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197 results for “Wavelengths”
Caecilians maintain a functional long-wavelength-sensitive cone opsin gene despite signatures of relaxed selection and more than 200 million years of fossoriality
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Wavelength-division multiplexing optical Ising simulator enabling fully programmable spin couplings and external magnetic fields
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Data for: Long-wavelength-sensitive (lws) opsin gene expression, foraging and visual communication in coral reef fishes
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Data from: Photoacoustic imaging of rat kidney tissue oxygenation using NIR-II wavelengths
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Level 2 spectra of the global solar irradiance in the wavelength range 290 - 500 nm measured at Aosta - Saint Christophe, Italy by the Bentham DTMc300 with serial number 5541 in 2006 - 2019
<p>The provided dataset includes the Level 2 <strong>spectral measurements</strong> (in Watt/m<sup>2</sup>/nm) of the solar irradiance in the range 290 - 500 nm, performed by the Bentham DTMc300 spectroradiometer with serial number 5541. The particular instrument performs automated continuous, high quality measurements at Aosta - Saint Christophe, Italy (45.7° N, 7.4° E, 570 m a.s.l.) since 2006. The Level 2 spectra are re-evaluated and homogenized and are currently available for the period 24 July 2006 - 8 July 2019. Each file contains the spectra for one day. The time (in UTC) for the measurements at 290, 400, and 500 nm is also provided for each spectral scan so that the user has also information for the duration of each scan.</p> <p>The daily <strong>noon UV index</strong> is also provided for the same period in the file "<strong>aao_noon_uvi_l2.dat</strong>". Erythemal doses have been calculated by weighting each spectrum with the CIE (1999) effective spectrum, and then integrating in the range 290 - 400 nm. Then the UV index has been calculated by dividing erythemal dose (in mWatt/m<sup>2</sup>) by 25. The noon UV index for each day has been calculated as the average of available measurements for ±15 minutes around the exact local noon.</p> <p>For further information for file format and contents please see the <strong>readme.txt</strong> file.</p> <p>Reference</p> <p>CIE: CIE S007/E-1998 Erythema reference action spectrum and standard erythema dose, Color Research & Application, 24, 158-158, 10.1002/(sici)1520-6378(199904)24:2<158::aid-col11>3.0.co;2-4, 1999.</p>
Multi-wavelength AGN Properties of Post-Merger Galaxies
<p>It’s well studied that galaxy mergers can have a profound impact on triggering both star formation and an Active Galactic Nucleus (AGN). The AGN is expected to quench star formation through “feedback” processes, by heating or expelling gas out of the galaxy, leaving behind a merger remnant. Unfortunately, confirming that mergers trigger AGN is observationally challenging, because AGN in different merger stages can have discrepant luminosities and lifetimes. In addition, a multi-wavelength approach is required to provide a complete census of AGN. Here I present results based on a volume limited (0.02<z<0.06, 10.5<logM<12.0), visually identified sample of post-merger galaxies from SDSS-DR14. I will describe the multi-wavelength AGN demographics of this sample using Chandra, XMM X-ray imaging, optical BPT diagnostics based on SDSS single-fiber spectra, WISE infrared color and VLA FIRST radio images. I will discuss plans to expand our analysis of the merger-AGN connection to post merger galaxies at higher redshift using the Nancy Grace Roman Space Telescope and other multi-wavelength data.</p>
Data from: Short- and mid-wavelength artificial light influences the flash signals of Aquatica ficta fireflies (Coleoptera: Lampyridae)
Urbanization can radically disrupt natural ecosystems through alteration of the sensory environment. Habitat disturbances are predicted to favor behaviorally flexible species capable of adapting to altered environments. When artificial light at night (ALAN) is introduced into urban areas, it has the potential to impede reproduction of local firefly populations by obscuring their bioluminescent courtship signals. Whether individual fireflies can brighten their signals to maintain visibility against an illuminated background remains unknown. In this study, we exposed male Aquatica ficta fireflies to diffused light of varying wavelength and intensity, and recorded their alarm flash signals. When exposed to wavelengths at or below 533 nm, males emitted brighter signals with decreased frequency. This is the first evidence of individual-level light signal plasticity in fireflies. In contrast, long wavelength ambient light (≥ 597 nm) did not affect signal morphology, likely because A. ficta cannot perceive these wavelengths. These results suggest long wavelength lighting is less likely to impact firefly courtship, and its use in place of broad spectrum white lighting could augment firefly conservation efforts. More generally, this study demonstrates benefits of bioluminescent signal plasticity in a "noisy" signaling environment, and sheds light on an important yet understudied consequence of urbanization.
