Enhanced QRD-M algorithm for soft-output MIMO detection

Kim, Tae‐Kyoung; Kim, Hyun-Myung; Im, Gi-Hong

doi:10.1109/glocom.2012.6503669

Cited by 4 publications

(2 citation statements)

References 12 publications

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“…Optical and NIR magnitudes, not corrected for the Galactic reddening E B−V = 0.29 (Schlafly & Finkbeiner 2011), are reported in Table 2 (Online Material). These data supersede those published in Kuin et al (2012), Covino et al (2012), Gorosabel et al (2012), LaClyuze et al (2012, Meehan et al (2012), Im et al (2012), Cobb (2012),…”

Section: Observationssupporting

confidence: 76%

Colour variations in the GRB 120327A afterglow

Melandri

Covino

Zaninoni

et al. 2017

A&A

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Aims. We present a comprehensive temporal and spectral analysis of the long Swift GRB 120327A afterglow data to investigate the possible causes of the observed early time colour variations. Methods. We collected data from various instruments/telescopes in different bands (X-rays, ultra-violet, optical and near-infrared) and determined the shapes of the afterglow early-time light curves. We studied the overall temporal behaviour and the spectral energy distributions from early to late times. Results. The ultra-violet, optical, and near-infrared light curves can be modelled with a single power-law component between 200 and 2 × 10 4 s after the burst event. The X-ray light curve shows a canonical steep-shallow-steep behaviour, typical of long gamma-ray bursts. At early times a colour variation is observed in the ultra-violet/optical bands, while at very late times a hint of a re-brightening is visible. The observed early time colour change can be explained as a variation in the intrinsic optical spectral index, rather than an evolution of the optical extinction.

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Section: Observationssupporting

confidence: 76%

Colour variations in the GRB 120327A afterglow

Melandri

Covino

Zaninoni

et al. 2017

A&A

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“…Given these considerations and no readily available SFRs in the GLADE catalog, we consider the stellar mass to be proportional to the BNS merger rate for the target prioritization. Since the stellar mass was not available in the GLADE catalog at the time of the observations, we use K-band luminosity, which is known as a proxy for the stellar mass (e.g., Kim & Im 2012). The K-band luminosity is from the 2 Micron All-Sky Survey (2MASS) Extended Source Catalog (Jarrett et al 2000), and hence, many sources miss K-band luminosities.…”

Section: Gw Host Galaxy Candidate Selectionmentioning

confidence: 99%

Gravitational-wave Electromagnetic Counterpart Korean Observatory (GECKO): GECKO Follow-up Observation of GW190425

Paek,

Im,

Kim

et al. 2024

ApJ

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One of the keys to the success of multimessenger astronomy is the rapid identification of the electromagnetic wave counterpart, kilonova (KN), of the gravitational-wave (GW) event. Despite its importance, it is hard to find a KN associated with a GW event, due to a poorly constrained GW localization map and numerous signals that could be confused as a KN. Here, we present the Gravitational-wave Electromagnetic wave Counterpart Korean Observatory (GECKO) project, the GECKO observation of GW190425, and prospects of GECKO in the fourth observing run (O4) of the GW detectors. We outline our follow-up observation strategies during O3. In particular, we describe our galaxy-targeted observation criteria that prioritize based on galaxy properties. Armed with this strategy, we performed an optical and/or near-infrared follow-up observation of GW190425, the first binary neutron star merger event during the O3 run. Despite a vast localization area of 7460 deg2, we observed 621 host galaxy candidates, corresponding to 29.5% of the scores we assigned, with most of them observed within the first 3 days of the GW event. Ten transients were discovered during this search, including a new transient with a host galaxy. No plausible KN was found, but we were still able to constrain the properties of potential KNe using upper limits. The GECKO observation demonstrates that GECKO can possibly uncover a GW170817-like KN at a distance <200 Mpc if the localization area is of the order of hundreds of square degrees, providing a bright prospect for the identification of GW electromagnetic wave counterparts during the O4 run.

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Dual QR decomposition in K-best sphere detection for Internet of Things networks

Bokhari

Bhagyaveni

2017

Cluster Comput

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Enhanced QRD-M algorithm for soft-output MIMO detection

Cited by 4 publications

References 12 publications

Colour variations in the GRB 120327A afterglow

Colour variations in the GRB 120327A afterglow

Gravitational-wave Electromagnetic Counterpart Korean Observatory (GECKO): GECKO Follow-up Observation of GW190425

Dual QR decomposition in K-best sphere detection for Internet of Things networks

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