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We present observations and analysis of PS1-10bzj, a superluminous supernova
(SLSN) discovered in the Pan-STARRS Medium Deep Survey at a redshift z = 0.650.
Spectroscopically, PS1-10bzj is similar to the hydrogen-poor SLSNe 2005ap and
SCP 06F6, though with a steeper rise and lower peak luminosity (M_bol = -21.4
mag) than previous events. We constru...
Contexts in source publication
Context 1
... obtained four epochs of spectroscopy of PS1-10bzj. Details are given in Table 2. Our initial spectra were taken on 2011 January 18.2 using LDSS3 on the 6.5-m Magellan Clay telescope. ...
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Citations
... Hydrogen-poor (Type I) superluminous supernovae (SLSNe; Chomiuk et al. 2011;Quimby et al. 2011;Gal-Yam 2012) are a rare subclass of core-collapse supernovae (CCSNe) that are ∼10-100 times more luminous than normal SNe and have longer durations of several months to years (e.g., Nicholl et al. 2015;Inserra et al. 2017;De Cia et al. 2018;Lunnan et al. 2018). Originally defined to have a peak absolute magnitude of M < −21 (Gal-Yam 2012), they are now classified based on their spectra, which are dominated by a blue continuum devoid of hydrogen features, and typically exhibit distinctive earlytime, "W-shaped" O II absorption lines at ∼3600-4600 Å (Chomiuk et al. 2011;Quimby et al. 2011;Lunnan et al. 2013;Mazzali et al. 2016;Quimby et al. 2018). The volumetric rate of SLSNe is only ∼0.1% of the overall CCSN rate (Quimby et al. 2018;Frohmaier et al. 2021), but in magnitude-limited optical surveys they account for ∼2% of all transients (e.g., Villar et al. 2019;Perley et al. 2020;Gomez et al. 2021) thanks to their high luminosities. ...
... Studies of SLSN host galaxies have also been leveraged to shed light on their progenitors. These studies revealed a preference for low-metallicity dwarf galaxies with higher specific star formation rates (sSFRs) and lower luminosities than CCSNe (e.g., Chen et al. 2013;Lunnan et al. 2013Lunnan et al. , 2014Lunnan et al. , 2015Angus et al. 2016;Perley et al. 2016;Schulze et al. 2018). An investigation of the subgalactic environments of 16 SLSNe using high-resolution Hubble Space Telescope (HST) data suggested that SLSN locations track bright UV regions of their host galaxies (Lunnan et al. 2015;hereafter L15), consistent with massive progenitors. ...
We present an extensive Hubble Space Telescope rest-frame UV imaging study of the locations of Type I superluminous supernovae (SLSNe) within their host galaxies. The sample includes 65 SLSNe with detected host galaxies in the redshift range z ≈ 0.05–2. Using precise astrometric matching with SN images, we determine the distributions of the physical and host-normalized offsets relative to the host centers, as well as the fractional flux distribution relative to the underlying UV light distributions. We find that the host-normalized offsets of SLSNe roughly track an exponential disk profile, but exhibit an overabundance of sources with large offsets of 1.5–4 times their hosts' half-light radii. The SLSNe normalized offsets are systematically larger than those of long gamma-ray bursts (LGRBs), and even Type Ib/c and Type II SNe. Furthermore, we find from a Monte Carlo procedure that about 37 − 8 + 6 % of SLSNe occur in the dimmest regions of their host galaxies, with a median fractional flux value of 0.16, in stark contrast to LGRBs and Type Ib/c and Type II SNe. We do not detect any significant trends in the locations of SLSNe as a function of redshift, or as a function of explosion and magnetar engine parameters inferred from modeling of their optical light curves. The significant difference in SLSN locations compared to LGRBs (and normal core-collapse SNe) suggests that at least some of their progenitors follow a different evolutionary path. We speculate that SLSNe arise from massive runaway stars from disrupted binary systems, with velocities of ∼10 ² km s ⁻¹ .
