J/ApJ/912/46 ZTF Type II supernovae with follow-up obs. (Bruch+, 2021)
A large fraction of hydrogen-rich supernova progenitors experience elevated mass
loss shortly prior to explosion.
Bruch R.J., Gal-Yam A., Schulze S., Yaron O., Yang Yi, Soumagnac M.,
Rigault M., Strotjohann N.L., Ofek E., Sollerman J., Masci F.J.,
Barbarino C., Ho A.Y.Q., Fremling C., Perley D., Nordin J., Cenko S.B.,
Adams S., Adreoni I., Bellm E.C., Blagorodnova N., Bulla M., Burdge K.,
De K., Dhawan S., Drake A.J., Duev D.A., Dugas A., Graham M., Graham M.L.,
Irani I., Jencson J., Karamehmetoglu E., Kasliwal M., Kim Y.-L.,
Kulkarni S., Kupfer T., Liang J., Mahabal A., Miller A.A., Prince T.A.,
Riddle R., Sharma Y., Smith R., Taddia F., Taggart K., Walters R., Yan L.
<Astrophys. J., 912, 46 (2021)>
=2021ApJ...912...46B 2021ApJ...912...46B
ADC_Keywords: Supernovae; Photometry; Spectra, optical; Redshifts
Keywords: Type II supernovae ; Massive stars ; Flash spectra ;
Transient sources ; Stellar mass loss ; Observational astronomy
Abstract:
Spectroscopic detection of narrow emission lines traces the presence
of circumstellar mass distributions around massive stars exploding as
core-collapse supernovae. Transient emission lines disappearing
shortly after the supernova explosion suggest that the material
spatial extent is compact and implies an increased mass loss shortly
prior to explosion. Here, we present a systematic survey for such
transient emission lines (Flash Spectroscopy) among Type II supernovae
detected in the first year of the Zwicky Transient Facility survey. We
find that at least six out of ten events for which a spectrum was
obtained within two days of the estimated explosion time show evidence
for such transient flash lines. Our measured flash event fraction
(>30% at 95% confidence level) indicates that elevated mass loss is a
common process occurring in massive stars that are about to explode as
supernovae.
Description:
The Zwicky Transient Facility (ZTF) is a wide-field, high cadence,
multiband survey that started operating in 2018 March. ZTF imaging is
obtained using the Samuel Oschin 48" Schmidt telescope at Palomar
observatory (P48). ZTF observing time is divided into three programs:
the public (MSIP) 3 day all-sky survey, partnership surveys, and
Caltech programs. This paper is based on data obtained by the
high-cadence partnership survey. As part of this program, during 2018,
extragalactic survey fields were observed in both the ZTF g- and
r-bands 2-3 times per night, per band. A 30s integration time was used
in both g- and r-band exposures. We conducted our year-1 ZTF survey
for infant SNe following the methodology of
Gal-Yam+ (2011, J/ApJ/736/159). See Sections 2.1 and 2.2.
Our goal was to obtain rapid spectroscopy of real infant (RI) SN
candidates. This was made possible using rapid ToO follow-up programs
as well as on-request access to scheduled nights on various
telescopes. The robotic Spectral Energy Distribution Machine (SEDm) at
Palomar observatory was triggered for all candidates brighter than a
threshold magnitude of 19mag in 2018. Higher-resolution spectra (using
the 4.2m William Herschel Telescope (WHT), Gemini, or other available
instruments) were triggered for events showing recent non-detection
limits (within 2.5 days prior to first detection) as well as a
significant rise in magnitude compared to a recent limit or within the
observing night. See Section 2.3.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 89 28 Sample of real infant 2018 (28 objects)