Data from: A cure for the blues: opsin duplication and subfunctionalization for short-wavelength sensitivity in jewel beetles (Coleoptera: Buprestidae)
Background: Arthropods have received much attention as a model for studying opsin evolution in invertebrates. Yet, relatively few studies have investigated the diversity of opsin proteins that underlie spectral sensitivity of the visual pigments within the diverse beetles (Insecta: Coleoptera). Previous work has demonstrated that beetles appear to lack the short-wavelength-sensitive (SWS) opsin class that typically confers sensitivity to the "blue" region of the light spectrum. However, this is contrary to established physiological data in a number of Coleoptera. To explore potential adaptations at the molecular level that may compensate for the loss of the SWS opsin, we carried out an exploration of the opsin proteins within a group of beetles (Buprestidae) where short-wave sensitivity has been demonstrated. RNA-seq data were generated to identify opsin proteins from nine taxa comprising six buprestid species (including three male/female pairs) across four subfamilies. Structural analyses of recovered opsins were conducted and compared to opsin sequences in other insects across the main opsin classes—ultraviolet, short-wavelength, and long-wavelength. Results: All nine buprestids were found to express two opsin copies in each of the ultraviolet and long-wavelength classes, contrary to the single copies recovered in all other molecular studies of adult beetle opsin expression. No SWS opsin class was recovered. Furthermore, the male Agrilus planipennis (emerald ash borer—EAB) expressed a third LWS opsin at low levels that is presumed to be a larval copy. Subsequent homology and structural analyses identified multiple amino acid substitutions in the UVS and LWS copies that could confer short-wavelength sensitivity. Conclusions: This work is the first to compare expressed opsin genes against known electrophysiological data that demonstrate multiple peak sensitivities in Coleoptera. We report the first instance of opsin duplication in adult beetles, which occurs in both the UVS and LWS opsin classes. Through structural comparisons of known insect opsins, we suggest that opsin duplication and amino acid variation within the chromophore binding pocket explains sensitivity in the short-wavelength portion of the visible light spectrum in these species. These findings are the first to reveal molecular complexity of the color vision system within beetles.
Hunting Down White Dwarf--Main Sequence Binaries Using Multi-Wavelength Observations
<p>Identification of white dwarfs (WD) with main-sequence (MS) companions and characterization of their properties can put important constraints on our understanding of binary stellar evolution and guide the theoretical predictions for a wide range of interesting transient events relevant for, e.g., Rubin Observatory (LSST), ZTF, and LISA. In this study, we combine ultraviolet (UV) and optical color-magnitude diagrams (CMDs) to identify unresolved WD--MS binaries. In particular, we combine high-precision astrometric and photometric data in the optical from \gaia\ -DR3 and UV data from GALEX GR6/7 to identify 93 WD--MS candidates within 100 pc. Of these, 80 are newly identified. Using the Virtual Observatory SED Analyzer (VOSA) we fit the spectral energy distributions (SEDs) of all our candidates and derive stellar parameters, such as effective temperature, bolometric luminosity, and radius for both companions. We find that our identification method helps identify hotter and smaller WD companions (majority with ≥ 10,000 K and ≤ 0.02 R_Sun) relative to the WDs identified by past surveys. We infer that these WDs are relatively more massive (median ~0.76 M_Sun). We find that most of the MS companions in our binaries are of the K and M spectral types. </p>
A Network-Based Phase-Gradient Stacking Method for Resolving Long-wavelength deformation from low-coherence SAR interferograms
