bluuebunny/crossref_metadata_2025_split huggingface dataset:
Transcription factor CaNAC1 regulates low-temperature-induced phospholipid degradation in green bell pepper
Authors: Kong Xi-man , Zhou Qian , Zhou Xin , Wei Bao-dong , Ji Shu-juan 
Published: October 2019

Abstract
Phospholipids constitute the main component of biomembranes. During low-temperature storage and transportation of harvested bell peppers, chilling injury participates in pepper decay. A primary cause of pepper chilling injury is phospholipid degradation. In this study, three phospholipase D (PLD)-encoding genes were identified from bell peppers and their activity were analyzed under cold stress. Low temperatures induced strong accumulation of the CaPLDα4 transcript, suggesting that this induction contributes to the phenomenon of phospholipid degradation and cell membrane destruction at 4°C. Low temperatures also significantly induced the transcript amounts of NAM-ATAF1/2-CUC2 (NAC) domain transcription factor. CaNAC1 was found to possess the capacity to interact with the promoter of CaPLD4 in a yeast one-hybrid screen. Furthermore, electrophoretic mobility shift and ß-glucuronidase reporter assays demonstrated that CaNAC1 binds to the CTGCAG motif in the CaPLDα4 promoter, thereby activating its transcription and controlling phospholipid degradation. The ubiquitination sites of the CaNAC1 protein were also characterized by liquid chromatography tandem-mass spectrometry. In conclusion, CaNAC1 is a transcriptional activator of CaPLDα4 and is suggested to participate in membrane lipid degradation of bell peppers when stored at low temperature.
Jewish Nationalism and Indifference between Posen and Poznań: The Jewish People’s Council, 1918–1920*
Authors: Rybak Jan 
Published: October 2019

Abstract
This article analyses the role of the Jüdischer Volksrat—the Jewish People’s Council—in Posen/Poznań between 1918 and 1920. In establishing this institution, Zionist activists gained a significant amount of influence in a traditionally German-acculturated Jewish space during the period of transition from German to Polish rule in the city. Claiming to represent the city’s ‘third nation’ and making demands for Jewish national autonomy, the Jüdischer Volksrat was instrumental in reshaping intercommunity relations and the Jews’ place in society, winning the support of sizeable sections of the Jewish population. This article argues that these successes can be attributed not to the reception of grand ideological concepts of Jewish nationalism, but rather to the fact that Jüdischer Volksrat activists played a central role in people’s everyday lives. They provided economic support, food deliveries, legal aid, and collective security, thereby placing themselves at the centre of the community. The article shows, however, that contrary to activists’ hopes, support for the Volksrat did not necessarily mean an immediate acceptance of Jewish-national concepts. As the debates around the establishment of a Jewish school illustrate, support for national claims and institutions was primarily situational and related to immediate local pressures.
What is the physics behind the Larson mass–size relation?
Authors: Ballesteros-Paredes J , Román-Zúñiga C , Salomé Q , Zamora-Avilés M , Jiménez-Donaire M J 
Published: October 2019

ABSTRACTDifferent studies have reported a power-law mass–size relation M ∝ Rq for ensembles of molecular clouds. In the case of nearby clouds, the index of the power-law q is close to 2. However, for clouds spread all over the Galaxy, indexes larger than 2 are reported. We show that indexes larger than 2 could be the result of line-of-sight superposition of emission that does not belong to the cloud itself. We found that a random factor of gas contamination, between 0.001 per cent and 10 per cent of the line of sight, allows to reproduce the mass–size relation with q ∼ 2.2–2.3 observed in Galactic CO surveys. Furthermore, for dense cores within a single cloud, or molecular clouds within a single galaxy, we argue that, even in these cases, there is observational and theoretical evidence that some degree of superposition may be occurring. However, additional effects may be present in each case, and are briefly discussed. We also argue that defining the fractal dimension of clouds via the mass–size relation is not adequate, since the mass is not necessarily a proxy to the area, and the size reported in M−R relations is typically obtained from the square root of the area, rather than from an estimation of the size independent from the area. Finally, we argue that the statistical analysis of finding clouds satisfying the Larson’s relations does not mean that each individual cloud is in virial equilibrium.
Fractional polarization of extragalactic sources in the 500 deg2 SPTpol survey
Authors: Gupta N , Reichardt C L , Ade P A R , Anderson A J , Archipley M , Austermann J E , Avva J S , Beall J A , Bender A N , Benson B A , Bianchini F , Bleem L E , Carlstrom J E , Chang C L , Chiang H C , Citron R , Moran C Corbett , Crawford T M , Crites A T , de Haan T , Dobbs M A , Everett W , Feng C , Gallicchio J , George E M , Gilbert A , Halverson N W , Harrington N , Henning J W , Hilton G C , Holder G P , Holzapfel W L , Hou Z , Hrubes J D , Huang N , Hubmayr J , Irwin K D , Knox L , Lee A T , Li D , Lowitz A , Luong-Van D , Marrone D P , McMahon J J , Meyer S S , Mocanu L M , Mohr J J , Montgomery J , Nadolski A , Natoli T , Nibarger J P , Noble G I , Novosad V , Padin S , Patil S , Pryke C , Ruhl J E , Saliwanchik B R , Sayre J T , Schaffer K K , Shirokoff E , Sievers C , Smecher G , Staniszewski Z , Stark A A , Story K T , Switzer E R , Tucker C , Vanderlinde K , Veach T , Vieira J D , Wang G , Whitehorn N , Williamson R , Wu W L K , Yefremenko V , Zhang L 
Published: October 2019

