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Journal articles on the topic 'Cosmic infall'

Author: Grafiati

Published: 4 June 2021

Last updated: 6 February 2022

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1

Jiang, I. G., and J. Binney. "Warps and cosmic infall." Monthly Notices of the Royal Astronomical Society 303, no. 1 (1999): L7—L10. http://dx.doi.org/10.1046/j.1365-8711.1999.02333.x.

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Shen, J., and J. A. Sellwood. "Galactic warps induced by cosmic infall." Monthly Notices of the Royal Astronomical Society 370, no. 1 (2006): 2–14. http://dx.doi.org/10.1111/j.1365-2966.2006.10477.x.

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Kraljic, Katarina, Christophe Pichon, Sandrine Codis, et al. "The impact of the connectivity of the cosmic web on the physical properties of galaxies at its nodes." Monthly Notices of the Royal Astronomical Society 491, no. 3 (2019): 4294–309. http://dx.doi.org/10.1093/mnras/stz3319.

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ABSTRACT We investigate the impact of the number of filaments connected to the nodes of the cosmic web on the physical properties of their galaxies using the Sloan Digital Sky Survey. We compare these measurements to the cosmological hydrodynamical simulations H orizon-(no)AGN and Simba. We find that more massive galaxies are more connected, in qualitative agreement with theoretical predictions and measurements in dark-matter-only simulations. The star formation activity and morphology of observed galaxies both display some dependence on the connectivity of the cosmic web at a fixed stellar ma

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Libeskind, Noam I. "The beaming of subhalo accretion." Proceedings of the International Astronomical Union 11, S308 (2014): 456–61. http://dx.doi.org/10.1017/s174392131601036x.

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AbstractWe examine the infall pattern of subhaloes onto hosts in the context of the large-scale structure. We find that the infall pattern is essentially driven by the shear tensor of the ambient velocity field. Dark matter subhaloes are preferentially accreted along the principal axis of the shear tensor which corresponds to the direction of weakest collapse. We examine the dependence of this preferential infall on subhalo mass, host halo mass and redshift. Although strongest for the most massive hosts and the most massive subhaloes at high redshift, the preferential infall of subhaloes is ef

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Fattahi, Azadeh, Alis J. Deason, Carlos S. Frenk, et al. "A tale of two populations: surviving and destroyed dwarf galaxies and the build-up of the Milky Way’s stellar halo." Monthly Notices of the Royal Astronomical Society 497, no. 4 (2020): 4459–71. http://dx.doi.org/10.1093/mnras/staa2221.

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ABSTRACT We use magnetohydrodynamical simulations of Milky Way-mass haloes from the Auriga project to investigate the properties of surviving and destroyed dwarf galaxies that are accreted by these haloes over cosmic time. We show that the combined luminosity function of surviving and destroyed dwarfs at infall is similar in the various Auriga haloes, and is dominated by the destroyed dwarfs. There is, however, a strong dependence on infall time: destroyed dwarfs typically have early infall times of less than 6 Gyr (since the big bang), whereas the majority of dwarfs accreted after 10 Gyr have

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Impey, Chris D. "Dim Baryons in the Cosmic Web." Proceedings of the International Astronomical Union 3, S244 (2007): 157–66. http://dx.doi.org/10.1017/s1743921307013956.

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AbstractThe distribution of baryons beyond galaxies is descibed. The majority of the baryons, which represent 4% of the cosmic mass and energy budget, lie far from individual galaxies in the diffuse intergalactic medium (IGM). Many of these baryons are in a warm phase that can be probed by quasar absorption in the Lyman-α line of hydrogen. The mature field of quasar spectroscopy can diagnose the location, physical state, metallicity, and general geometry of this gas, which is called the “cosmic web.” The remainder of the gas is kept very hot by infall and shocks and is mostly in higher density

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Peper, Marius, and Boudewijn F. Roukema. "The role of the elaphrocentre in void galaxy formation." Monthly Notices of the Royal Astronomical Society 505, no. 1 (2021): 1223–38. http://dx.doi.org/10.1093/mnras/stab1342.

