bluuebunny/crossref_metadata_2025_split huggingface dataset:
HAWC Study of the Very-high-energy γ-Ray Spectrum of HAWC J1844−034
Authors: Albert A. , Alvarez C. , Avila Rojas D. , Ayala Solares H. A. , Babu R. , Belmont-Moreno E. , Breuhaus M. , Capistrán T. , Carramiñana A. , Casanova S. , Cotzomi J. , Coutiño de León S. , De la Fuente E. , Depaoli D. , Diaz Hernandez R. , Dingus B. L. , DuVernois M. A. , Durocher M. , Engel K. , Espinoza C. , Fan K. L. , Fang K. , Fraija N. , García-González J. A. , González M. M. , Goodman J. A. , Groetsch S. , Harding J. P. , Herzog I. , Hinton J. , Huang D. , Hueyotl-Zahuantitla F. , Humensky T. B. , Hüntemeyer P. , Joshi V. , Kaufmann S. , Lee J. , Vargas H. León , Longinotti A. L. , Luis-Raya G. , Malone K. , Martinez O. , Martínez-Castro J. , Matthews J. A. , Miranda-Romagnoli P. , Morales-Soto J. A. , Moreno E. , Mostafá M. , Nellen L. , Noriega-Papaqui R. , Olivera-Nieto L. , Omodei N. , Pérez-Pérez E. G. , Rho C. D. , Rosa-González D. , Ruiz-Velasco E. , Salazar H. , Salazar-Gallegos D. , Sandoval A. , Schneider M. , Serna-Franco J. , Smith A. J. , Son Y. , Springer R. W. , Tibolla O. , Tollefson K. , Torres I. , Torres-Escobedo R. , Turner R. , Ureña-Mena F. , Varela E. , Villaseñor L. , Wang X. , Watson I. J. , Willox E. , Zhou H. ,   HAWC collaboration
Published: September 2023

AbstractRecently, the region surrounding eHWC J1842−035 has been studied extensively by γ-ray observatories due to its extended emission reaching up to a few hundred TeV and potential as a hadronic accelerator. In this work, we use 1910 days of cumulative data from the High Altitude Water Cherenkov (HAWC) observatory to carry out a dedicated systematic source search of the eHWC J1842−035 region. During the search, we found three sources in the region, namely, HAWC J1844−034, HAWC J1843−032, and HAWC J1846−025. We have identified HAWC J1844−034 as the extended source that emits photons with energies up to 175 TeV. We compute the spectrum for HAWC J1844−034, and by comparing with the observational results from other experiments, we have identified HESS J1843−033, LHAASO J1843−0338, and TASG J1844−038 as very-high-energy γ-ray sources with a matching origin. Also, we present and use the multiwavelength data to fit the hadronic and leptonic particle spectra. We have identified four pulsar candidates in the nearby region in which PSR J1844−0346 is found to be the most likely candidate due to its proximity to HAWC J1844−034 and the computed energy budget. We have also found SNR G28.6−0.1 as a potential counterpart source of HAWC J1844−034 for which both leptonic and hadronic scenarios are feasible.
Effects of Coronal Magnetic Field Configuration on Particle Acceleration and Release during the Ground Level Enhancement Events in Solar Cycle 24
Authors: Liu Wenlong , Kong Xiangliang , Guo Fan , Zhao Lulu , Feng Shiwei , Yu Feiyu , Jiang Zelong , Chen Yao , Giacalone Joe 
Published: September 2023

Abstract
Ground level enhancements (GLEs) are extreme solar energetic particle (SEP) events that are of particular importance in space weather. In solar cycle 24, two GLEs were recorded on 2012 May 17 (GLE 71) and 2017 September 10 (GLE 72), respectively, using a range of advanced modern instruments. Here we conduct a comparative analysis of the two events by focusing on the effects of large-scale magnetic field configuration near active regions on particle acceleration and release. Although the active regions are both located near the western limb, temporal variations of SEP intensities and energy spectra measured in situ display different behaviors at early stages. By combining a potential field model, we find the coronal mass ejection (CME) in GLE 71 originated below the streamer belt, while in GLE 72 it originated near the edge of the streamer belt. We reconstruct the CME shock fronts with an ellipsoid model based on nearly simultaneous coronagraph images from multiple viewpoints and further derive the 3D shock geometry at the GLE onset. The highest-energy particles are primarily accelerated in the shock–streamer interaction regions, i.e., likely at the nose of the shock in GLE 71 and the eastern flank in GLE 72, due to quasi-perpendicular shock geometry and confinement of closed fields. Subsequently, they are released to the field lines connecting to near-Earth spacecraft when the shocks move through the streamer cusp region. This suggests that magnetic structures in the corona, especially shock–streamer interactions, may have played an important role in the acceleration and release of the highest-energy particles in the two events.
The Sun’s Magnetic Power Spectra over Two Solar Cycles. I. Calibration between SDO/HMI and SOHO/MDI Magnetograms
Authors: Luo Yukun , Jiang Jie , Wang Ruihui 
Published: September 2023