ABSTRACT
We study the polarization properties of extragalactic sources at 95 and 150 GHz in the SPTpol 500 deg2 survey. We estimate the polarized power by stacking maps at known source positions, and correct for noise bias by subtracting the mean polarized power at random positions in the maps. We show that the method is unbiased using a set of simulated maps with similar noise properties to the real SPTpol maps. We find a flux-weighted mean-squared polarization fraction 〈p2〉 = [8.9 ± 1.1] × 10−4 at 95 GHz and [6.9 ± 1.1] × 10−4 at 150 GHz for the full sample. This is consistent with the values obtained for a subsample of active galactic nuclei. For dusty sources, we find 95 per cent upper limits of 〈p2〉95 &lt; 16.9 × 10−3 and 〈p2〉150 &lt; 2.6 × 10−3. We find no evidence that the polarization fraction depends on the source flux or observing frequency. The 1σ upper limit on measured mean-squared polarization fraction at 150 GHz implies that extragalactic foregrounds will be subdominant to the CMB E and B mode polarization power spectra out to at least ℓ ≲ 5700 (ℓ ≲ 4700) and ℓ ≲ 5300 (ℓ ≲ 3600), respectively, at 95 (150) GHz.
Discovery of a new WZ Sagittae-type cataclysmic variable in the Kepler/K2 data
Authors: Ridden-Harper R , Tucker B E , Garnavich P , Rest A , Margheim S , Shaya E J , Littlefield C , Barensten G , Hedges C , Gully-Santiago M 
Published: October 2019

ABSTRACT
We identify a new, bright transient in the K2/Kepler Campaign 11 field. Its light curve rises over 7 mag in a day and then declines 3 mag over a month before quickly fading another 2 mag. The transient was still detectable at the end of the campaign. The light curve is consistent with a WZ Sge-type dwarf nova outburst. Early superhumps with a period of 82 min are seen in the first 10 days and suggest that this is the orbital period of the binary, which is typical for the WZ Sge class. Strong superhump oscillations develop 10 days after peak brightness with periods ranging between 83 and 84 min. At 25 days after the peak brightness a bump in the light curve appears to signal a subtle rebrightening phase implying that this was an unusual type-A outburst. This is the only WZ Sge-type system observed by K2/Kepler during an outburst. The early rise of this outburst is well fitted with a broken power law. In first 10 h, the system brightened linearly and then transitioned to a steep rise with a power-law index of 4.8. Looking at archival K2/Kepler data and new TESS observations, a linear rise in the first several hours at the initiation of a superoutburst appears to be common in SU Ursa Majoris stars.
The rotational profiles of cluster galaxies
Authors: Bilton Lawrence E , Hunt Matthew , Pimbblet Kevin A , Roediger Elke 
Published: October 2019