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ABSTRACT Voids may affect galaxy formation via weakening mass infall or increasing disk sizes, which could potentially play a role in the formation of giant low surface brightness galaxies (LSBGs). If a dark matter halo forms at the potential hill corresponding to a void of the cosmic web, which we denote the ‘elaphrocentre’ in contrast to a barycentre, then the elaphrocentre should weaken the infall rate to the halo when compared to infall rates towards barycentres. We investigate this hypothesis numerically. We present a complete software pipeline to simulate galaxy formation, starting from

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Kashibadze, Olga G., and Igor D. Karachentsev. "Cosmic flow around local massive galaxies." Astronomy & Astrophysics 609 (December 22, 2017): A11. http://dx.doi.org/10.1051/0004-6361/201731645.

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Aims. We use accurate data on distances and radial velocities of galaxies around the Local Group, as well as around 14 other massive nearby groups, to estimate their radius of the zero-velocity surface, R0, which separates any group against the global cosmic expansion. Methods. Our R0 estimate was based on fitting the data to the velocity field expected from the spherical infall model, including effects of the cosmological constant. The reported uncertainties were derived by a Monte Carlo simulation. Results. Testing various assumptions about a location of the group barycentre, we found the op

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Hellwing, Wojciech A. "Dynamics of pairwise motions in the Cosmic Web." Proceedings of the International Astronomical Union 11, S308 (2014): 322–27. http://dx.doi.org/10.1017/s1743921316010085.

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AbstractWe present results of analysis of the dark matter (DM) pairwise velocity statistics in different Cosmic Web environments. We use the DM velocity and density field from the Millennium 2 simulation together with the NEXUS+ algorithm to segment the simulation volume into voxels uniquely identifying one of the four possible environments: nodes, filaments, walls or cosmic voids. We show that the PDFs of the mean infall velocities v12 as well as its spatial dependence together with the perpendicular and parallel velocity dispersions bear a significant signal of the large-scale structure envi

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Almeida, J. Sánchez, A. Olmo-García, B. G. Elmegreen, et al. "Gas accretion from the cosmic web feeding disk galaxies." Proceedings of the International Astronomical Union 11, S321 (2016): 208–10. http://dx.doi.org/10.1017/s1743921316008863.

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AbstractDisk galaxies in cosmological numerical simulations grow by accreting gas from the cosmic web. This gas reaches the external disk, and then spirals in dragged along by tidal forces and/or disk instabilities. The importance of gas infall is as clear from numerical simulations as it is obscure to observations. Extremely metal poor (XMP) galaxies seem to be the best example we have of the gas accretion process at work. They have large off-center starbursts which show significant metallicity drop compared with the host galaxy. This observation is naturally explained as a gas accretion even

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Kuchner, Ulrike, Alfonso Aragón-Salamanca, Agustín Rost, et al. "Cosmic filaments in galaxy cluster outskirts: quantifying finding filaments in redshift space." Monthly Notices of the Royal Astronomical Society 503, no. 2 (2021): 2065–76. http://dx.doi.org/10.1093/mnras/stab567.

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ABSTRACT Inferring line-of-sight distances from redshifts in and around galaxy clusters is complicated by peculiar velocities, a phenomenon known as the ‘Fingers of God’ (FoG). This presents a significant challenge for finding filaments in large observational data sets as these artificial elongations can be wrongly identified as cosmic web filaments by extraction algorithms. Upcoming targeted wide-field spectroscopic surveys of galaxy clusters and their infall regions, such as the WEAVE Wide-Field Cluster Survey, motivate our investigation of the impact of FoG on finding filaments connected to

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Mayer, Lucio. "Environmental Mechanisms Shaping the Nature of Dwarf Spheroidal Galaxies: The View of Computer Simulations." Advances in Astronomy 2010 (2010): 1–21. http://dx.doi.org/10.1155/2010/278434.

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We review numerical works carried out over the last decade on the role of environmental mechanisms in shaping nature of the faintest galaxies known, dwarf spheroidals (dSphs). The combination of tidally induced morphological transformation, termed tidal stirring, with mass loss due to tidal and ram-pressure stripping aided by heating due to the cosmic ionizing background can turn late-type dwarfs resembling present-day dIrrs into classic dSphs. The time of infall into the primary halo is shown to be a key parameter. Dwarfs accreting at when the cosmic ultraviolet ionizing flux was much higher

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Blaña, Matías, Andreas Burkert, Michael Fellhauer, Marc Schartmann, and Christian Alig. "Dwarfs in the Milky Way halo outer rim: first infall or backsplash satellites?" Monthly Notices of the Royal Astronomical Society 497, no. 3 (2020): 3601–22. http://dx.doi.org/10.1093/mnras/staa2153.

