17 research outputs found
Circumstellar interaction models for the early bolometric light curve of SN 2023ixf
SNe II show growing evidence of interaction with CSM surrounding their
progenitor stars as a consequence of enhanced mass loss during the last years
of the progenitor's life. We present an analysis of the progenitor mass-loss
history of SN2023ixf, a nearby SN II showing signs of interaction. We calculate
the early-time bolometric light curve (LC) for SN2023ixf based on the
integration of the observed flux covering UV, optical and NIR bands, and
black-body extrapolations for the unobserved flux. Our calculations spot the
sudden increase to maximum luminosity and temperature, in addition to the
subsequent fall, displaying an evident peak. This is the first time that this
phase can be precisely estimated for a SN II showing interesting
characteristics as: 1) slope changes during the rise to maximum luminosity; and
2) a very sharp peak with a maximum luminosity of 310erg
s. We use the bolometric LC of SN2023ixf to test the calibrations of
bolometric corrections against colours from the literature. In addition, we
include SN2023ixf into some of the available calibrations to extend their use
to earlier epochs. Comparison of the observed bolometric LC to SN II explosion
models with CSM interaction suggests a progenitor mass-loss rate of
310yr confined to 12000 and a wind
acceleration parameter of =5. This model reproduces the early bolometric
LC, expansion velocities, and the epoch of disappearance of interacting lines
in the spectra. This model indicates that the wind was launched 80yr
before the explosion. If the effect of the wind acceleration is not taken into
account, the enhanced wind must have developed over the final months to years
prior to the SN, which may not be consistent with the lack of outburst
detection in pre-explosion images over the last 20yr before explosion.Comment: Submitted to A&
The progenitor of SN 2023ixf from hydrodynamical modelling
Context: Supernova (SN) 2023ixf is among the most nearby Type II SNe in the
last decades. As such, there is a wealth of observational data of both the
event itself and of the associated object identified in pre-explosion images.
This allows to perform a variety of studies that aim at determining the SN
properties and the nature of the putative progenitor star. Modelling of the
light curve is a powerful method to derive physical properties independently of
direct progenitor analyses. Aims: To investigate the physical nature of SN
2023ixf based on hydrodynamical modelling of its bolometric light curve and
expansion velocities during the complete photospheric phase. Methods: A grid of
one dimensional explosions was calculated for evolved stars of different
masses. We derived properties of SN 2023ixf and its progenitor by comparing our
models with the observations. Results: The observations are well reproduced by
the explosion of a star with zero age main sequence mass of f , an explosion energy of erg, and a nickel
production of 0.05M . This indicates that SN 2023ixf was a normal event. Our
modelling suggests a limit of and therefore
favours the low mass range among the results from pre-explosion observations.Comment: Accepted - A&A Lette
Type II supernovae from the Carnegie Supernova Project-I: I. Bolometric light curves of 74 SNe II using uBgVriYJH photometry
The present study is the first of a series of three papers where we characterise the type II supernovae (SNe II) from the Carnegie Supernova Project-I to understand their diversity in terms of progenitor and explosion properties. In this first paper, we present bolometric light curves of 74 SNe II. We outline our methodology to calculate the bolometric luminosity, which consists of the integration of the observed fluxes in numerous photometric bands (uBgVriYJH) and black-body (BB) extrapolations to account for the unobserved flux at shorter and longer wavelengths. BB fits were performed using all available broadband data except when line blanketing effects appeared. Photometric bands bluer than r that are affected by line blanketing were removed from the fit, which makes near-infrared (NIR) observations highly important to estimate reliable BB extrapolations to the infrared. BB fits without NIR data produce notably different bolometric light curves, and therefore different estimates of SN II progenitor and explosion properties when data are modelled. We present two methods to address the absence of NIR