J/A+A/629/A134ivo://CDS.VizieR/J/A+A/629/A134doi:10.26093/cds/vizier.36290134CDSGoetberg Y.de Mink S.E.Groh J.H.Leitherer C.Norman C.2023-05-26T15:06:49Z2019-09-17T11:08:26ZCDS support team

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

cds-question@unistra.frastronomical-modelsgalaxiesvisible-astronomystellar-populationsspectroscopyStars stripped of their envelopes from interaction with a binary companion emit a significant fraction of their radiation as ionizing photons. They are potentially important stellar sources of ionizing radiation, however, they are still often neglected in spectral synthesis simulations or simulations of stellar feedback. In anticipating the large datasets of galaxy spectra from the upcoming James Webb Space Telescope, we modeled the radiative contribution from stripped stars by using detailed evolutionary and spectral models. We estimated their impact on the integrated spectra and specifically on the emission rates of HI-, HeI-, and HeII-ionizing photons from stellar populations. We find that stripped stars have the largest impact on the ionizing spectrum of a population in which star formation halted several Myr ago. In such stellar populations, stripped stars dominate the emission of ionizing photons, mimicking a younger stellar population in which massive stars are still present. Our models also suggest that stripped stars have harder ionizing spectra than massive stars. The additional ionizing radiation, with which stripped stars contribute affects observable properties that are related to the emission of ionizing photons from stellar populations. In co-eval stellar populations, the ionizing radiation from stripped stars increases the ionization parameter and the production efficiency of hydrogen ionizing photons. They also cause high values for these parameters for about ten times longer than what is predicted for massive stars. The effect on properties related to non-ionizing wavelengths is less pronounced, such as on the ultraviolet continuum slope or stellar contribution to emission lines. However, the hard ionizing radiation from stripped stars likely introduces a characteristic ionization structure of the nebula, which leads to the emission of highly ionized elements such as O^2+^ and C^3+^. We, therefore, expect that the presence of stripped stars affects the location in the BPT diagram and the diagnostic ratio of OIII to OII nebular emission lines. Our models are publicly available through CDS database and on the STARBURST99 website.2019A&A...629A.134Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/629/A134CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/629/A134https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/629/A134http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/629/A134https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/629/A134https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/629/A134http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/629/A134GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/629/A134/nbrs0002Z=0.0002 number of stripped starsNgtr10Number of stripped stars that have progenitors that were initially more massive than 10M_{sun}_ (nbr_gtr_10)meta.numberfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTimeTimeyrtime.agedoubleNTotTotal number of stripped stars present in the population at the given time (total_nbr)meta.numberfloatNcaseANumber of stripped stars present that were formed via Case A type mass transfer (nbr_caseA)meta.numberfloatNCaseBNumber of stripped stars present that were formed via Case B type mass transfer (nbr_caseB)meta.numberfloatNBCEENumber of stripped stars present that were formed via successful ejection of a common envelope that was initiated during the Hertzsprung gap passage of the donor star (nbr_BCEE)meta.numberfloatNgtr5Number of stripped stars that have progenitors that were initially more massive than 5M_{sun}_ (nbr_gtr_5)meta.numberfloatNgtr3Number of stripped stars that have progenitors that were initially more massive than 3M_{sun}_ (nbr_gtr_3)meta.numberfloatJ/A+A/629/A134/nbrs002Z=0.002 number of stripped starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTimeTimeyrtime.agedoubleNTotTotal number of stripped stars present in the population at the given time (total_nbr)meta.numberfloatNcaseANumber of stripped stars present that were formed via Case A type mass transfer (nbr_caseA)meta.numberfloatNCaseBNumber of stripped stars present that were formed via Case B type mass transfer (nbr_caseB)meta.numberfloatNBCEENumber of stripped stars present that were formed via successful ejection of a common envelope that was initiated during the