<p><span><span><strong>This dataset includes the key results, primary </strong></span></span><strong>InSAR and GNS observatons </strong><strong> in our study. </strong></p>
Data from: Insect visual sensitivity to long wavelengths enhances colour contrast against vegetation
<p><span><span><span><span><span><span><span><span><span><span><span>The sensitivity of animal photoreceptors to different wavelengths of light strongly influence the perceived visual contrast of objects in the environment. Outside of the human visual wavelength range, ultraviolet sensitivity in many species provides important and behaviourally relevant visual contrast between objects. However, at the opposite end of the spectrum, the potential advantage of red sensitivity remains unclear. We investigated the potential benefit of long wavelength sensitivity by modelling the visual contrast of a wide range of jewel beetle colours against flowers and leaves of their host plants to hypothetical insect visual systems. We find that the presence of a long wavelength sensitive photoreceptor increases estimated colour contrast, particularly of beetles against leaves. Moreover, under our model parameters, a trichromatic visual system with ultraviolet (λ<sub>max</sub> = 355 nm), short (λ<sub>max</sub> = 445 nm) and long (λ<sub>max</sub> = 600 nm) wavelength photoreceptors performed as well as a tetrachromatic visual system, which had an additional medium wavelength photoreceptor (λ<sub>max</sub> = 530 nm). When we varied λ<sub>max</sub> for the long wavelength sensitive receptor in a tetrachromatic system, contrast values between beetles, flowers and leaves were all enhanced with increasing λ<sub>max</sub> from 580 nm to at least 640 nm. These results suggest a potential advantage of red sensitivity in visual discrimination of insect colours against vegetation and highlight the potential adaptive value of long wavelength sensitivity in insects.</span></span></span></span></span></span></span></span></span></span></span></p>
Raw data for: Dual-Comb Swept-Wavelength Interferometry: Theory and Experiment
<p>This document includes the raw data and Python codes to obtain the figures included in the paper "Dual-Comb Swept-Wavelength Interferometry: Theory and Experiment"</p>
Cross-correlation coefficient maps generated in the paper "Correlation of Venusian Mesoscale Cloud Morphology Between Images Acquired at Various Wavelengths" by Narita et al. published in Journal of Geophysical Research - Planets
<p>This data archive contains the cross-correlation coefficient maps. Unzipping the compressed file, the following directories corresponding to different wavelength pairs appear. </p> <p> IR1_IR2/ : 0.9 micron & 2.02 micron<br> UVI283_UVI365/ : 283 nm & 365 nm<br> IR2_UVI365/ : 2.02 micron &. 365 nm<br> IR2_UVI283/ : 2.02 micron & 283 nm<br> IR2_LIR/ : 2.02 micron & 10 micron</p> <p>If usual unzip tools do not work, the use of 7zip is recommended:<br> https://www.7-zip.org/download.html</p> <p>Each directory contains CSV files for the longitude-latitude distribution of the correlation coefficient. The 2880 longitude grids cover the longitude range of 0 - 360 degrees, and the 1440 latitude grids cover the latitude range of -90 - +90 degrees, with a pixel resolution of 0.125 degree/pixel. Invalid regions are filled with the value of 1.1.</p> <p>Each filename is composed of the date, the instrument (wavelength), and the time. For example, for the file "20160720_ir2_150821_hp6_IR1_150209_hp6_sb24.csv":</p> <p> 20160720 : July 20, 2016<br> ir2 : 2.02 micron filter of IR2 camera<br> 150821 : IR2 exposure at 15:08:21<br> hp6: High-pass filtering size is 6 deg x 6 deg<br> IR1 : 0.9 micron filter of IR1 camera<br> 150209 : IR1 exposure at 15:02:09<br> sb24 : Sliding box size is 24 deg x 24 deg</p>
Dataset for "Long-wavelength pulse generation via light-sail backscattering"
<p>Dataset for "Long-wavelength pulse generation via light-sail backscattering", paper submitted to PPCF</p>
LAMOST RVM and wavelength data.
