J/MNRAS/496/2422ivo://CDS.VizieR/J/MNRAS/496/2422doi:10.26093/cds/vizier.74962422CDSHawkins K.Lucey M.Curtis J.2024-08-21T20:15:14Z2020-07-21T06:41:21ZCDS support team

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

cds-question@unistra.frmilky-way-galaxychemical-abundancesvisible-astronomyspectroscopyRecently, a new cylindrical-shaped stream of stars, up to 700pc long, was discovered hiding in the Galactic disk using kinematic data enabled by the Gaia mission. This curious stream of stars, dubbed the Pisces-Eridanus stream, was initially thought to be as old as 1Gyr, yet its stars shared a rotation period distribution consistent with the 120-Myr-old Pleiades cluster. In this work, we explore the detailed chemical nature of this stellar stream. We carried out high-resolution spectroscopic follow-up of 42 Pisces-Eridanus stream stars using McDonald Observatory, and combined these data with information for 40 members observed with the low-resolution LAMOST spectroscopic survey. Together, these data enabled us to measure the abundance distribution of light/odd-Z (Li, C, Na, Al, Sc, V), {alpha} (Mg, Si, Ca, Ti), Fe-peak (Cr, Mn, Fe, Co, Ni, Zn), and neutron capture (Sr, Y, Zr, Ba, La, Nd, Eu) elements across the Pisces-Eridanus stream. We find that the stream is (1) near solar metallicity with [Fe/H] = -0.03 dex and (2) has a metallicity spread of 0.07 dex (or 0.04 dex when removing outliers). We also find that (3) the abundance of Li indicates that Pisces-Eridanus is ~120Myr old, consistent with the gyrochronology result. We find that (4) the stream has a [X/Fe] abundance spreads of 0.06<{sigma}_[X/Fe]_<0.20dex in most elements, and (5) no significant abundance gradients across its major axis except a potentially weak gradient in [Si/Fe]. These results together show that the Pisces-Eridanus stream is a uniquely close, young, chemically interesting laboratory for testing our understanding of star and planet formation.2020MNRAS.496.2422Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/496/2422CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toI/345 : Gaia DR2 (Gaia Collaboration, 2018)J/A+A/622/A13 : VLA double-double radio galaxy candidates imageshttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/496/2422https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/496/2422http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/496/2422https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/496/2422https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/496/2422http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/496/2422GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/496/2422/table1 (Observational properties of observed targets)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/496/2422/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/496/2422/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/496/2422/table1?GETtext/xml+votable180.050000true36.947711.24090.0055555555555555566/175 17259 17359 17407 17497 17701 17715 17736 17859 18103 18312 18642 18655 18824 18876 18895 18932 19199 19241 19243 19249 19270 19273 19336 19381 19438 19461 19465 19480 19505 19617 19629 20000 22648 22691 22721 22724 22728 36696 36799 36805https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/496/2422?format=asciiOpticaldefaultJ/MNRAS/496/2422/table1Observational properties of observed targetsSimbadSimbad column added by the CDSmeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGaiaDR2Gaia DR2 Source IDmeta.id;meta.mainRA_ICRSGaia DR2 right ascension (ICRS) at Ep=2015.5degpos.eq.ra;meta.main_DE.icrsDeclination (ICRS) at Epoch=J2015.5 (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.decnullableindexed_RA.icrsRight ascension (ICRS) at Epoch=J2015.5 (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.ranullableindexedLAMOST[Y/N] whether each observed star has also been observed in the LAMOST surveymeta.codecharDE_ICRSGaia DR2 declination (ICRS) at Ep=2015.5degpos.eq.dec;meta.mainPlxGaia DR2 parallaxmaspos.parallaxfloate_PlxGaia DR2 parallax errormasstat.error;pos.parallaxfloatRVGGaia DR2 radial velocitykm/sphys.veloc;pos.heliocentricfloate_RVGGaia DR2 radial velocity errorkm/sstat.errorfloatRVRadial velocity, this workkm/sphys.veloc;pos.heliocentricfloate_RVRadial velocity error, this