Abstract
The Sun’s magnetic field is strongly structured over a broad range of scales. Magnetic spatial power spectral analysis provides a powerful tool for understanding the various scales of magnetic fields and their interactions with plasma motions. We aim to investigate the power spectra using spherical harmonic decomposition of high-resolution Solar and Heliospheric Observatory (SOHO)/Michelson Doppler Imager (MDI) and Solar Dynamics Observatory (SDO)/Helioseismic and Magnetic Imager (HMI) synoptic magnetograms covering three consecutive solar cycle minima, in a series of papers. As the first of the series, we calibrate and analyze the power spectra based on cotemporal SDO/HMI and SOHO/MDI data in this paper. For the first time, we find that the calibration factor r between SOHO/MDI and SDO/HMI varies with the spatial scale l of the magnetic field, where l is the degree of the spherical harmonic. The calibration factor satisfies

r
(
l
)
=

−
0.021

l

0.64

+
2

(
5
<
l
≤
539
)

. With the calibration function, most contemporaneous SOHO/MDI and SDO/HMI magnetograms show consistent power spectra from about 8 Mm to the global scales over about three orders of magnitude. Moreover, magnetic power spectra from SOHO/MDI and SDO/HMI maps show peaks/knees at l ≈ 120, corresponding to the typical supergranular scale (about 35 Mm) constrained from direct velocimetric measurements. This study paves the way for investigating the solar cycle dependence of supergranulation and magnetic power spectra in subsequent studies.
Metallicities of Classical Cepheids in the Inner Galactic Disk
Authors: Matsunaga Noriyuki , Taniguchi Daisuke , Elgueta Scarlet S. , Tsujimoto Takuji , Baba Junichi , McWilliam Andrew , Otsubo Shogo , Sarugaku Yuki , Takeuchi Tomomi , Katoh Haruki , Hamano Satoshi , Ikeda Yuji , Kawakita Hideyo , Hull Charlie , Albarracín Rogelio , Bono Giuseppe , D’Orazi Valentina 
Published: September 2023

Abstract
Metallicity gradients refer to the sloped radial profiles of the metallicities of gas and stars and are commonly seen in disk galaxies. A well-defined metallicity gradient of the Galactic disk is observed particularly well with classical Cepheids, which are good stellar tracers thanks to their period–luminosity relation, allowing precise distance estimation and other advantages. However, the measurement of the inner-disk gradient has been impeded by the incompleteness of previous samples of Cepheids and the limitations of optical spectroscopy in observing highly reddened objects. Here we report the metallicities of 16 Cepheids measured with high-resolution spectra in the near-infrared YJ bands. These Cepheids are located at 3–5.6 kpc in Galactocentric distance, R
GC, and reveal the metallicity gradient in this range for the first time. Their metallicities are mostly between 0.1 and 0.3 dex in [Fe/H] and more or less follow the extrapolation of the metallicity gradient found in the outer part, R
GC > 6.5 kpc. The gradient in the inner disk may be shallower or even flat, but the small sample does not allow the determination of the slope precisely. More extensive spectroscopic observations would also be necessary for studying minor populations, if any, with higher or lower metallicities that were reported in previous literature. In addition, the 3D velocities of our inner-disk Cepheids show a kinematic pattern that indicates noncircular orbits caused by the Galactic bar, which is consistent with the patterns reported in recent studies on high-mass star-forming regions and red giant branch stars.
The Multiwavelength Environment of Second Bologna Catalog Sources
Authors: Paggi A. , Massaro F. , Penã-Herazo H. , Missaglia V. , Jimenez-Gallardo A. , Ricci F. , Ettori S. , Giovannini G. , Govoni F. , Baldi R. D. , Mingo B. , Murgia M. , Liuzzo E. , Galati F. 
Published: September 2023

