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HI line observations of 290 evolved stars made with the Nancay Radio Telescope - I. Data: online Tables
<p>--- Table B.1: Clear NRT HI detections - basic data </p> <p>Description of the columns:</p> <p>(1) Name: common catalogue name of the target. <br> An ^n after a name indicates that it is clearly not an AGB star, <br> a ^d that we consider its classification as an AGB to be dubious, <br> and a ^* indicates that notes on the object can be found in Appendix A;<br>(2,3) RA,DEC: literature right ascension and declination of the target from Gaia EDR 3, <br> for epoch J2000.0;<br>(4) Type: target type. <br> Primarily the variability type as listed in Version 5.1 of the General Catalogue of Variable Stars, <br> GCVS (A description of GCVS types is given in https://cdsarc.u-strasbg.fr/ftp/cats/B/gcvs/vartype.txt),<br> but if an object is not included in the GCVS, other identifiers are listed in brackets: <br> HPM = high proper motion star, (OH/IR) = OH/IR maser, LPVc = long-period variable candidate, <br> PN = planetary nebula, pPN = proto-planetary nebula, and post-AGB star;<br>(5,6) Spec & ref: spectral type of the star, followed by its literature reference, <br> as retrieved from the SIMBAD database. If none was listed there, the reference is noted as 'SIMBAD';<br>(7,8) Teff & ref: effective temperature of the star, in K, followed by its literature reference; <br>(9) d: distance of the target, based on its parallax (mainly from the Gaia EDR3), in pc.<br> If no Gaia parallax was available a reference to the distance we adopted is given in Appendix A<br> (for RAFGL 3099, mu Cep, and V Peg);<br>(10) Vlit: published radial velocity of the target in the LSR reference frame, in km/s;<br>(11) Vexp: literature expansion velocity measured from CO or OH 1612 MHz line observations, in km/s. <br> If a pair of values was published for a two-velocity component CO line fit, the largest value is listed here;<br>(12) ref: literature references to the published Vlit and Vexp values; <br>(13) line: spectral line on which the published radial velocity measurement (Vlit) was based;<br>(14,15) Mdot & ref: literature mass loss rates, in solar masses per year, <br> followed by its literature reference.</p> <p>Notes to Table B.1:</p> <p>References: see Table B.1 in the Astronomy & Astrophysics paper.</p> <p><br>--- Table B.2: Clear NRT HI detections - HI data </p> <p>Description of the columns:</p> <p>(1) Name: common catalogue name of the target. <br> A ^T after a name indicates that HI line parameters are based on a 'total' spectrum, whereas <br> a ^P indicates that a 'peak' spectrum was used. <br> An ^n indicates that it is clearly not an AGB star, <br> a ^d that we consider its classification as an AGB to be dubious, <br> and a ^* indicates that notes on the object can be found in Appendix A;<br>(2) VHI: our central radial velocity in the LSR reference frame of the Gaussian fitted <br> to the HI profile, in km/s.<br>(3) FWHM: our full width half maximum of the Gaussian fitted to the HI line profile, in km/s;<br>(4) Speak: our peak flux density of the HI line profile, in Jy;<br>(5) diam: our estimated angular size of the HI CSE in the east-west direction, in arcmin;<br>(6) FHI: our integrated line flux of the HI profile, in Jy km/s;<br>(7) MHI: our total HI mass, in Msun;<br>(8) HI ref: references to previously published HI studies,<br> see Table B.2 in the Astronomy & Astrophysics paper.</p> <p><br>--- Table B.3: Possible NRT HI detections - basic data</p> <p>Description of the columns:</p> <p>(1) Name: common catalogue name of the target. <br> An ^n after a name indicates that it is clearly not an AGB star, <br> a ^d that we consider its classification as an AGB to be dubious, <br> and a ^* indicates that notes on the object can be found in Appendix A;<br>(2,3) RA,DEC: literature right ascension and declination of the target from Gaia EDR 3, <br> for epoch J2000.0;<br>(4) Type: target type. <br> Primarily the variability type as listed in Version 5.1 of the General Catalogue of Variable Stars, <br> GCVS (A description of GCVS types is given in https://cdsarc.u-strasbg.fr/ftp/cats/B/gcvs/vartype.txt),<br> but if an object is not included in the GCVS, other identifiers are listed in brackets: <br> HPM = high proper motion star, (OH/IR) = OH/IR maser, LPVc = long-period variable candidate, <br> PN = planetary nebula, pPN = proto-planetary nebula, and post-AGB star;<br>(5,6) Spec & ref: spectral type of the star, followed by its literature reference, <br> as retrieved from the SIMBAD database. If none was listed there, the reference is noted as 'SIMBAD';<br>(7,8) Teff & ref: effective temperature of the star, in K, followed by its literature reference; <br>(9) d: distance of the target, based on its parallax (mainly from the Gaia ED33), in pc.