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33 results for “LOFAR”
LOFAR Observation (MS file) from the Boötes Field and the Toothbrush cluster used in the paper: "Looking beyond pixels with continuous-space EstimAtion of Point sources"
<p>The dataset contains the measurement sets (MS file) of the LOFAR observations from the Boötes field and the Toothbrush cluster. The dataset was used in the experiments of the paper: </p> <blockquote> <p>LEAP: Looking beyond pixels with continuous-spaceEstimAtion of Point sources</p> <p>Pan, H., Simeoni, M., Hurley, P., Blu, T. & Vetterli, M. In: Astronomy & Astrophysics, in press, 2017</p> </blockquote> <p>The data was provided as a collaboration between ASTRON and IBM within the DOME project. The data was acquired for a LOFAR sky survey of the Boötes field:</p> <blockquote> <p>LOFAR 150-MHz observations of the Boötes field: Catalogue and Source Counts</p> <p>Williams, W. L. , Hardcastle, M. J. & 33 others In: Monthly Notices of the Royal Astronomical Society. 460, 3, p. 2385–2412</p> </blockquote> <p>and the Toothbrush cluster (RX J0603.3+4214):</p> <blockquote> <p>Simulating the toothbrush: evidence for a triple merger of galaxy clusters</p> <p>Brüggen, M., van Weeren, R. J., Röttgering, H. J. A. In: Monthly Notices of the Royal Astronomical Society: Letters. 425, 1, p. L76--L80</p> </blockquote> <p>In case of questions concerning the measurement set, please contact the original authors for details.</p> <p> </p> <p>We have also included the three catalogs used in the experiments, which are converted from their original FITS table to Numpy arrays:</p> <ul> <li>skycatalog.npz is the catalog of the Boötes field: https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stw1056</li> <li>TGSSADR1_7sigma_catalog.npz is the TGSS ADR1 source catalog: http://tgssadr.strw.leidenuniv.nl/catalogs/TGSSADR1_7sigma_catalog.fits</li> <li>NVSS_CATALOG.npz is the NRAO/VLA Sky Survey: ftp://nvss.cv.nrao.edu/pub/nvss/CATALOG/</li> </ul>
CSV equivalent of LOFAR ACC files
<p>These are conversions of LOFAR ACC files by Griffin Foster from <a href="https://zenodo.org/record/840405/files/20120513_052251_acc_512x192x192.dat">https://zenodo.org/record/840405</a> to demonstrate the use of the ACC to CSV converter developed at DIAS</p>
Pulse Profiles and Times of Arrival Measurements from a Rotating Radio Transient Census with the Irish LOFAR station
<p>The reduced data produced as a part of a census of rotating radio transients (RRATs) with the Irish LOFAR station.</p> <p> </p> <p>This deposit contains:</p> <ul> <li>Metadata regarding observed data</li> <li>A copy of RFI-zapped, single pulse archives</li> <li>A copy of the time-flattened periodic emission archives</li> <li>A copy of the measured pulse times of arrival</li> <li>Ephemerides used and produced as a part of the work</li> </ul> <p>Additional data can be made available on request to the author.</p>
LOFAR dataset for deep learning assisted data Inspection for radio astronomy
<p>This dataset is used for the training of the magnitude and phase-based VAE in the paper entitled "Deep learning assisted data inspection for radio astronomy".</p> <p>For uploading purposes the dataset has been separated into 4 different .zip files. In order to use this dataset each of the zip files should be extracted into a single directory so that the training can be performed on all files at the same time. <br> <br> More information can be found on <a href="https://github.com/mesarcik/DL4DI">the project github repository</a>. </p>
Example LOFAR Station Correlations
<p>Example cross-correlation data sets from the LOFAR stations at Chilbolton Observatory and Onsala Space Observatory. Used in the python SWHT package (https://github.com/griffinfoster/SWHT) and station imaging scripts (https://github.com/griffinfoster/lss).</p>
Reproduction package for "Searching for low radio-frequency gravitational wave counterparts in wide-field LOFAR data"