Abstract
We present the first results of the Chandra Cool Targets (CCT) survey of the Second Bologna Catalog (B2CAT) of powerful radio sources, aimed at investigating the extended X-ray emission surrounding these sources. For the first 33 sources observed in the B2CAT CCT survey, we performed both imaging and spectral X-ray analysis, producing multiband Chandra images, and compared these images with radio observations. To evaluate the presence of extended emission in the X-rays, we extracted surface flux profiles comparing them with simulated ACIS point-spread functions. We detected X-ray nuclear emission for 28 sources. In addition, we detected eight regions of increased X-ray flux originating from radio hot spots or jet knots, and a region of decreased flux, possibly associated with an X-ray cavity. We performed X-ray spectral analysis for 15 nuclei and found intrinsic absorption significantly larger than the Galactic values in four of them. We detected significant extended X-ray emission in five sources, and fitted their spectra with thermal models with gas temperatures ∼2 keV. In the case of B2.1 0742+31, the surrounding hot gas is compatible with the intracluster medium of low-luminosity clusters of galaxies, while the X-ray diffuse emission surrounding the highly disturbed wide-angle-tailed radio galaxy B2.3 2254+35 features a luminosity similar to those of relatively bright galaxy groups, although its temperature is similar to those of low-luminosity galaxy clusters. These results highlight the power of low-frequency radio selection, combined with short Chandra snapshot observations, for investigating the properties of X-ray emission from radio sources.
Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation
Authors: Long Liu , Bi Shaolan , Zhang Jinghua , Zhang Xianfei , Zhang Liyun , Ge Zhishuai , Li Tanda , Chen Xunzhou , Li YaGuang , Ye LiFei , Sun TianCheng , Zhou JianZhao 
Published: September 2023

Abstract
Using data from Gaia Data Release 3 and Kepler/K2, we present a catalog of 16 open clusters with ages ranging from 4–4000 Myr that provides detailed information on membership, binary systems, and rotation. We assess the memberships in 5D phase space, and estimate the basic parameters of each cluster. Among the 20,160 members, there are 4381 stars identified as binary candidates and 49 stars identified as blue straggler stars. The fraction of binaries varies in each cluster, and the range is between 9% and 44%. We obtain the rotation periods of 5467 members, of which 4304 are determined in this work. To establish a benchmark for the rotation–age–color relation, we construct color–period diagrams. We find that the rotational features of binaries are similar to that of single stars, while the features for binaries are more scattered in the rotation period. Moreover, the morphology of the color–period relationship is already established for Upper Scorpius at the age of 19 Myr, and some stars of varying spectral types (i.e., FG, K, and M type) show different spin-down rates after the age of ∼110 Myr. By incorporating the effects of stalled spin-down into our analysis, we develop an empirical rotation–age–color relation, which is valid with ages between 700–4000 Myr and colors corresponding to a range of 0.5 <

(

G

BP

−

G

RP

)

0

< 2.5 mag.
The Disturbed and Globular-cluster-rich Ultradiffuse Galaxy UGC 9050-Dw1
Authors: Fielder Catherine E. , Jones Michael G. , Sand David J. , Bennet Paul , Crnojević Denija , Karunakaran Ananthan , Mutlu-Pakdil Burçin , Spekkens Kristine 
Published: September 2023

Abstract
We investigate the ultradiffuse galaxy (UDG) UGC 9050-Dw1, which was selected because of its disturbed morphology as part of a larger sample of UDGs that display evidence for significant interactions. We use the Hubble Space Telescope’s Advanced Camera for Surveys to identify globular clusters (GCs) associated with UGC 9050-Dw1, and the Jansky Very Large Array to measure its H i content. UGC 9050-Dw1, a neighbor to the low surface brightness spiral UGC 9050, exhibits a unique UV-bright central “clump” with clearly associated H i gas and an extended stellar tidal plume to the north. We identify 52 ± 12 GCs, implying a specific frequency of S

N
= 122 ± 38, one of the highest reported for a UDG of this luminosity (

log

L

V

/

L

⊙

=
7.5
±
0.1

). Additionally, ∼20% of the total light of the galaxy is contributed by GCs. Nearly uniform GC colors suggest they were formed during a single intense episode of star formation. We posit that UGC 9050-Dw1 represents the initial definitive observational example of UDG formation resulting from a dwarf merger event, where subsequent clumpy star formation has contributed to its present observed characteristics.
COOL-LAMPS. Discovery of COOL J0335−1927, a Gravitationally Lensed Quasar at z = 3.27 with an Image Separation of 23.″3
Authors: Napier Kate , Gladders Michael D. , Sharon Keren , Dahle Håkon , Cloonan Aidan P. , Mahler Guillaume , Escapa Isaiah , Garza Josh , Kisare Andrew , Malagon Natalie , Mork Simon , Niu Kunwanhui , Rosener Riley , Sullivan Jamar , Tagliavia Marie , Tamargo-Arizmendi Marcos , Teixeira Raul , Tsiane Kabelo , Wagner Grace , Zhang Yunchong , Zhao Megan 
Published: September 2023

