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Abstract Fast X-ray transients (FXTs) are a new observational class of phenomena with no clear physical origin. This is at least partially a consequence of limited multiwavelength follow-up of this class of transients in real time. Here we present deep optical (g- andi-band) photometry with Keck, and prompt radio observations with the Very Large Array of FXT 210423 obtained atδt≈ 14–36 days since the X-ray trigger. We use these multiband observations, combined with publicly available data sets, to constrain the presence and physical properties of on-axis and off-axis relativistic jets such as those that can be launched by neutron star mergers and tidal disruption events, which are among the proposed theoretical scenarios of FXTs. Considering a wide range of possible redshiftsz≤ 3.5, circumstellar medium densityn= 10⁻⁶–10⁻¹cm⁻³, and isotropic-equivalent jet kinetic energyE_k,iso= 10⁴⁸–10⁵⁵erg, we find that we can rule out wide jets with opening angleθ_j= 15° viewed within 10° off-axis. For more collimated jets (θ_j= 3°) we can only rule out on-axis (θ_obs= 0°) orientations. This study highlights the constraining power of prompt multiwavelength observations of FXTs discovered in real time by current (e.g., Einstein Probe) and future facilities. 

Student reflections and using individual development plans (IDPs) for mentoring have been an integral part of an NSF S-STEM project focusing on students pursuing baccalaureate degrees in Engineering Technology (ET). The Engineering Technology Scholars – IMProving Retention and Student Success (ETS-IMPRESS) project provides financial support and offers students several high-impact curricular and co-curricular activities to increase the success of academically talented students. This interdisciplinary project brings together the Electrical Engineering Technology, and Computer Network and System Administration programs in the College of Computing and the College of Engineering’s Mechanical Engineering Technology program, with programs in the Pavlis Honors College, an inclusive and unique college designed around high-impact educational practices. An IDP is commonly used in business and industry to assist employees in meeting short- and long-term goals in their professional career. This tool has been adapted for use in the educational setting in a faculty mentoring capacity. The ET program advisors assign the freshman or transfer S-STEM student scholars with faculty mentors to match their area of research interest. The faculty mentors meet with the students a minimum of three to four times a year to review their IDP, make suggestions, and provide input for reaching their goals. The goals of the IDP process are to develop a deeper more meaningful relationship between the advisor and student, reflect and develop a strategy for the scholar’s educational and career success, and manage expectations and identify opportunities. In the initial meeting there are several prompts for the student to write about their goals, strengths, weaknesses and perceived challenges. In subsequent meetings the advisor and student revisit the IDP to discuss progress towards those goals. This study will describe some outcomes of the IDP process providing specific examples from each of the ET programs. Although it is difficult to measure the effect of these relationships, it is one of the high impact practices that have been noted as increasing student engagement and retention. The consequences of COVID-19 introducing a virtual environment to the IDP process will also be examined from the viewpoint of both student and advisor. An advantage of the IDP meetings for students is that advisors may provide personal business connections for internship opportunities and/or research projects that otherwise would not be discussed in a typical office hour or classroom session. One of the innovations of the ETS-IMPRESS program was requiring participation in the Honors Pathway Program, which generally emphasizes intrinsic motivation (and does not use GPA in admissions or awarding of credentials). The honors program consists of three seminar classes and four experiential components; for all of these, students write reflections designed to promote their development of self-authorship. Preliminary survey results show no difference between ETS and other honors students in the areas of student motivation, intention to persist, and professional skill development. ETS students see a closer link between their current major and their future career than non-ETS honors students. A comparative analysis of reflections will investigate students’ perceptions of the program’s effect. 

Abstract Among known neutron stars, the Vela pulsar is one of the best targets for gravitational-wave searches. It is also one of the most prolific in terms of glitches, which are sudden frequency changes in a pulsar’s rotation. Such glitches could cause a variety of transient gravitational-wave signals. Here, we search for signals associated with a Vela glitch on 2024 April 29 in data of the two LIGO detectors from the fourth LIGO–Virgo–KAGRA observing run. We search both for seconds-scale burst-like emission, primarily from fundamental (f-)mode oscillations, and for longer quasi-monochromatic transients up to 4 months in duration, primarily from quasi-static quadrupolar deformations. We find no significant detection candidates, but for the first time we set direct observational upper limits on gravitational strain amplitude that are stricter than what can be indirectly inferred from the overall glitch energy scale. We discuss the short- and long-duration observational constraints in the context of specific emission models. These results demonstrate the potential of gravitational-wave probes of glitching pulsars as detector sensitivity continues to improve. 

Abstract Version 4.0 of the Gravitational-Wave Transient Catalog (GWTC-4.0) adds new candidates detected by the LIGO, Virgo, and KAGRA observatories through the first part of the fourth observing run (O4a: 2023 May 24 15:00:00 to 2024 January 16 16:00:00 UTC) and a preceding engineering run. In these new data, we find 128 compact binary coalescence candidates that are identified by at least one of our search algorithms with a probability of astrophysical originp_astro≥ 0.5 and that are not vetoed during event validation. We also provide detailed source property measurements for 86 of these that have a false-alarm rate <1 yr⁻¹. Based on the inferred component masses, these candidates are consistent with signals from binary black holes (BBHs) and neutron star–black hole binaries (GW230518_125908 and GW230529_181500). Median-inferred component masses of BBHs in the catalog now range from 5.79M⊙ (GW230627_015337) to 137 $M_{\odot }$(GW231123_135430), while GW231123_135430 was probably produced by the most massive binary observed in the catalog. For the first time, we have discovered BBH signals with network signal-to-noise ratio exceeding 30, GW230814_230901 and GW231226_101520, enabling high-fidelity studies of the waveforms and astrophysical properties of these systems. Combined with the 90 candidates included in GWTC-3.0, the catalog now contains 218 candidates withp_astro≥ 0.5 and not otherwise vetoed, more than doubling the size of the catalog and further opening our view of the gravitational-wave Universe. 

