMT).

Figures 11–16 in Extinct or extant? A new species of Termitodius Wasmann, 1894, (Coleoptera: Scarabaeidae: Aphodiinae: Rhyparini) with a short review of the genus

Figures 11–16. Termitodius woodruffi, recent specimen, holotype. 11) Dorsal habitus. 12) Ventral habitus. 13) Lateral habitus. 14) Elytra apex, caudal view. 15) Head, anterior view. 16) Labels.

opencc-zeroMar 2022View details →

dryad40/100

Monitoring demography of resurrected populations of locally extinct and extant species to investigate drivers of species loss

Extinctions are predicted to rise by an order of magnitude over the next century. Although contemporary documented extinctions are uncommon, local extirpations likely provide hints about global extinction risks. Comparing responses to global change of locally extinct versus extant species pairs in a phylogenetic framework could highlight why certain species are more vulnerable to extinction than others and which anthropogenic changes are most relevant to their decline. As anthropogenic changes likely interact to affect population declines, demographic studies partitioning the effects of multifactorial stressors are needed but remain rare. I examine demographic responses to nitrogen addition and deer herbivory, two major drivers of species losses in grasslands, in experimental reintroductions of fourteen locally extinct and extant confamilial native plants from Michigan prairies. Nitrogen consistently reduces survival, especially in locally extinct species, and growth of locally extinct species benefits less from nitrogen than growth of extant species. Nitrogen reduces population growth rates, largely via reductions in survival. Deer herbivory, meanwhile, had inconsistent effects on vital rates among species and did not affect population growth. Nitrogen and herbivory rarely interacted to affect vital rates. These results link community-level patterns of species loss under nitrogen addition to the population-level processes underlying those losses.

Fig. 4 in A New Species Of The Extinct Ant Genus Electromyrmex (Hymenoptera, Formicidae)

Fig. 4. Electromyrmex wheeleri sp. n., line drawing of holotype male based on photo, body in lateral view.

Fig. 8–9 in A New Species Of The Extinct Ant Genus Electromyrmex (Hymenoptera, Formicidae)

Fig. 8–9. Electromyrmex wheeleri sp. n., line drawings of paratype male made based on photos: 8 — body in lateral view, 9 — mandible.

Fig. 5–7 in A New Species Of The Extinct Ant Genus Electromyrmex (Hymenoptera, Formicidae)

Fig. 5–7. Electromyrmex wheeleri sp. n., line drawings of holotype male made based on photos: 5 — head and antennae in lateral view, 6 — forewing, 7 — propodeum, waist and gaster in lateral view.

Fig. 2 in A New Species Of The Extinct Ant Genus Electromyrmex (Hymenoptera, Formicidae)

Fig. 2. Electromyrmex wheeleri sp. n., holotype male, head and antennae in lateral view (photo by E. Martynova).

opencc-by-4.0Sep 2016View details →

Figs 3–4 in Further Data On The Extinct Ant Genus Eocenomyrma (Hymenoptera, Formicidae)

Figs 3–4. Eocenomyrma ukrainica sp. n., line drawings of holotype male made based on photos: 1 — body in dorsal view; 2 — head in dorsal view (sculpture omitted). Scale bar 1 mm.

opencc-by-4.0Sep 2016View details →

Figs 12–13 in Further Data On The Extinct Ant Genus Eocenomyrma (Hymenoptera, Formicidae)

Figs 12–13. Line drawings of Eocenomyrma rugosostriata (Mayr), neotype worker (12, body in dorso-lateral view) and E. elegantula Dlussky et Radchenko, holotype worker (13, body in lateral view). Scale bar 1 mm.

opencc-by-4.0Sep 2014View details →

Fig. 3 in New Extinct Carp Fish Species (Teleostei, Cyprinidae) From The Late Neogene Of Southeastern Europe

Fig. 3. Scardinius ponticus sp. n.: 1 — isolated pharyngeal tooth, holotype (NMNH–P 41/2358, Odesa Pontian Lectostratotype); 2 — paratype (NMNH–P 41/2359). Scardinius erythrophthalmus, recent (used for comparison). Рис. 3. Scardinius ponticus sp. n.: 1 — изолированный глоточный зуб, голотип (NMNH–P 41/2358, лектостратотип понта); 2 — паратип (NMNH–P 41/2359). Scardinius erythrophthalmus, современный (использован для сравнения).