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<ri:Resource created="2025-05-06T15:07:19Z" status="active" updated="2025-07-01T06:26:59Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>Euclid final merged catalog. Q1 data release</title><shortName>II/388</shortName><identifier>ivo://CDS.VizieR/II/388</identifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Euclid Collaboration</name></creator><creator><name>Mellier Y.</name></creator><creator><name>Abdurrouf</name></creator><creator><name>Acevedo Barroso J.A.,Achucarro A.</name></creator><creator><name>Adamek J.</name></creator><creator><name>Adam R.</name></creator><creator><name>Addison G.E.</name></creator><creator><name>Aghanim N.</name></creator><creator><name>Aguena M. et al.</name></creator><date role="Updated">2025-07-01T06:26:59Z</date><date role="Created">2025-05-06T15:07:19Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>surveys</subject><subject>photometry</subject><subject>visible-astronomy</subject><subject>infrared-astronomy</subject><description>The current standard model of cosmology successfully describes a variety of measurements, but the nature of its main ingredients, dark matter and dark energy, remains unknown. Euclid is a medium-class mission in the Cosmic Vision 2015-2025 programme of the European Space Agency (ESA) that will provide high-resolution optical imaging, as well as near-infrared imaging and spectroscopy, over about 14000deg^2^ of extragalactic sky. In addition to accurate weak lensing and clustering measurements that probe structure formation over half of the age of the Universe, its primary probes for cosmology, these exquisite data will enable a wide range of science. This paper provides a high-level overview of the mission, summarising the survey characteristics, the various data-processing steps, and data products. 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VIS band source flux error from the Sersic fit (FLUXERR_VIS_SERSIC)</description><unit>uJy</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>e_FluxYSer</name><description>? NIR Y band source flux error from the Sersic fit (FLUXERR_Y_SERSIC)</description><unit>uJy</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>e_FluxJSer</name><description>? NIR J band source flux error from the Sersic fit (FLUXERR_J_SERSIC)</description><unit>uJy</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>e_FluxHSer</name><description>? NIR H band source flux error from the Sersic fit (FLUXERR_H_SERSIC)</description><unit>uJy</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>FlagVis</name><description>[0/10] Objects flag keeping track of the flagged pixels in the VIS flag image (FLAG_VIS)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>FlagY</name><description>[0/10] Objects flag keeping track of the flagged pixels in the NIR Y flag image (FLAG_Y)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>FlagJ</name><description>[0/10] Objects flag keeping track of the flagged pixels in the NIR J flag image (FLAG_J)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>FlagH</name><description>[0/10] Objects flag keeping track of the flagged pixels in the NIR H flag image (FLAG_H)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>FlagNIR</name><description>[0/10] Objects flag keeping track of the flagged pixels in the NIR stack flag image (FLAG_NIR_STACK)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>FlagDeblend</name><description>[0/1] Flag marking if the object was originally blended with another one (DEBLENDED_FLAG)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>ParentID</name><description>ID of the parent sources of a deblended object (PARENT_ID)</description><ucd>meta.id.parent</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>ParentVisNIR</name><description>ID of the parent sources of a deblended object (PARENT_VISNIR)</description><ucd>meta.id.parent</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>FlagPL</name><description>[1]? Point-like flag (POINT_LIKE_FLAG) (1)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType">int</dataType><flag>nullable</flag></column><column><name>PPL</name><description>? Probability between 0 and 1 that the source is point-like (POINT_LIKE_PROB) (2)</description><ucd>stat.fit.goodness</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>FlagSpur</name><description>[0/1] Spurious source flag (SPURIOUS_FLAG)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>PSpur</name><description>Probability between 0 and 1 that the source is spurious (SPURIOUS_PROB)</description><ucd>stat.fit.goodness</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>magSG</name><description>? Magnitude used to compute POINT_LIKE_PROB (MAG_STARGAL_SEP)</description><unit>mag</unit><ucd>phot.mag</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>FQualDet</name><description>Detection step flags that could indicate the possible corruption of the MAG_STARGAL_SEP values (DET_QUALITY_FLAG)</description><ucd>meta.code.qual</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>muMax</name><description>? Peak surface brightness above the background in the detection band (directly from SExtractor) (MU_MAX)</description><unit>mag.arcsec**-2</unit><ucd>phot.mag.sb</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>Diffmu</name><description>? The difference between MU_MAX and MAG_STARGAL_SEP; valid even for NIR-only sources (MUMAX_MINUS_MAG)</description><unit>mag.arcsec**-2</unit><ucd>phot.mag.sb</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>SegArea</name><description>Isophotal area of the source above the analysis threshold (SExtractor ISOAREA_IMAGE) (SEGMENTATION_AREA)</description><unit>pix</unit><ucd>phys.angSize</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>amaj</name><description>Semi-major axis of the source (from Asterism) (SEMIMAJOR_AXIS)</description><unit>pix</unit><ucd>phys.angSize;src</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>PA</name><description>[-90/90] Position angle (CCW/x) of the source (SExtractor THETA_IMAGE) (POSITION_ANGLE)</description><unit>deg</unit><ucd>pos.posAng</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Ell</name><description>A parametrization of how stretched an object is in the detection band (ELLIPTICITY) (3)</description><ucd>src.ellipticity</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>RadKron</name><description>? Major semi-axis (in pixels) of the elliptical aperture used for total (Kron) aperture photometry on the detection image (KRON_RADIUS)</description><unit>pix</unit><ucd>phys.angSize;src</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>FWHM</name><description>FWHM (in arcsec) used in a-phot to compute colors (FWHM) (4)</description><unit>arcsec</unit><ucd>phys.angSize</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>E(B-V)</name><description>Estimated galactic E(B-V) at the source centroid according to the reference Planck map (GAL_EBV)</description><unit>mag</unit><ucd>phot.color;em.opt.B;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>e_E(B-V)</name><description>Error on galactic E(B-V) according to the reference Planck map (GAL_EBV_ERR)</description><unit>mag</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>Gaia</name><description>The associated GAIA source id (GAIA_ID)</description><ucd>meta.id</ucd></column><column><name>QualGaia</name><description>? The quality of the GAIA match (GAIA_MATCH_QUALITY)</description><ucd>meta.code.qual</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column></table></schema></tableset></ri:Resource>