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New submissions for Tue, 4 Feb 20

[1]  arXiv:2002.00012 [pdf, other]

Title: The Birth of a Massive First-Star Binary

Authors: Kazuyuki Sugimura, Tomoaki Matsumoto, Takashi Hosokawa, Shingo Hirano, Kazuyuki Omukai

Comments: 6 pages, 3 figures, submitted to ApJ Letters

Subjects: Astrophysics of Galaxies (astro-ph.GA); High Energy Astrophysical Phenomena (astro-ph.HE); Solar and Stellar Astrophysics (astro-ph.SR)

We study the formation of massive Pop III binary stars using a newly developed radiation hydrodynamics code with the adaptive mesh refinement and adaptive ray-tracing methods. We follow the evolution of a typical primordial star-forming cloud obtained from a cosmological hydrodynamics simulation. Several protostars form as a result of disk fragmentation and grow in mass by the gas accretion, which is finally quenched by the radiation feedback from the protostars. Our code enables us, for the first time, to consider the feedback by both the ionizing and dissociating radiation from the multiple protostars, which is essential for self-consistently determining their final masses. At the final step of the simulation, we observe a very wide ($\gtrsim 10^4\,\mathrm{au}$) binary stellar system consisting of $60$ and $70\,M_\odot$ stars. One of the member stars also has two smaller mass ($10\,M_\odot$) companion stars orbiting at $200$ and $800\,\mathrm{au}$, making up a mini-triplet system. Our results suggest that massive binary or multiple systems are common among Pop III stars.

[2]  arXiv:2002.00014 [pdf, other]

Title: Close Binary Companions to APOGEE DR16 Stars: 20,000 Binary-star Systems Across the Color-Magnitude Diagram

Authors: Adrian M. Price-Whelan, David W. Hogg, Hans-Walter Rix, Rachael L. Beaton, Hannah Lewis, David L. Nidever, Rodolfo Barba, Joleen K. Carlberg, Nathan De Lee, José G. Fernández-Trincado, Peter M. Frinchaboy, D. A. García-Hernández, Paul J. Green, Sten Hasselquist, Penélope Longa-Peña, Steven R. Majewski, Christian Nitschelm, Jennifer Sobeck, Keivan G. Stassun, Nicholas W. Troup

Comments: 35 pages, 12 figures, but check out Figure 5. Data tables available at this http URL Submitted to AAS journals

Subjects: Solar and Stellar Astrophysics (astro-ph.SR); Astrophysics of Galaxies (astro-ph.GA)

Many problems in contemporary astrophysics---from understanding the formation of black holes to untangling the chemical evolution of galaxies---rely on knowledge about binary stars. This, in turn, depends on discovery and characterization of binary companions for large numbers of different kinds of stars in different chemical and dynamical environments. Current stellar spectroscopic surveys observe hundreds of thousands to millions of stars with (typically) few observational epochs, which allows binary discovery but makes orbital characterization challenging. We use a custom Monte Carlo sampler (The Joker) to perform discovery and characterization of binary systems through radial-velocities, in the regime of sparse, noisy, and poorly sampled multi-epoch data. We use it to generate posterior samplings in Keplerian parameters for 232,531 sources released in APOGEE Data Release 16. Our final catalog contains 19,635 high-confidence close-binary (P < few years, a < few AU) systems that show interesting relationships between binary occurrence rate and location in the color-magnitude diagram. We find notable faint companions at high masses (black-hole candidates), at low masses (substellar candidates), and at very close separations (mass-transfer candidates). We also use the posterior samplings in a (toy) hierarchical inference to measure the long-period binary-star eccentricity distribution. We release the full set of posterior samplings for the entire parent sample of 232,531 stars. This set of samplings involves no heuristic "discovery" threshold and therefore can be used for myriad statistical purposes, including hierarchical inferences about binary-star populations and sub-threshold searches.

[3]  arXiv:2002.00015 [pdf, other]

Title: More accurate simulations with separate initial conditions for baryons and dark matter

Authors: Simeon Bird, Yu Feng, Christian Pedersen, Andreu Font-Ribera

Comments: 16 pages, 5 figures

Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO)

We revisit techniques for performing cosmological simulations with both baryons and cold dark matter when each fluid has different initial conditions, as is the case at the end of the radiation era. Most simulations do not reproduce the linear prediction for the difference between the cold dark matter and baryon perturbations. We show that this is due to the common use of offset regular grids when setting up the particle initial conditions. The correct behaviour can be obtained without any loss of simulation resolution by using a Lagrangian glass for the baryon particles. We further show that the difference between cold dark matter and baryons may affect predictions for the Lyman-alpha forest flux power spectrum at the 5% level, potentially impacting current cosmological constraints.

