Search for gravitational-wave transients associated with magnetar bursts in advanced LIGO and advanced Virgo data from the third observing run

Gravitational waves are expected to be produced from neutron star oscillations associated with magnetar giant f lares and short bursts. We present the results of a search for short-duration (milliseconds to seconds) and longduration (∼100 s) transient gravitational waves from 13 magnetar short bursts observed during Advanced LIGO, Advanced Virgo, and KAGRA’s third observation run. These 13 bursts come from two magnetars, SGR1935 +2154 and SwiftJ1818.0−1607. We also include three other electromagnetic burst events detected by FermiGBM which were identified as likely coming from one or more magnetars, but they have no association with a known magnetar. No magnetar giant flares were detected during the analysis period. We find no evidence of gravitational waves associated with any of these 16 bursts. We place upper limits on the rms of the integrated incident gravitational-wave strain that reach 3.6 × 10−²³ Hz at 100 Hz for the short-duration search and 1.1 ×10−²² Hz at 450 Hz for the long-duration search. For a ringdown signal at 1590 Hz targeted by the short-duration search the limit is set to 2.3 × 10−²² Hz. Using the estimated distance to each magnetar, we derive upper limits upper limits on the emitted gravitational-wave energy of 1.5 × 1044 erg (1.0 × 1044 erg) for SGR 1935+2154 and 9.4 × 10^43 erg (1.3 × 1044 erg) for Swift J1818.0−1607, for the short-duration (long-duration) search. Assuming isotropic emission of electromagnetic radiation of the burst fluences, we constrain the ratio of gravitational-wave energy to electromagnetic energy for bursts from SGR 1935+2154 with the available fluence information. The lowest of these ratios is 4.5 × 103

Open data from the third observing run of LIGO, Virgo, KAGRA, and GEO

The global network of gravitational-wave observatories now includes five detectors, namely LIGO Hanford, LIGO Livingston, Virgo, KAGRA, and GEO 600. These detectors collected data during their third observing run, O3, composed of three phases: O3a starting in 2019 April and lasting six months, O3b starting in 2019 November and lasting five months, and O3GK starting in 2020 April and lasting two weeks. In this paper we describe these data and various other science products that can be freely accessed through the Gravitational Wave Open Science Center at https://gwosc.org. The main data set, consisting of the gravitational-wave strain time series that contains the astrophysical signals, is released together with supporting data useful for their analysis and documentation, tutorials, as well as analysis software packages

A joint Fermi-GBM and Swift-BAT analysis of gravitational-wave candidates from the third gravitational-wave observing run

We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) searches for gamma-ray/X-ray counterparts to gravitational-wave (GW) candidate events identified during the third observing run of the Advanced LIGO and Advanced Virgo detectors. Using Fermi-GBM onboard triggers and subthreshold gamma-ray burst (GRB) candidates found in the Fermi-GBM ground analyses, the Targeted Search and the Untargeted Search, we investigate whether there are any coincident GRBs associated with the GWs. We also search the Swift-BAT rate data around the GW times to determine whether a GRB counterpart is present. No counterparts are found. Using both the Fermi-GBM Targeted Search and the Swift-BAT search, we calculate flux upper limits and present joint upper limits on the gamma-ray luminosity of each GW. Given these limits, we constrain theoretical models for the emission of gamma rays from binary black hole mergers

Constraints on the cosmic expansion history from GWTC–3

We use 47 gravitational wave sources from the Third LIGO–Virgo–Kamioka Gravitational Wave Detector Gravitational Wave Transient Catalog (GWTC–3) to estimate the Hubble parameter H(z), including its current value, the Hubble constant H0. Each gravitational wave (GW) signal provides the luminosity distance to the source, and we estimate the corresponding redshift using two methods: the redshifted masses and a galaxy catalog. Using the binary black hole (BBH) redshifted masses, we simultaneously infer the source mass distribution and H(z). The source mass distribution displays a peak around 34 M⊙, followed by a drop-off. Assuming this mass scale does not evolve with the redshift results in a H(z) measurement, yielding ${H}_{0}={68}_{-8}^{+12}\,\mathrm{km}\ \,\ {{\rm{s}}}^{-1}\,{\mathrm{Mpc}}^{-1}$ (68% credible interval) when combined with the H0 measurement from GW170817 and its electromagnetic counterpart. This represents an improvement of 17% with respect to the H0 estimate from GWTC–1. The second method associates each GW event with its probable host galaxy in the catalog GLADE+, statistically marginalizing over the redshifts of each event's potential hosts. Assuming a fixed BBH population, we estimate a value of ${H}_{0}={68}_{-6}^{+8}\,\mathrm{km}\ \,\ {{\rm{s}}}^{-1}\,{\mathrm{Mpc}}^{-1}$ with the galaxy catalog method, an improvement of 42% with respect to our GWTC–1 result and 20% with respect to recent H0 studies using GWTC–2 events. However, we show that this result is strongly impacted by assumptions about the BBH source mass distribution; the only event which is not strongly impacted by such assumptions (and is thus informative about H0) is the well-localized event GW190814

