Lowest Rated Papers
Sri Lanka Building Construction Industry Report 2024-2034
Kushan Liyana Arachchige
Research Mind·2025
Comprehensive market research report on Sri Lanka's building construction industry. Market size LKR 1,535 billion, 6.2% CAGR growth forecast, Porter's analysis & strategic insights.
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View paper →The (Limited) Effect of Viscosity in Multiphase Turbulent Mixing
Tirso Marin-Gilabert, Max Gronke, S. Peng Oh
arXiv·2025
Multiphase gas can be found in many astrophysical environments, such as galactic outflows, stellar wind bubbles, and the circumgalactic medium, where the interplay between turbulence, cooling, and viscosity can significantly influence gas dynamics and star formation processes. We investigate the role of viscosity in modulating turbulence and radiative cooling in turbulent radiative mixing layers (TRMLs). In particular, we aim to determine how different amounts of viscosity affect the Kelvin-Helmholtz instability (KHI), turbulence evolution, and the efficiency of gas mixing and cooling. Using idealized 2D numerical setups, we compute the critical viscosity required to suppress the KHI in shear flows characterized by different density contrasts and Mach numbers. These results are then used in a 3D shear layer setup to explore the impact of viscosity on cooling efficiency and turbulence across different cooling regimes. We find that the critical viscosity follows the expected dependence on overdensity and Mach number. Our viscous TRMLs simulations show different behaviors in the weak and strong cooling regimes. In the weak cooling regime, viscosity has a strong impact, resulting in laminar flows and breaking previously established inviscid relations between cooling and turbulence (albeit leaving the total luminosity unaffected). However, in the strong cooling regime, when cooling timescales are shorter than viscous timescales, key scaling relations in TRMLs remain largely intact. In this regime -- which must hold for gas to remain multiphase -- radiative losses dominate, and the system effectively behaves as non-viscous regardless of the actual level of viscosity. Our findings have direct implications for both the interpretation of observational diagnostics and the development of subgrid models in large-scale simulations.
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View paper →A [CII]-158-micron Survey of DLA galaxies at z~4: Observations of Dense and Metal-Enriched Neutral Gas within the Circumgalactic Medium of Star-Forming Galaxies
Marcel Neeleman, Nissim Kanekar, J. Xavier Prochaska, Marc A. Rafelski, Lordrick A. Kahinga
arXiv·2025
We present a survey undertaken with the Atacama Large Millimeter/submillimeter Array (ALMA) to study the galaxies associated with a representative sample of 16 damped Ly-alpha absorbers (DLAs) at z~4.1-4.5, using the [CII]-158-micron ([CII]) line. We detect seven [CII]-emitting galaxies in the fields of 5 DLAs, all of which have absorption metallicity [M/H] > -1.5. We find that the detectability of these HI-selected galaxies with ALMA is a strong function of DLA metallicity, with a detection rate of 71^{+11}_{-20}% for DLAs with [M/H] > -1.5 and 0^{+18}% for DLAs with [M/H] <-1.5. The identified DLA galaxies have far-infrared properties similar to those of typical star-forming galaxies at z ~ 4, with estimated obscured star-formation rates ranging from ~6 Msun/yr to 110 Msun/yr. High-metallicity DLAs therefore provide an efficient way to identify and study samples of high-redshift, star-forming galaxies without preselecting the galaxies by their emission properties. The agreement between the velocities of the metal absorption lines of the DLA and the [CII] emission line of the DLA galaxy indicates that the metals within the DLA originated in the galaxy. With observed impact parameters between 14 and 59 kpc, this indicates that star-forming galaxies at z ~ 4 have a substantial reservoir of dense, cold neutral gas within their circumgalactic medium that has been enriched with metals from the galaxy.
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View paper →Controlling Language and Diffusion Models by Transporting Activations
Pau Rodriguez, Arno Blaas, Michal Klein, Luca Zappella, Nicholas Apostoloff, Marco Cuturi, Xavier Suau
arXiv·2024
The increasing capabilities of large generative models and their ever more widespread deployment have raised concerns about their reliability, safety, and potential misuse. To address these issues, recent works have proposed to control model generation by steering model activations in order to effectively induce or prevent the emergence of concepts or behaviors in the generated output. In this paper we introduce Activation Transport (AcT), a general framework to steer activations guided by optimal transport theory that generalizes many previous activation-steering works. AcT is modality-agnostic and provides fine-grained control over the model behavior with negligible computational overhead, while minimally impacting model abilities. We experimentally show the effectiveness and versatility of our approach by addressing key challenges in large language models (LLMs) and text-to-image diffusion models (T2Is). For LLMs, we show that AcT can effectively mitigate toxicity, induce arbitrary concepts, and increase their truthfulness. In T2Is, we show how AcT enables fine-grained style control and concept negation.
