bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Atacama Cosmology Telescope: A Search for Planet 9
Authors: Naess Sigurd , Aiola Simone , Battaglia Nick , Bond Richard J. , Calabrese Erminia , Choi Steve K. , Cothard Nicholas F. , Halpern Mark , Hill J. Colin , Koopman Brian J. , Devlin Mark , McMahon Jeff , Dicker Simon , Duivenvoorden Adriaan J. , Dunkley Jo , Fanfani Valentina , Ferraro Simone , Gallardo Patricio A. , Guan Yilun , Han Dongwon , Hasselfield Matthew , Hincks Adam D. , Huffenberger Kevin , Kosowsky Arthur B. , Louis Thibaut , Macinnis Amanda , Madhavacheril Mathew S. , Nati Federico , Niemack Michael D. , Page Lyman , Salatino Maria , Schaan Emmanuel , Orlowski-Scherer John , Schillaci Alessandro , Schmitt Benjamin , Sehgal Neelima , Sifón Cristóbal , Staggs Suzanne , Engelen Alexander Van , Wollack Edward J. 
Published: December 2021

Abstract
We use Atacama Cosmology Telescope (ACT) observations at 98 GHz (2015–2019), 150 GHz (2013–2019), and 229 GHz (2017–2019) to perform a blind shift-and-stack search for Planet 9. The search explores distances from 300 au to 2000 au and velocities up to 6.′3 per year, depending on the distance (r). For a 5 Earth-mass Planet 9 the detection limit varies from 325 au to 625 au, depending on the sky location. For a 10 Earth-mass planet the corresponding range is 425 au to 775 au. The predicted aphelion and most likely location of the planet corresponds to the shallower end of these ranges. The search covers the whole 18,000 square degrees of the ACT survey. No significant detections are found, which is used to place limits on the millimeter-wave flux density of Planet 9 over much of its orbit. Overall we eliminate roughly 17% and 9% of the parameter space for a 5 and 10 Earth-mass Planet 9, respectively. These bounds approach those of a recent INPOP19a ephemeris-based analysis, but do not exceed it. We also provide a list of the 10 strongest candidates from the search for possible follow-up. More generally, we exclude (at 95% confidence) the presence of an unknown solar system object within our survey area brighter than 4–12 mJy (depending on position) at 150 GHz with current distance 300 au < r < 600 au and heliocentric angular velocity

1
.′
5

yr

−
1

<
v
·

500

au

r

<
2
.″
3

yr

−
1

, corresponding to low-to-moderate eccentricities. These limits worsen gradually beyond 600 au, reaching 5–15 mJy by 1500 au.
Swift/XRT Deep Galactic Plane Survey Discovery of a New Intermediate Polar Cataclysmic Variable, Swift J183920.1-045350
Authors: Gorgone Nicholas M. , Woudt Patrick A. , Buckley David , Mukai Koji , Kouveliotou Chryssa , Huppenkothen Daniela , Göğüş Ersin , Bellm Eric , Linford Justin D. , van der Horst Alexander J. , Baring Matthew G. , Hartmann Dieter , Barrett Paul , Cenko Bradley , Graham Melissa , Granot Johnathan , Harrison Fiona , Kennea Jamie , O’Connor Brendan M. , Potter Stephen , Stern Daniel , Slane Patrick , Wijers Ralph 
Published: December 2021

Abstract
We report on the Swift/XRT Deep Galactic Plane Survey discovery and multiwavelength follow-up observations of a new intermediate polar (IP) cataclysmic variable, Swift J183920.1-045350. A 449.7 s spin period is found in XMM-Newton and NuSTAR data, accompanied by a 459.9 s optical period that is most likely the synodic, or beat period, produced from a 5.6 hr orbital period. The orbital period is seen with moderate significance in independent long-baseline optical photometry observations taken with the ZTF and SAAO telescopes. We find that the X-ray pulse fraction of the source decreases with increasing energy. The X-ray spectra are consistent with the presence of an Fe emission line complex with both local and interstellar absorption. In the optical spectra, strong Hα, H i, He i, and He ii emission lines are observed, all common features in magnetic CVs. The source properties are thus typical of known IPs, with the exception of its estimated distance of

2.26

−
0.83

+
1.93

kpc, which is larger than typical, extending the reach of the CV population in our Galaxy.
Why is it So Hot in Here? Exploring Population Trends in Spitzer Thermal Emission Observations of Hot Jupiters Using Planet-specific, Self-consistent Atmospheric Models
Authors: Goyal Jayesh M. , Lewis Nikole K. , Wakeford Hannah R. , MacDonald Ryan J. , Mayne Nathan J. 
Published: December 2021

