RAS_WEB (Page 2,353)

Dual-temperature acceleration radiation. (arXiv:2102.00158v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Good_M/0/1/0/all/0/1">Michael R.R. Good</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Mitra_A/0/1/0/all/0/1">Ayan Mitra</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Zarikas_V/0/1/0/all/0/1">Vasileios Zarikas</a> We solve for a system that emits acceleration radiation at two different temperatures. The equilibrium states occur asymptotically in Planck distributions and transition non-thermally. The model is simple enough to obtain a global solution for the radiation spectrum analytically. We present it as a potentially useful model for investigation of non-thermal vacuum acceleration radiation in the presence of final(initial) asymptotic thermodynamic horizon(less) states in equilibrium. We solve for a system that emits acceleration radiation at two different temperatures. The equilibrium states occur asymptotically in Planck distributions and transition non-thermally.Read More →

Screening the Higgs portal. (arXiv:2101.10693v2 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Brax_P/0/1/0/all/0/1">Philippe Brax</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Burrage_C/0/1/0/all/0/1">Clare Burrage</a> Light scalar fields that couple to matter through the Higgs portal mediate long range fifth forces. We show how the mixing of a light scalar with the Higgs field can lead to this fifth force being screened around macroscopic objects. This behaviour can only be seen by considering both scalar fields as dynamical, and is missed if the mixing between the Higgs field and the scalar field is not taken into account. We explain under which conditions the naive “integrating out” procedure fails, i.e. when the mass matrix of the Higgs-scalars systemRead More →

A Long Stream of Metal-Poor Cool Gas around a Massive Starburst Galaxy at z = 2.67. (arXiv:2101.06273v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Fu_H/0/1/0/all/0/1">Hai Fu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xue_R/0/1/0/all/0/1">Rui Xue</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prochaska_J/0/1/0/all/0/1">J. Xavier Prochaska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stockton_A/0/1/0/all/0/1">Alan Stockton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ponnada_S/0/1/0/all/0/1">Sam Ponnada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lau_M/0/1/0/all/0/1">Marie Wingyee Lau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cooray_A/0/1/0/all/0/1">Asantha Cooray</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Narayanan_D/0/1/0/all/0/1">Desika Narayanan</a> We present the first detailed dissection of the circumgalactic medium (CGM) of massive starburst galaxies at z > 2. Our target is a submillimeter galaxy (SMG) at z = 2.674 that has a star formation rate of 1200 $M_odot$/yr and a molecular gas reservoir of $1.3times10^{11} M_odot$. We characterize its CGM with two background QSOs at impact parameters of 93Read More →

Composite Bulges — II. Classical Bulges and Nuclear Discs in Barred Galaxies: The Contrasting Cases of NGC 4608 and NGC 4643. (arXiv:2101.05321v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Erwin_P/0/1/0/all/0/1">Peter Erwin</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Seth_A/0/1/0/all/0/1">Anil Seth</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Debattista_V/0/1/0/all/0/1">Victor P. Debattista</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Seidel_M/0/1/0/all/0/1">Marja Seidel</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Mehrgan_K/0/1/0/all/0/1">Kianusch Mehrgan</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Thomas_J/0/1/0/all/0/1">Jens Thomas</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Saglia_R/0/1/0/all/0/1">Roberto Saglia</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Lorenzo_Caceres_A/0/1/0/all/0/1">Adriana de Lorenzo-C&#xe1;ceres</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Maciejewski_W/0/1/0/all/0/1">Witold Maciejewski</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Fabricius_M/0/1/0/all/0/1">Maximilian Fabricius</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Mendez_Abreu_J/0/1/0/all/0/1">Jairo M&#xe9;ndez-Abreu</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Hopp_U/0/1/0/all/0/1">Ulrich Hopp</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Kluge_M/0/1/0/all/0/1">Matthias Kluge</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Beckman_J/0/1/0/all/0/1">John E. Beckman</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Bender_R/0/1/0/all/0/1">Ralf Bender</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Drory_N/0/1/0/all/0/1">Niv Drory</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Fisher_D/0/1/0/all/0/1">Deanne Fisher</a> (8) ((1) Max-Planck-Institut fuer extraterrestrische Physik, Garching, Germany, (2) Department ofRead More →

