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10 results for “Parallax”

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zenodo44/100

UniDAM results with Gaia eDR3 parallaxes

<p>Results of UniDAM run with Gaia eDR3 parallaxes included.</p> <p>+------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | &nbsp; &nbsp; &nbsp; &nbsp; Survey &nbsp; &nbsp; &nbsp; &nbsp; | Input catalogue size | Stars with estimates &nbsp;| &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; Reference &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; |<br> | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;| &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;| &nbsp; &nbsp; &nbsp;done using &nbsp; &nbsp; &nbsp; | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; |<br> | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;| &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;| &nbsp;Gaia eDR3 parallaxes | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | APOGEE (DR16) &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;| &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; 473307 | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;326884 | Ahumada et al. (2020) &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | Bensby &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;714 | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; 547 | Bensby et al. (2014) &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;|<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | Gaia-ESO (DR3) &nbsp; &nbsp; &nbsp; &nbsp; | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;25533 | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; 20127 | Gilmore et al. (2012) G.Gilmore&amp; S.Randich (2016) |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | GALAH (DR3) &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;| &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; 564620 | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;505403 | Buder et al. (2020) &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | GCS &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;| &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;13565 | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;7633 | Casagrande et al. (2011) &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;|<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | LAMOST (DR6) &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;5581266 | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; 4377103 | Luo et al. (2015) &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | LAMOST MRS (DR6) &nbsp; &nbsp; &nbsp; | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; 328187 | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;223407 | Luo et al. (2015) &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | RAVE (DR6) &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; 491349 | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;347211 | Steinmetz et al. (2020) &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | SEGUE &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;| &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; 235595 | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;180012 | Yanny et al. (2009) &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+<br> | Total (unique sources) | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp;5856273 | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; 4616931 | &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; |<br> +------------------------+----------------------+-----------------------+---------------------------------------------------+</p>

opencc-by-4.0Dec 2020View details →
zenodo44/100

Accuracy or positions and parallaxes

<p>Two figures from a report soon to be placed on arXiv:&nbsp;</p> <p><strong>Astrometric Accuracy of Positions</strong></p> <p>Erik H&oslash;g, Niels Bohr Institute, Copenhagen University</p> <p><span>Figure 1. <span>The </span></span><span>accuracy of observed star positions for 2000 years, marked with red color for observations from the ground and with blue from space. The accuracy was greatly improved shortly before 1600 AD by the Landgrave in Kassel and by Tycho Brahe in Denmark. The following 400 years brought even larger but much more gradual improvement before space techniques with the European Hipparcos satellite started a new era of astrometry. Catalogs before 1900 are plotted at the mean epoch of observation, but after 1900 at the time of publication. &ndash; The 17 million brightest stars in the sky have accuracies of 0.014 milliarcsec </span></p> <p>Figure 1b. Astrometric accuracy, update of Fig.5 from 1995 to our 2024 knowledge, including both parallaxes and positions. Gaia produces millions of accurate proper motions and parallaxes in addition to the positions shown in this diagram, see Gaia DR3 (2022). The important astrometry from space obtained with the HST should also be mentioned, and the very accurate astrometry by interferometry with radio telescopes.</p>

opencc-by-4.0Apr 2024View details →
zenodo44/100

Spectrophotometric Parallaxes

<p>Spectrophotometric distances to 44,784 RGB stars predicted with a data-driven model combining spectroscopy from APOGEE DR14 and photometric information from 2MASS, Gaia, and WISE. The columns show 2MASS ID, parallax measurements from Gaia DR2 and their uncertainty, predicted spectrophotometric parallaxes and uncertainties, whether the star is part of our training set or not, and whether it is in sample A or B. For details please refer to Hogg, Eilers &amp; Rix (2018).</p> <p>If the data is being used, please cite Hogg, Eilers &amp; Rix (2018), as well as Gaia, 2MASS, WISE, APOGEE, and SDSS-IV.</p> <p>&nbsp;</p>