Abstract
Thermal emission has now been observed from dozens of exoplanet atmospheres, opening the gateway to population-level characterization. Here, we provide theoretical explanations for observed trends in Spitzer IRAC channel 1 (3.6 μm) and channel 2 (4.5 μm) photometric eclipse depths (EDs) across a population of 34 hot Jupiters. We apply planet-specific, self-consistent atmospheric models, spanning a range of recirculation factors, metallicities, and C/O ratios, to probe the information content of Spitzer secondary eclipse observations across the hot-Jupiter population. We show that most hot Jupiters are inconsistent with blackbodies from Spitzer observations alone. We demonstrate that the majority of hot Jupiters are consistent with low-energy redistribution between the dayside and nightside (hotter dayside than expected with efficient recirculation). We also see that high-equilibrium temperature planets (T
eq ≥ 1800 K) favor inefficient recirculation in comparison to the low temperature planets. Our planet-specific models do not reveal any definitive population trends in metallicity and C/O ratio with current data precision, but more than 59% of our sample size is consistent with the C/O ratio ≤ 1 and 35% are consistent with whole range (0.35 ≤ C/O ≤ 1.5). We also find that for most of the planets in our sample, 3.6 and 4.5 μm model EDs lie within ±1σ of the observed EDs. Intriguingly, few hot Jupiters exhibit greater thermal emission than predicted by the hottest atmospheric models (lowest recirculation) in our grid. Future spectroscopic observations of thermal emission from hot Jupiters with the James Webb Space Telescope will be necessary to robustly identify population trends in chemical compositions with its increased spectral resolution, range, and data precision.
Small Protoplanetary Disks in the Orion Nebula Cluster and OMC1 with ALMA
Authors: Otter Justin , Ginsburg Adam , Ballering Nicholas P. , Bally John , Eisner J. A. , Goddi Ciriaco , Plambeck Richard , Wright Melvyn 
Published: December 2021

Abstract
The Orion Nebula Cluster (ONC) is the nearest dense star-forming region at ∼400 pc away, making it an ideal target to study the impact of high stellar density and proximity to massive stars (the Trapezium) on protoplanetary disk evolution. The OMC1 molecular cloud is a region of high extinction situated behind the Trapezium in which actively forming stars are shielded from the Trapezium’s strong radiation. In this work, we survey disks at high resolution with Atacama Large Millimeter/submillimeter Array at three wavelengths with resolutions of 0.″095 (3 mm; Band 3), 0.″048 (1.3 mm; Band 6), and 0.″030 (0.85 mm; Band 7) centered on radio Source I. We detect 127 sources, including 15 new sources that have not previously been detected at any wavelength. 72 sources are spatially resolved at 3 mm, with sizes from ∼8–100 au. We classify 76 infrared-detected sources as foreground ONC disks and the remainder as embedded OMC1 disks. The two samples have similar disk sizes, but the OMC1 sources have a dense and centrally concentrated spatial distribution, indicating they may constitute a spatially distinct subcluster. We find smaller disk sizes and a lack of large (>75 au) disks in both our samples compared to other nearby star-forming regions, indicating that environmental disk truncation processes are significant. While photoevaporation from nearby massive Trapezium stars may account for the smaller disks in the ONC, the embedded sources in OMC1 are hidden from this radiation and thus must truncated by some other mechanism, possibly dynamical truncation or accretion-driven contraction.
Near-infrared Supernova Ia Distances: Host Galaxy Extinction and Mass-step Corrections Revisited
Authors: Johansson J. , Cenko S. B. , Fox O. D. , Dhawan S. , Goobar A. , Stanishev V. , Butler N. , Lee W. H. , Watson A. M. , Fremling U. C. , Kasliwal M. M. , Nugent P. E. , Petrushevska T. , Sollerman J. , Yan L. , Burke J. , Hosseinzadeh G. , Howell D. A. , McCully C. , Valenti S. 
Published: December 2021

Abstract
We present optical and near-infrared (NIR, Y-, J-,
H-band) observations of 42 Type Ia supernovae (SNe Ia) discovered by the untargeted intermediate Palomar Transient Factory survey. This new data set covers a broad range of redshifts and host galaxy stellar masses, compared to previous SN Ia efforts in the NIR. We construct a sample, using also literature data at optical and NIR wavelengths, to examine claimed correlations between the host stellar masses and the Hubble diagram residuals. The SN magnitudes are corrected for host galaxy extinction using either a global total-to-selective extinction ratio, R