Accretion Geometry in the Hard State of the Black-Hole X-Ray Binary MAXI J1820+070. (arXiv:2101.04482v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Zdziarski_A/0/1/0/all/0/1">Andrzej A. Zdziarski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dzielak_M/0/1/0/all/0/1">Marta A. Dzielak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marco_B/0/1/0/all/0/1">Barbara De Marco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Szanecki_M/0/1/0/all/0/1">Michal Szanecki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Niedzwiecki_A/0/1/0/all/0/1">Andrzej Niedzwiecki</a> We study X-ray spectra from the outburst rise of the accreting black-hole binary MAXI J1820+070. We find that models having the disk inclinations within those of either the binary or the jet imply significant changes of the accretion disk inner radius during the luminous part of the hard spectral state, with that radius changing from $>$100 to $sim$10 gravitational radii. The main trend is a decrease with the decreasing spectral hardness.Read More →

Development of highly radiopure NaI(Tl) scintillator for PICOLON dark matter search project. (arXiv:2101.00759v2 [physics.ins-det] UPDATED) <a href="http://arxiv.org/find/physics/1/au:+Fushimi_K/0/1/0/all/0/1">K. Fushimi</a>, <a href="http://arxiv.org/find/physics/1/au:+Kanemitsu_Y/0/1/0/all/0/1">Y. Kanemitsu</a>, <a href="http://arxiv.org/find/physics/1/au:+Hirata_S/0/1/0/all/0/1">S. Hirata</a>, <a href="http://arxiv.org/find/physics/1/au:+Chernyak_D/0/1/0/all/0/1">D. Chernyak</a>, <a href="http://arxiv.org/find/physics/1/au:+Hazama_R/0/1/0/all/0/1">R. Hazama</a>, <a href="http://arxiv.org/find/physics/1/au:+Ikeda_H/0/1/0/all/0/1">H. Ikeda</a>, <a href="http://arxiv.org/find/physics/1/au:+Imagawa_K/0/1/0/all/0/1">K. Imagawa</a>, <a href="http://arxiv.org/find/physics/1/au:+Ishiura_H/0/1/0/all/0/1">H. Ishiura</a>, <a href="http://arxiv.org/find/physics/1/au:+Ito_H/0/1/0/all/0/1">H. Ito</a>, <a href="http://arxiv.org/find/physics/1/au:+Kisimoto_T/0/1/0/all/0/1">T. Kisimoto</a>, <a href="http://arxiv.org/find/physics/1/au:+Kozlov_A/0/1/0/all/0/1">A. Kozlov</a>, <a href="http://arxiv.org/find/physics/1/au:+Takemoto_Y/0/1/0/all/0/1">Y. Takemoto</a>, <a href="http://arxiv.org/find/physics/1/au:+Yasuda_K/0/1/0/all/0/1">K. Yasuda</a>, <a href="http://arxiv.org/find/physics/1/au:+Ejiri_H/0/1/0/all/0/1">H. Ejiri</a>, <a href="http://arxiv.org/find/physics/1/au:+Hata_K/0/1/0/all/0/1">K. Hata</a>, <a href="http://arxiv.org/find/physics/1/au:+Iida_T/0/1/0/all/0/1">T. Iida</a>, <a href="http://arxiv.org/find/physics/1/au:+Inoue_K/0/1/0/all/0/1">K. Inoue</a>, <a href="http://arxiv.org/find/physics/1/au:+Koga_M/0/1/0/all/0/1">M. Koga</a>, <a href="http://arxiv.org/find/physics/1/au:+Nakamura_K/0/1/0/all/0/1">K. Nakamura</a>, <a href="http://arxiv.org/find/physics/1/au:+Orito_R/0/1/0/all/0/1">R. Orito</a>, <a href="http://arxiv.org/find/physics/1/au:+Shima_T/0/1/0/all/0/1">T. Shima</a>, <a href="http://arxiv.org/find/physics/1/au:+Umehara_S/0/1/0/all/0/1">S. Umehara</a>, <a href="http://arxiv.org/find/physics/1/au:+Yoshida_S/0/1/0/all/0/1">S. Yoshida</a> The highly radiopure NaI(Tl) was developed to search for particle candidates of dark matter. The optimized methods were combined to reduceRead More →

