bluuebunny/crossref_metadata_2025_split huggingface dataset:
Prebiosignature Molecules Can Be Detected in Temperate Exoplanet Atmospheres with JWST
Authors: Claringbold A. B. , Rimmer P. B. , Rugheimer S. , Shorttle O. 
Published: July 2023

Abstract
The search for biosignatures on exoplanets connects the fields of biology and biochemistry to astronomical observation, with the hope that we might detect evidence of active biological processes on worlds outside the solar system. Here we focus on a complementary aspect of exoplanet characterization connecting astronomy to prebiotic chemistry: the search for molecules associated with the origin of life, prebiosignatures. Prebiosignature surveys in planetary atmospheres offer the potential to both constrain the ubiquity of life in the galaxy and provide important tests of current prebiotic syntheses outside of the laboratory setting. Here, we quantify the minimum abundance of identified prebiosignature molecules that would be required for detection by transmission spectroscopy using JWST. We consider prebiosignatures on five classes of terrestrial planets: an ocean planet, a volcanic planet, a post-impact planet, a super-Earth, and an early-Earth analog. Using a novel modeling and detection test pipeline, with simulated JWST noise, we find the detection thresholds of hydrogen cyanide (

HCN

), hydrogen sulfide (H2S), cyanoacetylene (HC3N), ammonia (NH3), methane (CH4), acetylene (C2H2), sulfur dioxide (SO2), nitric oxide (NO), formaldehyde (CH2O), and carbon monoxide (CO) in a variety of low-mean-molecular-weight (<5) atmospheres. We test the dependence of these detection thresholds on an M dwarf target star and the number of observed transits, finding that a modest number of transits (1–10) are required to detect prebiosignatures in numerous candidate planets, including TRAPPIST-1e with a high-mean-molecular-weight atmosphere. We find that the Near Infrared Spectrograph G395M/H instrument is best suited for detecting most prebiosignatures.
Doppler Broadening and Line-of-sight Effects in Core-collapse Supernovae and Young Remnants
Authors: Jacovich Taylor , Patnaude Daniel , Slane Patrick , Badenes Carles , Lee Shiu-Hang , Nagataki Shigehiro , Milisavljevic Dan 
Published: July 2023

Abstract
The dynamics and spectral characteristics of supernova ejecta reveal details of the supernova energetics, explosive nucleosynthesis, and evolution of the progenitor. However, in practice, this important diagnostic information is only derived from CCD-resolution X-ray spectra of shock-heated material. If the spectra were to be observed at higher resolution, then important clues to the explosion energetics would be obvious through measurements of bulk Doppler motions and turbulence in the ejecta. Likewise, the unshocked ejecta in supernovae and young remnants are responsible for obscuring the emission from ejecta on the back side of the remnant. In light of these important effects, we present line-of-sight spectral maps of core-collapse supernova remnant models. We explore the bulk Doppler broadening of spectral lines, including line-of-sight effects. We also explore the time-dependent absorption from both shocked and unshocked ejecta. Finally, we discuss how future X-ray missions such as XRISM and Athena will be able to resolve these effects in nearby and extragalactic supernovae and their remnants.
The Solar Minimum Eclipse of 2019 July 2. III. Inferring the Coronal T

e
with a Radiative Differential Emission Measure Inversion
Authors: Boe Benjamin , Downs Cooper , Habbal Shadia 
Published: July 2023

Abstract
Differential emission measure (DEM) inversion methods use the brightness of a set of emission lines to infer the line-of-sight (LOS) distribution of the electron temperature (T

e
) in the corona. DEM inversions have been traditionally performed with collisionally excited lines at wavelengths in the extreme ultraviolet and X-ray. However, such emission is difficult to observe beyond the inner corona (1.5 R
⊙), particularly in coronal holes. Given the importance of the T

e
distribution in the corona for exploring the viability of different heating processes, we introduce an analog of the DEM specifically for radiatively excited coronal emission lines, such as those observed during total solar eclipses (TSEs) and with coronagraphs. This radiative-DEM (R-DEM) inversion utilizes visible and infrared emission lines that are excited by photospheric radiation out to at least 3 R
⊙. Specifically, we use the Fe x (637 nm), Fe xi (789 nm), and Fe xiv (530 nm) coronal emission lines observed during the 2019 July 2 TSE near solar minimum. We find that, despite a large T

e
spread in the inner corona, the distribution converges to an almost isothermal yet bimodal distribution beyond 1.4 R
⊙, with T

e
ranging from 1.1 to 1.4 in coronal holes and from 1.4 to 1.65 MK in quiescent streamers. Application of the R-DEM inversion to the Predictive Science Inc. magnetohydrodynamic simulation for the 2019 eclipse validates the R-DEM method and yields a similar LOS Te
distribution to the eclipse data.
Magnetic Field Extrapolation in Active Region Well Comparable to Observations in Multiple Layers
Authors: Yu Fu , Zhao Jie , Su Yang , Zhu Xiaoshuai , Guo Yang , Shen Jinhua , Li Hui 
Published: July 2023

