bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Simons Observatory: Pipeline comparison and validation for large-scale B-modes
Authors: Wolz Kevin , Azzoni Susanna , Hervías-Caimapo Carlos , Errard Josquin , Krachmalnicoff Nicoletta , Alonso David , Baccigalupi Carlo , Baleato Lizancos Antón , Brown Michael L. , Calabrese Erminia , Chluba Jens , Dunkley Jo , Fabbian Giulio , Galitzki Nicholas , Jost Baptiste , Morshed Magdy , Nati Federico 
Published: March 2024

Context. The upcoming Simons Observatory Small Aperture Telescopes aim at achieving a constraint on the primordial tensor-to-scalar ratio r at the level of σ(r = 0)≲0.003, observing the polarized CMB in the presence of partial sky coverage, cosmic variance, inhomogeneous non-white noise, and Galactic foregrounds.
Aims. We present three different analysis pipelines able to constrain r given the latest available instrument performance, and compare their predictions on a set of sky simulations that allow us to explore a number of Galactic foreground models and elements of instrumental noise, relevant for the Simons Observatory.
Methods. The three pipelines employ different combinations of parametric and non-parametric component separation at the map and power spectrum levels, and use B-mode purification to estimate the CMB B-mode power spectrum. We applied them to a common set of simulated realistic frequency maps, and compared and validated them with focus on their ability to extract robust constraints on the tensor-to-scalar ratio r. We evaluated their performance in terms of bias and statistical uncertainty on this parameter.
Results. In most of the scenarios the three methodologies achieve similar performance. Nevertheless, several simulations with complex foreground signals lead to a > 2σ bias on r if analyzed with the default versions of these pipelines, highlighting the need for more sophisticated pipeline components that marginalize over foreground residuals. We show two such extensions, using power-spectrum-based and map-based methods, that are able to fully reduce the bias on r below the statistical uncertainties in all foreground models explored, at a moderate cost in terms of σ(r).
Characterizing B stars from Kepler/K2 Campaign 11
Authors: Pereira Alan W. , Janot-Pacheco Eduardo , Emilio Marcelo , Andrade Laerte , Armstrong James D. , Eidam Jéssica M. , Rabello-Soares M. Cristina , da Silva Bergerson V. H. V. 
Published: March 2024

Aims. In this study, we analyze 122 B-type star candidates observed during Campaign 11 of the Kepler/K2 mission to investigate their variability and pulsation characteristics. A subset of 45 B star candidates was observed during the Kepler/K2 mission’s Campaign 11 between September and December 2016. Our analyses aim to gain a deeper understanding of the physical characteristics of these massive stars. Our methods involve both spectroscopy and seismology. The spectroscopic analysis was performed through mediumresolution blue spectra, which also allowed us to perform a spectral classification of the objects. Our results will contribute to the ongoing effort to expand our knowledge of variable B stars and the processes that drive their variability.
Methods. We used the iterative prewhitening and wavelet frequency searching algorithms to analyze the light curves to identify the different types of variability in the data. The frequencies were carefully chosen based on the signal-to-noise ratio and the magnitude of errors. We applied spectroscopic analysis techniques to enhance our understanding of the observed stars, including SME and MESA algorithms. A spectral classification was performed based on the observed spectra. The resulting astrophysical parameters were compared to Gaia mission data. Additionally, a seismology technique was applied to determine the average internal rotation frequency (vrot) and buoyancy travel time (P0) for selected stars in the sample.
Results. We detected several types of variability among the B-type stars, including slowly pulsating B (SPB) stars, hybrid pulsators showing both β Cep and SPB pulsations, stars with stochastic low-frequency (SLF) variability, Maia variables, and SPB/Maia hybrids. Their positions in our Gaia and classical HR diagrams are compatible with the theoretical expectations. We also found stars exhibiting variability attributed to binarity and rotation. We determined the physical characteristics for 45 of our targets and conducted a seismic analysis for 14 objects. Two SPB/Maia stars show internal velocities comparable to those of fast SPB stars. The derived average rotation frequencies, vrot, for these 14 stars lie between the critical vcritRoche and the minimal frequency values of vlimrot implied by the υ sin i measured from the spectra.
Conclusions. Our analysis classified 41 stars as SPB stars and attributed the primary variability of 53 objects to binarity, rotation, or both. We identified five stars as Maia/fast-rotating SPB variables. Two stars were classified as hybrid SPB/β Cep pulsators, and one as a β Cep binary. Thirteen stars exhibited prominent, low-frequency power excess, indicating SLF variability. Additionally, we found a positive correlation between the dominant fg frequency and the internal average rotation frequency.
ALMA-IMF
Authors: Armante M. , Gusdorf A. , Louvet F. , Motte F. , Pouteau Y. , Lesaffre P. , Galván-Madrid R. , Dell’Ova P. , Bonfand M. , Nony T. , Brouillet N. , Cunningham N. , Ginsburg A. , Men’shchikov A. , Bontemps S. , Díaz-González D. , Csengeri T. , Fernández-López M. , González M. , Herpin F. , Liu H.-L. , Sanhueza P. , Stutz A.M. , Valeille-Manet M. 
Published: March 2024