... When binning SNe and SF by oxygen abundance, we find a clear decreasing occurrence of CCSNe per unit SF with increasing [O/H]. Previous works have explored the metallicity dependence of the occurrence of long gamma-ray bursts (which are connected to SNe Ic-BL; Fruchter et al. 2006;Stanek et al. 2006Stanek et al. , 2007Kewley et al. 2007;Modjaz et al. 2008;Mannucci et al. 2011;Graham & Fruchter 2013 and superluminous (SL)SNe (Stoll et al. 2011;Chen et al. 2013Chen et al. , 2017Lunnan et al. 2013;Frohmaier et al. 2021). Some works also discussed a metallicity effect on the rate of SNe Ia (Sullivan et al. 2006;Li et al. 2011;Graur & Maoz 2013;Kistler et al. 2013;Graur et al. 2017;Brown et al. 2019;Johnson et al. 2022). ...
Core-collapse supernovae (CCSNe) are widely accepted to be caused by the explosive death of massive stars with initial masses ≳8 M ⊙ . There is, however, a comparatively poor understanding of how properties of the progenitors—mass, metallicity, multiplicity, rotation, etc.—manifest in the resultant CCSN population. Here, we present a minimally biased sample of nearby CCSNe from the All-Sky Automated Survey for Supernovae survey whose host galaxies were observed with integral-field spectroscopy using MUSE at the Very Large Telescope. This data set allows us to analyze the explosion sites of CCSNe within the context of global star formation properties across the host galaxies. We show that the CCSN explosion site oxygen abundance distribution is offset to lower values than the overall H ii region abundance distribution within the host galaxies. We further split the sample at 12 + log 10 ( O / H ) = 8.6 dex and show that within the subsample of low-metallicity host galaxies, the CCSNe unbiasedly trace the star formation with respect to oxygen abundance, while for the subsample of higher-metallicity host galaxies, they preferentially occur in lower-abundance star-forming regions. We estimate the occurrence of CCSNe as a function of oxygen abundance per unit star formation and show that there is a strong decrease as abundance increases. Such a strong and quantified metallicity dependence on CCSN production has not been shown before. Finally, we discuss possible explanations for our result and show that each of these has strong implications not only for our understanding of CCSNe and massive star evolution but also for star formation and galaxy evolution.
... Nicholl et al. 2015;Inserra et al. 2017;Lunnan et al. 2018;De Cia et al. 2018). Originally defined to have a peak absolute magnitude of M < −21 (Gal-Yam 2012), they are now classified based on their spectra, which are dominated by a blue continuum devoid of hydrogen features, and typically ex-hibit distinctive early-time, "W"-shaped O II absorption lines at ∼ 3600 − 4600Å (Chomiuk et al. 2011;Quimby et al. 2011;Lunnan et al. 2013;Mazzali et al. 2016;Quimby et al. 2018). The volumetric rate of SLSNe is only ∼ 0.1% of the overall CCSN rate (Quimby et al. 2018;Frohmaier et al. 2021), but in magnitude-limited optical surveys they account for ∼ 2% of all transients (e.g., Villar et al. 2019;Perley et al. 2020;Gomez et al. 2021) thanks to their large luminosity. ...
... Studies of SLSN host galaxies have also been leveraged to shed light on their progenitors. These studies revealed a preference for low-metallicity dwarf galaxies with higher specific star formations rates (sSFRs) and lower luminosity than CCSNe (e.g., Chen et al. 2013;Lunnan et al. 2013Lunnan et al. , 2014Lunnan et al. , 2015Perley et al. 2016;Angus et al. 2016;Schulze et al. 2018). An investigation of the sub-galactic environments of 16 SLSNe using high-resolution HST data suggested that SLSN locations track bright UV regions of their host galaxies (Lunnan et al. 2015;hereafter, L15), consistent with massive progenitors. ...