[4]  arXiv:2002.00046 [pdf, ps, other]

Title: Black hole, neutron star and white dwarf merger rates in AGN disks

Authors: B.McKernan, K.E.S. Ford, R. O'Shaughnessy

Comments: 6 pages, 4 figures, MNRAS (submitted)

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Astrophysics of Galaxies (astro-ph.GA)

Advanced LIGO \& Advanced Virgo are detecting a large number of binary stellar origin black hole (BH) mergers. A promising channel for accelerated BH merger lies in active galactic nucleus (AGN) disks of gas around super-masssive black holes. Here we investigate the relative number of compact object mergers in AGN disk models, including BH, neutron stars (NS) and white dwarfs, via Monte Carlo simulations. We find the number of all merger types in the bulk disk grows $\propto t^{1/3}$ which is driven by the Hill sphere of the more massive merger component. Median mass ratios of NS-BH mergers in AGN disks are $\tilde{q}=0.07\pm 0.06(0.14\pm 0.07)$ for mass functions (MF) $M^{-1(-2)}$. If a fraction $f_{AGN}$ of the observed rate of BH-BH mergers (${\cal}{R}_{BH-BH}$) come from AGN, we expect a rate of NS-BH (NS-NS) mergers from the AGN channel of ${\cal}{R}_{BH-NS} \sim f_{AGN}[10,300]\rm{Gpc}^{-3} \rm{yr}^{-1}$,(${\cal}{R}_{NS-NS} \leq f_{AGN}400\rm{Gpc}^{-3} \rm{yr}^{-1}$). Allowing for the ratio of NS-NS/BH-BH LIGO search volumes, from preliminary O3 results we can rule out the AGN channel as a dominant contribution to observed NS-NS mergers. The number of lower mass gap events in this channel is a strong function of the nuclear MF and mass segregation efficiency. Compact object merger ratios derived from LIGO can restrict models of MF, mass segregation and populations embedded in AGN disks. The expected number of EM counterparts to NS-BH mergers in AGN disks at $z<1$ is $\sim [30,900]{\rm{yr}}^{-1}(f_{AGN}/0.1)$. EM searches for flaring due to embedded events in large AGN surveys will complement LIGO constraints on AGN models and the embedded populations that must live in them.

[5]  arXiv:2002.00064 [pdf, ps, other]

Title: The ELM Survey. VIII. 98 Double White Dwarf Binaries

Authors: Warren R. Brown, Mukremin Kilic, Alekzander Kosakowski, Jeff J. Andrews, Craig O. Heinke, Marcel A. Agueros, Fernando Camilo, A. Gianninas, J.J. Hermes, Scott J. Kenyon

Comments: 22 pages, ApJ accepted

Subjects: Solar and Stellar Astrophysics (astro-ph.SR)

We present the final sample of 98 detached double white dwarf (WD) binaries found in the Extremely Low Mass (ELM) Survey, a spectroscopic survey targeting <0.3 Msun He-core WDs completed in the Sloan Digital Sky Survey footprint. Over the course of the survey we observed ancillary low mass WD candidates like GD278, which we show is a P=0.19 d double WD binary, as well as candidates that turn out to be field blue straggler/subdwarf A-type stars with luminosities too large to be WDs given their Gaia parallaxes. Here, we define a clean sample of ELM WDs that is complete within our target selection and magnitude range 15<g_0<20 mag. The measurements are consistent with 100% of ELM WDs being 0.0089 < P < 1.5 d double WD binaries, 35% of which belong to the Galactic halo. We infer these are mostly He+CO WD binaries given the measurement constraints. The merger rate of the observed He+CO WD binaries exceeds the formation rate of stable mass transfer AM CVn binaries by a factor of 25, and so the majority of He+CO WD binaries must experience unstable mass transfer and merge. The shortest-period systems like J0651+2844 are signature {\it LISA} verification binaries that can be studied with gravitational waves and light.

[6]  arXiv:2002.00095 [pdf, ps, other]

Title: Variation of fundamental constants and white dwarfs

Authors: Susana J. Landau

Comments: 15 pages, 2 figures, Proceedings article based on invited review talk for the IAU Symposium 357, "White Dwarfs as Probes of Fundamental Physics and Tracers of Planetary, Stellar, and Galactic Evolution"

Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Physics - Phenomenology (hep-ph)

Theories that attempt to unify the four fundamental interactions and alternative theories of gravity predict time and/or spatial variation of the fundamental constants of nature. Different versions of these theories predict different behaviours for these variations. In consequence, experimental and observational bounds are an important tool to check the validity of such proposals. In this paper, we review constraints on the possible variation of the fundamental constants from astronomical observations and geophysical experiments designed to test the constancy of the fundamental constants of nature over different timescales. We also focus on the limits that can be obtained from white dwarfs, which can constrain the variation of the constants with the gravitational potential.

[7]  arXiv:2002.00106 [pdf, ps, other]

Title: Orbital dynamics of highly probable but rare Orionid outbursts possibly observed by the ancient Maya

Authors: J. H. Kinsman, D. J. Asher

Comments: Monthly Notices of the Royal Astronomical Society. Accepted 2020 January 17. Received 2020 January 3; in original form 2019 May 30. 9 pages, 4 figures

Subjects: Earth and Planetary Astrophysics (astro-ph.EP); History and Philosophy of Physics (physics.hist-ph)

Using orbital integrations of particles ejected from Comet Halley's passages between 1404 BC and 240 BC, the authors investigate possible outbursts of the Orionids (twin shower of the Eta Aquariids) that may have been observed in the western hemisphere. In an earlier orbital integration study the authors determined there was a high probability linking probable outbursts of the Eta Aquariid meteor shower with certain events recorded in inscriptions during the Maya Classic Period, AD 250-900. This prior examination was the first scientific inquiry of its kind into ancient meteor outbursts possibly recorded in the western hemisphere where previously no pre-Columbian observations had existed. In the current paper the aim is to describe orbital dynamics of rare but probable Orionid outbursts that would have occurred on or near applicable dates recorded in the Classic Maya inscriptions. Specifically, significant probable outbursts are found in AD 417 and 585 out of 30 possible target years. The driving mechanisms for outbursts in those two years are Jovian 1:6 and 1:7 mean motion resonances acting to maintain compact structures within the Orionid stream for over 1 kyr. Furthermore, an Orionid outburst in AD 585 recorded by China is confirmed.

