bluuebunny/crossref_metadata_2025_split huggingface dataset:
A simple relationship for the spectro-temporal structure of bursts from FRB 121102
Authors: Rajabi Fereshteh , Chamma Mohammed A , Wyenberg Christopher M , Mathews Abhilash , Houde Martin 
Published: September 2020

ABSTRACT
We consider a simple dynamical and relativistic model to explain the spectro-temporal structure often displayed by repeating fast radio bursts (FRBs). We show how this model can account for the downward frequency drift in a sequence of sub-bursts of increasing arrival time (the ‘sad trombone’ effect) and their tendency for exhibiting a reduced pulse width with increasing frequency of observation. Most importantly, this model also predicts a systematic inverse relationship between the (steeper) slope of the frequency drift observed within a single sub-burst and its temporal duration. Using already published data for FRB 121102, we find and verify the relationship predicted by this model. We therefore argue that the overall behaviour observed for this object as a function of frequency is consistent with an underlying narrow-band emission process, where the wide-band nature of the measured FRB spectrum is due to relativistic motions. Although this scenario and the simple dynamics we consider could be applied to other theories, they are well suited for a model based upon Dicke’s superradiance as the physical process responsible for FRB radiation in this and similar sources.
On-sky measurements of atmospheric dispersion – I. Method validation
Authors: Wehbe B , Cabral A , Ávila G 
Published: September 2020

ABSTRACT
Observations with ground-based telescopes are affected by differential atmospheric dispersion due to the wavelength-dependent index of refraction of the atmosphere. The usage of an atmospheric dispersion corrector (ADC) is fundamental to compensate this effect. Atmospheric dispersion correction residuals above the level of ∼100 milliarcseconds (mas) will affect astronomical observations, in particular radial velocity and flux losses. The design of an ADC is based on atmospheric models. To the best of our knowledge, those models have never been tested on-sky. In this paper, we present a new method to measure the atmospheric dispersion on-sky in the optical range. We require an accuracy better than 50 mas that is equal to the difference between atmospheric models. The method is based on the use of cross-dispersion spectrographs to determine the position of the centroid of the spatial profile at each wavelength of each spectral order. The method is validated using cross-dispersed spectroscopic data acquired with the slit spectrograph UVES. We measure an instrumental dispersion of $\rm 47 ~ mas$ in the blue arm, and 15 and 23 mas in the two ranges of the red arm. We also measure a 4 per cent deviation in the pixel scale from the value cited in UVES manual. The accuracy of the method is ∼17 mas in the range of 315–665 nm. At this level, we can compare and characterize different atmospheric dispersion models for better future ADC designs.
CHIMPS2: survey description and 12CO emission in the Galactic Centre
Authors: Eden D J , Moore T J T , Currie M J , Rigby A J , Rosolowsky E , Su Y , Kim Kee-Tae , Parsons H , Morata O , Chen H-R , Minamidani T , Park Geumsook , Ragan S E , Urquhart J S , Rani R , Tahani K , Billington S J , Deb S , Figura C , Fujiyoshi T , Joncas G , Liao L W , Liu T , Ma H , Tuan-Anh P , Yun Hyeong-Sik , Zhang S , Zhu M , Henshaw J D , Longmore S N , Kobayashi M I N , Thompson M A , Ao Y , Campbell-White J , Ching T-C , Chung E J , Duarte-Cabral A , Fich M , Gao Y , Graves S F , Jiang X-J , Kemper F , Kuan Y-J , Kwon W , Lee C W , Lee J-E , Liu M , Peñaloza C H , Peretto N , Phuong N T , Pineda J E , Plume R , Puspitaningrum E , Samal M R , Soam A , Sun Y , Tang X D , Traficante A , White G J , Yan C-H , Yang A Y , Yuan J , Yue N , Bemis A , Brunt C M , Chen Z , Cho J , Clark P C , Cyganowski C J , Friberg P , Fuller G A , Han I , Hoare M G , Izumi N , Kim H-J , Kim J , Kim S , Koch E W , Kuno N , Lacialle K M , Lai S-P , Lee H , Lee Y-H , Li D L , Liu S-Y , Mairs S , Pan Z , Qian L , Scicluna P , Shi C-S , Shi H , Srinivasan S , Tan Q-H , Thomas H S , Torii K , Trejo A , Umemoto T , Violino G , Wallström S , Wang B , Wu Y , Yuan L , Zhang C , Zhang M , Zhou C , Zhou J J 
Published: September 2020