opencc-by-4.0Oct 2018View details →
zenodo40/100

Distances for the Gaia RV set with corrected parallaxes

<p>The datasets are described in <a href="https://arxiv.org/abs/1902.02355">https://arxiv.org/abs/1902.02355</a> , which is submitted to MNRAS.</p> <p>Each file contains a distance derivation under different assumptions for the Gaia RV dataset.</p> <p>Please note the following: to allow for freedom in choice of cuts, we have limited ourselves to just minimal cuts: parallax/parallaxerr &gt; 3, detected G,G_BP,G_RP magnitudes &gt; 0 mag, vlos_err &lt; 10 km/s, n_vis &gt; 5, reasonably measured RV (&lt;5550 km/s), distance and 1/parallax &lt; 10 kpc</p> <p>Note that these cuts are NOT sufficient to ensure quality of the sample. We strongly advise to use the quality criteria laid out in Schoenrich, McMillan and Eyer (2019), and test for the effects of a cut in galactic latitude b &gt; 10 degrees for most applications.</p> <p>The file format is .csv (comma separated) with the following columns (a key is in row 1)<br> index: running number in our sample<br> sourceid: Gaia Source ID<br> E_dist: expectation value for the distance, unit is kpc<br> distm2: second moment of distance probability distribution (use the usual formula to get the variance/dispersion)<br> distm3: third moment of distance probability distribution<br> distm4: fourth moment &quot;&quot;&quot;&quot;<br> parallax: The Gaia parallax _including_ the offset correction chosen, unit is mas<br> parallax/parallaxerr : ratio of parallax to parallax uncertainty. Again, both parallax and parallaxerror contain the corrections. Use this and the last column to obtain the parallax uncertainty for quality cuts<br> x: x coordinate (radial coordinate in local cartesian frame), unit is kpc<br> y: y coordinate in the azimuthal direction, unit is kpc<br> z: z coordinate (perpendicular to the plane), relative to the Sun, unit is kpc. Please add the solar offset from the plane that you favor (0.02 kpc, Joshi et al., or the Gerhard &amp; Bland-Hawthorn review are good values)<br> R: galactocentric radius (in-plane, cylindrical coordinates), unit is kpc<br> U_g: cylindrical radial velocity in a galactocentric frame (positive taken inwards), unit is km/s<br> v_phi: azimuthal velocity (V_g, azimuthal direction), unit is km/s<br> v_z: velocity component upwards perpendicular to the plane, unit is km/s<br> vlos: line-of-sight velocity as provided in the Gaia RV datasets<br> vloserr: line-of-sight velocity error as provided in the Gaia RV datasets<br> gl: Galactic longitude l (degrees)<br> gb: Galactic latitude b (degrees)<br> pml: proper motion in l (mas/yr)<br> pmb: proper motion in b (mas/yr)<br> pml_err: proper motion error/uncertainty in l (mas/yr)<br> pmb_err: proper motion error in b (mas/yr)<br> E_bprp: BP-RP excess flux factor (provided in Gaia catalogue)<br> excessnoise: astrometric excess noise<br> Gmag: Gaia G magnitude<br> Rmag: Gaia G_RP magnitude<br> B-Rcolour: G_BP - G_RP&nbsp; (colour in mag)<br> nvis: number of visibility periods<br> eclat: ecliptic latitude (degrees)</p> <p>Each file contains a different set of assumptions that result in a near-zero average distance bias, as discussed in the paper:</p> <p>We recommend using either:<br> gaiaRVdelp54delsp43 : Increased parallax uncertainty by 0.043 mas in quadrature, corrected for parallax offset of 0.054 mas</p> <p>gaiaRVdelpeqspdelsp43 : Increased parallax uncertainty by 0.043 mas in quadrature, corrected for a parallax offset = modified parallax error</p> <p>For comparison and applications that need long-range in distance s, it may be interesting to use:<br> gaiaRVdelp48delsp00 : only increased parallaxes by an offset of 0.048 mas. Distance bias on average is stable out to 4kpc or more, but you have to be wary of random errors.</p> <p><br> All distances were derived with the standard prior described in Schoenrich, McMillan and Eyer (2019); the parameter for the additional exponential function in the prior at very large s &gt; 4 kpc is 0.06/kpc</p> <p>If you need specific subsamples of stars, we advice to draw a new prior with the method of Schoenrich &amp; Aumer (2017) and then re-derive the distances. We are also happy to help with that and provide you with the necessary code.</p> <p>Please note that our definition (angular distance per time in the direction of l, b) of pml and pmb is frequently noted with a * in other derivations.</p> <p>Please also note that why we used z_Sun = 0.02 kpc in the underlying analysis and distance prior, the value in the catalogue is given relative to the Sun (i.e. add the Solar offset that you favour).</p>