[8]  arXiv:2002.00127 [pdf, other]

Title: Probabilistic direction-dependent ionospheric calibration for LOFAR-HBA

Authors: J. G. Albert, R. J. van Weeren, H. T. Intema, H. J. A. Röttgering

Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM)

Direction dependent calibration and imaging is a vital part of producing deep, high fidelity, high-dynamic range radio images with a wide-field low-frequency array like LOFAR. Currently, state-of-the-art facet-based direction dependent calibration algorithms rely on the assumption that the isoplanatic-patch size is much larger than the separation between bright in-field calibrators. This assumption is often violated due to the dynamic nature of the ionosphere, and as a result direction dependent errors affect image quality between calibrators. In this paper we propose a probabilistic physics-informed model for inferring ionospheric phase screens, providing a calibration for all sources in the field of view. We apply our method to a randomly selected observation from the LOFAR Two-Metre Sky Survey archive, and show that almost all direction dependent effects between bright calibrators are corrected and that the root-mean-squared residuals around bright sources is reduced by 32\% on average.

[9]  arXiv:2002.00128 [pdf, other]

Title: Lens Flare: Magnified X-Ray Binaries as Passive Beacons in SETI

Authors: Brian C. Lacki

Comments: Submitted, 15 pages, 4 figures, 1 table. An animated version of Figure 3 is available at this http URL

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Popular Physics (physics.pop-ph)

Low mass X-ray binaries (LMXBs) containing neutron stars are both extremely luminous and compact, emitting up to ~10^6 L_sun within a kilometer-scale boundary layer. This combination allows for easy modulation, motivating X-ray SETI. When X-ray lenses smaller than planets (100 - 1,000 km) magnify the LMXB boundary layer, it brightens by a factor of several thousand for about a second. In addition, there should be occultation events where the neutron star is blocked out. Passive X-ray lenses could require little maintenance and the LMXB light source itself shines for millions of years, serving as an effective beacon for interstellar communication. A very large number of lenses would be needed to ensure detection from all directions, however, and gathering material to construct them could be very difficult. Avoiding collisions between lenses and aiming them pose additional challenges. Both "lens flares" and eclipses of LMXBs are easily detectable in the Galaxy, although they would be rare events, occurring once per decade. Our X-ray instruments could detect the flares to several Mpc, but it is unlikely they would be observing the LMXB during a flare.

[10]  arXiv:2002.00129 [pdf, other]

Title: Broadband characterisation of the very intense TeV flares of the blazar 1ES 1959+650 in 2016

Authors: MAGIC Collaboration: V. A. Acciari, S. Ansoldi, L. A. Antonelli, A. Arbet Engels, D. Baack, A. Babić, B. Banerjee, U. Barres de Almeida, J. A. Barrio, J. Becerra González, W. Bednarek, L. Bellizzi, E. Bernardini, A. Berti, J. Besenrieder, W. Bhattacharyya, C. Bigongiari, A. Biland, O. Blanch, G. Bonnoli, Z. Bosnjak, G. Busetto, R. Carosi, G. Ceribella, Y. Chai, S. Cikota, S. M. Colak, U. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, V. D'Elia, P. Da Vela, F. Dazzi, A. De Angelis, B. De Lotto, M. Delfino, J. Delgado, F. Di Pierro, E. Do Souto Espiñeira, D. Dominis Prester, A. Donini, D. Dorner, M. Doro, D. Elsaesser, V. Fallah Ramazani, A. Fattorini, A. Fernández-Barral, G. Ferrara, D. Fidalgo, L. Foffano, M. V. Fonseca, L. Font, C. Fruck, S. Fukami, et al. (109 additional authors not shown)

