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Zeitschriftenartikel zum Thema „Fraction massique“

Autor: Grafiati

Veröffentlicht am 25. Januar 2025

Zuletzt aktualisiert am 31. Juli 2025

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1

Ousmane, Moctar, Dianda Boureima, Thierry Sikoudouin Maurice K.Y, et al. "ETUDE DES PERFORMANCES THERMIQUES DUN SECHOIR SOLAIRE." International Journal of Advanced Research 12, no. 01 (2024): 1062–72. http://dx.doi.org/10.21474/ijar01/18224.

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Les populations ouest africaines produisent de grandes quantites de recoltes. Malheureusement faute de moyens de conservation, ces produits pourrissent. Cest pour cette raison que nous nous sommes interesses au sechage solaire des produits agro-alimentaires avec comme produit la banana douce. Lobjectif de cette publication est letude des performances thermiques dun sechoir solaire Ã absorbeur Ã ailettes. Les materiels utilises sont : un sechoir complet constitue de cinq claies, des tranches de banane douce, dune balance de precision et dun enregistreur automatique de temperatures. Levolution d

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Davison, Thomas A., Mark A. Norris, Ryan Leaman, Harald Kuntschner, Alina Boecker, and Glenn van de Ven. "Mapping accreted stars in early-type galaxies across the mass–size plane." Monthly Notices of the Royal Astronomical Society 507, no. 2 (2021): 3089–112. http://dx.doi.org/10.1093/mnras/stab2362.

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ABSTRACT Galaxy mergers are instrumental in dictating the final mass, structure, stellar populations, and kinematics of galaxies. Cosmological galaxy simulations indicate that the most massive galaxies at z = 0 are dominated by high fractions of ‘ex-situ’ stars, which formed first in distinct independent galaxies, and then subsequently merged into the host galaxy. Using spatially resolved MUSE spectroscopy we quantify and map the ex-situ stars in thirteen massive early-type galaxies. We use full spectral fitting together with semi-analytic galaxy evolution models to isolate the signatures in t

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Sharma, Ray S., Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Angelo Ricarte, and Thomas R. Quinn. "A Hidden Population of Massive Black Holes in Simulated Dwarf Galaxies." Astrophysical Journal 936, no. 1 (2022): 82. http://dx.doi.org/10.3847/1538-4357/ac8664.

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Abstract We explore the characteristics of actively accreting massive black holes (MBHs) within dwarf galaxies in the Romulus25 cosmological hydrodynamic simulation. We examine the MBH occupation fraction, X-ray active fractions, and active galactic nucleus (AGN) scaling relations within dwarf galaxies of stellar mass 108 M ⊙ < M star < 1010 M ⊙ out to redshift z = 2. In the local universe, the MBH occupation fraction is consistent with observed constraints, dropping below unity at M star < 3 × 1010 M ⊙, M 200 < 3 × 1011 M ⊙. Local dwarf AGN in Romulus25 follow observed scaling rel

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Schootemeijer, Abel, Danny J. Lennon, Miriam Garcia, Norbert Langer, Ben Hastings, and Christoph Schürmann. "Massive stars in metal-poor dwarf galaxies are often extreme rotators." Proceedings of the International Astronomical Union 18, S361 (2022): 63–69. http://dx.doi.org/10.1017/s1743921322002538.

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AbstractWe probe how common extremely rapid rotation is among massive stars in the early universe by measuring the OBe star fraction in nearby metal-poor dwarf galaxies. We apply a new method that uses broad-band photometry to measure the galaxy-wide OBe star fractions in the Magellanic Clouds and three more distant, more metal-poor dwarf galaxies. We find OBe star fractions of ∼20% in the Large Magallanic Cloud (0.5Zȯ), and ∼30% in the Small Magellanic Cloud (0.2Zȯ) as well as in the so-far unexplored metallicity range 0.1 Z/Zȯ < 0.2 occupied by the other three dwarf galaxies. Our results

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Shenton, Robert G., René D. Oudmaijer, and Stuart L. Lumsden. "Binarity in Massive Young Stellar Objects." Proceedings of the International Astronomical Union 18, S361 (2022): 556–58. http://dx.doi.org/10.1017/s1743921322001909.

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AbstractMost massive stars (up to 100%) are thought to be in binary systems. The multiplicity of massive stars seems to be intrinsically linked to their formation and evolution, and so Massive Young Stellar Objects are key in observing this early stage of star formation. We have surveyed hundreds of MYSOs across the Galaxy from the RMS catalogue, using UKIDSS and VVV point source data. Preliminary results show binary fractions of 44±3% for the UKIDSS sample and 32±3% for the VVV sample. In addition we use the K-band magnitudes as a proxy for the companion mass, and find a significant fraction

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Contini, Emanuele, Seyoung Jeon, Jinsu Rhee, San Han, and Sukyoung K. Yi. "The Intracluster Light and Its Link with the Dynamical State of the Host Group/Cluster: The Role of the Halo Concentration." Astrophysical Journal 958, no. 1 (2023): 72. http://dx.doi.org/10.3847/1538-4357/acfd25.