Abstract
We report the discovery of COOL J0335−1927, a quasar at z = 3.27 lensed into three images with a maximum separation of 23.″3 by a galaxy cluster at z = 0.4178. To date, this is the highest redshift wide-separation lensed quasar known. In addition, COOL J0335−1927 shows several strong intervening absorbers visible in the spectra of all three quasar images with varying equivalent widths. The quasar also shows mini-broad line absorption. We construct a parametric strong gravitational lens model using ground-based imaging, constrained by the redshift and positions of the quasar images as well as the positions of three other multiply imaged background galaxies. Using our best-fit lens model, we calculate the predicted time delays between the three quasar images to be Δt
AB =

499

−
146

+
141

(stat) and Δt
AC =

−

127

−
17

+
83

(stat) days. Folding in systematic uncertainties, the model-predicted time delays are within the ranges 240 < Δt
AB < 700 and −300 < Δt
AC < −30. We also present g-band photometry from archival Dark Energy Camera Legacy Survey and Pan-STARRS imaging, and new multi-epoch observations obtained between 2022 September 18 UT and 2023 February 22 UT, which demonstrate significant variability in the quasar and will eventually enable the measurement of the time delay between the three quasar images. The currently available light curves are consistent with the model-predicted time delays. This is the fifth paper from the COOL-LAMPS collaboration.
« Génération crash test » : les doctorants face au RGPD
Authors: N’Diaye Marième 
Published: September 2023

Résumé À l'heure de la « science ouverte », les chercheurs sont soumis à des injonctions contradictoires : s'ils doivent partager leurs données, ils doivent également garantir la confidentialité de leurs enquêtés. Dans ce contexte de surveillance accrue qui entraîne des mises en cause plus fréquentes de leur travail, je me penche plus particulièrement sur les situations vécues par les doctorants, chercheurs les plus exposés car les plus précaires. Face à la multiplication des normes de contrôle, quel type d'enquête sont-ils susceptibles de mener ? Pour produire quel type de données ? Et comment cette redéfinition du métier influence-t-elle leur conception du monde de la recherche ? Je traite ces questions à partir de l'exemple de la mise en œuvre du RGPD (Règlement général sur la protection des données) par des doctorants en science politique qui ont des terrains à l'international. En rendant compte de la contrainte qu'ils ressentent effectivement aux différentes étapes de leurs parcours ­ en amont de l'enquête, sur le terrain et dans la phase d'exploitation des données et d'écriture ­, j'entends poser quelques jalons pour une réflexion sur les effets de la bureaucratisation de la recherche qui affectent aujourd'hui les chercheurs de demain.
Diffusion Depth and Efficacy of Different Infiltration Times for Rose Bengal/Green Light Corneal Cross-linking in Rabbit Eyes
Authors: Gao Rongrong , Chen Ming , Chen Xueyang , Liu Xinyu , Jiang Qingqing , Meek Keith M. , Wang Qinmei , Chen Shihao , Huang Jinhai 
Published: September 2023

Purpose:
To explore the diffusion depth and green light corneal cross-linking efficacy of different rose bengal (Rb) infiltration times in rabbit eyes.

Methods:
Twenty-eight fresh rabbit eyes were deepithelialized and infiltrated in 0.1% Rb solution for 2 to 30 minutes. Corneal frozen sections were cut and Rb diffusion depth was observed under the confocal microscope. A further 36 rabbits were randomly divided into eight groups according to the type of treatment (control, Rb infiltration only without irradiation, rose bengal/green light [RGX] for different infiltration times, or riboflavin/ultraviolet radiation [UVX]). The corneas' resistance to keratolysis and biomechanical properties were measured after treatment.

Results:
After 2, 10, 20, and 30 minutes of infiltration, Rb penetration depths in the corneal stroma were 100, 150, 200, and 270 µm, respectively. The times for complete digestion of the RGX 10 minutes (14.0 ± 1.4 hours), RGX 20 minutes (18.8 ± 1.1 hours), and UVX (51.2 ± 7.2 hours) groups were statistically greater than that of the control group (7.2 ± 1.1 hours). At 10% extension, the Young's modulus of the RGX 20 minutes (36.59 ± 4.90 MPa) and UVX (40.89 ± 2.57 MPa) groups was statistically greater than that of the control group (21.76 ± 5.69 MPa).

