Bulletin de la Société Royale des Sciences de Liège, Vol. 87, Actes de colloques, 2018, p. 356– 359
Core-collapse SNe of type IIP and their progenitors:
The case study of PNV J01315945+3328458
Raya Dastidar1∗, Brijesh Kumar1, Devendra Kumar Sahu2, Kuntal Misra1,
Mridweeka Singh1, Anjasha Gangopadhyay1, Gadiyara Chakrapani Anupama2,
Shashi Bhushan Pandey1.
1 Aryabhatta Research Institute of observational sciencES, Nainital, 263002, India
2 Indian Institute of Astrophysics, Koramangala, Bangalore, 560034, India
Abstract: The type II supernovae (SNe) are hydrogen-rich cosmic explosions resulting from the collapse of
massive stars. The impetus of studying individual events arises from its cosmological importance and the
diverse understanding of the evolution and explosion mechanism of such events. In this work, we present the
preliminary photometric and spectroscopic analysis of a recent type IIP explosion, PNV J01315945+3328458
in the galaxy NGC 582. While the initial phases of these energetic events are bright enough to be observed
with the 1-2m class telescopes, the supernovae fade below the detection limit of these telescopes in the nebular
phase. In addition, the class of sub-luminous events with Mv ∼ -15 or the events occurring at higher redshift,
fade below the detection limit of these telescopes very early in their evolution. Large aperture telescopes like
the newly installed 3.6m Devasthal Optical Telescope (DOT) will ensure a longer coverage of such events and
also to probe deeper into the Universe. With the 3.6m telescope installed in Devasthal (DOT), we plan to study
the progenitor environment of CCSNe to infer the metallicity at the explosion site.
1 Introduction
Massive stars typically in ZAMS mass range of 8-25 M (Heger et al. 2003; Eldridge and Tout 2004)
end their stellar lives in a cosmic explosion leaving behind a neutron star as a compact remnant. The
group of SNe which falls under this class and shows prominent hydrogen features in their spectra
can be further classified into normal type IIP, exhibiting a plateau in their light curve and peculiar
type IIP (SN 1987A like), showing a hump-like evolution in the corresponding plateau phase. The
plateau phase of the light curve is powered by the energy deposited in the shell after shock breakout.
The hydrogen layer ionized by the shock wave cools and recombines in this phase, allowing the
trapped energy to be radiated away. PNV J01315945+3328458 is a normal type IIP event which
exploded in the galaxy NGC 582. Monitoring campaigns were initiated soon after its discovery which
was reported around 2015 Oct.02.92241 UT. Both photometric and spectroscopic observations were
carried out with the 1-2m class telescopes in India.
∗rayadastidar@aries.res.in
”First Belgo-Indian Network for Astronomy & Astrophysics (BINA) workshop”, held in Nainital (India), 15-18 November 2016
Bulletin de la Société Royale des Sciences de Liège, Vol. 87, Actes de colloques, 2018, p. 356– 359
2 Observations and data reduction
16.0
I
R
16.5
V
17.0
SN
17.5
18.0
18.5
19.0
19.5
20 0 20 40 60 80 100 120
Days since discovery
Figure 1: Figure 2: Light curve of PNV J01315945+3328458 inPNV J01315945+3328458 in NGC 582. VRI bands.
V band image obtained with the 104cm Sampurnanand
Telescope, India.
We have used the ARIES 104cm Sampurnanand Telescope (ST) and the 130cm Devasthal Fast
Optical Telescope (DFOT) for monitoring this event with the Johnson-Cousin BVRI filters. We fol-
lowed this event up to 110 days post discovery. Standard tasks in IRAF were used for the pre-
processing of the images. Owing to the location of the supernova in the host galaxy, PSF photometry
was performed to eliminate the host galaxy contribution. We observed Landolt standard fields on 01
December 2015 along with the SN field to obtain the transformation coefficients from instrumental
magnitude to standard magnitude. These transformation coefficients were used to generate a set of
local standards in the SN field to perform differential photometry. Fig. 1 shows the location of the
supernova in the host galaxy and in Fig. 2, we have presented the time evolution of the supernova
through the V, R and I filters.