Abstract
Magnetic field extrapolation is a fundamental tool to reconstruct the three-dimensional magnetic field above the solar photosphere. However, the prevalently used force-free field model might not be applicable in the lower atmosphere with non-negligible plasma β, where the crucial process of flux rope formation and evolution could happen. In this work, we perform extrapolation in active region 12158, based on a recently developed magnetohydrostatic (MHS) method that takes plasma forces into account. By comparing the results with those from the force-free field extrapolation methods, we find that the overall properties, which are characterized by the magnetic free energy and helicity, are roughly the same. The major differences lie in the magnetic configuration and the twist number of the magnetic flux rope (MFR). Unlike previous works either obtained sheared arcades or one coherent flux rope, the MHS method derives two sets of MFR, which are highly twisted and slightly coupled. Specifically, the result in the present work is more comparable to the high-resolution observations from the chromosphere, through the transition region to the corona, such as the filament fibrils, pre-eruptive braiding characteristics, and the eruptive double-J-shaped hot channel. Overall, our work shows that the newly developed MHS method is more promising to reproduce the magnetic fine structures that can well match the observations at multiple layers, and future data-driven simulation based on such extrapolation will benefit in understanding the critical and precise dynamics of flux rope before eruption.
Probing the Circumgalactic Medium with Cosmic Microwave Background Polarization Statistical Anisotropy
Authors: Roy Anirban , van Engelen Alexander , Gluscevic Vera , Battaglia Nicholas 
Published: July 2023

Abstract
As cosmic microwave background (CMB) photons traverse the universe, anisotropies can be induced via Thomson scattering (proportional to the electron density; optical depth) and inverse Compton scattering (proportional to the electron pressure; thermal Sunyaev–Zel’dovich effect). Measurements of anisotropy in optical depth τ and Compton y parameters are imprinted by the galaxies and galaxy clusters and are thus sensitive to the thermodynamic properties of the circumgalactic medium and intergalactic medium. We use an analytic halo model to predict the power spectrum of the optical depth (τ
τ), the cross-correlation between the optical depth and the Compton y parameter (τ
y), and the cross-correlation between the optical depth and galaxy clustering (τ
g), and compare this model to cosmological simulations. We constrain the optical depths of halos at z ≲ 3 using a technique originally devised to constrain patchy reionization at a higher redshift range. The forecasted signal-to-noise ratio is 2.6, 8.5, and 13, respectively, for a CMB-S4-like experiment and a Vera C. Rubin Observatory–like optical survey. We show that a joint analysis of these probes can constrain the amplitude of the density profiles of halos to 6.5% and the pressure profiles to 13%. These constraints translate to astrophysical parameters, such as the gas mass fraction, f
g, which can be constrained to 5.3% uncertainty at z ∼ 0. The cross-correlations presented here are complementary to other CMB and galaxy cross-correlations since they do not require spectroscopic galaxy redshifts and are another example of how such correlations are a powerful probe of the astrophysics of galaxy evolution.
HALO7D. III. Chemical Abundances of Milky Way Halo Stars from Medium-resolution Spectra
Authors: McKinnon Kevin A. , Cunningham Emily C. , Rockosi Constance M. , Guhathakurta Puragra , Escala Ivanna , Kirby Evan N. , Deason Alis J. 
Published: July 2023

Abstract
The Halo Assembly in Lambda Cold Dark Matter: Observations in 7 Dimensions (HALO7D) survey measures the kinematics and chemical properties of stars in the Milky Way (MW) stellar halo to learn about the formation of our Galaxy. HALO7D consists of Keck II/DEIMOS spectroscopy and Hubble Space Telescope–measured proper motions of MW halo main-sequence turnoff stars in the four Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey fields. HALO7D consists of deep pencil beams, making it complementary to other contemporary wide-field surveys. We present the [Fe/H] and [α/Fe] abundances for 113 HALO7D stars in the Galactocentric radial range of ∼10–40 kpc along four separate pointings. Using the full 7D chemodynamical data (3D positions, 3D velocities, and abundances) of HALO7D, we measure the velocity anisotropy, β, of the halo velocity ellipsoid for each field and for different metallicity-binned subsamples. We find that two of the four fields have stars on very radial orbits, while the remaining two have stars on more isotropic orbits. Separating the stars into high-, mid-, and low-[Fe/H] bins at −2.2 and −1.1 dex for each field separately, we find differences in the anisotropies between the fields and between the bins; some fields appear dominated by radial orbits in all bins, while other fields show variation between the [Fe/H] bins. These chemodynamical differences are evidence that the HALO7D fields have different fractional contributions from the progenitors that built up the MW stellar halo. Our results highlight the additional information available on smaller spatial scales compared to results from a spherical average of the stellar halo.
Updated Orbital Ephemeris and Detection of Superhump Modulation in X-Ray Band for the Ultra-compact Low Mass X-Ray Binary 4U 1820-30
Authors: Chou Yi , Jhang Yao-Wun 
Published: July 2023