Conclusions:
The diffusion depth of Rb in corneal stroma increased by prolonging the infiltration time. The longer the infiltration time, the better the RGX effect. RGX for 20 minutes showed the best cross-linking efficacy among all RGX groups, albeit not as good as UVX.

[
J Refract Surg
. 2023;39(9):620–626.]
Visual Performance at All Distances and Patient Satisfaction With a New Aspheric Inverted Meniscus Intraocular Lens
Authors: Marín José M. , Hervella Lucía , Villegas Eloy , Robles Consuelo , Alcón Encarna , Yago Inés , Artal Pablo 
Published: September 2023

Purpose:
To evaluate visual performance, spectacle independence, and quality of vision of new intraocular lenses (IOLs) for presbyopia correction with an aspheric inverted meniscus optical design (ArtIOLs; Voptica SL) in patients undergoing bilateral cataract surgery.

Methods:
In this prospective study, 60 eyes from 30 patients implanted bilaterally with Art40 and Art70 IOLs were included. These new IOLs were designed with an inverted meniscus shape to improve the peripheral performance and with aspheric surfaces to induce different amounts of negative spherical aberration in each IOL model. Distance-corrected and uncorrected through-focus visual acuities and contrast sensitivity were measured 1 to 3 months after surgery. Twenty-eight patients answered Patient Reported Spectacle Independence (PRSIQ) and Quality of Vision (QoV) questionnaires.

Results:
Mean monocular (Art40 and Art70) and binocular (Art40/70) corrected distance visual acuities (CDVA) were zero logMAR (20/20). Binocular uncorrected distance visual acuity (UDVA) at far, intermediate (66 cm), and near (40 cm) distances was 0.00 ± 0.01, 0.01 ± 0.03, and 0.09 ± 0.09 logMAR, respectively. Spectacle independence was achieved by 24 (85.7%) patients for far and intermediate vision and 20 patients (71.4%) for near vision. The number of patients never reporting experiencing glare, halos, and starbursts was 28, 27, and 26 (100%, 96.4%, and 92.9%), respectively.

Conclusions:
The binocular combination of two ArtIOLs models (Art40 and Art70) significantly extended the depth of focus up to at least 40 cm. This combination resulted in a full range of vision with a high level of spectacle independence and without the compromise of halos or dysphotopsias.

[
J Refract Surg
. 2023;39(9):582–588.]
Surgical Technique to Treat Presbyopic Inlay-Associated Corneal Haze With Sequential Excimer Photoablation: A Case Series
Authors: Lee Brian J. H. , Ong Hon Shing , Fenner Beau J. , Mehta Jodhbir S. 
Published: September 2023

Purpose:
To describe an approach using sequential excimer laser ablation of the stromal surface of the corneal flap with or without subsequent excimer ablation to the stromal bed to reduce presbyopic inlay–associated corneal haze.

Methods:
Twelve patients who underwent KAMRA inlay (Acufocus) explantation due to corneal haze were included. The mean interval between explantation and the primary surgery (phototherapeutic keratotomy [PTK] to corneal flap) was 16.2 ± 29.7 months (range = 1 to 83 months). The corneal flap was lifted and laid on an evisceration spoon and an excimer laser was used to ablate the flap stroma by 30 to 40 µm depth. Subsequently, an excimer laser was used to ablate and treat the stromal bed following a second flap lift according to the manifest refraction, leaving a minimal residual stromal bed thickness of greater than 300 µm. For both procedures, mitomycin C 0.02% was applied to the stromal bed before the flap was replaced and a bandage contact lens applied.

Results:

Reductions in corneal haze were observed, following PTK to the corneal flap with or without photorefractive keratectomy (PRK) to the stromal bed, both clinically and on imaging. No significant changes in uncorrected distance visual acuity (
P
= .442) and corrected distance visual acuity (
P
= .565) were observed. Improvements were observed for both spherical equivalent refractive errors (
P
= .036) and corneal light backscatter (
P
= .019). There were significant improvements in spherical aberrations (
P
= .014) but no changes in total lower and higher order aberrations.

Conclusions:
PTK to the corneal flap with or without subsequent stromal bed PRK is an effective technique in treating corneal haze following presbyopic inlay explantation.

[
J Refract Surg
. 2023;39(9):639–646.]