table3.dat 96 9722 Forced photometry of the real infant (RI) sample
table4.dat 84 33 Peak absolute magnitudes of the 17 objects
within the 7-day spectroscopic sub-sample
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/MNRAS/395/1409 : Type II-P SN progenitor constraints (Smartt+, 2009)
J/ApJ/736/159 : Photometry monitoring of the SN PTF10vdl (Gal-Yam+, 2011)
J/other/Nat/494.65 : SN 2010mc outburst before explosion (Ofek+, 2013)
J/A+A/555/A10 : Light curves of 5 type IIn supernovae (Taddia+, 2013)
J/MNRAS/441/1186 : Cataclysmic variables from CRTS (Drake+, 2014)
J/ApJ/789/104 : SNe IIn observations and properties (Ofek+, 2014)
J/ApJ/811/117 : R-band PTF observations of SNe IIb (Strotjohann+, 2015)
J/MNRAS/449/1753 : I-band LCs of SNe II from OGLE-IV (Poznanski+, 2015)
J/A+A/587/L7 : Metallicity from Type II SN from (i)PTF (Taddia+, 2016)
J/A+A/589/A110 : SN II in host HII regions (Anderson+, 2016)
J/MNRAS/459/3939 : Type II supernova light curves (Valenti+, 2016)
J/ApJ/820/33 : R-band light curves of type II supernovae (Rubin+, 2016)
J/ApJ/828/111 : Unsupervised clustering of type II SNe LCs (Rubin+, 2016)
J/ApJ/835/166 : SNe type II from CSP-I, SDSS-II & SNLS (de Jaeger+, 2017)
J/ApJS/233/6 : SNe II light curves & spectra from the CfA (Hicken+, 2017)
J/ApJ/861/63 : Type IIP SN 2016bkv LCs and spectra (Hosseinzadeh+, 2018)
J/A+A/611/A25 : Updated Type II supernova Hubble diagram (Gall+, 2018)
J/MNRAS/483/5459 : SNeII as distance indicators at near-IR (Rodriguez+, 2019)
J/A+A/637/A73 : Type IIn supernova photometry (Nyholm+, 2020)
J/ApJ/895/31 : Phot. observations of Type II SN 2018ivc (Bostroem+, 2020)
J/ApJ/902/6 : UV to visible-light obs. of SN 2018fif (Soumagnac+, 2020)
J/ApJ/907/99 : Pre-explosion light curve of 227 SNe (Strotjohann+, 2021)
http://www.wis-tns.org/ : Transient Name Server home page
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- SN IAU identifier (YYYYaaa)
9- 17 A9 --- ZTF Internal ZTF identifier
19- 24 A6 --- Type TNS classification
26- 27 I2 --- r_Type [1/28] Classification report (1)
29- 33 F5.3 --- z [0.01/0.07] Spectroscopic redshift
35- 46 F12.4 d JD Julian Date of estimated explosion date, EED
48- 53 F6.4 d e_JD [0.001/3.5] Uncertainty in JD
55- 61 F7.4 d FD [-0.47/3.5] Date of first detection relative
to to EED in JD
63- 69 F7.4 d LD [-3.5/1.95] Last non-detection relative
to EED in JD
71- 77 F7.4 d FS [0.14/55.05] First spectrum relative to EED in JD
79- 87 A9 --- Inst Telescope/Instrument identifiers (2)
89 A1 --- Flash Flash detected (c=Yes; x=No or ?=unknown)
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Note (1): Report references as follows:
1 = Fremling et al. (2018TNSCR1519....1F 2018TNSCR1519....1F)
2 = Fremling et al. (2018TNSCR1404....1F 2018TNSCR1404....1F)
3 = Hiramatsu et al. (2018TNSCR.974....1H 2018TNSCR.974....1H)
4 = Fremling & Sharma (2018TNSCR1028....1F 2018TNSCR1028....1F)
5 = Fremling & Sharma (2018TNSCR1034....1F 2018TNSCR1034....1F)
6 = Gal-Yam et al. (2018TNSCR1237....1G 2018TNSCR1237....1G)
7 = Fremling et al. (2018TNSCR1567....1F 2018TNSCR1567....1F)
8 = Fremling & Sharma (2018TNSCR.939....1F 2018TNSCR.939....1F)
9 = Fremling & Sharma (2018TNSCR.904....1F 2018TNSCR.904....1F)
10 = Bruch (2020TNSCR1575....1B 2020TNSCR1575....1B)
11 = Bruch (2020TNSCR1575....1B 2020TNSCR1575....1B)
12 = Fremling et al. (2018TNSCR1444....1F 2018TNSCR1444....1F)
13 = Prentice (2018TNSCR.630....1P 2018TNSCR.630....1P)
14 = Dugas et al. (2019TNSCR1402....1D 2019TNSCR1402....1D)
15 = Bruch (2020TNSCR1575....1B 2020TNSCR1575....1B)