Abstract
The 4U 1820-30 is an ultra-compact low-mass X-ray binary (LMXB) near the center of the globular cluster NGC 6624. Its negative orbital period derivative, observed from the phase evolution of its sinusoidal-like orbital variation, contradicts the positive value that was obtained from the theoretical prediction. In this paper, we present the analysis of the 4U 1820-30 orbital modulation from light curves obtained from the Neutron star Interior Composition ExploreR (NICER) observations from 2017 to mid-2022. Combined with historical records, the orbital derivative is measured from the orbital phase evolution between 1976 and 2002 is

P

̇

/

P
=
(
−
5.21
±
0.13
)
×

10

−
8

yr−1. No significant second order orbital period derivative is detected with a 2σ upper limit of

∣

P

̈

∣
<
5.48
×

10

−
22

s s−2. We discuss the possible intrinsic orbital period derivative of 4U 1820-30 and suggest that this binary system may have a significant mass outflow similar to some other LMXBs. In addition, a periodic modulation with a period of 691.6 ± 0.7 s, which is consistent with the superhump period discovered in the far-ultraviolet band of the Hubble Space Telescope, was also detected in the X-ray light curves that were collected by NICER. We conclude that this modulation is probably caused by a period of 0.8 ± 0.1 day apsidal precession of the accretion disk, similar to the SU UMa type dwarf novae and some LMXBs. However we cannot exclude the possibility that it is induced by a hierarchical third star that orbits around the binary system.
Inferences from Surface Brightness Fluctuations of Zwicky 3146 via the Sunyaev–Zel’dovich Effect and X-Ray Observations
Authors: Romero Charles E. , Gaspari Massimo , Schellenberger Gerrit , Bhandarkar Tanay , Devlin Mark , Dicker Simon R. , Forman William , Khatri Rishi , Kraft Ralph , Di Mascolo Luca , Mason Brian S. , Moravec Emily , Mroczkowski Tony , Nulsen Paul , Orlowski-Scherer John , Sarmiento Karen Perez , Sarazin Craig , Sievers Jonathan , Su Yuanyuan 
Published: July 2023

Abstract
The galaxy cluster Zwicky 3146 is a sloshing cool-core cluster at z = 0.291 that in Sunyaev–Zel’dovich (SZ) imaging does not appear to exhibit significant pressure substructure in the intracluster medium. We perform a surface brightness fluctuation analysis via Fourier amplitude spectra on SZ (MUSTANG-2) and X-ray (XMM-Newton) images of this cluster. These surface brightness fluctuations can be deprojected to infer pressure and density fluctuations from the SZ and X-ray data, respectively. In the central region (Ring 1, r < 100″ = 440 kpc, in our analysis), we find fluctuation spectra that suggest injection scales around 200 kpc (∼140 kpc from pressure fluctuations and ∼250 kpc from density fluctuations). When comparing the pressure and density fluctuations in the central region, we observe a change in the effective thermodynamic state from large to small scales, from isobaric (likely due to the slow sloshing) to adiabatic (due to more vigorous motions). By leveraging scalings from hydrodynamical simulations, we find an average 3D Mach number ≈0.5. We further compare our results to other studies of Zwicky 3146 and, more broadly, to other studies of fluctuations in other clusters.
Drop in the Hard Pulsed Fraction and a Candidate Cyclotron Line in IGR J16320–4751 Seen by NuSTAR
Authors: Bodaghee A. , Chiu J.-L. , Tomsick J. A. , Bhalerao V. , Bottacini E. , Clavel M. , Cox C. , Fürst F. , Middleton M. J. , Rahoui F. , Rodriguez J. , Romano P. , Wilms J. 
Published: July 2023

Abstract
We report on a timing and spectral analysis of a 50 ks NuSTAR observation of IGR J16320−4751 (= AX J1631.9−4752), a high-mass X-ray binary hosting a slowly rotating neutron star. In this observation from 2015, the spin period was 1308.8 ± 0.4 s giving a period derivative