Context. One of the central questions in astrophysics is the origin of the initial mass function (IMF). It is intrinsically linked to the processes from which it originates, and hence its connection with the core mass function (CMF) must be elucidated.
Aims. We aim to measure the CMF in the evolved W33-Main star-forming protocluster to compare it with CMF recently obtained in other Galactic star-forming regions, including the ones that are part of the ALMA-IMF program.
Methods. We used observations from the ALMA-IMF large programme: ~2′ × 2′ maps of emission from the continuum and selected lines at 1.3 mm and 3 mm observed by the ALMA 12m only antennas. Our angular resolution was typically 1″, that is, ~2400 au at a distance of 2.4 kpc. The lines we analysed are CO (2–1), SiO (5–4), N2H+ (1–0), H41α as well as He41α blended with C41α. We built a census of dense cores in the region, and we measured the associated CMF based on a core-dependent temperature value.
Results. We confirmed the ‘evolved’ status of W33-Main by identifiying three H II regions within the field, and to a lesser extent based on the number and extension of N2H+ filaments. We produced a filtered core catalogue of 94 candidates that we refined to take into account the contamination of the continuum by free-free and line emission, obtaining 80 cores with masses that range from 0.03 to 13.2 M⊙. We fitted the resulting high-mass end of the CMF with a single power law of the form N(log(M)) ∝ Mα, obtaining α = −1.44−0.22+0.16, which is slightly steeper but consistent with the Salpeter index. We categorised our cores as prestellar and protostellar, mostly based on outflow activity and hot core nature. We found the prestellar CMF to be steeper than a Salpeter-like distribution, and the protostellar CMF to be slightly top heavy. We found a higher proportion of cores within the H II regions and their surroundings than in the rest of the field. We also found that the cores’ masses were rather low (maximum mass of ~13 M⊙).
Conclusions. We find that star formation in W33-Main could be compatible with a ‘clump-fed’ scenario of star formation in an evolved cloud characterised by stellar feedback in the form of H II regions, and under the influence of massive stars outside the field. Our results differ from those found in less evolved young star-forming regions in the ALMA-IMF program. Further investigations are needed to elucidate the evolution of late CMFs towards the IMF over statistically significant samples.
A deep search for large complex organic species toward IRAS16293-2422 B at 3 mm with ALMA
Authors: Nazari P. , Cheung J. S. Y. , Asensio J. Ferrer , Murillo N. M. , van Dishoeck E. F. , Jørgensen J. K. , Bourke T. L. , Chuang K.-J. , Drozdovskaya M. N. , Fedoseev G. , Garrod R. T. , Ioppolo S. , Linnartz H. , McGuire B. A. , Müller H. S. P. , Qasim D. , Wampfler S. F. 
Published: March 2024

