Raspodjela kapi tropskih kiša po veličini nad južnom Indijom

Drop size distributions (DSD) associated with tropical rainfall at Cuddalore in the south-eastern part of India have been measured by a Joss-Waldvogel disdrometer (RD–80 model) during September to November 2002. The rainfall data corrected for instrumental error, matches very well with rainfall rates measured by a self recording raingauge, at the same site. For further analysis of the DSD, the rainfall events were separated into convective and stratiform rainfall by an algorithm based on variation of DSD parameters. One rain event in the form of a squall line of 15 September 2002, was analysed in greater detail to investigate the validity of the classification scheme as well as to study the variation of the DSD parameters during the course of a rain event. It was observed that, the algorithm was robust and had quite good correspondence with other independent rainfall separation algorithms. During the rain event, at low rainrates, the convective phase of the rainfall event was marked by DSD spectra that have greater population of small droplets as compared to stratiform DSDs at the same rainrates. At higher rainrates, the convective regime is characterised by narrow spectra centred at higher diameters. At the transition region between convective and stratiform spectra, mixed large and small drop spectra are observed. Similar variation was also observed in the averaged drop spectra. In addition, the averaged spectra also reveal an equilibrium distribution of the drop population in DSDs at higher rainrates (>39 /hr) for diameter range (>1.91 mm) corresponding to nearly constant values of the slope of the distribution, the intercept and the mean mass diameter. The value of the shape parameter, which for small rainrates varies the same as the slope parameter, starts to increase with increasing rainrate as the other two parameters of the gamma distribution approach a constant value corresponding to equilibrium shape. The value of the intercept parameter is highest for low to moderate convective rainfall and decreases as the rainrate increases.Raspodjela kapi po veličini (RKV) koja je povezana s tropskim kišama u Cuddalore u jugoistočnom dijelu Indije, mjerena je Joss-Waldvogel disdrometrom (model RD-80) od rujna do studenog 2002. Mjerenja kiše su korigirana uvažavajući pogreške instrumenta te se vrlo dobro podudaraju s mjerenjima koja su dobivena automatskom kišomjernom postajom na istoj lokaciji. Radi daljnje analize RKV, količine oborine su podijeljene na konvektivnu i stratiformnu količinu oborine na temelju logaritma koji se zasniva na varijacijama RKV parametara. Jedan slučaj obilne kiše za vrijeme olujne pruge 15. rujna 2002. odabran je za detaljnu analizu radi ispitivanja valjanosti klasifikacijske sheme kao i za proučavanje promjena RKV parametara za vrijeme pomicanja olujne pruge. Pokazalo se da je algoritam robustan i da je imao dobro slaganje s drugim algoritmima za separaciju oborine. Tijekom ispitivanog slučaja, kod malih količina kiše, konvektivnu fazu oborine karakterizira izrazit RKV spektar koji ima veliki broj malih kapljica u odnosu na statiformnu RKV za istu količinu kiše. Za veće količine kiše, konvektivni režim karakterizira uzak spektar velikih kapljica. U području prijelaza između konvektivnog i stratiformnog spektra, uočeno je miješanje velikih i malih kapljica kiše. Slične promjene prisutne su i u spektru srednjih kapljica kiše. Srednji spektar također pokazuje ravnomjernu raspodjelu kapi RKV za veće količine kiše (>39/sat) promjera kapi (>1.91 mm) što odgovara skoro konstantnim vrijednostima nagiba distribucije, presjeka s ordinatnom osi i srednjeg promjera. Vrijednost parametra oblika, koji za male količine kiše varira isto kao i parametar nagiba, počinje se povećavati s povećanjem količine oborine kao i ostala dva parametra gama razdiobe dosežući konstantnu vrijednost koja odgovara ravnotežnom obliku. Vrijednost presjeka s ordinatnom osi je najviša za male ili umjerene konvektivne količine oborine i smanjuje se s povećanjem količine kiše

A Joint Fermi-GBM and LIGO/Virgo Analysis of Compact Binary Mergers from the First and Second Gravitational-wave Observing Runs

We present results from offline searches of Fermi Gamma-ray Burst Monitor (GBM) data for gamma-ray transients coincident with the compact binary coalescences observed by the gravitational-wave (GW) detectors Advanced LIGO and Advanced Virgo during their first and second observing runs. In particular, we perform follow-up for both confirmed events and low significance candidates reported in the LIGO/Virgo catalog GWTC-1. We search for temporal coincidences between these GW signals and GBM-triggered gamma-ray bursts (GRBs). We also use the GBM Untargeted and Targeted subthreshold searches to find coincident gamma-rays below the onboard triggering threshold. This work implements a refined statistical approach by incorporating GW astrophysical source probabilities and GBM visibilities of LIGO/Virgo sky localizations to search for cumulative signatures of coincident subthreshold gamma-rays. All search methods recover the short gamma-ray burst GRB 170817A occurring ~1.7 s after the binary neutron-star merger GW170817. We also present results from a new search seeking GBM counterparts to LIGO single-interferometer triggers. This search finds a candidate joint event, but given the nature of the GBM signal and localization, as well as the high joint false alarm rate of 1.1 × 10−6 Hz, we do not consider it an astrophysical association. We find no additional coincidences