<p>This is a basic reproduction package for the paper "Searching for low radio-frequency gravitational wave counterparts in wide-field LOFAR data" by Gourdji et al. (2021) published in MNRAS. It describes the software and settings used to obtain the final data products of the analysis. It also includes a Jupyter notebook and required data to reproduce the tables and figures of this paper.</p>
Plots of Observations of CasA from LOFAR Station IE613 HBA against Frequency, Altitude and Azimuth
<p>A series of plots of the variation of linear polarisation channels and Stokes parameters of an observation of CasA on the 16th-17th March 2018 against frequency and local horizontal coordinates.</p>
Sample ACC Data Set for LOFAR Station IE613 LBA whole sky observation
<p>This is a large sample of data from Station IE613 suitable for use with <a href="https://github.com/creaneroDIAS/beamModelTester">beamModelTester</a> and <a href="https://github.com/2baOrNot2ba/iLiSA">iLiSA</a>. To use with these systems, transfer it to a directory of the form :</p> <p><em>{STN_ID}_YYYYMMDD_HHMMSS_rcu{RCU_MODE}<em>dur{DURATION}</em>{SOURCE}_acc</em><br> e.g. IE613_20180406_091321_rcu3_dur85635_CasA_acc</p>
Sample single frequency plots of various channels against Altitude and Azimuth for LOFAR single station
<p>Sample of outputs indicating the variation in stokes and linear polarisation channels for LOFAR single station</p>
LOFAR Carbon Footprint and Energy Consumption
<p>The LOw Frequency ARray (LOFAR) is a European radio telescope operating since 2010 in the frequency bands 10 - 80 MHz and 110 - 250 MHz. This Excel model provides an analysis of the energy consumption and the carbon footprint of LOFAR. The analysis uses a Life Cycle Analysis following the Green House Gas protocol. Results include the footprint stemming from operations of all LOFAR stations and central processing. The impact of a number of typical science projects is analyzed as well. This model provides a transparent baseline to the sustainability of LOFAR and can serve as a blueprint for the analysis of other research infrastructures.</p>
The Energy consumption and Carbon Footprint of the LOFAR Telescope V2.0
<p>The LOw Frequency ARray (LOFAR) is a European radio telescope operating since 2010 in the frequency bands 10 - 80 MHz and 110 - 250 MHz. This article provides an analysis of the energy consumption and the carbon footprint of LOFAR. The approach used is a Life Cycle Analysis (LCA). We find that one year of LOFAR operations requires 3,627 MWh of electricity, 48,714 m3 gas and 135,497 liters of fuel. The associated carbon emission is 2,624 tCO2e/year. Results include the footprint stemming from operations of all LOFAR stations and central processing, but exclude scientific post-processing and activities. The potential recovery of embodied footprint in construction materials at the end of life equals 17%. The electrical energy required for scientific processing is assessed separately. It ranges from 1% (standard The Energy Consumption and Carbon Footprint of the LOFAR Telescope imaging and time-domain), to 40% (wide field long baseline imaging) of the energy consumption for the observation. The outcome provides<br> a transparent baseline in making LOFAR more sustainable and can serve as a blueprint for the analysis of other research infrastructures.</p>
LOFAR Interferometric Dataset
<p>This dataset represents the output snapshot images (from the WSClean software) of solar type III radio bursts observed by the LOFAR/LBA instrument (max. baseline around 76 km) on April 3, 2019, between 12:15 - 12:45 UT.<br> <a href="http://arxiv.org/abs/2310.02677">Reference to the paper</a></p>
Reproduction package for 'Low-frequency radio observations of recurrent nova RS Ophiuchi with MeerKAT and LOFAR'
<p>This is a basic reproduction package for the paper "Low-frequency radio observations of recurrent nova RS Ophiuchi with MeerKAT and LOFAR".</p><p> </p><p> </p>
Reproduction package for the paper "A LOFAR sample of luminous compact sources coincident with nearby dwarf galaxies"
<p>Scripts to reproduce analyses from Vohl et al. 2023, A&A.</p>
HETDEX-LOFAR Spectroscopic Redshift Catalog