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ABSTRACT Leo T is a gas-rich dwarf located at $414\, {\rm kpc}$ (1.4Rvir) distance from the Milky Way (MW) and it is currently assumed to be on its first approach. Here, we present an analysis of orbits calculated backwards in time for the dwarf with our new code delorean, exploring a range of systematic uncertainties, e.g. MW virial mass and accretion, M31 potential, and cosmic expansion. We discover that orbits with tangential velocities in the Galactic standard-of-rest frame lower than $| \vec{u}_{\rm t}^{\rm GSR}| \le 63^{+47}_{-39}\, {\rm km}\, {\rm s}^{\rm -1}$ result in backsplash solut

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Aubert, D., C. Pichon, and S. Colombi. "The origin and implications of dark matter anisotropic cosmic infall on ≈L★haloes." Monthly Notices of the Royal Astronomical Society 352, no. 2 (2004): 376–98. http://dx.doi.org/10.1111/j.1365-2966.2004.07883.x.

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Pomarède, Daniel, Hélène Courtois, and R. Brent Tully. "Visualization of structures and cosmic flows in the local Universe." Proceedings of the International Astronomical Union 8, S289 (2012): 323–26. http://dx.doi.org/10.1017/s174392131202162x.

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AbstractA visualization of 3D structures and cosmic flows is presented using information from the Extragalactic Distance Database V8k redshift catalog and peculiar velocities from the Cosmicflows-1 survey. Structures within a volume bounded at 8000 km s−1 on the cardinal Supergalactic axes are explored in terms of both displaying the positions of the 30,124 galaxies of the catalog and its reconstructed luminosity density field, corrected to account for growing incompleteness with increasing distance. Cosmography of the local Universe is discussed with the intent to identify the most prominent

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Daddi, E., F. Valentino, R. M. Rich та ін. "Three Lyman-α-emitting filaments converging to a massive galaxy group at z = 2.91: discussing the case for cold gas infall". Astronomy & Astrophysics 649 (травень 2021): A78. http://dx.doi.org/10.1051/0004-6361/202038700.

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We have discovered a 300 kpc-wide giant Lyman-α (Lyα) nebula centered on the massive galaxy group RO-1001 at z = 2.91 in the Cosmic Evolution Survey field. Keck Cosmic Web Imager observations reveal three cold gas filaments converging into the center of the potential well of its ∼4 × 1013 M⊙ dark matter halo, hosting 1200 M⊙ yr−1 of star formation as probed by Atacama Large Millimeter Array and NOrthern Extended Millimeter Array observations. The nebula morphological and kinematics properties and the prevalence of blueshifted components in the Lyα spectra are consistent with a scenario of gas

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Hopkins, Andrew. "Galaxy Metabolism." Publications of the Astronomical Society of Australia 27, no. 3 (2010): 233. http://dx.doi.org/10.1071/as10012.

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‘Galaxy Metabolism' was the second in the annual ‘Southern Cross Astrophysics Conference Series’ (http://www.aao.gov.au/AAO/southerncross/), supported by the Anglo-Australian Observatory and the Australia Telescope National Facility. It was held at the Australian National Maritime Museum in Darling Harbour, Sydney, from 22 to 26 June 2009, and was attended by 91 delegates from around the world.Over the past decade, both the star formation history and stellar mass density in galaxies spanning most of cosmic history have been well constrained. This provides the backdrop and framework within whic

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Malavasi, Nicola, Nabila Aghanim, Hideki Tanimura, Victor Bonjean, and Marian Douspis. "Like a spider in its web: a study of the large-scale structure around the Coma cluster." Astronomy & Astrophysics 634 (January 31, 2020): A30. http://dx.doi.org/10.1051/0004-6361/201936629.

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The Cosmic Web is a complex network of filaments, walls, and voids that represent the largest structures in the Universe. In this network, which is the direct result of structure formation, galaxy clusters occupy central positions that form the nodes and these are connected by filaments. In this work, we investigate the position in the Cosmic Web of one of the most well-known and best-studied clusters of galaxies, the Coma cluster. We make use of the Sloan Digital Sky Survey Data Release 7 Main Galaxy Sample and of the Discrete Persistent Structure Extractor to detect large-scale filaments aro

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Sarron, F., C. Adami, F. Durret, and C. Laigle. "Pre-processing of galaxies in cosmic filaments around AMASCFI clusters in the CFHTLS." Astronomy & Astrophysics 632 (November 26, 2019): A49. http://dx.doi.org/10.1051/0004-6361/201935394.