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View paper →Sri Lanka Advertising Industry Analysis 2024: Leo Burnett Strategy
Kushan Liyana Arachchige
Research Mind·2025
Explore the dynamic landscape of the Sri Lanka advertising industry amid digital disruption with insights into market growth.
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View paper →Sri Lanka Marketing Industry Analysis 2024-2034
Kushan Liyana Arachchige
Research Mind·2025
Explore the Sri Lanka marketing industry analysis highlighting digital transformation and growth from US$462 million to US$1.3 billion.
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View paper →Goop Inc.: Aspirational Brand or Snake Oil?
Arpita Agnihotri, Saurabh Bhattacharya
2021
No abstract available
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View paper →Mapping the z ~ 2 Circumgalactic Medium using KBSS Galaxy Pairs
Nikolaus Z. Prusinski, Charles C. Steidel, Yuguang Chen
arXiv·2025
We present new results on the spatial structure and kinematics of the circumgalactic medium (CGM) of z ~ 2 star-forming galaxies drawn from the Keck Baryonic Structure Survey, using Lya and metallic ion absorption recorded in spectra of background galaxies whose sightlines are projected within ~ 30" (physical distances D_tran < 250 kpc) of the foreground galaxy. The sample of 1033 foreground galaxies (<z_fg> = 2.03; 8 < log(M_star/M_sun) < 11) is probed by the spectra of 736 background galaxies obtained using Keck/KCWI (R ~ 1800) and Keck/LRIS (R ~ 1200). Using the galaxy pair ensemble, we present measurements of absorption strength (W_lambda) and line-of-sight velocity dispersion (sigma) as a function of D_tran, which together with "down-the-barrel" spectra of the foreground galaxies provide unprecedented maps of neutral hydrogen and ionized metals throughout the CGM of star-forming galaxies at "cosmic noon". A 2D map of Lya absorption depth (vs. line-of-sight velocity and D_tran) for the full ensemble shows a distinct transition near D_tran ~ 80 kpc (close to the virial radius of the average foreground galaxy) where the line-of-sight velocity dispersion reaches a minimum and beyond which the Lya absorption depth flattens. Splitting the sample into subsets based on foreground galaxy properties, we find a strong and monotonic correlation of both W_lambda(C IV) and sigma(C IV) with stellar mass (M_star) at all D_tran including DTB (i.e., D_tran ~ 0 - 250 kpc). Taken together, our results suggest that the kinematics, covering fraction, and spatial extent of CGM gas traced by Lya and (especially) CIV are modulated primarily by halo mass, and that a significant fraction of the CGM gas may be unbound.
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View paper →Deep Ultraviolet, Emission-Line Imaging of the Makani Galactic Wind
Triet Ha, David Rupke, Shane Caraker, Jack Harper, Alison Coil, Miao Li, Christy Tremonti, Aleksandar Diamond-Stanic, James Geach, Ryan Hickox, Sean Johnson, Gene Leung, John Moustakas, Serena Perrotta, Gregory Rudnick, Paul Sell, Kelly Whalen
arXiv·2025
The OVI 1032, 1038 A line is a key probe of cooling gas in the circumgalactic medium (CGM) of galaxies, but has been observed to date primarily in absorption along single sightlines. We present deep HST ACS-SBC observations of the compact, massive starburst Makani. Makani hosts a 100 kpc, [OII]-emitting galactic wind driven by two episodes of star formation over 400 Myr. We detect OVI and Ly$α$ emission across the [OII] nebula with similar morphology and extent, out to r ~ 50 kpc. Using differential narrow-band imaging, we separate Ly$α$ and OVI and show that the OVI emission is comparable in brightness to [OII], with $L_{OVI} = 4\times10^{42}$ erg/s. The similar hourglass morphology and size of [OII] and OVI implicate radiative cooling at $T = 10^{5.5}$ K in a hot-cold interface. This may occur as the $T > 10^7$ K CGM -- or the hot fluid driving the wind -- exchanges mass with the $T \approx 10^4$ K clouds entrained in (or formed by) the wind. The optical/UV line ratios may be consistent with shock ionization, though uncertain attenuation and Ly$α$ radiative transfer complicate the interpretation. The detection of OVI in Makani lies at the bleeding edge of the UV imaging capabilities of HST, and provides a benchmark for future emission-line imaging of the CGM with a wide-area UV telescope.
