J/ApJ/857/111ivo://CDS.VizieR/J/ApJ/857/111doi:10.26093/cds/vizier.18570111CDSTakahashi K.Yoshida T.Umeda H.2019-05-10T11:06:44Z2019-03-28T09:31:21ZCDS support team

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

cds-question@unistra.frchemical-abundancesstellar-evolutionary-modelsRecent theory predicts that first stars are born with a massive initial mass of >~100M_{sun}_. Pair-instability supernova (PISN) is a common fate for such massive stars. Our final goal is to prove the existence of PISNe and thus the high-mass nature of the initial mass function in the early universe by conducting abundance profiling, in which properties of a hypothetical first star is constrained by metal-poor star abundances. In order to determine reliable and useful abundances, we investigate the PISN nucleosynthesis taking both rotating and nonrotating progenitors for the first time. We show that the initial and CO core mass ranges for PISNe depend on the envelope structures: nonmagnetic rotating models developing inflated envelopes have a lower shifted CO mass range of ~70-125_M{sun}_, while nonrotating and magnetic rotating models with deflated envelopes have a range of ~80-135_M{sun}_. However, we find no significant difference in explosive yields from rotating and nonrotating progenitors, except for large nitrogen production in nonmagnetic rotating models. Furthermore, we conduct the first systematic comparison between theoretical yields and a large sample of metal-poor star abundances. We find that the predicted low [Na/Mg]~-1.5 and high [Ca/Mg]~0.5-1.3 abundance ratios are the most important to discriminate PISN signatures from normal metal-poor star abundances, and confirm that no currently observed metal-poor star matches with the PISN abundance. An extensive discussion on the nondetection is presented.2018ApJ...857..111Thttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/857/111CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/ApJS/155/651 : Evolution of extremely metal-poor stars (Herwig+, 2004)J/A+A/490/769 : Yields from extremely metal-poor stars (Campbell+, 2008)J/ApJ/681/1524 : Detailed abundances for 28 metal-poor stars (Lai+, 2008)J/ApJ/724/975 : Abundances of metal-poor stars (Roederer+, 2010)J/ApJ/742/54 : CASH project II. 14 EMP stars (Hollek+, 2011)J/MNRAS/412/843 : SAGA extremely metal-poor stars (Suda+, 2011)J/A+A/537/A146 : Stellar models with rotation. 0.8<M<120 (Ekstrom+, 2012)J/other/Sci/337.444 : RV curves of Galactic massive O stars (Sana+, 2012)J/AJ/145/13 : Metal-poor stars from SDSS/SEGUE. I. Abundances (Aoki+, 2013)J/ApJ/764/21 : Stellar evolutionary models with 13-120Msun (Chieffi+, 2013)J/ApJ/778/56 : Hamburg/ESO Survey extremely metal-poor stars (Cohen+, 2013)J/A+A/558/A103 : Stellar models with rotation. 0.8<M<120 (Georgy+, 2013)J/ApJ/762/27 : Most metal-poor stars. III. [Fe/H]<=-3.0 stars (Yong+, 2013)J/ApJ/762/26 : Most metal-poor stars. II. Galactic halo stars (Yong+, 2013)J/A+A/566/A146 : Pair-instability supernovae models (Kozyreva+, 2014)J/ApJ/781/40 : Metal-poor stars from HES survey. II. (Placco+, 2014)J/AJ/147/136 : Stars of very low metal abundance. VI. (Roederer+, 2014)J/ApJ/807/171 : SkyMapper Survey metal-poor star spectrosc. (Jacobson+, 2015)J/A+A/606/A55 : Rotational mixing in CEMP-s stars (Matrozis+, 2017)J/ApJ/857/46 : Modelled vs obs. abundances of EMP stars (Ishigaki+, 2018)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/857/111https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/857/111http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/857/111https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/857/111https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/857/111http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/857/111GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJ/857/111/table5 (Stellar sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/857/111/table5?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/857/111/table5?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/857/111/table5?GETtext/xml+votable180.050000true178.4055139-2.01020170.0055555555555555566/4639 8228 16514 16665 16666 17040 17159 17253 17353 17357 17460 17642 18511 18582 18683 18707 18768 18778 19083 25595 25753 26366 28059 28540 29001 31377 31585 33464 33470 33471 33635 33703 33708 34600 35009 35395 35408 35553 35750 35889 36098 36737 38935 38953 42308 42326 43926 44460 44575 44776 45401 45468 45470 45504 45591 45796 46563 46646 47193 47204 47217 47306 47344 47360 47389 47458 47852 48162 48375 48625 48862https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJ/857/111?format=asciidefaultJ/ApJ/857/111/table2Model propertiesu_Etot[)] Flag on Etotmeta.code.errorcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintModModel (G1)meta.notecharMini[100/290] Initial model masssolMassphys.mass;meta.modelledintMfin[94.7/290] Final model masssolMassphys.mass;meta.modelledfloatVini[0/806] Surface rotation velocitykm/sphys.veloc.rotatintVini/Vk[0/0.3] Vini to Vk value (1)stat.fit.omcfloattauH[1.5/2.5] Lifetime of the core hydrogen burning stageMyrtime.lifetime;phys.abund.XfloattauHe[2.6/3.4] Lifetime of the core helium burning stage100000yrtime.lifetime;phys.abund.YfloatMcHe[45.9/150] Mass of the Helium and carbon coresolMassphys.mass;meta.modelledfloatMcCO[42/140.1] Mass of the carbon-oxygen coresolMassphys.mass;meta.modelledfloatFateFate (2)meta.codecharEtot[1/94.5]? Explosion energy in 10^51^ erg units1e+44Jphys.energyfloatnullableM56Ni[0.009/48]? Ejected ^56^Ni masssolMassphys.mass;meta.modelledfloatnullableu_M56Ni[)] Flag on Etotmeta.code.errorcharYieldsDisplay the yields results for this model (link to Table 3) if anymeta.numberintnullableJ/ApJ/857/111/table5Stellar sampleSimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSeq[1/72] Sequential IDmeta.id;meta.mainintNameObject namemeta.idchar[Fe/H][-4.2/-1.8]? Fe/H abundancephys.abund.Fefloatnullable[Na/Mg][-0.7/1.4]? Na/Mg abundancephys.abundfloatnullable[Al/Mg][-1.5/0]? Al/Mg abundancephys.abundfloatnullable[Si/Mg][0.1/1]? Si/Mg abundancephys.abundfloatnullable[Ca/Mg][-0.4/0.5]? Ca/Mg abundancephys.abundfloatnullablel_[Sc/Mg]Limit flag for [Sc/Mg]meta.code.errorchar[Sc/Mg][-1.1/0.3]? Sc/Mg abundancephys.abundfloatnullablel_[Zn/Fe]Limit flag for [Zn/Fe]meta.code.error;phys.abundchar[Zn/Fe][-3.3/1.4]? Zn/Fe abundancephys.abundfloatnullableRefsReferences (1)meta.ref;pos.framechar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/ApJ/857/111/yieldsPair-instability supernova (PISN) yields for the models (table 3)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintModModel (G1)stat.param;meta.modelledcharMini[160/280] Initial model mass, solar unitssolMassmeta.unit;phys.mass;meta.modelledintElementElement, in LaTeX formattingphys.atmol.elementYield[1.6e-33/85] Yield, solar unitssolMassphys.composition.yielddouble