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Context. Galaxy clusters and groups are thought to accrete material along the preferred direction of cosmic filaments. These structures have proven difficult to detect because their contrast is low, however, and only a few studies have focused on cluster infall regions. Aims. We detect cosmic filaments around galaxy clusters using photometric redshifts in the range 0.15 < z < 0.7. We characterise galaxy populations in these structures to study the influence of pre-processing by cosmic filaments and galaxy groups on star formation quenching. Methods. We detected cosmic filaments in the Ca

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Hsu, Hsiang-Wen, Jürgen Schmidt, Sascha Kempf, et al. "In situ collection of dust grains falling from Saturn’s rings into its atmosphere." Science 362, no. 6410 (2018): eaat3185. http://dx.doi.org/10.1126/science.aat3185.

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Saturn’s main rings are composed of >95% water ice, and the nature of the remaining few percent has remained unclear. The Cassini spacecraft’s traversals between Saturn and its innermost D ring allowed its cosmic dust analyzer (CDA) to collect material released from the main rings and to characterize the ring material infall into Saturn. We report the direct in situ detection of material from Saturn’s dense rings by the CDA impact mass spectrometer. Most detected grains are a few tens of nanometers in size and dynamically associated with the previously inferred “ring rain.” Silicate and wat

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Kraljic, Katarina, Romeel Davé, and Christophe Pichon. "And yet it flips: connecting galactic spin and the cosmic web." Monthly Notices of the Royal Astronomical Society 493, no. 1 (2020): 362–81. http://dx.doi.org/10.1093/mnras/staa250.

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ABSTRACT We study the spin alignment of galaxies and haloes with respect to filaments and walls of the cosmic web, identified with DisPerSE , using the Simba simulation from z = 0 − 2. Massive haloes’ spins are oriented perpendicularly to their closest filament’s axis and walls, while low-mass haloes tend to have their spins parallel to filaments and in the plane of walls. A similar mass-dependent spin flip is found for galaxies, albeit with a weaker signal particularly at low mass and low-z, suggesting that galaxies’ spins retain memory of their larger scale environment. Low-z star-forming an

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Vallés-Pérez, David, Susana Planelles, and Vicent Quilis. "Troubled cosmic flows: turbulence, enstrophy, and helicity from the assembly history of the intracluster medium." Monthly Notices of the Royal Astronomical Society 504, no. 1 (2021): 510–27. http://dx.doi.org/10.1093/mnras/stab880.

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ABSTRACT Both simulations and observations have shown that turbulence is a pervasive phenomenon in cosmic scenarios, yet it is particularly difficult to model numerically due to its intrinsically multiscale character which demands high resolutions. Additionally, turbulence is tightly connected to the dynamical state and the formation history of galaxies and galaxy clusters, producing a diverse phenomenology which requires large samples of such structures to attain robust conclusions. In this work, we use an adaptive mesh refinement (AMR) cosmological simulation to explore the generation and di

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Totani, Tomonori. "Luminosity Density Evolution in the Universe and Cosmological Parameters." Symposium - International Astronomical Union 183 (1999): 145–50. http://dx.doi.org/10.1017/s0074180900132309.

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Star formation history in galaxies is strongly correlated to their present-day colors and the Hubble sequence can be considered as a sequence of different star formation history. Therefore we can model the cosmic star formation history based on the colors of local galaxies, and comparison to direct observations of luminosity density evolution at high redshift gives a new test for the cosmological parameters which is insensitive to merger history of galaxies. The luminosity density evolution in 0 < z < 1 observed by the Canada-France Redshift Survey in three wavebands of 2800Å, 4400Å, and

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Kashibadze, Olga, Igor Karachentsev, and Valentina Karachentseva. "Dwarfs in the entourage of the Local Volume groups: flow tracers and cosmological probes." Proceedings of the International Astronomical Union 14, S344 (2018): 488–90. http://dx.doi.org/10.1017/s1743921318005586.

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AbstractWe consider a sample of dwarf galaxies with accurate distances and velocities around 14 massive groups in the Local Volume. We combine all the data into a single synthetic group, and then determine its radius of the zero-velocity surface, separating it against the global cosmic expansion. Our estimation is derived from fitting the the spherical infall model (including effects of the cosmological constant) to the observational data.We found the optimal value of the radius to be 0.93 ± 0.02 Mpc. Assuming the Planck model parameters, it corresponds to the total mass of the synthetic group

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Goerdt, Tobias. "Cold streams: detectability, relation to structure and characteristics." Proceedings of the International Astronomical Union 10, S309 (2014): 269–72. http://dx.doi.org/10.1017/s1743921314009843.