<p>We combine the power of blind integral field spectroscopy from the Hobby-Eberly Telescope (HET) Dark Energy Experiment (HETDEX) with sources detected by the Low Frequency Array (LOFAR) to construct the HETDEX-LOFAR Spectroscopic Redshift Catalog. Starting from the first data release of the LOFAR Two-metre Sky Survey (LoTSS), including a value-added catalog with photometric redshifts, we extracted 28,705 HETDEX spectra. Using an automatic classifying algorithm, we assigned each object a star, galaxy, or quasar label along with a velocity/redshift, with supplemental classifications coming from the continuum and emission line catalogs of the internal, fourth data release from HETDEX (HDR4). We measured 9,087 new redshifts; in combination with the value-added catalog, our final spectroscopic redshift sample is 9,710 sources. This new catalog contains the highest substantial fraction of LOFAR galaxies with spectroscopic redshift information; it improves archival spectroscopic redshifts, and facilitates research to determine the [O II] emission properties of radio galaxies from 0.0 < z < 0.5, and the Lyα emission characteristics of both radio galaxies and quasars from 1.9 < z < 3.5. Additionally, by combining the unique properties of LOFAR and HETDEX, we are able to measure star formation rates (SFR) and stellar masses. Using the Visible Integral-field Replicable Unit Spectrograph (VIRUS), we measure the emission lines of [O III], [Ne III], and [O II] and evaluate line-ratio diagnostics to determine whether the emission from these galaxies is dominated by AGN or star formation.</p> <p> </p> <p>The catalog is comprised of one FITS file with two extensions:</p> <ul> <li>No. 0 (1036, 28705): The first extension contains the spectrum, of length 1036, for each object. The corresponding wavelength values range from 3470 - 5540 angstroms.</li> <li>No. 1 (28705 rows x 13 columns): The second extension contains the derived values found for each source. The table below describes each column: <table> <tbody> <tr> <td><strong>COLUMN NAME</strong></td> <td><strong>DESCRIPTION</strong></td> <td><strong>DATA TYPE</strong></td> </tr> <tr> <td>objID</td> <td>LoTSS Object ID</td> <td>string</td> </tr> <tr> <td>source_name</td> <td>Source Name</td> <td>string</td> </tr> <tr> <td>RA</td> <td>PanSTARRS1 Right Ascension (J2000)</td> <td>float</td> </tr> <tr> <td>Dec</td> <td>PanSTARRS1 Declination (J2000)</td> <td>float</td> </tr> <tr> <td>z_diagnose</td> <td>Best fit redshift from Diagnose</td> <td>float</td> </tr> <tr> <td>z_hdr4</td> <td>Best fit redshift from ELiXer</td> <td>float</td> </tr> <tr> <td>z_archive</td> <td>Spectroscopic redshift from value-added LoTSS catalog</td> <td>float</td> </tr> <tr> <td>z_best</td> <td>HETDEX-LOFAR redshift</td> <td>float</td> </tr> <tr> <td>z_best_src</td> <td>1 = Diagnose, 2 = HDR4, 3 = Archive</td> <td>integer</td> </tr> <tr> <td>classification</td> <td>STAR, AGN, LOWZGAL, HIGHZGAL, or ARCHIVE</td> <td>string</td> </tr> <tr> <td>log_mass</td> <td>MCSED derived stellar mass</td> <td>float</td> </tr> <tr> <td>log_SFR</td> <td>MCSED derived star formation rate</td> <td>float</td> </tr> <tr> <td>log_L150</td> <td>MCSED derived 150 MHz luminosity</td> <td>float</td> </tr> </tbody> </table> </li> </ul> <p> </p> <p>We request that the following acknowledgement be included in any paper using HETDEX-LOFAR data:</p> <blockquote> <p>HETDEX is led by the University of Texas at Austin McDonald Observatory and Department of Astronomy with participation from the Ludwig-Maximilians-Universität München, Max-Planck-Institut für Extraterrestrische Physik (MPE), Leibniz-Institut für Astrophysik Potsdam (AIP), Texas A&M University, Pennsylvania State University, Institut für Astrophysik Göttingen, The University of Oxford, Max-Planck-Institut für Astrophysik (MPA), The University of Tokyo and Missouri University of Science and Technology.