J/A+A/481/411ivo://CDS.VizieR/J/A+A/481/411doi:10.26093/cds/vizier.34810411CDSDesert F.-X.Macias-Perez J.F.Mayet F.Giardino G.Renault C.,Aumont J.Benoit A.Bernard J.-P.Ponthieu N.Tristram M.2017-06-20T13:16:31Z2008-05-06T22:23:54ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frinterstellar-mediummillimeter-astronomysubmillimeter-astronomyArcheops is a balloon-borne experiment, mainly designed to measure the Cosmic Microwave Background (CMB) temperature anisotropies at high angular resolution (~12 arcminutes). By-products of the mission are shallow sensitivity maps over a large fraction of the sky (about 30 %) in the millimetre and submillimetre range at 143, 217, 353 and 545GHz. From these maps, we produce a catalog of bright submillimetre point sources. We present in this paper the processing and analysis of the Archeops point sources. Redundancy across detectors is the key factor allowing us to distinguish glitches from genuine point sources in the 20 independent maps. We look at the properties of the most reliable point sources, totalling 304. Fluxes range from 1 to 10000Jy (at the frequencies covering 143 to 545GHz). All sources are either planets (2) or of galactic origin. The longitude range is from 75 to 198-degrees. Some of the sources are associated with the well-known Lynds Nebulae and HII compact regions in the galactic plane. A large fraction of the sources have an IRAS counterpart. Except for Jupiter, Saturn, the Crab and Cas A, all sources show a dust-emission-like modified blackbody emission spectrum. Temperatures cover a range from 7 to 27K. For the coldest sources (T<10K), a steep nu^beta^ emissivity law is found with a surprising beta~3 to 4. An inverse relationship between T and beta is observed. The number density of sources at 353GHz with flux brighter than 100Jy is of the order of 1 per degree of Galactic longitude. These sources will provide a strong check for the calibration of the Planck HFI focal plane geometry as a complement to planets. These very cold sources observed by Archeops should be prime targets for mapping observations by the Akari and Herschel space missions and ground-based observatories.2008A&A...481..411Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/481/411CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/397/213 : Galactic HII regions (Paladini+, 2003)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/481/411https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/481/411http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/481/411https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/481/411https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/481/411http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/481/411GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/481/411/table34 (Cloud position, fluxes, model fit parameters and associations)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/481/411/table34?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/481/411/table34?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/481/411/table34?GETtext/xml+votable180.050000true286.582532.0208330.0055555555555555565/3920 6/341 597 860-862 881 1031 1048 1050 1054 1061 1063 1082 1090 1159 1168 1231 1287 1538-1539 1542 1781 1790 1824 1850 1930 1959 1963 3005 3011 3035 3037 3039 3047 3061 3067-3069 3071 3157 3161 3175 3183 3194 3198 3268 3282 3290 3301-3303 3306 3308 3311 3349 3459 3466 3482 3497 3605 3611 3627-3628 3630-3631 3633 3641 3645 3648-3650 3689-3690 3692-3693 3725 3730 3732 3735-3737 3744 3746-3750 3753 3755 3757 14014 14031 14205 14254-14255 14263 14266-14267 14269 14279 14285-14286 14290 14293-14294 14299 14304 14306 14309-14310 14312 14314 14317 14319 14323 14328-14329 14333-14334 14515 14622 14637 14644 14647 14652 14666-14667 14670-14671 14677 14682-14683 14688-14690 14692-14693 14697 14699 14701-14702 14704 14706-14707 14709 14713 14716 14719 14741 15362 15368 15370-15371 15374 15383 15385 15390 15394 15403 15408-15409 15412 15415 15421 15423 15427 15430 15435 15440 15442 15447 15449 15453 15458 15464 15473 15477 15479 15488 15541 15564 15569 15578 15582 15589 15607 15626-15629 15634-15636 15642 15645 15665 15667 15671 15685 15689 15697 15700 15707 15713-15714 15716 15718 15720-15721 15725 15728-15730 15749 15752-15753 15759 15761 15767 15778-15779 15781-15782 15785 15810 15941 15962 15964 16128 23541 23549 23763 23770 23773-23774 23795 23798 23807 23938 23946 23969-23970 23974 23980 23982 23991 23996 23998-23999 24040 24093 24177 24185 24189 24191 24203 24325 24337 24352 24365 24367 24378 24427 24487 245541.6558465556080236e-21 3.953759050367298e-21https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/481/411?format=asciiRadiodefaultJ/A+A/481/411/table34Cloud position, fluxes, model fit parameters and associationsT? TemperatureKphys.temperaturefloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordint[DMM2008][1/302] Sequential numbermeta.idintArchArch name (GLLL.ll+BB.bb)meta.id;meta.maincharn_Arch[*] * for positional uncertainty >4' (1sigma)meta.notecharRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainl_F143Limit flag on F143meta.code.errorcharF143Flux density at 143GHzJyphot.flux.density;em.mm.100-200GHzfloate_F143rms uncertainty on F143Jystat.errorfloatl_S/N143Limit flag on S/N143meta.code.errorcharS/N143Signal-to-noise ratio for F143stat.snrintl_F217Limit flag on F217meta.code.errorcharF217Flux density at 217GHzJyphot.flux.density;em.mm.200-400GHzfloate_F217rms uncertainty on F217Jystat.errorfloatl_S/N217Limit flag on S/N217meta.code.errorcharS/N217Signal-to-noise ratio for F217stat.snrintl_F353Limit flag on F353meta.code.errorcharF353? Flux density at 353GHzJyphot.flux.density;em.mm.200-400GHzintnullablee_F353? rms uncertainty on F353Jystat.errorintnullablel_S/N353Limit flag on S/N353meta.code.errorcharS/N353? Signal-to-noise ratio for F353stat.snrintnullablel_F545Limit flag on F545meta.code.errorcharF545? Flux density at 545GHzJyphot.flux.density;em.mm.400-750GHzintnullablee_F545? rms uncertainty on F545Jystat.errorintnullablel_S/N545Limit flag on F545meta.code.errorcharS/N545? Signal-to-noise ratio for F545stat.snrintnullablebeta? Emissivity exponent betastat.fit.paramfloatnullablee_beta? rms uncertainty on betastat.errorfloatnullablee_T? rms uncertainty on TKstat.errorfloatnullablechi2r? Reduced chi^2^ valuestat.fit.chi2floatnullablebeta11? Emissivity exponent beta for fixed T=11Kstat.fit.paramfloatnullablee_beta11? rms uncertainty on beta11stat.errorfloatnullableT2? Temperature for fixed beta=2Kphys.temperaturefloatnullablee_T2? rms uncertainty on T2Kstat.errorfloatnullableIRASAssociated IRAS sourcemeta.idcharn_IRAS[*] * for IRAS source having IRAS colours of an ultra-compact HII regionmeta.notecharF100um? IRAS flux at 100umJyphot.flux.density;em.IR.60-100umfloatnullableF60um? IRAS flux at 60umJyphot.flux.density;em.IR.30-60umfloatnullableName(s)Associations with a commonly used name with Lynds Dark Nebulae, Bright Nebulae, Sharpless and other common catalogsmeta.idchar