16 = Fremling et al. (2018TNSCR1597....1F 2018TNSCR1597....1F)
17 = Fremling et al. (2018TNSCR1071....1F 2018TNSCR1071....1F)
18 = Fremling et al. (2019TNSCR.826....1F 2019TNSCR.826....1F)
19 = Bruch (2020TNSCR1575....1B 2020TNSCR1575....1B)
20 = Fremling et al. (2018TNSCR1828....1F 2018TNSCR1828....1F)
21 = Bruch (2020TNSCR1575....1B 2020TNSCR1575....1B)
22 = Fremling et al. (2018TNSCR1349....1F 2018TNSCR1349....1F)
23 = Fremling et al. (2018TNSCR1108....1F 2018TNSCR1108....1F)
24 = Bruch (2020TNSCR1575....1B 2020TNSCR1575....1B)
25 = Bruch (2020TNSCR1575....1B 2020TNSCR1575....1B)
26 = Bruch (2020TNSCR1575....1B 2020TNSCR1575....1B)
27 = Fremling et al. (2018TNSCR1340....1F 2018TNSCR1340....1F)
28 = Bruch (2020TNSCR1575....1B 2020TNSCR1575....1B)
Note (2): Instrument as follows:
P60/SEDm = The Spectral Energy Distribution Machine low-resolution (R∼100)
spectrograph mounted on the 60" robotic telescope (P60) at
Palomar observatory (17 occurrences)
P200/DBSP = The Double Beam SPectrograph mounted on the 5m Hale telescope
(P200) at Palomar Observatory (5 occurrences)
Keck/LRIS = The Low-Resolution Imaging Spectrometer mounted on the Keck I
10m telescope at the W. M. Keck Observatory in Hawaii
(2 occurrences)
WHT/ISIS = The ISIS spectrograph on the 4.2m William Herschel Telescope at
the Observatorio del Roque de los Muchachos in La Palma, Spain,
via the Optical Infrared Coordination Network for Astronomy
(OPTICON) program, R∼1000 (2 occurrences)
WHT/ACAM = The ACAM spectrograph on the 4.2m William Herschel Telescope at
the Observatorio del Roque de los Muchachos in La Palma, Spain,
via the Optical Infrared Coordination Network for Astronomy
(OPTICON) program, R∼400 (1 occurrence)
APO/DIS = The Dual Imaging Spectrograph on the Astrophysical Research
Consortium (ARC) 3.5m telescope at Apache Point Observatory
(1 occurrence)
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- SN IAU identifier (YYYYaaa)
9- 11 A3 --- --- [ZTF]
12- 20 A9 --- ZTF Internal ZTF identifier
22 A1 --- Filt [gr] Filter used
24- 38 F15.7 d JD Julian Date of the observation
40- 50 E11.4 mJy Flux [-4.43e-8/1.02e-7] Flux density in Filt
52- 61 E10.4 mJy e_Flux [3e-11/2e-8] Uncertainty in Flux
63- 68 F6.3 mag mag [17.48/38.91]? Apparent AB magnitude in Filt
70- 76 F7.3 mag Mag [-18.61/2.4]? Absolute AB magnitude in Filt
not corrected for extinction
78- 88 F11.3 mag e_mag [0.006/2735450]? AB magnitude uncertainty
90- 96 F7.3 d Time [-2.1/298.1] Time from alert system's first
detection
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- --- [SN]
3- 9 A7 --- SN IAU identifier (YYYYaaa)
11 A1 --- Filt [gr] Filter
13- 20 F8.6 --- z [0.01/0.054] Spectroscopic redshift
22- 28 F7.5 --- e_z [1e-5/0.004] Uncertainty in z
30- 31 A2 --- f_z Flag on z (1)
33- 38 F6.3 mag DM [33.5/37] Distance modulus
40- 45 F6.3 mag Pkmag [17.09/19.55] Apparent peak AB magnitude in
Filt
47- 51 F5.3 mag e_Pkmag [0.001/0.05] Uncertainty in Pkmag
53- 58 F6.3 d Pkday [1.8/22.65] Peak with respect to the EED
60- 64 F5.3 d e_Pkday [0.16/3.3] Uncertainty in Pkday
66- 70 F5.3 mag Ext [0.017/0.84] Filter AB magnitude extinction
72- 78 F7.3 mag PkMag [-18.91/-14.39] Absolute peak AB magnitude
in Filt
80- 84 F5.3 mag e_PkMag [0.009/3.8] Uncertainty in PkMag
--------------------------------------------------------------------------------
Note (1): Flag as follows:
d = The redshift was measured based on a higher resolution spectrum
(e.g. DBSP and APO, here).
dd = The redshift was measured based on a spectrum from SEDm.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 26-Oct-2022