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Abstract We investigate the role of halo concentration in the formation of intracluster light (ICL) in galaxy groups and clusters, as predicted by a state-of-the-art semianalytic model of galaxy formation, coupled with a set of high-resolution dark-matter-only simulations. The analysis focuses on how the fraction of ICL correlates with halo mass, concentration, and fraction of early-type galaxies (ETGs) in a large sample of groups and clusters with 13.0 ≤ log M halo ≤ 15.0 . The fraction of ICL follows a normal distribution, a consequence of the stochastic nature of the physical processes resp

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Mukherjee, Sampath, Léon V. E. Koopmans, Crescenzo Tortora, et al. "SEAGLE – III: Towards resolving the mismatch in the dark-matter fraction in early-type galaxies between simulations and observations." Monthly Notices of the Royal Astronomical Society 509, no. 1 (2021): 1245–51. http://dx.doi.org/10.1093/mnras/stab3014.

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ABSTRACT The central dark-matter fraction of galaxies is sensitive to feedback processes during galaxy formation. Strong gravitational lensing has been effective in the precise measurement of the dark-matter fraction inside massive early-type galaxies. Here, we compare the projected dark-matter fraction of early-type galaxies inferred from the SLACS (Sloan Lens ACS Survey) strong-lens survey with those obtained from the Evolution and Assembly of GaLaxies and their Environment (EAGLE), Illustris, and IllustrisTNG hydrodynamical simulations. Previous comparisons with some simulations revealed a

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Grylls, Philip J., F. Shankar, and C. J. Conselice. "The significant effects of stellar mass estimation on galaxy pair fractions." Monthly Notices of the Royal Astronomical Society 499, no. 2 (2020): 2265–75. http://dx.doi.org/10.1093/mnras/staa2966.

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ABSTRACT Theoretical models suggest that galaxy mergers may have profoundly shaped galaxy morphologies through cosmic time. However, observational estimates of galaxy pair fractions, and implied galaxy mergers, still do not converge, suggesting different numbers and redshift evolution. This paper explores the connection between stellar mass estimation and the pair fraction of galaxies using $\rm {\small STEEL}$, the Statistical sEmi-Emprical modeL, in which galaxies are mapped on to host dark matter haloes via a stellar mass–halo mass (SMHM) relation. As haloes of different mass are predicted

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Yoo, Taehwa, Taysun Kimm, and Joakim Rosdahl. "On the origin of low escape fractions of ionizing radiation from massive star-forming galaxies at high redshift." Monthly Notices of the Royal Astronomical Society 499, no. 4 (2020): 5175–93. http://dx.doi.org/10.1093/mnras/staa3187.

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ABSTRACT The physical origin of low escape fractions of ionizing radiation derived from massive star-forming galaxies at z ∼ 3–4 is not well understood. We perform idealized disc galaxy simulations to understand how galactic properties such as metallicity and gas mass affect the escape of Lyman continuum (LyC) photons using radiation-hydrodynamic simulations with strong stellar feedback. We find that the luminosity-weighted escape fraction from a metal-poor (Z = 0.002) galaxy embedded in a halo of mass $M_{\rm h}\simeq 10^{11}\, \mathrm{M}_\odot$ is $\left\langle {f_{\rm esc}^{\rm 3D}}\right\r

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Liu, Shuang, Yizhou Gu, Qirong Yuan, et al. "Morphological Transformation and Star Formation Quenching of Massive Galaxies at 0.5 ≤ z ≤ 2.5 in 3D-HST/CANDELS." Astrophysical Journal 923, no. 1 (2021): 46. http://dx.doi.org/10.3847/1538-4357/ac2817.

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Abstract To figure out the effect of stellar mass and local environment on morphological transformation and star formation quenching in galaxies, we use the massive (M * ≥ 1010 M ⊙) galaxies at 0.5 ≤ z ≤ 2.5 in five fields of 3D-HST/CANDELS. Based on the UVJ diagnosis and the possibility of possessing a spheroid, our sample of massive galaxies is classified into four populations: quiescent early-type galaxies (qEs), quiescent late-type galaxies (qLs), star-forming early-type galaxies (sEs), and star-forming late-type galaxies (sLs). It is found that the quiescent fraction is significantly elev

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Hashimoto, Tetsuya, Tomotsugu Goto, Rieko Momose, et al. "A young galaxy cluster in the old Universe." Monthly Notices of the Royal Astronomical Society 489, no. 2 (2019): 2014–29. http://dx.doi.org/10.1093/mnras/stz2182.

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ABSTRACT Galaxies evolve from a blue star-forming phase into a red quiescent one by quenching their star formation activity. In high-density environments, this galaxy evolution proceeds earlier and more efficiently. Therefore, local galaxy clusters are dominated by well-evolved red elliptical galaxies. The fraction of blue galaxies in clusters monotonically declines with decreasing redshift, i.e. the Butcher–Oemler effect. In the local Universe, observed blue fractions of massive clusters are as small as ≲0.2. Here we report a discovery of a ‘blue cluster’ that is a local galaxy cluster with a

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Kaviraj, Sugata, Garreth Martin, and Joseph Silk. "AGN in dwarf galaxies: frequency, triggering processes and the plausibility of AGN feedback." Monthly Notices of the Royal Astronomical Society: Letters 489, no. 1 (2019): L12—L16. http://dx.doi.org/10.1093/mnrasl/slz102.