ABSTRACT
The latest generation of Galactic Plane surveys is enhancing our ability to study the effects of galactic environment upon the process of star formation. We present the first data from CO Heterodyne Inner Milky Way Plane Survey 2 (CHIMPS2). CHIMPS2 is a survey that will observe the Inner Galaxy, the Central Molecular Zone (CMZ), and a section of the Outer Galaxy in 12CO, 13CO, and C18O $(J = 3\rightarrow 2)$ emission with the Heterodyne Array Receiver Program on the James Clerk Maxwell Telescope (JCMT). The first CHIMPS2 data presented here are a first look towards the CMZ in 12CO J = 3 → 2 and cover ${-}3^{\circ }\, \le \, \ell \, \le \, 5^{\circ }$ and $\mid {b} \mid \, \le \, 0{_{.}^{\circ}} 5$ with angular resolution of 15 arcsec, velocity resolution of 1 km s−1, and rms $\Delta \, T_A ^\ast =$ 0.58 K at these resolutions. Such high-resolution observations of the CMZ will be a valuable data set for future studies, whilst complementing the existing Galactic Plane surveys, such as SEDIGISM, the ${Herschel}$ infrared Galactic Plane Survey, and ATLASGAL. In this paper, we discuss the survey plan, the current observations and data, as well as presenting position–position maps of the region. The position–velocity maps detect foreground spiral arms in both absorption and emission.
Removing imaging systematics from galaxy clustering measurements with Obiwan: application to the SDSS-IV extended Baryon Oscillation Spectroscopic Survey emission-line galaxy sample
Authors: Kong Hui , Burleigh Kaylan J , Ross Ashley , Moustakas John , Chuang Chia-Hsun , Comparat Johan , de Mattia Arnaud , du Mas des Bourboux Hélion , Honscheid Klaus , Lin Sichen , Raichoor Anand , Rossi Graziano , Zhao Cheng 
Published: September 2020

ABSTRACT
This work presents the application of a new tool, Obiwan, which uses image simulations to determine the selection function of a galaxy redshift survey and calculate three-dimensional (3D) clustering statistics. Obiwan relies on a forward model of the process by which images of the night sky are transformed into a 3D large-scale structure catalogue, and offers several advantages over more traditional map-based techniques – such as operating on individual exposures and adopting a maximum likelihood approach. The photometric pipeline automatically detects and models galaxies and then generates a catalogue of such galaxies with detailed information for each one of them, including their location, redshift, and so on. Systematic biases in the imaging data are therefore imparted into the catalogues and must be accounted for in any scientific analysis of their information content. Obiwan simulates this process for samples selected from the Legacy Surveys imaging data. This imaging data will be used to select target samples for the next-generation Dark Energy Spectroscopic Instrument (DESI) experiment. Here, we apply Obiwan to a portion of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey emission-line galaxies (ELGs). Systematic biases in the data are clearly identified and removed. We compare the 3D clustering results to those obtained by the map-based approach applied to the complete eBOSS Data Release 16 (DR16) sample. We find the results are consistent, thereby validating the eBOSS DR16 ELG catalogues, which is used to obtain cosmological results.
Dissecting the turbulent weather driven by mechanical AGN feedback
Authors: Wittor D , Gaspari M 
Published: September 2020

ABSTRACT
Turbulence in the intracluster, intragroup, and circumgalactic medium plays a crucial role in the self-regulated feeding and feedback loop of central supermassive black holes. We dissect the 3D turbulent ‘weather’ in a high-resolution Eulerian simulation of active galactic nucleus (AGN) feedback, shown to be consistent with multiple multiwavelength observables of massive galaxies. We carry out post-processing simulations of Lagrangian tracers to track the evolution of enstrophy, a proxy of turbulence, and its related sinks and sources. This allows us to isolate in depth the physical processes that determine the evolution of turbulence during the recurring strong and weak AGN feedback events, which repeat self-similarly over the Gyr evolution. We find that the evolution of enstrophy/turbulence in the gaseous halo is highly dynamic and variable over small temporal and spatial scales, similar to the chaotic weather processes on Earth. We observe major correlations between the enstrophy amplification and recurrent AGN activity, especially via its kinetic power. While advective and baroclinc motions are always subdominant, stretching motions are the key sources of the amplification of enstrophy, in particular along the jet/cocoon, while rarefactions decrease it throughout the bulk of the volume. This natural self-regulation is able to preserve, as ensemble, the typically observed subsonic turbulence during cosmic time, superposed by recurrent spikes via impulsive anisotropic AGN features (wide outflows, bubbles, cocoon shocks). This study facilitates the preparation and interpretation of the thermo-kinematical observations enabled by new revolutionary X-ray integral field unit telescopes, such as XRISM and Athena.
Leveraging HST with MUSE – I. Sodium abundance variations within the 2-Gyr-old cluster NGC 1978
Authors: Saracino S , Kamann S , Usher C , Bastian N , Martocchia S , Lardo C , Latour M , Cabrera-Ziri I , Dreizler S , Giesers B , Husser T-O , Kacharov N , Salaris M 
Published: September 2020