Context. Complex organic molecules (COMs) have been detected ubiquitously in protostellar systems. However, at shorter wavelengths (~0.8 mm), it is generally more difficult to detect larger molecules than at longer wavelengths (~3 mm) because of the increase in millimeter dust opacity, line confusion, and unfavorable partition function.
Aims. We aim to search for large molecules (more than eight atoms) in the Atacama Large Millimeter/submillimeter Array (ALMA) Band 3 spectrum of IRAS 16293-2422 B. In particular, the goal is to quantify the usability of ALMA Band 3 for molecular line surveys in comparison to similar studies at shorter wavelengths.
Methods. We used deep ALMA Band 3 observations of IRAS 16293-2422 B to search for more than 70 molecules and identified as many lines as possible in the spectrum. The spectral settings were set to specifically target three-carbon species such as i- and n-propanol and glycerol, the next step after glycolaldehyde and ethylene glycol in the hydrogenation of CO. We then derived the column densities and excitation temperatures of the detected species and compared the ratios with respect to methanol between Band 3 (~3 mm) and Band 7 (~1 mm, Protostellar Interferometric Line Survey) observations of this source to examine the effect of the dust optical depth.
Results. We identified lines of 31 molecules including many oxygen-bearing COMs such as CH3OH, CH2OHCHO, CH3CH2OH, and c-C2H4O and a few nitrogen- and sulfur-bearing ones such as HOCH2CN and CH3SH. The largest detected molecules are gGg-(CH2OH)2 and CH3COCH3. We did not detect glycerol or i- and n-propanol, but we do provide upper limits for them which are in line with previous laboratory and observational studies. The line density in Band 3 is only ~2.5 times lower in frequency space than in Band 7. From the detected lines in Band 3 at a ≳ 6σ level, ~25–30% of them could not be identified indicating the need for more laboratory data of rotational spectra. We find similar column densities and column density ratios of COMs (within a factor ~2) between Band 3 and Band 7.
Conclusions. The effect of the dust optical depth for IRAS 16293-2422 B at an off-source location on column densities and column density ratios is minimal. Moreover, for warm protostars, long wavelength spectra (~3 mm) are not only crowded and complex, but they also take significantly longer integration times than shorter wavelength observations (~0.8 mm) to reach the same sensitivity limit. The 3 mm search has not yet resulted in the detection of larger and more complex molecules in warm sources. A full deep ALMA Band 2–3 (i.e., ~3–4 mm wavelengths) survey is needed to assess whether low frequency data have the potential to reveal more complex molecules in warm sources.
First evidence of a connection between cluster-scale diffuse radio emission in cool-core galaxy clusters and sloshing features
Authors: Biava N. , Bonafede A. , Gastaldello F. , Botteon A. , Brienza M. , Shimwell T. W. , Brunetti G. , Bruno L. , Rajpurohit K. , Riseley C. J. , van Weeren R. J. , Rossetti M. , Cassano R. , De Gasperin F. , Drabent A. , Rottgering H. J. A. , Edge A. C. , Tasse C. 
Published: March 2024

Context. Radio observations of a few cool-core galaxy clusters have revealed the presence of diffuse emission on cluster scales, similar to what was found in merging clusters in the form of radio halos. These sources might suggest that a minor merger, while not sufficiently energetic to disrupt the cool core, could still trigger particle acceleration in the intracluster medium on scales of hundreds of kiloparsecs.
Aims. We aim to verify the occurrence of cluster-scale diffuse radio emission in cool-core clusters and test the minor merger scenario.
Methods. With the LOw Frequency ARray (LOFAR) at 144 MHz, we observed a sample of twelve cool-core galaxy clusters presenting some level of dynamical disturbances, according to X-ray data. We also performed a systematic search of cold fronts in these clusters, re-analysing archival Chandra observations.
Results. The clusters PSZ1G139.61+24, A1068 (new detection), MS 1455.0+2232, and RX J1720.1+2638 present diffuse radio emission on a cluster scale (r ≥ 0.2R500). This emission is characterised by a double component: a central mini-halo confined by cold fronts and diffuse emission on larger scales, whose radio power at 144 MHz is comparable to that of radio halos detected in merging systems with the same cluster mass. The cold fronts in A1068 are a new detection. We also found a candidate plasma depletion layer in this cluster. No sloshing features are found in the other eight clusters. Two of them present a mini-halo, with diffuse radio emission confined to the cluster core. We also found a new candidate mini-halo. Whereas, for the remaining five clusters, we did not detect halo-like emission. For clusters without cluster-scale halos, we derived upper limits to the radio halo power.
Conclusions. We found that cluster-scale diffuse radio emission is not present in all cool-core clusters when observed at a low frequency, but it is correlated to the presence of cold fronts. The coexistence of cluster-scale diffuse radio emission and cold fronts in cool-core clusters requires a specific configuration of the merger and so it puts some constraints on the turbulence, which deserves to be investigated in the future with theoretical works.
Search for radio halos in starburst galaxies
Authors: Galante C. A. , Saponara J. , Romero G. E. , Benaglia P. 
Published: March 2024