observations: (a) colour-colour relationships from which NIR magnitudes can be estimated using optical colours, and (b) new prescriptions for bolometric corrections as a function of observed SN II colours. Using our 74 SN II bolometric light curves, we provide a full characterisation of their properties based on several observed parameters. We measured magnitudes at different epochs, as well as durations and decline rates of different phases of the evolution. An analysis of the light-curve parameter distributions was performed, finding a wide range and a continuous sequence of observed parameters which is consistent with previous analyses using optical light curves.The work of the Carnegie Supernova Project was supported by the National Science Foundation under grants AST-0306969, AST-0607438, AST-1008343, AST-1613426, AST-1613472, and AST-1613455. L. M. acknowledges support from a CONICET fellowship. L. M. and M. O. acknowledge support from UNRN PI2018 40B885 grant. M. H. acknowledges support from the Hagler Institute of Advanced Study at Texas A&M University. S. G. G. acknowledges support by FCT under Project CRISP PTDC/FIS-AST-31546/2017 and Project No. UIDB/00099/2020. M. S. is supported by grants from the VILLUM FONDEN (grant number 28021) and the Independent Research Fund Denmark (IRFD; 8021-00170B). F. F. acknowledges support from the National Agency for Research and Development (ANID) grants: BASAL Center of Mathematical Modelling AFB-170001, Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC12009, awarded to the Millennium Institute of Astrophysics, and FONDECYT Regular #1200710. L. G. acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MICIU) under the 2019 Ramón y Cajal program RYC2019-027683 and from the Spanish MICIU project PID2020-115253GA-I00. P.H. acknowledges the support by National Science Foundation (NSF) grant AST-1715133
Type II supernovae from the Carnegie Supernova Project-I. II. Physical parameter distributions from hydrodynamical modelling
Linking supernovae to their progenitors is a powerful method for furthering
our understanding of the physical origin of their observed differences, while
at the same time testing stellar evolution theory. In this second study of a
series of three papers where we characterise SNe II to understand their
diversity, we derive progenitor properties (initial and ejecta masses, and
radius), explosion energy, Ni mass, and its degree of mixing within the
ejecta for a large sample of SNe II. This dataset was obtained by the Carnegie
Supernova Project-I and is characterised by a high cadence of their optical and
NIR light curves and optical spectra that were homogeneously observed and
processed. A large grid of hydrodynamical models and a fitting procedure based
on MCMC methods were used to fit the bolometric light curve and the evolution
of the photospheric velocity of 53 SNe II. We infer ejecta masses between 7.9
and 14.8 , explosion energies between 0.15 and 1.40 foe, and
Ni masses between 0.006 and 0.069 . We define a subset of
24~SNe (the `gold sample') with well-sampled bolometric light curves and
expansion velocities for which we consider the results more robust. Most SNe~II
in the gold sample (88%) are found with ejecta masses in the range of
8-10 , coming from low zero-age main-sequence masses (9-12
). The modelling of the initial-mass distribution of the gold sample
gives an upper mass limit of 21.3 and a much
steeper distribution than that for a Salpeter massive-star IMF. This IMF
incompatibility is due to the large number of low-mass progenitors found --
when assuming standard stellar evolution. This may imply that high-mass
progenitors lose more mass during their lives than predicted. However, a deeper
analysis of all stellar evolution assumptions is required to test this
hypothesis.Comment: Accepted for publication in Astronomy & Astrophysic
Type II supernovae from the Carnegie Supernova Project-I. I. Bolometric light curves of 74 SNe II using uBgVriYJH photometry
The present study is the first of a series of three papers where we
characterise the type II supernovae (SNe~II) from the Carnegie Supernova
Project-I to understand their diversity in terms of progenitor and explosion
properties. In this first paper, we present bolometric light curves of 74
SNe~II. We outline our methodology to calculate the bolometric luminosity,
which consists of the integration of the observed fluxes in numerous
photometric bands () and black-body (BB) extrapolations to account