The Parallax of Omega Centauri Measured from Gaia EDR3 and a Direct, Geometric Calibration of the Tip of the Red Giant Branch and the Hubble Constant. (arXiv:2012.09196v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Soltis_J/0/1/0/all/0/1">John Soltis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Casertano_S/0/1/0/all/0/1">Stefano Casertano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riess_A/0/1/0/all/0/1">Adam G. Riess</a> We use data from the ESA Gaia mission Early Data Release 3 (EDR3) to measure the trigonometric parallax of $omega$ Cen, the first high precision parallax measurement for the most massive globular cluster in the Milky Way. We use a combination of positional and high quality proper motion data from EDR3 to identify over 100,000 cluster members, of which 67,000 are in the magnitude and colorRead More →

Shape noise and dispersion in precision weak lensing. (arXiv:2012.09175v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Gurri_P/0/1/0/all/0/1">Pol Gurri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taylor_E/0/1/0/all/0/1">Edward N. Taylor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fluke_C/0/1/0/all/0/1">Christopher J. Fluke</a> We analyse the first measurements from precision weak lensing (PWL): a new methodology for measuring individual galaxy-galaxy weak lensing through velocity information. Our goal is to understand the observed shear distribution from PWL, which is broader than can be explained by the statistical measurement errors. We identify two possible sources of scatter to explain the observed distribution: a shape noise term associated with the underlying assumption of circular stable rotation, and an astrophysical signal consistent with a log-normal dispersion around the stellar-to-halo massRead More →

A giant central red disk galaxy at redshift $z=0.76$: challenge to theories of galaxy formation. (arXiv:2012.08798v4 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_K/0/1/0/all/0/1">Kun Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_C/0/1/0/all/0/1">Chengze Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jing_Y/0/1/0/all/0/1">Yipeng Jing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sawicki_M/0/1/0/all/0/1">Marcin Sawicki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gwyn_S/0/1/0/all/0/1">Stephen Gwyn</a> We report a giant red central disk galaxy in the XMM-LSS north region. The region is covered with a rich variety of multiband photometric and spectroscopic observations. Using the photometric data of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) and spectroscopic observation of the Baryon Oscillation Spectroscopic Survey (BOSS), we find that the galaxy has a stellar mass of $sim 10^{11.6}$ times of the solar mass $M_odot$. The galaxy has a red colorRead More →

Ultra-fast model emulation with PRISM; analyzing the Meraxes galaxy formation model. (arXiv:2011.14530v2 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Velden_E/0/1/0/all/0/1">Ellert van der Velden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duffy_A/0/1/0/all/0/1">Alan R. Duffy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Croton_D/0/1/0/all/0/1">Darren Croton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mutch_S/0/1/0/all/0/1">Simon J. Mutch</a> We demonstrate the potential of an emulator-based approach to analyzing galaxy formation models in the domain where constraining data is limited. We have applied the open-source Python package PRISM to the galaxy formation model Meraxes. Meraxes is a semi-analytic model, purposefully built to study the growth of galaxies during the Epoch of Reionization (EoR). Constraining such models is however complicated by the scarcity of observational data in the EoR. PRISM’s ability to rapidly construct accurateRead More →

Identifying Black Hole Central Engines in Gamma-Ray Bursts. (arXiv:2008.07544v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Sharma_V/0/1/0/all/0/1">Vidushi Sharma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iyyani_S/0/1/0/all/0/1">Shabnam Iyyani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhattacharya_D/0/1/0/all/0/1">Dipankar Bhattacharya</a> The nature of the gamma-ray burst (GRB) central engine still remains an enigma. Entities widely believed to be capable of powering the extreme jets are magnetars and black holes. The maximum rotational energy that is available in a millisecond magnetar to form a jet is ~10^52 erg. We identify 8 long GRBs whose jet opening angle corrected energetics of the prompt emission episode are >10^52 erg with high confidence level and therefore, their central engines are expected to be black holes. Majority of these GRBsRead More →