Comments: 18 pages, 9 figures, accepted to A&A

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

1ES 1959+650 is a bright TeV high-frequency-peaked BL Lac object exhibiting interesting features like "orphan" TeV flares and a broad emission in the high-energy regime, that are difficult to interpret using conventional one-zone Synchrotron Self-Compton (SSC) scenarios. We report the results from the Major Atmospheric Gamma Imaging Cherenkov (MAGIC) observations in 2016 along with the multi-wavelength data from the Fermi Large Area Telescope (LAT) and Swift instruments. MAGIC observed 1ES 1959+650 with different emission levels in the very-high-energy (VHE, E >100 GeV) gamma-ray band during 2016. In the long-term data, the X-ray spectrum becomes harder with increasing flux and a hint of a similar trend is also visible in the VHE band. An exceptionally high VHE flux reaching ~ 3 times the Crab Nebula flux was measured by MAGIC on the 13th, 14th of June and 1st July 2016 (the highest flux observed since 2002). During these flares, the high-energy peak of the spectral energy distribution (SED) lies in the VHE domain and extends up to several TeV. The spectrum in the gamma-ray (both Fermi-LAT and VHE bands) and the X-ray bands are quite hard. On 13th June and 1st July 2016, the source showed rapid variations of the VHE flux within timescales of less than an hour. A simple one-zone SSC model can describe the data during the flares requiring moderate to high values of the Doppler factors (>=30-60). Alternatively, the high-energy peak of the SED can be explained by a purely hadronic model attributed to proton-synchrotron radiation with jet power L_{jet}~10^{46} erg/s and under high values of the magnetic field strength (~100 G) and maximum proton energy (~few EeV). Mixed lepto-hadronic models require super-Eddington values of the jet power. We conclude that it is difficult to get detectable neutrino emission from the source during the extreme VHE flaring period of 2016.

[11]  arXiv:2002.00144 [pdf]

Title: Full-field modeling of heat transfer in asteroid regolith: Radiative thermal conductivity of polydisperse particulates

Authors: Andrew J. Ryan, Daniel Pino Muñoz, Marc Bernacki, Marco Delbo

Comments: Submitted to the Journal of Geophysical Research: Planets

Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Geophysics (physics.geo-ph)

Characterizing the surface material of an asteroid is important for understanding its geology and for informing mission decisions, such as the selection of a sample site. Diurnal surface temperature amplitudes are directly related to the thermal properties of the materials on the surface. We describe a numerical model for studying the thermal conductivity of particulate regolith in vacuum. Heat diffusion and surface-to-surface radiation calculations are performed using the finite element (FE) method in three-dimensional meshed geometries of randomly packed spherical particles. We validate the model for test cases where the total solid and radiative conductivity values of particulates with monodisperse particle size frequency distributions (SFDs) are determined at steady-state thermal conditions. Then, we use the model to study the bulk radiative thermal conductivity of particulates with polydisperse, cumulative power-law particle SFDs. We show that for each polydisperse particulate geometry tested, there is a corresponding monodisperse geometry with some effective particle diameter that has an identical radiative thermal conductivity. These effective diameters are found to correspond very well to the Sauter mean particle diameter, which is essentially the surface-area-weighted mean. Next, we show that the thermal conductivity of the particle material can have an important effect on the radiative component of the thermal conductivity of particulates, especially if the particle material conductivity is very low or the spheres are relatively large, owing to non-isothermality in each particle. We provide an empirical correlation to predict the effects of non-isothermality on radiative thermal conductivity in both monodisperse and polydisperse particulates.

[12]  arXiv:2002.00147 [pdf, other]

Title: On-sky SiPM Performance Measurements for Millisecond to Sub-Microsecond Optical Source Variability Studies

Authors: Albert Wai Kit Lau, Mehdi Shafiee, George F. Smoot, Bruce Grossan, Siyang Li, Zhanat Maksut

Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM)

We present initial measurement of silicon photomultiplier (SiPM) for Ultra-Fast Astronomy (UFA) which will be able to enhance detection of variability of the optical sky in the millisecond and shorter time scale. In this experiment two different SiPM models S14160-3050HS and S14520-3050VS were mounted on the 0.7 meter Nazarbayev University Transient Telescope at the Assy-Turgen Astrophysical Observatory (NUTTelA-TAO) on two consecutive nights. By coupling the 3mm$\times$3mm SiPM onto NUTTelA-TAO, we obtain 2.2716'$\times$2.2716' viewing solid-angle on one SiPM channel. As a first test we measured sky background, bright stars and artificial millisecond alternative source. we compare detected SiPM counts with Gaia satellite G band flux which showed they are in a good linear agreement. The obtained photon signal is also analysed on millisecond and microsecond time windows. According to our experiments, dark count of SiPM S14520-3050VS and S14160-3050HS are measured to be $\sim$130 and $\sim$85 kilo count per second (kcps) while sky background is $\sim$191 and 203 kcps respectively. Also intrinsic crosstalk of both detectors are measured to be 10.34$\%$ and 10.52$\%$ respectively while light sensitivity of them has a lower limit of 14.7 and 15.2 Gaia G-band magnitude under 200ms of observation per target with $5\sigma$ criterion. For transient events, we propagated the 10$\mu s$ sensitivity to be 20 photon detected or 6.1 Gaia G-band magnitude. For even shorter timescale like Sub-Microsecond, the sensitivity is limited by crosstalk to 12 photons detected. magnitude. For even shorter timescale like Sub-Microsecond, the sensitivity is limited by crosstalk to 12 photons detected.

