bluuebunny/crossref_metadata_2025_split huggingface dataset:
Lack of influence of the environment in the earliest stages of massive galaxy formation
Authors: Annunziatella Marianna , Pérez-González Pablo G , García Argumánez Ángela , Barro Guillermo , Alcalde Pampliega Belén , Costantin Luca , Koekemoer Anton M , Mérida Rosa M 
Published: September 2022

ABSTRACT
We investigate how the environment affects the assembly history of massive galaxies. For that purpose, we make use of Survey for High-z Absorption Red and Dead Sources (SHARDS) and HST spectrophotometric data, whose depth, spectral resolution, and wavelength coverage allow to perform a detailed analysis of the stellar emission as well as obtaining unprecedentedly accurate photometric redshifts. This expedites a sufficiently accurate estimate of the local environment and a robust derivation of the star formation histories of a complete sample of 332 massive galaxies (&gt;1010M⊙) at redshift 1 ≤ z ≤ 1.5 in the GOODS-N field. We find that massive galaxies in this redshift range avoid the lowest density environments. Moreover, we observed that the oldest galaxies in our sample with mass-weighted formation redshift $\mathrm{\overline{z}_{M-w} \ge 2.5}$, avoid the highest density regions, preferring intermediate environments. Younger galaxies, including those with active star formation, tend to live in denser environments ($\Sigma = \mathrm{5.0_{1.1}^{24.8}\times 10^{10}\, M_{\odot }\, Mpc^{-2}}$). This behaviour could be expected if those massive galaxies starting their formation first would merge with neighbours and sweep their environment earlier. On the other hand, galaxies formed more recently ($\overline{z}_{M-w} \lt 2.5$) are accreted into large-scale structures at later times and we are observing them before sweeping their environment or, alternatively, they are less likely to affect their environment. However, given that both number and mass surface densities of neighbour galaxies is relatively low for the oldest galaxies, our results reveal a very weak correlation between environment and the first formation stages of the earliest massive galaxies.
X-ray spectral and timing analysis of the Compton Thick Seyfert 2 galaxy NGC 1068
Authors: Pal Indrani , Stalin C S , Parker M L , Agrawal Vivek K , Marchesi S 
Published: September 2022

ABSTRACT
We present the timing and spectral analysis of the Compton Thick Seyfert 2 active galactic nuclei NGC 1068 observed using NuSTAR and XMM–Newton. In this work for the first time we calculated the coronal temperature ($\rm {kT_{e}}$) of the source and checked for its variation between the epochs if any. The data analysed in this work comprised of (a) eight epochs of observations with NuSTAR carried out during the period 2012 December to 2017 November, and, (b) six epochs of observations with XMM–fNewton carried out during 2000 July to 2015 February. From timing analysis of the NuSTAR observations, we found tfhe source not to show any variations in the soft band. However, on examination of the flux at energies beyond 20 keV, during 2014 August and 2017 August the source was brighter by about 20 and 30 per cent, respectively, compared to the mean flux of the three 2012 NuSTAR observations as in agreement with earlier results in literature. From an analysis of XMM–Newton data we found no variation in the hard band (2–4 keV) between epochs as well as within epochs. In the soft band (0.2–2 keV), while the source was found to be not variable within epochs, it was found to be brighter in epoch B relative to epoch A. By fitting physical models we determined $\rm {kT_{e}}$ to range between 8.46$^{+0.39}_{-0.66}$ and 9.13$^{+0.63}_{-0.98}$ keV. From our analysis, we conclude that we found no variation of $\rm {kT_{e}}$ in the source.
Tidal tracks and artificial disruption of cold dark matter haloes
Authors: Benson Andrew J , Du Xiaolong 
Published: September 2022

ABSTRACT
We describe a simple extension to existing models for the tidal heating of dark matter subhaloes which takes into account second-order terms in the impulse approximation for tidal heating. We show that this revised model can accurately match the tidal tracks along which subhaloes evolve as measured in high-resolution N-body simulations. We further demonstrate that, when a constant density core is introduced into a subhalo, this model is able to quantitatively reproduce the evolution and artificial disruption of N-body subhaloes arising from finite resolution effects. Combining these results we confirm prior work indicating that artificial disruption in N-body simulations can result in a factor two underestimate of the subhalo mass function in the inner regions of host haloes, and a 10–20 per cent reduction over the entire virial volume.
The impact of phase equilibrium cloud models on GCM simulations of GJ 1214b
Authors: Christie D A , Mayne N J , Gillard R M , Manners J , Hébrard E , Lines S , Kohary K 
Published: September 2022

