J/ApJ/956/108 TESS 4yrs obs. of Type Ia supernovae (Fausnaugh+, 2023)
Four years of type Ia supernovae observed by TESS: early-time light-curve shapes
and constraints on companion interaction models.
Fausnaugh M.M., Vallely P.J., Tucker M.A., Kochanek C.S., Shappee B.J.,
Stanek K.Z., Ricker G.R., Vanderspek R., Agarwal M., Daylan T.,
Jayaraman R., Hounsell R., Muthukrishna D.
<Astrophys. J., 956, 108 (2023)>
=2023ApJ...956..108F 2023ApJ...956..108F
ADC_Keywords: Supernovae; Photometry; Optical; Magnitudes, absolute; Redshifts
Keywords: Type Ia supernovae
Abstract:
We present 307 type Ia supernova (SN) light curves from the first 4yr
of the Transiting Exoplanet Survey Satellite mission. We use this
sample to characterize the shapes of the early-time light curves,
measure the rise times from first light to peak, and search for
companion star interactions. Using simulations, we show that light
curves must have noise <10% of the peak flux to avoid biases in the
early-time light-curve shape, restricting our quantitative analysis to
74 light curves. We find that the mean power-law index tβ1 of
the early-time light curves is β1=1.93±0.57, and the mean
rise time to peak is 15.7±3.5 days. The underlying population
distribution for β1 may instead consist of a Gaussian component
with mean 2.29, width 0.34, and a long tail extending to values less
than 1.0. We find that the data can rarely distinguish between models
with and without companion interaction models. Nevertheless, we find
three high-quality light curves that tentatively prefer the addition
of a companion interaction model, but the statistical evidence for the
companion interactions is not robust. We also find two SNe that
disfavor the addition of a companion interaction model to a curved
power-law model. Taking the 74 SNe together, we calculate 3σ
upper limits on the presence of companion signatures to control for
orientation effects that can hide companions in individual light
curves. Our results rule out common progenitor systems with companions
having Roche lobe radii >31R☉ (separations >5.7x1012cm, 99.9%
confidence level) and disfavor companions having Roche lobe radii
>10R☉ (separations >1.9x1012cm, 95% confidence level). Lastly,
we discuss the implications of our results for the intrinsic fraction
of single degenerate progenitor systems.
Description:
The TESS primary mission sky survey operated from 2018 July to 2020 July,
and the first extended mission operated from 2020 July to 2022 Sept.
TESS sweeps out one ecliptic hemisphere each year, using 13 pointings
that divide the hemisphere into 24x96 square degree "sectors". TESS
stares at each sector continuously for about 27 days, with ∼1day
interruptions halfway through to download the accumulated data. The
main exceptions to this pattern are for TESS sectors 42-46, which
observed the ecliptic plane. The TESS full-frame images (FFIs) were
collected at a 30 minutes cadence in the primary mission (sectors
1-26) and at a 10 minutes cadence in the extended mission (sectors
27-50). The TESS passband ranges from 600-1000nm.
We extracted light curves for type Ia SNe in the TESS fields of view
discovered by ground-based surveys while TESS was observing. We also
included SNe discovered up to 30 days after the TESS observations,
because TESS may still capture the early-time rise of the light curve.
In total, there are 850 such type Ia SNe, drawn from reports to the
Transient Name Server (TNS). All of these SNe have spectroscopic
classifications, which provide estimates of the redshifts, distances,
and luminosities.
If the SN has a host galaxy reported to TNS, we use the host galaxy
redshift. Otherwise, we use the reported SN redshift, and we assume an
uncertainty of 1000km/s that we propagate to the distance and
luminosity estimates.
