J/ApJ/926/125 Fast-evolving SNIbn with LCO LCs & FLOYDS sp. (Pellegrino+, 2022)
Circumstellar interaction powers the light curves of luminous rapidly evolving
optical transients.
Pellegrino C., Howell D.A., Vinko J., Gangopadhyay A., Xiang D.,
Arcavi I., Brown P., Burke J., Hiramatsu D., Hosseinzadeh G., Li Z.,
McCully C., Misra K., Newsome M., Gonzalez E.P., Pritchard T.A.,
Valenti S., Wang X., Zhang T.
<Astrophys. J., 926, 125 (2022)>
=2022ApJ...926..125P 2022ApJ...926..125P
ADC_Keywords: Supernovae; Transient; Photometry, UBVRI; Spectra, optical;
Redshifts
Keywords: Supernovae ; Core-collapse supernovae ; Circumstellar matter
Abstract:
Rapidly evolving transients, or objects that rise and fade in
brightness on timescales two to three times shorter than those of
typical Type Ia or Type II supernovae (SNe), have uncertain progenitor
systems and powering mechanisms. Recent studies have noted
similarities between rapidly evolving transients and Type Ibn SNe,
which are powered by ejecta interacting with He-rich circumstellar
material (CSM). In this work we present multiband photometric and
spectroscopic observations from Las Cumbres Observatory and Swift of
four fast-evolving Type Ibn SNe. We compare these observations with
those of rapidly evolving transients identified in the literature. We
discuss several common characteristics between these two samples,
including their light curve and color evolution as well as their
spectral features. To investigate a common powering mechanism we
construct a grid of analytical model light curves with luminosity
inputs from CSM interaction as well as 56Ni radioactive decay. We
find that models with ejecta masses of ∼1-3M☉, CSM masses of
∼0.2-1M☉, and CSM radii of ∼20-65au can explain the diversity of
peak luminosities, rise times, and decline rates observed in Type Ibn
SNe and rapidly evolving transients. This suggests that a common
progenitor system-the core collapse of a high-mass star within a dense
CSM shell-can reproduce the light curves of even the most luminous and
fast-evolving objects, such as AT 2018cow. This work is one of the
first to reproduce the light curves of both SNe Ibn and other rapidly
evolving transients with a single model.
Description:
In this work we present Las Cumbres Observatory (LCO) photometry and
spectra of SN 2019deh and SN 2021jpk, two fast-evolving SNe Ibn. ZTF
observations of SN 2019deh were discussed in Ho+ (2023ApJ...949..120H 2023ApJ...949..120H)
while SN 2021jpk has no published data thus far.
SN 2019deh and SN 2021jpk were discovered by ZTF on MJD 58580.36
(2019-Apr-7.36 UT) and MJD 59317.29 (2021-Apr-13.29) at r-band
magnitude 20.75±0.28 and g-band magnitude 19.26±0.09,
respectively. Assuming a standard cosmology with H0=73km/s/Mpc,
Ωm=0.27, and ΩΛ=0.73, the luminosity distances
we use for SN 2019deh and SN 2021jpk are 237Mpc and 164Mpc, respectively.
LCO light curves for both objects along with detections from ZTF, the
Asteroid Terrestrial-impact Last Alert System (ATLAS), Swift, and the
Tsinghua NAOC Telescope (TNT) are shown in Figure 1.
LCO UBgVri-band data were obtained with the Sinistro camera on LCO 1m
telescopes.
We also obtained two epochs of BgVri-band photometry of SN 2021jpk
using the 0.8m TNT.