ABSTRACT
We investigate the impact of clouds on the atmosphere of GJ 1214b using the radiatively coupled, phase-equilibrium cloud model EddySed coupled to the Unified Model general circulation model. We find that, consistent with previous investigations, high metallicity (100 × solar) and clouds with large vertical extents (a sedimentation factor of fsed = 0.1) are required to best match the observations, although metallicities even higher than those investigated here may be required to improve agreement further. We additionally find that in our case which best matches the observations (fsed = 0.1), the velocity structures change relative to the clear sky case with the formation of a superrotating jet being suppressed, although further investigation is required to understand the cause of the suppression. The increase in cloud extent with fsed results in a cooler planet due to a higher albedo, causing the atmosphere to contract. This also results in a reduced day–night contrast seen in the phase curves, although the introduction of cloud still results in a reduction of the phase offset. We additionally investigate the impact the Unified Model’s pseudo-spherical irradiation scheme on the calculation of heating rates, finding that the introduction of nightside shortwave heating results in slower mid-latitude jets compared to the plane-parallel irradiation scheme used in previous works. We also consider the impact of a gamma distribution, as opposed to a lognormal distribution, for the distribution of cloud particle radii and find the impact to be relatively minor.
The origin of the photospheric emission of GRB 220426A
Authors: Song Xin-Ying , Zhang Shuang-Nan , Ge Ming-Yu , Zhang Shu 
Published: September 2022

ABSTRACT
GRB 220426A is a bright gamma-ray burst (GRB) dominated by the photospheric emission. We perform several tests to speculate the origin of this photospheric emission. The dimensionless entropy η is large, which is not usual if we assume that it is a pure hot fireball launched by neutrino–antineutrino annihilation mechanism only. Moreover, the outflow has larger η with lower luminosity L in the first few seconds, so that the trend of time-resolved η − L can not be described as a monotonically positive correlation between η and L. A hybrid outflow with almost completely thermalized Poynting flux could account for the quasi-thermal spectrum as well as large η. More importantly, the existence of magnetic field could affect the proton density and neutron–proton coupling effect, so that it could account for the observed trend of time-resolved η − L. The other origins for the photospheric emission, such as non-dissipative hybrid outflow or magnetic reconnection, are not supported because their radiation efficiencies are low, which is not consistent with non-detection of the afterglow for GRB 220426A. Therefore, we think the hybrid outflow may be the most likely origin.
The relation between accretion rate and jet power in early-type galaxies with thermally unstable hot atmospheres
Authors: Plšek T , Werner N , Grossová R , Topinka M , Simionescu A , Allen S W 
Published: September 2022

ABSTRACT
We use Chandra X-ray data and Very Large Array radio observations for a sample of 20 nearby, massive, X-ray bright, early-type galaxies to investigate the relation between the Bondi accretion rates and the mechanical jet powers. We find a strong correlation ($\rho = 0.96^{+0.03}_{-0.09}$; BF10 &gt; 100) between the Bondi accretion power, PBondi, and the mechanical jet power, Pjet, for a subsample of 14 galaxies, which also host cool H α+[N ii] line emitting gas and thus likely have thermally unstable atmospheres. The relation between the Bondi accretion power and the mechanical jet power for this subsample is well described by a power-law model $\log \frac{P_{\mathrm{Bondi}}}{{10^{43} \, \mathrm{erg \, s^{-1}}}} = \alpha + \beta \log \frac{P_{\mathrm{jet}}}{{10^{43} \, \mathrm{erg \, s^{-1}}}}$, where α = 1.10 ± 0.25 and β = 1.10 ± 0.24 with an intrinsic scatter $\sigma = 0.08^{+0.14}_{-0.06}$ dex. The results indicate that in all galaxies with thermally unstable atmospheres the cooling atmospheric gas feeds the central black holes at a similar jet-to-Bondi power ratio. For the full sample of 20 galaxies, the correlation is weaker and in a subset of galaxies with no signs of H α+[N ii] emission, we see a hint for a systematically lower jet-to-Bondi power ratio. We also investigate the dependence of jet power on individual quantities in the Bondi formula such as the supermassive black hole mass (M•) and the specific entropy of the gas (K) at the Bondi radius. For the subsample of H α+[N ii] emitting galaxies, we find a very tight correlation of Pjet with M• ($\rho = 0.91^{+0.06}_{-0.11}$; BF10 &gt; 100) and, although poorly constrained, a hint of an anticorrelation for Pjet and K ($\rho = -0.47^{+0.60}_{-0.37}$; BF10 = 1.1).
Spectral and timing properties of the recently discovered Be/X-ray pulsar eRASSUJ 052914.9−662446
Authors: Rai Binay , Ghising Manoj , Tobrej Mohammed , Tamang Ruchi , Paul Bikash Chandra 
Published: September 2022

