RAS_WEB (Page 2,671)

Modeling the survival of Population III stars till present day. (arXiv:1712.06912v4 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Dutta_J/0/1/0/all/0/1">Jayanta Dutta</a> (IISER Mohali, India), <a href="http://arxiv.org/find/astro-ph/1/au:+Sur_S/0/1/0/all/0/1">Sharanya Sur</a> (IIA, Bengaluru, India), <a href="http://arxiv.org/find/astro-ph/1/au:+Stacy_A/0/1/0/all/0/1">Athena Stacy</a> (UC Berkeley, USA), <a href="http://arxiv.org/find/astro-ph/1/au:+Bagla_J/0/1/0/all/0/1">Jasjeet Singh Bagla</a> (IISER Mohali, India) Recent numerical simulations have suggested the probability of a fraction of the primordial stars being ejected from the cluster of their origin. We explore the possibility that some of these can remain on the main sequence until the present epoch. We develop a semianalytical model guided by results of cosmological simulations to study the mass accretion by these protostars as a function of the original stellar massRead More →

Strengthening the bound on the mass of the lightest neutrino with terrestrial and cosmological experiments. (arXiv:2009.03287v1 [astro-ph.CO]) 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:+Stocker_P/0/1/0/all/0/1">Patrick St&#xf6;cker</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:+Bloor_S/0/1/0/all/0/1">Sanjay Bloor</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:+Hotinli_S/0/1/0/all/0/1">Selim Hotinli</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:+Renk_J/0/1/0/all/0/1">Janina J. Renk</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 determine the upper limit on the mass of the lightest neutrino from the most robust recent cosmological and terrestrial data. Marginalising over possible effective relativistic degrees of freedom at early times ($N_mathrm{eff}$) and assuming normal mass ordering, the mass ofRead More →

CosmoBit: A GAMBIT module for computing cosmological observables and likelihoods. (arXiv:2009.03286v1 [astro-ph.CO]) 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 the effectiveRead More →

A SETI Survey of the Vela Region using the Murchison Widefield Array: Orders of Magnitude Expansion in Search Space. (arXiv:2009.03267v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Tremblay_C/0/1/0/all/0/1">Chenoa D. Tremblay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tingay_S/0/1/0/all/0/1">Steven J. Tingay</a> Following the results of our previous low frequency searches for extraterrestrial intelligence (SETI) using the Murchison Widefield Array (MWA), directed toward the Galactic Centre and the Orion Molecular Cloud (Galactic Anticentre), we report a new large-scale survey toward the Vela region with the lowest upper limits thus far obtained with the MWA. Using the MWA in the frequency range 98-128 MHz over a 17 hour period, a $sim$400 deg$^2$ field centred on the Vela Supernova RemnantRead More →

Obtaining non-linear galaxy bias constraints from galaxy-lensing phase differences. (arXiv:2009.03256v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Manera_M/0/1/0/all/0/1">Marc Manera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bacon_D/0/1/0/all/0/1">David Bacon</a> We demonstrate the utility and constraining power of a new statistic for investigating galaxy bias: the galaxy-lensing phase difference. The statistic consists in taking the differences of the phases of the harmonic wave-modes between the weak lensing convergence field and the galaxy count field. We use dark matter simulations populated with galaxies up to redshift $z=1$ to test the performance of this estimator. We find that phase differences are sensitive to the absolute value of the second order bias ($c_2=b_2/b_1$), and demonstrate why this is the case. ForRead More →

