Host-Galaxy Properties of 32 Low-Redshift Superluminous Supernovae From the Palomar Transient Factory

Perley, D. A.; Quimby, R.; Yan, Lin; Vreeswijk, P.M.; De, A.; Lunnan, R.; Gal‐Yam, A.; Yaron, O.; Filippenko, A. V.; Graham, M. L.; Laher, Russ R.; Nugent, P.

doi:10.3847/0004-637x/830/1/13

Cited by 248 publications

(392 citation statements)

References 140 publications

(220 reference statements)

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“…Lee et al 2004;Peeples et al 2009). This is also seen for other SLSN type I host galaxies with disturbed morphologies (Lunnan et al 2015;Perley et al 2016). However, none of the three systems in LSQ14mo have particularly high sSFR or low Z g for their stellar mass.…”

Section: Interacting Galaxy Systemmentioning

confidence: 72%

The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system

Chen

Nicholl

Smartt

et al. 2017

A&A

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We present and analyse an extensive dataset of the superluminous supernova (SLSN) LSQ14mo (z = 0.256), consisting of a multicolour lightcurve from −30 d to +70 d in the rest-frame (relative to maximum light) and a series of six spectra from PESSTO covering −7 d to +50 d. This is among the densest spectroscopic coverage, and best-constrained rising lightcurve, for a fast-declining hydrogenpoor SLSN. The bolometric lightcurve can be reproduced with a millisecond magnetar model with ∼ 4 M ejecta mass, and the temperature and velocity evolution is also suggestive of a magnetar as the power source. Spectral modelling indicates that the SN ejected ∼ 6 M of CO-rich material with a kinetic energy of ∼ 7 × 10 51 erg, and suggests a partially thermalised additional source of luminosity between −2 d and +22 d. This may be due to interaction with a shell of material originating from pre-explosion mass loss. We further present a detailed analysis of the host galaxy system of LSQ14mo. PESSTO and GROND imaging show three spatially resolved bright regions, and we used the VLT and FORS2 to obtain a deep (five-hour exposure) spectra of the SN position and the three star-forming regions, which are at a similar redshift. The FORS spectrum at +300 days shows no trace of SN emission lines and we place limits on the strength of [O i] from comparisons with other Ic supernovae. The deep spectra provides a unique chance to investigate spatial variations in the host star-formation activity and metallicity. The specific star-formation rate is similar in all three components, as is the presence of a young stellar population. However, the position of LSQ14mo exhibits a lower metallicity, with 12 + log(O/H) = 8.2 in both the R 23 and N2 scales (corresponding to ∼ 0.3 Z ). We propose that the three bright regions in the host system are interacting, which thus triggers star formation and forms young stellar populations.

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Section: Interacting Galaxy Systemmentioning

confidence: 72%

The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system

Chen

Nicholl

Smartt

et al. 2017

A&A

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“…If FRBs are indeed more commonly hosted by dwarf galaxies in the low-redshift universe, they would share this preference with two other classes of high-energy transientslong-duration gamma-ray bursts and superluminous supernovae, both of which prefer low-mass, low-metallicity, and high star formation rate hosts (e.g., Fruchter et al 2006;Perley et al 2013Perley et al , 2016Vergani et al 2015; and other works). Indeed, superluminous supernovae are preferentially hosted by EELGs (Leloudas et al 2015).…”

Section: Relation To Dwarf Galaxiesmentioning

confidence: 99%

The Host Galaxy and Redshift of the Repeating Fast Radio Burst FRB 121102

Tendulkar

Bassa

Cordes

et al. 2017

ApJL

691

775

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The precise localization of the repeating fast radio burst (FRB 121102) has provided the first unambiguous association (chance coincidence probability p3×10 −4 ) of an FRB with an optical and persistent radio counterpart. We report on optical imaging and spectroscopy of the counterpart and find that it is an extended (0 6-0 8) object displaying prominent Balmer and [O III] emission lines. Based on the spectrum and emission line ratios, we classify the counterpart as a low-metallicity, star-forming, m r′ = 25.1 AB mag dwarf galaxy at a redshift of z = 0.19273(8), corresponding to a luminosity distance of 972 Mpc. From the angular size, the redshift, and luminosity, we estimate the host galaxy to have a diameter 4 kpc and a stellar mass of M * ∼(4-7)×107 M e , assuming a mass-to-light ratio between 2 to 3 M e L e −1 . Based on the Hα flux, we estimate the star formation rate of the host to be 0.4 M e yr −1 and a substantial host dispersion measure (DM) depth 324 pc cm −3 . The net DM contribution of the host galaxy to FRB 121102 is likely to be lower than this value depending on geometrical factors. We show that the persistent radio source at FRB 121102's location reported by Marcote et al. is offset from the galaxy's center of light by ∼200 mas and the host galaxy does not show optical signatures for AGN activity. If FRB 121102 is typical of the wider FRB population and if future interferometric localizations preferentially find them in dwarf galaxies with low metallicities and prominent emission lines, they would share such a preference with long gamma-ray bursts and superluminous supernovae.

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“…If an object like ASASSN-15lh, which peaked at −23.5 mag, were indeed an SLSN (Dong et al 2016;Godoy-Rivera et al 2017), it would be significantly more extreme than any of the objects found in PS1MDS. Given this transient's location at the center of a massive galaxy (while SLSN-I are almost exclusively found in low-mass, lowmetallicity galaxies; e.g., Lunnan et al 2014Lunnan et al , 2015Leloudas et al 2015;Perley et al 2016), it has also been suggested that this transient was a tidal disruption event rather than a true SLSN (Perley et al 2016;Leloudas et al 2016;Margutti et al 2017b). …”

Section: Luminosity Function Of H-poor Slsnementioning

confidence: 99%

Hydrogen-poor Superluminous Supernovae from the Pan-STARRS1 Medium Deep Survey

Lunnan

Chornock

Berger

et al. 2018

ApJ

Self Cite

113

103

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The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractWe present light curves and classification spectra of 17 hydrogen-poor superluminous supernovae (SLSNe) from the Pan-STARRS1 Medium Deep Survey (PS1 MDS). Our sample contains all objects from the PS1MDS sample with spectroscopic classification that are similar to either of the prototypes SN 2005ap or SN 2007bi, without an explicit limit on luminosity. With a redshift range z 0.3 1.6 < < , PS1MDS is the first SLSN sample primarily probing the high-redshift population; our multifilter PS1 light curves probe the rest-frame UV emission, and hence the peak of the spectral energy distribution. We measure the temperature evolution and construct bolometric light curves, and find peak luminosities of 0.5 5 10 44 ( -) ergs −1 and lower limits on the total radiated energies of 0.3 2 10 51 ( -) erg. The light curve shapes are diverse, with both rise and decline times spanning a factor of ∼5 and several examples of double-peaked light curves. When correcting for the flux-limited nature of our survey, we find a median peak luminosity at 4000Å of M 21.1 mag 4000 = -and a spread of 0.7 mag s = .

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Host-Galaxy Properties of 32 Low-Redshift Superluminous Supernovae From the Palomar Transient Factory

Cited by 248 publications

References 140 publications

The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system

The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system

The Host Galaxy and Redshift of the Repeating Fast Radio Burst FRB 121102

Hydrogen-poor Superluminous Supernovae from the Pan-STARRS1 Medium Deep Survey

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