ABSTRACT
We have presented NuSTAR and Swift observations of the newly discovered Be/X-ray pulsar eRASSU J052914.9−662446. This is the first detailed study of the temporal and spectral properties of the pulsar using 2020 observations. A coherent pulsation of 1411.5 ± 0.5 s was detected from the source. The pulse profile was found to resemble a simple single-peaked feature that may be due to emission from the surface of the neutron star only. Pulse profiles are highly energy dependent. The variation of the pulse fraction of the pulse profiles is found to be non-monotonic with energy. The 0.5–20 keV Swift and NuSTAR simultaneous can be fitted well with power law modified by high-energy cut-off of ∼5.7 keV. The NuSTAR luminosity in the 0.5–79 keV energy range was ∼7.9 × 1035$\text{erg}\,\text{s}^{ -1}\,$. The spectral flux in 3–79 keV shows modulation with the pulse phase.
QU Vul: An integral field spectroscopy case study of a nova shell
Authors: Santamaría E , Guerrero M A , Toalá J A , Ramos-Larios G , Sabin L 
Published: September 2022

ABSTRACT
We present GTC MEGARA high-dispersion integral field spectroscopic observations of the nova remnant QU Vul, which provide a comprehensive 3D view of this nova shell. The tomographic analysis of the H α emission reveals a complex physical structure characterized by an inhomogeneous and clumpy distribution of the material within this shell. The overall structure can be described as a prolate ellipsoid with an axial ratio of 1.4 ± 0.2, a major axis inclination with the line of sight of 12° ± 6°, and polar and equatorial expansion velocities ≈560 km s−1 and 400 ± 60 km s−1, respectively. The comparison of the expansion velocity on the plane of the sky with the angular expansion implies a distance of 1.43 ± 0.23 kpc. The ionized mass is found to be ≈2 × 10−4 M⊙, noting that the information on the 3D distribution of material within the nova shell has allowed us to reduce the uncertainty on its filling factor. The nova shell is still in its free expansion phase, which can be expected as the ejecta mass is much larger than the swept-up circumstellar medium mass. The 3D distribution and radial velocity of material within the nova shell provide an interpretation of the so-called ‘castellated’ line profiles observed in early optical spectra of nova shells, which can be attributed to knots and clumps moving radially along different directions.
High-altitude meteors detected by the interferometric MU radar
Authors: Kastinen Daniel , Kero Johan 
Published: September 2022

ABSTRACTWe have re-analysed part of the middle and upper atmosphere (MU) radar meteor head echo data set collected during 2009–2010 and confirmed the existence of a rare high-altitude radar meteor population reaching up to ∼150 km altitude. The number of detections decreases significantly as a function of initial altitude. Out of the total amount of 106 000 events, 74 had an initial altitude &gt;130 km while four of those had an initial altitude &gt;145 km. High-altitude radar meteor observations have been reported before, e.g. using the EISCAT VHF radar and the Jicamarca Radio Observatory. The main novelty of this study is that the observations were performed using methods that render the final data set unambiguous in direction of arrival together with rigorously tested analysis routines that were validated by noisy raw data simulations. Due to our experimental set-up the maximum detectable range was limited to 148 km. Hence, we cannot confirm or deny the existence of radar meteors above that altitude.
Abundance matching analysis of the emission-line galaxy sample in the extended Baryon Oscillation Spectroscopic Survey
Authors: Lin Sicheng , Tinker Jeremy L , Blanton Michael R , Guo Hong , Raichoor Anand , Comparat Johan , Brownstein Joel R 
Published: September 2022