Context. Starburst galaxies are undergoing intense episodes of star formation. In these galaxies, gas is ejected into the surrounding environment through winds created by the effect of hot stars and supernova explosions. When interacting with the intergalactic medium, these winds can produce strong shocks capable of accelerating cosmic rays. The radiation from these cosmic rays mainly occurs in radio and gamma rays. The radio halo can be characterized using the scale height, which is an important parameter for understanding cosmic ray acceleration and transport.
Aims. We searched for the presence of radio halos in a sample of edge-on starburst galaxies gathered from the MeerKAT 1.28 GHz Atlas of Southern Sources in the IRAS Revised Bright Galaxy Sample. The investigation of how the radio halos relate to the global properties of the galaxies can shed light on the understanding of the halo origin and the underlying cosmic ray population.
Methods. We selected a sample of 25 galaxies with inclinations i > 80° from the original sample and modeled their disk and halo contributions. We determined the scale heights and the radio luminosity of the halos when detected.
Results. We have detected and characterized 11 radio halos from a sample of 25 edge-on galaxies. Seven of them are reported here for the first time. The average radio scale height is ∼1 kpc. We found that the halo scale heights increase linearly with the radio diameters and this relation does not depend on the star formation rate. All galaxies in our sample follow the radio-infrared relation with a q parameter value of 2.5 ± 0.1. The halo luminosity linearly increases with the infrared luminosity and star formation rate.
Conclusions. The dependence of the halo luminosity on the star formation rate and the infrared luminosity supports the hypothesis that the radio halos are the result of synchrotron radiation produced by relativistic electrons and points toward the fact that the star formation activity plays a crucial role in halo creation. The average scale height of 1 kpc implies a dynamical range of 4 Myr, several orders of magnitude greater than the synchrotron losses for electrons of 10 TeV. This suggests that some process must exist to reaccelerate cosmic rays in the halo if gamma-ray emission of a leptonic origin is detected from the halo. According to the relation between the radio and gamma-ray luminosities, we found that NGC 4666 is a potential gamma-ray source for future observations.
Cloud properties across spatial scales in simulations of the interstellar medium
Authors: Colman Tine , Brucy Noé , Girichidis Philipp , Glover Simon C. O. , Benedettini Milena , Soler Juan D. , Tress Robin G. , Traficante Alessio , Hennebelle Patrick , Klessen Ralf S. , Molinari Sergio , Miville-Deschênes Marc-Antoine 
Published: March 2024