for the unobserved flux at shorter and longer wavelengths. BB fits were
performed using all available broadband data except when line blanketing
effects appeared. Photometric bands bluer than that are affected by line
blanketing were removed from the fit, which makes near-infrared (NIR)
observations highly important to estimate reliable BB extrapolations to the
infrared. BB fits without NIR data produce notably different bolometric light
curves, and therefore different estimates of SN~II progenitor and explosion
properties when data are modelled. We present two methods to address the
absence of NIR observations: (a) colour-colour relationships from which NIR
magnitudes can be estimated using optical colours, and (b) new prescriptions
for bolometric corrections as a function of observed SN~II colours. Using our
74 SN~II bolometric light curves, we provide a full characterisation of their
properties based on several observed parameters. We measured magnitudes at
different epochs, as well as durations and decline rates of different phases of
the evolution. An analysis of the light-curve parameter distributions was
performed, finding a wide range and a continuous sequence of observed
parameters which is consistent with previous analyses using optical light
curves.Comment: Accepted for publication in A&
Type II supernovae from the Carnegie Supernova Project-I. I. Bolometric light curves of 74 SNe II using uBgVriYJH photometry
The present study is the first of a series of three papers where we characterise the type II supernovae (SNe~II) from the Carnegie Supernova Project-I to understand their diversity in terms of progenitor and explosion properties. In this first paper, we present bolometric light curves of 74 SNe~II. We outline our methodology to calculate the bolometric luminosity, which consists of the integration of the observed fluxes in numerous photometric bands () and black-body (BB) extrapolations to account for the unobserved flux at shorter and longer wavelengths. BB fits were performed using all available broadband data except when line blanketing effects appeared. Photometric bands bluer than that are affected by line blanketing were removed from the fit, which makes near-infrared (NIR) observations highly important to estimate reliable BB extrapolations to the infrared. BB fits without NIR data produce notably different bolometric light curves, and therefore different estimates of SN~II progenitor and explosion properties when data are modelled. We present two methods to address the absence of NIR observations: (a) colour-colour relationships from which NIR magnitudes can be estimated using optical colours, and (b) new prescriptions for bolometric corrections as a function of observed SN~II colours. Using our 74 SN~II bolometric light curves, we provide a full characterisation of their properties based on several observed parameters. We measured magnitudes at different epochs, as well as durations and decline rates of different phases of the evolution. An analysis of the light-curve parameter distributions was performed, finding a wide range and a continuous sequence of observed parameters which is consistent with previous analyses using optical light curves...
SN 2021gno: a Calcium-rich transient with double-peaked light curves
We present extensive ultraviolet (UV) and optical photometric and optical
spectroscopic follow-up of supernova (SN)~2021gno by the "Precision
Observations of Infant Supernova Explosions" (POISE) project, starting less
than two days after the explosion. Given its intermediate luminosity, fast
photometric evolution, and quick transition to the nebular phase with spectra
dominated by [Ca~II] lines, SN~2021gno belongs to the small family of
Calcium-rich transients. Moreover, it shows double-peaked light curves, a
phenomenon shared with only four other Calcium-rich events. The projected
distance from the center of the host galaxy is not as large as other objects in
this family. The initial optical light-curve peaks coincide with a very quick
decline of the UV flux, indicating a fast initial cooling phase. Through
hydrodynamical modelling of the bolometric light curve and line velocity
evolution, we found that the observations are compatible with the explosion of
a highly-stripped massive star with an ejecta mass of and a
Ni mass of . The initial cooling phase (first light
curve peak) is explained by the presence of an extended circumstellar material
comprising with an extension of .