P

̇

∼
2
×

10

−
8

s s−1 when compared with the period measured in 2004. In addition, the pulsed fraction decreased as a function of energy, as opposed to the constant trend that was seen previously. This suggests a change in the accretion geometry of the system during the intervening 11 yr. The phase-averaged spectra were fit with the typical model for accreting pulsars: a power law with an exponential cutoff. This left positive residuals at 6.4 keV attributable to the known iron Kα line, as well as negative residuals around 14 keV from a candidate cyclotron line detected at a significance of 5σ. We found no significant differences in the spectral parameters across the spin period, other than the expected changes in flux and component normalizations. A flare lasting around 5 ks was captured during the first half of the observation, where the X-ray emission hardened and the local column density decreased. Finally, the binary orbital period was refined to 8.9912 ± 0.0078 days thanks to Swift/BAT monitoring data from 2005–2022.
Misaligned Jets from Sgr A* and the Origin of Fermi/eROSITA Bubbles
Authors: Sarkar Kartick C. , Mondal Santanu , Sharma Prateek , Piran Tsvi 
Published: July 2023

Abstract
One of the leading explanations for the origin of Fermi Bubbles is past jet activity in the Galactic center supermassive black hole Sgr A*. The claimed jets are often assumed to be perpendicular to the Galactic plane. Motivated by the orientation of pc-scale nuclear stellar disk and gas streams, as well as a low inclination of the accretion disk around Sgr A* inferred by the Event Horizon Telescope, we perform hydrodynamical simulations of nuclear jets significantly tilted relative to the Galactic rotation axis. The observed axisymmetry and hemisymmetry (north–south symmetry) of Fermi/eROSITA bubbles (FEBs) due to quasi-steady jets in Sgr A* could be produced if the jet had a super-Eddington power (≳5 × 1044 erg s−1) for a short time (jet active period ≲6 kyr) for a reasonable jet opening angle (≲10°). Such powerful explosions are, however, incompatible with the observed O viii/O vii line ratio toward the bubbles, even after considering electron–proton temperature nonequilibrium. We argue that the only remaining options for producing FEBs are (i) a low-luminosity (≈1040.5−41 erg s−1) magnetically dominated jet or accretion wind from the Sgr A*, or (ii) a supernovae or tidal disruption event driven wind of a similar luminosity from the Galactic center.
A Catalog of Young Stellar Objects from the LAMOST and ZTF Surveys
Authors: Zhang Jingyi , Zhang Yanxia , Kang Zihan , Li Changhua , Zhao Yongheng 
Published: July 2023

Abstract
As astronomical data sets become too large for traditional analysis approaches, more machine-learning algorithms are employed in astronomy. A wealth of light variation data have been accumulated, which provide rich samples for astronomers to study variable stars. Facing the challenge of big data, this article takes the classification of variable and transient objects observed by the Zwicky Transient Facility (ZTF) as the main goal, and a self-paced ensemble (SPE) imbalanced-learning classifier is constructed to separate different classes. The performance of the classifier reveals that SPE is better than a traditional imbalanced-learning algorithm for the minority classes. In our work, the SPE classifier is satisfactory for young stellar objects (YSOs), and the completeness (recall) of YSOs is enhanced to 91%. As a result, 868,371 ZTF sources are classified into 15 classes by this classifier, which contains 8210 YSO candidates (YSO_prob ≥ 0.70). In order to further identify YSO candidates, these candidates are crossmatched with LAMOST DR9. Finally, 833 candidates are observed by LAMOST, among them 379 objects that are known YSOs in SIMBAD. For the remaining objects with good-quality LAMOST spectra, we visually check their spectral characteristics, and 238 objects are newly confirmed YSOs. These newfound YSOs supplement the present YSO sample, and other YSO candidates may be used for follow-up observation, which is useful for characterizing YSOs, finding more YSOs, and then giving a better stellar evolution model in the future. The classified ZTF sources by SPE provide reference to the study of variables and transients.
Taxonomic notes and key to the West Palearctic Antocha (Antocha) Osten Sacken, 1860 (Diptera, Limoniidae) with description of a new species from Morocco
Authors: Mabrouki Youness , Terec Andrei , Taybi Fouzi , Dénes Anna , Keresztes Lujza 
Published: July 2023