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Abstract While active galactic nuclei (AGN) are considered to be key drivers of the evolution of massive galaxies, their potentially significant role in the dwarf-galaxy regime (M* &lt; 109 M⊙) remains largely unexplored. We combine optical and infrared data, from the Hyper Suprime-Cam (HSC) and the Wide-field Infrared Explorer, respectively, to explore the properties of ∼800 AGN in dwarfs at low redshift (z &lt; 0.3). Infrared-selected AGN fractions are ∼10–30 per cent in dwarfs, which, for reasonable duty cycles, indicates a high black hole (BH)-occupation fraction. Visual inspection

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Xie, Lizhi, Gabriella De Lucia, Michaela Hirschmann, and Fabio Fontanot. "The influence of environment on satellite galaxies in the GAEA semi-analytic model." Monthly Notices of the Royal Astronomical Society 498, no. 3 (2020): 4327–44. http://dx.doi.org/10.1093/mnras/staa2370.

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ABSTRACT Reproducing the observed quenched fraction of satellite galaxies has been a long-standing issue for galaxy formation models. We modify the treatment of environmental effects in our state-of-the-art GAlaxy Evolution and Assembly (GAEA) semi-analytic model to improve our modelling of satellite galaxies. Specifically, we implement gradual stripping of hot gas, ram-pressure stripping of cold gas, and an updated algorithm to account for angular momentum exchanges between the gaseous and stellar disc components of model galaxies. Our updated model predicts quenched fractions that are in goo

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Martínez-Marín, M., K. Glazebrook, T. Nanayakkara, et al. "The origin of large emission line widths in massive galaxies at redshifts z ∼ 3–4." Monthly Notices of the Royal Astronomical Society 531, no. 3 (2024): 3187–202. http://dx.doi.org/10.1093/mnras/stae1335.

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ABSTRACT We present a sample of 22 massive galaxies with stellar masses &gt;1010 M⊙ at 3 &lt; z &lt; 4 with deep H and K-band high resolution spectra (R = 3500–3000) from Keck/MOSFIRE and VLT/KMOS near-infrared spectrographs. We find a large fraction have strong [O iii] 5007 and Hβ emission lines with large line widths (σ 100–450 km s−1). We measure the sizes of our galaxies from Hubble Space Telescope images and consider the potential kinematic scaling relations of our sample, and rule out an explanation for these broad lines in terms of galaxy-wide kinematics. Based on considerat

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Zahorecz, S., I. Jimenez-Serra, L. Testi, et al. "Singly and doubly deuterated formaldehyde in massive star-forming regions." Astronomy & Astrophysics 653 (September 2021): A45. http://dx.doi.org/10.1051/0004-6361/201937012.

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Context. Deuterated molecules are good tracers of the evolutionary stage of star-forming cores. During the star formation process, deuterated molecules are expected to be enhanced in cold, dense pre-stellar cores and to deplete after protostellar birth. Aims. In this paper, we study the deuteration fraction of formaldehyde in high-mass star-forming cores at different evolutionary stages to investigate whether the deuteration fraction of formaldehyde can be used as an evolutionary tracer. Methods. Using the APEX SEPIA Band 5 receiver, we extended our pilot study of the J = 3 →2 rotational lines

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Loverde, Marilena, and Zachary J. Weiner. "Massive neutrinos and cosmic composition." Journal of Cosmology and Astroparticle Physics 2024, no. 12 (2024): 048. https://doi.org/10.1088/1475-7516/2024/12/048.

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Abstract Cosmological data probe massive neutrinos via their effects on the geometry of the Universe and the growth of structure, both of which are degenerate with the late-time expansion history. We clarify the nature of these degeneracies and the individual roles of both probes in neutrino mass inference. Geometry is strongly sensitive to neutrino masses: within ΛCDM, the primary cosmic microwave background anisotropies alone impose that the matter fraction Ω m must increase fivefold with increasing neutrino mass. Moreover, large-scale structure observables, like weak lensing of the CMB, are

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Gilhuly, Colleen, Allison Merritt, Roberto Abraham, et al. "Stellar Halos from the The Dragonfly Edge-on Galaxies Survey." Astrophysical Journal 932, no. 1 (2022): 44. http://dx.doi.org/10.3847/1538-4357/ac6750.

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Abstract We present the primary results from the Dragonfly Edge-on Galaxies Survey, an exploration of the stellar halos of twelve nearby (d < 25 Mpc) edge-on disk galaxies with the Dragonfly Telephoto Array. The edge-on orientation of these galaxies allows their stellar halos to be explored with minimal obscuration by or confusion with the much brighter disk light. Galaxies in the sample span a range of stellar masses from 109.68 to 1010.88 M ⊙. We confirm that the wide range of stellar halo mass fractions previously seen for Milky Way–mass galaxies is also found among less massive spiral g

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Chamberlain, Katie, Gurtina Besla, Ekta Patel, et al. "A Physically Motivated Framework to Compare Pair Fractions of Isolated Low- and High-mass Galaxies across Cosmic Time." Astrophysical Journal 962, no. 2 (2024): 162. http://dx.doi.org/10.3847/1538-4357/ad19d0.

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Abstract Low-mass galaxy pair fractions are understudied, and it is unclear whether low-mass pair fractions evolve in the same way as more massive systems over cosmic time. In the era of JWST, Roman, and Rubin, selecting galaxy pairs in a self-consistent way will be critical to connect observed pair fractions to cosmological merger rates across all mass scales and redshifts. Utilizing the Illustris TNG100 simulation, we create a sample of physically associated low-mass (108 < M * < 5 × 109 M ⊙) and high-mass (5 × 109 < M * < 1011 M ⊙) pairs between z = 0 and 4.2. The low-mass pair

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Beasley, Michael A., Ryan Leaman, Ignacio Trujillo, et al. "Reconstructing the mass accretion histories of nearby red nuggets with their globular cluster systems." Proceedings of the International Astronomical Union 15, S359 (2020): 381–85. http://dx.doi.org/10.1017/s1743921320004020.

