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Abstract Rotating nonaxisymmetric neutron stars (NSs) are promising sources for continuous gravitational waves (CWs). CWs may, if detected, inform us about the internal structure and equation of state of NSs. Here, we present a narrowband search for CWs from known pulsars, for which a matched-filter search can be applied. Narrowband searches are robust to mismatches between electromagnetic (EM) and gravitational emissions, in contrast to fully targeted searches where they are assumed to be phase-locked. In this work, we search for the CW counterparts emitted by 34 pulsars using data from the first and second parts of the fourth LIGO–Virgo–KAGRA observing run. We use the 5n-vector narrowband pipeline, which applies frequency-domain matched filtering. In previous searches, it covered a narrow range in the frequency—frequency time derivative (f— $\dot{f}$) space. Here, we also explore a range in the second time derivative of the frequency $\ddot{f}$around the EM observations. Additionally, for the first time, we target sources in a binary system with this kind of search. We find no evidence for CWs and therefore set upper limits on the strain amplitude emitted by each pulsar. For 20 analyses, we report an upper limit below the theoretical spin-down limit. The tightest constraint is for pulsar PSR J0534+2200 (the Crab pulsar), for which our strain upper limit on the CW amplitude corresponds to ≤0.04% of the spin-down power being radiated in the CW channel. 

Abstract We detail the population properties of binary neutron star, neutron star–black hole binary, and binary black hole mergers using 158 events from the cumulative Gravitational-Wave Transient Catalog 4.0. The black hole primary mass distribution consists of a power-law-like continuum that steepens above 35M_⊙with overdensities at 10M_⊙and 35M_⊙. Binary black holes with primary masses near 10M_⊙are more likely to have less massive secondaries, with a mass ratio distribution peaking at $q=0.71_{-0.11}^{+0.12}$, potentially a signature of stable mass transfer during binary evolution. Black hole spins are inferred to be nonextremal, with 90% of black holes havingχ < 0.6, and preferentially aligned with binary orbits, implying many merging binaries form in isolation. However, we find that a significant fraction, 0.23–0.41, of binaries have negative effective inspiral spins, suggesting many could be formed dynamically in gas-free environments. We find evidence for correlation between effective inspiral spin and mass ratio, driven either by variation in the mode of the distribution or the width. The binary black hole merger rate increases with redshift, consistent with the cosmic star formation density. While there is no evidence of the mass spectrum evolving with redshift, the distribution of effective inspiral spin is found to broaden as redshift increases out toz ≈ 1. We infer the local merger rates (atz= 0) to be 8.8–250 Gpc⁻³yr⁻¹for binary neutron stars, 9.3–86 Gpc⁻³yr⁻¹for neutron star–black hole binaries, and 13–26 Gpc⁻³yr⁻¹for binary black holes; all values reflect central 90% credible intervals. 

In literature, Nocardia cholesterolicum NRRL 5767 (NC NRRL5767) is well-known for its ability to transform ~95% of added oleic acid, an abundant agricultural commodity, to value-added product of 10-hydroxystearic acid (10-HSA). A small amount of unwanted 10-ketostearic acid (10-KSA) was also produced. This microbe also transforms ~80% of added linoleic acid to 10-hydroxy-12(Z)-octadecenoic acid (10-OH-12-OD) (an isomer of ricinoleic acid) with minor 10-oxo-12(Z)-octadecenoic acid (10-oxo-12-OD). The conversion of oleic acid to 10-HSA and then to 10-KSA (or linoleic acid to 10-OH-12-OD and then to 10-oxo-12-OD) is catalyzed by oleate hydratase and secondary alcohol dehydrogenase (2o-ADH), respectively. The objective of this project was to knockout the 2o-ADH gene in NC NRRL5767 so that the sole biotransformation product from oleic acid would be 10-HSA. Here, we report construction of CRISPR/Cas9/sgRNA chimeric plasmid that specifically target 5’ coding region of the 2o-ADH gene by Golden Gate Assembly. The construct was confirmed by DNA sequencing and transformed into NC NRRL 5767 via electroporation. The transformants were selected by apramycin resistance and screened for the presence of the target insert (crRNA) by PCR. The ability of the selected transformants to transform oleic acid to 10-HSA was screened by TLC and further confirmed by GC-MS. Our results showed that two of the transformants produced only 10-HSA with no detectable 10-KSA from oleic acid suggesting successful knockout of the 2o-ADH gene. Final confirmation came from the isolation of genomic DNA from these two transformants and the wild type NC NRRL5767 (used as DNA template) and using 17 primers (locate at different positions along the 2o-ADH gene and the 5’ upstream of this gene) for PCR. To our best knowledge, this is the first report to knockout the target gene in Nocardia species by CRISPR-Cas9 technology. 

The angular distribution of gravitational-wave power from persistent sources may exhibit anisotropies arising from the large-scale structure of the Universe. This motivates directional searches for astrophysical and cosmological gravitational-wave backgrounds, as well as continuous-wave emitters. We present results of such a search using data from the first observing run through the first portion of the fourth observing run of the LIGO-Virgo-KAGRA Collaborations. We apply gravitational-wave radiometer techniques to generate skymaps and search for both narrowband and broadband persistent gravitational-wave sources. Additionally, we use spherical harmonic decomposition to probe spatially extended sources. No evidence of persistent gravitational-wave signals is found, and we set the most stringent constraints to date on such emissions. For narrowband point sources, our sensitivity estimate to effective strain amplitude lies in the range $\left(0.03–8.4\right)\times {10}^{-24}$across all-sky and frequency range ( $20-160$) Hz. For targeted sources—Scorpius X-1, SN 1987A, the Galactic Center, Terzan 5, and NGC 6397—we constrain the strain amplitude with best limits ranging from $\sim 1.1\times {10}^{-25}$to $6.5\times {10}^{-24}$. For persistent broadband sources, we constrain the gravitational-wave flux $F_{\alpha ,\hat{n}}^{95\%,\mathrm{UL}}\left(25\mathrm{Hz}\right)<\left(0.008–5.5\right)\times {10}^{-8}\mathrm{erg}{\mathrm{cm}}^{-2}{\mathrm{s}}^{-1}{\mathrm{Hz}}^{-1}$, depending on the sky direction $\hat{n}$and spectral index $\alpha =0,2/3$, 3. Finally, for extended sources, we place upper limits on the angular power spectrum $C_{\ell }^{1/2}<\left(0.63–17\right)\times {10}^{-10}{\mathrm{sr}}^{-1}$. 

We present a search for gravitational waves from inspiraling, planetary-mass ultracompact binaries using data from the first part of the fourth observing run of LIGO, Virgo, and KAGRA. Finding no evidence of such systems, we determine the maximum distance reach for such objects and their merger rate densities. Then, we identify classes of primordial black hole mass distributions for which these rate limits can be translated into relevant constraints on the mass distribution of primordial black holes, assuming that they are all composed of dark matter, in the mass range $[{10}^{-6},{10}^{-3}]M_{\odot }$. Our constraints for the class of primordial black hole mass distribution functions $f\left(m\right)$we consider reach down to $f\left(m\right)\sim 0.1$. They are consistent with existing microlensing results in the planetary-mass range, provide a complementary probe to subsolar mass objects, and are publicly available [1].