<br> If no Gaia parallax was available a reference to the distance we adopted is given in Appendix A<br> (for RAFGL 3099, mu Cep, and V Peg);<br>(10) Vlit: published radial velocity of the target in the LSR reference frame, in km/s;<br>(11) Vexp: literature expansion velocity measured from CO or OH 1612 MHz line observations, in km/s. <br> If a pair of values was published for a two-velocity component CO line fit, the largest value is listed here;<br>(12) Mdot : literature mass loss rates, in solar masses per year, <br>(13) line: spectral line on which the published radial velocity measurement (Vlit) was based;<br>(14) ref: literature references to the published Vlit, Vexp and Mdot values; </p> <p>Notes to Table B.3:</p> <p>References: see Table B.1 in the Astronomy & Astrophysics paper.</p> <p><br>--- Table B.4: Possible NRT HI detections - HI data</p> <p>Description of the columns:</p> <p>See the description of the columns of Table B.2.</p> <p><br>--- Online only Table 5: Upper limits to NRT HI lines </p> <p>Description of the columns:</p> <p>(1) Name: common catalogue name of the target. <br> An ^n after a name indicates that it is clearly not an AGB star, <br> a ^d that we consider its classification as an AGB to be dubious, <br> and a ^* indicates that notes on the object can be found in Appendix A;<br>(2,3) RA,DEC: literature right ascension and declination of the target from Gaia EDR 3, <br> for epoch J2000.0;<br>(4) Type: target type. <br> Primarily the variability type as listed in Version 5.1 of the General Catalogue of Variable Stars, <br> GCVS (A description of GCVS types is given in https://cdsarc.u-strasbg.fr/ftp/cats/B/gcvs/vartype.txt),<br> but if an object is not included in the GCVS, other identifiers are listed in brackets: <br> HPM = high proper motion star, (OH/IR) = OH/IR maser, LPVc = long-period variable candidate, <br> PN = planetary nebula, pPN = proto-planetary nebula, and post-AGB star;<br>(5,6) spec & ref: spectral type of the star, followed by its literature reference, <br> as retrieved from the SIMBAD database. If none was listed there, the reference is noted as 'SIMBAD';<br>(7,8) Teff & ref: effective temperature of the star, in K, followed by its literature reference; <br>(9) d: distance of the target, based on its parallax (mainly from the Gaia EDR3, in pc.<br> If no Gaia parallax was available a reference to the distance we adopted is given in Appendix A<br> (for RAFGL 3099, mu Cep, and V Peg);<br>(10) Vlit: published radial velocity of the target in the LSR reference frame, in km/s;<br>(11) Vexp: literature expansion velocity measured from CO or OH 1612 MHz line observations, in km/s. <br> If a pair of values was published for a two-velocity component CO line fit, the largest value is listed here;<br>(12) Mdot : literature mass loss rates, in solar masses per year, <br>(13) ref: literature references for Vlit, Vexp and Mdot, as applicable;<br>(14) line: spectral line on which the published radial velocity measurement (Vlit) was based;<br>(15) Speak: peak flux density of our HI line profile, in Jy;<br>(16) notes: 'old data' indicates objects observed only in 1992/1993, before the renovation of the NRT; <br> 'blue/red side' indicates that either the blue or red side of the HI profile could be used to measure <br> an upper limit to the line flux;<br>(17) HI ref: references to previously published HI studies;</p> <p>Notes to online only Table 5: </p> <p>HI references: see Table B.2 in the Astronomy & Astrophysics paper.<br>Other references: see Table B.1 in the Astronomy & Astrophysics paper.</p> <p><br>--- Online only Table 6: Confused NRT HI spectra</p> <p>Description of the columns:</p> <p>(1) Name: common catalogue name of the target. <br>(2,3) RA, DEC: literature right ascension and declination of the target from Gaia EDR3, <br> for epoch J2000.0; <br>(4) type: target type. Primarily the variability type as listed in Version 5.1 of the <br> General Catalogue of Variable Stars, GCVS; but if an object is not included in the GCVS, <br> other identifiers are listed in brackets: HPM = high proper motion star, (OH/IR) = OH/IR maser, <br> LPVc = long-period variable candidate, PN = planetary nebula, pPN = proto-planetary nebula, <br> and post-AGB star; <br>(5,6) spec & ref spectral type of the star, followed by its literature reference, <br> as retrieved from the SIMBAD database. If none was listed there, the reference is noted as 'SIMBAD'; <br>(7,8) Vlit & ref: published radial velocity of the target in the LSR reference frame, in km/s; <br>(9) line: spectral line on which the published radial velocity measurement (Vlit) was based; <br>(10) notes: 'old data' denotes objects observed only in 1992/1993, before the renovation of the NRT<br> (see Section 3), for which no observations in digital form are available; <br>(11) HI ref: references to previously published HI studies.</p> <p>Notes to online only Table 6:</p> <p>HI references: see Table B.2 in the Astronomy & Astrophysics paper.<br>Other references: see Table B.1 in the Astronomy & Astrophysics paper.</p>
Cherenkov Telescope Data for Ordinal Quantification