The Accretion Geometry of the Asynchronous Polar V1432 Aql. (arXiv:2011.13088v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_Q/0/1/0/all/0/1">Qishan Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Qian_S/0/1/0/all/0/1">Shengbang Qian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_L/0/1/0/all/0/1">Liying Zhu</a> As the only eclipsing asynchronous polar (AP), V1432 Aql provides an excellent laboratory to study the interaction between the accreted matter and the magnetic field. However, due to its complex emission, a more physical understanding of its accretion geometry is still outstanding. Here, we report an X-ray spectral study using contemporaneous observations from nustar and swift. We detect significant Compton reflection and confirm earlier reports of a high soft X-ray temperature $sim52$ keV. We suggest that the multi-temperature emission is due to a distributionRead More →

$R$-mode Stability of GW190814’s Secondary Component as a Supermassive and Superfast Pulsar. (arXiv:2011.11934v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhou_X/0/1/0/all/0/1">Xia Zhou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_A/0/1/0/all/0/1">Ang Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_B/0/1/0/all/0/1">Bao-An Li</a> The nature of GW190814’s secondary component $m_2$ of mass $(2.50-2.67),text{M}_{odot}$ in the mass gap between the currently known maximum mass of neutron stars and the minimum mass of black holes is currently under hot debate. Among the many possibilities proposed in the literature, the $m_2$ was suggested as a superfast pulsar while its r-mode stability against the run-away gravitational radiation through the Chandrasekhar-Friedman-Schutz mechanism is still unknown. Using those fulfilling all currently known astrophysical and nuclear physics constraints among a sampleRead More →

Measurements of $H_0$ and reconstruction of the dark energy properties from a model-independent joint analysis. (arXiv:2011.07140v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Bonilla_A/0/1/0/all/0/1">Alexander Bonilla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kumar_S/0/1/0/all/0/1">Suresh Kumar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nunes_R/0/1/0/all/0/1">Rafael C. Nunes</a> Gaussian processes (GP) provide an elegant and model-independent method for extracting cosmological information from the observational data. In this work, we employ GP to perform a joint analysis by using the geometrical cosmological probes such as Supernova Type Ia (SN), Cosmic chronometers (CC), Baryon Acoustic Oscillations (BAO), and the H0LiCOW lenses sample to constrain the Hubble constant $H_0$, and reconstruct some properties of dark energy (DE), viz., the equation of state parameter $w$, the sound speed ofRead More →

Constraining dark energy using the cross correlations of weak lensing with post-reionization probes of neutral hydrogen. (arXiv:2010.05816v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Dash_C/0/1/0/all/0/1">Chandrachud B. V. Dash</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sarkar_T/0/1/0/all/0/1">Tapomoy Guha Sarkar</a> We investigate the prospects of detecting the cross correlation of CMBR weak-lensing convergence field with the large scale tracers of the underlying dark matter distribution in the post-reionization epoch. The cross-correlation is then used to make error projections for dark energy equation of state (EoS)for models with a time evolving dark energy. We study the cross-correlation angular power spectrum of the weak-lensing field with the Lyman-$alpha$ forest and the redshifted HI 21 cm signal from the postRead More →

FANTASY: User-Friendly Symplectic Geodesic Integrator for Arbitrary Metrics with Automatic Differentiation. (arXiv:2010.02237v4 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Christian_P/0/1/0/all/0/1">Pierre Christian</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Chan_C/0/1/0/all/0/1">Chi-kwan Chan</a> We present FANTASY (Finally A Numerical Trajectory Algorithm both Straightforward and sYmplectic), a user-friendly, open-source symplectic geodesic integrator written in Python. FANTASY is designed to work “out-of-the-box” and does not require anything from the user aside from the metric and the initial conditions for the geodesics. FANTASY efficiently computes derivatives up to machine precision using automatic differentiation, allowing the integration of geodesics in arbitrary space(times) without the need for the user to manually input Christoffel symbols or any other metric derivatives. Further, FANTASY utilizes aRead More →