We present an extensive $\textit{Hubble Space Telescope}$ ($\textit{HST}$) rest-frame ultraviolet (UV) imaging study of the locations of Type I superluminous supernovae (SLSNe) within their host galaxies. The sample includes 65 SLSNe with detected host galaxies in the redshift range $z\approx 0.05-2$. Using precise astrometric matching with SN images, we determine the distributions of physical and host-normalized offsets relative to the host centers, as well as the fractional flux distribution relative to the underlying UV light distribution. We find that the host-normalized offsets of SLSNe roughly track an exponential disk profile, but exhibit an overabundance of sources with large offsets of $1.5-4$ times their host half-light radius. The SLSNe normalized offsets are systematically larger than those of long gamma-ray bursts (LGRBs), and even Type Ib/c and II SNe. Furthermore, we find that about 40\% of all SLSNe occur in the dimmest regions of their host galaxies (fractional flux of 0), in stark contrast to LGRBs and Type Ib/c and II SNe. We do not detect any significant trends in the locations of SLSNe as a function of redshift, or as a function of explosion and magnetar engine parameters inferred from modeling of their optical lights curves. The significant difference in SLSN locations compared to LGRBs (and normal core-collapse SNe) suggests that at least some of their progenitors follow a different evolutionary path. We speculate that SLSNe arise from massive runaway stars from disrupted binary systems, with velocities of $\sim 10^2$ km s$^{-1}$.
... Superluminous supernovae (SLSNe) were disclosed near the start of the twenty-first century, as spatially rare but extremely bright stellar explosions usually occurring in dwarf galaxies having high specific star formation rate and low metallicity (e.g., Chen et al. 2013Chen et al. , 2017Lunnan et al. 2013Lunnan et al. , 2014Leloudas et al. 2015a;Angus et al. 2016;Japelj et al. 2016;Perley et al. 2016;Hatsukade et al. 2018;Schulze et al. 2018;Nicholl 2021). Their total radiated energy exceeds ∼10 51 erg, leading to an extremely high absolute brightness (M < −21) in the optical (e.g., Quimby et al. 2011;Gal-Yam 2012, 2019aNicholl et al. 2015a;Nicholl 2021). ...
We search for the reasons behind the spectroscopic diversity of hydrogen-poor superluminous supernovae (SLSNe-I) in the premaximum phase. Our analysis is a continuation of the paper of Könyves-Tóth & Vinkó, who disclosed two new subtypes of SLSNe-I characterized by the presence/absence of a W-shaped absorption feature in their premaximum spectra between 4000 and 5000 Å (called Type W and Type 15bn, respectively). However, the physical cause of this bimodality is still uncertain. Here we present premaximum spectral synthesis of 27 SLSNe-I with special attention to the photospheric temperature ( T phot ) and velocity ( v phot ) evolution. We find that a T phot limit of 12,000 K separates the Type W and Type 15bn SLSNe-I: Type W objects tend to show T phot ≥ 12,000 K, while Type 15bn ones have T phot ≤ 12,000 K. This is consistent with the chemical composition of the studied objects. Another difference between these groups may be found in their ejecta geometry: Type W SLSNe-I may show null polarization, implying spherical symmetry, while the polarization of Type 15bn objects may increase in time. This suggests a two-component model with a spherical outer carbon–oxygen layer and an asymmetric inner layer containing heavier ions. The two subgroups may have different light-curve evolution as well, since six Type W objects show early bumps, unlike Type 15bn SLSNe-I. This feature, however, needs further study, as it is based on only a few objects at present.
... SLSNe account for only ∼0.1% of the volumetric CCSN rate (Quimby et al. 2018;Frohmaier et al. 2021), but in magnitude-limited optical surveys they account for ∼2% of all transients (Perley et al. 2020;Gomez et al. 2021), thanks to their high luminosity. SLSNe are classified spectroscopically based on the lack of hydrogen Balmer lines, the presence of a blue continuum, and unique early-time "W"-shaped O II absorption lines at ∼3600-4600 Å (e.g., Lunnan et al. 2013;Mazzali et al. 2016;Quimby et al. 2018;Nicholl 2021). ...