<p>This labeled data set is targeted at ordinal quantification. The goal of quantification is not to predict the class label of each individual instance, but the distribution of labels in unlabeled sets of data.</p> <p>With the scripts provided, you can extract the relevant features and labels from the public data set of the FACT Cherenkov telescope. These features are precisely the ones that domain experts from astro-particle physics employ in their analyses. The labels stem from a binning of a continuous energy label, which is common practice in these analyses.</p> <p>We complement this data set with the indices of data items that appear in each sample of our evaluation. Hence, you can precisely replicate our samples by drawing the specified data items. The indices stem from two evaluation protocols that are well suited for ordinal quantification. To this end, each row in the files<em> app_val_indices.csv</em>, <em>app_tst_indices.csv</em>, <em>app-oq_val_indices.csv</em>, <em>app-oq_tst_indices.csv,</em> <em>real_val_indices.csv</em>, and <em>real_tst_indices.csv</em> represents one sample.</p> <p>Our first protocol is the artificial prevalence protocol (APP), where all possible distributions of labels are drawn with an equal probability. The second protocol, APP-OQ(5%), is a variant thereof, where only the smoothest 5% of all APP samples are considered. This variant is targeted at ordinal quantification tasks, where classes are ordered and a similarity of neighboring classes can be assumed. The labels of the FACT data lie on an ordinal scale and, hence, pose such an ordinal quantification task. The third protocol considers "real" distributions of labels. These distributions would be expected by observing the Crab Nebula through the FACT telescope.</p> <p><strong>Usage</strong></p> <p>You can extract the data <em>fact.csv</em> through the provided script <em>extract-fact.jl</em>, which is conveniently wrapped in a <em>Makefile</em>. The <em>Project.toml</em> and <em>Manifest.toml</em> specify the Julia package dependencies, similar to a requirements file in Python.</p> <p><strong>Preliminaries:</strong> You have to have a working Julia installation. We have used Julia v1.6.5 in our experiments.</p> <p><strong>Data Extraction:</strong> In your terminal, you can call either</p> <pre><code>make</code></pre> <p>(recommended) or</p> <pre><code>curl --fail -o fact.hdf5 https://factdata.app.tu-dortmund.de/dl2/FACT-Tools/v1.1.2/gamma_simulations_facttools_dl2.hdf5 julia --project="." --eval "using Pkg; Pkg.instantiate()" julia --project="." extract-fact.jl</code></pre> <p><strong>Outcome: </strong>The first row in the resulting <em>fact.csv</em> file is the header. The first column, named "class_label", is the ordinal class.</p> <p><strong>Further Reading</strong></p> <p>Implementation of our experiments: <a href="https://github.com/mirkobunse/regularized-oq">https://github.com/mirkobunse/regularized-oq</a></p> <p>Original data repository: <a href="https://factdata.app.tu-dortmund.de/">https://factdata.app.tu-dortmund.de/</a></p> <p>Reference analysis by astro-particle physicists: <a href="https://github.com/fact-project/open_crab_sample_analysis">https://github.com/fact-project/open_crab_sample_analysis</a></p>
CTAO Simulation Telescope Models for CORSIKA and sim_telarray - Prod6
<p>The <a href="https://www.cta-observatory.org/">Cherenkov Telescope Array Observatory</a> (CTAO) is the next-generation gamma-ray observatory under construction on the island of La Palma (Spain) and near Paranal (Chile). CTAO will cover a wide energy range and provide substantial improvements in sensitivity, angular resolution and energy resolution in comparison to any existing gamma-ray detector. Detailed Monte Carlo simulations enable the optimization of the instrument configuration and the estimation of observatory performance using realistic models of the telescope design. The CORSIKA air-shower simulation code and the sim_telarray code for simulation of arrays of Cherenkov telescopes are used for all CTAO Monte Carlo simulation productions.</p> <p>This repository provides access to the simulation configuration describing the site parameters and the telescope simulation models required for the generation of the CTAO Instrument Response Functions based on the Prod6 observatory model (to be published).</p> <p>In detail, these are:</p> <ul> <li>telescope simulation models for each telescope type (Prod6 includes models for large-size, medium-size, and small-size telescopes)</li> <li>CORSIKA input files defining (among others) site atmosphere, telescope positions, and interaction models;</li> <li>execution scripts required to run CORSIKA and sim_telarray.