ABSTRACT
Nearly all of the well-studied ancient globular clusters (GCs), in the Milky Way and in nearby galaxies, show star-to-star variations in specific elements (e.g. He, C, N, O, Na, and Al), known as ‘multiple populations’ (MPs). However, MPs are not restricted to ancient clusters, with massive clusters down to ∼2 Gyr showing signs of chemical variations. This suggests that young and old clusters share the same formation mechanism but most of the work to date on younger clusters has focused on N variations. Initial studies even suggested that younger clusters may not host spreads in other elements beyond N (e.g. Na), calling into question whether these abundance variations share the same origin as in the older GCs. In this work, we combine Hubble Space Telescope (HST) photometry with Very Large Telescope (VLT)/Multi-Unit Spectroscopic Explorer (MUSE) spectroscopy of a large sample of red giant branch (RGB) stars (338) in the Large Magellanic Cloud cluster NGC 1978, the youngest globular to date with reported MPs in the form of N spreads. By combining the spectra of individual RGB stars into N-normal and N-enhanced samples, based on the ‘chromosome map’ derived from HST, we search for mean abundance variations. Based on the NaD line, we find a Na difference of Δ[Na/Fe] = 0.07 ± 0.01 between the populations. While this difference is smaller than typically found in ancient GCs (which may suggest a correlation with age), this result further confirms that the MP phenomenon is the same, regardless of cluster age and host galaxy. As such, these young clusters offer some of the strictest tests for theories on the origin of MPs.
Discovery of thermonuclear (Type I) X-ray bursts in the X-ray binary Swift J1858.6–0814 observed with NICER and NuSTAR
Authors: Buisson D J K , Altamirano D , Bult P , Mancuso G C , Güver T , Jaisawal G K , Hare J , Albayati A C , Arzoumanian Z , Castro Segura N , Chakrabarty D , Gandhi P , Guillot S , Homan J , Gendreau K C , Jiang J , Malacaria C , Miller J M , Özbey Arabacı M , Remillard R , Strohmayer T E , Tombesi F , Tomsick J A , Vincentelli F M , Walton D J 
Published: September 2020

ABSTRACT
Swift J1858.6–0814 is a recently discovered X-ray binary notable for extremely strong variability (by factors of &gt;100 in soft X-rays) in its discovery state. We present the detection of five thermonuclear (Type I) X-ray bursts from Swift J1858.6–0814, implying that the compact object in the system is a neutron star (NS). Some of the bursts show photospheric radius expansion, so their peak flux can be used to estimate the distance to the system. The peak luminosity, and hence distance, can depend on several system parameters; for the most likely values, a high inclination and a helium atmosphere, $D=12.8_{-0.6}^{+0.8}$ kpc, although systematic effects allow a conservative range of 9–18 kpc. Before one burst, we detect a QPO at 9.6 ± 0.5 mHz with a fractional rms amplitude of 2.2 ± 0.2 per cent (0.5–10 keV), likely due to marginally stable burning of helium; similar oscillations may be present before the other bursts but the light curves are not long enough to allow their detection. We also search for burst oscillations but do not detect any, with an upper limit in the best case of 15 per cent fractional amplitude (over 1–8 keV). Finally, we discuss the implications of the NS accretor and this distance on other inferences which have been made about the system. In particular, we find that Swift J1858.6–0814 was observed at super-Eddington luminosities at least during bright flares during the variable stage of its outburst.
Assessing cosmic acceleration with the Alcock–Paczyński effect in the SDSS-IV quasar catalogue
Authors: Melia Fulvio , Qin Jin , Zhang Tong-Jie 
Published: September 2020