V
= 2.0, for all SNe, or a best-fit R

V
for each SN individually. Unlike previous studies that were based on a narrower range in host stellar mass, we do not find evidence for a “mass step,” between the color- and stretch-corrected peak J and H magnitudes for galaxies below and above

log
(

M

*

/

M

⊙

)
=
10

. However, the mass step remains significant (3σ) at optical wavelengths (g, r, i) when using a global R

V
, but vanishes when each SN is corrected using their individual best-fit R

V
. Our study confirms the benefits of the NIR SN Ia distance estimates, as these are largely exempted from the empirical corrections dominating the systematic uncertainties in the optical.
Rare Event Sampling Improves Mercury Instability Statistics
Authors: Abbot Dorian S. , Webber Robert J. , Hadden Sam , Seligman Darryl , Weare Jonathan 
Published: December 2021

Abstract
Due to the chaotic nature of planetary dynamics, there is a non-zero probability that Mercury’s orbit will become unstable in the future. Previous efforts have estimated the probability of this happening between 3 and 5 billion years in the future using a large number of direct numerical simulations with an N-body code, but were not able to obtain accurate estimates before 3 billion years in the future because Mercury instability events are too rare. In this paper we use a new rare-event sampling technique, Quantile Diffusion Monte Carlo (QDMC), to estimate that the probability of a Mercury instability event in the next 2 billion years is approximately 10−4 in the REBOUND N-body code. We show that QDMC provides unbiased probability estimates at a computational cost of up to 100 times less than direct numerical simulation. QDMC is easy to implement and could be applied to many problems in planetary dynamics in which it is necessary to estimate the probability of a rare event.
Star-forming Dwarf Galaxies in Filamentary Structures around the Virgo Cluster: Probing Chemical Pre-processing in Filament Environments
Authors: Chung Jiwon , Kim Suk , Rey Soo-Chang , Lee Youngdae 
Published: December 2021

Abstract
It has been proposed that the filament environment is closely connected to the pre-processing of galaxies, where their properties may have been changed by environmental effects in the filament before they fell into the galaxy cluster. We present the chemical properties of star-forming dwarf galaxies (SFDGs) in five filamentary structures (Virgo III, Leo Minor, Leo II A, Leo II B, and Canes Venatici) around the Virgo cluster using the Sloan Digital Sky Survey optical spectroscopic data and Galaxy Evolution Explorer ultraviolet photometric data. We investigate the relationship between stellar mass, gas-phase metallicity, and specific star formation rate (sSFR) of the SFDGs in the Virgo filaments in comparison to those in the Virgo cluster and field. We find that, at a given stellar mass, SFDGs in the Virgo filaments show lower metallicity and higher sSFR than those in the Virgo cluster on average. We observe that SFDGs in the Virgo III filament show enhanced metallicities and suppressed star formation activities comparable to those in the Virgo cluster, whereas SFDGs in the other four filaments exhibit similar properties to the field counterparts. Moreover, about half of the galaxies in the Virgo III filament are found to be morphologically transitional dwarf galaxies that are supposed to be on the way to transforming into quiescent dwarf early-type galaxies. Based on the analysis of the galaxy perturbation parameter, we propose that the local environment represented by the galaxy interactions might be responsible for the contrasting features in chemical pre-processing found in the Virgo filaments.
VLA and NOEMA Views of Bok Globule CB 17: The Starless Nature of a Proposed First Hydrostatic Core Candidate
Authors: Spear Stephanie , José Maureira María , Arce Héctor G. , Pineda Jaime E. , Dunham Michael , Caselli Paola , Segura-Cox Dominique 
Published: December 2021

Abstract
We use 3 mm continuum NOrthern Extended Millimeter Array and NH3 Very Large Array observations toward the First Hydrostatic Core (FHSC) candidate CB 17 MMS in order to reveal the dust structure and gas properties to 600–1100 au scales and to constrain its evolutionary stage. We do not detect any compact source at the previously identified 1.3 mm point source, despite expecting a minimum signal-to-noise ratio of 9. The gas traced by NH3 exhibits subsonic motions, with an average temperature of 10.4 K. A fit of the radial column density profile derived from the ammonia emission finds a flat inner region of radius ∼1800 au and a central density of ∼6 × 105 cm−3. Virial and density structure analysis reveals the core is marginally bound (α
vir = 0.73). The region is entirely consistent with that of a young starless core, hence ruling out CB 17 MMS as an FHSC candidate. Additionally, the core exhibits a velocity gradient aligned with the major axis, showing an arc-like structure in the position–velocity diagram and an off-center region with high velocity dispersion, caused by two distinct velocity peaks. These features could be due to interactions with the nearby outflow, which appears to deflect due to the dense gas near the NH3 column density peak. We investigate the specific angular momentum profile of the starless core, finding that it aligns closely with previous studies of similar radial profiles in Class 0 sources. This similarity to more evolved objects suggests that motions at 1000 au scales are determined by large-scale dense cloud motions, and may be preserved throughout the early stages of star formation.
SILVERRUSH. XI. Constraints on the Lyα Luminosity Function and Cosmic Reionization at z = 7.3 with Subaru/Hyper Suprime-Cam
Authors: Goto Hinako , Shimasaku Kazuhiro , Yamanaka Satoshi , Momose Rieko , Ando Makoto , Harikane Yuichi , Hashimoto Takuya , Inoue Akio K. , Ouchi Masami 
Published: December 2021