</li> </ul> <p>The CORSIKA air-shower simulation code is available from the Institute for Astroparticle Physics (KIT), see <a href="https://www.iap.kit.edu/corsika/index.php" target="_blank" rel="noopener">CORSIKA website</a>. The sim_telarray telescope simulation program, auxilliary libraries, and common configuration files are available at the <a href="https://www.mpi-hd.mpg.de/hfm/~bernlohr/sim_telarray/" target="_blank" rel="noopener">sim_telarray website</a>, with an up-to-date interface to CORSIKA at the <a href="https://www.mpi-hd.mpg.de/hfm/~bernlohr/iact-atmo/" target="_blank" rel="noopener">IACT/ATMO interface website</a>. For installation, copy all relevant tar.gz packages plus the ‘build_all’ script into the same directory and run `./build_all prod6 qgs2` (see `–help` for more options). Note that CORSIKA 7.7550 requires the corsika-77550.patch file available in bernlohr-1.68.tar.gz. Runing without it would lead to run-time errors. Placing the patch file in the top level of the directory structure is enough for the `build_all` script to pick it up.</p> <p>In cases for which the CTAO Simulation Telescope Models are used in a research project, we ask that the following acknowledgement is added in any resulting publication:</p> <p>“This research has made use of the CTAO Simulation Telescope Models provided by the CTAO Central Organisation and Consortium (version prod6 v1.0; [a]).”</p> <p>Please use the following BibTex Entry for [a] in the reference section of your publication: https://zenodo.org/records/14198379/export/bibtex</p> <p>References:</p> <p>[1] K.Bernlöhr, Simulation of imaging atmospheric Cherenkov telescopes with CORSIKA and sim_telarray, Astroparticle Physics 30 (2008) 149–158; <a href="https://arxiv.org/abs/0808.2253" target="_blank" rel="noopener">arXiv:0808.2253</a></p>
CTAO Simulation Telescope Models for CORSIKA and sim_telarray - prod3b
<p>The <a href="https://www.cta-observatory.org/">Cherenkov Telescope Array Observatory</a> (CTAO) will be the next-generation gamma-ray observatory under construction on the island of La Palma (Spain) and near Paranal (Chile). CTAO will cover a wide energy range and provide substantial improvements in sensitivity, angular resolution and energy resolution in comparison to any existing gamma-ray detector. Detailed Monte Carlo simulations allow us to optimise the instrument configuration and to estimate the observatory performance using realistic models of the telescope design. The CORSIKA air-shower simulation code and the sim_telarray code for simulation of arrays of Cherenkov telescopes are used for all CTAO Monte Carlo simulation productions.</p> <p>This repository provides access to the simulation configuration describing the site parameters and the telescope simulation models required for the generation of the <a href="https://doi.org/10.5281/zenodo.5163272">CTAO Instrument Response Functions - prod3b</a>.</p> <p>In detail, these are:</p> <ul> <li>telescope simulation models for each telescope type (prod3b includes models for large-size, medium-size, and small-size telescopes)</li> <li>CORSIKA input files defining (among others) site atmosphere, telescope positions, and interaction models;</li> <li>execution scripts required to run CORSIKA and sim_telarray.</li> </ul> <p>The CORSIKA air-shower simulation code is available from the Institute for Astroparticle Physics (KIT), see <a href="https://www.iap.kit.edu/corsika/index.php">CORSIKA website</a>. The sim_telarray telescope simulation program, auxilliary libraries, and common configuration files are available at the <a href="https://www.mpi-hd.mpg.de/hfm/~bernlohr/sim_telarray/">sim_telarray website</a>, with an up-to-date interface to CORSIKA at the <a href="https://www.mpi-hd.mpg.de/hfm/~bernlohr/iact-atmo/">IACT/ATMO interface website</a>. For installation, copy all relevant tar.gz packages plus the ‘build_all’ script into the same directory and run ‘./build_all prod3-la-palma qgs2' (see ‘--help’ for more options).</p> <p>In cases for which the CTAO Simulation Telescope Models are used in a research project, we ask that the following acknowledgement is added in any resulting publication:</p> <p>“This research has made use of the CTA Simulation Telescope Models provided by the CTA Observatory and Consortium (version prod3b v1.0; [a]).”</p> <p>Please use the following BibTex Entry for [a] in the reference section of your publication: <a href="https://zenodo.org/record/6219128/export/hx">https://zenodo.org/record/6219128/export/hx</a></p> <p>References:</p> <p>[1] K.Bernlöhr, Simulation of imaging atmospheric Cherenkov telescopes with CORSIKA and sim_telarray, Astroparticle Physics 30 (2008) 149–158; <a href="https://arxiv.org/abs/0808.2253">arXiv:0808.2253</a></p> <p>[2] A. Acharyya, for the CTA Consortium (2019), Monte Carlo studies for the optimisation of the Cherenkov Telescope Array layout, <a href="https://arxiv.org/abs/1904.01426">arXiv:1904.01426</a></p>
CTAO Simulation Telescope Models for CORSIKA and sim_telarray - prod5