Context. Molecular clouds (MCs) are structures of dense gas in the interstellar medium (ISM) that extend from ten to a few hundred parsecs and form the main gas reservoir available for star formation. Hydrodynamical simulations of a varying complexity are a promising way to investigate MCs evolution and their properties. However, each simulation typically has a limited range in resolution and different cloud extraction algorithms are used, which complicates the comparison between simulations.
Aims. In this work, we aim to extract clouds from different simulations covering a wide range of spatial scales. We compare their properties, such as size, shape, mass, internal velocity dispersion, and virial state.
Methods. We applied the HOP cloud detection algorithm on (M)HD numerical simulations of stratified ISM boxes and isolated galactic disk simulations that were produced using FLASH, RAMSES, and AREPO.
Results. We find that the extracted clouds are complex in shape, ranging from round objects to complex filamentary networks in all setups. Despite the wide range of scales, resolution, and sub-grid physics, we observe surprisingly robust trends in the investigated metrics. The mass spectrum matches in the overlap between simulations without rescaling and with a high-mass power-law index of −1 for logarithmic bins of mass, in accordance with theoretical predictions. The internal velocity dispersion scales with the size of the cloud as σ ∝ R0.75 for large clouds (R ≳ 3 pc). For small clouds we find larger σ compared to the power-law scaling, as seen in observations, which is due to supernova-driven turbulence. Almost all clouds are gravitationally unbound with the virial parameter scaling as αvir ∝ M−04, which is slightly flatter compared to observed scaling but in agreement given the large scatter. We note that the cloud distribution towards the low-mass end is only complete if the more dilute gas is also refined, rather than only the collapsing regions.
The GAPS Programme at TNG
Authors: Guilluy G. , D’Arpa M. C. , Bonomo A. S. , Spinelli R. , Biassoni F. , Fossati L. , Maggio A. , Giacobbe P. , Lanza A. F. , Sozzetti A. , Borsa F. , Rainer M. , Micela G. , Affer L. , Andreuzzi G. , Bignamini A. , Boschin W. , Carleo I. , Cecconi M. , Desidera S. , Fardella V. , Ghedina A. , Mantovan G. , Mancini L. , Nascimbeni V. , Knapic C. , Pedani M. , Petralia A. , Pino L. , Scandariato G. , Sicilia D. , Stangret M. , Zingales T. 
Published: March 2024

Context. Atmospheric escape plays a fundamental role in shaping the properties of exoplanets. The metastable near-infrared (nIR) helium triplet at 1083.3 nm (HeI) is a powerful proxy of extended and evaporating atmospheres.Aims. We used the GIARPS (GIANO-B + HARPS-N) observing mode of the Telescopio NazionaleGalileoto search for HeIabsorption in the upper atmospheres of five close-in giant planets hosted by the K and M dwarf stars of our sample, namely WASP-69 b, WASP-107 b, HAT-P-11 b, GJ 436 b, and GJ 3470 b.Methods. We focused our analysis on the nIR HeItriplet, performing high-resolution transmission spectroscopy by comparing the in-transit and out-of-transit observations. In instances where nightly variability in the HeIabsorption signal was identified, we investigated the potential influence of stellar magnetic activity on the planetary absorption signal by searching for variations in the Hαtransmission spectrum.Results. We spectrally resolve the HeItriplet and confirm the published detections for WASP-69 b (3.91 ± 0.22%, 17.6σ), WASP-107 b (8.17−0.76+0.80%, 10.5σ), HAT-P-11 b (1.36 ± 0.17%, 8.0σ), and GJ 3470 b (1.75−0.36+0.39%, 4.7σ). We do not find evidence of extra absorption for GJ 436 b. We observe night-to-night variations in the HeIabsorption signal for WASP-69 b, associated with variability in Hα, which likely indicates the influence of pseudo-signals related to stellar activity. Additionally, we find that the HeIsignal of GJ 3470 b originates from a single transit observation, thereby corroborating the discrepancies found in the existing literature. An inspection of the Hαline reveals an absorption signal during the same transit event.Conclusions. By combining our findings with previous analyses of GIANO-B HeImeasurements of planets orbiting K dwarfs, we explore potential trends with planetary and stellar parameters that are thought to affect the absorption of metastable HeI. Our analysis is unable to identify clear patterns, thus emphasising the necessity for additional measurements and the exploration of potential additional parameters that may be important in controlling HeIabsorption in planetary upper atmospheres.
Wirkung von Musik bei verschiedenen Krankheiten und besonderen medizinischen Situationen
Authors: Trappe Hans-Joachim 
Published: March 2024

SummaryMusik beeinflusst zahlreiche kognitive ­Funktionen und hat auch die Fähigkeit, Gehirnströme zu verändern. Bereits im Mutterleib können Ungeborene ab etwa der 20. Schwangerschaftswoche Musik wahrnehmen. Zahlreiche Studien belegen bereits positive Effekte auf den Verlauf verschiedener Erkrankungen, unter anderem Herz-Kreislauf-Erkrankungen, neurologische Erkrankungen wie Parkinson und Alzheimer, aber auch psychische Krankheiten wie Depressionen und Angststörungen. Auch vor, während und nach chirurgischen Eingriffen wirkt Musik positiv auf den Heilungsverlauf und das Wohlbefinden der Patient*innen.