J/A+A/637/A73 Type IIn supernova photometry (Nyholm+, 2020)
Type IIn supernova light-curve properties measured from an untargeted survey
sample.
Nyholm A., Sollerman J., Tartaglia L., Taddia F., Fremling C.,
Blagorodnova N., Filippenko A.V., Gal-Yam A., Howell D.A.,
Karamehmetoglu E., Kulkarni S.R., Laher R., Leloudas G., Masci F.,
Kasliwal M.M., Mora K., Moriya T.J., Ofek E.O., Papadogiannakis S.,
Quimby R., Rebbapragada U., Schulze S.
<Astron. Astrophys. 637, A73 (2020)>
=2020A&A...637A..73N 2020A&A...637A..73N (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Photometry
Keywords: supernovae: general
Abstract:
The evolution of a Type IIn supernova (SN IIn) is governed by the
interaction between the SN ejecta and a hydrogen-rich circumstellar
medium (CSM). SNe IIn thus allow us to probe the late-time mass-loss
history of their progenitor stars.
We present optical photometry of a sample of 42 Type IIn supernovae,
obtained by the Palomar Transient Factory (PTF) collaboration and its
successor, the intermediate PTF (iPTF), from 2009 to 2017 using the
1.2m Samuel Oschin telescope and the 1.52m telescope at Palomar
Observatory, California, USA.
Description:
We present AB magnitudes from PSF photometry (relative photometry
based on SDSS or, when unavailable, PS1) on reference subtracted
images. The magnitude errors given are statistical (1 sigma). The 1.2m
Samuel Oschin telescope (known as P48) equipped with the CFH12K mosaic
CCD was used with either a Mould R filter or an SDSS g filter. The P48
photometry was extracted with the PTFIDE (PTF Image Differencing and
Extraction) pipeline (2017PASP..129a4002M 2017PASP..129a4002M). The 1.52 m telescope
(known as P60) equipped with the GRBCam camera or the Spectral Energy
Distribution Machine (SEDM) integral field spectrograph was used with
SDSS griz and Johnson B filters. The P60 photometry was extracted with
the FPipe pipeline (2016A&A...593A..68F 2016A&A...593A..68F, Cat. J/A+A/593/A68). The
frames used for P48 reference subtraction were made by stacking
archival P48 images. The frames used for P60 reference subtraction
were made by stacking archival P60 images, or by using SDSS or PS1
images. The upper limits from the PTFIDE pipeline are reported at the
5 sigma level, upper limits from FPipe for GRBCam at 3 sigma and for
SEDM at 5 sigma. The epochs of the measurements are given in Julian
days (JD). When no value exists for the magnitude and error, or the
upper limit, this is written as "99" in the table.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
sample.dat 93 42 The 42 SNe IIn in the sample
(from table4 of the paper)
table2.dat 61 19246 Type IIn SN photometry
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See also:
J/A+A/593/A68 : PTF12os & iPTF13bvn spectra and light curves (Fremling+, 2016)
Byte-by-byte Description of file: sample.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name SN name
11- 12 I2 h RAh Right ascension (J2000.0)
14- 15 I2 min RAm Right ascension (J2000.0)
17- 21 F5.2 s RAs Right ascension (J2000.0)
23 A1 --- DE- Declination sign (J2000.0)
24- 25 I2 deg DEd Declination (J2000.0)
27- 28 I2 arcmin DEm Declination (J2000.0)
30- 33 F4.1 arcsec DEs Declination (J2000.0)
35- 41 F7.5 --- z Redshift (1)
43- 47 F5.2 mag MOD Distance modulus
49- 56 F8.2 d Disc Discovery date, refers to the time of
PTF/iPTF discovery (MJD) (2)
58- 62 F5.3 mag E(B-V)MW Milky Way colour excess for each SN is
obtained as described in Sect. 3.1
64- 69 F6.2 mag gMAGHost Host galaxy g-band absolute magnitude (3)
70- 93 A24 --- AName Alternative designations
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Note (1): The mean statistical error of the heliocentric redshifts z is
σz=0.00025, but the resolution of our spectra (typically a few
x102km/s) suggests that σz∼0.001 is a more realistic error estimate.
Note (2): The given discovery date refers to the time of PTF/iPTF discovery
(MJD=JD-2400000.5), i.e., the epoch of the image which prompted a human
scanner in the PTF/iPTF project to flag the transient as a candidate SN.
Note (3): The host galaxy g-band absolute magnitudes were obtained as described
in Sect. 4.7. The majority of SNe in our sample have been included in some
(or all) of the following three earlier SN IIn samples in the literature:
Ofek et al. (2014, Cat. J/ApJ/788/154), Ofek et al. (2014, Cat. J/ApJ/789/104)
and Ackermann et al. (2015, Cat. J/ApJ/807/169). The general SN II sample by
Arcavi et al. (2010ApJ...721..777A 2010ApJ...721..777A) and the work by Ganot et al.
(2016ApJ...820...57G 2016ApJ...820...57G) also included some of the SNe in our sample.
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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- 9 A9 --- Name PTF/iPTF name of the supernova
11- 22 F12.4 d JD Epoch (JD)
24- 28 F5.2 mag mag ?=99 Magnitude (AB) in filter
30- 34 F5.2 mag e_mag ?=99 Magnitude statistical error (1 sigma)
36- 40 F5.2 mag lmag ?=99 Upper limit magnitude (AB) in filter
42- 44 A3 --- Tel Telescope (P48 or P60)
46- 49 A4 --- Cam Camera (CFH12K for P48, GRBCam or SEDM for P60)
51 A1 --- Filter [RgrizB] Filter used (1)
53- 56 A4 --- Ref Reference frame (P48ref, P60ref, SDSS or PS1) (2)
58- 61 A4 --- Pipe Pipeline used (PTFIDE for P48, FPipe for P60)
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Note (1): Filters as follows:
R = Mould R
g = SDSS g
r = SDSS r
i = SDSS i
z = SDSS z
B = Johnson B
Note (2): PS1 means the Panoramic Survey Telescope and Rapid Response System,
and SDSS means the Sloan Digital Sky Survey.
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Acknowledgements:
Anders Nyholm, anders.nyholm(at)astro.su.se
(End) Patricia Vannier [CDS] 27-Jan-2020