Core-collapse supernova subtypes in luminous infrared galaxies
E. Kankare, A. Efstathiou, R. Kotak, E. C. Kool, T. Kangas, D. O'Neill, S. Mattila, P. Vaisanen, R. Ramphul, M. Mogotsi, S. D. Ryder, S. Parker, T. Reynolds, M. Fraser, A. Pastorello, E. Cappellaro, P. A. Mazzali, P. Ochner, L. Tomasella, M. Turatto, J. Kotilainen, H. Kuncarayakti, M. A. Perez-Torres, Z. Randriamanakoto, C. Romero-Canizales, M. Berton, R. Cartier, T.-W. Chen, L. Galbany, M. Gromadzki, C. Inserra, K. Maguire, S. Moran, T. E. Muller-Bravo, M. Nicholl, A. Reguitti, D. R. Young
aa r X i v : . [ a s t r o - ph . S R ] F e b Astronomy & Astrophysicsmanuscript no. aa © ESO 2021March 1, 2021
Core-collapse supernova subtypes in luminous infrared galaxies
E. Kankare , A. Efstathiou , R. Kotak , E. C. Kool , T. Kangas , D. O’Neill , S. Mattila , P. Väisänen , ,R. Ramphul , , M. Mogotsi , S. D. Ryder , , S. Parker , , T. Reynolds , M. Fraser , A. Pastorello ,E. Cappellaro , P. A. Mazzali , , P. Ochner , , L. Tomasella , M. Turatto , J. Kotilainen , ,H. Kuncarayakti , , M. A. Pérez-Torres , , Z. Randriamanakoto , C. Romero-Cañizales , M. Berton , ,R. Cartier , T.-W. Chen , L. Galbany , M. Gromadzki , C. Inserra , K. Maguire , S. Moran ,T. E. Müller-Bravo , M. Nicholl , , A. Reguitti , , , and D. R. Young (A ffi liations can be found after the references) March 1, 2021
ABSTRACT
The fraction of core-collapse supernovae (CCSNe) occurring in the central regions of galaxies is not well-constrained at present. This is partlybecause large-scale transient surveys operate at optical wavelengths, making it challenging to detect transient sources that occur in regions suscep-tible to high extinction factors. Here we present the discovery and follow-up observations of two CCSNe that occurred in the luminous infraredgalaxy (LIRG), NGC 3256. The first, SN 2018ec, was discovered using the ESO HAWK-I / GRAAL adaptive optics seeing enhancer, and wasclassified as a Type Ic with a host galaxy extinction of A V = . + . − . mag. The second, AT 2018cux, was discovered during the course of follow-upobservations of SN 2018ec, and is consistent with a sub-luminous Type IIP classification with an A V = . ± . HubbleSpace Telescope imaging. Based on template light-curve fitting, we favour a Type IIn classification for it with modest host galaxy extinction of A V = . + . − . mag. We also extend our study with follow-up data of the recent Type IIb SN 2019lqo and Type Ib SN 2020fkb that occurred in theLIRG system Arp 299 with host extinctions of A V = . + . − . and A V = . + . − . mag, respectively. Motivated by the above, we inspected, for the firsttime, a sample of 29 CCSNe located within a projected distance of 2.5 kpc from the host galaxy nuclei in a sample of 16 LIRGs. We find that, ifstar formation within these galaxies is modelled assuming a global starburst episode and normal IMF, there is evidence of a correlation betweenthe starburst age and the CCSN subtype. We infer that the two subgroups of 14 H-poor (Type IIb / Ib / Ic / Ibn) and 15 H-rich (Type II / IIn) CCSNehave di ff erent underlying progenitor age distributions, with the H-poor progenitors being younger at 3 σ significance. However, we do note thatthe available sample sizes of CCSNe and host LIRGs are so far small, and the statistical comparisons between subgroups do not take into accountpossible systematic or model errors related to the estimated starburst ages. Key words. galaxies: star formation – supernovae: general – galaxies: individual: NGC 3256, Arp 299 – supernovae: individual: SN 2018ec, AT2018cux, PSN J10275082-4354034, SN 2019lqo, SN 2020fkb – dust, extinction
1. Introduction
The local ( ≤
12 Mpc) core-collapse supernova (CCSN) popu-lation already clearly shows that optical transient survey pro-grammes are not discovering all SNe in normal spiral galax-ies due to host galaxy extinction (Mattila et al. 2012), consis-tent also with statistical studies of galaxy disk opacities (e.g.Kankare et al. 2009). Furthermore, recent surveys operating atlonger wavelengths have also discovered SNe missed by op-tical transient searches in nearby star-forming galaxies (e.g.,SPIRITS – the SPitzer InfraRed Intensive Transients Survey;Jencson et al. 2017, 2018, 2019). The e ff ect of a missing pop-ulation of CCSNe becomes even more prominent in luminous(10 L ⊙ < L IR < L ⊙ ) and ultraluminous ( L IR > L ⊙ )infrared galaxies (LIRGs and ULIRGs, respectively) which arehighly obscured and star-forming galaxies; it is also very com-mon that these objects are closely paired or merging galaxies(Sanders et al. 1988). Radio observations have shown the ex-istence of a rich population of radio SNe (and SN remnants)in ULIRGs (e.g. Parra et al. 2007; Varenius et al. 2019), LIRGs(e.g. Pérez-Torres et al. 2009; Ulvestad 2009), and starburstgalaxies (e.g. Fenech et al. 2008; Mattila et al. 2013), whichhave remained undetected by optical surveys. In particular,LIRGs are relatively rare in the local Universe; however, they dominate the cosmic star formation history and the resultingCCSN rate beyond z ∼ z ∼ A V ≈
16 mag, shows that there is a population of very highly red-dened CCSNe in these galaxies (Kankare et al. 2008). Further-more, SNe with very small projected nuclear distances but lowhost galaxy extinctions can also be missed by regular ground-based observations due to the high background luminosity of theLIRG host (e.g. SN 2010cu; Kankare et al. 2012). Therefore, itis not surprising that optical transient surveys miss a significantfraction of CCSNe in LIRGs even in the local Universe (e.g.Mattila et al. 2012; Kool et al. 2018).Previously, various statistical studies have been carried outon the properties of CCSNe in normal galaxies. Statistical stud-
Article number, page 1 of 25 & Aproofs: manuscript no. aa ies have shown that Type Ibc SNe are spatially more closelyassociated to H α regions than Type IIP SNe, and that withinType Ibc SNe, Type Ic events show the closest H α association(e.g. Anderson et al. 2012). This has been interpreted as TypeIbc SN progenitors having shorter stellar life times than TypeIIP SNe, which is expected from single stellar evolution models.Similar results have also been found e.g. by Crowther (2013),Aramyan et al. (2016), and Audcent-Ross et al. (2020). Further-more, Kangas et al. (2017) corroborated these previous resultswith their statistical study combining spatial distribution of mas-sive stars to those of di ff erent CCSN classes in local galaxies.Other statistical studies on the explosion site have also suggestedthat Type Ic SNe occur in more metal rich environments and havemore massive progenitors than Type Ib SNe (Leloudas et al.2011; Galbany et al. 2018; Kuncarayakti et al. 2018).Anderson & Soto (2013) suggested that normal galaxies tendto produce similar SN types if they host multiple SNe, and spec-ulated that this is connected to the episodic nature of the starburstevent and the resulting age range distribution of possible SN pro-genitor stars. LIRGs with their very high SN rates (SNR) o ff erlaboratories to investigate statistical SN characteristics, with theadvantage that the recent and more strongly episodic star forma-tion of the galaxy can be characterised more accurately. Onlyvery recently CCSN discoveries in central regions of LIRGsmade a statistically significant sample (Kool et al. 2018). In thesections that follow, we report discoveries of recent CCSNe inLIRGs NGC 3256 and Arp 299, and discuss the starburst age inhigh CCSN rate LIRGs with a connection to CCSN subtypes inthese galaxies.
2. NGC 3256
NGC 3256 is an ongoing LIRG merger at a redshift of z = . L IR = . L ⊙ (Sanders et al. 2003) scaled to a Tully-Fisher (TF) luminositydistance of D l = . . ± . H =
70 km s − Mpc − , Ω M = . Ω Λ = .
7) correctedfor the influence of Virgo Cluster and the Great Attractor infall(Mould et al. 2000). The IR luminosity of NGC 3256 suggestsa rate of ∼ − based on the empirical relation ofMattila & Meikle (2001). There is also some evidence of an ob-scured AGN in the system (Kotilainen et al. 1996; Emonts et al.2014; Ohyama et al. 2015). While the expected intrinsic SN rateof NGC 3256 is very high, only one spectroscopically confirmedSN has been previously reported in this nearby LIRG. This is theType II SN 2001db, discovered using near-IR observations andfound to have a significant line-of-sight extinction of A V ≈ . A V = .
334 mag (Schlafly & Finkbeiner 2011).
The High-Acuity Wide field K -band Imager (HAWK-I;Kissler-Patig et al. 2008) on the 8.2-m VLT UT4 consists of fourHAWAII 2RG 2048 × ′ × ′ and a pixel scale of 0 ′′ . / pix. We observed inthe Ks -band two LIRGs, i.e. NGC 3256 and IRAS 08355-4944,in the European Southern Observatory (ESO) Science Verifica-tion (SV) run of HAWK-I with the GRound Layer Adaptive op-tics Assisted by Lasers module (GRAAL; Paufique et al. 2010).The Tip-Tilt Star - free mode SV observations of NGC 3256were carried out on 2018 January 3.4 UT (FWHM ∼ ′′ .
4) and2018 January 6.4 UT (FWHM ∼ ′′ . m .
17 mag) in the field.The HAWK-I / GRAAL data were reduced in a standard man-ner for near-IR images, using iraf based tasks. We discov-ered a new transient source (SN 2018ec) in NGC 3256 by us-ing an archival ESO New Technology Telescope (NTT) Sonof ISAAC (SOFI; Moorwood et al. 1998) Ks -band image from2003 January 23.2 UT as a reference. We reported the discoveryin Kankare et al. (2018a), and spectroscopically classified it asa reddened Type Ic (Berton et al. 2018) via the extended Pub-lic ESO Spectroscopic Survey for Transient Objects (ePESSTO;Smartt et al. 2015). The discovery image is shown in Fig. 1. Toour knowledge, no optical large-scale sky survey has reported adetection of SN 2018ec, however, this might be in part due to theless-monitored southern declination of NGC 3256.Astrometry of the HAWK-I / GRAAL image was derived us-ing 17 stars selected from the Two Micron All-Sky Survey(2MASS), yielding RA = h m s .