ABSTRACT
We compile two samples of cluster galaxies with complimentary hydrodynamic and N-body analysis using flash code to ascertain how their differing populations drive their rotational profiles and to better understand their dynamical histories. We select our main cluster sample from the X-ray Galaxy Clusters Database (BAX), which are populated with Sloan Digital Sky Survey (SDSS) galaxies. The BAX clusters are tested for the presence of substructures, acting as proxies for core mergers, culminating in sub-samples of eight merging and 25 non-merging galaxy clusters. An additional sample of 12 galaxy clusters with known dumbbell components is procured using galaxy data from the NASA/IPAC Extragalactic Database (NED) to compare against more extreme environments. BAX clusters of each sample are stacked on to a common RA–Dec. space to produce rotational profiles within the range of 0.0–2.5 r200. Merging stacks possess stronger core rotation at ≲0.5r200 primarily contributed by a red galaxy sub-population from relaxing core mergers; this is alongside high rotational velocities from blue galaxy sub-populations, until they mix and homogenize with the red sub-populations at ∼r200, indicative of an infalling blue galaxy sub-population with interactive mixing between both sub-populations at ≳ r200. flash code is utilized to simulate the merger phase between two originally independent clusters and test the evolution of their rotational profiles. Comparisons with the dumbbell clusters leads to the inference that the peculiar core rotations of some dumbbell clusters are the result of the linear motions of core galaxies relaxing on to the potential during post second infall.
New outburst from the luminous supersoft source SSS1 in NGC 300 with periodic modulation
Authors: Carpano S , Haberl F , Maitra C 
Published: October 2019

ABSTRACT
The nearby galaxy NGC 300 is hosting two luminous transient supersoft X-ray sources with bolometric luminosities above 3 × 1038 erg s−1, assuming simple blackbody spectra with temperatures around 60–70 eV. For one of these, SSS1, a periodic modulation of 5.4 h was observed in an XMM–Newton observation from 2001 January 1 lasting 47 ks, but not visible six days earlier when the luminosity was higher. We report here the detection of a new outburst from this source, which occurred during two more recent XMM–Newton observations performed on 2016 December 17–20 lasting for 310 ks. The luminosity was similar as in 2000 December, and the 0.2–2.0 keV light curve revealed again a periodic modulation, with a period of 4.68 ± 0.26 h, significant only in the first of the two observations. Taking into account the large uncertainties (the 2001 period was re-estimated at 5.7 ± 1.1 h), the two values could be marginally compatible, and maybe associated with an orbital period, although the signal strength is highly variable. Due to the new long exposures, an additional absorption feature is now visible in the spectra, which we modelled with an absorption edge. This component decreases the bolometric luminosity below 3 × 1038 erg s−1 and would therefore allow the presence of a white dwarf with a mass close to the Chandrasekhar limit. The system was found in outburst in 1992, 2000, 2008, and 2016 suggesting a possible recurrence period of about eight years. We discuss viable models involving white dwarfs, neutron stars, or black holes.
On the accuracy of symplectic integrators for secularly evolving planetary systems
Authors: Rein Hanno , Brown Garett , Tamayo Daniel 
Published: October 2019

ABSTRACT
Symplectic integrators have made it possible to study the long-term evolution of planetary systems with direct N-body simulations. In this paper we reassess the accuracy of such simulations by running a convergence test on 20 Myr integrations of the Solar System using various symplectic integrators. We find that the specific choice of metric for determining a simulation’s accuracy is important. Only looking at metrics related to integrals of motions such as the energy error can overestimate the accuracy of a method. As one specific example, we show that symplectic correctors do not improve the accuracy of secular frequencies compared to the standard Wisdom–Holman method without symplectic correctors, despite the fact that the energy error is three orders of magnitudes smaller. We present a framework to trace the origin of this apparent paradox to one term in the shadow Hamiltonian. Specifically, we find a term that leads to negligible contributions to the energy error but introduces non-oscillatory errors that result in artificial periastron precession. This term is the dominant error when determining secular frequencies of the system. We show that higher order symplectic methods such as the Wisdom–Holman method with a modified kernel or the SABAC family of integrators perform significantly better in secularly evolving systems because they remove this specific term.
Comparing galaxy clustering in Horizon-AGN simulated light-cone mocks and VIDEO observations
Authors: Hatfield P W , Laigle C , Jarvis M J , Devriendt J , Davidzon I , Ilbert O , Pichon C , Dubois Y 
Published: October 2019