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AbstractCold gas streaming along the dark-matter filaments of the cosmic web is predicted to be the major provider of resources for disc buildup and star formation in massive galaxies in the early universe. We use hydrodynamical simulations to study to what extent these cold streams are traceable in the extended circum-galactic environment of galaxies via Ly alpha emission, Ly alpha absorption and selected low ionisation metal absorption lines. We predict the strength of the absorption signal produced by the streams and find that it is consistent with observations in high redshift galaxies. Th

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Bartlett, Deaglan J., Harry Desmond, Julien Devriendt, Pedro G. Ferreira, and Adrianne Slyz. "Spatially offset black holes in the Horizon-AGN simulation and comparison to observations." Monthly Notices of the Royal Astronomical Society 500, no. 4 (2020): 4639–57. http://dx.doi.org/10.1093/mnras/staa3516.

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ABSTRACT We study the displacements between the centres of galaxies and their supermassive black holes (BHs) in the cosmological hydrodynamical simulation Horizon-AGN, and in a variety of observations from the literature. The BHs in Horizon-AGN feel a subgrid dynamical friction force, sourced by the surrounding gas, which prevents recoiling BHs being ejected from the galaxy. We find that (i) the fraction of spatially offset BHs increases with cosmic time, (ii) BHs live on prograde orbits in the plane of the galaxy with an orbital radius that decays with time but stalls near z = 0, and (iii) th

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JAIN, DEEPAK, N. PANCHAPAKESAN, S. MAHAJAN, and V. B. BHATIA. "CONSTRAINTS ON GALAXY EVOLUTION THROUGH GRAVITATIONAL LENSING STATISTICS." Modern Physics Letters A 15, no. 01 (2000): 41–53. http://dx.doi.org/10.1142/s0217732300000074.

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Explaining the formation and evolution of galaxies is one of the most challenging problems in observational cosmology. Many observations suggest that galaxies we see today could have evolved from the merging of smaller subsystems. Evolution of galaxies tells us how the mass or number density of the lens varies with cosmic time. Merging between the galaxies and the infall of surrounding mass into galaxies are two possible processes that can change the comoving number density of galaxies and/or their mass. We consider five different evolutionary models of galaxies. These models are: Non-evolutio

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Nasonova, O., I. Karachentsev, and V. Karachentseva. "Structure and kinematics of the Bootes filament." Proceedings of the International Astronomical Union 11, S308 (2014): 187–92. http://dx.doi.org/10.1017/s1743921316009820.

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AbstractBootes filament of galaxies is a dispersed chain of groups residing on sky between the Local Void and the Virgo cluster. We consider a sample of 361 galaxies inside the sky area of RA = 13h0...18h.5 and Dec = .5°... + 10° with radial velocities VLG < 2000 km/s to clarify its structure and kinematics. In this region, 161 galaxies have individual distance estimates. We use these data to draw the Hubble relation for galaxy groups, pairs as well as the field galaxies, and to examine the galaxy distribution on peculiar velocities. Our analysis exposes the known Virgo-centric infall at RA

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Welker, C., Y. Dubois, C. Pichon, J. Devriendt, and N. E. Chisari. "Caught in the rhythm." Astronomy & Astrophysics 613 (May 2018): A4. http://dx.doi.org/10.1051/0004-6361/201629007.

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Context. The anisotropic distribution of satellites around the central galaxy of their host halo is both well-documented in observations and predicted by the ΛCDM model. However its amplitude, direction and possible biases associated to the specific dynamics of such satellite galaxies are still highly debated. Aims. Using the cosmological hydrodynamics simulation Horizon-AGN, we aim to quantify the anisotropy of the spatial distribution of satellite galaxies relative to their central counterpart and explore its connexion to the local cosmic web, in the redshift range between 0.3 and 0.8. Metho

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Clavico, S., S. De Grandi, S. Ghizzardi, et al. "Growth and disruption in the Lyra complex." Astronomy & Astrophysics 632 (November 22, 2019): A27. http://dx.doi.org/10.1051/0004-6361/201936467.