77 and Dec = − ◦ ′ ′′ . ′′ .
2W and 7 ′′ . Ks -band nucleus of NGC 3256, andcorresponds to a projected distance of 1.7 kpc. Typical forLIRGs, NGC 3256 hosts a large population of super star clus-ters (see e.g. Trancho et al. 2007), and such structures can verylikely contribute to the underlying emission seen at the loca-tion of SN 2018ec and other CCSNe in NGC 3256 in the pre-explosion reference images. Spectrophotometric follow-up dataof SN 2018ec were obtained with NTT as a part of ePESSTO us-ing the ESO Faint Object Spectrograph and Camera 2 (EFOSC2;Buzzoni et al. 1984) and SOFI. The data were reduced in a stan-dard manner using the pessto pipeline (Smartt et al. 2015) basedon standard iraf tasks.All images were template subtracted using the isis H and Ks -band reference images from FLAMINGOS-2 at Gemini Southobserved on 2017 March 26.3 and 2017 March 12.1 UT, respec-tively, while the J -band reference image was taken with SOFIat NTT on 2001 April 9.1 UT. The g , r , i , z -band archival ref-erence images were observed with Dark Energy Camera (DE-Cam; Flaugher et al. 2015) at the 4-m Blanco Telescope on 2017February 20.3, 2017 February 21.3, 2017 March 18.2, and 2017February 9.3 UT, respectively. The JHKs images were calibratedusing 2MASS magnitudes of stars in the field of SN 2018ec. The gri photometry was calibrated using the AAVSO (American As-sociation of Variable Star Observers) Photometric All-Sky Sur-vey magnitudes for stars in the large field of DECam imageswhich were then used to yield magnitudes for 15 sequence starsclose to SN 2018ec; these are shown in Fig. A.1 and the mag-nitudes reported in Table A.1. The z -band sequence stars werecalibrated using standard star field observations carried out withNTT. The point spread function (PSF) photometry of the SN wascarried out using the quba pipeline (Valenti et al. 2011). The pho-tometry is reported in Table A.2 with the griz magnitudes in theAB system and JHK magnitudes in the Vega system.Ryder et al. (2018) reported radio observations of the field ofSN 2018ec with the Australia Telescope Compact Array (ATCA)on 2018 January 23.8 UT. The observations yielded 3 σ upperlimits at the location of SN 2018ec of <
10 mJy / beam and < / beam at 5.5 and 9.0 GHz, respectively. This corresponds to < . × erg s − Hz − at 9 GHz; the limit is above the peak iraf is distributed by the National Optical Astronomy Observatories,which are operated by the Association of Universities for Research inAstronomy, Inc., under cooperative agreement with the National Sci-ence Foundation.Article number, page 2 of 25. Kankare et al.: CCSNe in LIRGs Fig. 1. a) 1 ′ × ′ subsection of the HAWK-I / GRAAL Ks -band discovery image of SN 2018ec in NGC 3256, b) SOFI reference image, and c) asubtraction between the images. The AO enhanced HAWK-I / GRAAL image with FWHM ∼ ′′ . ∼ ′′ .
8. The location of SN 2018ec is shown with tick marks in all the panels; the orientationand image scale are indicated in the first panel. of normal Type Ic SNe around 10 to 10 erg s − Hz − (e.g.Romero-Cañizales et al. 2014, and references therein). The lim-its are not particularly constraining, due to the high backgroundradio emission of the host galaxy. Further radio limits were re-ported by Nayana & Chandra (2018) based on observations withthe Giant Metrewave Radio Telescope (GMRT) at 1.39 GHz on2018 January 20.9 UT, yielding a 3 σ upper limit of 2.1 mJy( < . × erg s − Hz − ) at the SN 2018ec location.SN 2018ec is found to be spectroscopically a normal TypeIc SN, and in our analysis we find similarity to e.g. SN 2007gr(Hunter et al. 2009), see below. The line-of-sight host galaxy ex-tinction of SN 2018ec was estimated using a χ fit of broad-bandlight curves of SN 2018ec with those of SN 2007gr (includ-ing an extrapolation of the optical late-time light curves of SN2007gr based on the data beyond +
70 d using linear fits). Thefit was carried out simultaneously in all the bands with follow-up data of SN 2018ec. The method is the same as that used e.g.in Kankare et al. (2014a). The free parameters of the fit are thehost galaxy line-of-sight extinction A V , the discovery epoch t relative to a suitable reference (the estimated explosion date orlight-curve maximum), and fixed constant shift C applied to allthe bands representing the intrinsic di ff erences in the brightnessof SNe (and any systematic di ff erence in the distance estimatesof the two SNe). The Johnson-Cousins UBVRI light curves ofSN 2007gr (Hunter et al. 2009) were converted into the griz sys-tem with the transformations of Jester et al. (2005). We adoptedthe well-established Cardelli et al. (1989) extinction law for thefitting. The errors of the data points in the analysed light curvesare considered to be Gaussian. If the light curves are well sam-pled and the comparison SN is well suited for the comparison,the probability density functions of the fitted parameters fol-low approximately Gaussian distributions. The largest deviationsfrom this typically occur within the error of t if the light-curvefollow up was initiated post-maximum. The reported errors cor-responds to 68.3 % confidence intervals estimated based on theprobability density functions; systematic errors related e.g. to theuncertainty of the host extinction of the comparison SN are notincluded in the reported values. Based on the aforementionedcomparison with SN 2007gr we conclude that SN 2018ec wasdiscovered 19 + − days after optical maximum, has a host galaxyextinction of A V = . + . − . mag, and is C = . + . − . mag brighterthan SN 2007gr. The absolute magnitude light curves are shown Fig. 2.
Absolute magnitude light curves of SN 2018ec after correctingfor host extinction ( A V = . − . B -band maximum estimated for SN 2007gr by Hunter et al. (2009). in Fig. 2. Based on the fit we estimate that SN 2018ec peakedat M r ≈ −
18 mag; this is at the brighter end of the peak mag-nitude distribution of normal Type Ic SNe but not unusual (e.g.Taddia et al. 2018).The spectroscopic sequence of SN 2018ec is shown in Fig. 3,illustrating also the similarity to the normal Type Ic SN 2007gr(Hunter et al. 2009). Following a more detailed classificationscheme by Prentice & Mazzali (2017), SN 2018ec appears tobe a Ic-6 /
7. The most prominent SN feature is the Ca ii near-IRtriplet. The typically strong O i λ / c SNe isblended with the telluric A-band feature. No clear He i featuresarising from the SN are evident, supporting a Type Ic classifi-cation. Actually there are broad P Cygni profiles close to therest wavelengths of He i λ λ i D and C i λλ Article number, page 3 of 25 & Aproofs: manuscript no. aa respectively. These lines have an absorption minimum at ∼ − around +
33 d, which declines to ∼ − within ∼ ff erences compared to SN 2007gr,SN 2018ec does not show early C i λλ ii λ +
32 d. Furthermore, theMg i λ +
62 d spec-trum of SN 2018ec.
During the ePESSTO follow up of SN 2018ec the EFOSC2 dataled to a serendipitous discovery of another transient AT 2018cuxin NGC 3256 using images obtained on 2018 March 24.2 UTin comparison to images from 2018 January 17.2 UT as a refer-ence. The discovery was reported in Kankare et al. (2018b) andthe i -band discovery image is shown in Fig. 5. We yielded co-ordinates RA = h m s .
41 and Dec = − ◦ ′ ′′ . pessto pipeline. This corresponds to 1.7" E and 4.0" Sof the host galaxy main Ks -band nucleus. This translates to aprojected distance of 0.8 kpc. The location of AT 2018cux is rel-atively close, but not coincident, to the southern nucleus of NGC3256, located at RA = h m s .
22 and Dec = − ◦ ′ ′′ . ff et al. 2003).However, this southern nucleus is heavily obscured at opticaland near-IR wavelengths by dust and thus the association of AT2018cux observed in optical wavelengths to this component isuncertain. The PSF photometry of AT 2018cux was carried outsimilar to that of SN 2018ec and is listed in Table A.4. Late-time long-slit spectroscopy of AT 2018cux was obtained on 2018July 3.7 UT with the Southern African Large Telescope (SALT;Buckley et al. 2006) using the Robert Stobie Spectrograph (RSS;Burgh et al. 2003; Kobulnicky et al. 2003). The spectrum was re-duced in a standard manner with basic iraf tasks.We used a similar approach as previously described for SN2018ec to estimate the host galaxy extinction for AT 2018cux.The transient shows flat and plateau-like light curves, withcolours that are only somewhat reddened in combination withrelatively faint magnitudes, which suggest a subluminous TypeIIP SN (e.g. Spiro et al. 2014; Müller-Bravo et al. 2020). Thisis also supported by our one low signal-to-noise spectrumof the event, see the paragraph below. Therefore, SN 2005cs(Pastorello et al. 2009) was adopted as a canonical reference ex-ample of a normal subluminous Type IIP SN, with the opticallight curves transferred into the griz system with the Jester et al.(2005) conversions. Based on the comparison fit, AT 2018cuxwas found to be most consistent with a host galaxy extinctionof A V = . ± . + − d after the explosion,and a 0 . + . − . mag fainter plateau, see Fig. 6. With the estimatedline-of-sight extinction, at around +
50 d from the explosion, theplateau magnitudes reach M ≈ − . riz bands. How-ever, the faintest subluminous Type IIP events like SNe 1999brand 2001dc have plateau magnitudes of M V ≈ − . − . + + − d. In Fig. 7 the SALT spectrum is shown cor-rected for extinction, overlaid with an arbitrarily shifted +
106 dspectrum of SN 2005cs at the end of the plateau phase, consis-tent with a subluminous Type IIP SN classification. In particular,quite typical features for sub-luminous Type IIP SNe are the fluxattenuation below ∼ − ii and Ba ii lines. In addition to SN 2001db, SN 2018ec, and AT 2018cux inNGC 3256, an SN candidate PSN J10275082-4354034 (here-after, shortly referred to as PSN102750) has been reported in 2014 in the same LIRG at RA = h m s .
