J/MNRAS/493/1044 Nebular spectra of 111 Type Ia supernovae (Tucker+, 2020)
Nebular spectra of 111 Type Ia supernovae disfavour single-degenerate
progenitors.
Tucker M.A., Shappee B.J., Vallely P.J., Stanek K.Z., Prieto J.L.,
Botyanszki J., Kochanek C.S., Anderson J.P., Brown J., Galbany L.,
Holoien T.W.-S., Hsiao E.Y., Kumar S., Kuncarayakti H., Morrell N.,
Phillips M.M., Stritzinger M.D., Thompson T.A.
<Mon. Not. R. Astron. Soc., 493, 1044-1062 (2020)>
=2020MNRAS.493.1044T 2020MNRAS.493.1044T (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Spectral types ; Redshifts ; Spectra, optical ;
Photometry, UBVRI ; Photometry, ugriz
Keywords: supernovae - general; galaxies - distances and redshifts
Abstract:
We place statistical constraints on Type Ia supernova (SN Ia)
progenitors using 227 nebular-phase spectra of 111 SNe Ia. We find no
evidence of stripped companion emission in any of the nebular-phase
spectra. Upper limits are placed on the amount of mass that could go
undetected in each spectrum using recent hydrodynamic simulations.
With these null detections, we place an observational 3σ upper
limit on the fraction of SNe Ia that are produced through the
classical H-rich non-degenerate companion scenario of <5.5 per cent.
Additionally, we set a tentative 3σ upper limit on He star
progenitor scenarios of <6.4 per cent, although further theoretical
modelling is required. These limits refer to our most representative
sample including normal, 91bg-like, 91T-like, and
'super-Chandrasekhar' SNe Ia but excluding SNe Iax and SNe Ia-CSM. As
part of our analysis, we also derive a Nebular Phase Phillips
Relation, which approximates the brightness of an SN Ia from 150 to
500d after maximum using the peak magnitude and decline rate parameter
Δm15(B).
Description:
Our sample of 227 spectra of 111 SNe Ia comes from the 40 instruments
on the 29 telescopes listed in Table 1. All spectroscopically peculiar
SNe Ia are included except for those exhibiting signatures of
circumstellar material (SNe Ia-CSM). For non-CSM SNe Ia, we impose the
following criteria when selecting nebular spectra: Obtained between
200 and 500d after explosion to maintain consistency with the models
of Botyanszki et al. (2018ApJ...852L...6B 2018ApJ...852L...6B), assuming a typical rise
time of trise∼19d (Firth et al. 2015MNRAS.446.3895F 2015MNRAS.446.3895F, Cat.
J/MNRAS/446/3895); Cover ±1000km/s of at least one H or He line in
Table 2; Have at least one method of absolute flux calibration,
outlined in Section 2.3; Published, posted, or observed by our team
before the submission date of this article (2019 March 15).
The complete list of new and archival spectra is provided in Table B4.
Additionally, we include new and archival photometry to supplement our
spectral data and analysis. Early-phase photometry (~<50d after
maximum light) is used in deriving the photometric properties of each
SN Ia using the photometric fitting code SNOOPY (Burns et al.
2011AJ....141...19B 2011AJ....141...19B), including time of maximum (tmax), the decline
rate parameter Δm15, extinction along line of sight, and the
distance modulus. Late-phase photometry and nebular-phase photometry
are used for flux calibrating the nebular spectra and deriving a
Nebular Phase Phillips Relation (NPPR).
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tableb2.dat 176 111 All SNe Ia studied in this work
tableb3.dat 75 111 SN Ia light-curve parameters, the number of
late-time spectra, and the corresponding phases,
ordered by tmax
tableb4.dat 118 227 Spectra observations
tableb5.dat 75 111 Flux limits for each line in Table 2 and the
corresponding H/He mass limit
tableb6.dat 33 124 New photometry presented in this study
tableb7.dat 428 136 Photometry data for each SN Ia studied in this
work
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Byte-by-byte Description of file: tableb2.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- OName Discovery name
13- 23 A11 --- Name IAU name of the supernova
25- 33 A9 --- Type Supernova subtype (1)
35- 41 F7.5 --- z Redshift
43- 87 A45 --- r_z Reference for z
89-130 A42 --- refdisc Discovery reference
132-176 A45 --- r_Type Classification reference
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Note (1): Sub-type as follows:
N = Normal supernova (90/111)
91bg-like = 91bg-like supernova (8/111)
91T-like = 91T-like supernova (5/111)
Iax = Iax supernova (4/111)
SC = Super Chandrasekhar supernova (4/111)
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Byte-by-byte Description of file: tableb3.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Supernova name
13- 19 F7.1 d tmax Time of maximum light
21- 23 F3.1 d e_tmax Error on tmax
25- 28 F4.2 mag Dm15 ? Decline rate parameter Δm15
30- 33 F4.2 mag e_Dm15 ? Error on Dm15
35 A1 --- f_Dm15 [a] Flag on Dm15 (1)