With the upcoming Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST), it is expected that only ∼0.1% of all transients will be classified spectroscopically. To conduct studies of rare transients, such as Type I superluminous supernovae (SLSNe), we must instead rely on photometric classification. In this vein, here we carry out a pilot study of SLSNe from the Pan-STARRS1 Medium Deep Survey (PS1-MDS), classified photometrically with our SuperRAENN and Superphot algorithms. We first construct a subsample of the photometric sample using a list of simple selection metrics designed to minimize contamination and ensure sufficient data quality for modeling. We then fit the multiband light curves with a magnetar spin-down model using the Modular Open-Source Fitter for Transients ( MOSFiT ). Comparing the magnetar engine and ejecta parameter distributions of the photometric sample to those of the PS1-MDS spectroscopic sample and a larger literature spectroscopic sample, we find that these samples are consistent overall, but that the photometric sample extends to slower spins and lower ejecta masses, which correspond to lower-luminosity events, as expected for photometric selection. While our PS1-MDS photometric sample is still smaller than the overall SLSN spectroscopic sample, our methodology paves the way for an orders-of-magnitude increase in the SLSN sample in the LSST era through photometric selection and study.
... SLSNe account for only ∼ 0.1% of the volumetric CCSN rate (Quimby et al. 2018), but in magnitude-limited optical surveys they account for ∼ 2% of all transients (Perley et al. 2020;Gomez et al. 2021) thanks to their high luminosity. SLSNe are classified spectroscopically based on the lack of hydrogen Balmer lines, the presence of a blue continuum, and unique early time "W"-shaped O II absorption lines at ∼ 3600 − 4600Å (e.g., Lunnan et al. 2013;Mazzali et al. 2016;Quimby et al. 2018;Nicholl 2021). ...
With the upcoming Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST), it is expected that only $\sim 0.1\%$ of all transients will be classified spectroscopically. To conduct studies of rare transients, such as Type I superluminous supernovae (SLSNe), we must instead rely on photometric classification. In this vein, here we carry out a pilot study of SLSNe from the Pan-STARRS1 Medium-Deep Survey (PS1-MDS) classified photometrically with our SuperRAENN and Superphot algorithms. We first construct a sub-sample of the photometric sample using a list of simple selection metrics designed to minimize contamination and ensure sufficient data quality for modeling. We then fit the multi-band light curves with a magnetar spin-down model using the Modular Open-Source Fitter for Transients (MOSFiT). Comparing the magnetar engine and ejecta parameter distributions of the photometric sample to those of the PS1-MDS spectroscopic sample and a larger literature spectroscopic sample, we find that these samples are overall consistent, but that the photometric sample extends to slower spins and lower ejecta masses, which correspond to lower luminosity events, as expected for photometric selection. While our PS1-MDS photometric sample is still smaller than the overall SLSN spectroscopic sample, our methodology paves the way to an orders-of-magnitude increase in the SLSN sample in the LSST era through photometric selection and study.
... Type I superluminous supernovae (hereafter, SLSNe) are a rare subclass of core-collapse supernovae (CCSNe) that have been discovered by wide-field time-domain optical surveys over the past decade (Chomiuk et al. 2011;Quimby et al. 2011). They were originally defined to have a peak absolute magnitude of M < −21 (Gal-Yam 2012), but are now defined spectroscopically by an absence of hydrogen features, blue continua, and, usually, unique early time W-shaped O II absorption lines at ∼3600-4600 Å (e.g., Lunnan et al. 2013;Mazzali et al. 2016;Quimby et al. 2018). ...