<p>The <a href="https://www.cta-observatory.org/">Cherenkov Telescope Array Observatory</a> (CTAO) will be the next-generation gamma-ray observatory under construction on the island of La Palma (Spain) and near Paranal (Chile). CTAO will cover a wide energy range and provide substantial improvements in sensitivity, angular resolution and energy resolution in comparison to any existing gamma-ray detector. Detailed Monte Carlo simulations allow us to optimise the instrument configuration and to estimate the observatory performance using realistic models of the telescope design. The CORSIKA air-shower simulation code and the sim_telarray code for simulation of arrays of Cherenkov telescopes are used for all CTAO Monte Carlo simulation productions.</p> <p>This repository provides access to the simulation configuration describing the site parameters and the telescope simulation models required for the generation of the <a href="https://doi.org/10.5281/zenodo.5499839">CTAO Instrument Response Functions - prod5</a>.</p> <p>In detail, these are:</p> <ul> <li>telescope simulation models for each telescope type (prod5 includes models for large-size, medium-size, and small-size telescopes)</li> <li>CORSIKA input files defining (among others) site atmosphere, telescope positions, and interaction models;</li> <li>execution scripts required to run CORSIKA and sim_telarray.</li> </ul> <p>The CORSIKA air-shower simulation code is available from the Institute for Astroparticle Physics (KIT), see <a href="https://www.iap.kit.edu/corsika/index.php">CORSIKA website</a>. The sim_telarray telescope simulation program, auxilliary libraries, and common configuration files are available at the <a href="https://www.mpi-hd.mpg.de/hfm/~bernlohr/sim_telarray/">sim_telarray website</a>, with an up-to-date interface to CORSIKA at the <a href="https://www.mpi-hd.mpg.de/hfm/~bernlohr/iact-atmo/">IACT/ATMO interface website</a>. For installation, copy all relevant tar.gz packages plus the ‘build_all’ script into the same directory and run ‘./build_all prod5 qgs2’ (see ‘--help’ for more options).</p> <p>In cases for which the CTAO Simulation Telescope Models are used in a research project, we ask that the following acknowledgement is added in any resulting publication:</p> <p>“This research has made use of the CTA Simulation Telescope Models provided by the CTA Observatory and Consortium (version prod5 v1.0; [a]).”</p> <p>Please use the following BibTex Entry for [a] in the reference section of your publication: <a href="https://zenodo.org/record/6218687/export/hx">https://zenodo.org/record/6218687/export/hx</a></p> <p>References:</p> <p>[1] K.Bernlöhr, Simulation of imaging atmospheric Cherenkov telescopes with CORSIKA and sim_telarray, Astroparticle Physics 30 (2008) 149–158; <a href="https://arxiv.org/abs/0808.2253">arXiv:0808.2253</a></p> <p>[2] O.Gueta for the CTA Consortium and the CTA Observatory, The Cherenkov Telescope Array: layout, design and performance, Proceedings of the 37th International Cosmic Ray Conference (ICRC2021), Berlin, Germany; <a href="https://arxiv.org/abs/2108.04512">arXiv:2108.04512</a></p>
Local survey network and monitoring data of VLBI telescope at Metsähovi
<p>Observations of local surveying network and monitorin at Metsähovi. More information is in file Data_description.pdf.</p>
Assessing tropospheric turbulence impact on VGOS telescope placement in the Indian subcontinent for the estimation of Earth Orientation Parameters
<p>The dataset accompanying this study is composed of three distinct files, each integral to the research conducted. The file, named 'Simulated Data', includes the results derived from the simulations performed within this investigation. This file serves as a repository of the computed outcomes. The file, named 'Data and Code', includes the MATLAB scripts utilized to compute the Cn value from the Zenith Wet Delay (ZWD). Additionally, this file encompasses the relevant datasets for both wind speed and ZWD at various station locations. The third file contains the geographical coordinates of the Indian stations that were used in the study. Together, these files constitute a complete dataset that supports the study’s objectives and verification of the findings. </p>
SunspotsYoloDataset: annotated solar images captured with smart telescopes (January 2023 - May 2024)
<p><strong>SunspotsYoloDataset</strong> is a set of 1690+380+128 high-resolution RGB astronomical images captured with smart telescopes with specific solar filters and annotated with the positions of sunspots that are effectively in the images. Two instruments were used for several months from Luxembourg and France between January 2023 and May 2024: a Stellina smart telescope (<a href="https://vaonis.com/stellina">https://vaonis.com/stellina</a>) and a Vespera smart telescope (<a href="https://vaonis.com/vespera">https://vaonis.com/vespera</a>).</p> <p><strong>SunspotsYoloDataset</strong> can be used to train YOLO detection models on solar images, enabling the prediction of unexpected events such as Borealis Aurora with astronomical equipment accessible to the public.</p> <p><strong>SunspotsYoloDataset</strong> is formatted with the YOLO standard, i.e., with separated files for images and annotations, usable by state-of-the-art training tools and graphical software like MakeSense (<a href="https://www.makesense.ai">https://www.makesense.ai</a>). More precisely, there is a ZIP file containing RGB images in JPEG format (minimal compression), and text files containing the positions of sunspots. Each RGB image has a resolution of 640 × 640 pixels.</p> <p>For more details about the dataset, please contact the author: olivier.parisot@list.lu .</p> <p>For more information about Luxembourg of Science and Technology (LIST), please consult: <a href="https://www.list.lu">https://www.list.lu</a> .</p> <p> </p>