LCO spectra covering the optical range from 3500 to 10000Å at a
resolution R∼300-600 were obtained with the Folded Low Order
whYte-pupil Double-dispersed Spectrograph (FLOYDS) spectrographs on
the Faulkes Telescope North and Faulkes Telescope South through the
Global Supernova Project (GSP).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 92 4 SNe Ibn sample parameters
table2.dat 88 40 Optical photometry
table4.dat 54 8 Log of FLOYDS spectroscopic observations
sp/* . 8 Individual spectra in ASCII format
(Data behind Figure 5)
--------------------------------------------------------------------------------
See also:
II/183 : UBVRI Photometric Standards (Landolt 1992)
J/AJ/109/874 : Kinematics of MKW and AWM Poor Clusters (Beers+ 1995)
J/other/Sci/337.444 : RV curves of Galactic massive O stars (Sana+, 2012)
J/A+A/555/A10 : Light curves of 5 type IIn supernovae (Taddia+, 2013)
J/ApJS/213/19 : Optical and near-IR light curves of 64 SNe (Bianco+, 2014)
J/ApJ/794/23 : Pan-STARRS1 transients optical photometry (Drout+, 2014)
J/ApJ/789/104 : SNe IIn observations and properties (Ofek+, 2014)
J/A+A/574/A60 : Light curve templates of SNe Ib/c from SDSS (Taddia+, 2015)
J/ApJ/819/35 : LCs of four transients from PTF & SNLS (Arcavi+, 2016)
J/MNRAS/459/3939 : Type II supernova light curves (Valenti+, 2016)
J/MNRAS/481/894 : Rapidly evolving transients in the DES (Pursiainen+, 2018)
J/ApJ/895/L23 : Radio obs. of the transient CSS161010 (Coppejans+, 2020)
J/ApJ/895/32 : Zwicky Transient Facility BTS. I. (Fremling+, 2020)
J/ApJ/895/49 : Optical sp. of ZTF18abvkwla and its host galaxy (Ho+, 2020)
J/ApJ/912/46 : ZTF Type II supernovae with follow-up obs. (Bruch+, 2021)
J/ApJ/907/99 : Pre-explosion light curve of 227 SNe (Strotjohann+, 2021)
J/ApJ/917/97 : Spectroscopic obs. of type Ibn ASASSN-14ms (Wang+, 2021)
J/ApJ/910/42 : LCs and spectroscopic obs. of AT2018cow (Xiang+, 2021)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name SN name
12- 16 F5.3 --- z [0.02/0.054] Redshift
18- 25 F8.2 d MJD [58499.4/59316.3] Time of explosion
27- 30 F4.2 d e_MJD [0.25/3] MJD uncertainty
32 A1 --- n_MJD a=r-band; b=g-band
34- 41 F8.2 d MJDmax [58508.1/59324.1] Time of maximum
43- 46 F4.2 d e_MJDmax [0.45/2] MJDmax uncertainty
48- 52 F5.3 mag/d gRate [0.11/0.15] g-band decline rate
54- 58 F5.3 mag/d e_gRate [0.002/0.005] gRate uncertainty
60- 92 A33 --- Ref Reference
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name SN name
12- 18 F7.1 d MJD [58587.6/59333.2] Modified Julian date of
observation (JD-2400000.5)
20- 24 F5.2 mag Umag [16.5/20.1]? U band magnitude
26- 29 F4.2 mag e_Umag [0.06/0.5]? One sigma error in the U magnitude
31- 35 F5.2 mag Bmag [17.3/21.6]? B band magnitude
37- 40 F4.2 mag e_Bmag [0.03/0.8]? One sigma error in the B magnitude
42- 46 F5.2 mag gmag [17.3/21]? g band magnitude
48- 51 F4.2 mag e_gmag [0.01/0.3]? One sigma error in the g magnitude
53- 57 F5.2 mag Vmag [17.4/20.9]? V band magnitude
59- 62 F4.2 mag e_Vmag [0.03/0.6]? One sigma error in the V magnitude
64- 68 F5.2 mag rmag [17.4/21.5]? R band magnitude
70- 73 F4.2 mag e_rmag [0.01/0.6]? One sigma error in the r magnitude
75- 79 F5.2 mag imag [17.6/21.2]? I band magnitude
81- 84 F4.2 mag e_imag [0.02/0.8]? One sigma error in the i magnitude
86- 88 A3 --- Tel Observatory/telescope ("LCO" or "TNT")
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Transient name
12- 19 F8.2 d MJD [58309.3/59323.6] Modified Julian Date
21- 24 F4.1 d Phase [-3.6/22.3] Phase; days relative to g-band
maximum light
26- 29 I4 0.1nm lam1 [3500] Lower range of wavelength in Å
30 A1 --- --- [-]
31- 35 I5 0.1nm lam2 [9000/10000] Upper range of wavelength in Å
37- 54 A18 --- File File name in subdirectory "sp";
column added by CDS
--------------------------------------------------------------------------------
Byte-by-byte Description of file: sp/*
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 24 E24.19 0.1nm lambda [3499.5/10001.1] Wavelength, Angstroms
26- 50 E25.19 cW/m2/nm Flux [-6.1e-17/1.5e-15] Flux density,
erg/s/cm2/Å
--------------------------------------------------------------------------------
Acknowledgements:
Craig Pellegrino [cpellegrino at lco.global]
History:
From electronic version of the journal
* 22-Nov-2023: Insert into VizieR
* 27-nov-2023: Phase for SN 2021jpk corrected in Table 4.
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 30-Oct-2023