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Context. Nearby clusters of galaxies, z ≲ 0.1, are cosmic structures still under formation. Understanding the thermodynamic properties of merging clusters can provide crucial information on how they grow in the local universe. Aims. A detailed study of the intra-cluster medium (ICM) properties of un-relaxed systems is essential to understand the fate of in-falling structures and, more generally, the virialization process. Methods. We analyzed a mosaic of XMM-Newton observations (240 ks) of the Lyra system (z ∼ 0.067) that shows a complex dynamical state. Results. We find the main cluster RXC J

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KAMIONKOWSKI, MARC, and ANDREW H. JAFFE. "DETECTION OF GRAVITATIONAL WAVES FROM INFLATION." International Journal of Modern Physics A 16, supp01a (2001): 116–28. http://dx.doi.org/10.1142/s0217751x01006358.

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Recent measurements of temperature fluctuations in the cosmic microwave background (CMB) indicate that the Universe is flat and that large-scale structure grew via gravitational infall from primordial adiabatic perturbations. Both od these observations seem to indicate that we are on the right track with inflation. But what is the new physics responsible for inflation? This question can be answered with observations of the polarization of the CMB. Inflation predicts robustly the existence of a stochastic background of cosmological gravitational waves with an amplitude proportional to the squar

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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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Santana-Silva, L., T. S. Gonçalves, A. Basu-Zych, et al. "The environment of Lyman break analogues (ELBA) survey: star-forming galaxies in small groups." Monthly Notices of the Royal Astronomical Society 498, no. 4 (2020): 5183–93. http://dx.doi.org/10.1093/mnras/staa2757.

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ABSTRACT The environment of Lyman break analogues survey is an imaging survey of 33 deg2 of the southern sky. The survey was observed in u, g, r, and i bands with the Dark Energy Camera on the Blanco telescope. The main goal of this project is to investigate the environment of Lyman break analogues (LBAs) low-redshift (z ∼0.2) galaxies that are remarkably similar to typical star-forming galaxies at z ∼ 3. We explore whether the environment has any influence on the observed properties of these galaxies, providing valuable insight on the formation and evolution of galaxies over cosmic time. Usin

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Wright, Ruby J., Claudia del P. Lagos, Chris Power, and Peter D. Mitchell. "The impact of stellar and AGN feedback on halo-scale baryonic and dark matter accretion in the eagle simulations." Monthly Notices of the Royal Astronomical Society 498, no. 2 (2020): 1668–92. http://dx.doi.org/10.1093/mnras/staa2359.

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ABSTRACT We use the eagle suite of hydrodynamical simulations to analyse accretion rates (and the breakdown of their constituent channels) on to haloes over cosmic time, comparing the behaviour of baryons and dark matter (DM). We also investigate the influence of sub-grid baryon physics on halo-scale inflow, specifically the consequences of modelling radiative cooling, as well as feedback from stars and active galactic nuclei (AGNs). We find that variations in halo baryon fractions at fixed mass (particularly their circumgalactic medium gas content) are very well correlated with variations in

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Ruffle, Paul, Tom Millar, Helen Roberts, Don Lubowich, and Christian Henkel. "Molecular line observations and chemical modelling of galactic edge clouds." Proceedings of the International Astronomical Union 4, S251 (2008): 145–46. http://dx.doi.org/10.1017/s1743921308021418.

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AbstractEdge Clouds 1 and 2 (EC1 and EC2) are large molecular clouds with the largest galactocentric distances known to exist in the Milky Way. We present observations of these clouds and use them to determine physical characteristics. For EC2 we calculate a gas temperature of 20 K and a density ofn(H2) ~ 104cm−3. Based on our CO maps, we estimate the mass of EC2 at around 104M⊙, and continuum observations suggest a dust-to-gas mass ratio as low as 0.001. Chemical models have been developed to reproduce the abundances in EC2 and they indicate that: heavy element abundances may be reduced by a

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Hoffman, Yehuda, Adi Nusser, Aurélien Valade, Noam I. Libeskind, and R. Brent Tully. "From Cosmicflows distance moduli to unbiased distances and peculiar velocities." Monthly Notices of the Royal Astronomical Society 505, no. 3 (2021): 3380–92. http://dx.doi.org/10.1093/mnras/stab1457.