SURVEY OF IONIZED GAS OF THE GALAXY, MADE WITH THE ARECIBO TELESCOPE (SIGGMA): INNER GALAXY DATA RELEASE
<p>The Survey of Ionized Gas of the Galaxy, Made with the Arecibo telescope (SIGGMA) provides a fully-sampled view of the radio recombination line (RRL) emission from the portion of the Galactic plane visible by Arecibo. Observations use the Arecibo L-band Feed Array (ALFA), which has a FWHM beam size of 3 0 .4. Twelve hydrogen RRLs from H163α to H174α are located within the<br> instantaneous bandpass from 1225 MHz to 1525 MHz. We provide here cubes of average (“stacked”) RRL emission for the inner Galaxy region 32 ◦ ≤ ` ≤ 70 ◦ , |b| ≤ 1.5 ◦ , with an angular resolution of 6 0 . The stacked RRL rms at 5.1 km s<sup>−1</sup> velocity resolution is ∼ 0.65 mJy beam<sup>−1</sup> , making this the most sensitive large-scale fully-sampled RRL survey extant. We use SIGGMA data to catalogue 319 RRL detections in the direction of 244 known H ii regions, and 108 new detections in the direction of 79 HII region candidates. We identify 11 Carbon RRL emission regions, all of which are spatially coincident with known H ii regions. We detect RRL emission in the direction of 14 of the 32 supernova remnants (SNRs) found in the survey area. </p>
Hubble and Webb Space Telescope data for the cluster field RXJ-2129
<p>This repository contains reduced image mosaics from the Hubble and Webb Space Telescopes of the galaxy cluster RXJ-2129.</p> <p>Data were processed with the <a href="https://github.com/gbrammer/grizli">grizli</a> software pipeline, as described by <a href="https://arxiv.org/abs/2302.10936">Valentino et al. (2023, ApJ, in press)</a>, with the software and observatory calibrations available as of October 2022.</p> <p>For a given broad-band filter, the science data are given in the "sci.fits" files. Inverse variance weight images are provided in the "wht.fits" files. </p> <p>Aperture photometry following the methodology described by Valentino et al. is provided in "rxj2129-grizli-v4.0-fix_phot_apcorr.fits", and photometric redshift estimates derived with the <a href="https://github.com/gbrammer/eazy-py/">eazy-py </a>software are tabulated in "rxj2129-grizli-v4.0-fix.zout.fits".</p>
2m Perek telescope images of symmetrical object LAMOST J053944.81+531825.7
<p>The pictures of the object LAMOST J053944.81+531825.7 showing the unusual symmetric triple star configuration and complex emission line profiles. Images were taken by newly commissioned photometric camera G2 Mark II 3200 of Ondrejov 2m Perek telescope in primary focus. Plate scale 0.2 arcsec /pixel . The whole field is 7x5 arcmin. The distance of both satellites from the central bright star is 6.7 arcsec. The zoomed composed image is 16x16arcsec in SDSS spectral filter g' (left) and r' (right).</p> <p>Exposure time 300 s. Observed on 15th April 2020, 19:13 and 19:19 UTC respectively.</p> <p>The same region was observed by PanSTARRS-1 in the years 2011 to 2014. See for reference <a href="https://ps1images.stsci.edu/cgi-bin/ps1cutouts?pos=05+39+44.81+%2B53+18+25.7">PS1 image web service</a></p>
Dataset for the `Performance of the EUDET-type beam telescopes' publication (EPJ TI)
<p>This repository holds the data on which the publication `Performance of the EUDET-type beam telescopes' is based on.</p> <p>The substructure is as follows:</p> <p>Files in the range of run000060.raw until run000112.raw belong to a geometry with plane distance dz = 150 mm.<br> Files in the range of run000114.raw until run000171.raw belong to a geometry with plane distance dz = 20 mm.<br> A run corresponds to a doublet of beam energy and sensor threshold settings. The numbers are detailed in the README file.</p>
Tutorial Photonics Explorer Module 3 part 2: lenses, imaging rules, optical setups and telescopes
<p>Photonics Austria (PhAu) has conducted Teacher Training Programmes about Phoronics - the Photonics Explorer- in order to promote the potential of photonics to enliven physics lessons. This video is concerned with the topic polarisation and optical activity.</p> <p> </p>
Tutorial Photonics Explorer Module 3 part 1: lenses, imaging rules, optical setups and telescopes
