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J/MNRAS/454/3816   Cobalt emission in nebular phase spectra   (Childress+, 2015)

Measuring nickel masses in Type Ia supernovae using cobalt emission in nebular phase spectra. Childress M.J., Hillier D.J., Seitenzahl I., Sullivan M., Maguire K., Taubenberger S., Scalzo R., Ruiter A., Blagorodnova N., Camacho Y., Castillo J., Elias-Rosa N., Fraser M., Gal-Yam A., Graham M., Howell D.A., Inserra C., Jha S.W., Kumar S., Mazzali P.A., McCully C., Morales-Garoffolo A., Pandya V., Polshaw J., Schmidt B., Smartt S., Smith K.W., Sollerman J., Spyromilio J., Tucker B., Valenti S., Walton N., Wolf C., Yaron O., Young D.R., Yuan F., Zhang B. <Mon. Not. R. Astron. Soc., 454, 3816-3842 (2015)> =2015MNRAS.454.3816C (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Nebulae ; Redshifts ; Photometry, UBV ; Spectroscopy Keywords: supernovae: general Abstract: The light curves of Type Ia supernovae (SNe Ia) are powered by the radioactive decay of 56Ni to 56Co at early times, and the decay of 56Co to 56Fe from ∼60 d after explosion. We examine the evolution of the [CoIII] λ5893 emission complex during the nebular phase for SNe Ia with multiple nebular spectra and show that the line flux follows the square of the mass of 56Co as a function of time. This result indicates both efficient local energy deposition from positrons produced in 56Co decay and long-term stability of the ionization state of the nebula. We compile SN Ia nebular spectra from the literature and present 21 new late-phase spectra of 7 SNe Ia, including SN 2014J. From these we measure the flux in the [CoIII] λ5893 line and remove its well-behaved time dependence to infer the initial mass of 56Ni (MNi) produced in the explosion. We then examine 56Ni yields for different SN Ia ejected masses (Mej - calculated using the relation between light-curve width and ejected mass) and find that the 56Ni masses of SNe Ia fall into two regimes: for narrow light curves (low stretch s∼0.7-0.9), MNi is clustered near MNi∼0.4M and shows a shallow increase as Mej increases from ∼1 to 1.4M; at high stretch, Mej clusters at the Chandrasekhar mass (1.4M) while MNi spans a broad range from 0.6 to 1.2M. This could constitute evidence for two distinct SN Ia explosion mechanisms. Description: The analysis in this work relies on a compilation of SN Ia nebular spectra from the literature as well as new observations. We obtained new late-phase (+50=<t=<+150 d) and nebular (t≥+150 d) spectra of several nearby SNe Ia from numerous telescopes. Several late-phase spectra of very nearby SNe Ia were collected with the Wide Field Spectrograph (WiFeS; Dopita et al. 2007Ap&SS.310..255D, 2010Ap&SS.327..245D) on the Australian National University (ANU) 2.3 m telescope at Siding Spring Observatory in northern New South Wales, Australia. New nebular spectra for three nearby SNe Ia were collected with DEIMOS (Faber et al. 2003SPIE.4841.1657F) on the Keck-II telescope on Mauna Kea, Hawaii. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tableb1.dat 160 32 Nebular SN Ia host information tableb2.dat 140 32 Light-curve fit results and sources tableb3.dat 82 77 Late-phase photometry tableb4.dat 55 73 Co line fluxes from spectra
See also: B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-) J/AJ/131/527 : UBVRI light curves of 44 type Ia supernovae (Jha+, 2006) J/MNRAS/376/1301 : UBVRI light-curves of SN 2005cf (Pastorello+, 2007) J/MNRAS/377/1531 : Optical + infrared photometry of SN 2004eo (Pastorello+, 2007) J/AJ/135/1598 : Optical spectroscopy of type Ia supernovae (Matheson+, 2008) J/ApJ/700/331 : Light curves of type Ia supernovae (CfA3) (Hicken+, 2009) J/AJ/139/519 : Carnegie supernova project. SNe Ia (Contreras+, 2010) J/ApJS/190/418 : Light curves for 165 SNe (Ganeshalingam+, 2010) J/PASP/122/1 : BVRI light curves of SN 2007gi (Zhang+, 2010) J/AJ/142/156 : The CSP (DR2): photometry of SNe Ia (Stritzinger+, 2011) J/ApJ/730/119 : HST/WFC3 observations of Cepheids in SN Ia hosts (Riess+, 2011) J/ApJS/200/12 : CfA4: light curves for 94 type Ia SNe (Hicken+, 2012) J/AJ/148/1 : Optical and ultraviolet photometry of SN 2012fr (Zhang+, 2014) J/A+A/585/A19 : SN 2014J BV light curves (Bonanos+, 2016) J/AJ/151/125 : Optical and UV photometry of SN 2013dy (Zhai+, 2016) Byte-by-byte Description of file: tableb1.dat