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AbstractIt is generally recognized that massive galaxies form through a combination of in-situ collapse and ex-situ accretion. The in-situ component forms early, where gas collapse and compaction leads to the formation of massive compact systems (blue and red “nuggets”) seen at z > 1. The subsequent accretion of satellites brings in ex-situ material, growing these nuggets in size and mass to appear as the massive early-type galaxies (ETGs) we see locally. Due to stochasticity in the accretion process, in a few rare cases a red nugget will evolve to the present day having undergone little ex

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Eckert, D., V. Ghirardini, S. Ettori, et al. "Non-thermal pressure support in X-COP galaxy clusters." Astronomy & Astrophysics 621 (January 2019): A40. http://dx.doi.org/10.1051/0004-6361/201833324.

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Galaxy clusters are the endpoints of structure formation and are continuously growing through the merging and accretion of smaller structures. Numerical simulations predict that a fraction of their energy content is not yet thermalized, mainly in the form of kinetic motions (turbulence, bulk motions). Measuring the level of non-thermal pressure support is necessary to understand the processes leading to the virialization of the gas within the potential well of the main halo and to calibrate the biases in hydrostatic mass estimates. We present high-quality measurements of hydrostatic masses and

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Bodensteiner, J., H. Sana, C. Wang, et al. "The young massive SMC cluster NGC 330 seen by MUSE." Astronomy & Astrophysics 652 (August 2021): A70. http://dx.doi.org/10.1051/0004-6361/202140507.

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Context. Observations of massive stars in open clusters younger than ∼8 Myr have shown that a majority of them are in binary systems, most of which will interact during their life. While these can be used as a proxy of the initial multiplicity properties, studying populations of massive stars older than ∼20 Myr allows us to probe the outcome of these interactions after a significant number of systems have experienced mass and angular momentum transfer and may even have merged. Aims. Using multi-epoch integral-field spectroscopy, we aim to investigate the multiplicity properties of the massive-

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Courteau, Stéphane, and Aaron A. Dutton. "The Mass Distribution in Disk Galaxies." Proceedings of the International Astronomical Union 11, A29B (2015): 195–96. http://dx.doi.org/10.1017/s1743921316004865.

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AbstractWe present the relative fraction of baryons and dark matter at various radii in galaxies. For spiral galaxies, this fraction measured in a galaxy's inner parts is typically baryon-dominated (maximal) and dark-matter dominated (sub-maximal) in the outskirts. The transition from maximal to sub-maximal baryons occurs within the inner parts of low-mass disk galaxies (with Vtot ≤ 200 km s−1) and in the outer disk for more massive systems. The mean mass fractions for late- and early-type galaxies vary significantly at the same fiducial radius and circular velocity, suggesting a range of gala

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Tanaka, Toshiyuki, and Kenji Hasegawa. "Modelling population III stars for seminumerical simulations." Monthly Notices of the Royal Astronomical Society 502, no. 1 (2021): 463–71. http://dx.doi.org/10.1093/mnras/stab072.

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ABSTRACT Theoretically modelling the 21-cm signals caused by Population III stars (Pop III stars) is the key to extracting fruitful information on Pop III stars from current and forthcoming 21-cm observations. In this work, we develop a new module of Pop III stars in which the escape fractions of ionizing photons and Lyman–Werner (LW) photons, photoheating by UV radiation, and LW feedback are consistently incorporated. By implementing the module into a public 21-cm seminumerical simulation code, 21cmfast, we demonstrate 21-cm signal calculations, neglecting X-ray heating and focusing on the hi

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Rivero, H. D., José A. García, E. Cándido Atlatenco, Alejandro D. Basso, and J. Sicora. "Effect of the ratio Mo/Cr in the precipitation and distribution of carbides in alloyed nodular iron." MRS Proceedings 1485 (2012): 113–18. http://dx.doi.org/10.1557/opl.2013.278.

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ABSTRACTThis investigation deals with the effect of 2/0, 1/1 and 1/0.5 Cr/Mo ratios on the local fraction, distribution and the comparative size of carbides precipitated in cast nodular iron. “Y” block castings with a thickness of 1.5 cm are cast in green sand molds. Two samples are cut from each casting, one located on the center and another on the wall. The carbide volume fraction is evaluated by a digital analysis system. Each sample is analyzed in three zones: bottom, middle and top. Carbide mappings are generated according to the average local carbide fraction in order to get the distribu

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McConachie, Ian, Gillian Wilson, Ben Forrest, et al. "MAGAZ3NE: Evidence for Galactic Conformity in z ≳ 3 Protoclusters*." Astrophysical Journal 978, no. 1 (2024): 17. https://doi.org/10.3847/1538-4357/ad8f36.

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Abstract We examine the quiescent fractions of massive galaxies in six z ≳ 3 spectroscopically confirmed protoclusters in the COSMOS field, one of which is newly confirmed and presented here. We report the spectroscopic confirmation of MAGAZ3NE J100143+023021 at z = 3.122 − 0.004 + 0.007 by the Massive Ancient Galaxies At z > 3 NEar-infrared (MAGAZ3NE) survey. MAGAZ3NE J100143+023021 contains a total of 79 protocluster members (28 spectroscopic and 51 photometric). Three spectroscopically confirmed members are star-forming ultramassive galaxies (UMGs; log ( M ⋆ / M ⊙ ) > 11), the most ma

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Reddish, J., K. Kraljic, M. S. Petersen, et al. "The NewHorizon simulation – to bar or not to bar." Monthly Notices of the Royal Astronomical Society 512, no. 1 (2022): 160–85. http://dx.doi.org/10.1093/mnras/stac494.

