J/ApJ/908/51 TESS early light curves of type Ia Supernovae (Fausnaugh+, 2021)
Early-time Light Curves of Type Ia Supernovae Observed with TESS.
Fausnaugh M.M., Vallely P.J., Kochanek C.S., Shappee B.J., Stanek K.Z.,
Tucker M.A., Ricker G.R., Vanderspek R., Latham D.W., Seager S., Winn J.N.,
Jenkins J.M., Berta-Thompson Z.K., Daylan T., Doty J.P., Furesz G.,
Levine A.M., Morris R., Pal A., Sha L., Ting E.B., Wohler B.
<Astrophys. J., 908, 51 (2021)>
=2021ApJ...908...51F 2021ApJ...908...51F
ADC_Keywords: Supernovae; Photometry, VRI
Keywords: Type Ia supernovae ; Supernovae
Abstract:
We present the early-time light curves of Type Ia supernovae (SNeIa)
observed in the first six sectors of Transiting Exoplanet Survey
Satellite (TESS) data. Ten of these SNe were discovered by ASAS-SN,
seven by ATLAS, six by ZTF, and one by Gaia. For nine of these objects
with sufficient dynamic range (>3.0mag from detection to peak), we fit
power-law models and searched for signatures of companion stars. We
found a diversity of early-time light-curve shapes, although most of
our sources are consistent with fireball models where the flux
increases as ∝t2. Three SNe displayed a flatter rise with flux
∝t. We did not find any obvious evidence for additional
structures, such as multiple power-law components, in the early rising
light curves. For assumptions about the SN properties and the observer
viewing angle (ejecta mass of 1.4M☉, expansion velocity of
104km/s, opacity of 0.2cm2/g, and viewing angle of 45°) and a
further assumption that any companion stars would be in Roche lobe
overflow, it is possible to place upper limits on the radii of any
companion stars. Six of the nine SNe had complete coverage of the
early-time light curves, and we placed upper limits on the radii of
companion stars of ≲32R☉ for these SNe, ≲20R☉ for five of
the six, and ≲4R☉ for two of the six. The small sample size did
not allow us to put limits on the occurrence rate of companion stars
in the progenitors of SNe Ia. However, we expect that TESS observed
enough SNe in its two-year primary mission (26 sectors) to either
detect the signature of a large companion (R>20R☉) or constrain
the occurrence rate of such systems, at least for the fiducial SN
properties adopted here. We also show that TESS is capable of
detecting emission from a 1R☉ companion for an SN Ia within 50Mpc
and has a reasonable chance of doing so after about six years.
Description:
Transiting Exoplanet Survey Satellite (TESS) observes in a single
broadband filter ranging from about 600 to 1000nm with an effective
wavelength of 800nm.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 91 24 Properties of the supernova sample
table2.dat 48 27705 TESS supernova light curves
table5.dat 130 768 *TESS light curves
refs.dat 44 43 References used for table1
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Note on table5.dat: For Kasen, 2010ApJ...708.1025K 2010ApJ...708.1025K models at 100Mpc.
In the local universe, the effects of time dilation and K corrections
are negligible, and these light curves can be rescaled based on
luminosity distance alone.