<p>LAMOST RVM and wavelength data.</p>
SNID template data set v2.0.0 extended to 2 microns (1024 and 2048 wavelength bins)
<p>This set of SNID templates extends the v2.0.0 set out to 2 microns (wavelength range 2500 Ang-2 microns). It should be used when the input spectrum has data extending beyond 1 micron, since the original templates-2.0 set only covers 2500-10000 Ang.</p> <p>Two versions of the data set are published, one with 1024 wavelength bins, the other with 2048 wavelength bins.</p> <p> Reading template files...sn1979C sn1980K sn1981B sn1983N sn1983V sn1984A sn1984L sn1986G sn1987A sn1988L sn1989B sn1990B sn1990I sn1990K sn1990N sn1990O sn1990U sn1990aa sn1991A sn1991M sn1991N sn1991T sn1991ar sn1991bg sn1992A sn1992H sn1992ar sn1993J sn1993ac sn1994D sn1994I sn1994M sn1994Q sn1994S sn1994T sn1994ae sn1995D sn1995E sn1995F sn1995ac sn1995ak sn1995al sn1995bd sn1996C sn1996L sn1996X sn1996Z sn1996ab sn1996ai sn1996bk sn1996bl sn1996bo sn1996bv sn1996cb sn1997E sn1997Y sn1997bp sn1997bq sn1997br sn1997cn sn1997cy sn1997dc sn1997dd sn1997do sn1997dq sn1997dt sn1997ef sn1997ei sn1998S sn1998T sn1998V sn1998ab sn1998aq sn1998bp sn1998bu sn1998bw sn1998co sn1998de sn1998dh sn1998dk sn1998dm sn1998dt sn1998dx sn1998ec sn1998ef sn1998eg sn1998es sn1999X sn1999aa sn1999ac sn1999aw sn1999bh sn1999by sn1999cc sn1999cl sn1999cp sn1999cw sn1999da sn1999di sn1999dn sn1999dq sn1999ee sn1999ef sn1999ej sn1999ek sn1999em sn1999ex sn1999gd sn1999gh sn1999gi sn1999gp sn2000B sn2000E sn2000H sn2000bh sn2000bk sn2000ce sn2000cf sn2000cn sn2000cp sn2000cu sn2000cw sn2000cx sn2000dg sn2000dk sn2000dm sn2000dn sn2000fa sn2001E sn2001G sn2001N sn2001V sn2001ah sn2001ay sn2001az sn2001bf sn2001bg sn2001br sn2001cj sn2001ck sn2001cp sn2001da sn2001eh sn2001el sn2001en sn2001ep sn2001ex sn2001fe sn2001fh sn2001gc sn2002G sn2002ap sn2002aw sn2002bf sn2002bo sn2002cd sn2002cf sn2002ck sn2002cr sn2002cs sn2002cu sn2002cx sn2002de sn2002dj sn2002dl sn2002do sn2002dp sn2002ef sn2002er sn2002es sn2002eu sn2002fb sn2002fk sn2002ha sn2002hd sn2002he sn2002hu sn2002hw sn2002ic sn2002jg sn2002jy sn2002kf sn2003U sn2003W sn2003Y sn2003bg sn2003cg sn2003ch sn2003cq sn2003du sn2003fa sn2003gn sn2003hu sn2003hv sn2003ic sn2003it sn2003iv sn2003kc sn2003kf sn2004L sn2004S sn2004as sn2004at sn2004aw sn2004bd sn2004bg sn2004bk sn2004dj sn2004dt sn2004ef sn2004eo sn2004et sn2004fu sn2004fz sn2004gc sn2004gs sn2005A sn2005M sn2005am sn2005bc sn2005be sn2005bf sn2005bl sn2005bo sn2005cc sn2005cf sn2005cg sn2005cs sn2005el sn2005eq sn2005eu sn2005gj sn2005hc sn2005hf sn2005hj sn2005hk sn2005iq sn2005kc sn2005ke sn2005ki sn2005kl sn2005ls sn2005lu sn2005mc sn2005mz sn2005na sn2006D sn2006H sn2006N sn2006S sn2006X sn2006ac sn2006aj sn2006ak sn2006al sn2006ax sn2006az sn2006bp sn2006bq sn2006br sn2006bt sn2006bw sn2006bz sn2006cc sn2006cf sn2006cj sn2006cm sn2006cp sn2006cq sn2006cz sn2006em sn2006eq sn2006et sn2006eu sn2006ev sn2006gj sn2006gr sn2006gt sn2006gz sn2006hb sn2006kf sn2006le sn2006lf sn2006mo sn2006nz sn2006oa sn2006ot sn2006sr sn2006te sn2007A sn2007F sn2007S sn2007Y sn2007ae sn2007af sn2007al sn2007ap sn2007au sn2007ax sn2007ba sn2007bc sn2007bd sn2007bj sn2007bm sn2007bz sn2007ca sn2007cg sn2007ci sn2007co sn2007cq sn2007fb sn2007fs sn2007hj sn2007if sn2007jg sn2007kk sn2007le sn2007nq sn2007qe sn2007sr sn2007ux sn2008A sn2008C sn2008D sn2008L sn2008Q sn2008R sn2008Z sn2008ae sn2008af sn2008ar sn2008bf snls03D3bb done<br> Loaded 4388 spectra out of 333 templates</p>
Data - Ultralow noise preamplified optical receiver using conventional single wavelength transmission
<p>This dataset contains measurement data and processing code for the results published in "Ultralow noise preamplified optical receiver using conventional single wavelength transmission". Raw measurement batches from the BER-measurement can be made available upon request, at rasmus.larsson@chalmers.se.</p> <p>This work was funded by the Swedish Research Council (grant VR-2015-00535).</p>
A Unified Multi-Wavelength Data Analysis Workflow with gammapy.
