J/ApJ/960/72 ZTF light curves of 29 BTS supernovae (Strotjohann+, 2024)
Search for supernova progenitor stars with ZTF and LSST.
Strotjohann N.L., Ofek E.O., Gal-Yam A., Sollerman J., Chen P., Yaron O.,
Zackay B., Rehemtulla N., Gris P., Masci F.J., Rusholme B., Purdum J.
<Astrophys. J., 960, 72 (2024)>
=2024ApJ...960...72S 2024ApJ...960...72S
ADC_Keywords: Supernovae; Photometry; Optical; Surveys
Keywords: Core-collapse supernovae ; Massive stars ; Red supergiant stars ;
Sky surveys
Abstract:
The direct detection of core-collapse supernova (SN) progenitor stars
is a powerful way of probing the last stages of stellar evolution.
However, detections in archival Hubble Space Telescope images are
limited to about one detection per year. Here, we explore whether we
can increase the detection rate by using data from ground-based
wide-field surveys. Due to crowding and atmospheric blurring,
progenitor stars can typically not be identified in preexplosion
images alone. Instead, we combine many pre-SN and late-time images to
search for the disappearance of the progenitor star. As a proof of
concept, we implement our search of ZTF data. For a few hundred
images, we achieve limiting magnitudes of ∼23mag in the g and r bands.
However, no progenitor stars or long-lived outbursts are detected for
29 SNe within z≤0.01, and the ZTF limits are typically several
magnitudes less constraining than detected progenitors in the
literature. Next, we estimate progenitor detection rates for the
Legacy Survey of Space and Time (LSST) with the Vera C. Rubin
telescope by simulating a population of nearby SNe. The background
from bright host galaxies reduces the nominal LSST sensitivity by, on
average, 0.4 mag. Over the 10 yr survey, we expect the detection of
∼50 red supergiant progenitors and several yellow and blue
supergiants. The progenitors of Type Ib and Ic SNe will be detectable
if they are brighter than -4.7 or -4.0 mag in the LSST i band,
respectively. In addition, we expect the detection of hundreds of
pre-SN outbursts depending on their brightness and duration.
Description:
Our ZTF search is based on SNe detected by the Bright Transient Survey
(BTS; Fremling+ 2020, J/ApJ/895/32; Perley+ 2020ApJ...904...35P 2020ApJ...904...35P).
For our search, we select 60 SNe that exploded between 2018 and 2021
within z≤0.01 or 45Mpc.
We download IPAC difference images (IRSA 2022; doi: 10.26131/IRSA539)
and calculate ZTF forced-photometry light curves for the selected SNe
as described in Appendix A.1. We inspect the light curves visually
and, if necessary, correct the approximate explosion date, t0, to
ensure that the selected pre-SN observations do not contain any SN
light. Conservatively, we only combine observations obtained more than
10d before t0 to calculate the preexplosion flux.
Of the 52 nearby SNe with pre-SN observations 29 have already faded
below magnitude 23 and Table 1 lists their properties.
See Section 2.1.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 119 29 *Nearby Bright Transient Survey (BTS) supernovae
(SNe)
table2.dat 52 29982 *Unbinned ZTF forced-photometry light curves for 29
nearby SNe
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Note on table1.dat: All SNe with ≤20 data points before and after the
SN in the same field. Data obtained more than 10 days before JD are
used to measure the pre-explosion flux.
Note on table2.dat: We removed all data points that do not pass our
quality cuts, applied a baseline correction, and rescaled flux
uncertainties based on the observed scatter of pre-SN observations
(see Appendix A).