[13]  arXiv:2002.00150 [pdf, ps, other]

Title: Local galaxies with compact cores as the possible descendants of massive compact quiescent galaxies at high redshift

Authors: Ying Gao (SDU), Lulu Fan (USTC, SDU)

Comments: 12 pages, 6 figures, accepted for publication in Research in Astronomy and Astrophysics

Subjects: Astrophysics of Galaxies (astro-ph.GA)

In order to test a possible evolutionary scenario of high-$z$ compact quiescent galaxies (cQGs) that they can survive as local compact cores embedded in local massive galaxies with different morphology classes, we explore the star formation histories of local compact cores according to their spectral analysis. We build a sample of 182 massive galaxies with compact cores (${M}_{*,{\rm core}} > 10^{10.6} {\rm M}_\odot$) at $0.02 \leq z \leq 0.06$ from SDSS DR7 spectroscopic catalogue. STARLIGHT package is used to analyze the median stacked spectra and derive the stellar ages and metallicities. Our main results show that local compact cores have the average age of about $12.1\pm0.6$ Gyr, indicating their early formation at $z > 3$, which is consistent with the formation redshifts of cQGs at $1<z<3$. Together with previous studies, our result that local compact cores have similar formation redshifts as those of high-$z$ cQGs, supports that local massive galaxies with compact cores are possible descendants of cQGs. Morphological study of local galaxies with compact cores suggests that there would be multiple possible evolutionary paths for high-$z$ cQGs: most of them ($> 80\%$) will evolve into local massive ETGs according to dry minor merger, while some of them ($\sim 15\%$) will build a substantial stellar/gas discs according to the late-time gas accretion and sustaining star formation, and finally grow up to spiral galaxies.

[14]  arXiv:2002.00173 [pdf, other]

Title: Photon-induced desorption of larger species in UV-irradiated methane (CH4) ice

Authors: H. Carrascosa, G.A. Cruz-Díaz, G. M. Muñoz Caro, E. Dartois, Y. -J. Chen

Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM)

At the low temperatures found in the interior of dense clouds and circumstellar regions, along with H$_2$O and smaller amounts of species such as CO, CO$_2$, or CH$_3$OH, the infrared features of CH$_4$ have been observed on icy dust grains. Ultraviolet (UV) photons induce different processes in ice mantles, affecting the molecular abundances detected in the gas-phase. This work aims to understand the processes that occur in a pure CH$_4$ ice mantle submitted to UV irradiation. We studied photon-induced processes for the different photoproducts arising in the ice upon UV irradiation. Experiments were carried out in ISAC, an ultra-high vacuum chamber equipped with a cryostat and an F-type UV-lamp reproducing the secondary UV-field induced by cosmic rays in dense clouds. Infrared spectroscopy and quadrupole mass spectrometry were used to monitor the solid and gas-phase, respectively, during the formation, irradiation, and warm-up of the ice. Direct photodesorption of pure CH$_4$ was not observed. UV photons form CH$_x\cdot$ and H$\cdot$ radicals, leading to photoproducts such as H$_2$, C$_2$H$_2$, C$_2$H$_6$, and C$_3$H$_8$. Evidence for the photodesorption of C$_2$H$_2$ and photochemidesorption of C$_2$H$_6$ and C$_3$H$_8$ was found, the latter species is so far the largest molecule found to photochemidesorb. $^{13}$CH$_4$ experiments were also carried out to confirm the reliability of these results.

[15]  arXiv:2002.00214 [pdf, other]

Title: ORIGIN: Blind detection of faint emission line galaxies in MUSE datacubes

Authors: David Mary, Roland Bacon, Simon Conseil, Laure Piqueras, Antony Schutz

Comments: Accepted to Astronomy & Astrophysics

Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM)

One of the major science cases of the MUSE integral field spectrograph is the detection of Lyman-alpha emitters at high redshifts. The on-going and planned deep fields observations will allow for one large sample of these sources. An efficient tool to perform blind detection of faint emitters in MUSE datacubes is a prerequisite of such an endeavor.
Several line detection algorithms exist but their performance during the deepest MUSE exposures is hard to quantify, in particular with respect to their actual false detection rate, or purity. {The aim of this work is to design and validate} an algorithm that efficiently detects faint spatial-spectral emission signatures, while allowing for a stable false detection rate over the data cube and providing in the same time an automated and reliable estimation of the purity.
Results on simulated data cubes providing ground truth show that the method reaches its aims in terms of purity and completeness. When applied to the deep 30-hour exposure MUSE datacube in the Hubble Ultra Deep Field, the algorithms allows for the confirmed detection of 133 intermediate redshifts galaxies and 248 Lyman Alpha Emitters, including 86 sources with no HST counterpart.
The algorithm fulfills its aims in terms of detection power and reliability. It is consequently implemented as a Python package whose code and documentation are available on GitHub and readthedocs.

[16]  arXiv:2002.00231 [pdf, other]

Title: Water delivery to dry protoplanets by hit-and-run collisions

Authors: C. Burger (1 and 2), T. I. Maindl (1), C. M. Schäfer (2) ((1) University of Vienna, Department of Astrophysics, Austria, (2) University of Tübingen, Institute of Astronomy and Astrophysics, Germany)

Comments: Published as IAU Symposium Proceedings

Journal-ref: Proceedings IAU Symposium No. 345, Jan 2020, pages 287-288

Subjects: Earth and Planetary Astrophysics (astro-ph.EP)

Final water inventories of newly formed terrestrial planets are shaped by their collision history. A setting where volatiles are transported from beyond the snowline to habitable-zone planets suggests collisions of very dry with water-rich bodies. By means of smooth particle hydrodynamics (SPH) simulations we study water delivery in scenarios where a dry target is hit by a water-rich projectile, focusing on hit-and-run encounters with two large surviving bodies, which probably comprise about half of all similar-sized collisions.