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ABSTRACT We use the NewHorizon simulation to study the redshift evolution of bar properties and fractions within galaxies in the stellar masses range M⋆ = 107.25–1011.4$\, \rm {M}_\odot$ over the redshift range of z = 0.25–1.3. We select disc galaxies using stellar kinematics as a proxy for galaxy morphology. We employ two different automated bar detection methods, coupled with visual inspection, resulting in observable bar fractions of fbar = 0.070$_{{-0.012}}^{{+0.018}}$ at z ∼ 1.3, decreasing to fbar = 0.011$_{{-0.003}}^{{+0.014}}$ at z ∼ 0.25. Only one galaxy is visually confirmed as stron

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Bladt, S., and H. Wagner. "Inhibition of MAO by Fractions and Constituents of Hypericum Extract." Journal of Geriatric Psychiatry and Neurology 7, no. 1 (1994): 57–59. http://dx.doi.org/10.1177/089198879400700115.

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The inhibition of monoamine oxidase (MAO) by six fractions from hypericum extract and three characteristic constituents (as pure substances) were analyzed in vitro and ex vivo to study the antidepressive mechanism of action. Rat brain homogenates were used as the in vitro model, while the ex vivo analysis was performed after intraperitoneal application of the test substances to albino rats. Massive inhibition of MAO-A could be shown with the total extract and all fractions only at the concentration of 10-3 mol/L. At 10-4 mol/L, one fraction rich in flavonoides showed an inhibition of 39%, and

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Bladt, S., and H. Wagner. "Inhibition of MAO by Fractions and Constituents of Hypericum Extract." Journal of Geriatric Psychiatry and Neurology 7, no. 1_suppl (1994): 57–59. http://dx.doi.org/10.1177/089198879400701s15.

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The inhibition of monoamine oxidase (MAO) by six fractions from hypericum extract and three characteristic constituents (as pure substances) were analyzed in vitro and ex vivo to study the antidepressive mechanism of action. Rat brain homogenates were used as the in vitro model, while the ex vivo analysis was performed after intraperitoneal application of the test substances to albino rats. Massive inhibition of MAO-A could be shown with the total extract and all fractions only at the concentration of 10-3 mol/L. At 10-4 mol/L, one fraction rich in flavonoides showed an inhibition of 39%, and

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Patrick, L. R., D. J. Lennon, C. J. Evans, et al. "Multiplicity of the red supergiant population in the young massive cluster NGC 330." Astronomy & Astrophysics 635 (March 2020): A29. http://dx.doi.org/10.1051/0004-6361/201936741.

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Context. The multiplicity properties of massive stars are one of the important outstanding issues in stellar evolution. Quantifying the binary statistics of all evolutionary phases is essential to paint a complete picture of how and when massive stars interact with their companions, and to determine the consequences of these interactions. Aims. We investigate the multiplicity of an almost complete census of red supergiant stars (RSGs) in NGC 330, a young massive cluster in the Small Magellanic Cloud. Methods. Using a combination of multi-epoch HARPS and MUSE spectroscopy, we estimate radial ve

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Nestor Shachar, A., S. H. Price, N. M. Förster Schreiber, et al. "RC100: Rotation Curves of 100 Massive Star-forming Galaxies at z = 0.6–2.5 Reveal Little Dark Matter on Galactic Scales." Astrophysical Journal 944, no. 1 (2023): 78. http://dx.doi.org/10.3847/1538-4357/aca9cf.

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Abstract We analyze Hα or CO rotation curves extending out to several galaxy effective radii for 100 massive, large, star-forming disk galaxies (SFGs) across the peak of cosmic galaxy star formation (z ∼ 0.6–2.5), more than doubling the previous sample presented by Genzel et al. and Price et al. The observations were taken with SINFONI and KMOS integral-field spectrographs at the ESO-Very Large Telescope, LUCI-LBT, NOEMA-IRAM, and Atacama Large Millimeter/submillimeter Array. We fit the major-axis kinematics with beam-convolved, forward models of turbulent rotating disks with bulges embedded i

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Donnari, Martina, Annalisa Pillepich, Gandhali D. Joshi, et al. "Quenched fractions in the IllustrisTNG simulations: the roles of AGN feedback, environment, and pre-processing." Monthly Notices of the Royal Astronomical Society 500, no. 3 (2020): 4004–24. http://dx.doi.org/10.1093/mnras/staa3006.

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ABSTRACT We use the IllustrisTNG hydrodynamical simulations to show how the fractions of quenched galaxies vary across different environments and cosmic time, and to quantify the role AGN feedback and pre-processing play in quenching group and cluster satellites. At z = 0, we select galaxies with Mstars = 109−12 M⊙ residing within (≤R200c) massive groups and clusters of total host mass M200c = 1013−15.2 M⊙ in TNG100 and TNG300. The model predicts a quenched fraction of ∼70–90 per cent (on average) for centrals and satellites of mass ≳ 1010.5 M⊙, regardless of host mass, cosmic time (0 ≤ z ≤ 0.