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ABSTRACT Surveys of galaxy distances and radial peculiar velocities can be used to reconstruct the large-scale structure. Other than systematic errors in the zero-point calibration of the galaxy distances the main source of uncertainties of such data is errors on the distance moduli, assumed here to be Gaussian and thus turning into lognormal errors on distances and velocities. Naively treated, this leads to spurious nearby outflow and strong infall at larger distances. The lognormal bias is corrected here and tested against mock data extracted from a ΛCDM simulation, designed to statistically

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Behroozi, Peter, Risa H. Wechsler, Andrew P. Hearin, and Charlie Conroy. "UniverseMachine: The correlation between galaxy growth and dark matter halo assembly from z = 0−10." Monthly Notices of the Royal Astronomical Society 488, no. 3 (2019): 3143–94. http://dx.doi.org/10.1093/mnras/stz1182.

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ABSTRACTWe present a method to flexibly and self-consistently determine individual galaxies’ star formation rates (SFRs) from their host haloes’ potential well depths, assembly histories, and redshifts. The method is constrained by galaxies’ observed stellar mass functions, SFRs (specific and cosmic), quenched fractions, ultraviolet (UV) luminosity functions, UV–stellar mass relations, IRX–UV relations, auto- and cross-correlation functions (including quenched and star-forming subsamples), and quenching dependence on environment; each observable is reproduced over the full redshift range avail

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Zu, Ying. "Kinematics of Mg ii absorbers from the redshift-space distortion around massive quiescent galaxies." Monthly Notices of the Royal Astronomical Society 506, no. 1 (2021): 115–27. http://dx.doi.org/10.1093/mnras/stab1752.

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ABSTRACT The kinematics of Mg ii absorbers is the key to understanding the origin of cool, metal-enriched gas clouds in the circumgalactic medium of massive quiescent galaxies. Exploiting the fact that the cloud line-of-sight velocity distribution is the only unknown for predicting the redshift-space distortion (RSD) of Mg ii absorbers from their 3D real-space distribution around galaxies, we develop a novel method to infer the cool cloud kinematics from the redshift-space galaxy–cloud cross-correlation ξs. We measure ξs for ∼104 Mg ii absorbers around ∼8 × 105 CMASS galaxies at 0.4 &lt; z

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Gallazzi, Anna R., A. Pasquali, S. Zibetti та F. La Barbera. "Galaxy evolution across environments as probed by the ages, stellar metallicities, and [α /Fe] of central and satellite galaxies". Monthly Notices of the Royal Astronomical Society 502, № 3 (2021): 4457–78. http://dx.doi.org/10.1093/mnras/stab265.

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ABSTRACT We explore how the star formation and metal enrichment histories of present-day galaxies have been affected by environment combining stellar population parameter estimates and group environment characterization for SDSS DR7. We compare stellar ages, stellar metallicities, and crucially, element abundance ratios $\rm [\alpha /Fe]$ of satellite and central galaxies, as a function of their stellar and host group halo mass, controlling for the current star formation rate and for the infall epoch. We confirm that below M* ∼ 1010.5 M⊙ satellites are older and slightly metal richer than equa

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Einasto, Maret, Boris Deshev, Heidi Lietzen, et al. "Infalling groups and galaxy transformations in the cluster A2142." Astronomy & Astrophysics 610 (February 2018): A82. http://dx.doi.org/10.1051/0004-6361/201731600.

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Context. Superclusters of galaxies provide dynamical environments for the study of the formation and evolution of structures in the cosmic web from galaxies, to the richest galaxy clusters, and superclusters themselves. Aims. We study galaxy populations and search for possible merging substructures in the rich galaxy cluster A2142 in the collapsing core of the supercluster SCl A2142, which may give rise to radio and X-ray structures in the cluster, and affect galaxy properties of this cluster. Methods. We used normal mixture modelling to select substructure of the cluster A2142. We compared al

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Beckman, John, Peter Erwin, and Leonel Gutiérrez. "What Disc Brightness Profiles Can Tell us about Galaxy Evolution." Proceedings of the International Astronomical Union 10, H16 (2012): 361. http://dx.doi.org/10.1017/s1743921314011338.