[17]  arXiv:2002.00299 [pdf, other]

Title: Inclination Dependence of Kilonova Light Curves from Globally Aspherical Geometries

Authors: Siva Darbha, Daniel Kasen

Comments: 16 pages, 11 figures

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

The merger of two neutron stars (NSs) or a neutron star and a black hole (BH) produces a radioactively-powered transient known as a kilonova, first observed accompanying the gravitational wave event GW170817. While kilonovae are frequently modeled in spherical symmetry, the dynamical ejecta and disk outflows can be considerably asymmetric. We use Monte Carlo radiative transfer calculations to study the light curves of kilonovae with globally axisymmetric geometries (e.g. an ellipsoid and a torus). We find that the variation in luminosity in these models is most pronounced at early times, and decreases until the light curves become isotropic in the late optically thin phase. The light curve shape and peak time are not significantly modified by the global asymmetry. We show that the projected surface area along the line of sight captures the primary geometric effects, and use this fact to provide a simple analytic estimate of the direction-dependent light curves of the aspherical ejecta. For the kilonova accompanying GW170817, accounting for asymmetry with an oblate (prolate) ellipsoid of axial ratio $2$ ($1/2$) leads to a $\sim 40 \%$ decrease (increase) in the inferred ejecta mass compared to the spherical case. The pole-to-equator orientation effects are expected to be significantly larger (a factor of $\sim 5 - 10$) for the more extreme asymmetries expected for some NS-BH mergers.

[18]  arXiv:2002.00305 [pdf, ps, other]

Title: Physical origin of GeV emission in the early phase of GRB 170405A: Clues from emission onsets with multi-wavelength observations

Authors: Makoto Arimoto, Katsuaki Asano, Yutaro Tachibana, Magnus Axelsson

Comments: 18pages, 5 figures, accepted for publication in The Astrophysical Journal

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

The origin of GeV emission from the early epoch of gamma-ray bursts (GRBs) is a widely discussed issue. The long gamma-ray burst GRB 170405A, observed by the Fermi Gamma-ray Space Telescope showed high-energy emission delayed by $\sim$20 s with respect to the X-ray emission, followed by temporally fading gamma-ray emission lasting for $\sim$1,000 s, as commonly observed in high-energy GRBs. In addition, a high-energy spectral cutoff at $\sim$50 MeV was detected in the prompt emission phase. If this feature is caused by pair-production opacity, the bulk Lorentz factor of the GRB ejecta can be estimated to be $\Gamma_{\rm bulk}$ = 170-420. Simultaneously with Fermi, GRB 170405A was observed by Swift/Burst Alert Telescope (BAT) and X-ray telescope (XRT), and a clear optical onset was detected $\sim$200 s after the burst by Swift/UltraViolet Optical Telescope (UVOT). By coupling the deceleration time to the derived bulk Lorentz factor, the deceleration time was found to correspond to the delayed onset in the optical band. While the delayed onset in the optical band is evidence that this emission had an external shock origin, the temporally extended emission in the GeV band before the optical onset is hard to reconcile with the standard synchrotron emission from the same external shock. This may imply that the common feature of GeV emission with a power-law decay does not necessarily have the same origin of the optical afterglow in all Fermi/LAT GRBs, particularly in their early epoch. Another emission mechanism to explain the GeV emission in GRB 170405A can be required such as an internal-shock or inverse Compton emission.

[19]  arXiv:2002.00335 [pdf, ps, other]

Title: Fast Radio Bursts from Interacting Binary Neutron Star Systems

Authors: Bing Zhang

Comments: ApJL, in press

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

Recent observations of repeating fast radio bursts (FRBs) suggest that some FRBs reside in an environment consistent with that of binary neutron star (BNS) mergers. The bursting rate for repeaters could be very high and the emission site is likely from a magnetosphere. We discuss a hypothesis of producing abundant repeating FRBs in BNS systems. Decades to centuries before a BNS system coalesces, the magnetospheres of the two neutron stars start to interact relentlessly. Abrupt magnetic reconnection accelerates particles, which emit coherent radio waves in bunches via curvature radiation. FRBs are detected as these bright radiation beams point towards Earth. This model predicts quasi-periodicity of the bursts at the rotation periods of the two merging neutron stars (tens of milliseconds and seconds, respectively) as well as the period of orbital motion (of the order of 100 s). The bursting activities are expected to elevate with time as the two neutron stars get closer. The repeating FRB sources should be gravitational wave (GW) sources for space-borne detectors such as LISA if the sources are close enough, and will be eventually detected by ground-based detectors when the two neutron stars coalesce.

[20]  arXiv:2002.00348 [pdf, ps, other]

Title: The Alcock Paczynski test with 21cm intensity field

Authors: Takao Endo, Hiroyuki Tashiro, Atsushi J. Nishizawa

Comments: 10 pages, 9 figures

Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO)

Feasibility of the Alcock Paczynski (AP) test by stacking voids in the 21cm line intensity field is presented. We analyze the Illstris-TNG simulation to obtain the 21cm signal map. We then randomly distribute particles depending on the 21cm intensity field to find voids by using publicly available code, VIDE. As in the galaxy clustering, the shape of the stacked void in the 21cm field is squashed along the line of sight due to the peculiar velocities in redshift-space, although it becomes spherical in real-space. The redshift-space distortion for the stacked void weakly depends on redshift and we show that the dependency can be well described by the linear prediction, with the amplitude of the offset being free parameters. We find that the AP test using the stacked voids in a 21cm intensity map is feasible and the parameter estimation on $\Omega_{\rm m}$ and $w$ is unbiased.