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Xu, Dandan, Ling Zhu, Robert Grand, et al. "A study of stellar orbit fractions: simulated IllustrisTNG galaxies compared to CALIFA observations." Monthly Notices of the Royal Astronomical Society 489, no. 1 (2019): 842–54. http://dx.doi.org/10.1093/mnras/stz2164.

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ABSTRACT Motivated by the recently discovered kinematic ‘Hubble sequence’ shown by the stellar orbit-circularity distribution of 260 CALIFA galaxies, we make use of a comparable galaxy sample at z = 0 with a stellar mass range of $M_{*}/\mathrm{M}_{\odot }\in [10^{9.7},\, 10^{11.4}]$ selected from the IllustrisTNG simulation and study their stellar orbit compositions in relation to a number of other fundamental galaxy properties. We find that the TNG100 simulation broadly reproduces the observed fractions of different orbital components and their stellar mass dependences. In particular, the me

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Gonzalez, Anthony H., Dennis Zaritsky, and Ann I. Zabludoff. "A Census of Baryons in Galaxy Clusters and Groups." Proceedings of the International Astronomical Union 3, S244 (2007): 167–75. http://dx.doi.org/10.1017/s1743921307013968.

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AbstractWhile the baryon fraction in galaxy groups and clusters may be expected to reflect the universal value, observations of cluster baryon fractions have generally fallen short of this expectation and indicated a possible correlation with cluster mass. We present a new determination of the total baryon budget in nearby galaxy groups and clusters that includes the contributions from stars in galaxies, intracluster stars, and the intracluster medium. We find that the baryon mass fraction within r500 is independent of system mass and lower than the WMAP value. We conclude however that the pre

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Ren, Jian, F. S. Liu, Nan Li, et al. "The Evolution of the Size and Merger Fraction of Submillimeter Galaxies across 1 < z ≲ 6 as Observed by JWST." Astrophysical Journal 982, no. 2 (2025): 200. https://doi.org/10.3847/1538-4357/adb961.

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Abstract Precise tracking of the growth in galaxy size and the evolution of merger fractions with redshift is vital for understanding the formation history of submillimeter galaxies (SMGs). This study investigates this evolution over a broad redshift range (1 < z ≲ 6) using a sample of 222 SMGs with a median redshift of z = 2.6 1 − 0.82 + 0.89 identified by the Atacama Large Millimeter/submillimeter Array and the James Clerk Maxwell Telescope, enhanced by the advanced imaging capabilities of the JWST/NIRCam and MIRI. We find significant evolution in effective radii (R e ) in the rest-frame

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Juvela, Mika, Vincent Guillet, Tie Liu та ін. "Dust spectrum and polarisation at 850 μm in the massive IRDC G035.39-00.33". Astronomy & Astrophysics 620 (23 листопада 2018): A26. http://dx.doi.org/10.1051/0004-6361/201833245.

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Context. The sub-millimetre polarisation of dust emission from star-forming clouds carries information on grain properties and on the effects that magnetic fields have on cloud evolution. Aims. Using observations of a dense filamentary cloud G035.39-00.33, we aim to characterise the dust emission properties and the variations of the polarisation fraction. Methods. JCMT SCUBA-2/POL-2 observations at 850 μm were combined with Planck 850 μm(353 GHz) data to map polarisation fraction at small and large scales. With previous total intensity SCUBA-2 observations (450 and 850 μm) and Herschel data, t

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Chang, Wenjun, Guanwen Fang, Yizhou Gu, Zesen Lin, Shiying Lu, and Xu Kong. "The Physical Properties of Massive Green Valley Galaxies as a Function of Environments at 0.5 < z < 2.5 in 3D-HST/Candels Fields." Astrophysical Journal 936, no. 1 (2022): 47. http://dx.doi.org/10.3847/1538-4357/ac8748.

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Abstract To investigate the effects of environment in the quenching phase, we study the empirical relations for green valley (GV) galaxies between overdensity and other physical properties (i.e., effective radius r e , Sérsic indices n, and specific star formation rate (sSFR)). Based on five 3D-HST/CANDELS fields, we construct a large sample of 2126 massive (M ⋆ > 1010 M ☉) GV galaxies at 0.5 < z < 2.5 and split it into the higher overdensity quarter and the lower overdensity quarter. The results shows that GV galaxies in denser environments have higher n values and lower sSFR at 0.5

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Sorooshian, A., S. M. Murphy, S. Hersey, et al. "Comprehensive airborne characterization of aerosol from a major bovine source." Atmospheric Chemistry and Physics Discussions 8, no. 3 (2008): 10415–79. http://dx.doi.org/10.5194/acpd-8-10415-2008.

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Abstract. We report an extensive airborne characterization of aerosol downwind of a massive bovine source in the San Joaquin Valley (California) on two flights during July 2007. The Center for Interdisciplinary Remotely-Piloted Aircraft Studies (CIRPAS) Twin Otter probed chemical composition, particle size distribution, mixing state, sub- and supersaturated water uptake behavior, light scattering properties, and the interrelationship between these parameters and meteorology. Total PM1.0 levels and concentrations of organics, nitrate, and ammonium were enhanced in the plume from the source as c

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Sorooshian, A., S. M. Murphy, S. Hersey, et al. "Comprehensive airborne characterization of aerosol from a major bovine source." Atmospheric Chemistry and Physics 8, no. 17 (2008): 5489–520. http://dx.doi.org/10.5194/acp-8-5489-2008.

