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opencc-by-4.0Dec 2003View details →

Figure 4 in A powerful new light source for ultraviolet detection of scorpions in the field

Figure 4: Excitation spectrum of a blacklight tube and fluorescence spectrum of the scorpion cuticle. The data were recorded with a scanning spectrometer during blacklight illumination of Hadrurus obscurus (Iuridae). The broad peak below 400 nm and the discrete Hg lines correspond to the tube emission (F6T5/BLB, Sylvania), and the broad peak in the visible region (450-550 nm) corresponds to the blue-green fluorescence of the scorpion. This visible peak disappeared when the scorpion was removed and only light from the BLB tube was scanned. Identically shaped 450- 550 nm fluorescence spectra were obtained from Paruroctonus silvestrii and Paruroctonus becki (Vaejovidae), which suggests that the chemistry of fluorescence is conserved across different scorpion families. We therefore expect that UV detection results presented here will be applicable to a wide variety of scorpion taxa. We did not record the UV LED spectrum. Typical published spectra for these devices peak sharply at the rated wavelength of 395 nm, with 50% peak widths of only about 20 nm.

opencc-by-4.0Dec 2003View details →

Figure 3 in A powerful new light source for ultraviolet detection of scorpions in the field

Figure 3: Comparison of scorpion fluorescence excited by different light sources. The pair of CCD camera images show a Vaejovis confusus illuminated by (A) a fluorescent lamp equipped with two 15 W BLB tubes (2.3 A current), and (B) a 168-diode UV LED array (1.8 A current). The scorpion fluorescence in (B) was attenuated 10.5-fold by a neutral density filter to prevent CCD saturation, so it appears equally bright in this picture. Scale bar: 15 mm.

opencc-by-4.0Dec 2003View details →

Figure 1 in A powerful new light source for ultraviolet detection of scorpions in the field

Figure 1: Circuit diagram of the prototype LED array. The array has a scalable architecture, here with N = 56 parallel branches. Each branch includes three LEDs in series with a single current-limiting resistor (Rs = 39 Ω). Typical forward voltage drop measured across one diode was 3.4 V, giving a total diode drop of 10.2 V in each branch. During operation, voltage across the 12 V battery terminals was Vb = 11.5 V, so the current in each branch was (11.5-10.2)/39 A ~ 33 mA. This kept the current near the maximum rating of 30 mA specified by the manufacturer for 100,000 h lifetime. Each resistor dissipates ~ 1.3 V × 33 mA = 43 mW; the 3 diodes in a branch dissipate 3 × 3.4 × 33 mA = 337 mW. By using 3 diodes to maximizing total diode voltage drop, resistor power loss is kept down to about 13% of the total power. We have implemented the simplest possible circuit to drive the LEDs, one that can be easily built by biologists who have not trained in electronic engineering. More sophisticated driver circuits might be devised to regulate or balance current flow to different branches of the array, but they probably offer little additional benefit for the purposes of scorpion detection.

opencc-zeroJan 2024View details →

Linked collectors and determiners for: Taxonomic synthesis of the eastern North American millipede genus Pseudopolydesmus (Diplopoda: Polydesmida: Polydesmidae), utilizing high-detail ultraviolet fluorescence imaging.

Natural history specimen data linked to collectors and determiners held within, "Taxonomic synthesis of the eastern North American millipede genus Pseudopolydesmus (Diplopoda: Polydesmida: Polydesmidae), utilizing high-detail ultraviolet fluorescence imaging". Claims or attributions were made on Bionomia by volunteer Scribes, <a href="https://bionomia.net/dataset/7226548c-af21-4648-85ea-733acdfda22e">https://bionomia.net/dataset/7226548c-af21-4648-85ea-733acdfda22e</a> using specimen data from the dataset aggregated by the Global Biodiversity Information Facility, <a href="https://gbif.org/dataset/7226548c-af21-4648-85ea-733acdfda22e">https://gbif.org/dataset/7226548c-af21-4648-85ea-733acdfda22e</a>. Formatted as a Frictionless Data package.

opencc-zeroJul 2021View details →

Fitness cost from fluctuating ultraviolet radiation in Daphnia magna

Solar ultraviolet radiation (UVR) is an important environmental threat for organisms in aquatic systems, but its temporally variable nature makes the understanding of its effects ambiguous. The aim of our study was to assess potential fitness costs associated with fluctuating UVR in the aquatic zooplankter Daphnia magna. We investigated individual survival, reproduction and behaviour when exposed to different UVR treatments. Individuals exposed to fluctuating UVR, resembling natural variations in cloud cover, had the lowest fitness (measured as the number of offspring produced during their lifespan). In contrast, individuals exposed to the same, but constant UVR dose, had similar fitness as control individuals (not exposed to UVR), but they showed a significant reduction in daily movement. The re-occurring threat response to the fluctuating UVR treatment thus had strong fitness costs for D. magna, and we found no evidence for plastic behavioural responses when continually being exposed to UVR, despite the regular, predictable exposure schedule. In a broader context, our results imply that depending on how variable a stressor is in nature, populations may respond with alternative strategies, a framework that could promote rapid population differentiation and local adaptation.