Abstract
The Lyα luminosity function (LF) of Lyα emitters (LAEs) has been used to constrain the neutral hydrogen fraction in the intergalactic medium (IGM) and thus the timeline of cosmic reionization. Here we present the results of a new narrowband imaging survey for z = 7.3 LAEs in a large area of ∼3 deg2 with Subaru/Hyper Suprime-Cam. No LAEs are detected down to L
Lyα
≃ 1043.2 erg s−1 in an effective cosmic volume of ∼2 × 106 Mpc3, placing an upper limit on the bright part of the z = 7.3 Lyα LF for the first time and confirming a decrease in bright LAEs from z = 7.0. By comparing this upper limit with the Lyα LF in the case of fully ionized IGM, which is predicted using an observed z = 5.7 Lyα LF on the assumption that the intrinsic Lyα LF evolves in the same way as the UV LF, we obtain the relative IGM transmission

T

Ly
α

IGM

(
7.3
)

/

T

Ly
α

IGM

(
5.7
)
<
0.77

and then the volume-averaged neutral fraction x
H I(7.3) > 0.28. Cosmic reionization is thus still ongoing at z = 7.3, consistent with results from other x
H I estimation methods. A similar analysis using literature Lyα LFs finds that at z = 6.6 and 7.0, the observed Lyα LF agrees with the predicted one, consistent with full ionization.
Radio Proper Motions of the Energetic Pulsar PSR J1813–1749
Authors: Dzib Sergio A. , Rodríguez Luis F. 
Published: December 2021

Abstract
PSR J1813–1749 has peculiarities that make it a very interesting object of study. It is one of the most energetic and the most scattered pulsars known. It is associated with HESS J1813–178, one of the brightest and most compact TeV sources in the sky. Recently, Ho et al. used archival X-ray Chandra observations separated by more than 10 yr and determined that the total proper motion of PSR J1813–1749 is ∼66 mas yr−1, corresponding to a velocity of ∼1900 km s−1 for a distance of 6.2 kpc. These results would imply that this pulsar is the fastest neutron star known in the Galaxy and, by estimating the angular separation with respect to the center of the associated supernova remnant, has an age of only ∼300 yr, making it one of the youngest pulsars known. Using archival high angular resolution VLA observations taken over 12 yr we have estimated the radio proper motions of PSR J1813–1748 to be much smaller: (

μ

α

·
cos
(
δ
)
,

μ

δ

) = (−5.0 ± 3.7, −13.2 ± 6.7) mas yr−1, or a total proper motion of 14.8 ± 5.9 mas yr−1. The positions referenced against quasars make our results reliable. We conclude that PSR J1813–1749 is not a very fast moving source. Its kinematic age using the new total proper motion is ∼1350 yr. This age is consistent within a factor of a few with the characteristic age of the pulsar and with the age estimated from the broadband spectral energy distribution of HESS J1813–178, as well as the age of the associated supernova remnant.
Weak Damping of Propagating MHD Kink Waves in the Quiescent Corona
Authors: Morton Richard J. , Tiwari Ajay K. , Van Doorsselaere Tom , McLaughlin James A. 
Published: December 2021

Abstract
Propagating transverse waves are thought to be a key transporter of Poynting flux throughout the Sun’s atmosphere. Recent studies have shown that these transverse motions, interpreted as the magnetohydrodynamic kink mode, are prevalent throughout the corona. The associated energy estimates suggest the waves carry enough energy to meet the demands of coronal radiative losses in the quiescent Sun. However, it is still unclear how the waves deposit their energy into the coronal plasma. We present the results from a large-scale study of propagating kink waves in the quiescent corona using data from the Coronal Multi-channel Polarimeter (CoMP). The analysis reveals that the kink waves appear to be weakly damped, which would imply low rates of energy transfer from the large-scale transverse motions to smaller scales via either uniturbulence or resonant absorption. This raises questions about how the observed kink modes would deposit their energy into the coronal plasma. Moreover, these observations, combined with the results of Monte Carlo simulations, lead us to infer that the solar corona displays a spectrum of density ratios, with a smaller density ratio (relative to the ambient corona) in quiescent coronal loops and a higher density ratio in active-region coronal loops.
Die Linke . Analyse d’un quasi-désastre électoral
Authors: Landwehrlen Thomas 
Published: December 2021