opencc-by-4.0Feb 2019View details →
zenodo40/100

Radio Parallax of the Crab Pulsar Data Release

<p>This is the companion dataset to the publication <strong>&quot;Radio Parallax of the Crab Pulsar: A First VLBI Measurement Calibrated with Giant Pulses&quot;&nbsp;</strong>by <em>Lin, et al., (2023, submitted, preprint:&nbsp;<a href="https://arxiv.org/abs/2306.01617">https://arxiv.org/abs/2306.01617</a>)</em>.</p> <p>The FITS files contain images of the Crab Pulsar, SE_CAND3 and NE_CAND4 sources created from <a href="https://www.evlbi.org/">European VLBI Network</a> EK036A-D observations using the technique described in the paper. See the <strong>README.md</strong> and paper&nbsp;for more details.</p>

opencc-by-4.0May 2023View details →
dryad36/100

Ventral motion parallax enhances fruit fly steering to visual sideslip

Open the record for dataset details and reuse information.

publicApr 2020View details →
zenodo32/100

Parallax xrd-ct datasets

<p>Simulated and experimental xrd-ct sinogram data containing parallax artefacts (0-180 deg scans).</p>

opencc-by-4.0Sep 2023View details →
zenodo28/100

Parallax_AI4QC

<div>This dataset was used in the AI4QC project (Artificial Intelligence for Quality Control), in the context of parallax detection through an object detection task. It consists of a set of labeled parallax artefacts. This effect appears as a colorful pattern in images where cloud/heavy haze is present. Bounding boxes were defined around parallax artefacts in 1764 Sentinel-2 true colour images (jpg format). A parallax artefact appears mostly over clouds, although it can also be found over land. The bounding boxes are associated to one out of four labels:</div> <div>&nbsp;</div> <div>0 : Parallax - Cloud (9529 bounding boxes)<br>1 : Parallax - Land (245 bounding boxes)<br>2 : Other Anomaly (4 bounding boxes)<br>3 : Missing Data - Land (2 bounding boxes)</div> <div>&nbsp;</div> <div>The label files are available in COCO format (json files). Two sets of labels are available: rotated_bboxes and straight_bboxes. This comes from the fact that parallax artefacts are often rotated on the image. The "rotated_bboxes" folder contains labels with an additional attribute which is a rotation value. These bounding boxes will contain only the rotated parallax artefact and not the background. However since most machine learning models don't account for a rotation value, straight bounding boxes were created as well. These are found in the "straight_bboxes" folder and the bounding boxes will contain some of the background as well as the parallax.&nbsp;</div> <div>&nbsp;</div> <div>One can combine the label files with the S2 images to train object detection algorithms to automatically detect parallax effects in a satellite image. A predefined train/test split is available (80% training and 20% testing), with training and testing zip folders containing the images and labels for each subset. The data was split according to 2 criterias: parallax over cloud vs land and geographic location.&nbsp;</div>

restrictedcc-by-4.0Oct 2024View details →
zenodo28/100

Sentinel-2 parallax-based cloud detection - sample dataset

<p>This repository archives the Sentinel-2 sample data used in:</p> <p>D. Frantz, E. Ha&szlig;, A. Uhl, J. Stoffels, and J. Hill (2018): Improvement of the Fmask algorithm for Sentinel-2 images: Separating clouds from bright surfaces based on parallax effects. Remote Sensing of Environment 215, 471-481.&nbsp;<a href="https://doi.org/10.1016/j.rse.2018.04.046">https://doi.org/10.1016/j.rse.2018.04.046</a></p>

openAug 2021View details →
zenodo24/100

Evaluating the effects of parallax in archaeological geometric morphometric analyses

<p>Geometric morphometric dataset for Epipalaeolithic microliths. These files include the data used in the publication&nbsp;<em>Evaluating the effects of parallax in archaeological geometric morphometric analyses,&nbsp;</em>submitted to Archaeological and Anthropological Sciences, as well as the image files.&nbsp;</p>

opencc-by-4.0May 2020View details →

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