J/MNRAS/454/3771ivo://CDS.VizieR/J/MNRAS/454/3771doi:10.26093/cds/vizier.74543771CDSPacucci F.Ferrara A.Volonteri M.Dubus G.2024-08-15T20:16:13Z2016-09-20T13:29:18ZCDS support team

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

cds-question@unistra.frastronomical-modelsspectroscopyMassive black hole (MBH) seeds at redshift z>~10 are now thought to be key ingredients to explain the presence of the supermassive (10^9-10^M_{sun}_) black holes in place <1Gyr after the big bang. Once formed, massive seeds grow and emit copious amounts of radiation by accreting the left-over halo gas; their spectrum can then provide crucial information on their evolution. By combining radiation-hydrodynamic and spectral synthesis codes, we simulate the time-evolving spectrum emerging from the host halo of a MBH seed with initial mass 10^5^M_{sun}_, assuming both standard Eddington-limited accretion, or slim accretion discs, appropriate for super-Eddington flows. The emission occurs predominantly in the observed infrared-submm (1-1000{mu}m) and X-ray (0.1-100keV) bands. Such signal should be easily detectable by JWST around ~1{mu}m up to z~25, and by ATHENA (between 0.1 and 10keV, up to z~15). Ultra-deep X-ray surveys like the Chandra Deep Field South could have already detected these systems up to z~15. Based on this, we provide an upper limit for the z>~6 MBH mass density of {rho}{blackdot}<~2.5x10^2^M_{sun}_/Mpc^3^ assuming standard Eddington-limited accretion. If accretion occurs in the slim disc mode the limits are much weaker, {rho}{blackdot}<~7.6x10^3^M_{sun}_/Mpc^3^ in the most constraining case.2015MNRAS.454.3771Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/454/3771CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/454/3771https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/454/3771http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/454/3771https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/454/3771https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/454/3771http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/454/3771GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/MNRAS/454/3771/hdpStandard accretion high-density profile (HDP) spectrumrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintEEnergy (z=9)keVphys.energydoublenufnu0Source {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu1Time 1 {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu2Time 2 {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu3Time 3 {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu4Time 4 {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu5Time 5 {nu}f{nu} flux densitymW.m**-2phot.fluxdoubleJ/MNRAS/454/3771/hdp_sdSlim disc accretion high-density profile (HDP) spectrumrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintEEnergy (z=9)keVphys.energydoublenufnu0Source {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu1Time 1 {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu2Time 2 {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu3Time 3 {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu4Time 4 {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu5Time 5 {nu}f{nu} flux densitymW.m**-2phot.fluxdoubleJ/MNRAS/454/3771/ldpStandard accretion low-density profile (LDP) spectrumrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintEEnergy (z=9)keVphys.energydoublenufnu0Source {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu1Time 1 {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu2Time 2 {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu3Time 3 {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu4Time 4 {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu5Time 5 {nu}f{nu} flux densitymW.m**-2phot.fluxdoubleJ/MNRAS/454/3771/ldp_sdSlim disc accretion low-density profile (LDP) spectrumEEnergy (z=9)keVphys.energydoublenufnu0Source {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu1Time 1 {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu2Time 2 {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu3Time 3 {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu4Time 4 {nu}f{nu} flux densitymW.m**-2phot.fluxdoublenufnu5Time 5 {nu}f{nu} flux densitymW.m**-2phot.fluxdoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordint