bluuebunny/crossref_metadata_2025_split huggingface dataset:
Nosocomial COVID: the moral and clinical imperative for worldwide data collection and action
Authors: Junaid Fatima , Badrinath Padmanabhan 
Published: June 2022

Abstract
There is a wide disparity worldwide in data collection and sharing of rates of hospital-acquired coronavirus disease (COVID). There is an ethical imperative that such information is systematically gathered, distributed and acted on to reduce rates of this form of preventable and devastating transmission during a pandemic.
Spinal myxomas: review of a rare entity
Authors: Patel Sabina , Suji Trisha , Pang Graeme , Alg Varinder S , Visagan Ravindran , Reisz Zita , Lavrador Jose P , Kailaya-Vasan Ahilan , Grahovac Gordan 
Published: June 2022

Abstract
Intramuscular myxomas are rare, benign mesenchymal tumours, occurring predominantly in large skeletal muscles as large, slow-growing and painless masses. Spinal occurrence is rare, and may present incidentally, or diagnosed via localized symptoms secondary to local infiltration of surrounding structures. Differential diagnosis based on imaging includes sarcomas, meningiomas and lipomas. We discuss two contrasting cases presenting with well-circumscribed cystic paraspinal lesions indicative of an infiltrative tumour and discuss the radiological and histological differences that distinguish myxomas from similar tumours. Surgical resection of the tumour was performed in both cases, however one patient required surgical fixation due to bony erosion secondary to tumour infiltration. Immuno-histopathological analysis confirmed the diagnosis of a cellular myxoma. Follow up imaging at 6 months confirmed no symptomatic or tumour recurrence in both cases. Histological analysis is the definitive means for diagnosis to differentiate myxomas from other tumours. Recurrence is rare if full resection is achieved.
PyNAPLE: Lunar Surface Impact Crater Detection
Authors: Sheward D , Avdellidou C , Cook A , Sefton-Nash E , Delbo M , Cantarella B , Zanatta L 
Published: June 2022

ABSTRACT
In the last 20 yr, over 600 impact flashes have been documented on the lunar surface. This wealth of data presents a unique opportunity to study the meteoroid flux of the Earth–Moon environment, and in recent years the physical properties of the impactors. However, other than through serendipitous events, there has not been yet a systematic search and discovery of the craters associated to these events. Such a meteoroid-crater link would allow us to get insight into the crater formation via these live observations of collisions. Here, we present the pynaple (python NAC Automated Pair Lunar Evaluator) software pipeline for locating newly formed craters using the location and epoch of an observed impact flash. We present the first results from pynaple, having been implemented on the 2017-09-27 impact flash. A rudimentary analysis on the impact flash and linked impact crater is also performed, finding that the crater’s ejecta pattern indicates an impact angle between 10–30°, and although the rim-to-rim diameter of the crater is not resolvable in current LRO NAC images, using crater scaling laws we predict this diameter to be 24.1–55.3 m, and using ejecta scaling predict a diameter of 27.3–37.7 m. We discuss how pynaple will enable large scale analyses of sub-kilometer scale cratering rates and refinement of both scaling laws, and the luminous efficiency.
SIRIUS Project – IV. The formation history of the Orion Nebula Cluster driven by clump mergers
Authors: Fujii Michiko S , Wang Long , Hirai Yutaka , Shimajiri Yoshito , Kumamoto Jun , Saitoh Takayuki 
Published: June 2022

ABSTRACT
The Orion Nebula Cluster (ONC) is an excellent example for understanding the formation of star clusters. Recent studies have shown that ONC has three distinct age populations and anisotropy in velocity dispersions, which are key characteristics for understanding the formation history of the ONC. In this study, we perform a smoothed-particle hydrodynamics/N-body simulation of star cluster formation from a turbulent molecular cloud. In this simulation, stellar orbits are integrated using a high-order integrator without gravitational softening; therefore, we can follow the collisional evolution of star clusters. We find that hierarchical formation causes episodic star formation that is observed in the ONC. In our simulation, star clusters evolve due to mergers of subclumps. The mergers bring cold gas with the clumps into the forming cluster. This enhances the star formation in the cluster centre. The dense cold gas in the cluster centre continues to form stars until the latest time. This explains the compact distribution of the youngest stars observed in the ONC. Subclump mergers also contribute to the anisotropy in the velocity dispersions and the formation of runaway stars. However, the anisotropy disappears within 0.5 Myr. The virial ratio of the cluster also increases after a merger due to the runaways. These results suggest that the ONC recently experienced a clump merger. We predict that most runaways originated from the ONC have already been found, but walkaways have not.
The diversity of spiral galaxies explained
Authors: Frosst Matthew , Courteau Stéphane , Arora Nikhil , Stone Connor , Macciò Andrea V , Blank Marvin 
Published: June 2022

ABSTRACT
An extensive catalogue of spatially resolved galaxy rotation curves (RCs) and multiband optical light profiles for 1752 observed spiral galaxies is assembled to explore the drivers of diversity in galaxy structural parameters, RC shapes, and stellar mass profiles. Similar data were extracted from the ‘Numerical Investigation of a Hundred Astrophysical Objects’ galaxy simulations to identify any differences between observations and simulations. Several parameters, including the inner slope $\mathcal {S}$ of a RC, were tested for diversity. Two distinct populations are found in observed and simulated galaxies: (i) blue, low-mass spirals with stellar mass M⋆ ≲ 109.3 M⊙ and roughly constant $\mathcal {S}$; and (ii) redder, more massive and more diverse spirals with rapidly increasing $\mathcal {S}$. In all cases, the value of $\mathcal {S}$ seems equally contributed by the baryonic and non-baryonic (dark) matter. Diversity is shown to increase mildly with mass. Numerical simulations reproduce well most baryon-dominated galaxy parameter distributions, such as the inner stellar mass profile slope and baryonic scaling relations, but they struggle to match the full diversity of observed galaxy RCs (through $\mathcal {S}$) and most dark matter-dominated parameters. To reproduce observations, the error broadening of the simulation’s intrinsic spread of RC metrics would have to be tripled. The differences in various projections of observed and simulated scaling relations may reflect limitations of current subgrid physics models to fully capture the complex nature of galaxies. For instance, active galactic nuclei (AGNs) are shown to have a significant effect on the shapes of simulated RCs. The inclusion of AGN feedback brings simulated and observed inner RC shapes into closer agreement.
SDSS-IV MaNGA: Identification and multiwavelength properties of Type-1 AGN in the DR15 sample
Authors: Cortes-Suárez Edgar , Negrete C A , Hernández-Toledo H M , Ibarra-Medel H , Lacerna I 
Published: June 2022

ABSTRACT
We present a method to identify type-1 active galactic nuclei (AGNs) in the central 3 arcsec integrated spectra of galaxies in the MaNGA DR15 sample. It is based on flux ratios estimates in spectral bands flanking the expected h α broad component h αBC. The high signal-to-noise ratio obtained (mean S/N = 84) permits the identification of h αBC without prior subtraction of the host galaxy (HG) stellar component. A final sample of 47 type-1 AGN is reported out of 4700 galaxies at z &lt; 0.15. The results were compared with those from other methods based on the SDSS DR7 and MaNGA data. Detection of type-1 AGN in those works compared to our method goes from 26 per cent to 81 per cent. Spectral indexes were used to classify the type-1 AGN spectra according to different levels of AGN-HG contribution, finding 9 AGN-dominated, 14 intermediate, and 24 HG-dominated objects. Complementary data in NIR-MIR allowed us to identify type I AGN-dominated objects as blue and HG-dominated as red in the WISE colours. From NVSS and FIRST radio continuum data, we identify 5 HERGs (high-excitation radio galaxies) and 4 LERGs (low-excitation radio galaxies), three showing evidence of radio-jets in the FIRST maps. Additional X-ray data from ROSAT allowed us to build [O iii] and h αBC versus X-ray, NIR-MIR, and radio continuum diagrams, showing that L(h αBC) and L([O iii]) provide good correlations. The range in h αBC luminosity is wide 38 &lt; logL(h αBC) &lt; 44, with log FWHM(h αBC) ∼ 3–4, covering a range of Eddington ratios of −5.15 &lt; log Lbol/LEdd &lt; 0.70. Finally, we also identify and report ten possible changing-look AGN candidates.
Galaxy pairs in the Sloan Digital Sky Survey – XV. Properties of ionized outflows
Authors: Matzko William , Satyapal Shobita , Ellison Sara L , Sexton Remington O , Secrest Nathan J , Canalizo Gabriela , Blecha Laura , Patton David R , Scudder Jillian M 
Published: June 2022

ABSTRACT
Powerful outflows are thought to play a critical role in galaxy evolution and black hole growth. We present the first large-scale systematic study of ionized outflows in paired galaxies and post-mergers compared to a robust control sample of isolated galaxies. We isolate the impact of the merger environment to determine if outflow properties depend on merger stage. Our sample contains ∼4000 paired galaxies and ∼250 post-mergers in the local universe (0.02 ≤ z ≤ 0.2) from the Sloan Digital Sky Survey Data Release 7 (SDSS DR 7) matched in stellar mass, redshift, local density of galaxies, and [O iii] λ5007 luminosity to a control sample of isolated galaxies. By fitting the [O iii] λ5007 line, we find ionized outflows in ∼15 per cent of our entire sample. Outflows are much rarer in star-forming galaxies compared to active galactic nuclei (AGNs), and outflow incidence and velocity increase with [O iii] λ5007 luminosity. Outflow incidence is significantly elevated in the optical + mid-infrared selected AGN compared to purely optical AGN; over 60 per cent show outflows at the highest luminosities ($L_{\mathrm{[OIII]~\lambda 5007}}\, \gtrsim$ 1042 erg s−1), suggesting mid-infrared AGN selection favours galaxies with powerful outflows, at least for higher [O iii] λ5007 luminosities. However, we find no statistically significant difference in outflow incidence, velocity, and luminosity in mergers compared to isolated galaxies, and there is no dependence on merger stage. Therefore, while interactions are predicted to drive gas inflows and subsequently trigger nuclear star formation and accretion activity, when the power source of the outflow is controlled for, the merging environment has no further impact on the large-scale ionized outflows as traced by [O iii] λ5007.
Dark lenses through the dust: parallax microlensing events in the VVV
Authors: Kaczmarek Zofia , McGill Peter , Evans N Wyn , Smith Leigh C , Wyrzykowski Łukasz , Howil Kornel , Jabłońska Maja 
Published: June 2022

ABSTRACT
We use near-infrared photometry and astrometry from the VISTA Variables in the Via Lactea (VVV) survey to analyse microlensing events containing annual microlensing parallax information. These events are located in highly extincted and low-latitude regions of the Galactic bulge typically off-limits to optical microlensing surveys. We fit a catalogue of 1959 events previously found in the VVV and extract 21 microlensing parallax candidates. The fitting is done using nested sampling to automatically characterize the multimodal and degenerate posterior distributions of the annual microlensing parallax signal. We compute the probability density in lens mass-distance using the source proper motion and a Galactic model of disc and bulge deflectors. By comparing the expected flux from a main sequence lens to the baseline magnitude and blending parameter, we identify four candidates which have probability &gt;50 per cent that the lens is dark. The strongest candidate corresponds to a nearby (≈0.78 kpc), medium-mass ($1.46^{+1.13}_{-0.71} \ M_{\odot }$) dark remnant as lens. In the next strongest, the lens is located at heliocentric distance ≈5.3 kpc. It is a dark remnant with a mass of $1.63^{+1.15}_{-0.70} \ M_{\odot }$. Both of those candidates are most likely neutron stars, though possibly high-mass white dwarfs. The last two events may also be caused by dark remnants, though we are unable to rule out other possibilities because of limitations in the data. We are also demonstrating future possibilities of studying similar events with the Roman Space Telescopeby modelling a mock dataset of Roman photometry and astrometry for an event resembling our strongest candidate.
The Pristine survey – XVIII. C-19: tidal debris of a dark matter-dominated globular cluster?
Authors: Errani Raphaël , Navarro Julio F , Ibata Rodrigo , Martin Nicolas , Yuan Zhen , Aguado David S , Bonifacio Piercarlo , Caffau Elisabetta , González Hernández Jonay I , Malhan Khyati , Sánchez-Janssen Rubén , Sestito Federico , Starkenburg Else , Thomas Guillaume F , Venn Kim A 
Published: June 2022

ABSTRACT
The recently discovered C-19 stellar stream is a collection of kinematically associated metal-poor stars in the halo of the Milky Way lacking an obvious progenitor. The stream spans across an arc of ∼15° in the sky, and orbit-fitting suggests an apocentric distance of ${\sim} 20\, \mathrm{kpc}$ and a pericentre of ${\sim} 10\, \mathrm{kpc}$. The narrow metallicity dispersion of stars with available spectra, together with light element abundance variations, suggests a globular cluster (GC) origin. The observed metallicity ([Fe/H] ≈ −3.4), however, is much lower than that of any known GC. In addition, the width and velocity dispersion of the stream are similar to those expected from disrupting dwarf galaxies, and substantially larger than the tidal debris of GCs able to disrupt on C-19’s orbit. We propose here an unconventional model where the C-19 progenitor is a dark matter-dominated stellar system with GC-like abundance patterns. We use N-body simulations to show that the tidal disruption of a ∼100 pc King-model stellar component embedded in a ∼20 km s−1 cuspy cold dark matter halo yields debris consistent with C-19’s observed width and velocity dispersion. The stellar component of the progenitor is fully disrupted, and is spread over two distinct streams, one corresponding to C-19 and another possibly hiding behind the Galactic plane. If such companion stream were found, it would suggest that dark matter-dominated dwarfs may also develop GC-like enrichment patterns, a finding that would inform our theoretical understanding of the formation of multiple populations in GCs and dwarf galaxies alike.
Observations of the very young Type Ia Supernova 2019np with early-excess emission
Authors: Sai Hanna , Wang Xiaofeng , Elias-Rosa Nancy , Yang(杨轶) Yi , Zhang Jujia , Lin Weili , Mo Jun , Piro Anthony L , Zeng Xiangyun , Andrea Reguitti , Brown Peter , Burns Christopher R , Cai Yongzhi , Fiore Achille , Hsiao Eric Y , Isern Jordi , Itagaki K , Li Wenxiong , Li Zhitong , Pessi Priscila J , Phillips M M , Schuldt Stefan , Shahbandeh Melissa , Stritzinger Maximilian D , Tomasella Lina , Vogl Christian , Wang Bo , Wang Lingzhi , Wu Chengyuan , Yang Sheng , Zhang Jicheng , Zhang Tianmeng , Zhang Xinghan 
Published: June 2022

ABSTRACT
Early-time radiative signals from Type Ia supernovae (SNe Ia) can provide important constraints on the explosion mechanism and the progenitor system. We present observations and analysis of SN 2019np, a nearby SN Ia discovered within 1–2 days after the explosion. Follow-up observations were conducted in optical, ultraviolet, and near-infrared bands, covering the phases from ∼−16.7 d to ∼+ 367.8 d relative to its B-band peak luminosity. The photometric and spectral evolutions of SN 2019np resemble the average behaviour of normal SNe Ia. The absolute B-band peak magnitude and the post-peak decline rate are Mmax(B) = −19.52 ± 0.47 mag and Δm15(B) = 1.04 ± 0.04 mag, respectively. No Hydrogen line has been detected in the nebular-phase spectra of SN 2019np. Assuming that the 56Ni powering the light curve is centrally located, we find that the bolometric light curve of SN 2019np shows a flux excess up to 5.0 per cent in the early phase compared to the radiative diffusion model. Such an extra radiation perhaps suggests the presence of an additional energy source beyond the radioactive decay of central nickel. Comparing the observed colour evolution with that predicted by different models, such as interactions of SN ejecta with circumstellar matter (CSM)/companion star, a double-detonation explosion from a sub-Chandrasekhar mass white dwarf (WD) and surface 56Ni mixing, we propose that the nickel mixing is more favoured for SN 2019np.
Large-scale expansion of OB stars in Cygnus
Authors: Quintana Alexis L , Wright Nicholas J 
Published: June 2022