[21]  arXiv:2002.00380 [pdf, other]

Title: Hall-magnetohydrodynamic waves in flowing ideal incompressible solar-wind plasmas: Reconsidered

Authors: I. Zhelyazkov, Z. Dimitrov, M. Bogdanova

Comments: 16 pages, 10 figures

Subjects: Solar and Stellar Astrophysics (astro-ph.SR); Plasma Physics (physics.plasm-ph); Space Physics (physics.space-ph)

It is well established that the magnetically structured solar atmosphere supports the propagation of MHD waves along various kind of jets including also the solar wind. It is well-known as well that under some conditions, namely high enough jet speeds, the propagating MHD modes can become unstable against to the most common Kelvin--Helmholtz instability (KHI). In this article, we explore how the propagation and instability characteristics of running along a slow solar wind MHD modes are affected when they are investigated in the framework of the ideal Hall-magnetohydrodynamics. Hall-MHD is applicable if the jet width is shorter than or comparable to the so called Hall parameter $l_\mathrm{Hall} = c/\omega_\mathrm{pi}$ (where $c$ is the speed of light and $\omega_\mathrm{pi}$ is the ion plasma frequency). We model the solar wind as a moving with velocity $\vec{v}_0$ cylindrical flux tube of radius $a$, containing incompressible plasma with density $\rho_\mathrm{i}$ permeated by a constant magnetic field $\vec{B}_\mathrm{i}$. The surrounding plasma is characterized with its density $\rho_\mathrm{e}$ and magnetic field $\vec{B}_\mathrm{e}$. The dispersion relation of MHD waves is derived in the framework of both standard and Hall-MHD and is numerically solved with input parameters: the density contrast $\eta = \rho_\mathrm{e}/\rho_\mathrm{i}$, the magnetic fields ratio $b = {B}_\mathrm{e}/{B}_\mathrm{i}$, and the Hall scale parameter $l_\mathrm{Hall}/a$. It is found that the Hall current, at moderate values of $l_\mathrm{Hall}/a$, stimulates the emerging of KHI of the kink ($m = 1)$ and high-mode ($m \geqslant 2$) MHD waves, while for the sausage wave ($m = 0$) the trend is just the opposite---the KHI is suppressed.

[22]  arXiv:2002.00393 [pdf, other]

Title: Observations of the low-luminosity Type Iax supernova 2019gsc: a fainter clone of SN 2008ha?

Authors: Lina Tomasella, Maximilian Stritzinger, Stefano Benetti, Nancy Elias-Rosa, Enrico Cappellaro, Erkki Kankare, Peter Lundqvist, Mark Magee, Kate Maguire, Andrea Pastorello, Simon Prentice, Andrea Reguitti

Comments: 12 pages, 10 figures. Submitted to MNRAS

Subjects: Solar and Stellar Astrophysics (astro-ph.SR); Astrophysics of Galaxies (astro-ph.GA); High Energy Astrophysical Phenomena (astro-ph.HE)

We present optical photometric and spectroscopic observations of the faint-and-fast evolving type Iax SN 2019gsc, extending from the time of g-band maximum until about fifty days post maximum, when the object faded to an apparent r-band magnitude of about 22 mag. SN 2019gsc reached a peak luminosity of only M_g = -13.68 +/- 0.22 mag, and is characterised with a post-maximum decline rate Delta(m_15)_g = 1.66 +/- 0.15 mag. These light curve parameters are similar to those measured for SN 2008ha of M_g = -14.01 +/- 0.14 mag at peak and Delta(m_15)_g = 1.80 +/- 0.03 mag. The spectral features of SN 2019gsc also resemble those of SN 2008ha at similar phases. This includes both the extremely low ejecta velocity at maximum, about 3,000 km/s, and at late-time (phase +52 d) strong forbidden iron, nickel and cobalt lines as well as both forbidden and permitted calcium features. Furthermore, akin to SN 2008ha, the bolometric light curve of SN 2019gsc is consistent with the production of 0.003 +/- 0.001 Msol of nickel. The explosion parameters, M_ej = 0.13 Msol and E_k = 12 x 10E48 erg, are also similar to those inferred for SN 2008ha. We estimate a slightly sub-solar oxygen abundance for the host galaxy of SN 2019gsc, (12 + log10(O/H) = 8.10 +/- 0.18 dex), consistent with the equally metal-poor environment of SN 2008ha. Altogether, our dataset of SN 2019gsc indicates that it is a member of a small but growing group of extreme SN Iax that include SN 2008ha and SN 2010ae.