Study of individual SNe at various redshifts is necessary in order to constrain the parameters
such as the ejecta velocity, the Ni-56 mass and the explosion energy of a particular class of events.
However, a collection of good quality data of Type II SN is lacking as they evolve during some
hundreds of days, making follow-up observations very time consuming. PNV J01315945+3328458
is a mere addition to such campaigns. Later, we plan to form a sample of type IIP SN to study the
typical properties of this subclass.
3 Preliminary results and discussion
The results reported here are the following:
1. We have made a comparative study of the absolute V band light curve of PNV J01315945+3328458
with other type IIP supernovae (Fig. 3). It suggests that PNV J01315945+3328458 is most likely a
normal type IIP event.
2. Valenti et al. (2016) made a comparative study of a sample of type IIP supernovae to find out
the correlation between the various light curve parameters. They found a clear correlation between
s2, the decline rate of the shallower slope of the light curve and the length of the plateau. A rough
estimate of the s2 parameter obtained from our light curve is -0.18 in mag/50 days and from the
357
Apparent Magnitude
Bulletin de la Société Royale des Sciences de Liège, Vol. 87, Actes de colloques, 2018, p. 356– 359
correlation, we find that the plateau length corresponding to this value is around 100 days. However,
in our case, the plateau length is nearly 90 days.
3. We could not continue the observation of this event post 110 days as the event went behind
the sun and when it reappeared in the night sky, the magnitude had gone below the detection limit of
1-2m class telescopes. This emphasizes the possible contribution of the 3.6m DOT in our field.
18
pnvj01
SN2013ab
17 SN2012aw
SN2008gz
SN2004et
16
SN1999gi
SN1999em
15
14 1999em 4m
13 PNVJ01 2m
12
50 0 50 100 150 200 250 300
Phase in days
4500 5000 5500 6000 6500 7000 7500 8000
Rest Wavelength ( )
Figure 3: Comparison of the absolute V-band light
curve of PNV J01315945+3328458 with those of other
type IIP SNe like SN 1999em (Leonard et al. 2002), Figure 4: Comparison of the spectrum of SN 1999em
SN 1999gi (Leonard et al. 2002), SN 2004et (Sahu et (WiseRep) obtained with a 4m class telescope with the
al. 2006), SN 2008gz (Roy et al. 2011), SN 2012aw spectrum of PNV J01315945+3328458 obtained with a
(Bose et al. 2013) and SN 2013ab (Bose et al. 2015). 2m class telescope at similar epoch. The spectrum ob-
The magnitudes are distance and redshift corrected. The tained with a 4m class telescope shows enhanced and
absolute V band magnitude of PNV J01315945+3328458 more prominent spectral features while that obtained with
falls over other normal type IIP events indicating that it is a 2m class telescope exhibits more line blending.
most likely a normal type IIP event.
4 Scope of study with the 3.6m Devasthal Optical Telescope
Most of the cosmic explosions that are considered for the study comes from surveys which are partial
towards brighter events. This leads to a bias in the observational results as we mostly ignore their
fainter cousins. With the help of the 3.6m DOT, we expect to have a complete sample by considering
the low-luminosity events from the untargeted surveys.
Also, the nebular phase magnitude of most SNe reaches below the detection limit of 1-2m class
telescopes. With the 3.6m DOT, we can carry out deep nebular phase studies of these events using
optical filters up to 25 mag in a 300s exposure with a good signal-to-noise ratio.
Moreover, it is apparent that bigger aperture telescopes will enhance the resolution of the spectra.
In Fig. 4, we have compared spectra obtained with 2m and 4m class telescopes. There is clearly less
blending of lines and more prominent features in the spectra obtained with a 4m class telescope. The
higher resolution spectra will also allow the study of high velocity components of lines arising from
circumstellar interaction which often gets blended with the normal component of these lines in low
resolution spectra.
358
MV
Normalized Flux
Hβ 4861
FeII 5169
ScII multiplet
NaID 5890,5896
Hα 6563
Bulletin de la Société Royale des Sciences de Liège, Vol. 87, Actes de colloques, 2018, p. 356– 359
Acknowledgements
We are thankful to the observing staff of 1.04m ST, 1.3m DFOT and 2.01m HCT for their kind support
and cooperation.
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