37- 41 F5.2 mag mu ? Distance modulus
43- 46 F4.2 mag e_mu ? Error on mu
48 A1 --- f_mu [a] Flag on mu (1)
50- 51 I2 --- r_mu ? Reference for mu (2)
53- 57 F5.2 --- E(B-V) ? Colour excess
59- 62 F4.2 --- e_E(B-V) ? Error on E(B-V)
64 A1 --- f_E(B-V) [a] Flag on E(B-V) (1)
66- 67 I2 --- Nspec Number of nebular-phase spectra
69- 75 A7 d Phase Phase
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Note (1): Flag as follows:
a = To be presented in P. Chen et al. (in preparation)
Note (2): References as follows:
1 = Tully et al. (2013AJ....146...86T 2013AJ....146...86T, Cat. J/AJ/146/86)
2 = Riess et al. (2016ApJ...826...56R 2016ApJ...826...56R, Cat. J/ApJ/826/56)
3 = Villegas et al. (2010ApJ...717..603V 2010ApJ...717..603V)
4 = Freedman et al. (2001ApJ...553...47F 2001ApJ...553...47F)
5 = Saha et al. (2006ApJS..165..108S 2006ApJS..165..108S)
6 = Larsen et al. (2001AJ....121.2974L 2001AJ....121.2974L)
7 = Derived from redshift
8 = Theureau et al. (2007A&A...465...71T 2007A&A...465...71T, Cat. J/A+A/465/71)
9 = Blakeslee et al. (2010ApJ...724..657B 2010ApJ...724..657B)
10 = Huang et al. (2017ApJ...836..157H 2017ApJ...836..157H)
11 = Tonry et al. (2001ApJ...546..681T 2001ApJ...546..681T)
12 = Holmbo et al. (2019A&A...627A.174H 2019A&A...627A.174H, Cat. J/A+A/627/A174)
13 = Saulder et al. (2016A&A...596A..14S 2016A&A...596A..14S, Cat. J/A+A/596/A14)
14 = Springob et al. (2014MNRAS.445.2677S 2014MNRAS.445.2677S, Cat. J/MNRAS/445/2677)
15 = Li et al. (2019ApJ...870...12L 2019ApJ...870...12L)
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Byte-by-byte Description of file: tableb4.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Supernova name
13- 20 F8.2 d Date Observation Date (MJD)
22- 26 F5.1 d Phase Phase relative to tmax
28- 34 A7 --- Tel Telescope used for the observations (1)
36- 42 A7 --- Inst Instrument used for the observations (1)
44- 54 A11 0.1nm Range Wavelenght range of the instrument
56- 60 I5 s ExpTime ? Exposure time
62- 66 I5 km/s vexp Expansion velocity (2)
68- 71 I4 km/s e_vexp ? Error on vexp
73- 76 A4 --- Qual Quality of the spectrum (Low, Med or High) (3)
78-118 A41 --- Ref Reference
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Note (1): See Section 2 of the article for definitions and references
Note (2): If the SNR of the spectrum is too low for the widths of at least two
lines to be measured confidently, we assume a typical width of
3000km/s
Note (3): Quality as follows:
High = The spectrum clearly shows the major Fe and Co emission lines between
∼4000 and 7000Å. The spectrum exhibits little to no host
contamination or instrumental artefacts.
Med = The major Fe lines are visible, while the Co lines are noisy or absent.
The spectrum may also suffer from minor to moderate host galaxy
contamination and/or instrumental artefacts.
Low = The major Fe lines are barely detectable above the spectral noise, and
the Co lines mostly below the detection threshold. This category also
includes overall medium-quality spectra with significant host galaxy
contamination and/or instrumental artefacts.
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Byte-by-byte Description of file: tableb5.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Supernova name
13- 17 F5.1 d PhaseH Phase relative to tmax
19- 25 A7 --- LineH Hydrogen line (1)
27- 34 E8.3 mW/m2 FlimH Flux limit for LineH
36 A1 --- l_MlimH Limit flag on MlimH
38- 44 E7.3 Msun MlimH Derived mass-limit for the H-rich model
46- 50 F5.1 d PhaseHe ? Phase relative to tmax
52- 56 A5 --- LineHe Helium line (1)
58- 65 E8.3 mW/m2 FlimHe ? Flux limit for LineHe
67 A1 --- l_MlimHe Limit flag on MlimHe
69- 75 E7.3 Msun MlimHe ? Derived mass-limit for the He-rich model
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Note (1): Corresponds to the lines listed in Table 2 of the article
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Byte-by-byte Description of file: tableb6.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Supernova name
13- 20 F8.2 d MJD Modified Julian date
22 A1 --- Filter Filter used (B,V,R,I,g,r or i)
24- 28 F5.2 mag ABmag AB magnitude corresponding to the Filter
30- 33 F4.2 mag e_ABmag Error on ABmag
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Byte-by-byte Description of file: tableb7.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Supernova name
13 A1 --- f_Name [*] Flag on Name (1)
15- 18 I4 --- Ntot Total number of photometric points
20- 26 A7 d Phase Phase relative to maximum light
28- 63 A36 --- Filters Filters used
65-428 A364 --- Ref References
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Note (1): Flag as follows:
* = Object used in deriving the Nebular Phase Phillip's relation (NPPR)
(see Appendix A of the article)
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 04-Apr-2023