The Mediterranean Region of the West Palearctic is one of the most species-rich biomes in the world, hosting a high level of endemism and relict species with important conservation value. The North Africa Atlas Mountains (spanning Morocco, Algeria and Tunisia) belong to a poorly-investigated region of the Mediterranean area, with overlooked aquatic biodiversity; hence, a number of species still remain to be discovered.
The subgenus Antocha (Antocha) Osten Sacken, 1860 is recorded for the first time from Africa, with a description of A. (A.) staryi Keresztes & Mabrouki sp. nov. from hilly regions of the Middle Atlas region, Morocco. The unique design of the male terminalia differentiates well the newly-discovered species from its closely-related and range-restricted A. (A.) phoenicia Thomas and Dia, 1982. This is in contrast with the high intraspecific and geographically poorly-defined variability of the widespread A. (A.) vitripennis (Meigen, 1830), for which morphological variability of male genital structures is discussed.
Illustrations of male genital parts, distribution data and key to the species from the West Palearctic area are also provided.
Escolha da contracepção hormonal por mulheres assistidas na atenção primária: fatores limitantes e medo
Authors: Monçalves Kelvin Leandro Marques , Wilhelm Laís Antunes , Silveira Andressa da , Ferreira Carla Lizandra de Lima , Silva Silvana Cruz da , Soliz Paola Piovenzano de , Soccol Keity Laís Siepmann 
Published: July 2023

Objetivo: Conhecer como ocorre a escolha pela contracepção hormonal por mulheres assistidas na Atenção Primária à Saúde. Método: Estudo qualitativo, descritivo e exploratório realizado em uma Estratégia Saúde da Família na região central do Rio Grande do Sul entre os meses de janeiro a março de 2022. Participaram 20 mulheres entre 18-43 anos. A produção de dados ocorreu mediante entrevista composta por questões abertas, as enunciações foram transcritas e submetidas à análise temática. Resultados: As participantes revelaram a falta de opção fornecida pelo Sistema Único de Saúde na escolha da contracepção hormonal, bem como apresentam fatores limitantes como dúvidas, dificuldades e medo ao utilizar o anticoncepcional hormonal devido à falta de orientação profissional na Atenção Primária à Saúde. Conclusão: A escolha do método contraceptivo precisa levar em consideração a autonomia da mulher e os profissionais de saúde que atuam na Atenção Primária à Saúde devem garantir o direito de escolha, minimizar as dúvidas, medos e tabus que circundam o processo de anticoncepção hormonal. Ademais, as consultas de saúde da mulher devem oportunizar a educação em saúde, o diálogo e a troca de saberes.
Adaptation of the Tumor Antigen Presentation Machinery to Ionizing Radiation
Authors: Lee Mi-Heon , Ratanachan Duang , Wang Zitian , Hack Jacob , Adbulrahman Lobna , Shamlin Nicholas P , Kalayjian Mirna , Nesseler Jean Philippe , Ganapathy Ekambaram , Nguyen Christine , Ratikan Josephine A , Cacalano Nicolas A , Austin David , Damoiseaux Robert , DiPardo Benjamin J , Graham Danielle S , Kalbasi Anusha , Sayre James W , McBride William H , Schaue Dörthe 
Published: July 2023

Abstract
Ionizing radiation (IR) can reprogram proteasome structure and function in cells and tissues. In this article, we show that IR can promote immunoproteasome synthesis with important implications for Ag processing and presentation and tumor immunity. Irradiation of a murine fibrosarcoma (FSA) induced dose-dependent de novo biosynthesis of the immunoproteasome subunits LMP7, LMP2, and Mecl-1, in concert with other changes in the Ag-presentation machinery (APM) essential for CD8+ T cell–mediated immunity, including enhanced expression of MHC class I (MHC-I), β2-microglobulin, transporters associated with Ag processing molecules, and their key transcriptional activator NOD-like receptor family CARD domain containing 5. In contrast, in another less immunogenic, murine fibrosarcoma (NFSA), LMP7 transcripts and expression of components of the immunoproteasome and the APM were muted after IR, which affected MHC-I expression and CD8+ T lymphocyte infiltration into NFSA tumors in vivo. Introduction of LMP7 into NFSA largely corrected these deficiencies, enhancing MHC-I expression and in vivo tumor immunogenicity. The immune adaptation in response to IR mirrored many aspects of the response to IFN-γ in coordinating the transcriptional MHC-I program, albeit with notable differences. Further investigations showed divergent upstream pathways in that, unlike IFN-γ, IR failed to activate STAT-1 in either FSA or NFSA cells while heavily relying on NF-κB activation. The IR-induced shift toward immunoproteasome production within a tumor indicates that proteasomal reprogramming is part of an integrated and dynamic tumor–host response that is specific to the stressor and the tumor and therefore is of clinical relevance for radiation oncology.