<p>Repository containing multi-wavelength (MWL) data of the distant quasar OP 313 (z=0.997) taken during the nights of MJD 60373 (3-4 March 2024) and MJD 60384 (14-15 March 2024) using <em>Fermi</em>-LAT, <em>Swift</em>-XRT, <em>Swift</em>-UVOT, and the Liverpool IO:O photometric data.</p> <div> <h3>Directory structure:</h3> <a href="https://github.com/mireianievas/gammapy_mwl_workflow/tree/main#directory-structure"></a></div> <ul> <li>Notebooks/DatasetGenerator: Notebooks (one per instrument) that summarize the steps to generate gammapy-compliant 1D and 3D binned datasets.</li> <li>Notebooks/DatasetAnalysis: Notebooks (one per instrument) to analyse each dataset independently and one notebook to perform the MWL joint analysis.</li> <li>Helpers: Auxiliary functions to generate native multiplicative models for dust extinction (out of xspec's redden), neutral hydrogen (out of xspec's tbabs), EBL absorption, and utility functions for file handling and plotting.</li> <li>Models: multiplicative models in tabular format for easy 2d interpolation.</li> <li>Figures: collection of figures for the paper.</li> </ul> <p>Link: <a href="https://github.com/mireianievas/gammapy_mwl_workflow">https://github.com/mireianievas/gammapy_mwl_workflow/ </a></p> <p>Based on the original work from <a href="https://github.com/luca-giunti/gammapyXray">https://github.com/luca-giunti/gammapyXray</a></p>
Effect of Light Wavelength on Soybean Growth and Development in a Context of Speed Breeding
<p>Soybean breeding involves crossing and inbreeding for multiple generations to develop genetically-stable lines. The long generation times and the absence of easily-scalable double-haploid technologies cause early generations to be the major bottleneck in soybean breeding. Here we tested the effect of red and blue lights (RB) and full spectrum white lights (FS) generated by light emitting diode (LED) panels, coupled with 12 h light (29 °C) / 12 h darkness (27 °C) photothermal conditions, on the growth and development of soybean lines and breeding materials of diverse maturity groups in a context of speed breeding. We observed that RB light, when compared to FS light, reduced plant height by an average of 17.3 cm but did not affect vegetative biomass, pods and seeds per plants, nor the ability to meet a minimum of one seed per plant. Overall, the RB light treatment reduced days after planting (DAP) to physiological maturity (R7) by 1.5 d as compared to FS. The period between planting and the harvest of seeds (cycle time) of mid- and late-maturity soybean ranged from 63 to 81 d in the greenhouse, as compared to approximately 120 d typically observed in field conditions. Also, DAP to R7 was dependent on soybean maturity group. The use of RB lights, coupled with photothermal conditions herein reported, would allow to advance up to 5 generations of US-adapted soybean under a controlled environment, instead of the 1-3 generations currently possible. This methodology is simple and easily scalable for it maintains stable growing conditions throughout the crop cycle and it allows for simultaneous planting and harvesting within the same growth room. This could have a significant impact in genetic gain of U.S. soybean breeding programs.</p>
Ultrahigh-responsivity waveguide-coupled optical power monitor for Si photonic circuits operating at near-infrared wavelengths
<p>The simulation code and script of Lumerical for the Simulation in the Supplementary figures: Fig. S4 and Fig. S5.</p>
ScienceDex guides
Understand access before you commit
These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.