ABSTRACT
Hydrodynamical cosmological simulations have recently made great advances in reproducing galaxy mass assembly over cosmic time – as often quantified from the comparison of their predicted stellar mass functions to observed stellar mass functions from data. In this paper, we compare the clustering of galaxies from the hydrodynamical cosmological simulated light-cone Horizon-AGN to clustering measurements from the VIDEO survey observations. Using mocks built from a VIDEO-like photometry, we first explore the bias introduced into clustering measurements by using stellar masses and redshifts derived from spectral energy distribution fitting, rather than the intrinsic values. The propagation of redshift and mass statistical and systematic uncertainties in the clustering measurements causes us to underestimate the clustering amplitude. We then find that clustering and halo occupation distribution (HOD) modelling results are qualitatively similar in Horizon-AGN and VIDEO. However, at low stellar masses, Horizon-AGN underestimates the observed clustering by up to a factor of ∼3, reflecting the known excess stellar mass to halo mass ratio for Horizon-AGN low-mass haloes, already discussed in previous works. This reinforces the need for stronger regulation of star formation in low-mass haloes in the simulation. Finally, the comparison of the stellar mass to halo mass ratio in the simulated catalogue, inferred from angular clustering, to that directly measured from the simulation validates HOD modelling of clustering as a probe of the galaxy–halo connection.
Quasar and galaxy classification in Gaia Data Release 2
Authors: Bailer-Jones Coryn A L , Fouesneau Morgan , Andrae Rene 
Published: October 2019

ABSTRACT
We construct a supervised classifier based on Gaussian Mixture Models to probabilistically classify objects in Gaia data release 2 (GDR2) using only photometric and astrometric data in that release. The model is trained empirically to classify objects into three classes – star, quasar, galaxy – for G ≥ 14.5 mag down to the Gaia magnitude limit of G = 21.0 mag. Galaxies and quasars are identified for the training set by a cross-match to objects with spectroscopic classifications from the Sloan Digital Sky Survey. Stars are defined directly from GDR2. When allowing for the expectation that quasars are 500 times rarer than stars, and galaxies 7500 times rarer than stars (the class imbalance problem), samples classified with a threshold probability of 0.5 are predicted to have purities of 0.43 for quasars and 0.28 for galaxies, and completenesses of 0.58 and 0.72, respectively. The purities can be increased up to 0.60 by adopting a higher threshold. Not accounting for this expected low frequency of extragalactic objects (the class prior) would give both erroneously optimistic performance predictions and severely impure samples. Applying our model to all 1.20 billion objects in GDR2 with the required features, we classify 2.3 million objects as quasars and 0.37 million objects as galaxies (with individual probabilities above 0.5). The small number of galaxies is due to the strong bias of the satellite detection algorithm and on-ground data selection against extended objects. We infer the true number of quasars and galaxies – as these classes are defined by our training set – to be 690 000 and 110 000, respectively (±50 per cent). The aim of this work is to see how well extragalactic objects can be classified using only GDR2 data. Better classifications should be possible with the low resolution spectroscopy (BP/RP) planned for GDR3.
More than just a wrinkle: a wave-like pattern in Ug versus Lz from Gaia data
Authors: Friske Jennifer K S , Schönrich Ralph 
Published: October 2019

ABSTRACT
We present a newly found wave-like pattern in mean Galactocentric radial velocity ${\overline{U}_\mathrm{ g}}$ versus guiding centre radius Rg or angular momentum Lz of stars in the RV subsample of Gaia DR2. The short-wave pattern has a wavelength of order $1.2 \, {\rm kpc}$ in Rg or $285 \, {\rm kpc}\, {\rm km}\, {\rm s}^{-1}$ in Lz. The pattern shows only weak changes with Galactocentric radius R and little change in strength in particular with the vertical energy Ez of the stars or the distance to the Galactic plane |z|. The pattern is to first order symmetric around the plane, i.e. has no significant odd terms in z. There is a weak phase shift with the pattern moving towards slightly lower Lz (i.e. trailing) with |z| and Ez. However, we observe a highly significant phase shift in Galactic azimuth ϕ, which is different for different peaks. The peak around $L_{z}\sim 2100 \, {\rm kpc}\, {\rm km}\, {\rm s}^{-1}$ only shows a weak change with ϕ, while the rest of the pattern shows a clearly detectable shift of $\text{d} L_{z}/\text{d} \phi = (200 \pm 22) \, {\rm kpc}\, {\rm km}\, {\rm s}^{-1}\, {\rm rad}^{-1}$. If we consider all peaks to belong to the same pattern, this would suggest a wavenumber m = 4. We further find that the wave-like pattern in Ug appears to be related to the ${\overline{W}}$ versus Lz pattern detected in Gaia DR1. A comparison of the ${\overline{U}_\mathrm{ g}}\!-\!L_{z}$ wave pattern with changes of ${\overline{U}_\mathrm{ g}}$ versus R, which have been previously discussed, suggests that the latter can be understood as just the ${\overline{U}_\mathrm{ g}}\!-\!L_{z}$ pattern washed out by blurring (i.e. orbital excursions around their guiding centre) of disc stars.
Deep GMRT 610 MHz observations of the ELAIS N1 field: catalogue and source counts
Authors: Ocran E F , Taylor A R , Vaccari M , Ishwara-Chandra C H , Prandoni I 
Published: October 2019