ABSTRACT
The geometry of the Universe may be probed using the Alcock–Paczyński (AP) effect, in which the observed redshift size of a spherical distribution of sources relative to its angular size varies according to the assumed cosmological model. Past applications of this effect have been limited, however, by a paucity of suitable sources and mitigating astrophysical factors, such as internal redshift-space distortions and poorly known source evolution. In this Letter, we introduce a new test based on the AP effect that avoids the use of spatially bound systems, relying instead on sub-samples of quasars at redshifts z ≲ 1.5 in the Sloan Digital Sky Survey IV, with a possible extension to higher redshifts and improved precision when this catalogue is expanded by upcoming surveys. We here use this method to probe the redshift-dependent expansion rate in three pertinent Friedmann–Lemaître–Robertson–Walker cosmologies: Λ cold dark matter (ΛCDM), which predicts a transition from deceleration to acceleration at z ∼ 0.7; Einstein–de Sitter, in which the Universe is always decelerating; and the Rh = ct universe, which expands at a constant rate. ΛCDM is consistent with these data, but Rh = ct is favoured overall.
Background for gravitational wave signal at LISA from refractive index of solar wind plasma
Authors: Smetana Adam 
Published: September 2020

ABSTRACT
A strong indication is presented that the space-based gravitational antennas, in particular the Laser Interferometer Space Antenna (LISA) concept introduced in 2017 in response to the ESA call for L3 mission concepts, are going to be sensitive to a strong background signal interfering with the prospected signal of gravitational waves. The false signal is due to variations in the electron number density of the solar wind, causing variations in the refractive index of plasma flowing through interplanetary space. As countermeasures, two solutions are proposed. The first solution is to deploy enough solar wind detectors to the LISA mission to allow for reliable knowledge of the solar wind background. The second solution is to equip the LISA interferometer with a second laser beam with a distinct wavelength to allow cancelling of the background solar wind signal from the interferometric data.
UV spectroscopy confirms SU Lyn to be a symbiotic star
Authors: Kumar Vipin , Srivastava Mudit K , Banerjee Dipankar P K , Joshi Vishal 
Published: September 2020

ABSTRACT
SU Lyn, a star that ostensibly appears to be an unremarkable late M type giant, has recently been proposed to be a symbiotic star largely based on its hard X-ray properties. The star does not display, in low-resolution optical spectra, the high excitation lines typically seen in the spectra of symbiotic stars. In this work, ultraviolet (UV), optical, and near-infrared observations are presented, aimed at exploring and strengthening the proposed symbiotic classification for this star. Our far-UV 1300–1800 Å spectrum of SU Lyn, obtained with the ASTROSAT mission’s UVIT payload, shows emission lines of Si iv, C iv, O iii, and N iii in a spectrum typical of symbiotic stars. The UV spectrum robustly confirms SU Lyn’s symbiotic nature. The detection of high excitation lines in a high-resolution optical spectrum further consolidates its symbiotic nature. As is being recognized, the potential existence of other similar symbiotic systems could significantly impact the census of symbiotic stars in the Galaxy.
Racial, Ethnic, and Geographic Disparities in Novel Coronavirus (Severe Acute Respiratory Syndrome Coronavirus 2) Test Positivity in North Carolina
Authors: Turner Nicholas A , Pan William , Martinez-Bianchi Viviana S , Panayotti Gabriela M Maradiaga , Planey Arrianna M , Woods Christopher W , Lantos Paul M 
Published: September 2020

Abstract

Background
Emerging evidence suggests that black and Hispanic communities in the United States are disproportionately affected by coronavirus disease 2019 (COVID-19). A complex interplay of socioeconomic and healthcare disparities likely contribute to disproportionate COVID-19 risk.

Methods
We conducted a geospatial analysis to determine whether individual- and neighborhood-level attributes predict local odds of testing positive for severe acute respiratory syndrome coronavirus 2 (SARS-CoV-2). We analyzed 29 138 SARS-CoV-2 tests within the 6-county catchment area for Duke University Health System from March to June 2020. We used generalized additive models to analyze the spatial distribution of SARS-CoV-2 positivity. Adjusted models included individual-level age, gender, and race, as well as neighborhood-level Area Deprivation Index, population density, demographic composition, and household size.

Results
Our dataset included 27 099 negative and 2039 positive unique SARS-CoV-2 tests. The odds of a positive SARS-CoV-2 test were higher for males (odds ratio [OR], 1.43; 95% credible interval [CI], 1.30–1.58), blacks (OR, 1.47; 95% CI, 1.27–1.70), and Hispanics (OR, 4.25; 955 CI, 3.55–5.12). Among neighborhood-level predictors, percentage of black population (OR, 1.14; 95% CI, 1.05–1.25), and percentage Hispanic population (OR, 1.23; 95% CI, 1.07–1.41) also influenced the odds of a positive SARS-CoV-2 test. Population density, average household size, and Area Deprivation Index were not associated with SARS-CoV-2 test results after adjusting for race.