Superluminous supernovae (SLSNe) are luminous transients that can be detected to high redshifts with upcoming optical time-domain surveys such as the Vera C. Rubin Observatory Legacy Survey of Space and Time. An interesting open question is whether the properties of SLSNe evolve through cosmic time. To address this question, in this paper we model the multicolor light curves of all 21 Type I SLSNe from the Dark Energy Survey (DES) with a magnetar spin-down engine, implemented in the Modular Open-Source Fitter for Transients ( MOSFiT ). With redshifts up to z ≈ 2, this sample includes some of the highest-redshift SLSNe. We find that the DES SLSNe span a similar range of ejecta and magnetar engine parameters as previous samples of mostly lower-redshift SLSNe (spin period P ≈ 0.79–13.61 ms, magnetic field B ≈ (0.03–7.33) × 10 ¹⁴ G, ejecta mass M ej ≈ 1.54–30.32 M ⊙ , and ejecta velocity v ej ≈ (0.55–1.45) × 10 ⁴ km s ⁻¹ ). The DES SLSN sample by itself exhibits the previously found negative correlation between M ej and P , with a pronounced absence of SLSNe with low ejecta mass and rapid spin. Combining our results for the DES SLSNe with 60 previous SLSNe modeled in the same way, we find no evidence for redshift evolution in any of the key physical parameters.
... They were originally defined to have a peak absolute magnitude of M < −21 (Gal-Yam 2012), but are now defined spectroscopically by an absence of hydrogen features, blue continua, and unique early-time "W"-shaped O II absorption lines at ∼ 3600 − 4600Å (e.g. Lunnan et al. 2013;Mazzali et al. 2016;Quimby et al. 2018). ...
Superluminous supernovae (SLSNe) are luminous transients that can be detected to high redshifts with upcoming optical time-domain surveys such as the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST). An interesting open question is whether the properties of SLSNe evolve through cosmic time. To address this question, in this paper we model for the first time the multi-color light curves of all 21 Type I SLSNe from the Dark Energy Survey (DES) with a magnetar spin-down engine, implemented in the Modular Open Source Fitter for Transients (MOSFiT). With redshifts up to $z\approx 2$, this sample includes some of the highest-redshift SLSNe. We find that the DES SLSNe span a similar range of ejecta and magnetar engine parameters to previous samples of mostly lower-redshift SLSNe (spin period $P\approx 0.79-13.64$ ms, magnetic field $B\approx (0.03-7.12)\times10^{14}$ G, ejecta mass $M_{\rm ej}\approx 1.51-30.50$ M$_{\odot}$, and ejecta velocity $v_{\rm ej}\approx (0.56-1.45)\times 10^4$ km s$^{-1}$). The DES SLSN sample by itself exhibits the previously found negative correlation between $M_{\rm ej}$ and $P$, with a pronounced absence of SLSNe with low ejecta mass and rapid spin. Combining our results for the DES SLSNe with 60 previous SLSNe modeled in the same way, we find no evidence for redshift evolution in any of the key physical parameters.
... Type I superluminous supernovae (SLSNe) on the other hand are a much more rare type of CCSNe. SLSNe also represent the explosions of stripped stars, but they be up to 100 times more luminous than SNe Ic, with peak magnitudes of M r ≈ −20.0 to −23 mag (e.g., Chomiuk et al. 2011;Quimby et al. 2011;Lunnan et al. 2013;Gal-Yam 2019;Gomez et al. 2020a). The primary energy source of SLSNe appears to be the spin-down energy of a newly formed millisecond magnetar, with typical spin periods of P spin ≈ 1.2 − 4 ms and magnetic fields of B ≈ 0.2 − 1.8 × 10 14 G ). ...