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AbstractAzimuthally averaged surface brightness profiles of disc galaxies provide a most useful practical classification scheme which gives insights into their evolution. Freeman (1970) first classified disc profiles into Type I, with a single exponential decline in surface brightness, and Type II, having a split exponential profile, whose inner radial portion is shallower than its outer section. Van der Kruit & and Searle, (1981) drew attention to sharply truncated profiles of outer discs observed edge-on, but more recently Pohlen et al. (2004) showed that if these same galaxies were obse

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Babichev, Eugeny, Philippe Brax, Chiara Caprini, Jérôme Martin, and Danièle A. Steer. "Dirac Born Infeld (DBI) cosmic strings." Journal of High Energy Physics 2009, no. 03 (2009): 091. http://dx.doi.org/10.1088/1126-6708/2009/03/091.

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Ikrima, Ika, Handhika S. Ramadhan, and Terry Mart. "Cosmic String Global Superconducting Dirac Born Infeld." Journal of Physics: Conference Series 739 (August 2016): 012061. http://dx.doi.org/10.1088/1742-6596/739/1/012061.

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Ferraro, Rafael, and Franco Fiorini. "The regular cosmic string in Born-Infeld gravity." Journal of Physics: Conference Series 314 (September 22, 2011): 012114. http://dx.doi.org/10.1088/1742-6596/314/1/012114.

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Narayanan, Desika, and Chris Carilli. "A cosmic growth spurt in an infant galaxy." Nature 496, no. 7445 (2013): 303–4. http://dx.doi.org/10.1038/496303a.

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Lee, Ha-Na, Kwang-Ho Kwon, and Jin-Koo Kim. "Progressive Collapse Resisting Capacity of Building Structures with Infill Steel Panels." Journal of the Computational Structural Engineering Institute of Korea 25, no. 1 (2012): 19–26. http://dx.doi.org/10.7734/coseik.2012.25.1.019.

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Capozziello, Salvatore, Mariafelicia De Laurentis, and Ratbay Myrzakulov. "Noether symmetry approach for Dirac–Born–Infeld cosmology." International Journal of Geometric Methods in Modern Physics 12, no. 05 (2015): 1550065. http://dx.doi.org/10.1142/s0219887815500656.

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We consider the Noether Symmetry Approach for a cosmological model derived from a tachyon scalar field T with a Dirac–Born–Infeld Lagrangian and a potential V(T). Furthermore, we assume a coupled canonical scalar field ϕ with an arbitrary interaction potential B(T, ϕ). Exact solutions are derived consistent with the accelerated behavior of cosmic fluid.

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Cruz, N. M. Jiménez, and Celia Escamilla-Rivera. "Dynamical cosmologies in Eddington-inspired-Born–Infeld theory." International Journal of Modern Physics D 28, no. 15 (2019): 1950167. http://dx.doi.org/10.1142/s0218271819501670.

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In this paper, we study the cosmological evolution of the universe filled with a perfect fluid in the Eddington-inspired-Born–Infeld gravity. Applying an alternative method in which the evolution of the scale factor for this theory is linked to the cosmographic parameters, we obtain a dynamical dark energy solution where the singularity (through a regular bounce or a loitering phase) still can be avoided for [Formula: see text] with [Formula: see text]. For the range [Formula: see text], the results lead us to universes that experience an unlimited rate of expansion with finite density. Also,

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Holt, Ewa M. "Estimating the mass of cosmic rays by combining radio and muon measurements." EPJ Web of Conferences 216 (2019): 02002. http://dx.doi.org/10.1051/epjconf/201921602002.

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The Auger Engineering Radio Array (AERA) is a radio detector at the Pierre Auger Observatory and it is dedicated to measure the radio emission of cosmic-ray air showers. AERA is co-located with the underground muon detectors of the Auger Muons and Infill for the Ground Array (AMIGA). This provides a perfect setup to experimentally test the benefits of combining muons and radio emission for estimating the primary mass. We have investigated this combination using air-shower simulations. We compared the performance for mass separation of this new method to alternative methods in which the electro

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DeYOUNG, TYCE. "NEUTRINO ASTRONOMY WITH ICECUBE." Modern Physics Letters A 24, no. 20 (2009): 1543–57. http://dx.doi.org/10.1142/s0217732309031417.

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IceCube is a kilometer-scale high energy neutrino telescope under construction at the South Pole, a second-generation instrument expanding the capabilities of the AMANDA telescope. The scientific portfolio of IceCube includes the detection of neutrinos from astrophysical objects such as the sources of the cosmic rays, the search for dark matter, and fundamental physics using a very large data set of atmospheric neutrinos. The design and status of IceCube are briefly reviewed, followed by a summary of results to date from AMANDA and initial IceCube results from the 2007 run, with 22 of a planne

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