workkm/sstat.errorfloatXGalactic X position (1)pcpos.distance;pos.cartesian.x;pos.galacticfloatYGalactic Y position (1)pcpos.distance;pos.cartesian.y;pos.galacticfloatZGalactic Z position (1)pcpos.distance;pos.cartesian.z;pos.galacticfloatSNRSignal-to-noise ratio measured in at the continuum level at ~5350{AA} of our optical spectrapixel**-1stat.snrintGAIA2Display the Gaia DR2 data (Gaia Coll., 2018, Cat. I/345)meta.ref.urlcharJ/MNRAS/496/2422/table3Stellar atmospheric parameters and chemical abundances of observed targetso_ALiNumber of Li linesmeta.numberinte_Teffrms uncertainty on TeffKstat.error;phys.temperature.effectiveintloggSurface gravitylog(cm.s**-2)phys.gravityfloate_loggrms uncertainty on logglog(cm.s**-2)stat.errorfloat[Fe/H]Metallicity, [Fe/H]phys.abund.Zfloate_[Fe/H]rms uncertainty on [Fe/H]stat.error;phys.abund.FefloatvmicroMicro-turbulent velocitykm/sphys.veloc.microTurbfloate_vmicrorms uncertainty on vmicrokm/sstat.errorfloat[Na/Fe]Abundance [Na/Fe]phys.abundfloate_[Na/Fe]rms uncertainty on [Na/Fe]stat.error;phys.abundfloato_[Na/Fe]Number of Na linesmeta.numberintALi? Li abundancephys.abundfloatnullablee_ALi? rms uncertainty on AListat.errorfloatnullable[Mg/Fe]Abundance [Mg/Fe]phys.abundfloate_[Mg/Fe]rms uncertainty on [Mg/Fe]stat.error;phys.abundfloato_[Mg/Fe]Number of Mg linesmeta.numberint[Al/Fe]? Abundance [Al/Fe]phys.abundfloatnullablee_[Al/Fe]? rms uncertainty on [Al/Fe]stat.error;phys.abundfloatnullableo_[Al/Fe]Number of Al linesmeta.numberint[Si/Fe]Abundance [Si/Fe]phys.abundfloate_[Si/Fe]rms uncertainty on [Si/Fe]stat.error;phys.abundfloato_[Cr/Fe]Number of Cr linesmeta.numberfloat[Cu/Fe]Abundance [Cu/Fe]phys.abundfloate_[Cu/Fe]rms uncertainty on [Cu/Fe]stat.error;phys.abundfloato_[Cu/Fe]Number of Cu linesmeta.numberint[Zn/Fe]? Abundance [Zn/Fe]phys.abundfloatnullablee_[Zn/Fe]? rms uncertainty on [Zn/Fe]stat.error;phys.abundfloatnullableo_[Zn/Fe]Number of Zn linesmeta.numberint[Sr/Fe]? Abundance [Sr/Fe]phys.abundfloatnullablee_[Sr/Fe]? rms uncertainty on [Sr/Fe]stat.error;phys.abundfloatnullableo_[Sr/Fe]Number of Sr linesmeta.numberint[Y/Fe]Abundance [Y/Fe]phys.abundfloate_[Y/Fe]rms uncertainty on [Y/Fe]stat.error;phys.abundfloato_[Y/Fe]Number of Y linesmeta.numberint[Zr/Fe]? Abundance [Zr/Fe]phys.abundfloatnullablee_[Zr/Fe]? rms uncertainty on [Zr/Fe]stat.error;phys.abundfloatnullableo_[Zr/Fe]Number of Zr linesmeta.numberint[Ba/Fe]Abundance [Ba/Fe]phys.abundfloate_[Ba/Fe]rms uncertainty on [Ba/Fe]stat.error;phys.abundfloato_[Ba/Fe]Number of Ba linesmeta.numberint[La/Fe]Abundance [La/Fe]phys.abundfloate_[La/Fe]rms uncertainty on [La/Fe]stat.error;phys.abundfloato_[La/Fe]Number of La linesmeta.numberint[Nd/Fe]Abundance [Nd/Fe]phys.abundfloate_[Nd/Fe]rms uncertainty on [Nd/Fe]stat.error;phys.abundfloato_[Nd/Fe]Number of Nd linesmeta.numberint[Eu/Fe]? Abundance [Eu/Fe]phys.abundfloatnullablee_[Eu/Fe]? rms uncertainty on [Eu/Fe]stat.error;phys.abundfloatnullableo_[Eu/Fe]Number of Eu linesmeta.numberintGAIA2Display the Gaia DR2 data (Gaia Coll., 2018, Cat. I/345)meta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGaiaDR2Gaia DR2 Source IDmeta.id;meta.mainTeffEffective temperatureKphys.temperature.effectiveinto_[Si/Fe]Number of Si linesmeta.numberint[Ca/Fe]Abundance [Ca/Fe]phys.abundfloate_[Ca/Fe]rms uncertainty on [Ca/Fe]stat.error;phys.abundfloato_[Ca/Fe]Number of Ca linesmeta.numberint[Ti/Fe]Abundance [Ti/Fe]phys.abundfloate_[Ti/Fe]rms uncertainty on [Ti/Fe]stat.error;phys.abundfloato_[Ti/Fe]Number of Li linesmeta.numberint[V/Fe]Abundance [V/Fe]phys.abundfloate_[V/Fe]rms uncertainty on [V/Fe]stat.error;phys.abundfloato_[V/Fe]Number of V linesmeta.numberint[Sc/Fe]Abundance [Sc/Fe]phys.abundfloate_[Sc/Fe]rms uncertainty on [Sc/Fe]stat.error;phys.abundfloato_[Sc/Fe]Number of Sc linesmeta.numberfloat[Cr/Fe]Abundance [Cr/Fe]phys.abundfloate_[Cr/Fe]rms uncertainty on [Cr/Fe]stat.error;phys.abundfloat[Mn/Fe]Abundance [Mn/Fe]phys.abundfloate_[Mn/Fe]rms uncertainty on [Mn/Fe]stat.error;phys.abundfloato_[Mn/Fe]Number of Mn linesmeta.numberfloat[Co/Fe]Abundance [Co/Fe]phys.abundfloate_[Co/Fe]rms uncertainty on [Co/Fe]stat.error;phys.abundfloato_[Co/Fe]Number of Co linesmeta.numberfloat[Ni/Fe]Abundance [Ni/Fe]phys.abundfloate_[Ni/Fe]rms uncertainty on [Ni/Fe]stat.error;phys.abundfloato_[Ni/Fe]Number of Ni linesmeta.numberint