opencc-by-4.0Jul 2021View details →

The Ultraviolet Beach Corpus

The dataset for the Ultraviolet Beach Corpus, consisting of comments from online message boards. The topic of discussion is President Trump's statements about using ultraviolet light and disinfectants to treat COVID-19 during a televised White House briefing (Apr.24, 2020).

opencc-by-4.0Aug 2021View details →

An Extreme Ultraviolet Spectrum of a Coronal Loop Footpoint (from Landi & Young 2009)

This record contains a spectrum from the Hinode EUV Imaging Spectrometer (EIS) that was analyzed by Landi & Young (2009, ApJ, 706, 1) and Young & Landi (2009, ApJ, 707, 173). The spectrum was shown in Figures 2-5 of Landi & Young (2009). The items are: sw_spectrum.txt  - Spectrum from the EIS short wavelength (SW) channel [format: ASCII] lw_spectrum.txt  - Spectrum from the EIS long wavelength (LW) channel [format: ASCII] mask.fits - A FITS file containing a 2D bitmap image that shows the spatial pixels that were averaged to yield the spectrum. The mask applies to the wavelength 194.66 angstroms. The spectra are created from the EIS data file beginning at 01:12 UT on 21-Feb-2007. After calibrating the dataset to level-1, the spectra are generated from the pixel mask using the IDL routine eis_mask_spectrum.pro that is available in the Solarsoft library. Further details about this software are available in EIS Software note 16, which is also available in Solarsoft. The Hinode data are publicly available through the Virtual Solar Observatory (https://sdac.virtualsolar.org/). The Solarsoft library is also publicly available at https://www.lmsal.com/solarsoft/. The spectrum is described at https://iopscience.iop.org/article/10.1088/0004-637X/706/1/1.

opencc-by-4.0Sep 2021View details →

Quantitative Ultraviolet Spectroscopy for Magnetic Massive Stars

Ultraviolet (UV) spectroscopy represents a particularly useful observational diagnostic of the dense, radiatively driven winds that are characteristic of OB stars, as UV resonance lines are sensitive to both the density and velocity structure of these outflows. Coupled with appropriate models, it can yield quantitative estimates of the wind parameters of these stars. However, given the usual assumptions that subtend such models, any break in spherical symmetry -- such as in the case of magnetized winds -- will lead to unreliable conclusions. To address this issue in the context of magnetic massive stars, we join parametrized prescriptions for the structure of their magnetospheres to a simplified radiative transfer scheme to generate synthetic line profiles. We compare our results to more realistic techniques (using full magnetohydrodynamic simulations and/or more detailed radiative transfer) and generally find good agreement. As a result, we develop a grid of models that paired with observations can be used to derive quantitative constraints on the wind and magnetic parameters of these stars in a computationally tractable way. This will prove invaluable in interpreting the large quantity of UV spectroscopic data that will be obtained by upcoming projects, such as the ULLYSES project.

opencc-zeroJan 2023View details →

Ultraviolet vision in anemonefish improves color discrimination

In many animals, ultraviolet (UV) vision guides navigation, foraging, and communication, but few studies have addressed the contribution of UV vision to color discrimination, or behaviorally assessed UV discrimination thresholds. Here, we tested UV-color vision in an anemonefish (Amphiprion ocellaris) using a novel five-channel (RGB-V-UV) LED display designed to test UV perception. We first determined that the maximal sensitivity of the A. ocellaris UV cone was at ~386 nm using microspectrophotometry. Three additional cone spectral sensitivities had maxima at ~497, 515, and ~535 nm, which together informed the modelling of the fish's color vision. Anemonefish behavioral discrimination thresholds for nine sets of colors were determined from their ability to distinguish a colored target pixel from grey distractor pixels of varying intensity. We found that A. ocellaris used all four cones to process color information and is therefore tetrachromatic, and fish were better at discriminating colors (i.e., color discrimination thresholds were lower, or more acute) when targets had UV chromatic contrast elicited by greater stimulation of the UV cone relative to other cone types. These findings imply that a UV component of color signals and cues improves their detectability, which likely increases the salience of anemonefish body patterns used in communication and the silhouette of zooplankton prey.

opencc-by-4.0May 2023View details →

Dataset from: Ultraviolet refractive index values of organic aerosol extracted from deciduous forestry, urban and marine environments