ABSTRACT
We present the measurements of the small-scale clustering for the emission-line galaxy (ELG) sample from the extended Baryon Oscillation Spectroscopic Survey (eBOSS) in the Sloan Digital Sky Survey IV (SDSS-IV). We use conditional abundance matching method to interpret the clustering measurements from 0.34 to $70\, h^{-1}\, \textrm {Mpc}$. In order to account for the correlation between properties of ELGs and their environment, we add a secondary connection between star formation rate of ELGs and halo accretion rate. Three parameters are introduced to model the ELG [O ii] luminosity and to mimic the target selection of eBOSS ELGs. The parameters in our models are optimized using Markov Chain Monte Carlo (MCMC) method. We find that by conditionally matching star formation rate of galaxies and the halo accretion rate, we are able to reproduce the eBOSS ELG small-scale clustering within 1σ error level. Our best-fitting model shows that the eBOSS ELG sample only consists of $\sim 12{{\ \rm per\ cent}}$ of all star-forming galaxies, and the satellite fraction of eBOSS ELG sample is 19.3 per cent. We show that the effect of assembly bias is $\sim 20{{\ \rm per\ cent}}$ on the two-point correlation function and $\sim 5{{\ \rm per\ cent}}$ on the void probability function at scale of $r\sim 20 \, h^{-1}\, \rm Mpc$.
A detailed star formation history for the extremely diffuse Andromeda XIX dwarf galaxy
Authors: Collins Michelle L M , Williams Benjamin F , Tollerud Erik J , Balbinot Eduardo , Gilbert Karoline M , Dolphin Andrew 
Published: September 2022

ABSTRACT
We present deep imaging of the ultradiffuse Andromeda XIX dwarf galaxy from the Advance Camera for Surveys on the Hubble Space Telescope which resolves its stellar populations to below the oldest main-sequence turn-off. We derive a full star formation history for the galaxy using match, and find no evidence of star formation in the past 8 Gyr. We calculate a quenching time of τ90 = 9.7 ± 0.2 Gyr, suggesting And XIX ceased forming stars very early on. This early quenching, combined with its extremely large half-light radius, low-density dark matter halo and lower than expected metallicity make it a unique galaxy within the Local Group and raises questions about how it formed. The early quenching time allows us to rule out feedback from bursty star formation as a means to explain its diffuse stellar population and low-density dark matter halo. We find that the extended stellar population, low-density halo, and star formation could be explained by either tidal interactions (such as tidal shocking) or by late dry mergers, with the latter also explaining its low metallicity. Proper motions and detailed abundances would allow us to distinguish between these two scenarios.
Astrometry of variable compact radio sources: a search for Galactic black hole X-ray binaries
Authors: Atri P , Miller-Jones J C A , Bahramian A , Plotkin R M , Maccarone T J , Marcote B , Heinke C O , Sivakoff G R , Ginsburg A , Strader J , Chomiuk L 
Published: September 2022

ABSTRACT
We use the Very Long Baseline Array to conduct high precision astrometry of a sample of 33 compact, flat spectrum, variable radio sources in the direction of the Galactic plane (Becker et al. 2010). Although Becker et al. (2010) ruled out a few potential scenarios for the origin of the radio emission, the study could not rule out that these sources were black hole X-ray binaries (BHXBs). Most known BHXBs are first detected by X-ray or optical emission when they go into an outburst, leaving the larger quiescent BHXB population undiscovered. In this paper, we attempt to identify any Galactic sources amongst the Becker et al. (2010) sample by measuring their proper motions as a first step to finding quiescent BHXB candidates. Amongst the 33 targets, we could measure the proper motion of six sources. We find that G32.7193-0.6477 is a Galactic source and are able to constrain the parallax of this source with a 3σ significance. We found three strong Galactic candidates, G32.5898-0.4468, G29.1075-0.1546, and G31.1494-0.1727, based purely on their proper motions, and suggest that G29.1075-0.1546 is also likely Galactic. We detected two resolved targets for multiple epochs (G30.1038+0.3984 and G29.7161-0.3178). We find six targets are only detected in one epoch and have an extended structure. We cross-match our VLBA detections with the currently available optical, infrared, and X-ray surveys, and did not find any potential matches. We did not detect 19 targets in any VLBA epochs and suggest that this could be due to limited uv-coverage, drastic radio variability, or faint, extended nature of the sources.
Analysis of eight magnetic chemically peculiar stars with rotational modulation
Authors: Kobzar O , Khalack V , Bohlender D , Mathys G , Shultz M E , Bowman D M , Paunzen E , Lovekin C , David-Uraz A , Sikora J , Lampens P , Richard O 
Published: September 2022