82 and Dec = − ◦ ′ ′′ .
4, discovered by Peter Aldous at Geraldine Obser-vatory . Based on the coordinates the projected distance of thetransient from the Ks -band nucleus is 2.1 kpc. An unfiltered dis-covery magnitude on 2014 May 7.45 UT of 15.6 mag was re-ported. Unfortunately, no spectroscopic classification of the tran-sient was carried out by anyone to our knowledge.Follow-up imaging of PSN102750 was carried out by S.Parker. This included one epoch of luminance filter observationsusing the 50-cm T30 telescope with FLI-PL6303E CCD cameraat the Siding Springs Observatory, and two epochs of unfilteredobservations with a 35-cm Celestron C14 reflector and SBIG ST-10 CCD camera at the Parkdale Observatory. The data reductionincluded basic bias and dark subtraction steps and flat fielding.The quba pipeline was used to carry out the PSF photometry ofthe SN candidate by calibrating the images directly into R -band,reported in Table A.5.Furthermore, we recovered PSN102750 in Hubble SpaceTelescope (HST) archival images obtained with the Wide FieldCamera 3 (WFC3). NGC 3256 was observed in the
F467M (Strömgren b ) and F621M filters on 2014 June 10 and 2014November 13, respectively . Fig. 8 clearly shows the late-timedetection of PSN102750 in comparison to an archival imageobtained with a similar filter. Photometry on the images withthe transient was carried out using dolphot , an HST dedicatedphotometry package. The individual charge transfer e ffi ciency(CTE) corrected images were masked for bad pixels and the skybackground was fitted and subtracted, before being aligned toproduce the drizzle-combined image. PSFs were then fit to allthe identified sources present in the images, yielding their mag-nitude values. The magnitudes of the SN candidate in F467M and
F621M filters were adopted as those of B and R , respec-tively.The resulting light curve of PSN102750 was template fit-ted with the same method that was used for SN 2018ec andAT 2018cux, however, a selection of di ff erent CCSN subtypeswas used as templates to yield a tentative classification and hostgalaxy extinction for the transient. The comparison events in-clude Type IIn SNe 1998S (Fassia et al. 2000; Liu et al. 2000)and 2005ip (Stritzinger et al. 2012), a normal Type IIP SN2004et (Sahu et al. 2006), and a normal Type Ic SN 2007gr(Hunter et al. 2009). Furthermore, a comparison to the normalType Ia SN 2011fe (Munari et al. 2013) was also carried out. Reported at the Central Bureau for Astronomical Telegrams Tran-sient Objects Confirmation Page: http: // / unconf / followups / J10275082-4354034.html https: // geraldineobservatory.co.nz / https: // / t30 / Programme 13333, PI: Rich. http: // americano.dolphinsim.com / dolphot / Article number, page 4 of 25. Kankare et al.: CCSNe in LIRGs
Fig. 3.
Spectral time series of SN 2018ec. The spectra have been redshift corrected to rest frame. The spectra have been corrected for both Galactic A V = .
334 mag and estimated host galaxy extinction of A V = . ⊕ symbol. For comparison selected spectra of normal Type Ic SN 2007gr are overlaid (green). The continua of the opticalspectra of SN 2018ec are likely to be contaminated by the complex host background that was not successfully completely subtracted. Therefore,the optical SN features of SN 2018ec above and below the continuum level appear also less prominent compared to those of SN 2007gr. Thespectra have been shifted vertically for clarity. The fits are shown in Fig. 9. PSN102750 is most consistent witha Type IIn event that generally can show major diversity in theirlate-time evolution as shown by the comparisons. Our best fitis with SN 1998S, with PSN102750 discovered shortly beforethe peak magnitude. However, a Type IIP SN cannot be fully ex-cluded either, though the early photometry of PSN102750 showsdeviations from a flat plateau. H-poor stripped-envelope eventsare excluded based on the blue colours of PSN102750 even if anegligible host extinction is assumed; increasing the extinctionwould only make the discrepancy larger. A Type Ia SN classi-fication can be excluded primarily based on the bright late-timedetection of PSN102750. Based on the light curve fit with SN1998S as a template, we conclude that PSN102750 has a hostgalaxy extinction of A V = . + . − . mag, is 1 . + . − . mag fainter than SN 1998S, and discovered at − + − days relative to the light curvepeak of SN 1998S assuming the extinction law of Cardelli et al.(1989). For comparison, the Type IIP fit using SN 2004et as atemplate yields A V = . + . − . mag, a very small brightness dif-ference of 0 . + . − . mag, and t = + − days relative to the esti-mated explosion date. SN 2004et is at the bright end of the in-trinsic magnitude distribution of normal Type IIP SNe at plateau(Anderson et al. 2014).
3. Arp 299
Arp 299 is a nearby LIRG at a distance of 44.8 Mpc (Huo et al.2004). The IR luminosity of the galaxy, L IR = . L ⊙ (Sanders et al. 2003), suggests a rate of ∼ − based on the empirical relation of Mattila & Meikle (2001). Article number, page 5 of 25 & Aproofs: manuscript no. aa
Fig. 4.
Prominent P Cygni features of SN 2018ec at two selected epochs.The zero velocity is set to the rest wavelength of the shortest wavelengthcomponent of each line blend, i.e. at 5890 Å for the Na i D (blue), 8498Å for the Ca ii near-IR triplet (orange), and 10683 Å for a C i blend(red). Velocities at absorption minima shown by the features are sur-prisingly similar with ∼ − around ∼ ∼ − at ∼ The Galactic extinction towards Arp 299 is A V = .
046 mag(Schlafly & Finkbeiner 2011). The recent SNe 2019lqo and2020fkb presented here increase the total number of spectro-scopically classified CCSNe in Arp 299 to eight events, in ad-dition to one unclassified near-IR discovered SN 1992bu (seee.g. Mattila et al. 2012).
SN 2019lqo was discovered on 2019 July 21 07:33:36 UT (JD = Gaia spacecraft, and reported on behalf of the science alerts teamas Gaia19dcu (Hodgkin et al. 2019).The Gaia G -band AB dis-covery magnitude of SN 2019lqo was 18.33 ± m G > . = Gaia are RA = h m s .
460 andDec = + ◦ ′ ′′ .
82 (equinox J2000.0), pointing to compo-nent ‘A’ as the likely host (Fig. 10) of Arp 299. This yieldsa projected distance of 9 ′′ . ′′ . quba pipeline. The NOT near-IR Camera andspectrograph (NOTCam) imaging was reduced by making useof the external notcam package for iraf . The quba pipeline PSFphotometry of SN 2019lqo was calibrated with the sequence starmagnitudes obtained from Kankare et al. (2014b). The resultingphotometry is listed in Table A.6.The first Zwicky Transient Facility (ZTF; Bellm et al.2019) detections of SN 2019lqo (with an internal nameZTF19abgbbzy) are reported on the Transient Name Server; ad-ditional ZTF limits and detections are also available e.g., via thepublic MARS broker . Intriguingly, the first reported ZTF de-tection of m r = .
86 mag was obtained 24.7 hrs before thereported
Gaia non-detection of > Gaia sky scanning angle made the SN non-detectable, and re-sulted in the reported non-detection with a nominal limit. Fur-thermore, ZTF reports an r -band non-detection of > Gaia dis-covery epoch. However, the magnitude limits reported by ZTFare di ff erence image estimates over the whole CCD quadrant(Masci et al. 2019). The location of SN 2019lqo is quite crowdedwith a luminous galaxy background making image subtractionchallenging and sky condition dependent. Therefore, it is notsurprising if a limit yielded globally for the field is overly op-timistic for the location of SN 2019lqo if the subtraction has notbeen optimal. We proceeded to download the science data prod-uct files (Masci et al. 2019) from the ZTF data release 3 (DR3) covering the follow up of SN 2019lqo and corresponding tem-plate reference images. We carried out image subtractions usingthe isis > σ detection. This includes our measurements of m r = . ± . . ± .
12 mag for the epochfollowing the first detection for which a non-detection was pre-viously reported.Similar to the SNe in NGC 3256, the line-of-sight extinc-tion of SN 2019lqo was estimated with a simultaneous χ com-parison of UBVRIJHK light curves to those of well-sampledType IIb SNe 2011dh (Arcavi et al. 2011; Ergon et al. 2014,2015) and 1993J (Pressberger et al. 1993; Ripero et al. 1993;Richmond et al. 1994, 1996). The fitting was carried out withthe Cardelli et al. (1989) extinction law. The resulting absolutemagnitude light curves are shown in Fig. 11, including photom-etry based on publicly available data. The early public gGr -banddetections of SN 2019lqo suggest that the SN had a relativelylong rise time and was discovered possibly during a post-shockcooling phase, more similar to that of SN 1993J than the morerapidly evolving SN 2011dh, but this is fairly poorly constrained.The fit with SN 1993J as a template is superior compared to thatof SN 2011dh as a reference; this fit suggests that SN 2019lqohas a host galaxy extinction of A V = . + . − . mag, is 0 . + . − . mag brighter than SN 1993J, and peaked in R -band around JD = ± http: // / instruments / notcam / guide / observe.html https: // mars.lco.global / / https: // / page / dr3Article number, page 6 of 25. Kankare et al.: CCSNe in LIRGs Fig. 5. a) 1 ′ × ′ subsection of the EFOSC2 i -band discovery image (FWHM ∼ ′′ .
9) of AT 2018cux in NGC 3256, b) pre-discovery EFOSC2reference image (FWHM ∼ ′′ . Fig. 6.
Absolute magnitude light curves of AT 2018cux including anestimated host galaxy extinction of A V = . + of E ( B − V ) = . i and Ca ii near-IR triplet lines compared toSN 1993J (Fig. 12). Therefore, it seems that SN 2019lqo bridgesthe observational characteristics of these two canonical Type IIbSNe. SN 2020fkb in Arp 299 was discovered by the ZTF sur-vey, reported by Pignata et al. (2020), with an internal nameZTF18aarlpzd. The transient was first detected on 2020 March
Fig. 7.