ABSTRACT
This is the first of a series of papers based on sensitive 610 MHz observations of the ELAIS N1 field, using the Giant Metrewave Radio Telescope. We describe the observations, processing and source catalogue extraction from a deep image with area of 1.86 deg2 and minimum noise of ∼7.1 μJy beam−1. We compile a catalogue of 4290 sources with flux densities in the range of 28.9 μJy– 0.503 Jy and derive the Euclidean-normalized differential source counts for sources with flux densities brighter than $\rm {35.5\, \mu Jy}$. Our counts show a flattening at 610 MHz flux densities below 1 mJy. Below the break the counts are higher than previous observations at this frequency, but generally consistent with recent models of the low-frequency source population. The radio catalogue is cross-matched against multiwavelength data leading to identifications for 92 per cent and reliable redshifts for 72 per cent of our sample, with 19 per cent of the redshifts based on spectroscopy. For the sources with redshifts, we use radio and X-ray luminosity, optical spectroscopy and mid-infrared colours to search for evidence of the presence of an active galactic nucleus (AGN). We compare our identifications to predictions of the flux density distributions of star-forming galaxies (SFGs) and AGN, and find a good agreement assuming the majority of the sources without redshifts are SFGs. We derive spectral index distributions for a sub-sample. The majority of the sources are steep spectra, with a median spectral index that steepens with frequency: $\mathrm{\alpha ^{610}_{325}\, =\, -0.80\, \pm \, 0.29}$, $\mathrm{\alpha ^{610}_{1400}\, =\, -0.83\, \pm \, 0.31}$, and $\mathrm{\alpha ^{610}_{5000}\, =\, -1.12\, \pm \, 0.15}$.
SEVA 3.0: an update of the Standard European Vector Architecture for enabling portability of genetic constructs among diverse bacterial hosts
Authors: Martínez-García Esteban , Goñi-Moreno Angel , Bartley Bryan , McLaughlin James , Sánchez-Sampedro Lucas , Pascual del Pozo Héctor , Prieto Hernández Clara , Marletta Ada Serena , De Lucrezia Davide , Sánchez-Fernández Guzmán , Fraile Sofía , de Lorenzo Víctor 
Published: October 2019

Abstract
The Standard European Vector Architecture 3.0 database (SEVA-DB 3.0, http://seva.cnb.csic.es) is the update of the platform launched in 2013 both as a web-based resource and as a material repository of formatted genetic tools (mostly plasmids) for analysis, construction and deployment of complex bacterial phenotypes. The period between the first version of SEVA-DB and the present time has witnessed several technical, computational and conceptual advances in genetic/genomic engineering of prokaryotes that have enabled upgrading of the utilities of the updated database. Novelties include not only a more user-friendly web interface and many more plasmid vectors, but also new links of the plasmids to advanced bioinformatic tools. These provide an intuitive visualization of the constructs at stake and a range of virtual manipulations of DNA segments that were not possible before. Finally, the list of canonical SEVA plasmids is available in machine-readable SBOL (Synthetic Biology Open Language) format. This ensures interoperability with other platforms and affords simulations of their behaviour under different in vivo conditions. We argue that the SEVA-DB will remain a useful resource for extending Synthetic Biology approaches towards non-standard bacterial species as well as genetically programming new prokaryotic chassis for a suite of fundamental and biotechnological endeavours.