Die Linke apparaît de loin comme le principal perdant des élections fédérales allemandes de 2021. Avec seulement 4,9 % des voix, le parti de la gauche radicale allemande a enregistré sa plus mauvaise performance à un scrutin fédéral depuis sa création en 2007, et n’est parvenu à sauver sa représentation parlementaire au Bundestag que par l’élection directe de trois de ses candidats de circonscription. Par rapport au précédent scrutin de 2017, le parti a perdu un peu plus de deux millions de suffrages, soit près de 53 % de son électorat. Résultat : sur les 736 nouveaux députés entrés au Bundestag à l’issue des élections, seuls 39 portent les couleurs de La Gauche, qui dispose désormais du plus petit groupe parlementaire d’opposition à la chambre basse du Parlement allemand. L’ampleur de la défaite électorale subie par Die Linke ne peut qu’interroger. Après en avoir dressé un état des lieux, le présent article souhaite ainsi en présenter les causes. Sont-elles conjoncturelles ou structurelles ? Sont-elles spécifiques à l’Allemagne ou déploient-elles aussi leurs effets au-delà des frontières de la République fédérale ? Le déclin électoral du parti étant repérable dès 2012-2013, il apparaît que les facteurs explicatifs conjoncturels ne sont pas les plus déterminants. Des facteurs bien plus profonds sont responsables de la débâcle électorale de Die Linke , tels que la progressive érosion de sa spécificité programmatique ou le déplacement du vote protestataire au profit de l’AfD dans les Länder de l’Est.
Le laboratoire environnemental latino-américain au XXI e siècle
Authors: Gautreau Pierre 
Published: December 2021

Source intarissable de modèles et de contre-modèles pour penser la question environnementale contemporaine, l’Amérique latine occupe une place singulière sur la scène internationale au xxi e siècle. Cet article montre en quoi cette situation a pu entraîner des analyses biaisées des innovations que cet ensemble de pays a développé, en magnifiant certaines ou en invisibilisant d’autres. Les analyses critiques du « bilan » environnemental de la période négligent en général trois processus : la globalisation segmentaire des questions environnementales latino-américaines, la profondeur des contraintes politiques contraires aux volontés de régulation environnementale, ainsi que des évolutions décoloniales complexes. En décalant le regard, plusieurs phénomènes peuvent être considérés comme caractéristiques du continent, marquant son originalité : le rôle décisif des conflits populaires, la « latinisation » de l’extractivisme, et le maigre bilan de la néolibéralisation de la nature.
Participation des usagers : du champ des possibles aux modalités réelles de représentation
Authors: Scheider-Yilmaz Marion , Morales La Mura Raúl 
Published: December 2021

Au tournant des années 2000, les principes de démocratie participative dans le champ sanitaire ont connu un fort développement en France, déclinant la représentation des usagers dans un nombre important d’espaces de consultation. En cela, ils assoient et légitiment la figure du « représentant des usagers » dans les processus décisionnels visant l’élaboration ou la redéfinition des politiques publiques. Pour le handicap, comme pour les autres secteurs de l’action publique, une place est généralement destinée à cette figure spécifique au sein d’un collège intitulé « représentants des usagers ». À rebours de la consécration du « représentant des usagers » dans les espaces de consultation, nous choisissons de déconstruire cette formulation pour en interroger la pertinence sémantique. Ce sont plus généralement aussi les enjeux démocratiques relatifs à la participation des usagers que nous questionnons.
“Easy to learn” (rTogs par sla ba) (1737) as a source for the study of Tibetan-Mongolian lexicographic relations
Authors: Dorjsuren Burnee 
Published: December 2021

“Easy to learn” is the title of a Tibetan-Mongolian dictionary composed by Гomboǰab (Cl. Mo. mGonbo skyabs) et al. in 1737 for the purpose of teaching the Tibetan language to Mongols. Through a comparative analysis of its macro- and microstructures with related dictionaries, this paper finds that this dictionary was composed based on a Sanskrit and Tibetan lexicography, describes its distinctive lexicographic methodology, and illustrates how this source represents the Mongolian and Tibetan lexicographic relationships.