SALT spectrum (black) at the location of AT 2018cux correctedfor host galaxy extinction of A V = . + ⊕ sym-bol.
28 06:19:45 UT at m g = . ± .
08 mag with a reported non-detection on 2020 March 7 09:49:20 UT at m r = .
34 mag.The SN was classified by Tomasella et al. (2020) on 2020 April2.8 UT as a young Type Ib, roughly a week before maximum,using the 1.82 m Copernico Telescope with the Asiago FaintObject Spectrograph and Camera (AFOSC). We obtained fur-ther optical spectrophotometric follow up of SN 2020fkb usingAFOSC, and the NOT with ALFOSC; optical imaging with theAsiago 67 /
92 cm Schmidt telescope with the KAF-16803 CCD;optical and near-IR imaging with the Liverpool Telescope (LT;Steele et al. 2004) using the IO:O and IO:I (Barnsley et al. 2016)instruments; and near-IR imaging using the NOT with NOTCam.
Article number, page 7 of 25 & Aproofs: manuscript no. aa
Fig. 8. a) Late-time HST
F621M image of PSN102750 observed 190 d after the discovery of the transient, b) pre-explosion HST
F625W image ofthe field of the transient, and c) a subtraction between the images. In addition to the event, the subtraction results also in some faint residuals fromsources in the field likely due to the somewhat di ff erent filter widths of the two epochs of observations. The transient location is shown with tickmarks. The orientation and image scale are indicated in the left panel. The standard reduction of the Asiago observatory data wascarried out using the foscgui pipeline , and basic instrumentalpipeline reduction products of the LT data were obtained for theanalysis. A selection of pre-explosion images were used as im-age subtraction templates from the NOT, the Asiago telescope,and the Pan-STARRS1 (Chambers et al. 2016) data release 2archive . The resulting PSF photometry of SN 2020fkb is listedin Tables A.8 and A.9.The host galaxy extinction of SN 2020fkb was estimated us-ing light curves of a normal Type Ib SN 2004gq (Bianco et al.2014; Stritzinger et al. 2018a) with an excellent multiband cov-erage and a low host galaxy extinction estimate of A V = . = ± A V = . + . − . mag, and is 0 . + . − . mag fainter than SN 2004gq; the best match is shown in Fig. 13.For example, in r -band SN 2020fkb peaked at M r ≈ − . r -band distribution of theseSNe around −
17 to −
18 mag (e.g. Taddia et al. 2018). The afore-mentioned pre-explosion non-detection limit, at an epoch corre-sponding to −
33 d from maximum light, is not strongly con-straining the explosion epoch of SN 2020fkb, as normal Type IbSNe have typical r -band rise times of ∼
21 d (Taddia et al. 2015)with a distribution around a few days.The spectral time series of SN 2020fkb (Table A.10) isshown in Fig. 14, compared to a selection of SN 2004gq spectra.The evolution of SN 2020fkb is quite normal for a Type Ib SN.The spectra show broad and evolving P Cygni profiles of He i features, in particular the λλ ii H&K doublet, andbroad features arising likely from Fe ii blends. The He i λ − ∼ − ; this is consistent with typical velocities of this feature atthe corresponding phase of normal Type Ib SNe (Taddia et al.2018), whereas the photometrically similar SN 2004gq showsin fact overall larger velocities. The wavelength coverage ofthe +
20 d spectrum onwards extends further redwards and the https: // sngroup.oapd.inaf.it / foscgui.html https: // panstarrs.stsci.edu / Ca ii near-IR triplet is prominently visible. The +
72 d spectrumis not completely nebular, but some nebular features have ap-peared; the doublets [O i ] λλ ii ] λλ i ] / [Ca ii ] flux ratio of ∼ i ] λ i ] λ
4. Starburst age in high CCSN rate LIRGs
The numerous CCSN subtypes are expected to originate fromdi ff erent populations of massive stars, that have di ff erences e.g.in their life times. Motivated by this, we aimed to model the basicstarburst parameters in all LIRGs that have hosted nuclear CC-SNe to investigate, whether there is a the trend between CCSNsubtypes and starburst age, t SB . Our SN sample comprises theclassified CCSNe in LIRGs, at small projected distances fromthe host nucleus, listed in Kool et al. (2018) and Kool (2019), ex-panded by the new events presented in this manuscript. The sam-ple events are discovered either at optical or IR wavelengths (i.e.,we do not consider in our sample SN candidates detected only inradio). In addition to the new CCSNe in NGC 3256 and Arp 299,we also included in our analysis the recent Type II SN 2020cuj inNGC 1614 that has a limited data set, see Appendix A.1. As thestar formation in LIRGs is heavily concentrated in the nuclearregions ranging in size from ∼
100 to ∼ >
50 %. For example, 2 / ∼ ≤ ≤ D l ≤ / Ib / Ic, and 1 Ibn). We mod-elled the SEDs of these sample LIRGs to study the distribution ofthe CCSN subtypes and the host starburst age in these galaxies.
Article number, page 8 of 25. Kankare et al.: CCSNe in LIRGs
Fig. 9.
PSN102750 light curve comparisons to those of a) Type IIn SN 1998S, b) Type IIn SN 2005ip, c) Type IIP SN 2004et, d) Type Ic SN2007gr, and e) Type Ia SN 2011fe. The reported unfiltered discovery magnitude is also shown in the plot with a black symbol.
We note that we were not able to model the nearby and extendedIC 2163 / NGC 2207 system (host of SPIRITS 14buu and SPIR-ITS 15c; Jencson et al. 2017) due to the vastly di ff ering spatial coverage across the range of wavelengths we considered; thusthis LIRG is not part of our sample. Furthermore, we did not in-clude Type II SN 2004gh (Folatelli et al. 2004) in our analysis Article number, page 9 of 25 & Aproofs: manuscript no. aa
Fig. 10. a) 1 ′ × ′ subsection of a NOT V -band follow-up image of SN 2019lqo in Arp 299, b) follow-up image of SN 2020fkb, and c) a subtractionbetween the images. Tick marks indicate the locations of SNe 2019lqo and 2020fkb. The image scale and orientation are indicated in the left panel.The marked locations of IR bright main components (A, B, C, C ′ ) of Arp 299 (Gehrz et al. 1983) illustrate that some of these regions are obscuredin optical wavelengths. Fig. 11.
SN 2019lqo light curve fits to Type IIb SNe a) 2011dh and b) 1993J. The inset zoom-in panels show the pre-maximum light curvessuggesting a relatively long shock cooling phase. As previously noted, the
Gaia G -band upper limit is probably optimistic. The epoch 0 is set tothe estimated R -band peak. as the SED of its host galaxy MCG -04-25-06 has a very limitedwavelength coverage available, which would not enable robustmodelling.It is possible that due to chance alignment some of the CC-SNe with small projected distances are in fact located at muchlarger distances from the host nucleus. While this cannot be ac-curately constrained, the host galaxy extinction provides a hintof the true location of the CCSNe in LIRGs; CCSNe that aremore obscured by host galaxy extinction are also more likely tobe embedded in the dusty central regions of their hosts. This is astrong motivation to estimate host galaxy extinctions for CCSNein LIRGs, as we have done for the new events presented in thispaper. The sample CCSNe are listed in Table 1 with the availablereported host galaxy extinctions.We used a grid of radiative transfer models for a starburst(Efstathiou et al. 2000; Efstathiou & Siebenmorgen 2009), AGN(Efstathiou & Rowan-Robinson 1995; Efstathiou et al. 2013),and a spheroidal galaxy (Efstathiou et al., 2020, submitted) or a disc galaxy (Efstathiou & Siebenmorgen 2020, in prep.) tofit the SEDs using the SED Analysis Through Markov Chains(SATMC) Monte Carlo code (Johnson et al. 2013). The hostgalaxy model resulting for the best fit is indicated in Table 1.The starburst and host galaxy models incorporate the stellar pop-ulation synthesis model of Bruzual & Charlot (1993, 2003) andassume a solar metallicity and a Salpeter initial mass function(IMF). Alonso-Herrero et al. (2006) studied a local sample ofLIRGs and found them to have approximately solar metallicity.While adopting a di ff erent IMF can have some e ff ect on the de-rived parameters (see discussion in Herrero-Illana et al. 2017),we adopt the classical Salpeter IMF, consistently with previousstudies. The fitting predicts the starburst SED at di ff erent ageswith the assumption that the star formation rate declines expo-nentially. The spheroidal galaxy model used here is an evolu-tion of the cirrus model of Efstathiou & Rowan-Robinson (2003)and is similar to that of Silva et al. (1998), incorporated in theGRAphite and SILicate (GRASIL) code. The model assumes Article number, page 10 of 25. Kankare et al.: CCSNe in LIRGs
Fig. 12.
The spectra of SN 2019lqo compared to those of Type IIb SNe2011dh (Ergon et al. 2014) and 1993J (Matheson et al. 2000). The mostprominent SN lines are indicated based on Ergon et al. (2014). Thespectra have been extinction and redshift corrected, and shifted verti-cally for clarity. The main telluric band wavelengths for SN 2019lqoare indicated with a ⊕ symbol. Fig. 13.
SN 2020fkb absolute magnitude light curve (points) with anestimated host galaxy extinction of A V = . + .