Advances in Understanding High-Mass X-ray Binaries with INTEGRAL and Future Directions. (arXiv:2009.03244v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kretschmar_P/0/1/0/all/0/1">Peter Kretschmar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Furst_F/0/1/0/all/0/1">Felix F&#xfc;rst</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sidoli_L/0/1/0/all/0/1">Lara Sidoli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bozzo_E/0/1/0/all/0/1">Enrico Bozzo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alfonso_Garzon_J/0/1/0/all/0/1">Julia Alfonso-Garz&#xf3;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bodaghee_A/0/1/0/all/0/1">Arash Bodaghee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chaty_S/0/1/0/all/0/1">Sylvain Chaty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chernyakova_M/0/1/0/all/0/1">Masha Chernyakova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferrigno_C/0/1/0/all/0/1">Carlo Ferrigno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Manousakis_A/0/1/0/all/0/1">Antonios Manousakis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Negueruela_I/0/1/0/all/0/1">Ignacio Negueruela</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Postnov_K/0/1/0/all/0/1">Konstantin Postnov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paizis_A/0/1/0/all/0/1">Adamantia Paizis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reig_P/0/1/0/all/0/1">Pablo Reig</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodes_Roca_J/0/1/0/all/0/1">Jos&#xe9; Joaqu&#xed;n Rodes-Roca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tsygankov_S/0/1/0/all/0/1">Sergey Tsygankov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bird_A/0/1/0/all/0/1">Antony J. Bird</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuhnel_M/0/1/0/all/0/1">Matthias Bissinger n&#xe9; K&#xfc;hnel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blay_P/0/1/0/all/0/1">Pere Blay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caballero_I/0/1/0/all/0/1">Isabel Caballero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coe_M/0/1/0/all/0/1">Malcolm J. Coe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Domingo_A/0/1/0/all/0/1">Albert Domingo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doroshenko_V/0/1/0/all/0/1">Victor Doroshenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ducci_L/0/1/0/all/0/1">Lorenzo Ducci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Falanga_M/0/1/0/all/0/1">Maurizio Falanga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grebenev_S/0/1/0/all/0/1">Sergei A. Grebenev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grinberg_V/0/1/0/all/0/1">Victoria Grinberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hemphill_P/0/1/0/all/0/1">Paul Hemphill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kreykenbohm_I/0/1/0/all/0/1">IngoRead More →

Interstellar nitrile anions: Detection of C3N- and C5N- in TMC-1. (arXiv:2009.03240v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Cernicharo_J/0/1/0/all/0/1">J. Cernicharo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marcelino_N/0/1/0/all/0/1">N. Marcelino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pardo_J/0/1/0/all/0/1">J. R. Pardo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agundez_M/0/1/0/all/0/1">M. Agundez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tercero_B/0/1/0/all/0/1">B. Tercero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vicente_P/0/1/0/all/0/1">P. de Vicente</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cabezas_C/0/1/0/all/0/1">C. Cabezas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bermudez_C/0/1/0/all/0/1">C. Bermudez</a> We report on the first detection of C3N- and C5N- towards the cold dark core TMC-1 in the Taurus region, using the Yebes 40 m telescope. The observed C3N/C3N- and C5N/C5N- abundance ratios are 140 and 2, respectively; that is similar to those found in the circumstellar envelope of the carbon-rich star IRC+10216. Although the formation mechanisms for the neutrals are different in interstellar (ion-neutral reactions) andRead More →

INTEGRAL view of AGN. (arXiv:2009.03232v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Malizia_A/0/1/0/all/0/1">Angela Malizia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sazonov_S/0/1/0/all/0/1">Sergey Sazonov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bassani_L/0/1/0/all/0/1">Loredana Bassani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pian_E/0/1/0/all/0/1">Elena Pian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beckmann_V/0/1/0/all/0/1">Volker Beckmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Molina_M/0/1/0/all/0/1">Manuela Molina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mereminskiy_I/0/1/0/all/0/1">Ilya Mereminskiy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Belanger_G/0/1/0/all/0/1">Guillaume Belanger</a> AGN are among the most energetic phenomena in the Universe and in the last two decades INTEGRAL’s contribution in their study has had a significant impact. Thanks to the INTEGRAL extragalactic sky surveys, all classes of soft X-ray detected (in the 2-10 keV band) AGN have been observed at higher energies as well. Up to now, around 450 AGN have been catalogued and a conspicuous part of them are either objects observed at high-energies forRead More →

Active deep learning method for the discovery of objects of interest in large spectroscopic surveys. (arXiv:2009.03219v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Skoda_P/0/1/0/all/0/1">Petr &#x160;koda</a> (1 and 2), <a href="http://arxiv.org/find/astro-ph/1/au:+Podsztavek_O/0/1/0/all/0/1">Ond&#x159;ej Podsztavek</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Tvrdik_P/0/1/0/all/0/1">Pavel Tvrd&#xed;k</a> (2) ((1) Astronomical Institute of the Czech Academy of Sciences, (2) Faculty of Information Technology of the Czech Technical University in Prague) Current archives of the LAMOST telescope contain millions of pipeline-processed spectra that have probably never been seen by human eyes. Most of the rare objects with interesting physical properties, however, can only be identified by visual analysis of their characteristic spectral features. A proper combination of interactive visualisation with modern machine learning techniquesRead More →

