J/MNRAS/395/1409ivo://CDS.VizieR/J/MNRAS/395/1409doi:10.26093/cds/vizier.73951409CDSSmartt S.J.Eldridge J.J.Crockett R.M.Maund J.R.2024-07-08T20:15:45Z2015-09-30T14:21:06ZCDS support team

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

cds-question@unistra.frsupernovaeWe present the results of a 10.5-yr, volume-limited (28-Mpc) search for supernova (SN) progenitor stars. In doing so we compile all SNe discovered within this volume (132, of which 27 per cent are Type Ia) and determine the relative rates of each subtype from literature studies. The core-collapse SNe break down into 59 per cent II-P and 29 per cent Ib/c, with the remainder being IIb (5 per cent), IIn (4 per cent) and II-L (3 per cent). There have been 20 II-P SNe with high-quality optical or near-infrared pre-explosion images that allow a meaningful search for the progenitor stars. In five cases they are clearly red supergiants, one case is unconstrained, two fall on compact coeval star clusters and the other twelve have no progenitor detected. We review and update all the available data for the host galaxies and SN environments (distance, metallicity and extinction) and determine masses and upper mass estimates for these 20 progenitor stars using the stars stellar evolutionary code and a single consistent homogeneous method. A maximum likelihood calculation suggests that the minimum stellar mass for a Type II-P to form is m_min_= 8.5^+1^_-1.5_M_{sun}_ and the maximum mass for II-P progenitors is m_max_= 16.5+/-1.5M_{sun}_, assuming a Salpeter initial mass function holds for the progenitor population (in the range {Gamma}=-1.35^+0.3^_-0.7_). The minimum mass is consistent with current estimates for the upper limit to white dwarf progenitor masses, but the maximum mass does not appear consistent with massive star populations in Local Group galaxies. Red supergiants in the Local Group have masses up to 25M_{sun}_ and the minimum mass to produce a Wolf-Rayet star in single star evolution (between solar and LMC metallicity) is similarly 25-30M_{sun}_. The reason we have not detected any high-mass red supergiant progenitors above 17M_{sun}_ is unclear, but we estimate that it is statistically significant at 2.4{sigma} confidence. Two simple reasons for this could be that we have systematically underestimated the progenitor masses due to dust extinction or that stars between 17-25M_{sun}_produce other kinds of SNe which are not II-P. We discuss these possibilities and find that neither provides a satisfactory solution. We term this discrepancy the 'red supergiant problem' and speculate that these stars could have core masses high enough to form black holes and SNe which are too faint to have been detected. We compare the ^56^Ni masses ejected in the SNe to the progenitor mass estimates and find that low-luminosity SNe with low ^56^Ni production are most likely to arise from explosions of low-mass progenitors near the mass threshold that can produce a core-collapse.2009MNRAS.395.1409Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/395/1409CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toB/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)II/256 : Sternberg Supernova Catalogue, 2004 version (Tsvetkov+, 2004)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/395/1409https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/395/1409http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/395/1409https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/395/1409https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/395/1409http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/395/1409GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/395/1409/tablea1 (SNe discovered between 1998-2008.5 in galaxies with recessional velocities less than 2000km/s)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/395/1409/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/395/1409/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/395/1409/tablea1?GETtext/xml+votable180.050000true167.4597083-23.72863890.0055555555555555566/2372 3929 4447 5200 5244 5492 5504 5587 5589 5629 5715 5751 5797 5925 5975 5999 6082 7241 7385-7386 7424 7534 7584 7606 7743 8106 8195 8256 9437 10475 10632 10892 10905 10927 10935 11000 11027 11246-11247 11435 12015 12018 15592-15593 15847 15955 16120 16441 17340 17509 17592 17614 17761 18398 19710 20722 20739 21109 21198 22751 23528 24878 24949 25127 25344 25452 25513 25599 25788 25958 25960 25999 26068 26234 26303 26336 26432 27426 27512 27588 27727 27766 27828 27855 27907 27948 27955 28035 28045 28123 28213 28348 28517 30970 31882 33228 34361 34493 34531 34534 34701 35536 35966 35993 36045 36081 36131 36213 36287 36450 36789 37429 37436 38655 38956 39201 40454 40458 40712 43233 43325 44000 44915 45748 46491 46542 46568https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/395/1409?format=asciidefaultJ/MNRAS/395/1409/tablea1SNe discovered between 1998-2008.5 in galaxies with recessional velocities less than 2000km/srecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintClassType of supernovae: "Core-collapse", "Type Ia", "Unclassified" or "Uncertain")src.classcharSNSupernova namemeta.id;meta.maincharGalHost galaxy namemeta.id.parentcharVvir[-79/2283] Radial velocity of the host galaxy, corrected for the local group infall into Virgokm/sphys.veloc;pos.lgfloatTypeType of supernovae (or LBV)src.classcharHSTNotes if the host galaxy has been observed by HST prior to explosion and if the position of the SN is "in" or "out" of the camera field-of-viewmeta.codecharComComments (1)meta.notecharSimbadSimbad column added by the CDSmeta.ref.urlchar_RAPositions from Simbad (right ascension part)degpos.eq.ra;meta.main_DEPositions from Simbad (declination part)degpos.eq.dec;meta.main