13 mag. The epoch 0 is set to the estimated V -band maximum. that stars, dust and molecular clouds in which young stars areembedded are mixed in a spherical cloud with a Sersic profilewith index n =
4. The method for computing the disc modelis similar to that used for the spheroidal models, apart from thedi ff erence in the geometry. The SATMC fitting includes 13 and14 free parameters for the spherical and the disc models, respec-tively. The degrees of freedom (DOF) for the best fit are indi-cated in Table 1. The SATMC derives errors for the fitting pa-rameters, which Johnson et al. states to be the 68 % containedranges from the one-dimensional confidence levels, marginalisedover the other fitting parameters.For the usage of the SED fitting, we collated the opti-cal to far-IR photometric data of the sample LIRGs via the NASA / IPAC Extragalactic Database (NED) mainly from theGALEX ( Galaxy Evolution Explorer ), SDSS, 2MASS, IRAS(the
Infrared Astronomical Satellite ), and ISO (the
InfraredSpace Observatory ). Furthermore, we also used photomet-ric data obtained with the
Herschel Space Observatory fromChu et al. (2017).For three LIRGs (IC 883, IRAS 17138-1017, and IRAS18293-3413) the
Spitzer spectra used by Herrero-Illana et al.(2017) for their modelling were re-utilised for the re-analysishere. For five additional LIRGs in our sample (ESO 138-G27,NGC 1614, NGC 2388, NGC 317B, and NGC 838), low-resolution ( R ≈ − − µ m) and long-low (LL; 14 − µ m)modules of the Infrared Spectrograph (IRS; Houck et al. 2004)on board the Spitzer Space Telescope . For observations that werecarried out in mapping mode, we only selected those frameswhere the spectrograph slit included the nucleus of the galaxy.The data were processed using standard spectroscopic tech-niques. We began by subtracting one nod position from the otherto remove the sky background. All subsequent steps (extraction,wavelength calibration, and flux calibration) were carried out us-ing the optimal extraction mode of the Spitzer IRS Custom Ex-tractor (SPICE) tool (v2.5.1). The absolute flux calibration waschecked against the photometric data. In the case of nearby ( < ( λ rest /µ m) = . µ m silicate features. For each sample LIRG three sets ofMonte Carlo fits were carried out both for the spheroidal anddisc galaxy model cases, and the individual fit with the bestreduced χ value was adopted to yield the starburst parame-ters for the system. Our global estimates of the CCSN rate andstarburst properties of the sample galaxies are reported in Ta-ble 1 and an example SED fit of IRAS 18293-3413 is shown inFig. 15. The best SED fits for all the other sample galaxies areshown in Appendix Figs. A.3 and A.4. We note that the LIRGsample overlaps partly with that of Herrero-Illana et al. (2017),with some di ff erence in the yielded starburst values with sim-ilar simulations. The key di ff erence to those are the more ex-tended parameter ranges allowed in our simulations for the star-burst age (5 to 50 Myr) and the e-folding time of the starburst(1 to 40 Myr). While preparing this study we noticed that thestarburst age range used in the simulations of Herrero-Illana etal. had an upper limit of 29.5 Myr, which resulted in many oftheir older starburst age estimates to artificially cluster near thisvalue. However, the starburst age was not the focus of that studyand does not change their conclusions. Similarly any di ff erencesin the derived parameters previously reported by Mattila et al.(2012) and Mattila et al. (2018) result from the usage of di ff er-ent data sets for their SED fitting covering separately individualcomponents of Arp 299 with a more limited wavelength rangerather than fitting the SED of the whole system. Thus, the resultsfor the starburst age are not directly comparable.Fig. 16 shows our result with the host LIRG starburst agecomparison to the projected distance of the CCSN, with the dif-ferent CCSN subtypes highlighted. Due to the still relativelysmall number of discovered CCSNe in LIRGs, we combine TypeIIb, Ib and Ic SNe into a single group of H-poor IIb / Ib / Ic events.We see that the H-rich CCSNe around the central regions of these http: // ned.ipac.caltech.edu / Article number, page 11 of 25 & Aproofs: manuscript no. aa
Fig. 14.
Spectral time series of SN 2020fkb redshift corrected to rest frame. The spectra have been corrected for both Galactic and estimated hostgalaxy extinctions, and vertically shifted and normalised for clarity. The epochs are provided respective to the estimated light curve maximum.The most prominent spectral features are labelled arising either from the host galaxy (blue) or from the SN (red). The Doppler shifted positions ofthe He i and Fe ii lines are indicated with cyan vertical lines in early epochs as suggested by the velocity of the He i λ ⊕ symbol. The spectraof SN 2020fkb likely contain some host continuum contamination at the blue end, in particular in the late epochs. Selected spectra of normal TypeIb SN 2004gq (Modjaz et al. 2014) are shown for comparison (green) which shows very similar spectrophotometric evolution, but somewhat largerline velocities. galaxies are produced in LIRGs with relatively older starburstages ( ≥
30 Myr), while the H-poor CCSNe are produced pri-marily in younger starburst age regions. This is consistent withcanonical stellar evolution models. In younger starbursts onlythe most massive stars have had time to evolve to the SN phase,and explode as H-poor CCSNe; in the older starbursts the mostmassive stars have already exploded and the lower mass starshave had more time to evolve to the SN stage, and end their lifecycles as H-rich CCSNe (e.g. Heger et al. 2003). However, ro-tation, metallicity, and binarity (e.g. Podsiadlowski et al. 1992;Woosley 2019) all have an influence on this, and can reduce therelative initial progenitor star mass and life time di ff erences be-tween di ff erent CCSN subtypes.We carried out a two-sample Anderson-Darling (AD) sta-tistical test for the CCSN subtype distribution. The p -value forthe two basic CCSN subtypes of H-poor Type IIb / Ib / Ic / Ibn (14 SNe) and H-rich Type II / IIn (15 SNe) in these galaxies hav-ing the same underlying distribution is only 0.0027, and thusthe discussed trend is statistically significant at the 3.0 σ level.We also considered the case of only the LIRGs with the highestyielded SN rates of ≥ − . Then the p -value of the twobasic CCSN subtypes having the same underlying distributionis reduced to 0.0013 (3.2 σ ). We chose the AD test over otherempirical distribution statistics-based tests (e.g., a Kolmogorov-Smirnov test) because of its generally powerful ability to dis-tinguish between distributions that have the largest di ff erencesnear the minima and maxima of their cumulative distribution(Stephens 1974). As an additional AD test, we also comparedour SN samples to a ‘flat’ larger simulated comparison sampleof a su ffi ciently large number (10) of SNe distributed uniformlyin each of the corresponding sample galaxies. The resulting p -value for the Type IIb / Ib / Ic / Ibn SNe being uniformly distributed
Article number, page 12 of 25. Kankare et al.: CCSNe in LIRGs
Table 1.
Confirmed and likely CCSNe at the central regions ( d proj ≤ . Host D l log( L IR ) t SB SNR SB SFR L AGN
SED DOF CCSN Type d proj A host V Disc. Ref.(Mpc) ( L ⊙ ) (Myr) (SN yr − ) ( M ⊙ yr − ) (%) host (kpc) (mag)IRAS 18293-3413 84.1 11.89 40 + − . + . − . + − + − S 22 AT 2012iz IIP 0.6 1.8 IR (1)IRAS 18293-3413 . . . . . . . . . . . . . . . . . . . . . . . . SN 2013if IIP 0.2 0 IR (2)IC 883 107.1 11.73 38 + − . + . − . + − + − D 27 SN 2010cu IIP 0.2 0 IR (3)IC 883 . . . . . . . . . . . . . . . . . . . . . . . . SN 2011hi IIP 0.4 6 IR (3)NGC 5331 150.0 11.66 35 + − . + . − . + − + − D 5 AT 2017chi IIn 1.5 12 IR (1)Arp 299 44.8 11.82 16 + − . + . − . + − + − . + . − . + − + − S 33 SN 1996D Ic 2.1 ? Opt (2)NGC 1614 . . . . . . . . . . . . . . . . . . . . . . . . SN 2020cuj II 2.5 2.8 Opt (5)NGC 838 53.3 11.05 25 + − . + . − . + − + − S 7 SN 2005H II 0.4 ? Opt (2)IRAS 17138-1017 82.2 11.49 28 + − . + . − . + − + − S 22 SN 2008cs IIn 1.5 16 IR (7)IRAS 17138-1017 . . . . . . . . . . . . . . . . . . . . . . . . SN 2015cb IIP 0.6 4.6 IR (2)NGC 2388 61.1 11.28 25 + − . + . − . + − + − D 8 SN 2015U Ibn 1.8 3.1 Opt (8)NGC 317B 77.0 11.19 37 + − . + . − . + − + − S 30 SN 1999gl II 1.9 ? Opt (2)NGC 317B . . . . . . . . . . . . . . . . . . . . . . . . SN 2014dj Ic 1.5 ? Opt (2)NGC 3256 37.4 11.61 43 + − . + . − . + − + − S 16 SN 2001db II 2.1 5.5 IR (6)NGC 3256 . . . . . . . . . . . . . . . . . . . . . . . . PSN102750 IIn 2.1 0.3 Opt (6)NGC 3256 . . . . . . . . . . . . . . . . . . . . . . . . SN 2018ec Ic 1.7 2.1 IR (6)NGC 3256 . . . . . . . . . . . . . . . . . . . . . . . . AT 2018cux IIP 0.8 2.1 Opt (6)ESO 138-G27 96.1 11.41 31 + − . + . − . + − + − S 27 SN 2009ap Ic 1.2 ? Opt (2)NGC 6907 49.2 11.11 39 + − . + . − . + − + − S 2 SN 2008fq II 1.4 ? Opt (2)NGC 2146 18.0 11.15 30 + − . + . − . + − + − S 8 SN 2005V Ib / c 0.5 ? IR (2)MCG -02-01-052 115.2 11.48 41 + − . + . − . + − + − S 3 SN 2010hp II 2.1 0.5 IR (9)NGC 6000 28.1 10.95 11 + − . + . − . + − + − S 4 SN 2010as IIb 0.6 1.8 Opt (10)NGC 5433 70.3 11.01 46 + − < + − + − S 2 SN 2010gk Ic 2.0 ? Opt (2)
Notes.