Bytes Format Units Label Explanations
1- 2 A2 --- --- [SN] 4- 9 A6 --- SN SN name 11- 22 A12 --- Host Host galaxy name 24- 31 F8.6 --- z Redshift of host galaxy 33- 37 F5.2 mag DM [] Distance modulus of the SN host galaxy 39- 42 F4.2 mag e_DM Uncertainty in DM (1) 44- 54 A11 --- Meth Method used to derive the distance (2) 56-112 A57 --- r_z Reference for z 115-160 A46 --- r_DM Reference for DM
Note (1): For hosts with redshift-based µ, uncertainty includes a peculiar velocity term of 300 km/s. Note (2): Distances for SNe Ia in our sample are preferentially derived from Cepheid distances from Riess et al. (2011, J/ApJ/730/119) where available, and from host redshift with the Riess et al. (2011, J/ApJ/730/119) Hubble constant value (H0=73.8 km/s/Mpc). Generally, we avoid other distance indicators such as Tully-Fisher, surface brightness fluctuations, and planetary nebula luminosity functions. The one exception to this is SN 2012cg, for which we use the Cortes, Kenney & Hardy (2008ApJ...683...78C) Tully-Fisher distance modulus, as was done in Silverman et al. (2012ApJ...756L...7S).
Byte-by-byte Description of file: tableb2.dat
Bytes Format Units Label Explanations
1- 2 A2 --- --- [SN] 4- 9 A6 --- SN SN name 11- 18 F8.2 d MJD Modified Julian Date for B-band maximum magnitude 20- 25 F6.3 mag Brest Rest frame B-band maximum magnitude 27- 31 F5.3 mag e_Brest Uncertainty in Brest 33- 37 F5.3 --- s SN light-curve stretch 39- 43 F5.3 --- e_s Uncertainty in s 45- 50 F6.3 --- c Colour correction 52- 56 F5.3 --- e_c Uncertainty in c 58-140 A83 --- Ref Light-curve reference(s) (G1)
Byte-by-byte Description of file: tableb3.dat
Bytes Format Units Label Explanations
1- 2 A2 --- --- [SN] 4- 9 A6 --- SN SN name (1) 11- 13 I3 d Phase [144/430] Phase 15- 24 A10 "date" Date Observation date 26- 31 F6.3 mag Bmag B-band magnitude 33- 37 F5.3 mag e_Bmag Uncertainty in Bmag 39- 82 A44 --- Ref Photometry reference (G1)
Note (1): For SNe with poor late-time photometric coverage, the late light curve of a surrogate SN is employed.
Byte-by-byte Description of file: tableb4.dat
Bytes Format Units Label Explanations
1- 2 A2 --- --- [SN] 4- 9 A6 --- SN SN name 11- 20 A10 "date" Date Observation date 22- 27 F6.3 [mW/m2] logCoF Measured [Co III] λ5893 line flux (in erg/cm2/s) 29- 33 F5.3 [mW/m2] e_logCoF Uncertainty in logCoF 35- 41 F7.3 --- Resc Spectrum rescale (1) 43- 48 F6.1 0.1nm WaveMin ? Minimum wavelength integration bound for the [Co III] λ5893 flux measurement (Å) 50- 55 F6.1 0.1nm WaveMax ? Maximum wavelength integration bound for the [Co III] λ5893 flux measurement (Å)
Note (1): Factor applied to spectrum to enforce consistency with observed B-band magnitude.
Global note: Note (G1): Reference as follows: CfA = Riess et al. (1999AJ....117..707R), Jha et al. (2006, J/AJ/131/527), Hicken et al. (2009, J/ApJ/700/331; 2012, J/ApJS/200/12); LOSS = Ganeshalingam et al. (2010, J/ApJS/190/418); CSP = Contreras et al. (2010, J/AJ/139/519), Stritzinger et al. (2011, J/AJ/142/156); LCOGT = Brown et al. (2013PASP..125.1031B); T15b = Taubenberger et al. (in preparation).
History: From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 19-Jan-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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