Abstract LIGO, Virgo, and KAGRA form a network of gravitational-wave observatories. Data and analysis results from this network are made publicly available through the Gravitational Wave Open Science Center. This paper describes open data from this network, including the addition of data from the first part of the fourth observing run and selected periods from the preceding engineering run, collected from 2023 May to 2024 January. The public dataset includes calibrated strain time series for each instrument, data from additional channels used for noise subtraction and detector characterization, and analysis data products from version 4.0 of the Gravitational-Wave Transient Catalog. 

Abstract GW230814, detected by the LIGO Livingston observatory with a signal-to-noise ratio of 42.4, represents the loudest gravitational-wave signal in the GWTC-4.0 catalog. Its source is consistent with a binary black hole coalescence with component masses $m_1=33.7_{-2.2}^{+2.9}{M}_{\odot }$and $m_2=28.2_{-3.1}^{+2.2}{M}_{\odot }$and a small effective inspiral spin ${\chi }_{\mathrm{eff}}=-0.01_{-0.07}^{+0.06}$. The high signal-to-noise ratio enabled us to detect anℓ = ∣m∣ = 4 mode in the inspiral–merger–ringdown signal for the first time (with Bayes factor ≈10), as well as enabling a range of tests of consistency between theoretical predictions and the observed waveform. While most of these tests show agreement with theoretical predictions, there are suggestions of minor deviations in the ringdown phase. Simulations that incorporate general relativity and realistic detector noise reproduce similar deviations, suggesting that they do not constitute evidence for a breakdown of general relativity. The observation of GW230814 demonstrates that the unprecedented sensitivity of the detectors enables highly significant detections with a single observatory. However, without corroborating data from a multidetector network, the ability to draw rigorous conclusions about fundamental physics remains severely limited. 

Abstract The Gravitational-Wave Transient Catalog (GWTC) is a collection of candidate gravitational-wave transient signals identified and characterized by the LIGO–Virgo–KAGRA Collaboration. Producing the contents of the GWTC from detector data requires complex analysis methods. These comprise techniques to model the signal; identify the transients in the data; evaluate the quality of the data and mitigate possible instrumental issues; infer the parameters of each transient; compare the data with the waveform models for compact binary coalescences; and handle the large amount of results associated with all of these different analyses. In this paper, we describe the methods employed to produce the catalog’s fourth release, GWTC-4.0, focusing on the analysis of the first part of the fourth observing run of Advanced LIGO, Advanced Virgo and KAGRA. 

Abstract We present results from directed searches for continuous gravitational waves from a sample of 15 nearby supernova remnants, likely hosting young neutron star candidates, using data from the first eight months of the fourth observing run (O4) of the LIGO–Virgo–KAGRA Collaboration. The analysis employs five pipelines: four semicoherent methods—the Band-Sampled-Data directed pipeline, Weave, and two Viterbi pipelines (single- and dual-harmonic)—and PyStoch, a cross-correlation-based pipeline. These searches cover wide frequency bands and do not assume prior knowledge of the targets’ ephemerides. No evidence of a signal is found from any of the 15 sources. We set 95% confidence-level upper limits on the intrinsic strain amplitude, with the most stringent constraints reaching ∼4 × 10⁻²⁶near 300 Hz for the nearby source G266.2−1.2 (Vela Jr.). We also derive limits on neutron star ellipticity andr-mode amplitudes for the same source, with the best constraints reaching ≲10⁻⁷and ≲10⁻⁵, respectively, at frequencies above 400 Hz. For frequencies above 200 Hz, these results represent the most sensitive wide-band directed searches for continuous gravitational waves from supernova remnants to date. 

Background A better understanding of the pathophysiology involving coronary artery calcification (CAC) in patients on hemodialysis (HD) will help to develop new therapies. We sought to identify the differences in metabolomics profiles between patients on HD with and without CAC. Methods In this case-control study, nested within a cohort of 568 incident patients on HD, the cases were patients without diabetes with a CAC score >100 ( n =51), and controls were patients without diabetes with a CAC score of zero ( n =48). We measured 452 serum metabolites in each participant. Metabolites and pathway scores were compared using Mann–Whitney U tests, partial least squares–discriminant analyses, and pathway enrichment analyses. Results Compared with controls, cases were older (64±13 versus 42±12 years) and were less likely to be Black (51% versus 94%). We identified three metabolites in bile-acid synthesis (chenodeoxycholic, deoxycholic, and glycolithocholic acids) and one pathway (arginine/proline metabolism). After adjusting for demographics, higher levels of chenodeoxycholic, deoxycholic, and glycolithocholic acids were associated with higher odds of having CAC; comparing the third with the first tertile of each bile acid, the OR was 6.34 (95% CI, 1.12 to 36.06), 6.73 (95% CI, 1.20 to 37.82), and 8.53 (95% CI, 1.50 to 48.49), respectively. These associations were no longer significant after further adjustment for coronary artery disease and medication use. Per 1 unit higher in the first principal component score, arginine/proline metabolism was associated with CAC after adjusting for demographics (OR, 1.83; 95% CI, 1.06 to 3.15), and the association remained significant with additional adjustments for statin use (OR, 1.84; 95% CI, 1.04 to 3.27). Conclusions Among patients on HD without diabetes mellitus, chenodeoxycholic, deoxycholic, and glycolithocholic acids may be potential biomarkers for CAC, and arginine/proline metabolism is a plausible mechanism to study for CAC. These findings need to be confirmed in future studies.