1) Kool (2019), 2) Kool et al. (2018), 3) Kankare et al. (2012), 4) Mattila et al. (2012), 5) Kankare et al. (2014a), 6) This work, 7)Kankare et al. (2008), 8) Pastorello et al. (2015), 9) Miluzio et al. (2013), 10) Folatelli et al. (2014). among these galaxies is 0.011 (2.5 σ ). However, for the SNR ≥ − sample the p -value is reduced to 0.00060 (3.4 σ ).Type II / IIn SNe are consistent with the uniform distributionin these comparisons with a p -value of 0.14 (1.5 σ ) and 0.075(1.8 σ ) for the ≥ ≥ − samples, respectively.Furthermore, we also consider cases with the sample groups de-fined as Type II and Type IIb / Ib / Ic SNe. Generally, these groupswith reduced statistics appear to slightly increase the p -values.The full presentation of the yielded values are listed in Table 2.The p -values for the estimated probabilities of obtaining at leastas extreme a di ff erence as seen in the comparisons were con-verted to the corresponding standard deviation ( σ ) units z of ahalf-normal distribution by solving p / = (2 π ) − / R ∞ z ( e − x / ) dx .A half-normal distribution is warranted, as the AD test probesthe absolute di ff erence | t SB , − t SB , | between distributions. Wedo note that there is no standard method to take the data pointerrors into account with the AD (or other similar) statistical test.The obvious caveat of the aforementioned trends is that theresults are based on a relatively small sample of only 29 CC-SNe and their 16 host LIRGs. Furthermore, the model depen-dencies and errors associated with the starburst age estimationsare not taken into account in the significance calculations. This is a strong motivation to discover and study more CCSNe in thecentral regions of LIRGs to improve sample statistics. Removingan individual galaxy, and thus typically 1 or 2 CCSNe, from thestudied samples will not result in major di ff erences in the yielded p -values. However, arbitrarily removing Arp 299 from the sam-ple, and therefore 6 Type IIb / Ib SNe of the analysed sampleswould result in the disappearance of the discussed trends, seeFig. 17. For completeness, jackknife resampling averages of the p -values are also listed in Table 2 with the corresponding valuesof standard error of the mean.Our assumption was that very high CCSN rate LIRGs canhave e ff ectively dominating starburst episodes that produce themajority of CCSNe in these galaxies. However, even if thesegalaxies had one recent dominating starburst episode, this wouldnot quench the underlying and ongoing star formation and CCSNproduction on a lower e ffi ciency. Similarly, the sample LIRGscould also have other more minor non-dominating starburstepisodes. Therefore, these galaxies can still produce any SN sub-types, though at a more moderate rate and on average less con-centrated towards the central regions of their hosts.The starburst ages ranging from ∼
25 to 40 Myr, as foundfor LIRGs hosting primarily H-rich SNe in our sample, cor-
Article number, page 13 of 25 & Aproofs: manuscript no. aa
Table 2.
AD statistical test results of p -values and corresponding standard deviation ( σ ) units for our CCSN samples having the same underlyingdistributions of estimated global starburst age of the host. Additional tests include comparisons to a ‘flat’ simulated sample, including galaxieswhich have hosted ≥ θ p − value ) and standard error values, and the corresponding σ units ( θ σ ), which are dominated by the arbitrary removalof Arp 299 and its CCSNe from the samples. SNR ≥ ≥ p -value σ θ p − value θ σ p -value σ θ p − value θ σ IIb / Ib / Ic / Ibn vs II / IIn 0.0027 3.0 0.017 ± . + . − . ± . + . − . IIb / Ib / Ic vs II / IIn 0.0039 2.9 0.030 ± . + . − . ± . + . − . IIb / Ib / Ic vs II 0.0059 2.8 0.032 ± . + . − . ± . + . − . IIb / Ib / Ic / Ibn vs flat
IIb / Ib / Ic / Ibn / II / IIn ± . + . − . ± . + . − . IIb / Ib / Ic vs flat
IIb / Ib / Ic / II / IIn ± . + . − . ± . + . − . IIb / Ib / Ic vs flat
IIb / Ib / Ic / II ± . + . − . ± . + . − . II / IIn vs flat
IIb / Ib / Ic / Ibn / II / IIn ± . + . − . ± . + . − . II / IIn vs flat
IIb / Ib / Ic / II / IIn ± . + . − . ± . + . − . II vs flat
IIb / Ib / Ic / II ± . + . − . ± . + . − . Fig. 15.
An example SED fit (solid black curve) to the data of one ofthe sample LIRGs, IRAS 18293-3413 (points), with a combination of astarburst (dashed red), a spheroidal galaxy (dot-dashed orange), and anAGN (dotted blue) component. respond to progenitor life times for zero-age main sequence(ZAMS) mass M ZAMS of ∼
11 to 8 M ⊙ , respectively, accordingto the Geneva group single star stellar evolution tracks in So-lar metallicity with rotation (Ekström et al. 2012). This is con-sistent with both theory and the direct red supergiant (RSG)progenitor detections of nearby Type IIP SNe (Smartt 2009).Similarly, our estimate of the global starburst age of 16 + − Myrfor Arp 299 corresponds to progenitor masses of roughly 13to 18 M ⊙ (Ekström et al. 2012). Intriguingly, the progenitorsof many canonical Type IIb SNe are typically found withinthis range of initial mass, and in a binary system, e.g. 1993J(Nomoto et al. 1993; Podsiadlowski et al. 1993; Aldering et al.1994; Woosley et al. 1994), 2008ax (Crockett et al. 2008;Folatelli et al. 2015), 2011dh (Maund et al. 2011; Van Dyk et al.2011; Ergon et al. 2014), 2013df (Morales-Garo ff olo et al. 2014;Van Dyk et al. 2014), and 2016gkg (Bersten et al. 2018). Fromour sample of 6 central CCSNe in Arp 299, 50 % are Type IIb and 50 % are Type Ib events. Kangas et al. (2017) found consis-tent H α associations between Type IIb SNe and M ZAMS ∼ M ⊙ yellow super giants, and Type Ib SNe and M ZAMS ∼ M ⊙ RSGs. Here we find results consistent with those above, and notethe advantage of using LIRGs (in comparison to normal spiralgalaxies) for statistical studies as the starburst age can be morestrictly constrained in these galaxies.Anderson et al. (2011) and Anderson & Soto (2013) high-light the tendency of the Arp 299 system to produce Type Ib toType IIb SNe, compared to their normal fraction of all CCSNein the local Universe. This relative excess has been discussed torise either from young age of the recent star formation or from atop-heavy IMF (Anderson et al. 2011). The recent SNe 2019lqoand 2020fkb follow the trend of Type Ib / IIb SNe in Arp 299,which we argue to be consistent with the dominating episodeof recent star formation with a normal (Salpeter) IMF adopted.Pérez-Torres et al. (2009) reported the radio detection of 20 SNeor SN remnants within the <
150 pc nuclear region of the nu-cleus of Arp 299-A, including three young radio SNe. They con-cluded that the properties of the young SNe are consistent withthose of either Type IIb or normal Type II SNe. If Arp 299 pro-duces predominantly Type Ib / IIb SNe, this would suggest thatthese recent SNe are predominantly Type IIb SNe. For compari-son, Alonso-Herrero et al. (2000) inferred a starburst age of ∼ ′ ) they find indications of a somewhat youngerstarburst age, in particular in nuclei C ′ and C of ∼ ∼
50 to90 M ⊙ range are expected to explode as CCSNe. For a SalpeterIMF, the fraction of such massive stars is fairly insignificant, andthus the most recent star formation episode could not have con-tributed significantly to the observed CCSN rate and populationin Arp 299.
5. Conclusions
We discovered a new Type Ic SN 2018ec in the LIRG NGC 3256during the ESO science verification run of the adaptive opticsseeing enhancer instrument HAWK-I / GRAAL. While carryingout follow up of this SN, we discovered another transient, AT2018cux, in the same galaxy that was a subluminous type IIPSN. We derive the host galaxy extinctions of A V = . + . − . and2 . ± . Article number, page 14 of 25. Kankare et al.: CCSNe in LIRGs
Fig. 16.
Upper panel: Type distribution of classified CCSNe com-pared to our SED modelled global age of the host starburst at thecentral regions of our sample LIRGs. The sizes of the symbols indi-cate the derived host galaxy extinction of the SNe, with unknown (andlikely small) extinction cases indicated with square symbols. The sym-bol colours indicate the CCSN subtype classifications. The events aremarked with closed and open symbols based on their estimated hostCCSN rate above and below 0.5 CCSN yr − , respectively. Lower panel:A simplified cumulative distribution presentation of the upper paneldata of the Type IIb / Ib / Ic / Ibn and Type II / IIn samples of CCSNe. Thedata suggests that H-poor and H-rich CCSNe come from very young( .
30 Myr) and older ( &
30 Myr) starbursts, respectively. candidate from 2014, PSN102750, in the same galaxy was foundto be consistent with H-rich CCSN with a fairly low host galaxyextinction. A best fit for PSN102750 is provided by a Type IInusing a combination of early ground-based follow-up and late-time colours from HST; however, we cannot fully rule out a TypeIIP origin. We also report follow up of Type IIb SN 2019lqo andType Ib SN 2020fkb in Arp 299 and derive a line-of-sight hostextinction of A V = . + . − . and 0 . + . − . mag for them, respectively.We find evidence that the CCSN subtypes occurring within ∼ / IIn) and H-poor (TypeIIb / Ib / Ic / Ibn) CCSN progenitors have di ff erent underlying age Fig. 17.
Yielded σ values from a selection of statistical tests for the sam-ple with individual galaxies and their sample CCSNe removed from theanalysis as a test. While removing individual galaxies and thus typi-cally only 1 or 2 CCSNe from the sample will not have a major e ff ecton the resulting AD test values, the arbitrary removal of Arp 299 and its6 Type IIb / Ib SNe would make the discussed trends nonexistent. Openand closed symbols show the values for samples with the host SNR of ≥ ≥ − , respectively. Data points are not shown incases where the removal of the galaxy is irrelevant for the comparisonbetween the analysed samples. With the large number of hosted sam-ple CCSNe, the removal of the LIRG Arp 299 with a yielded youngstarburst age has also the largest weight in the jackknife resampling av-erages of the p -values for each set of comparisons, and result in meanvalues of θ p ≥ .
017 ( ≤ σ ). distributions in these galaxies at a 3 σ significance level. How-ever, the overall trend was drawn from a relatively small samplesize of CCSNe and their host galaxies, and the significance com-parisons between subgroups do not specifically take into accounterror ranges of the yielded starburst ages. Hence, future surveys,in particular in high spatial resolution IR, will be necessary todiscover and further study CCSNe in LIRGs.We predict, that LIRGs that have hosted multiple discov-ered circumnuclear CCSNe in their central regions will continueto produce (predominantly) the subtypes that they have alreadyshown to favour in their nuclear regions. New CCSN discov-eries in these galaxies will constrain more accurately a typicalprojected distance limit for this trend, or alternatively a pos-sible e ff ective radius limit that should be adopted. At the mo-ment, the very small number statistics of the currently avail-able sample of SNe in these galaxies do not allow for moresophisticated constraints. Furthermore, with improved statistics,the discussed trend o ff ers a possible new method to probe theprogenitor systems of di ff erent CCSN types by using high-IR-luminosity LIRGs as laboratories. Acknowledgements.