<p>Photonics Austria (PhAu) has conducted Teacher Training Programmes about Photonics - the Photonics Explorer- in order to promote the potential of photonics to enliven physics lessons. This video tutorial contains several experiments designed to illustrate imaging equation and the laws of lenses.</p>
Sagittarius A lunar occultation measured by Dwingeloo Radio Telescope 2023-12-13
<p>This dataset contains raw spectra from the Lunar occultation of Sagittarius A on December 13, 2023. The data were obtained with the Dwingeloo Radio Telescope, which is operated by Stichting CAMRAS.</p> <p>Three bands are measured:</p> <ul> <li>1418MHz, 6MHz wide. The spectra show absorption and emission of the hydrogen line.<br> <ul> <li>Spectra with 2000 bins, integration time 0.2 seconds (corrected for bandpass).</li> <li>Total power with integration time 1 second.</li> </ul> </li> <li>1330MHz, 10MHz wide. <ul> <li>Spectra with 5000 bins, integration time 1 second.</li> <li>Total power with integration time 1 second.</li> </ul> </li> <li>415MHz, 4MHz wide. This data is severely affected by radio frequency interference.<br> <ul> <li>Spectra with 2000 bins, integration time 1 second.</li> <li>Total power with integration time 1 second.</li> </ul> </li> </ul> <p>The telescope was tracking Sagittarius A* during the occultation. The altitude ranged from 1 to 8 degrees above the horizon during the measurements. This is very low, leading to quite severe radio frequency interference. Partially, these are caused by LTE masts transmitting at 1456 MHz, for which the receiving system is insufficiently shielded. All frequencies are topocentric, i.e. no LSR-correction has been applied.</p> <p>Files are in the ECSV format, which can be read with Astropy, or with any other program that can read CSV-data (such as Microsoft Excel). Apart from the spectra, also telescope pointing information and exact times are stored in every row.</p>
An unusual pulse shape change event in PSR J1713+0747 observed with the Green Bank Telescope and CHIME: Profile data and figure reproduction scripts
<p>This Zenodo entry contains data used in the paper "An unusual pulse shape change event in PSR J1713+0747 observed with the Green Bank Telescope and CHIME", to be published in The Astrophysical Journal. This includes minimally processed profile data in PSRFITS format, as well as pulsar ephemerides (.par files), time-of-arrival estimates (.tim files), and scripts which can be used to reproduce the figures and tables in the paper. For more information, see README.md.</p>
Solar and meteorological data collected from the Radio Telescope Bras D'Eau station (Mauritius) by the ENERGY-Lab at the University of La Reunion between November 2015 and March 2023
<p>Scientific data provided by ENERGY-Lab located at the University of La Reunion. These data come from solar and meteorological stations present in the following territories: La Reunion, Comoros, Madagascar, Mauritius, Seychelles and South Africa. A THREDDS Data Server was created as part of the IOS-net (Indian Ocean Solar Network, https://galilee.univ-reunion.fr) project which aims to study the solar field and the optimisation of intelligent solar energy systems in the countries of the IOC (Indian Ocean Commission). These data are served by Unidata's Thematic Realtime Environmental Distributed Data Services (THREDDS) Data Server (TDS) in a variety of interoperable data services and output formats.</p> <p>Dataset is available from the THREDDS Data Server to this url: <a href="https://galilee.univ-reunion.fr/thredds/catalog/dataStations/catalog.html"> https://galilee.univ-reunion.fr/thredds/catalog/dataStations/catalog.html</a>.</p> <p>Data are also viewable and exploitable on the mobile application of the IOS-net project. The SolarIO app is downloadable in all stores.</p> <p><strong><em>ENERGY-Lab data may be reused, provided that related metadata explaining the data has been reviewed by the user, and that the data are appropriately acknowledged.</em></strong></p>
WINTER: a new near-IR survey telescope
<p>The Wide-Field Infrared Transient Explorer (WINTER) is a new time-domain instrument which will perform a seeing-limited survey of the near-infrared sky. I will present the design and science goals of the WINTER instrument, which will be deployed on a dedicated 1-meter robotic telescope at Palomar Observatory. Among the many near-infrared targets of interest, WINTER is principally designed for follow-up of kilonovae from binary neutron star and neutron star-black hole mergers detected in gravitational waves. WINTER will be sensitive to kilonovae with 90% localization areas smaller than 150 (450) square degrees out to a distance of 350 (200) Mpc. In addition to kilonova follow-up, WINTER will conduct a wide range of time-domain surveys to a depth of J=21 magnitudes, building up a deep co-added image of the near-infrared sky and studying near-infrared transients including supernovae, tidal disruption events, and transiting exoplanets around low mass stars. WINTER’s custom camera combines six commercial large-format Indium Gallium Arsenide (InGaAs) sensors, observing in Y, J, and a short-H (Hs) band filters (0.9-1.7 microns), and employs a novel tiled optical design to cover a >1 degree squared field of view with 90% fill factor. I will include updates on the final integration of the WINTER instrument and commissioning at Palomar Observatory.</p>