We present optical photometry and spectroscopy of SN\,2019stc (=ZTF19acbonaa), an unusual Type Ic supernova (SN Ic) at a redshift of $z=0.117$. SN\,2019stc exhibits a broad double-peaked light curve, with the first peak having an absolute magnitude of $M_r=-20.0$ mag, and the second peak, about 80 rest-frame days later, $M_r=-19.2$ mag. The total radiated energy is large, $E_{\rm rad}\approx 2.5\times 10^{50}$ erg. Despite its large luminosity, approaching those of Type I superluminous supernovae (SLSNe), SN\,2019stc exhibits a typical SN Ic spectrum, bridging the gap between SLSNe and SNe Ic. The spectra indicate the presence of Fe-peak elements, but modeling of the first light curve peak with radioactive heating alone leads to an unusually high nickel mass fraction of $f_{\rm Ni}\approx 31\%$ ($M_{\rm Ni}\approx 3.2$ M$_\odot$). Instead, if we model the first peak with a combined magnetar spin-down and radioactive heating model we find a better match with $M_{\rm ej}\approx 4$ M$_\odot$, a magnetar spin period of $P_{\rm spin}\approx 7.2$ ms and magnetic field of $B\approx 10^{14}$ G, and $f_{\rm Ni}\lesssim 0.2$ (consistent with SNe Ic). The prominent second peak cannot be naturally accommodated with radioactive heating or magnetar spin-down, but instead can be explained as circumstellar interaction with $\approx 0.7$ $M_\odot$ of hydrogen-free material located $\approx 400$ AU from the progenitor. Including the remnant mass leads to a CO core mass prior to explosion of $\approx 6.5$ M$_\odot$. The host galaxy has a metallicity of $\approx 0.26$ Z$_\odot$, low for SNe Ic but consistent with SLSNe. Overall, we find that SN\,2019stc is a transition object between normal SNe Ic and SLSNe.
... These extremely luminous events have at least ∼10 51 erg total radiated energy, leading to an absolute brightness of M < −21 in all optical wavelength bands (Quimby et al. 2011;Gal-Yam 2012, 2019a. It has also been reported that these supernovae (SNe) prefer to explode in dwarf galaxies having low metallicity and high specific star formation rate (Chen et al. 2013(Chen et al. , 2017cLunnan et al. 2013Lunnan et al. , 2014Leloudas et al. 2015;Angus et al. 2016;Japelj et al. 2016;Perley et al. 2016;Hatsukade et al. 2018;Schulze et al. 2018), although some counterexamples are also known. For example, PTF10tpz (Arabsalmani et al. 2019), PTF10uhf , and SN 2017egm (Chen et al. 2017b;Nicholl et al. 2017b;Bose et al. 2018;Izzo et al. 2018;Yan et al. 2018;Hatsukade et al. 2020) occurred in relatively bright and metalrich, or, at least not metal-poor, host galaxies. ...
We present a study of 28 Type I superluminous supernovae (SLSNe) in the context of the ejecta mass and photospheric velocity. We combine photometry and spectroscopy to infer ejecta masses via the formalism of radiation diffusion equations. We present an improved method to determine the photospheric velocity by combining spectrum modeling and cross-correlation techniques. We find that Type I SLSNe can be divided into two groups according to their pre-maximum spectra. Members of the first group have a W-shaped absorption trough in their pre-maximum spectrum, usually identified as due to O ii . This feature is absent in the spectra of supernovae in the second group, whose spectra are similar to that of SN 2015bn. We confirm that the pre- or near-maximum photospheric velocities correlate with the velocity gradients: faster evolving SLSNe have larger photospheric velocities around maximum. We classify the studied SLSNe into the Fast or the Slow evolving group according to their estimated photospheric velocities, and find that all those objects that resemble SN 2015bn belong to the Slow evolving class, while SLSNe showing the W-like absorption are represented in both Fast and Slow evolving groups. We estimate the ejecta masses of all objects in our sample, and obtain values in the range 2.9 (±0.8)−208 (±61) M ⊙ , with a mean of 43 (±12) M ⊙ . We conclude that Slow evolving SLSNe tend to have higher ejecta masses compared to the Fast SLSNe. Our ejecta mass calculations suggests that SLSNe are caused by energetic explosions of very massive stars, irrespective of the powering mechanism of the light curve.
