The Radio Luminosity-risetime Function of Core-collapse Supernovae

Bietenholz, M. F.; Bartel, N.; Argo, M. K.; Dua, R.; Ryder, S. D.; Söderberg, A. M.

doi:10.3847/1538-4357/abccd9

Cited by 49 publications

(66 citation statements)

References 125 publications

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“…The 10 GHz light curve peaks at f ν = 0.180 ± 0.023 mJy, or L 10 GHz = (3.4 ± 0.4) × 10 29 erg s −1 Hz −1 . This is more luminous than any observed core-collapse supernova (Bietenholz et al 2021), but typical for events like AT2018cow (Ho et al 2019a;Margutti et al 2019;Ho et al 2020c;Coppejans et al 2020). The time to peak of t pk ≈ 60 d is common for core-collapse supernovae (Bietenholz et al 2021).…”

Section: Observationsmentioning

confidence: 77%

Luminous Millimeter, Radio, and X-ray Emission from ZTF20acigmel (AT2020xnd)

Ho,

Margalit,

Bremer

et al. 2021

Preprint

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We present millimeter (80-230 GHz), radio (6-45 GHz), and X-ray (0.2-10 keV) observations of ZTF20acigmel (AT2020xnd), a short-duration luminous optical transient at z = 0.2433. The 100 GHz peak luminosity is similar to that of long-duration gamma-ray bursts (2 × 10 30 erg s −1 Hz −1 ) but the light curve rises on a much longer timescale (one month). In the standard framework of synchrotron self-absorption of electrons in a power-law energy distribution, the data imply a fast (v ≈ 0.2c) shock with large energy (U 10 49 erg) propagating in a medium with a steep (n e ∝ r −3 ) density profile. The forward-shock properties are similar to those of the fast-luminous transient AT2018cow, and in both cases the model for the late-time (∆t > 70 d) low-frequency (ν < 40 GHz) data is not consistent with the early-time (∆t < 40 d) high-frequency (ν > 70 GHz) emission. Motivated by the observation of a steep spectral index (f ν ∝ ν −2 ) across the millimeter bands, we favor a thermal electron population (relativistic Maxwellian) for the synchrotron emission, the first such inference for a cosmic explosion. We find that the X-ray luminosity of L X ≈ 10 43 erg s −1 exceeds simple predictions from the radio and UVOIR luminosity and likely has a separate physical origin, such as a central engine. Our work suggests that luminous millimeter, radio, and X-ray emission are a generic feature of transients with fast (≈ 3 d) and luminous (M ≈ −21 mag) optical light curves. We estimate the rate at which transients like AT2018cow and AT2020xnd will be detected by future wide-field millimeter transient surveys like CMB-S4, and conclude that energetic explosions in dense environments may represent a significant population of extragalactic transients in the 100 GHz sky.

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Section: Observationsmentioning

confidence: 77%

Luminous Millimeter, Radio, and X-ray Emission from ZTF20acigmel (AT2020xnd)

Ho,

Margalit,

Bremer

et al. 2021

Preprint

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“…The rise in energy could be due to a sustained injection of energy from the central engine (accreting SMBH), or to a rapid initial ejection but with a spread of velocities. The latter effect is apparent in Type Ib/c SNe and in some long GRBs (Laskar et al 2014(Laskar et al , 2015Margutti et al 2014;Bietenholz et al 2021). In the case of AT 2019dsg since the velocity is roughly constant the more likely explanation for the increase in energy is continued injection due to sustained accretion onto the SMBH.…”

Section: Outflow Velocity and Kinetic Energymentioning

confidence: 88%

Radio Observations of an Ordinary Outflow from the Tidal Disruption Event AT2019dsg

Cendes,

Alexander,

Berger

et al. 2021

Preprint

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We present detailed radio observations of the tidal disruption event (TDE) AT2019dsg, obtained with the Very Large Array (VLA) and the Atacama Large Millimeter/submillimeter Array (ALMA), and spanning 55−560 days post-disruption. We find that the peak brightness of the radio emission increases until ∼ 200 days and subsequently begins to decrease steadily. Using the standard equipartition analysis, including the effects of synchrotron cooling as determined by the joint VLA-ALMA spectral energy distributions, we find that the outflow powering the radio emission is in roughly free expansion with a velocity of ≈ 0.07c, while its kinetic energy increases by a factor of about 5 from 55 to 200 days and plateaus at ≈ 5 × 10 48 erg thereafter. The ambient density traced by the outflow declines as ≈ R −1.6 on a scale of ≈ (1 − 4) × 10 16 cm (≈ 6300 − 25000 R s ), followed by a steeper decline to ≈ 6 × 10 16 cm (≈ 37500 R s ). Allowing for a collimated geometry, we find that to reach even mildly relativistic velocities (Γ = 2) the outflow requires an opening angle of θ j ≈ 2 • , which is narrow even by the standards of GRB jets; a truly relativistic outflow requires an unphysically narrow jet. The outflow velocity and kinetic energy in AT2019dsg are typical of previous non-relativistic TDEs, and comparable to those from Type Ib/c supernovae, raising doubts about the claimed association with a high-energy neutrino event.

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“…Radio emission related to active star-formation throughout the galaxy can be excluded through VLBI measurements or constraints on the star-formation rate (Ravi et al 2021;Fong et al 2021). The PRS luminosity limit also excludes all known typed supernovae (relativistic explosions such as SN Ic-BL are also excluded; Bietenholz et al 2021). However, this luminosity limit includes rare and extremely luminous radio tran-2 Millisecond radio transients undergo a frequency-dependent time delay as they propagate through ionized gas.…”

Section: Frb and Prs Populationsmentioning

confidence: 99%

On the Fast Radio Burst and Persistent Radio Source Populations

Law,

Connor,

Aggarwal

2021

Preprint

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The first Fast Radio Burst (FRB) to be precisely localized was associated with a luminous persistent radio source (PRS). Recently, a second FRB/PRS association was discovered for another repeating source of FRBs. However, it is not clear what makes FRBs or PRS or how they are related. We compile FRB and PRS properties to consider the population of FRB/PRS sources. We suggest a practical definition for PRS as FRB associations with luminosity greater than 10 29 erg s −1 Hz −1 that is not attributed to star-formation activity in the host galaxy. We model the probability distribution of the fraction of FRBs with PRS for repeaters and non-repeaters, showing there is not yet evidence for repeaters to be preferentially associated with PRS. We discuss how FRB/PRS sources may be distinguished by the combination of active repetition and an excess dispersion measure local to the FRB environment. We use CHIME/FRB event statistics to bound the mean per-source repetition rate of FRBs to be between 25 and 440 yr −1 . We use this to provide a bound on the density of FRB-emitting sources in the local universe of between 2.2 × 10 2 and 5.2 × 10 4 Gpc −3 assuming a pulsar-like beam width for FRB emission. This density implies that PRS may comprise as much as 1% of compact, luminous radio sources detected in the local universe. The cosmic density and phenomenology of PRS are similar to that of the newly-discovered, off-nuclear "wandering" AGN. We argue that it is likely that some PRS have already been detected and misidentified as AGN.

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The Radio Luminosity-risetime Function of Core-collapse Supernovae

Cited by 49 publications

References 125 publications

Luminous Millimeter, Radio, and X-ray Emission from ZTF20acigmel (AT2020xnd)

Luminous Millimeter, Radio, and X-ray Emission from ZTF20acigmel (AT2020xnd)

Radio Observations of an Ordinary Outflow from the Tidal Disruption Event AT2019dsg

On the Fast Radio Burst and Persistent Radio Source Populations

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