Nitrergic, peptidergic and substance P innervation of the chick thymus.

Journal für Hirnforschung384553-56

Study on Mycelial Growth Pattern of Five Wild Pleurotus Species from North West India

In the present paper five wild Pleurotus species viz., P. floridanus (Sing.)., P. pulmonarius (Fr.) Quél., P. sapidus Quél., P. cystidiosus O.K.Mill. and P. sajor-caju (Fr.) Sing., collected, identified and isolated from different regions of North West India to study the behavior of culture on solid medium (Potato Dextrose Agar). On the daily basis observations, all the species exhibited different growth characteristics with respect to growth rate, odor and colour. It was observed that among the five cultures the fastest growth was observed in Pleurotus cystidiosus (1.3 cm/day) on an average daily basis followed by Pleurotus pulmonarius (1.23 cm/day), P. sajor - caju (1.2 cm/day), P. sapidus (1.1 cm/day) and P. floridanus (0.8 cm/day) which has the slowest growth rate observed among all the species on an average daily basis. During the entire growth stage the colour of the mycelium remained white. A specialized feature among all the species was observed in P. cystidiosus with the formation of specialized black headed structure called coremia. Coremia formation started in the form of small protuberances on the entire tissue simultaneously. Initially tiny watery droplets having blackish color appeared on the white stalk which after 3 days of protuberance. Mycelial mat was observed to thin at initial stages but later on changing to thick. In all the species the hyphal construction was found to be monomitic having generative hyphae with prominent clamps. All the studied species emitted scented smel

Characterization of solid state forms of glipizide

In the present study various crystalline forms of glipizide were prepared in order to enhance dissolution rate of glipizide and to evaluate the stability of developed forms. Four different strategies have been followed to prepare crystalline forms of glipizide – a. crystallization from the methanolic solution of the drug under pH control b. crystallization by vapor diffusion c. crystallization by antisolvent precipitation technique and, d. quench cooling. It could be deciphered from the study of DSC, SEM, PXRD and Raman spectroscopic analysis that six different crystal forms of glipizide (form I, form II, form III, form IV, form V and form VI) were prepared. Among all crystalline forms, the fastest T50% drug release was observed with form III and form V (i.e. within 10 min). However, T50% drug release was not observed in case of pure glipizide even till 90 min Among all the crystal forms prepared, it was concluded that form V (JMD-7) prepared by diffusing vapors of chloroform in the saturated solution of glipizide in methanol could be considered the best due to its rapid dissolution rate (T50% is 10 min), considerably higher extent of dissolution (Q90 is 87.22%) and better stability (F2 value 65.39 between dissolution profiles of fresh and aged form V). Further, the dissolution profile (F2 = 75), PXRD pattern and DSC thermograms of form V of glipizide converted in capsule dosage form were found similar as that of glipizide powder (form V). This justifies that the manufacturing process will not change the dissolution rate or chemical properties of the difference forms of API

Second-order multiobjective symmetric duality with cone constraints

In this paper, we formulate Wolfe and Mond-Weir type second-order multiobjective symmetric dual problems over arbitrary cones. Weak, strong and converse duality theorems are established under [eta]-bonvexity/[eta]-pseudobonvexity assumptions. This work also removes several omissions in definitions, models and proofs for Wolfe type problems studied in Mishra [9]. Moreover, self-duality theorems for these pairs are obtained assuming the function involved to be skew symmetric.Multiobjective symmetric duality [eta]-bonvexity/[eta]-pseudobonvexity Cones Efficient solutions Properly efficient solutions