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See also:
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
J/ApJ/788/48 : X-ray through NIR photometry of NGC 2617 (Shappee+, 2014)
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/853/62 : Optical and NIR spectra and LCs of SN2016ija (Tartaglia+, 2018)
J/ApJ/870/L1 : K2 observations type Ia supernova SN2018oh (Dimitriadis+, 2019)
J/ApJ/883/111 : UV-Opt LCs of ASASSN-19bt detected by TESS (Holoien+, 2019)
J/ApJ/870/13 : K2 light curve analysis of ASASSN-18bt (Shappee+, 2019)
J/ApJ/886/152 : ZTF early observations of Type Ia SNe. I. LCs (Yao+, 2019)
J/ApJ/893/143 : UBVRIJHK & spec. obs. of type Ia SN2019ein (Kawabata+, 2020)
J/A+A/634/A37 : TURTLS Light curves of 56Ni distributions (Magee+, 2020)
J/ApJ/898/56 : UVOT, ZTF gri LCs & spectra of SN Ia 2019yvq (Miller+, 2020)
J/ApJ/902/47 : ZTF early obs. of type Ia SNe. II. Rise time (Miller+, 2020)
J/ApJ/897/159 : Type Ia supernova SN2019ein UBVgri photo. (Pellegrino+, 2020)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- SN Super Nova identifier
11- 23 A13 --- TNS Discovery survey identifier
25- 29 F5.2 mag mag [14.9/19.2]? Apparent peak magnitude
31- 34 F4.2 mag Dmag [0.59/4.89]? Differential magnitude
36- 41 F6.2 mag MAG [-20.9/-16.3]? Absolute magnitude (1)
43- 46 F4.2 mag e_MAG [0.09/2]? Error in MAG
48- 54 E7.3 erg/s vLv [3.7e+45/3.3e+47]? Luminosity
56- 61 F6.4 --- z [0.01/0.09] Redshift
63- 67 F5.3 mag B-V [0.005/0.3] E(B-V) color
69- 73 A5 --- Discov Discorvery reference
75- 79 A5 --- Class Classification reference
81 A1 --- Note1 X = fit with a power law to characterize the early
light curve (see section 4)
83 A1 --- Note2 X = searched for signatures of companion stars
(section 5)
85 A1 --- Note3 X = flux calibrated across two sectors using a
joint fit to both data sets (section 3)
87 A1 --- Note4 X = near strong scattered light backgrounds at the
time of first light
89 A1 --- Note5 X = affected by pixels with enhanced sensitivity
from "straps"
91 A1 --- Note6 X = near bright stars and required detrending
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Note (1): The absolute magnitude for SN2018kfv is implausibly low for
the redshift reported to TNS. The classification spectrum is
low-resolution and consistent with redshifts up to 0.03. At z=0.03,
the absolute magnitude of SN2018kfv would be -18.9.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- SN Supernova identifier
8- 21 A14 --- TNS Discovery survey identifier
24- 34 F11.6 d BJD [1325/1491] Barycentric Julian Date JD-2457000.0
36- 41 F6.2 e/s Flux [-30/168] Observed flux
43- 46 F4.2 e/s e_Flux [0.8/5] Uncertainty in Flux
48 I1 --- Asteroid [0/1] Asteroid flag (1)
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Note (1): A boolean value that marks epochs for which we identified
asteroids moving through the photometric apertures.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 9 F9.6 d Time [0.001/17] Time since explosion
11- 19 F9.6 e/s Flux50 [0.006/21.7] 50R* companion model flux
21- 27 F7.4 mag mag50 [17/25.9] 50R* companion model apparent magnitude
29- 37 F9.6 e/s Flux25 [0.005/12.9] 25R* companion model flux
39- 45 F7.4 mag mag25 [17.6/26.1] 25R* companion model apparent
magnitude
47- 54 F8.6 e/s Flux10 [0.004/6.42] 10R* companion model flux
56- 62 F7.4 mag mag10 [18.4/26.3] 10R* companion model apparent
magnitude
64- 71 F8.6 e/s Flux5 [0.003/3.78] 5R* companion model flux
73- 79 F7.4 mag mag5 [18.9/26.5] 5R* companion model apparent magnitude
81- 88 F8.6 e/s Flux1 [0.002/1.13] 1R* companion model flux
90- 96 F7.4 mag mag1 [20.3/27] 1R* companion model apparent magnitude
98-105 F8.6 e/s Flux0.5 [0.002/0.67] 0.5R* companion model flux
107-113 F7.4 mag mag0.5 [20.8/27.2] 0.5R* companion model apparent
magnitude
115-122 F8.6 e/s Flux0.1 [0.0004/0.2] 0.1R* companion model flux
124-130 F7.4 mag mag0.1 [22.2/28.9] 0.1R* companion model apparent
magnitude
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Ref Reference code
7- 24 A18 --- Autor Main autor
26- 44 A19 --- BIB BIBcode
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 27-Jun-2022