ABSTRACT
Since the end of 2018, the Transiting Exoplanet Survey Satellite (TESS) has provided stellar photometry to the astronomical community. We have used TESS data to study rotational modulation in the light curves of a sample of chemically peculiar stars with measured large-scale magnetic fields (mCP stars). In general, mCP stars show inhomogeneous distributions of elements in their atmospheres that lead to spectroscopic (line profile) and photometric (light curve) variations commensurate with the rotational period. We analyzed the available TESS data from 50 sectors for eight targets after post-processing them in order to minimize systematic instrumental trends. Analysis of the light curves allowed us to determine rotational periods for all eight of our targets. For each star, we provide a phase diagram calculated using the derived period from the light curves and from the available measurements of the disc-averaged longitudinal magnetic field 〈Bz〉. In most cases, the phased light curve and 〈Bz〉 measurements show consistent variability. Using our rotation periods, and global stellar parameters derived from fitting Balmer line profiles, and from Geneva and Strömgren–Crawford photometry, we determined the equatorial rotational velocities and calculated the respective critical rotational fractions veq/vcrit. We have shown from our sample that the critical rotational fraction decreases with stellar age, at a rate consistent with the magnetic braking observed in the larger population of mCP stars.
The DNA repair function of BCL11A suppresses senescence and promotes continued proliferation of triple-negative breast cancer cells
Authors: Vickridge Elise , Faraco Camila C F , Tehrani Payman S , Ramdzan Zubaidah M , Djerir Billel , Rahimian Hedyeh , Leduy Lam , Maréchal Alexandre , Gingras Anne-Claude , Nepveu Alain 
Published: September 2022

Abstract
We identified the BCL11A protein in a proximity-dependent biotinylation screen performed with the DNA glycosylase NTHL1. In vitro, DNA repair assays demonstrate that both BCL11A and a small recombinant BCL11A160–520 protein that is devoid of DNA binding and transcription regulatory domains can stimulate the enzymatic activities of two base excision repair enzymes: NTHL1 and DNA Pol β. Increased DNA repair efficiency, in particular of the base excision repair pathway, is essential for many cancer cells to proliferate in the presence of elevated reactive oxygen species (ROS) produced by cancer-associated metabolic changes. BCL11A is highly expressed in triple-negative breast cancers (TNBC) where its knockdown was reported to reduce clonogenicity and cause tumour regression. We show that BCL11A knockdown in TNBC cells delays repair of oxidative DNA damage, increases the number of oxidized bases and abasic sites in genomic DNA, slows down proliferation and induces cellular senescence. These phenotypes are rescued by ectopic expression of the short BCL11A160–520 protein. We further show that the BCL11A160–520 protein accelerates the repair of oxidative DNA damage and cooperates with RAS in cell transformation assays, thereby enabling cells to avoid senescence and continue to proliferate in the presence of high ROS levels.
Flour exposure, sensitization and respiratory health among Alberta trainee bakers
Authors: Beach J , Galarneau J -M , Cherry N 
Published: September 2022

Abstract

Background
Sensitization to allergens encountered in baking, and allergic disease including asthma and rhinitis, is recognized. Attempts to reduce this risk have been instituted in some workplaces, but awareness remains low. This study aimed to quantify the current risk among Alberta bakers.

Aims
To estimate the onset of sensitization to bakery allergens and allergic disease among trainee bakers at the outset of their career.

Methods
Trainees attending one of the two bakery programmes were recruited between 2015 and 2018. At entry, an interview was held and spirometry and skin prick tests were performed. Participants were contacted every 6 months by telephone or online interview for 3 years to update work and health information. An exit interview was completed between 2018 and 2019 for all who could be contacted. Exposure was estimated using collected work history and a job exposure matrix was prepared for this study.

Results
A total of 220 individuals participated in the entry interview, 204 completed one or more periodic interviews and 113 completed the exit interview. Six who completed exit testing developed new sensitization to bakery antigens, an incidence of 2.49/100 person-years. Positive skin prick tests for bakery antigens were associated with bread making. Rhinitis symptoms were associated with total flour dust and new-onset rhinitis to months in trade. New-onset asthma was related to cumulative exposure to flour improvers.

Conclusions
Trainee bakers in Alberta remain at risk of sensitization and occupational respiratory disease.