Primordial black holes from narrow peaks and the skew-lognormal distribution. (arXiv:2009.03204v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Gow_A/0/1/0/all/0/1">Andrew D. Gow</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Byrnes_C/0/1/0/all/0/1">Christian T. Byrnes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hall_A/0/1/0/all/0/1">Alex Hall</a> We examine the shape of the primordial black hole mass distribution arising from a peak in the primordial power spectrum. We show that, for sufficiently narrow peaks, the true mass distribution deviates significantly from lognormal, the most commonly assumed form of the mass distribution. The lognormal approximation is outperformed by a number of similar distributions which can generate negative skewness in log-mass. We highlight the skew-lognormal as the best of these possible modifications and suggest it be used instead of the lognormalRead More →

Characteristic mass in galaxy quenching: environmental versus internal effects. (arXiv:2003.09776v4 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Li_P/0/1/0/all/0/1">Pengfei Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_H/0/1/0/all/0/1">Huiyuan Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mo_H/0/1/0/all/0/1">H.J. Mo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_E/0/1/0/all/0/1">Enci Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hong_H/0/1/0/all/0/1">Hui Hong</a> A clear transition feature of galaxy quenching is identified in the multi-parameter space of stellar mass ($M_*$), bulge to total mass ratio ($B/T_{rm m}$), halo mass ($M_{rm h}$) and halo-centric distance ($r/r_{180}$). For given halo mass, the characteristic stellar mass ($M_{*, rm ch}$) for the transition is about one-fifth of that of the corresponding central galaxy, and almost independent of $B/T_{rm m}$. Once $B/T_{rm m}$ is fixed, the quenched fraction of galaxies with $M_*<M_{*, rm ch}$ increases withRead More →

Giants eating giants: Mass loss and giant planets modifying the luminosity of the Tip of the Giant Branch. (arXiv:2003.11499v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Jimenez_R/0/1/0/all/0/1">Raul Jimenez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jorgensen_U/0/1/0/all/0/1">Uffe Grae Jorgensen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Verde_L/0/1/0/all/0/1">Licia Verde</a> During the red giant phase, stars loose mass at the highest rate since birth. The mass-loss rate is not fixed, but varies from star-to-star by up to 5%, resulting in variations of the star’s luminosity at the tip of the red giant branch (TRGB). Also, most stars, during this phase, engulf part of their planetary system, including their gas giant planets and possibly brown dwarfs. Gas giant planet masses range between 0.1 to 2%Read More →

Luminous Blue Variables. (arXiv:2009.03144v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Weis_K/0/1/0/all/0/1">Kerstin Weis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bomans_D/0/1/0/all/0/1">Dominik J. Bomans</a> Luminous Blue Variables are massive evolved stars, here we introduce this outstanding class of objects. Described are the specific characteristics, the evolutionary state and what they are connected to other phases and types of massive stars. Our current knowledge of LBVs is limited by the fact that in comparison to other stellar classes and phases only a few “true” LBVs are known. This results from the lack of a unique, fast and always reliable identification scheme for LBVs. It literally takes time to get a true classification of a LBV. In addition theRead More →

Mapping Poincar'{e} gauge cosmology to Horndeski theory for emergent dark energy. (arXiv:2006.03581v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Barker_W/0/1/0/all/0/1">W. E. V. Barker</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Lasenby_A/0/1/0/all/0/1">A. N. Lasenby</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Hobson_M/0/1/0/all/0/1">M. P. Hobson</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Handley_W/0/1/0/all/0/1">W. J. Handley</a> The ten-parameter, quadratic Poincar’e gauge theory of gravity is a plausible alternative to general relativity. We show that the rich background cosmology of the gauge theory is described by a non-canonical bi-scalar-tensor theory in the Jordan frame: the `metrical analogue’. This provides a unified framework for future investigation by the broader community. For many parameter choices, the non-canonical term reduces to a Cuscuton field of the form $smash{sqrt{|X^{phiphi}|}}$. The Einstein-Cartan-Kibble-Sciama theory maps to aRead More →

Clusters of Solar Eclipses in the Maori Era. (arXiv:2009.01663v2 [physics.hist-ph] UPDATED) <a href="http://arxiv.org/find/physics/1/au:+Khalisi_E/0/1/0/all/0/1">Emil Khalisi</a> A dozen of high-magnitude solar eclipses accumulated near New Zealand in the 15th century AD when the Maori inhabited the two main islands. Taking today’s capital Wellington as the point of reference, we counted ten events with magnitude larger than 0.9 between 1409 and 1516 AD and two more just below this value. The eclipses need not have been all observed on account of weather conditions. An allusion to a particular event that could be conveyed in a myth is discussed, but the dating turns out far from certain. We takeRead More →