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See also:
VII/291 : GLADE+ (Galaxy List for the Advanced Detector Era) (Dalya+, 2022)
J/MNRAS/395/1409 : Type II-P SN progenitor constraints (Smartt+, 2009)
J/MNRAS/412/1441 : SNe luminosity functions (Li+, 2011)
J/ApJ/789/104 : SNe IIn observations and properties (Ofek+, 2014)
J/A+A/580/A142 : SN 2011dh. The first two years (Ergon+, 2015)
J/ApJ/811/117 : R-band PTF observations of SNe IIb (Strotjohann+, 2015)
J/ApJ/887/169 : UV-Opt light curves of the type Ic SN 2018gep (Ho+, 2019)
J/ApJ/882/L15 : SN 2018hna photometry & spectroscopy obs. (Singh+, 2019)
J/ApJ/875/136 : BVRI, sp. & IR obs. of type II-P SN2017eaw (Van Dyk+, 2019)
J/ApJ/886/152 : ZTF early observations of Type Ia SNe. I. LCs (Yao+, 2019)
J/ApJ/895/31 : Photometric obs. of Type II SN 2018ivc (Bostroem+, 2020)
J/ApJ/895/32 : Zwicky Transient Facility BTS. I. (Fremling+, 2020)
J/ApJ/898/166 : UV to NIR obs. of SN 2019ehk (Jacobson-Galan+, 2020)
J/ApJ/900/11 : Spectra of SN 2017eaw after explosion (Weil+, 2020)
J/ApJ/912/46 : ZTF Type II supernovae with follow-up obs. (Bruch+, 2021)
J/A+A/655/A105 : 3 SN multiwavelength light curves (Sollerman+, 2021)
J/ApJ/907/99 : Pre-explosion light curve of Supernovae (Strotjohann+, 2021)
J/A+A/655/A90 : SN 2020cxd multi-photometry (Yang+, 2021)
J/ApJ/924/55 : UV and optical obs. of type Ic SN 2020oi (Gagliano+, 2022)
J/ApJ/924/15 : Final moments. I. Type II SN 2020tlf (Jacobson-Galan+, 2022)
J/ApJ/932/58 : LCs and sp. of SNe 2021gno & 2021inl (Jacobson-Galan+, 2022)
J/A+A/660/A34 : X-Shooter Spectral Library (XSL). DR3 (Verro+, 2022)
J/ApJ/952/119 : SNII during ZTF 1st phase survey & follow-up (Bruch+, 2023)
J/ApJ/949/75 : ugriBV phot. & sp. of type II-P SN2019mhm (Vazquez+, 2023)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- --- [SN]
4- 11 A8 --- SN IAU identifier
13- 15 A3 --- --- [ZTF]
17- 25 A9 --- ZTF ZTF identifier
27- 36 F10.6 deg RAdeg [34/310.5] Right Ascension (J2000)
38- 47 F10.6 deg DEdeg [-26/71.1] Declination (J2000)
49- 63 A15 --- Type Supernova type
65- 65 A1 --- f_Type Flag on Type (1)
67- 75 F9.1 d JD Julian date of the approximate explosion
77- 79 I3 d t23 [305/772] Time after explosion when SN likely
faded to 23rd mag in r band
81- 92 A12 --- Host Host galaxy identifier
94- 97 F4.1 Mpc Dist [14.7/44.6] Distance
99- 99 A1 --- f_Dist [i] No host galaxy redshift available
101-101 A1 --- l_mag Limit flag on mag
102-106 F5.2 mag mag [24.8/28.7]? Detected progenitor magnitude
in Band
108-111 F4.2 mag e_mag [0.02/0.07]? Uncertainty in mag
113-117 A5 --- Band Observation band of progenitor (F555W, F606W,
F635W or F814W)
119-119 A1 --- f_mag Flag on mag (1)
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Note (1): Flag as follows:
e = Jacobson-Galan et al. (2022, J/ApJ/932/58)
g = Singh et al. (2019, J/ApJ/882/L15)
a = Sollerman et al. (2021A&A...665A.105S 2021A&A...665A.105S)
b = Tinanont et al. (2022MNRAS.512.2777T 2022MNRAS.512.2777T)
c = Jacobson-Galan et al. (2020, J/ApJ/898/166)
d = bright cluster. Gagliano et al. (2022, J/ApJ/924/55)
f = Bostroem et al. (2020, J/ApJ/895/31)
h = Kilpatrick et al. (2021MNRAS.504.2073K 2021MNRAS.504.2073K), likely a
binary system (Sun et al. 2022MNRAS.510.3701S 2022MNRAS.510.3701S).
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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- 2 A2 --- --- [SN]
3- 10 A8 --- SN IAU identifier
12- 24 F13.5 d JD Julian Date of the observation
26- 29 I4 --- Field [277/1876] The ZTF field (1)
30- 31 I2 --- CCID [1/16] The ZTF CCD ID (1)
32 I1 --- QID [1/4] The ZTF quadrant ID (1)
33 I1 --- Filt [1/2] The ZTF filter code (1=g, 2=r) (1)
35- 43 E9.2 3.63uJy Flux [-452/3060] Observed flux, in 10-9maggy (2)
45- 52 E8.2 3.63uJy e_Flux [0.04/114] Uncertainty in Flux (2)
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Note (1): The ZTF field, CCD ID, quadrant ID, and filter of the ZTF
observations give the FCQFID cited in the paper. The ZTF data
on IRSA are available at IPAC doi: 10.26131/IRSA539
Note (2): Fluxes are given in 10-9maggies. Maggies are a linear flux density
unit defined as where is the AB apparent magnitude. That is, 1 maggie
is the flux density in Janskys divided by 3631.
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History:
From electronic version of the journal (In MRT table 2,
Flux have been /1e-9, so that they are in nanomaggies as in the PDF version).
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 10-Mar-2026