VLBI observations of SN 2008iz

Brunthaler, A.; Martí-Vidal, Iván; Menten, K. M.; Reid, M. J.; Henkel, C.; Bower, Geoffrey C.; Falcke, H.; Feng, Hua; Kaaret, Philip; Butler, N.; Morgan, A. N.; Weiß, A.

doi:10.1051/0004-6361/201014133

Cited by 36 publications

(53 citation statements)

References 40 publications

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“…Its CCSN rate is estimated to be ∼ð2.1 − 20Þ × 10 −2 CCSNe yr −1 [118,119]. The most recent CCSN in M82 was SN2008iz, a Type II SN first observed on May 3, 2008 [120].…”

Section: A Location Of Snementioning

confidence: 99%

Observing gravitational waves from core-collapse supernovae in the advanced detector era

et al. 2016

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The next galactic core-collapse supernova (CCSN) has already exploded, and its electromagnetic (EM) waves, neutrinos, and gravitational waves (GWs) may arrive at any moment. We present an extensive study on the potential sensitivity of prospective detection scenarios for GWs from CCSNe within 5 Mpc, using realistic noise at the predicted sensitivity of the Advanced LIGO and Advanced Virgo detectors for 2015, 2017, and 2019. We quantify the detectability of GWs from CCSNe within the Milky Way and Large Magellanic Cloud, for which there will be an observed neutrino burst. We also consider extreme GW emission scenarios for more distant CCSNe with an associated EM signature. We find that a three-detector network at design sensitivity will be able to detect neutrino-driven CCSN explosions out to ∼5.5 kpc, while rapidly rotating core collapse will be detectable out to the Large Magellanic Cloud at 50 kpc. Of the phenomenological models for extreme GW emission scenarios considered in this study, such as long-lived bar-mode instabilities and disk fragmentation instabilities, all models considered will be detectable out to M31 at 0.77 Mpc, while the most extreme models will be detectable out to M82 at 3.52 Mpc and beyond.

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“…Its CCSN rate is estimated to be ∼ð2.1 − 20Þ × 10 −2 CCSNe yr −1 [118,119]. The most recent CCSN in M82 was SN2008iz, a Type II SN first observed on May 3, 2008 [120].…”

Section: A Location Of Snementioning

confidence: 99%

Observing gravitational waves from core-collapse supernovae in the advanced detector era

et al. 2016

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“…A fraction of supernovae, however, will be missed in optical surveys due to strong dust extinction. Indeed, a supernova SN 2008iz in M82 is discovered only in the radio bands (Brunthaler et al 2009(Brunthaler et al , 2010. Even if associated supernovae are not identifiable, they can be distinguished from merger events using timescale arguments, which are significantly longer than those of GW-radio counterparts, and radio spectral properties.…”

Section: False Positives: Extragalactic Radio Transients and Variablesmentioning

confidence: 99%

Radio Counterparts of Compact Binary Mergers Detectable in Gravitational Waves: A Simulation for an Optimized Survey

Hotokezaka

Nissanke

Hallinan

et al. 2016

ApJ

113

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Mergers of binary neutron stars and black hole-neutron star binaries produce gravitational-wave(GW) emission and outflows with significant kinetic energies. These outflows result in radio emissions through synchrotron radiation. We explore the detectability of these synchrotron-generated radio signals by follow-up observations of GW merger events lacking a detection of electromagnetic counterparts in other wavelengths. We model radio light curves arising from (i) sub-relativistic merger ejecta and (ii) ultra-relativistic jets. The former produce radio remnants on timescales of a few years and the latter produce γ-ray bursts in the direction of the jet and orphan-radio afterglows extending over wider angles on timescales of weeks. Based on the derived light curves, we suggest an optimized survey at 1.4 GHz with five epochs separated by a logarithmic time interval. We estimate the detectability of the radio counterparts of simulated GW-merger events to be detected by advanced LIGO and Virgo by current and future radio facilities. The detectable distances for these GW merger events could be as high as 1 Gpc. Around 20%-60% of the long-lasting radio remnants will be detectable in the case of the moderate kinetic energy of 3 10 50 · erg and a circum-merger density of -0.1 cm 3 or larger, while 5%-20% of the orphan-radio afterglows with kinetic energy of 10 48 erg will be detectable. The detection likelihood increases if one focuses on the well-localizable GW events. We discuss the background noise due to radio fluxes of host galaxies and false positives arising from extragalactic radio transients and variable activegalacticnuclei, and we show that the quiet radio transient sky is of great advantage when searching for the radio counterparts.

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“…Radio very long baseline interferometry studies of the innermost regions of LIRGs have, in fact, revealed scores of radio SNe and supernova (SN) remnants that have remained hidden at other wavelengths (Lonsdale et al 2006;Pérez-Torres et al 2009;Ulvestad 2009;Bondi et al 2012;Herrero-Illana et al 2012;Romero-Cañizales et al 2012). A few bona fide radio transients have also been identified as obscured SNeII, e.g., an SN in the starburst Galaxy Mrk297 (Yin & Heeschen 1991), VLA 121550.2+130654 (Gal-Yam et al 2006), and SN2008iz in M82 (A V > 10 mag ;Brunthaler et al 2009Brunthaler et al , 2010Mattila et al 2013).…”

Section: Introductionmentioning

confidence: 99%

SPIRITS 15c and SPIRITS 14buu: Two Obscured Supernovae in the Nearby Star-forming Galaxy IC 2163

Jencson

Kasliwal

Johansson

et al. 2017

ApJ

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SPitzer InfraRed Intensive Transients Survey-SPIRITS-is an ongoing survey of nearby galaxies searching for infrared (IR) transients with Spitzer/IRAC. We present the discovery and follow-up observations of one of our most luminous (M . Pre-discovery ground-based imaging revealed an associated, shorter-duration transient in the optical and near-IR (NIR). NIR spectroscopy showed a broad (≈8400 km s −1 ), double-peaked emission line of HeI at 1.083 μm, indicating an explosive origin. The NIR spectrum of SPIRITS 15c is similar to that of the Type IIb SN2011dh at a phase of ≈200days. Assuming an A V =2.2 mag of extinction in SPIRITS 15c provides a good match between their optical light curves. The NIR light curves, however, show some minor discrepancies when compared with SN2011dh, and the extreme [3.6]-[4.5] color has not been previously observed for any SNIIb. Another luminous (M 4.5 = −16.1 ± 0.4 mag) event, SPIRITS 14buu, was serendipitously discovered in the same galaxy. The source displays an optical plateau lasting 80days, and we suggest a scenario similar to the low-luminosity TypeIIP SN2005cs obscured by A V ≈1.5 mag. Other classes of IR-luminous transients can likely be ruled out in both cases. If both events are indeed SNe, this may suggest that 18% of nearby core-collapse SNe are missed by currently operating optical surveys.

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VLBI observations of SN 2008iz

Cited by 36 publications

References 40 publications

Observing gravitational waves from core-collapse supernovae in the advanced detector era

Observing gravitational waves from core-collapse supernovae in the advanced detector era

Radio Counterparts of Compact Binary Mergers Detectable in Gravitational Waves: A Simulation for an Optimized Survey

SPIRITS 15c and SPIRITS 14buu: Two Obscured Supernovae in the Nearby Star-forming Galaxy IC 2163

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