NIHAO XXVI: Nature versus nurture, the Star Formation Main Sequence and the origin of its scatter. (arXiv:2008.13379v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Blank_M/0/1/0/all/0/1">Marvin Blank</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meier_L/0/1/0/all/0/1">Liam E. Meier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maccio_A/0/1/0/all/0/1">Andrea V. Macci&#xf2;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dutton_A/0/1/0/all/0/1">Aaron A. Dutton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dixon_K/0/1/0/all/0/1">Keri L. Dixon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soliman_N/0/1/0/all/0/1">Nadine H. Soliman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kang_X/0/1/0/all/0/1">Xi Kang</a> We investigate how the NIHAO galaxies match the observed star formation main sequence (SFMS) and what the origin of its scatter is. The NIHAO galaxies reproduce the SFMS and generally agree with observations, but the slope is about unity and thus significantly larger than observed values. This is because observed galaxies at large stellar masses, although still being part ofRead More →

The abundance of primordial black holes from the global 21cm signal and extragalactic gamma-ray background. (arXiv:2008.11859v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_Y/0/1/0/all/0/1">Yupeng Yang</a> Primordial black holes (PBHs) formed in the early Universe can accret dark matter particles due to gravity and form ultracompact minihalos (UCMHs). The theoretical researches and simulations have shown that the density profile of dark matter in UCMHs is in the form of $rho (r) sim r^{-2.25}$. Compared with the popular dark matter halo model, e.g. NFW model, dark matter annihilation rate is larger in UCMHs. Considering dark matter annihilation, there is a maximum core density $rho_{rm max}$ in UCMHs which has been treatedRead More →

Cannibalism hinders growth: Cannibal Dark Matter and the $S_8$ tension. (arXiv:2008.08486v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Heimersheim_S/0/1/0/all/0/1">Stefan Heimersheim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schoneberg_N/0/1/0/all/0/1">Nils Sch&#xf6;neberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hooper_D/0/1/0/all/0/1">Deanna C. Hooper</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lesgourgues_J/0/1/0/all/0/1">Julien Lesgourgues</a> Many models of dark matter have been proposed in attempt to ease the $S_8$ tension between weak lensing and CMB experiments. One such exciting possibility is cannibalistic dark matter (CanDM), which has exothermal number-changing interactions allowing it to stay warm far into its non-relativistic regime. Here we investigate the cosmological implications of CanDM and how it impacts CMB anisotropies and the matter power spectrum, by implementing the model within a linear Einstein-Boltzmann solver. We show that CanDM suppresses theRead More →

Monitoring of transiting exoplanets and their host stars with small aperture telescopes. (arXiv:2008.08379v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Salisbury_M/0/1/0/all/0/1">M.A.Salisbury</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kolb_U/0/1/0/all/0/1">U.C.Kolb</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Norton_A/0/1/0/all/0/1">A.J.Norton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haswell_C/0/1/0/all/0/1">C.A.Haswell</a> Exoplanet research is now target rich with a wide diversity of systems making it difficult for high demand observatories to undertake follow up observations over extended periods of time. We investigate the effectiveness of using 0.4m-class telescopes for monitoring transiting hot Jupiters and their host stars. We consider two representative case studies: WASP-52b with 13 new transits, and HAT-P-23b with 17 new transits and concurrent photometric monitoring covering 78 days. We present updated system parameters and combine our new transit times withRead More →

BVRI Photometric Observations, Light Curve Solutions and Orbital Period Analysis of BF Pav. (arXiv:2008.05068v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Poro_A/0/1/0/all/0/1">Atila Poro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blackford_M/0/1/0/all/0/1">Mark G. Blackford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alicavus_F/0/1/0/all/0/1">Fahri Alicavus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davoudi_F/0/1/0/all/0/1">Fatemeh Davoudi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+MirshafieKhozani_P/0/1/0/all/0/1">PegahSadat MirshafieKhozani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fernandez_Lajus_E/0/1/0/all/0/1">Eduardo Fern&#xe1;ndez-Laj&#xfa;s</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rahimi_J/0/1/0/all/0/1">Jabar Rahimi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jalalabadi_B/0/1/0/all/0/1">Behjat Zarei Jalalabadi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Farahani_F/0/1/0/all/0/1">Farzaneh Ahangarani Farahani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Budding_E/0/1/0/all/0/1">Edwin Budding</a> The new ephemeris and light curve analysis by synthesizing our mid-eclipse times and the former observations of BF Pav, that is classified as a W UMa-type eclipsing binary, are presented in this study. We also obtain this binary system’s period changes using the Wilson-Devinney code after eight nights of observation in BVRI filters from two observatoriesRead More →