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Abstract. We report an extensive airborne characterization of aerosol downwind of a massive bovine source in the San Joaquin Valley (California) on two flights during July 2007. The Center for Interdisciplinary Remotely-Piloted Aircraft Studies (CIRPAS) Twin Otter probed chemical composition, particle size distribution, mixing state, sub- and supersaturated water uptake behavior, light scattering properties, and the interrelationship between these parameters and meteorology. Total PM1.0 levels and concentrations of organics, nitrate, and ammonium were enhanced in the plume from the source as c

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Rosas-Guevara, Yetli, Silvia Bonoli, Massimo Dotti, et al. "The evolution of the barred galaxy population in the TNG50 simulation." Monthly Notices of the Royal Astronomical Society 512, no. 4 (2022): 5339–57. http://dx.doi.org/10.1093/mnras/stac816.

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ABSTRACT We use the magnetic-hydrodynamical simulation TNG50 to study the evolution of barred massive disc galaxies. Massive spiral galaxies are already present as early as z = 4, and bar formation takes place already at those early times. The bars grow longer and stronger as the host galaxies evolve, with the bar sizes increasing at a pace similar to that of the disc scalelengths. The bar fraction mildly evolves with redshift for galaxies with $M_{*}\ge 10^{10}\rm M_{\odot }$, being greater than $\sim 40{{\ \rm per\ cent}}$ at 0.5 &lt; z &lt; 3 and $\sim 30{{\ \rm per\ cent}}$ at z =

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Bower, Dan J., Kaustubh Hakim, Paolo A. Sossi, and Patrick Sanan. "Retention of Water in Terrestrial Magma Oceans and Carbon-rich Early Atmospheres." Planetary Science Journal 3, no. 4 (2022): 93. http://dx.doi.org/10.3847/psj/ac5fb1.

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Abstract Massive steam and CO2 atmospheres have been proposed for magma ocean outgassing of Earth and terrestrial planets. Yet formation of such atmospheres depends on volatile exchange with the molten interior, governed by volatile solubilities and redox reactions. We determine the evolution of magma ocean–atmosphere systems for a range of oxygen fugacities, C/H ratios, and hydrogen budgets that include redox reactions for hydrogen (H2–H2O), carbon (CO–CO2), methane (CH4), and solubility laws for H2O and CO2. We find that small initial budgets of hydrogen, high C/H ratios, and oxidizing condi

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Bower, Dan J., Kaustubh Hakim, Paolo A. Sossi, and Patrick Sanan. "Retention of Water in Terrestrial Magma Oceans and Carbon-rich Early Atmospheres." Planetary Science Journal 3, no. 4 (2022): 93. http://dx.doi.org/10.3847/psj/ac5fb1.

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Abstract Massive steam and CO2 atmospheres have been proposed for magma ocean outgassing of Earth and terrestrial planets. Yet formation of such atmospheres depends on volatile exchange with the molten interior, governed by volatile solubilities and redox reactions. We determine the evolution of magma ocean–atmosphere systems for a range of oxygen fugacities, C/H ratios, and hydrogen budgets that include redox reactions for hydrogen (H2–H2O), carbon (CO–CO2), methane (CH4), and solubility laws for H2O and CO2. We find that small initial budgets of hydrogen, high C/H ratios, and oxidizing condi

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Kimmig, Lucas C., Rhea-Silvia Remus, Klaus Dolag, and Veronica Biffi. "The Hateful Eight: Connecting Massive Substructures in Galaxy Clusters like A2744 to Their Dynamical Assembly State Using the Magneticum Simulations." Astrophysical Journal 949, no. 2 (2023): 92. http://dx.doi.org/10.3847/1538-4357/acc740.

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Abstract Substructures are known to be good tracers for the dynamical states and recent accretion histories of the most massive collapsed structures in the universe, galaxy clusters. Observations find extremely massive substructures in some clusters, especially Abell 2744 (A2744), which are potentially in tension with the ΛCDM paradigm because they are not found in simulations directly. However, the methods to measure substructure masses strongly differ between observations and simulations. Using the fully hydrodynamical cosmological simulation suite Magneticum Pathfinder, we develop a method

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Radice, David, and Sebastiano Bernuzzi. "Secular Outflows from Long-Lived Neutron Star Merger Remnants." Journal of Physics: Conference Series 2742, no. 1 (2024): 012009. http://dx.doi.org/10.1088/1742-6596/2742/1/012009.

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Abstract We study mass ejection from a binary neutron star merger producing a long-lived massive neutron star remnant with general-relativistic neutrino-radiation hydrodynamics simulations. In addition to outflows generated by shocks and tidal torques during and shortly after the merger, we observe the appearance of a wind driven by spiral density waves in the disk. This spiral-wave-driven outflow is predominantly located close to the disk orbital plane and have a broad distribution of electron fractions. At higher latitudes, a high electron-fraction wind is driven by neutrino radiation. The c

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Reina-Campos, Marta, Meghan E. Hughes, J. M. Diederik Kruijssen, et al. "The mass fraction of halo stars contributed by the disruption of globular clusters in the E-MOSAICS simulations." Monthly Notices of the Royal Astronomical Society 493, no. 3 (2020): 3422–28. http://dx.doi.org/10.1093/mnras/staa483.