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View paper →Impacts of the Metagalactic Ultraviolet Background on Circumgalactic Medium Absorption Systems
Elias Taira, Claire Kopenhafer, Brian W. Oshea, Alexis Manning, Evelyn Fuhrman, Molly S. Peeples, Jason Tumlinson, Britton D. Smith
arXiv·2025
Among the many different pieces of physics that go into simulations of the circumgalactic medium (CGM), the metagalactic ultraviolet background (UVB) plays a significant role in determining the ionization state of different metal species. However, the UVB is uncertain with multiple models having been developed by various research groups over the past several decades. In this work, we examine how different UVB models influence the ionic column densities of CGM absorbers. We use these UVB models to infer ion number densities in the FOGGIE galaxy simulations at $z=2.5$ and use the Synthetic Absorption Line Surveyor Application (SALSA) package to identify absorbers. Absorbers are then matched across UVB models based on their line of sight position so that their column densities can be compared. From our analysis, we find that changing the UVB model produces significant changes in ionization, specifically at lower gas densities and higher temperatures where photoionization dominates over collisional ionization. We also find that the scatter of column density differences between models tends to increase with increasing ionization energy, with the exception of \hi, which has the highest scatter of all species we examined.
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View paper →A Comprehensive Characterization of Galaxy-cool CGM Connections at $z<0.4$ with DESI Year 1 Data
Yu Voon Ng, Ting-Wen Lan, J. Xavier Prochaska, Amélie Saintonge, Yu-Ling Chang, Małgorzata Siudek, Jessica Nicole Aguilar, Steven Ahlen, Davide Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, Arjun Dey, Peter Doel, Simone Ferraro, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Mustapha Ishak, Stephanie Juneau, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Adam Myers, Seshadri Nadathur, Claire Poppett, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
arXiv·2025
We investigate the relationships between the cool circumgalactic medium (CGM), traced by Ca II absorption lines, and galaxy properties at $z<0.4$ using $\sim900{,}000$ galaxy-quasar pairs within $200\,\rm kpc$ from the Year 1 data of the Dark Energy Spectroscopic Instrument (DESI). This large data set enables us to obtain composite spectra with sensitivity reaching to the $\text{mÅ}$ level and to explore the Ca II absorption as a function of stellar mass, star formation rate (SFR), redshift, and galaxy types, including active galactic nuclei (AGNs). Our results show a positive correlation between the absorption strength and stellar mass of star-forming galaxies with $\langle W_{0}^{\rm Ca\ II}\rangle \propto M_{*}^{0.5}$ over 3 orders of magnitude in stellar mass from $\sim 10^{8}$ to $10^{11} \, M_{\odot}$, while such a mass dependence is weaker for quiescent galaxies. At a fixed mass, Ca II absorption is stronger around star-forming galaxies than quiescent ones especially within impact parameters $<30\,\rm kpc$. Among star-forming galaxies, the Ca II absorption further correlates with SFR, following $\propto \mathrm{SFR^{0.3}}$. However, in contrast to the results at higher redshifts, stronger absorption is not preferentially observed along the minor axis of star-forming galaxies, indicating a possible redshift evolution of CGM dynamics resulting from galactic feedback. Moreover, no significant difference between the properties of the cool gas around AGNs and galaxies is detected. Finally, we measure the absorption profiles with respect to the virial radius of dark matter halos and show that the total Ca II mass in the CGM is comparable to the Ca mass in the ISM of galaxies.
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View paper →A Detection of Circumgalactic Dust at Megaparsec Scales with Maximum Likelihood Estimation
Jacqueline E. McCleary, Eric M. Huff, James W. Bartlett, Brandon S. Hensley
arXiv·2025
One of the more surprising astrophysical discoveries of the last decade has been the presence of enormous quantities of dust at megaparsec distances from galaxies, which has important implications for galaxy evolution, the circumgalactic and intergalactic medium, and observational cosmology. In this work, we present a novel method for studying these vast halos of circumgalactic dust: a maximum-likelihood estimator for dust-induced extinction of background galaxies. This estimator can accommodate a broad range of archival photometric data and can incorporate different dust reddening prescriptions, making it applicable to diverse galaxy types and redshifts. We apply the estimator to the redMaGiC catalog of luminous red galaxies, selected for their tight dispersion in color and well-constrained photometric redshifts, and measure the resulting extinction as a function of projected distance from WISExSuperCOSMOS and redMaGiC foreground galaxies. We detect significant dust-induced extinction profiles extending to at least 1 megaparsec from galactic disks, with noticeable differences between star-forming and quiescent galaxies: star-forming galaxies exhibit a pronounced rise in extinction within the inner 50 kiloparsecs and a steep decline beyond 1 megaparsec, while the quiescent galaxies host little dust in the inner halo but have detectable extinction out to 30 megaparsecs. We test the robustness of our results using star catalogs and inverted foreground and background samples and find no evidence for significant systematic error. Our approach provides a powerful tool for studying the interplay between circumgalactic dust, galaxy evolution, and large-scale structure, with potential applications in a number of astrophysical subfields.
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