</p> <p>Observations for HETDEX were obtained with the Hobby-Eberly Telescope (HET), which is a joint project of the University of Texas at Austin, the Pennsylvania State University, Ludwig-Maximilians-Universität München, and Georg-August-Universität Göttingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Visible Integral-field Replicable Unit Spectrograph (VIRUS) was used for HETDEX observations. VIRUS is a joint project of the University of Texas at Austin, Leibniz-Institut für Astrophysik Potsdam (AIP), Texas A&M University, Max-Planck-Institut fürExtraterrestrische Physik (MPE), Ludwig-Maximilians-Universität München, Pennsylvania State University, Institut für Astrophysik Göttingen, University of Oxford, and the Max-Planck-Institut fur Astrophysik (MPA).</p> <p>Funding for HETDEX has been provided by the partner institutions, the National Science Foundation, the State of Texas, the US Air Force, and by generous support from private individuals and foundations.</p> </blockquote> <p>We request that the following papers are cited when using any HETDEX-LOFAR data:</p> <p>Debski, M. H., Zeimann, G. R., Hill, G. J., et al. 2024, arXiv e-prints, arXiv:2411.08974, doi: 10.48550/arXiv.2411.08974</p>
Animated plots of the spectrum and polarisation of Cassiopeia A based on a 24 hour observation with LOFAR Station IE613 (LBA)
<p>This collection of animated plots over time of the variation in channel flux for the linear polarisation channels XX, XY and YY and Stokes Parameters U, V, I and Q against frequency for Cassiopeia A as observed at LOFAR station SE607 between 2018-04-06 and 2018-04-07 using the LBA</p>
Animated plots of the spectrum and polarisation of Cassiopeia A based on a 24 hour observation with LOFAR Station IE613 (LBA)
<p>This collection of animated plots over time of the variation in channel flux for the linear polarisation channels XX, XY and YY and Stokes Parameters U, V, I and Q against frequency for Cassiopeia A as observed at LOFAR station IE613 between 2018-04-06 and 2018-04-07 using the LBA</p>
Animated Plots of the variance of observed data from LOFAR Station IE613
<p>This series of animated plots illustrates the variation of the linear polarisation channels and Stokes parameters for an observation of CasA from LOFAR station IE613 against altitude and azimuth throughout the frequency range of LOFAR HBA.</p>
Sample clean frequency set for use with LOFAR station SE607 and beamModelTester
<p>This is a pair of files each containing a list of frequencies with low RFI as observed from LOFAR Station SE607 designed for use with the tutorial for beamModelTester.</p>
Appendix Figures B.1–B.7 from the article 'Core Prominence as a Signature of Restarted Jet Activity in the LOFAR Radio-Galaxy Population' (Accepted for publication in the journal Astronomy & Astrophysics on August 23, 2024)
<p><strong>Figure captions:</strong></p> <p> </p> <p><strong>Figs. B.1–B.5.</strong> Images of 69 candidate restarted galaxies selected based on high radio $\mathrm{CP_{1400}}$ combined with low SB of extended emission, a steep spectrum of the core, and USS extended emission coupled with a bright core and summarised in Tables A.1 and A.2. Radio contours from VLA FIRST maps (white, $5^{\prime\prime}$), LOFAR high-resolution maps (black, $6^{\prime\prime}$), and NVSS maps (purple, $45^{\prime\prime}$) are overlaid on the LOFAR low-resolution resolution maps (orange, $20^{\prime\prime}$). The contouring of all the maps is made at $\,\sigma_\mathrm{local}\times(-3,3,5,10,20,30,40,50,100,150,200)$ levels, with $\sigma_\mathrm{local}$ representing the local RMS noise of the corresponding maps. The host galaxy position is marked with a yellow cross.</p> <p> </p> <p><strong>Figs. B.6–B.7. </strong>Images of sources excluded from the sample of restarted candidates following the criteria discussed in Sect. 3.1, Sect. 3.2 and Sect. 3.3 and summarised in Tables A.3 and A.4. Radio contours from VLA FIRST maps (white, $5^{\prime\prime}$), LOFAR high-resolution maps (black, $6^{\prime\prime}$), and NVSS maps (purple, $45^{\prime\prime}$) are overlaid on the LOFAR low-resolution resolution maps (orange, $20^{\prime\prime}$). The contouring of all the maps is made at $\,\sigma_\mathrm{local}\times(-3,3,5,10,20,30,40,50,100,150,200)$ levels, with $\sigma_\mathrm{local}$ representing the local RMS noise of the corresponding maps. The host galaxy position is marked with a yellow cross.</p> <p> </p>
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