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ABSTRACT Globular clusters (GCs) have been posited, alongside dwarf galaxies, as significant contributors to the field stellar population of the Galactic halo. In order to quantify their contribution, we examine the fraction of halo stars formed in stellar clusters in the suite of 25 present-day Milky Way-mass cosmological zoom simulations from the E-MOSAICS project. We find that a median of 2.3 and 0.3 per cent of the mass in halo field stars formed in clusters and GCs, defined as clusters more massive than 5 × 103 and 105 M⊙, respectively, with the 25–75th percentiles spanning 1.9–3.0 and 0.

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Chen, Guoyin, Meixia Zhang, Xianyu Yao, et al. "Soil Organic Carbon Sequestration after 20-Year Afforestation of Mangrove Plantations on Qi’ao Island, Southern China." Agronomy 13, no. 9 (2023): 2389. http://dx.doi.org/10.3390/agronomy13092389.

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Mangrove afforestation is considered an important measure in the “natural-based solution” for mitigating climate warming through sequestering massive carbon (C) into vegetation biomass, yet how the planted mangrove species facilitate soil C sequestration remains unclear. Here, we investigated the stock, source, and fraction of soil organic carbon (SOC) over 1 m depth after 20-year afforestation of five mangrove pure plantations (Acrostichum aureum, Acanthus ilicifolius, Aegiceras corniculatum, Kandelia obovate, and Excoecaria agallocha) on Qi’ao Island, South China. The results showed that SOC

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Chen, Zhiwei, Youjun Lu, and Yuetong Zhao. "Constraining the Origin of Stellar Binary Black Hole Mergers by Detections of Their Lensed Host Galaxies and Gravitational Wave Signals." Astrophysical Journal 940, no. 1 (2022): 17. http://dx.doi.org/10.3847/1538-4357/ac98b7.

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Abstract A significant number of stellar binary black hole (sBBH) mergers may be lensed and detected by the third generation of gravitational wave (GW) detectors. Their lensed host galaxies may be detectable, which would thus help to accurately localize these sources and provide a new approach to study the origin of sBBHs. In this paper, we investigate the detectability of lensed host galaxies for lensed sBBH mergers. We find that the detection fraction of galaxies hosting lensed GW events can be significantly different for a survey with a given limiting magnitude if sBBHs are produced by diff

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Ogihara, Masahiro, Yasunori Hori, Masanobu Kunitomo, and Kenji Kurosaki. "Formation of giant planets with large metal masses and metal fractions via giant impacts in a rapidly dissipating disk." Astronomy & Astrophysics 648 (April 2021): L1. http://dx.doi.org/10.1051/0004-6361/202140464.

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Context. According to planetary interior models, some giant planets contain large metal masses with large metal-mass fractions. HD 149026b and TOI-849b are characteristic examples of these giant planets. It has been suggested that the envelope mass loss during giant impacts plays a key role in the formation of such giant planets. Aims. The aim of the present Letter is to propose a mechanism that can explain the origin of such giant planets. Methods. We investigate the formation of giant planets in a rapidly dissipating disk using N-body simulations that consider pebble accretion. Results. The

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Kimbrell, Seth J., Amy E. Reines, Jenny E. Greene, and Marla Geha. "A Comparison between the Morphologies and Structures of Dwarf Galaxies with and without Active Massive Black Holes." Astrophysical Journal 958, no. 2 (2023): 115. http://dx.doi.org/10.3847/1538-4357/acf762.

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Abstract We study the morphologies and structures of 57 dwarf galaxies that are representative of the general population of dwarf galaxies and compare their demographics to a sample of dwarf galaxies hosting optically selected active galactic nuclei (AGNs). The two samples span the same galaxy stellar mass (109 ≲ M ⋆/M ⊙ ≲ 109.5) and color range, and the observations are well-matched in physical resolution. The fractions of irregular galaxies (14%) and early types/ellipticals (∼18%) are nearly identical among the two samples. However, among galaxies with disks (the majority of each sample), th

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Newnham, L., Kelley M. Hess, Karen L. Masters, et al. "The H i morphology and stellar properties of strongly barred galaxies: support for bar quenching in massive spirals." Monthly Notices of the Royal Astronomical Society 492, no. 4 (2020): 4697–715. http://dx.doi.org/10.1093/mnras/staa064.

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ABSTRACT Galactic bars are able to affect the evolution of galaxies by redistributing their gas, possibly contributing to the cessation of star formation. Several recent works point to ‘bar quenching’ playing an important role in massive disc galaxies. We construct a sample of six gas-rich and strongly barred disc galaxies with resolved H i observations. This sample of galaxies, which we call H i-rich barred galaxies, was identified with the help of Galaxy Zoo to find galaxies hosting a strong bar, and the Arecibo Legacy Fast Arecibo L-band Feed Array blind H i survey to identify galaxies with

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Sana, Hugues, and Christopher J. Evans. "The multiplicity of massive stars." Proceedings of the International Astronomical Union 6, S272 (2010): 474–85. http://dx.doi.org/10.1017/s1743921311011124.

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AbstractBinaries are excellent astrophysical laboratories that provide us with direct measurements of fundamental stellar parameters. Compared to single isolated stars, multiplicity induces new processes, offering the opportunity to confront our understanding of a broad range of physics under the extreme conditions found in, and close to, astrophysical objects.In this contribution, we will discuss the parameter space occupied by massive binaries, and the observational means to investigate it. We will review the multiplicity fraction of OB stars within each regime, and in different astrophysica

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