See Section 2.1.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 104 307 Properties of the supernova sample
table2.dat 81 680384 SN light curves
table3.dat 91 307 Curved Power Law posterior medians
table4.dat 120 307 Curved Power Law with companion interaction
posterior medians
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See also:
J/MNRAS/446/3895 : The rising light curves of Type Ia supernovae (Firth+, 2015)
J/ApJ/799/105 : KELT light curve of the M82 SN 2014J (Siverd+, 2015)
J/ApJ/870/L1 : K2 obs. of type Ia supernova SN 2018oh (Dimitriadis+, 2019)
J/ApJ/883/111 : UV-Opt LCs of ASASSN-19bt detected by TESS (Holoien+, 2019)
J/MNRAS/483/5045 : R-band LC properties of SN Ia (Papadogiannakis+, 2019)
J/ApJ/870/13 : K2 LC alternative analysis of ASASSN-18bt (Shappee+, 2019)
J/ApJ/899/136 : TESS light curve of AGN NGC 4395 (Burke+, 2020)
J/A+A/634/A37 : TURTLS Light curves of 56Ni distributions (Magee+, 2020)
J/ApJ/898/56 : UVOT, ZTF gri LCs and sp. of SN Ia 2019yvq (Miller+, 2020)
J/ApJ/902/47 : ZTF early obs. of type Ia SNe. II. Rise time (Miller+, 2020)
J/MNRAS/493/1044 : Nebular spectra of 111 Type Ia supernovae (Tucker+, 2020)
J/ApJ/908/51 : TESS early light curves of type Ia SNe (Fausnaugh+, 2021)
J/ApJ/923/L8 : Follow-up phot. & sp. of SNIa 2020hvf (Jiang+, 2021)
J/ApJ/910/125 : Follow-up photometry of ASASSN-14ko (Payne+, 2021)
J/ApJ/914/50 : Opt. phot. and GMOS & NIRES sp. of SN2019yvq (Tucker+, 2021)
J/ApJ/923/167 : SN 2018agk spectra and NIR-UV light curves (Wang+, 2021)
J/ApJ/930/12 : Phot. & sp. follow-up of ASASSN-20hx (Hinkle+, 2022)
J/ApJ/933/L45 : LCs and spectra of type Ia SN 2021aefx (Hosseinzadeh+, 2022)
J/ApJ/926/142 : UV, opt. and X-ray evolution of ASASSN-14ko (Payne+, 2022)
http://www.wis-tns.org/ : Transient Name Server homepage
http://heasarc.gsfc.nasa.gov/docs/tess/ : NASA TESS Science Support Center
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name SN identifier
12- 24 A13 --- OName Other identifier
26- 30 F5.2 mag TmagP [14/21.3] Peak TESS band magnitude
(Tpeak)
32- 35 F4.2 mag e_TmagP [0.05/0.5] Uncertainty in TmagP (1)
37- 41 F5.2 mag TmagL [17.9/22.4] Limiting TESS band magnitude
(Tlim)
43- 47 F5.2 mag delTmag [-0.94/5.4] Magnitude increase in TESS band
(ΔT)
49- 55 F7.2 d tPeak [1352.4/2691.6] BJD of peak TESS band
magnitude; tPeak-2457000.0
57- 62 F6.2 mag TMag [-21.51/-15.21] Absolute TESS band magnitude
(2)
64- 67 F4.2 mag e_TMag [0.05/0.9] Uncertainty in TMag
69- 73 F5.2 10+35W nuLum [0.13/48.2] Luminosity; 1e+42erg/s
75- 78 F4.2 10+35W e_nuLum [0.01/9.6] Uncertainty in nuLum
80- 85 F6.4 --- z [0.006/0.2] Spectroscopic redshift of host
galaxy
87- 91 F5.3 mag E(B-V) [0.004/0.4] THe (B-V) color excess
93- 95 I03 --- Reduc [0/110] Data reduction bitmask (3)
97- 99 I03 --- Treduc [0/110] TESSreduce bitmask (4)
101- 104 I04 --- Qual [0/1110] Quality bitmask (5)
--------------------------------------------------------------------------------
Note (1): Uncertainty includes the TESS instrument flux calibration (0.05mag,
Appendix A), uncertainty in the fit to the baseline flux
(Section 3.1), and any uncertainty in the calibration offset of
the second sector, if applicable (Section 3.1).
Note (2): Absolute TESS magnitude. Includes uncertainty in Tpeak (column 2)
and an assumed uncertainty of 1000km/s in the redshift if the
host galaxy is not reported to TNS.
Note (3): Marks SN where we applied the "background model" correction (first
bit, "100"), where we detrended variable star signals (second bit,
"010"), or where the light curve is affected by asteroids (third
bit, "001"). See Section A.1 for details.
Note (4): Marks SN where we extracted a TESSreduce light curve (first bit,
"100"), where we elected to use the TESSreduce light curve rather
than the ISIS light curve (second bit, "010"), or where the two
light curves show different shapes/amplitudes (third bit, "001").
See Section A.2 for details.
Note (5): Marks SN where TESS did not observe the peak flux (first bit,
"1000", see Appendix C), the SN is part of the "No First Light"
subsample (second bit, "0100", see Appendix C), the SN is part of
the "High Quality" subsample (third bit, "0010", see Appendix C.1),
or the SN is part of the "High Dynamic Range" subsample (fourth bit,
"0001", see Appendix C.2).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name SN identifier
12- 21 F10.5 d BJD [1325.3/2691.6] Barycentric JD - TDB;
BJD-2457000
23- 30 F8.4 ct/s CRate [-84.2/974.8] Count rate
32- 38 F7.4 ct/s e_CRate [0.16/14.5] Uncertainty in CRate
40- 47 F8.4 --- Frac [-16.2/16] Fraction of Peak
49- 54 F6.4 --- e_Frac [0.007/4] Uncertainty in Frac
56- 62 F7.4 mag Tmag [14/22.4]? Apparent TESS band magnitude (1)
64- 70 F7.4 mag e_Tmag [0.008/28.5]? Uncertainty in Tmag (1)
72- 81 F10.6 --- CalOff [-0.7/363]? Calibration offset (2)
--------------------------------------------------------------------------------
Note (1): For fluxes below the 8 hour detection limits (including zero and
negative flux due to noise), the magnitudes are represented by TmagL
from Table 1 and the uncertainties are blank.