ABSTRACT
The proper motions (PMs) of OB stars in Cygnus have recently been found to exhibit two large-scale kinematic patterns suggestive of expansion. We perform a 3D traceback on these OB stars, the newly identified OB associations and related open clusters in the region. We find that there are two groups of stars, associations and clusters and that they were each more compact in the past, reaching their closest approach $7.9^{+3.0}_{-1.8}$ and $8.5^{+0.8}_{-2.8}$ Myr ago. We consider two main scenarios for the driver of these large-scale expansion patterns: feedback-driven expansion from a previous generation of massive stars, and expansion as a result of the turbulent velocity field in the primordial molecular cloud. While it is tempting to attribute such large-scale expansion patterns to feedback processes, we find that the observed kinematics are fully consistent with the turbulent origin, and therefore that the injection of further energy or momentum from feedback is not required. Similar conclusions may be drawn for other star forming regions with large-scale expansion patterns.
Anthropogenic monoterpenes aggravating ozone pollution
Authors: Wang Haichao , Ma Xuefei , Tan Zhaofeng , Wang Hongli , Chen Xiaorui , Chen Shiyi , Gao Yaqin , Liu Ying , Liu Yuhan , Yang Xinping , Yuan Bin , Zeng Limin , Huang Cheng , Lu Keding , Zhang Yuanhang 
Published: June 2022

Abstract
Monoterpenes have been known to have a critical influence on air quality and climate change through their impact on the formation of fine particles. Here we present field evidence that monoterpene oxidations largely enhanced local ozone production in a regional site in eastern China. The observed monoterpene was most likely from biomass burning rather than biogenic emissions, as indicated by the high correlation with CO at night-time, and the observed ratio of these two species was consistent with previously determined values from biomass burning experiments. Fast monoterpene oxidations were determined experimentally based on direct radical measurements, leading to a daily ozone enhancement of 4–18 parts per billion by volume (ppb), which was 6%–16% of the total ozone production, depending on the speciation of monoterpenes. It demonstrates that the previously overlooked anthropogenic monoterpenes make an important contribution to O3 production in eastern China. The role could possibly be important at similar locations across China and other parts of the world that are characterized by massive emissions, especially where there are high NOx levels. Our results highlight that anthropogenic monoterpenes should be taken into account when proceeding with the coordinated mitigation of O3 and particulate matter pollution.
Benefits and Concerns regarding Use of Cannabis for Therapeutic Purposes Among People Living with Chronic Pain: A Qualitative Research Study
Authors: AminiLari Mahmood , Kithulegoda Natasha , Strachan Patricia , MacKillop James , Wang Li , Pallapothu Sushmitha , Neumark Samuel , Sharma Sangita , Sethi Jagmeet , Zacharias Ramesh , Blain Allison , Patterson Lisa , Busse Jason W 
Published: June 2022

AbstractObjectiveAlthough there is growing interest in medically authorized cannabis for chronic pain, little is known about patients’ perspectives. We explored perceptions of people living with chronic pain regarding benefits and concerns surrounding their use of cannabis for therapeutic purposes.SettingA hospital-based clinic in Hamilton and two community-based interdisciplinary pain clinics in Burlington, Ontario, Canada.MethodsIn this qualitative descriptive study, we conducted semi-structured interviews with 13 people living with chronic pain who used cannabis therapeutically, living in Ontario, Canada. We used thematic analysis, with data collection, coding, and analysis occurring concurrently.ResultsPeople living with chronic pain reported important benefits associated with use of cannabis for therapeutic purposes, including reduced pain, improved functionality, and less risk of harms compared to prescription opioids. Most patients also acknowledged harms, such as grogginess and coughing, and there was considerable variability in patient experiences. Financial costs and stigma were identified as important barriers to use of cannabis.ConclusionEvidence-based guidance that incorporates patients’ values and preferences may be helpful to inform the role of cannabis in the management of chronic pain.