J/ApJ/922/21ivo://CDS.VizieR/J/ApJ/922/21doi:10.26093/cds/vizier.19220021CDSSand D.J.Sarbadhicary S.K.Pellegrino C.Misra K.Dastidar R.,Brown P.J.Itagaki K.Valenti S.Swift J.J.Andrews J.E.,Bostroem K.A.Burke J.Chomiuk L.Dong Y.Galbany L.Graham M.L.,Hiramatsu D.Howell D.A.Hsiao E.Y.Janzen D.Jencson J.E.,Lundquist M.J.McCully C.Reichart D.Smith N.Wang L.Wyatt S.2023-08-25T12:25:25Z2023-04-24T15:36:25ZCDS support team

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

cds-question@unistra.frsupernovaeinfrared-photometryvisible-astronomybroad-band-photometryspectroscopyWe present deep Chandra X-ray observations of two nearby Type Ia supernovae, SN 2017cbv and SN 2020nlb, which reveal no X-ray emission down to a luminosity L_X_<~5.3x10^37^ and <~5.4x10^37^erg/s (0.3-10keV), respectively, at ~16-18 days after the explosion. With these limits, we constrain the pre-explosion mass-loss rate of the progenitor system to be dM/dt<7.2x10^-9^ and <9.7x10^-9^M_{sun}_/yr for each (at a wind velocity v_w_=100km/s and a radius of R~10^16^cm), assuming any X-ray emission would originate from inverse Compton emission from optical photons upscattered by the supernova shock. If the supernova environment was a constant-density medium, we would find a number density limit of n_CSM_<36 and <65cm^-3^, respectively. These X-ray limits rule out all plausible symbiotic progenitor systems, as well as large swathes of parameter space associated with the single degenerate scenario, such as mass loss at the outer Lagrange point and accretion winds. We also present late-time optical spectroscopy of SN2020nlb, and set strong limits on any swept up hydrogen (L_H{alpha}_<2.7x10^37^erg/s) and helium (L_He,{lambda}6678_<2.7x10^37^erg/s) from a nondegenerate companion, corresponding to M_H_<~0.7-2x10^-3^M_{sun}_ and M_He_<~4x10^-3^M_{sun}_. Radio observations of SN 2020nlb at 14.6 days after explosion also yield a non-detection, ruling out most plausible symbiotic progenitor systems. While we have doubled the sample of normal Type Ia supernovae with deep X-ray limits, more observations are needed to sample the full range of luminosities and subtypes of these explosions, and set statistical constraints on their circumbinary environments.2021ApJ...922...21Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/922/21CatalogResearchIsServedByTAP VizieR generic servicerelated-toB/chandra : The Chandra Archive Log (CXC, 1999-2014)VIII/76 : Leiden/Argentine/Bonn (LAB) Survey of Galactic HI (Kalberla+ 2005)J/MNRAS/313/469 : Streaming motions of galaxy clusters. I. (Smith+, 2000)J/ApJ/655/144 : ACS Virgo Cluster Survey. XIII. (Mei+, 2007)J/MNRAS/377/1531 : Optical & IR photometry of SN 2004eo (Pastorello+, 2007)J/ApJ/699/L139 : Spectral parameters of SNe Ia (Wang+, 2009)J/AJ/143/126 : Spectroscopy of nearby Type Ia supernovae (Blondin+, 2012)J/ApJ/749/18 : Swift/UVOT observations of 12 nearby SN-Ia (Brown+, 2012)J/ApJ/748/L29 : SN Ia supernovae observed by Swift/XRT (Russell+, 2012)J/ApJ/773/53 : Type Ia SNe spectroscopy by the CSP (Folatelli+, 2013)J/A+A/554/A27 : 2011fe spectrophotometric time series (Pereira+, 2013)J/MNRAS/438/L101 : First month on SN 2013ej (Valenti+, 2014)J/MNRAS/459/3939 : Type II supernova light curves (Valenti+, 2016)J/ApJ/853/62 : Opt. and NIR spectra and LCs of SN2016ija (Tartaglia+, 2018)J/ApJ/870/L1 : K2 obs. of type Ia supernova SN 2018oh (Dimitriadis+, 2019)J/A+A/627/A174 : Early light curve of SN 2013gy (Holmbo+, 2019)J/ApJ/870/13 : K2 LC alternative analysis of ASASSN-18bt (Shappee+, 2019)J/ApJ/895/118 : Opt. & NIR photometry of 2 Ia type supernovae (Burns+, 2020)J/ApJ/898/56 : UVOT, ZTF gri LCs & spectra of SN Ia 2019yvq (Miller+, 2020)J/ApJ/897/159 : Type Ia SN 2019ein UBVgri photometry (Pellegrino+, 2020)J/ApJ/904/14 : Optical and NIR observation of SN (Ia) 2017cbv (Wang+, 2020)J/ApJ/914/50 : Opt. phot. & GMOS & NIRES sp. of SN2019yvq (Tucker+, 2021)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/922/21https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/922/21http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/922/21https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/922/21https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/922/21http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/922/21GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticalInfrareddefaultJ/ApJ/922/21/fig1aSwift UVOT photometry of SN 2020nlbrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFiltFilter (UBV, UVM2, UVW1, UVW2)meta.id;instr.filtercharMJD[59025.7/59068.3] Modified Julian Datedtime.epochdoublemag[11.77/19.02] Apparent Vega magnitude in Filtmagphot.magfloate_mag[0.029/0.4] Uncertainty in magmagstat.error;phot.magfloatJ/ApJ/922/21/fig1bThacher Observatory optical photometry of SN 2020nlbrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFilt[griz] Filtermeta.id;instr.filtercharBJDBarycentric Julian Datedtime.epochdoublemag[12/16.6] Apparent AB magnitude in Filtmagphot.magfloate_mag[0/0.2] Uncertainty in magmagstat.error;phot.magfloatJ/ApJ/922/21/fig1cLas Cumbres Observatory optical photometry of SN 2020nlbrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFilt[UBVgri] Filtermeta.id;instr.filtercharJDJulian Datedtime.epochdoublemag[11.93/16.7] Apparent magnitude in Filt (1)magphot.magfloate_mag[0.008/0.6] Uncertainty in magmagstat.error;phot.magfloatJ/ApJ/922/21/fig1dThe FLOYDS +0.5 day spectrum of SN 2020nlbrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda[3500.6/10000.5] Wavelength; Angstroms0.1nmem.wldoubleFlux[4.7e-15/1.5e-13] Flux density; erg/s/cm^2^/{AA}cW.m**-2.nm**-1phot.fluxdoubleJ/ApJ/922/21/fig4Nebular-phase MMT/BCS spectrum of SN 2020nlbrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambda[3735.7/9013.7] Wavelength; Angstroms0.1nmem.wldoubleFlux[1.6e-19/5.1e-16]? Flux density; in erg/s/cm^2^/{AA} unitscW.m**-2.nm**-1meta.unit;phot.fluxdoublenullable