Repository 2 of 2 of the Level 0 (raw FITS) images from the DMI Mauna Loa Earthshine telescope experiment (2010-2012)
<h2>Raw data upload</h2> <p>These are tar files of the raw data obtained with the earthshine refractor conceived, designed and built by Danish Meteorological Institute and Lunds Observatory and operated on Mauna Loa at the NOAA observatory during 2011-2012.</p> <p>The present doi relates to one of two - each one holds roughly 50Gb tar file. Get all for the complete dataset. The other doi is: 10.5281/zenodo.11442378</p> <p>The data are in the form of FITS files. There are data for 5 different photometric filters - Johnson B and V and then 3 red or nIR filters - IRCUT, VE1 and VE2. Some frames are without filters.</p> <p>Examples:</p> <p>2455945.1760145MOON_B_AIR.fits.gz - image of the Moon through the B filter</p> <p>2455945.0413946DARK_DARK.fits.gz - a DARK frame image taken with same exposure time as the adjacent MOON image. <br>A DARK is typically taken before and after all MOON images.</p> <p>The file-naming strategy for the file inside the archive files is simple - names start with the (fractional) Julian day of the observation, followed by target name and two indicators of the filters or other light-path devices that were used, e.g.: _VE1_AIR indicates the VE1 colour filter with just 'air' (ie nothing) in the second option. The second option may include names of knife-edge devices or neutral density filters that could be inserted.</p> <p>There are also some FLAT images taken on inside of dome or of the sky or of the Hohlraum source.</p> <p>The MOON images may well be 100-image 3D-cubes taken within a minute or two.</p> <p>Future upgrades (in new dois, but in this Community) will include dark-frame subtracted, aligned and averaged images (Level 1). A Level 2 may include actual model fits of the full lunar disks, in which terrestrial albedo is a model-parameter.</p> <p>The file called "index_justJD.csv" lists which Julian days are present in which archive file. Note that some days are spread over several tar files.</p> <p>The images were acquired with the remotely-operated telescope by Peter Thejll, Hans Gleinser, Chris Flynn, as well as Henriette Schwarz.</p> <p>Notes updated May 3 2024.</p> <p>Peter Thejll</p> <p>write pth@dmi.dk for queries</p>
Repository 1 of 2 of the Level 0 (raw FITS) images from the DMI Mauna Loa Earthshine telescope experiment (2010-2012)
<h2>Raw data upload</h2> <p>These are tar files of the raw data obtained with the earthshine refractor conceived, designed and built by Danish Meteorological Institute and Lunds Observatory and operated on Mauna Loa at the NOAA observatory during 2011-2012.</p> <p>The present doi relates to one of two - each one holds roughly 50Gb tar file. Get all for the complete dataset. The other doi is: 10.5281/zenodo.11500335</p> <p>The data are in the form of FITS files. There are data for 5 different photometric filters - Johnson B and V and then 3 red or nIR filters - IRCUT, VE1 and VE2. Some frames are without filters.</p> <p>Examples:</p> <p>2455945.1760145MOON_B_AIR.fits.gz - image of the Moon through the B filter</p> <p>2455945.0413946DARK_DARK.fits.gz - a DARK frame image taken with same exposure time as the adjacent MOON image. <br>A DARK is typically taken before and after all MOON images.</p> <p>The file-naming strategy for the file inside the archive files is simple - names start with the (fractional) Julian day of the observation, followed by target name and two indicators of the filters or other light-path devices that were used, e.g.: _VE1_AIR indicates the VE1 colour filter with just 'air' (ie nothing) in the second option. The second option may include names of knife-edge devices or neutral density filters that could be inserted.</p> <p>There are also some FLAT images taken on inside of dome or of the sky or of the Hohlraum source.</p> <p>The MOON images may well be 100-image 3D-cubes taken within a minute or two.</p> <p>Future upgrades (in new dois, but in this Community) will include dark-frame subtracted, aligned and averaged images (Level 1). A Level 2 may include actual model fits of the full lunar disks, in which terrestrial albedo is a model-parameter.</p> <p>The file called "index_justJD.csv" lists which Julian days are present in which archive file. Note that some days are spread over several tar files.</p> <p>The images were acquired with the remotely-operated telescope by Peter Thejll, Hans Gleinser, Chris Flynn, as well as Henriette Schwarz.</p> <p>Notes updated May 3 2024.</p> <p>Peter Thejll</p> <p>write pth@dmi.dk for queries</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.