We discuss if hydrogen features are present in both maximum-light and nebular
spectra, and its implications in terms of the proposed progenitor scenarios for
Calcium-rich transients.Comment: 21 pages, 13 figures, accepted for publication in MNRA
The double-peaked Type Ic supernova 2019cad: another SN 2005bf-like object
We present the photometric and spectroscopic evolution of supernova (SN) 2019cad during the first similar to 100 d from explosion. Based on the light-curve morphology, we find that SN 2019cad resembles the double-peaked Type Ib/c SN 2005bf and the Type Ic PTF11mnb. Unlike those two objects, SN 2019cad also shows the initial peak in the redder bands. Inspection of the g-band light curve indicates the initial peak is reached in similar to 8 d, while the r-band peak occurred similar to 15 d post-explosion. A second and more prominent peak is reached in all bands at similar to 45 d past explosion, followed by a fast decline from similar to 60 d. During the first 30 d, the spectra of SN 2019cad show the typical features of a Type Ic SN, however, after 40 d, a blue continuum with prominent lines of Si II lambda 6355 and C II lambda 6580 is observed again. Comparing the bolometric light curve to hydrodynamical models, we find that SN 2019cad is consistent with a pre-SN mass of 11 M-circle dot, and an explosion energy of 3.5 x 10(51) erg. The light-curve morphology can be reproduced either by a double-peaked Ni-56 distribution with an external component of 0.041 M-circle dot, and an internal component of 0.3 M-circle dot or a double-peaked Ni-56 distribution plus magnetar model (P similar to 11 ms and B similar to 26 x 10(14) G). If SN 2019cad were to suffer from significant host reddening (which cannot be ruled out), the Ni-56 model would require extreme values, while the magnetar model would still be feasible
SN 2013ai: A Link between Hydrogen-rich and Hydrogen-poor Core-collapse Supernovae
We present a study of the optical and near-infrared (NIR) spectra of SN
2013ai along with its light curves. These data range from discovery
until 380 days after explosion. SN 2013ai is a fast declining Type II
supernova (SN II) with an unusually long rise time, 18.9 ± 2.7 days in
the V-band, and a bright V-band peak absolute magnitude of
−18.7 ± 0.06 mag. The spectra are dominated by hydrogen features in the
optical and NIR. The spectral features of SN 2013ai are unique in their
expansion velocities, which, when compared to large samples of SNe II,
are more than 1,000 km s−1 faster at 50 days past explosion.
In addition, the long rise time of the light curve more closely
resembles SNe IIb rather than SNe II. If SN 2013ai is coeval with a
nearby compact cluster, we infer a progenitor zero-age main-sequence
mass of ~17 M⊙. After performing light-curve modeling,
we find that SN 2013ai could be the result of the explosion of a star
with little hydrogen mass, a large amount of synthesized 56Ni, 0.3–0.4 M⊙, and an explosion energy of 2.5–3.0 × 1051
erg. The density structure and expansion velocities of SN 2013ai are
similar to those of the prototypical SN IIb, SN 1993J. However, SN
2013ai shows no strong helium features in the optical, likely due to the
presence of a dense core that prevents the majority of γ-rays
from escaping to excite helium. Our analysis suggests that SN 2013ai
could be a link between SNe II and stripped-envelope SNe
SN 2021gno: a calcium-rich transient with double-peaked light curves
We present extensive ultraviolet (UV) and optical photometric and optical spectroscopic follow-up of supernova (SN) 2021gno by the 'Precision Observations of Infant Supernova Explosions' (POISE) project, starting less than 2 d after the explosion. Given its intermediate luminosity, fast photometric evolution, and quick transition to the nebular phase with spectra dominated by [Ca ii] lines, SN 2021gno belongs to the small family of Calcium-rich transients. Moreover, it shows double-peaked light curves, a phenomenon shared with only four other Calcium-rich events. The projected distance from the centre of the host galaxy is not as large as other objects in this family. The initial optical light-curve peaks coincide with a very quick decline of the UV flux, indicating a fast initial cooling phase. Through hydrodynamical modelling of the bolometric light curve and line velocity evolution, we found that the observations are compatible with the explosion of a highly stripped massive star with an ejecta mass of and a 56Ni mass of 0.024 M⊙. The initial cooling phase (first light-curve peak) is explained by the presence of an extended circumstellar material comprising ∼ with an extension of. We discuss if hydrogen features are present in both maximum-light and nebular spectra, and their implications in terms of the proposed progenitor scenarios for Calcium-rich transients