The refractive index values of atmospheric aerosols are required to address the large uncertainties in the magnitude of atmospheric radiative forcing and measurements of the refractive index dispersion with wavelength of particulate matter sampled from the atmosphere are rare over ultraviolet wavelengths. An ultraviolet-optimized spectroscopic system illuminates optically-trapped single particles from a range of tropospheric environments to determine the particle’s optical properties. Aerosol from remote marine, polluted urban, and forestry environments is collected on quartz filters, and the organic fraction is extracted and nebulized to form micron-sized spherical particles. The radius and the real component of refractive index dispersion with wavelength of the optically trapped particles are determined to a precision of 0.001 µm and 0.002 respectively over a near-ultraviolet-visible wavelength range of 0.320–0.480 µm. Remote marine aerosol is observed to have the lowest refractive index (n=1.442 (λ=0.350 µm)), with above-canopy rural forestry aerosol (n=1.462–1.481 (λ=0.350 µm)) and polluted urban aerosol (n=1.444–1.485 (λ=0.350 µm)) showing similar refractive index dispersions with wavelength. In-canopy rural forestry aerosol is observed to have the highest refractive index value (n=1.508 (λ=0.350 µm)). The study presents the first single particle measurements of the dispersion of refractive index with wavelength of atmospheric aerosol samples below wavelengths of 0.350 µm. The Cauchy dispersion equation, commonly used to describe the visible refractive index variation of aerosol particles, is demonstrated to extend to ultraviolet wavelengths below 0.350 µm for the urban, forestry, and atmospheric aerosol water-insoluble extracts from these environments. A 1D radiative-transfer calculation of the difference in top-of-the-atmosphere albedo between atmospheric core-shell mineral aerosol with and without films of this material demonstrates the importance of organic films forming on mineral aerosol. The raw experimental spectra collected and analysed in this study are provided, as well as files for the calibrated wavelengths.

Figure 3 in Effects of Ultraviolet Light and Pheromone Release Rate in Trapping Coconut Rhinoceros Beetles, Oryctes rhinoceros (Coleoptera: Scarabaeidae), on Guam

Figure 3. Capture rates (mean ± SE) of beetle caught in double-vaned bucket. UV = trap equipped with UV LED diodes, RL = trap with reduced release rate of oryctalure, SL = trap with standard release rate of oryctalure. Comparisons of mean trap capture between traps with and without UV light and between traps with different oryctalure release rates are shown at right. Bars with different letters indicate significantly different means (UV light: t-test, Lure: ANOVA, Tukey's HSD).

Figure 4 in Effects of Ultraviolet Light and Pheromone Release Rate in Trapping Coconut Rhinoceros Beetles, Oryctes rhinoceros (Coleoptera: Scarabaeidae), on Guam

Figure 4. Capture rate as a function of oryctalure release rate for traps without (A) and with (B) ultraviolet light emitting diodes. UV = trap equipped with UV LED diodes, RL = trap with reduced release rate of oryctalure, SL = trap with standard release rate of oryctalure. Lines are ordinary least-squares fits. The equation for traps without UV LEDs is y = 0.0059 + 0.0015x; slope is not significantly different from zero (P = 0.118). The equation for traps with UV LEDs is y = 0.0182 + 0.0070x; slope is significantly different from zero (P = 0.005).

Figure 2. Reduced release rate pheromone dispenser. A 2 in Effects of Ultraviolet Light and Pheromone Release Rate in Trapping Coconut Rhinoceros Beetles, Oryctes rhinoceros (Coleoptera: Scarabaeidae), on Guam

Figure 2. Reduced release rate pheromone dispenser. A 2 mm hole in the tops of the Eppendorf centrifuge tube allows a slow release of the attractant oryctalure. The bottle shown acts as a rain and wind shield. This entire release device is placed within a bucket trap for field deployment.

Figure 1 in Effects of Ultraviolet Light and Pheromone Release Rate in Trapping Coconut Rhinoceros Beetles, Oryctes rhinoceros (Coleoptera: Scarabaeidae), on Guam

Figure 1. Trap line locations, from north to south, were located at the University of Guam Agricultural Experiment Station in Yigo, the GICC Golf Course in Dededo, the Temple Baptist Church in Chalan Pago, the Leo Palace Golf Course in Yona, the Windward Hills Golf Course in Yona, and the Chargalauf Farm in Inarajan. An on-line interactive version of this map is available at https://github.com/ aubreymoore/CRB- trapimprovement/ blob/master/map.geojson.

opencc-by-4.0Aug 2023View details →

Dataset: vacuum-ultraviolet laser source for spectroscopy of trapped thorium ions

This is a data set accompanying the publication "Vacuum-ultraviolet laser source for spectroscopy of trapped thorium ions" in the New Journal of Physics. https://doi.org/10.1088/1367-2630/aced1b

publicJun 2022View details →

Data from: Active regulation of ultraviolet light exposure overrides thermal preference behaviour in eastern fence lizards

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publicJul 2021View details →

Fitness cost from fluctuating ultraviolet radiation in Daphnia magna

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