We thank the anonymous referee for useful comments. Wethank Marco Fiaschi for carrying out some of the Asiago observations. EK issupported by the Turku Collegium of Science, Medicine and Technology. EKalso acknowledge support from the Science and Technology Facilities Coun-cil (STFC; ST / P000312 / Article number, page 15 of 25 & Aproofs: manuscript no. aa
European Union’s Horizon 2020 research and innovation programme under theMarie Skłodowska-Curie grant agreement No. 839090. This work has been par-tially supported by the Spanish grant PGC2018-095317-B-C21 within the Euro-pean Funds for Regional Development (FEDER). MG is supported by the Pol-ish NCN MAESTRO grant 2014 / / A / ST9 / / DOCTORADOBECAS CHILE / / WK / /
07. Based on observations made with the Nordic Opti-cal Telescope, operated by the Nordic Optical Telescope Scientific Association atthe Observatorio del Roque de los Muchachos, La Palma, Spain, of the Institutode Astrofisica de Canarias. The data presented here were obtained in part withALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA)under a joint agreement with the University of Copenhagen and NOTSA. Thiswork is partly based on the NUTS2 programme carried out at the NOT. NUTS2is funded in part by the Instrument Center for Danish Astrophysics (IDA). TheLiverpool Telescope is operated on the island of La Palma by Liverpool JohnMoores University in the Spanish Observatorio del Roque de los Muchachosof the Instituto de Astrofisica de Canarias with financial support from the UKScience and Technology Facilities Council. This paper is also based on obser-vations collected at the Copernico 1.82 m and Schmidt 67 /
92 Telescopes op-erated by INAF – Osservatorio Astronomico di Padova at Asiago, Italy. Basedon observations obtained at the Gemini Observatory, which is operated by theAssociation of Universities for Research in Astronomy, Inc., under a coopera-tive agreement with the NSF on behalf of the Gemini partnership: the NationalScience Foundation (United States), the National Research Council (Canada),CONICYT (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva(Argentina), and Ministério da Ciência, Tecnologia e Inovação (Brazil). Obser-vations were carried out under programme GS-2017A-C-1. This project useddata obtained with the Dark Energy Camera (DECam), which was constructedby the Dark Energy Survey (DES) collaboration. Funding for the DES Projectshas been provided by the DOE and NSF (USA), MISE (Spain), STFC (UK),HEFCE (UK), NCSA (UIUC), KICP (U. Chicago), CCAPP (Ohio State), MIFPA(Texas A&M University), CNPQ, FAPERJ, FINEP (Brazil), MINECO (Spain),DFG (Germany) and the collaborating institutions in the Dark Energy Survey,which are Argonne Lab, UC Santa Cruz, University of Cambridge, CIEMAT-Madrid, University of Chicago, University College London, DES-Brazil Con-sortium, University of Edinburgh, ETH Zürich, Fermilab, University of Illinois,ICE (IEEC-CSIC), IFAE Barcelona, Lawrence Berkeley Lab, LMU Münchenand the associated Excellence Cluster Universe, University of Michigan, NOAO,University of Nottingham, Ohio State University, OzDES Membership Consor-tium, University of Pennsylvania, University of Portsmouth, SLAC National Lab,Stanford University, University of Sussex, and Texas A&M University. Based onobservations obtained with the Samuel Oschin 48-inch Telescope at the PalomarObservatory as part of the Zwicky Transient Facility project. ZTF is supportedby the National Science Foundation under Grant No. AST-1440341 and a collab-oration including Caltech, IPAC, the Weizmann Institute for Science, the OskarKlein Center at Stockholm University, the University of Maryland, the Univer-sity of Washington, Deutsches Elektronen-Synchrotron and Humboldt Univer-sity, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, theUniversity of Wisconsin at Milwaukee, and Lawrence Berkeley National Labo-ratories. Operations are conducted by COO, IPAC, and UW. Based on observa-tions at Cerro Tololo Inter-American Observatory, National Optical AstronomyObservatory (NOAO Prop. ID 2017A-0260; and PI: Soares-Santos), which isoperated by the Association of Universities for Research in Astronomy (AURA)under a cooperative agreement with the National Science Foundation. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been madepossible through contributions by the Institute for Astronomy, the University ofHawaii, the Pan-STARRS Project O ffi ce, the Max-Planck Society and its partic-ipating institutes, the Max Planck Institute for Astronomy, Heidelberg and theMax Planck Institute for Extraterrestrial Physics, Garching, The Johns HopkinsUniversity, Durham University, the University of Edinburgh, the Queen’s Univer-sity Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las CumbresObservatory Global Telescope Network Incorporated, the National Central Uni-versity of Taiwan, the Space Telescope Science Institute, the National Aeronau-tics and Space Administration under Grant No. NNX08AR22G issued throughthe Planetary Science Division of the NASA Science Mission Directorate, theNational Science Foundation Grant No. AST-1238877, the University of Mary-land, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory,and the Gordon and Betty Moore Foundation. Some of the data presented in thispaper were obtained from the Mikulski Archive for Space Telescopes (MAST).STScI is operated by the Association of Universities for Research in Astron-omy, Inc., under NASA contract NAS5-26555. This work is based in part onarchival data obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a con-tract with NASA. This research has made use of NED which is operated bythe Jet Propulsion Laboratory, California Institute of Technology, under contractwith the National Aeronautics and Space Administration. We have made use ofthe Weizmann Interactive Supernova Data Repository (Yaron & Gal-Yam 2012,https: // wiserep.weizmann.ac.il). References
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Box 9, Observatory 7935,Cape Town, South Africa Department of Astronomy, University of Cape Town, Private BagX3, Rondebosch 7701, South Africa Department of Physics and Astronomy, Macquarie University, NSW2109, Australia Macquarie University Research Centre for Astronomy, Astrophysics& Astrophotonics, Sydney, NSW 2109, Australia Parkdale Observatory, 225 Warren Road, RDl Oxford, Canterbury7495, New Zealand Backyard Observatory Supernova Search (BOSS) School of Physics, O’Brien Centre for Science North, UniversityCollege Dublin, Belfield, Dublin 4, Ireland INAF – Osservatorio Astronomico, Vicolo Osservatorio 5, I-35122Padova, Italy Astrophysics Research Institute, Liverpool John Moores University,IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF,UK Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany Dipartimento di Fisica e Astronomia, Universitá di Padova, VicoloOsservatorio 2, I-35122 Padova, Italy Finnish Centre for Astronomy with ESO (FINCA), University ofTurku, Vesilinnantie 5, FI-20014 Turku, Finland Instituto de Astrofísica de Andalucía, Glorieta de las Astronomía,s / n, E-18008 Granada, Spain Departamento de Física Teorica, Facultad de Ciencias, Universidadde Zaragoza, Spain Institute of Astronomy and Astrophysics, Academia Sinica, 11F ofAstronomy-Mathematics Building, AS / NTU No. 1, Sec. 4, Roo-sevelt Rd, Taipei 10617, Taiwan, R.O.C Aalto University Metsähovi Radio Observatory, Metsähovintie 114,FI-02540 Kylmälä, Finland Cerro Tololo Inter-American Observatory, NSF’s National Optical-Infrared Astronomy Research Laboratory, Casilla 603, La Serena,Chile Departamento de Física Teórica y del Cosmos, Universidad deGranada, E-18071 Granada, Spain Astronomical Observatory, University of Warsaw, Al. Ujazdowskie4, 00-478 Warszawa, Poland School of Physics & Astronomy, Cardi ff University, Queens Build-ings, The Parade, Cardi ff , CF24 3AA, UK School of Physics, Trinity College Dublin, The University ofDublin, Dublin 2, Ireland School of Physics and Astronomy, University of Southampton,Southampton, Hampshire, SO17 1BJ, UK Birmingham Institute for Gravitational Wave Astronomy and Schoolof Physics and Astronomy, University of Birmingham, BirminghamB15 2TT, UK Institute for Astronomy, University of Edinburgh, Royal Observa-tory, Blackford Hill, EH9 3HJ, UK Departamento de Ciencias Físicas, Universidad Andrés Bello, Avda.República 252, Santiago, Chile Millennium Institute of Astrophysics, Nuncio Monsenor SóteroSanz 100, Providencia, Santiago, ChileArticle number, page 18 of 25. Kankare et al.: CCSNe in LIRGs
Appendix A: Appendix
Fig. A.1. ′ × ′ ePESSTO NTT + EFOSC2 r -band image of the fieldof NGC 3256 on 2018 January 16. The locations of sequence stars,SN 2018ec (green), AT 2018cux (red), PSN102750 (brown), and SN2001db (orange) are indicated. North is up, east is left. AppendixA.1: SN2020cujin NGC 1614
SN 2020cuj in NGC 1614 was discovered by ZTFon 2020 February 12 03:06:02 UT with the internalname of ZTF20aao ff ej (De 2020), and classified byDahiwale & Fremling (2020) as a Type II SN. The SNwas also detected by Gaia (internal name Gaia20ayu).
Gaia de-rives coordinates RA = h m s .
53 and Dec = − ◦ ′ ′′ . + EFOSC2 (via ePESSTO + )image of m V = . ± .
06 mag (on JD = + NOTCam image of m K = . ± .
04 mag (on JD = A V = . ± . . + . − . mag brighterthan SN 2013ej. The light curve fit is shown in Fig. A.2. Thelate-time Gaia detection could indicate a more linearly decliningType IIL SN, however, the
Gaia data points are not templatesubtracted and likely contain background contamination fromthe host galaxy, which can be significant at late phases.We note that public ZTF brokers list also another eventZTF19acyfumm in NGC 1614 at RA = h m s .
06 and Dec = − ◦ ′ ′′ .
47 discovered on 2019 November 25 07:59:00 UT.The coordinates are consistent with the host galaxy nucleus, butnot with SN 2020cuj and the two events appear to be unrelated.The ePESSTO + programme obtained an optical spectrum at thelocation on 2019 December 18 with the NTT and EFOSC2, how-ever, the spectrum was reported to be red and dominated by thehost galaxy without clear transient features (Müller Bravo et al.2019). To our knowledge no other transient programme has car- Fig. A.2.