GW190521: A Binary Black Hole Merger with a Total Mass of 150 M⊙

On May 21, 2019 at 03:02:29 UTC Advanced LIGO and Advanced Virgo observed a short duration gravitational-wave signal, GW190521, with a three-detector network signal-to-noise ratio of 14.7, and an estimated false-alarm rate of 1 in 4900 yr using a search sensitive to generic transients. If GW190521 is from a quasicircular binary inspiral, then the detected signal is consistent with the merger of two black holes with masses of 85+21−14  M⊙ and 66+17−18  M⊙ (90% credible intervals). We infer that the primary black hole mass lies within the gap produced by (pulsational) pair-instability supernova processes, with only a 0.32% probability of being below 65  M⊙. We calculate the mass of the remnant to be 142+28−16  M⊙, which can be considered an intermediate mass black hole (IMBH). The luminosity distance of the source is 5.3+2.4−2.6  Gpc, corresponding to a redshift of 0.82+0.28−0.34. The inferred rate of mergers similar to GW190521 is 0.13+0.30−0.11  Gpc−3 yr−1

Search for Gravitational Waves Associated with Gamma-Ray Bursts Detected by Fermi and Swift during the LIGO–Virgo Run O3a

We search for gravitational-wave transients associated with gamma-ray bursts (GRBs) detected by the Fermi and Swift satellites during the first part of the third observing run of Advanced LIGO and Advanced Virgo (2019 April 1 15:00 UTC–2019 October 1 15:00 UTC). A total of 105 GRBs were analyzed using a search for generic gravitational-wave transients; 32 GRBs were analyzed with a search that specifically targets neutron star binary mergers as short GRB progenitors. We find no significant evidence for gravitational-wave signals associated with the GRBs that we followed up, nor for a population of unidentified subthreshold signals. We consider several source types and signal morphologies, and report for these lower bounds on the distance to each GRB

Characterization of an Ionization Readout Tile for nEXO

A new design for the anode of a time projection chamber, consisting of a charge-detecting "tile", is investigated for use in large scale liquid xenon detectors. The tile is produced by depositing 60 orthogonal metal charge-collecting strips, 3~mm wide, on a 10~\si{\cm} $\times$ 10~\si{\cm} fused-silica wafer. These charge tiles may be employed by large detectors, such as the proposed tonne-scale nEXO experiment to search for neutrinoless double-beta decay. Modular by design, an array of tiles can cover a sizable area. The width of each strip is small compared to the size of the tile, so a Frisch grid is not required. A grid-less, tiled anode design is beneficial for an experiment such as nEXO, where a wire tensioning support structure and Frisch grid might contribute radioactive backgrounds and would have to be designed to accommodate cycling to cryogenic temperatures. The segmented anode also reduces some degeneracies in signal reconstruction that arise in large-area crossed-wire time projection chambers. A prototype tile was tested in a cell containing liquid xenon. Very good agreement is achieved between the measured ionization spectrum of a $^{207}$Bi source and simulations that include the microphysics of recombination in xenon and a detailed modeling of the electrostatic field of the detector. An energy resolution $\sigma/E$=5.5\% is observed at 570~\si{keV}, comparable to the best intrinsic ionization-only resolution reported in literature for liquid xenon at 936~V/\si{cm}.Comment: 18 pages, 13 figures, as publishe

Sensitivity and discovery potential of the proposed nEXO experiment to neutrinoless double beta decay

The next-generation Enriched Xenon Observatory (nEXO) is a proposed experiment to search for neutrinoless double beta ($0\nu\beta\beta$) decay in $^{136}$Xe with a target half-life sensitivity of approximately $10^{28}$ years using $5\times10^3$ kg of isotopically enriched liquid-xenon in a time projection chamber. This improvement of two orders of magnitude in sensitivity over current limits is obtained by a significant increase of the $^{136}$Xe mass, the monolithic and homogeneous configuration of the active medium, and the multi-parameter measurements of the interactions enabled by the time projection chamber. The detector concept and anticipated performance are presented based upon demonstrated realizable background rates.Comment: v2 as publishe

Differential effects of testosterone, dihydrotestosterone and estradiol on carotenoid deposition in an avian sexually selected signal

Recent studies have demonstrated that carotenoid-based traits are under the control of testosterone (T) by up-regulation of carotenoid carriers (lipoproteins) and/or tissue-specific uptake of carotenoids. T can be converted to dihydrotestosterone (DHT) and estradiol (E2), and variation in conversion rate may partly explain some contradictory findings in the literature. Moreover, most studies on the effect of T on sexual signals have focused on the male sex only, while in many species females show the same signal, albeit to a lesser extent. We studied the effects of T, DHT, and E2 treatment in male and female diamond doves Geopelia cuneata in which both sexes have an enlarged red eye ring, which is more pronounced in males. We first showed that this periorbital ring contains very high concentration of carotenoids, of which most are lutein esters. Both T and DHT were effective in enhancing hue, UV-chroma and size in both sexes, while E2 was ineffective. However, E2 dramatically increased the concentration of circulating lipoproteins. We conclude that in both sexes both color and size of the secondary sexual trait are androgen dependent. The action of androgens is independent of lipoproteins regulation. Potential mechanisms and their consequences for trade-off are discussed