Hertzsprung gap passage of the donor star (nbr_BCEE)meta.numberfloatNgtr10Number of stripped stars that have progenitors that were initially more massive than 10M_{sun}_ (nbr_gtr_10)meta.numberfloatNgtr5Number of stripped stars that have progenitors that were initially more massive than 5M_{sun}_ (nbr_gtr_5)meta.numberfloatNgtr3Number of stripped stars that have progenitors that were initially more massive than 3M_{sun}_ (nbr_gtr_3)meta.numberfloatJ/A+A/629/A134/nbrs006Z=0.006 number of stripped starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTimeTimeyrtime.agedoubleNTotTotal number of stripped stars present in the population at the given time (total_nbr)meta.numberfloatNcaseANumber of stripped stars present that were formed via Case A type mass transfer (nbr_caseA)meta.numberfloatNCaseBNumber of stripped stars present that were formed via Case B type mass transfer (nbr_caseB)meta.numberfloatNBCEENumber of stripped stars present that were formed via successful ejection of a common envelope that was initiated during the Hertzsprung gap passage of the donor star (nbr_BCEE)meta.numberfloatNgtr10Number of stripped stars that have progenitors that were initially more massive than 10M_{sun}_ (nbr_gtr_10)meta.numberfloatNgtr5Number of stripped stars that have progenitors that were initially more massive than 5M_{sun}_ (nbr_gtr_5)meta.numberfloatNgtr3Number of stripped stars that have progenitors that were initially more massive than 3M_{sun}_ (nbr_gtr_3)meta.numberfloatJ/A+A/629/A134/nbrs014Z=0.014 number of stripped starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTimeTimeyrtime.agedoubleNTotTotal number of stripped stars present in the population at the given time (total_nbr)meta.numberfloatNcaseANumber of stripped stars present that were formed via Case A type mass transfer (nbr_caseA)meta.numberfloatNCaseBNumber of stripped stars present that were formed via Case B type mass transfer (nbr_caseB)meta.numberfloatNBCEENumber of stripped stars present that were formed via successful ejection of a common envelope that was initiated during the Hertzsprung gap passage of the donor star (nbr_BCEE)meta.numberfloatNgtr10Number of stripped stars that have progenitors that were initially more massive than 10M_{sun}_ (nbr_gtr_10)meta.numberfloatNgtr5Number of stripped stars that have progenitors that were initially more massive than 5M_{sun}_ (nbr_gtr_5)meta.numberfloatNgtr3Number of stripped stars that have progenitors that were initially more massive than 3M_{sun}_ (nbr_gtr_3)meta.numberfloatJ/A+A/629/A134/q0002Z=0.0002 emission rates of ionizing photons from stripped starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTimeTimeyrtime.agedoublelog10(Q0)? logarithm of the emission rates of HI-ionizing photons from stripped starslog(s**-1)phys.emissMeasuredoublenullablelog10(Q1)? logarithm of the emission rates of HeI-ionizing photons from stripped starslog(s**-1)phys.emissMeasuredoublenullablelog10(Q2)? logarithm of the emission rates of HeII-ionizing photons from stripped starslog(s**-1)phys.emissMeasuredoublenullableJ/A+A/629/A134/q002Z=0.002 emission rates of ionizing photons from stripped starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTimeTimeyrtime.agedoublelog10(Q0)? logarithm of the emission rates of HI-ionizing photons from stripped starslog(s**-1)phys.emissMeasuredoublenullablelog10(Q1)? logarithm of the emission rates of HeI-ionizing photons from stripped starslog(s**-1)phys.emissMeasuredoublenullablelog10(Q2)? logarithm of the emission rates of HeII-ionizing photons from stripped starslog(s**-1)phys.emissMeasuredoublenullableJ/A+A/629/A134/q006Z=0.006 emission rates of ionizing photons from stripped starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTimeTimeyrtime.agedoublelog10(Q0)? logarithm of the emission rates of HI-ionizing photons from stripped starslog(s**-1)phys.emissMeasuredoublenullablelog10(Q1)? logarithm of the emission rates of HeI-ionizing photons from stripped starslog(s**-1)phys.emissMeasuredoublenullablelog10(Q2)? logarithm of the emission rates of HeII-ionizing photons from stripped starslog(s**-1)phys.emissMeasuredoublenullableJ/A+A/629/A134/q014Z=0.014 emission rates of ionizing photons from stripped starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTimeTimeyrtime.agedoublelog10(Q0)? logarithm of the emission rates of HI-ionizing photons from stripped starslog(s**-1)phys.emissMeasuredoublenullablelog10(Q1)? logarithm of the emission rates of HeI-ionizing photons from stripped starslog(s**-1)phys.emissMeasuredoublenullablelog10(Q2)? logarithm of the emission rates of HeII-ionizing photons from stripped starslog(s**-1)phys.emissMeasuredoublenullable