Note (2): Gives the shift applied to flux calibrate the second sector
of TESS observations for supernova observed near the ecliptic
poles (see Appendix B).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name SN identifier
12- 18 F7.2 d BJD [1330.74/2688.48] Time of first light;
BJD-2470000.0
20- 23 F4.2 d e_BJD [0.01/3.6] Uncertainty in BJD
25- 29 F5.2 d tRise [3.49/28.81]? Rise time (1)
31- 34 F4.2 --- PLbeta1 [0.02/3.75] Mean power law index, tβ1
36- 39 F4.2 --- e_PLbeta1 [0.01/0.92] Uncertainty in PLbeta1
41- 47 F7.4 --- PLbeta2 [-0.095/-0.0001] Mean power law index,
tβ2
49- 54 F6.4 --- e_PLbeta2 [0.0001/0.03] Uncertainty in PLbeta2
56- 63 F8.2 [-] lnZ [-7151.2/11349.7] Natural log of Bayesian
Evidence Z from dynesty
65- 68 F4.2 [-] e_lnZ [0.04/0.2] Uncertainty in lnZ
70- 78 F9.2 --- BIC [-22731.4/14303.7] Bayesian Information
Criterion (2)
80- 85 F6.4 --- Ratio [0.06/0.98] Noise metric,
rmsGauss/rmsobserved (3)
87- 91 I05 --- Mask [0/1110] BitMask (4)
--------------------------------------------------------------------------------
Note (1): The uncertainty on the rise time is determined by the uncertainty
on the time of first light (column 3).
Note (2): BIC=klnN-lnL
where k is the number of parameters, N is the number of data points in
the fit, and L is the likelihood. See Appendix B.
Note (3): Defined in Section 4, which quantifies departures of the light curves
from random Gaussian noise. Values near zero indicate very little
improvement from binning (systematic errors dominate over random
noise), while 1 indicates perfect Gaussian noise scaling (random
noise only).
Note (4): The same Quality Bitmask from Table 1, which marks the subsamples of
SNe: TESS did not observe the peak flux of this SN (first bit,
"1000", see Appendix C), the SN is part of the "No First Light"
subsample (second bit, "0100", see Appendix C), the SN is part of
the "High Quality" subsample (third bit, "0010", see Appendix C.1),
or the SN is part of the "High Dynamic Range" subsample (fourth bit,
"0001", see Appendix C.2).
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Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name SN identifier
12- 18 F7.2 d BJD [1331.15/2689.25] Time of first light;
BJD-2470000.0
20- 23 F4.2 d e_BJD [0.01/3.3] Uncertainty in BJD
25- 29 F5.2 d tRise [2.8/28.01]? Rise time (1)
31- 34 F4.2 --- PLbeta1 [0.01/3.9] Mean power law index,
tβ1_^
36- 39 F4.2 --- e_PLbeta1 [0.01/0.95] Uncertainty in PLbeta1
41- 47 F7.4 --- PLbeta2 [-0.094/-0.0001] Mean power law index,
tβ2_^
49- 54 F6.4 --- e_PLbeta2 [0.0001/0.03] Uncertainty in PLbeta2
56- 61 F6.2 Rsun MedRad [1/223.2] Median (50th percentile)
companion Roche lobe radius
63- 67 F5.2 Rsun e_MedRad [0/55.5] Uncertainty in MedRad
69- 74 F6.2 Rsun MaxRad [1/223.2] The 3σ (99.9th
percentile) companion Roche lobe radius
76- 80 F5.2 10+12cm MedSep [0.2/40.2] Median (50th percentile)
companion Roche lobe radius
82- 85 F4.2 10+12cm e_MedSep [0/9.99] Uncertainty in MedSep
87- 91 F5.2 10+12cm MaxSep [0.2/40.2] The 3σ (99.9th percentile)
companion Roche lobe radius
93- 100 F8.2 [-] lnZ [-7151.4/11354.3] Natural log of Bayesian
Evidence Z from dynesty
102- 105 F4.2 [-] e_lnZ [0.04/0.2] Uncertainty in lnZ
107- 115 F9.2 --- BIC [-22733.8/14311.4] Bayesian Information
Criterion
117- 120 I04 --- Mask [0/1110] BitMask (2)
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Note (1): The uncertainty on the rise time is determined by the uncertainty
on the time of first light (column 3).
Note (2): The same Quality Bitmask from Table 1, which marks the subsamples of
SNe: TESS did not observe the peak flux of this SN (first bit,
"1000", see Appendix C), the SN is part of the "No First Light"
subsample (second bit, "0100", see Appendix C), the SN is part of
the "High Quality" subsample (third bit, "0010", see Appendix C.1),
or the SN is part of the "High Dynamic Range" subsample (fourth bit,
"0001", see Appendix C.2).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 14-Jan-2026