Conclusions
The odds of testing positive for SARS-CoV-2 were higher for both black and Hispanic individuals, as well as within neighborhoods with a higher proportion of black or Hispanic residents—confirming that black and Hispanic communities are disproportionately affected by SARS-CoV-2.
Effectiveness of Ultrasound-Guided Percutaneous Electrolysis for Musculoskeletal Pain: A Systematic Review and Meta-Analysis
Authors: Gómez-Chiguano Guido F , Navarro-Santana Marcos J , Cleland Joshua A , Arias-Buría Jose L , Fernández-de-las-Peñas César , Ortega-Santiago Ricardo , Plaza-Manzano Gustavo 
Published: September 2020

AbstractObjectiveTo evaluate the effects of ultrasound-guided percutaneous electrolysis alone or as an adjunct to other interventions on pain and pain-related disability for musculoskeletal pain conditions.Databases and Data TreatmentSearch of MEDLINE database, Allied and Complementary Medicine Database, EMBASE database, Cumulative Index to Nursing & Allied Health Literature database, EBSCO database, PubMed database, Physiotherapy Evidence Database, Cochrane Library database, Scopus database, and Web of Science database. Randomized controlled trials in which at least one group received ultrasound-guided percutaneous electrolysis for treatment of musculoskeletal pain. To be eligible, studies had to include humans and collect outcomes on pain intensity and pain-related disability for musculoskeletal pain syndromes. Data were extracted by two reviewers. The risk of bias was assessed by the Cochrane Guidelines and the quality of evidence was reported using the Grading of Recommendations Assessment, Development and Evaluation approach. Standardized mean differences (SMDs) and random effects were calculated.ResultsTen studies were included. The meta-analysis found that ultrasound-guided percutaneous electrolysis reduced the mean pain intensity by –2.06 (95% confidence interval [CI], –2.69 to –1.42) and the pain intensity as assessed with a visual analog scale or a numeric pain rating scale with a large size effect (SMD = –1.15; 95% CI, –1.48 to –0.81) and also improved pain-related disability with a large size effect (SMD = 0.95; 95% CI, 0.73–1.18) as compared with comparison groups. No differences in effect sizes were found among the short-term, midterm, and long-term follow-ups. The risk of bias was generally low, but the heterogeneity of the overall result downgraded the evidence level. Trials included heterogeneous musculoskeletal pain conditions and short-term, midterm, and long-term follow-ups.ConclusionModerate evidence suggests positive effects of ultrasound-guided percutaneous electrolysis for pain and pain-related disability in musculoskeletal pain conditions relative to a comparison group in the short term, midterm, and long term.
An Interventional Pain Algorithm for the Treatment of Postmastectomy Pain Syndrome: A Single-Center Retrospective Review
Authors: Yang Ajax , Nadav Danielle , Legler Aron , Chen Grant H , Hingula Lee , Puttanniah Vinay , Gulati Amitabh 
Published: September 2020

AbstractObjectiveBreast cancer is the most common female malignancy worldwide. Breast surgery and adjuvant oncological therapies are often required to increase survival. Treatment-related pain may persist and evolve into postmastectomy pain syndrome (PMPS) in a significant subset of breast cancer survivors. In this retrospective investigation, we will present our experience in applying an interventional algorithmic approach to treat PMPS.DesignA retrospective study.SettingAn academic cancer hospital.SubjectsAdult females with PMPS diagnosis.MethodsWe reviewed 169 records with the diagnosis of PMPS from 2015 to 2019 within our health system. Pre- and post-injection pain scores, relief duration, and medication usage changes were collected. The decision to perform each procedure was based on the anatomic location of the painful area with the corresponding peripheral sensory innervation. Decision-making flow diagrams were created to present our experience in managing PMPS beyond peripheral nerve blocks.ResultsUltrasound-guided peripheral nerve block results (n=350) were analyzed. The mean baseline pain score was 7, compared with the post-treatment mean score of 3 (95% confidence interval: 3.58 to 3.98, P = 0.0001). Among the responders, the mean pain relief duration was 45 days, with a median of 84 days. Opioid medication consumption was reduced by 11% (t = 0.72, P = 0.47).ConclusionsUltrasound-guided nerve blocks of this area could be performed safely and effectively after breast surgeries. We also present our proposed algorithm to provide a stepwise application for selecting the appropriate therapies in the management of more complex PMPS.