Density profile evolution during prestellar core collapse: Collapse starts at the large scale. (arXiv:2009.14151v3 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Gomez_G/0/1/0/all/0/1">Gilberto C. G&#xf3;mez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vazquez_Semadeni_E/0/1/0/all/0/1">Enrique V&#xe1;zquez-Semadeni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Palau_A/0/1/0/all/0/1">Aina Palau</a> We study the gravitationally-dominated, accretion-driven evolution of a prestellar core. In our model, as the core’s density increases, it remains immersed in a constant-density environment and so it accretes from this environment, increasing its mass and reducing its Jeans length. Assuming a power-law density profile $rho propto r^{-p}$, we compute the rate of change of the slope $p$, and show that the value $p=2$ is stationary, and furthermore, an attractor. The radial profile of the Jeans length scales asRead More →

Bounds on neutrino-scalar nonstandard interactions from big bang nucleosynthesis. (arXiv:2009.08104v2 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Venzor_J/0/1/0/all/0/1">Jorge Venzor</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Perez_Lorenzana_A/0/1/0/all/0/1">Abdel P&#xe9;rez-Lorenzana</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+De_Santiago_J/0/1/0/all/0/1">Josue De-Santiago</a> Coherent forward scattering processes by neutrino-scalar nonstandard interactions (SNSI) induce an effective neutrino mass. In the Early Universe, a large neutrino effective mass restricts the production of neutrinos. The SNSI effect is modulated by two effective couplings, these account for the coupling between neutrinos and electrons/positrons, $G_{rm eff}$, and the neutrino self-interaction, $G_{rm S}$. These parameters are directly related to the effective number of relativistic species and non-zero values imply a smaller than expected $N_{rm eff}$. We employ big bang nucleosynthesis to constraint theRead More →

Hybrid stars with sequential phase transitions: the emergence of the g$_2$ mode. (arXiv:2009.03769v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_M/0/1/0/all/0/1">M. C. Rodriguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ranea_Sandoval_I/0/1/0/all/0/1">I. F. Ranea-Sandoval</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mariani_M/0/1/0/all/0/1">M. Mariani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Orsaria_M/0/1/0/all/0/1">M. G. Orsaria</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malfatti_G/0/1/0/all/0/1">G. Malfatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guilera_O/0/1/0/all/0/1">O. M. Guilera</a> Neutron stars are the densest objects in the Universe, with $M sim 1.4 M_{odot}$ and $R sim 12$ km, and the equation of state associated to their internal composition is still unknown. The extreme conditions to which matter is subjected inside neutron stars could lead to a phase transition in their inner cores, giving rise to a hybrid compact object. The observation of $2M_{odot}$ binary pulsars (PSR~J1614-2230, PSR~J0343$+$0432Read More →

CosmoBit: A GAMBIT module for computing cosmological observables and likelihoods. (arXiv:2009.03286v3 [astro-ph.CO] UPDATED) The <a href="http://arxiv.org/find/astro-ph/1/au:+Workgroup_G/0/1/0/all/0/1">GAMBIT Cosmology Workgroup</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Renk_J/0/1/0/all/0/1">Janina J. Renk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stocker_P/0/1/0/all/0/1">Patrick St&#xf6;cker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bloor_S/0/1/0/all/0/1">Sanjay Bloor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hotinli_S/0/1/0/all/0/1">Selim Hotinli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Balazs_C/0/1/0/all/0/1">Csaba Bal&#xe1;zs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bringmann_T/0/1/0/all/0/1">Torsten Bringmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalo_T/0/1/0/all/0/1">Tom&#xe1;s E. Gonzalo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Handley_W/0/1/0/all/0/1">Will Handley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoof_S/0/1/0/all/0/1">Sebastian Hoof</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Howlett_C/0/1/0/all/0/1">Cullan Howlett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kahlhoefer_F/0/1/0/all/0/1">Felix Kahlhoefer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scott_P/0/1/0/all/0/1">Pat Scott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vincent_A/0/1/0/all/0/1">Aaron C. Vincent</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+White_M/0/1/0/all/0/1">Martin White</a> We introduce $sf{CosmoBit}$, a module within the open-source $sf{GAMBIT}$ software framework for exploring connections between cosmology and particle physics with joint global fits. $sf{CosmoBit}$ provides a flexible framework for studying various scenarios beyond $Lambda$CDM, such as models of inflation, modifications of theRead More →