Discovery of a bright radio transient in M 82:  a new radio supernova?

Brunthaler, A.; Menten, K. M.; Reid, M. J.; Henkel, C.; Bower, Geoffrey C.; Falcke, H.

doi:10.1051/0004-6361/200912327

Cited by 63 publications

(85 citation statements)

References 34 publications

(48 reference statements)

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“…We adopt a distance of the Sun from the Galactic Center  = R 8300 pc (Brunthaler et al 2011). 9 Recent estimates of  z range between +6 pc and +30 pc (Joshi et al 2016).…”

Section: Components Of the Modelmentioning

confidence: 99%

A New Electron-Density Model for Estimation of Pulsar and FRB Distances

Yao¹,

Manchester²,

Wang³

2017

ApJ

1,021

997

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We present a new model for the distribution of free electrons in the Galaxy, the Magellanic Clouds, and the intergalactic medium (IGM) that can be used to estimate distances to real or simulated pulsars and fast radio bursts (FRBs) based on their dispersion measure (DM). The Galactic model has an extended thick disk representing the so-called warm interstellar medium, a thin disk representing the Galactic molecular ring, spiral arms based on a recent fit to Galactic H II regions, a Galactic Center disk, and seven local features including the Gum Nebula, Galactic Loop I, and the Local Bubble. An offset of the Sun from the Galactic plane and a warp of the outer Galactic disk are included in the model. Parameters of the Galactic model are determined by fitting to 189 pulsars with independently determined distances and DMs. Simple models are used for the Magellanic Clouds and the IGM. Galactic model distances are within the uncertainty range for 86 of the 189 independently determined distances and within 20% of the nearest limit for a further 38 pulsars. We estimate that 95% of predicted Galactic pulsar distances will have a relative error of less than a factor of 0.9. The predictions of YMW16 are compared to those of the TC93 and NE2001 models showing that YMW16 performs significantly better on all measures. Timescales for pulse broadening due to interstellar scattering are estimated for (real or simulated) Galactic and Magellanic Cloud pulsars and FRBs.

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“…We adopt a distance of the Sun from the Galactic Center  = R 8300 pc (Brunthaler et al 2011). 9 Recent estimates of  z range between +6 pc and +30 pc (Joshi et al 2016).…”

Section: Components Of the Modelmentioning

confidence: 99%

A New Electron-Density Model for Estimation of Pulsar and FRB Distances

Yao¹,

Manchester²,

Wang³

2017

ApJ

1,021

997

View full text Add to dashboard Cite

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“…These two conditions allow one to separate the proper motion from the parallax signature. Each observation lasted 12 h and made use of geodetic-like observing blocks to calibrate the tropospheric zenith delays at each antenna (see Reid & Brunthaler 2004;Brunthaler et al 2005;Reid et al 2009a, for a detailed discussion).…”

Section: Evn Methanol Maser Observationsmentioning

confidence: 99%

Parallaxes and proper motions of interstellar masers toward the Cygnus X star-forming complex

Rygl

Brunthaler

Sanna

et al. 2012

A&A

Self Cite

318

322

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Context. Whether the Cygnus X complex consists of one physically connected region of star formation or of multiple independent regions projected close together on the sky has been debated for decades. The main reason for this puzzling scenario is the lack of trustworthy distance measurements. Aims. We aim to understand the structure and dynamics of the star-forming regions toward Cygnus X by accurate distance and proper motion measurements. Methods. To measure trigonometric parallaxes, we observed 6.7 GHz methanol and 22 GHz water masers with the European VLBI Network and the Very Long Baseline Array. Results. We measured the trigonometric parallaxes and proper motions of five massive star-forming regions toward the Cygnus X complex and report the following distances within a 10% accuracy: 1.30 +0.07 −0.07 kpc for W 75N, 1.46 +0.09 −0.08 kpc for DR 20, 1.50 +0.08 −0.07 kpc for DR 21, 1.36 +0.12 −0.11 kpc for IRAS 20290+4052, and 3.33 +0.11 −0.11 kpc for AFGL 2591. While the distances of W 75N, DR 20, DR 21, and IRAS 20290+4052 are consistent with a single distance of 1.40 ± 0.08 kpc for the Cygnus X complex, AFGL 2591 is located at a much greater distance than previously assumed. The space velocities of the four star-forming regions in the Cygnus X complex do not suggest an expanding Strömgren sphere.

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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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Discovery of a bright radio transient in M 82: a new radio supernova?

Cited by 63 publications

References 34 publications

A New Electron-Density Model for Estimation of Pulsar and FRB Distances

A New Electron-Density Model for Estimation of Pulsar and FRB Distances

Parallaxes and proper motions of interstellar masers toward the Cygnus X star-forming complex

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

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