Absolute magnitude light curves of AT 2020cuj (points) inNGC 1614 corrected for the host galaxy extinction of A V = . Gaia light curve is not template subtracted,it is likely that it contains flux excess from the luminous host back-ground, which has an e ff ect in particular to the late-time data points. ried out any observations of ZTF19acyfumm and due to the un-clear nature of the event it is not part of our study. Article number, page 19 of 25 & Aproofs: manuscript no. aa
Table A.1.
Optical sequence star magnitudes in the field of SN 2018ec with the errors given in brackets. m g m r m i m z (mag) (mag) (mag) (mag)1 18.538(0.014) 17.920(0.018) 17.703(0.019) 17.603(0.042)2 19.121(0.015) 18.364(0.018) 18.101(0.019) 17.973(0.048)3 18.741(0.014) 18.115(0.017) 17.862(0.019) 17.786(0.059)4 17.824(0.012) 17.400(0.018) 17.221(0.018) 17.121(0.050)5 17.557(0.014) 16.782(0.017) 16.482(0.018) 16.232(0.023)6 17.176(0.014) 16.726(0.018) 16.545(0.019) 16.366(0.019)7 18.022(0.015) 17.170(0.018) 16.840(0.019) 16.594(0.022)8 18.532(0.016) 17.797(0.017) 17.537(0.020) 17.318(0.020)9 18.180(0.014) 17.644(0.017) 17.429(0.019) 17.253(0.022)10 17.547(0.014) 17.066(0.018) 16.881(0.019) 16.667(0.021)11 18.892(0.016) 18.376(0.018) 18.163(0.020) 18.026(0.030)12 18.509(0.016) 18.026(0.018) 17.820(0.020) 17.605(0.018)13 19.572(0.021) 18.125(0.018) 16.861(0.020) 16.284(0.018)14 19.602(0.019) 18.873(0.043) 18.729(0.020) 18.437(0.018)15 18.521(0.014) 18.114(0.018) 17.943(0.020) 17.671(0.022) Table A.2.
Photometry for SN 2018ec with the errors given in brackets. JD m g m r m i m z m J m H m K Telescope(2400000 + ) (mag) (mag) (mag) (mag) (mag) (mag) (mag)58121.86 - - - - - - 15.13(0.05) VLT58124.86 - - - - - - 15.22(0.04) VLT58130.76 - - - 17.15(0.03) - - - NTT58134.77 - - - - 16.35(0.04) 15.79(0.03) 15.72(0.05) NTT58135.71 20.25(0.03) 18.79(0.06) 18.02(0.01) 17.40(0.03) - - - NTT58154.82 - - - - 17.04(0.09) 16.30(0.03) 16.37(0.06) NTT58162.83 20.74(0.07) 19.16(0.07) 18.48(0.02) 17.85(0.03) - - - NTT58164.86 - - - - 17.38(0.10) 16.51(0.04) 16.62(0.06) NTT58169.80 20.89(0.06) 19.31(0.10) 18.70(0.03) 18.04(0.03) - - - NTT58186.61 - - - - - - 17.08(0.16) NTT58186.79 20.97(0.17) 19.64(0.15) 19.02(0.03) 18.32(0.08) - - - NTT58201.70 21.21(0.07) 19.67(0.12) 19.20(0.03) 18.62(0.04) - - - NTT58204.61 - - - - 18.64(0.20) 17.51(0.06) 17.44(0.10) NTT58215.72 21.38(0.23) 20.01(0.17) 19.41(0.05) 18.98(0.07) - - - NTT58216.53 - - - - 18.71(0.41) 17.52(0.10) 17.76(0.11) NTT58228.57 - 20.29(0.20) 19.72(0.05) 19.12(0.09) - - - NTT58230.58 - - - - 18.84(0.29) - - NTT58243.55 - 20.11(0.20) 19.94(0.04) 19.37(0.06) - - - NTT58250.65 - 20.72(0.45) 20.09(0.04) 19.67(0.06) - - - NTT58251.58 - - - - 19.04(0.25) 18.47(0.15) 18.42(0.30) NTT58260.46 - 20.15(0.27) 20.17(0.05) 19.85(0.08) - - - NTT Table A.3.
Spectroscopic log for SN 2018ec.
JD Epoch Grism Slit R PA Exp. time λ Telescope(2400000 + ) (d) ( ′′ ) ( λ/ ∆ λ ) ( ◦ ) (s) (Å)58130.8 +
28 Gr13 1.0 355 121 1500 3645 − +
32 GB 1.0 550 0 12 × ×
90 9370 − +
33 Gr13 1.0 355 83,91 2 × − +
52 GB 1.0 550 0 6 × ×
90 9370 − +
62 GB 1.0 550 0 12 × ×
90 9370 − +
63 Gr13 1.0 355 228,249 2 × − +
85 Gr13 1.0 355 236,252 2 × − Article number, page 20 of 25. Kankare et al.: CCSNe in LIRGs
Fig. A.3.
Our SED models (solid black curves) for the observations (black points) of our initial sample of LIRGs for which a spherical host galaxymodel is favoured. The model components include a spheroidal galaxy (dot-dashed orange), starburst contribution (dashed red), and an AGN(dotted blue). Article number, page 21 of 25 & Aproofs: manuscript no. aa
Fig. A.3. – continued Table A.4.
Photometry for AT 2018cux with the errors given in brackets. JD m g m r m i m z m J m H m K Telescope(2400000 + ) (mag) (mag) (mag) (mag) (mag) (mag) (mag)58169.81 > > > > > > > > > > Table A.5.
Photometry for PSN102750 with the errors given in brackets. JD m B m R Telescope(2400000 + ) (mag) (mag)56785.93 - 15.67(0.22) T3056793.41 - 15.37(0.15) C1456813.38 - 15.95(0.13) C1456818.84 17.065(0.001) - HST56975.16 - 19.116(0.004) HST Article number, page 22 of 25. Kankare et al.: CCSNe in LIRGs
Fig. A.4.
Our SED models (solid black curves) for the observations (black points) of our initial sample of LIRGs for which a disc host galaxymodel is favoured. The model components include a disc galaxy (dot-dashed green), starburst contribution (dashed red), and an AGN (dotted blue).
Table A.6.
Our photometry for SN 2019lqo with the errors given in brackets. JD m U m B m V m R m I m J m H m K Telescope(2400000 + ) (mag) (mag) (mag) (mag) (mag) (mag) (mag) (mag)58689.37 - - - 17.77(0.08) - - - - NOT58694.39 19.13(0.12) 19.03(0.07) 17.92(0.03) 17.42(0.02) 17.01(0.02) - - - NOT58699.38 19.21(0.07) 18.93(0.08) 17.77(0.02) 17.22(0.02) 16.75(0.02) - - - NOT58706.36 19.96(0.25) 19.48(0.12) 17.88(0.03) 17.24(0.03) 16.77(0.03) - - - NOT58712.37 - 20.11(0.33) 18.10(0.04) 17.44(0.03) 16.90(0.03) - - - NOT58714.36 - - - - - 16.18(0.02) 15.95(0.04) - NOT58780.70 - - - - - 17.95(0.04) 17.19(0.04) 16.97(0.09) NOT58864.56 - - 21.31(0.18) 20.49(0.06) 19.97(0.06) - - - NOT Article number, page 23 of 25 & Aproofs: manuscript no. aa
Table A.7.
Photometry for SN 2019lqo based on public data including our measurements from the ZTF DR3 with the errors given in brackets. JD m g m G m r Telescope(2400000 + ) (mag) (mag) (mag)58679.68 20.27(0.15) - - ZTF58679.70 - - 19.04(0.09) ZTF58680.73 - > Table A.8.
Our optical photometry for SN 2020fkb with the errors given in brackets, and early public ZTF photometry listed for completeness. JD m u m B m g m V m r m i m z Telescope(2400000 + ) (mag) (mag) (mag) (mag) (mag) (mag) (mag)58936.66 - - 17.83(0.08) - - - - ZTF58939.62 - - - - 16.97(0.07) - - ZTF58939.83 - - 17.33(0.07) - - - - ZTF58939.87 - - - - 16.93(0.09) - - ZTF58942.33 - 17.53(0.11) 17.17(0.04) 17.00(0.07) 16.85(0.09) 17.04(0.05) 17.00(0.11) A1.82m58943.30 - 17.38(0.04) - 16.80(0.06) 16.72(0.05) 16.86(0.03) 16.99(0.07) A1.82m58944.44 17.98(0.11) 17.51(0.24) 16.88(0.04) 16.75(0.06) 16.56(0.04) 16.75(0.03) 16.79(0.07) A1.82m58945.31 18.61(0.57) 17.44(0.11) 16.88(0.04) 16.87(0.06) 16.63(0.03) 16.78(0.04) 16.85(0.04) A1.82m58947.32 18.26(0.41) 17.41(0.09) 16.94(0.09) 16.69(0.04) 16.45(0.08) 16.36(0.09) - A67 / / / / / Article number, page 24 of 25. Kankare et al.: CCSNe in LIRGs
Table A.9.
Our near-IR photometry for SN 2020fkb with the errors given in brackets. JD m J m H m K Telescope(2400000 + ) (mag) (mag) (mag)58945.37 - 15.95(0.05) - LT58964.45 - 15.69(0.08) - LT58970.38 - 15.88(0.04) - LT58974.36 - 15.99(0.04) - LT58978.44 16.43(0.04) - 15.88(0.13) NOT58979.45 - 16.31(0.05) - LT59000.39 17.09(0.06) 16.68(0.08) 16.60(0.06) NOT59025.47 17.95(0.16) 17.55(0.14) 17.34(0.35) NOT Table A.10.
Spectroscopic log for SN 2020fkb.
JD Epoch Grism Slit R PA Exp. time λ Telescope(2400000 + ) (d) ( ′′ ) ( λ/ ∆ λ ) ( ◦ ) (s) (Å)58942.3 − − − − − − + − +
20 Gr4 1.3 280 124 1800 3500 − +
72 Gr4 1.3 280 122 2400 3400 − +
87 Gr4 1.3 280 101 2400 3500 −9300 NOT