[23]  arXiv:2002.00405 [pdf]

Title: Accretion disks around young stars: the cradles of planet formation

Authors: Dmitry A. Semenov (1,2), Richard. D. Teague (3) ((1) Max Planck Institute for Astronomy, Heidelberg, Germany, (2) Department of Chemistry, Ludwig Maximilian University, Munich, Germany, (3) Center for Astrophysics, Harvard and Smithsonian, Boston, USA)

Comments: 7 pages, 3 figures, to appear in Europhysics News 51/1

Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Astrophysics of Galaxies (astro-ph.GA); Solar and Stellar Astrophysics (astro-ph.SR)

Protoplanetary disks around young stars are the birth sights of planetary systems like our own. Disks represent the gaseous dusty matter left after the formation of their central stars. The mass and luminosity of the star, initial disk mass and angular momentum, and gas viscosity govern disk evolution and accretion. Protoplanetary disks are the cosmic nurseries where microscopic dust grains grow into pebbles, planetesimals, and planets.

[24]  arXiv:2002.00430 [pdf, other]

Title: Assessing and Minimizing Collisions in Satellite Mega-Constellations

Authors: Nathan Reiland, Aaron J. Rosengren, Renu Malhotra, Claudio Bombardelli

Comments: 32 pages, 19 figures; submitted for publication in Adv. Space Res.; comments welcome

Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Dynamical Systems (math.DS)

We aim to provide satellite operators and researchers with an efficient means for evaluating and mitigating collision risk during the design process of mega-constellations. We first establish a baseline for evaluating various techniques for close-encounter prediction and collision-probability calculation (Hoots et al. 1984, Gronchi 2005, JeongAhn and Malhotra 2015) by carrying out brute-force numerical simulations and using a sequence of filters to greatly reduce the computational expense of the algorithm. Next, we estimate conjunction events in the orbital environment following the anticipated deployments of the OneWeb LEO and SpaceX Starlink mega-constellations. As a final step, we investigate Minimum Space Occupancy (MiSO) orbits (Bombardelli et al. 2018), a generalization of the well-known frozen orbits that account for the perturbed-Keplerian dynamics of the Earth-Moon-Sun-satellite system. We evaluate the ability of MiSO configurations of the proposed mega-constellations, as suggested by Bombardelli et al. 2018, to reduce the risk of endogenous (intra-constellation) collisions. The results indicate that the adoption of the MiSO orbital configuration can significantly reduce risk with nearly indistinguishable adjustments to the nominal orbital elements of the constellation satellites.

[25]  arXiv:2002.00572 [pdf, other]

Title: Upcoming new era of 21 cm cosmology based on SKA

Authors: Yidong Xu, Xin Zhang

Comments: 6 pages, 3 figures

Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); Astrophysics of Galaxies (astro-ph.GA); General Relativity and Quantum Cosmology (gr-qc); High Energy Physics - Phenomenology (hep-ph)

In order to precisely measure the cosmological parameters and answer the fundamental questions in cosmology, it is necessary to develop new, powerful cosmological probes, in addition to the proposed next-generation optical survey projects. The neutral hydrogen 21 cm sky surveys will definitely provide a promising tool to study the late-universe evolution, helping in elucidating the nature of dark energy. The Square Kilometre Array, the largest radio telescope in the world, which is scheduled to be constructed in the near future, will undoubtedly push the 21 cm cosmology into a new era, and greatly promote the development of cosmology in the forthcoming decades.

[26]  arXiv:2002.00592 [pdf, ps, other]

Title: Questioning the spatial origin of complex organic molecules in young protostars with the CALYPSO survey

Authors: A. Belloche, A. J. Maury, S. Maret, S. Anderl, A. Bacmann, Ph. André, S. Bontemps, S. Cabrit, C. Codella, M. Gaudel, F. Gueth, C. Lefèvre, B. Lefloch, L. Podio, L. Testi

Comments: Accepted for publication in Astronomy and Astrophysics

Subjects: Astrophysics of Galaxies (astro-ph.GA)

Complex organic molecules (COMs) have been detected in a few Class 0 protostars but their origin is not well understood. Going beyond studies of individual objects, we want to investigate the origin of COMs in young protostars on a statistical basis. We use the CALYPSO survey performed with the IRAM PdBI to search for COMs at high angular resolution in a sample of 26 solar-type protostars, including 22 Class 0 and four Class I objects. Methanol is detected in 12 sources and tentatively in one source, which represents half of the sample. Eight sources (30%) have detections of at least three COMs. We find a strong chemical differentiation in multiple systems with five systems having one component with at least three COMs detected but the other component devoid of COM emission. The internal luminosity is found to be the source parameter impacting the most the COM chemical composition of the sources, while there is no obvious correlation between the detection of COM emission and that of a disk-like structure. A canonical hot-corino origin may explain the COM emission in four sources, an accretion-shock origin in two or possibly three sources, and an outflow origin in three sources. The CALYPSO sources with COM detections can be classified into three groups on the basis of the abundances of oxygen-bearing molecules, cyanides, and CHO-bearing molecules. These chemical groups correlate neither with the COM origin scenarii, nor with the evolutionary status of the sources if we take the ratio of envelope mass to internal luminosity as an evolutionary tracer. We find strong correlations between molecules that are a priori not related chemically (for instance methanol and methyl cyanide), implying that the existence of a correlation does not imply a chemical link. [abridged]

[27]  arXiv:2002.00599 [pdf, ps, other]

Title: On Fabry-Pérot Etalon-based Instruments. III. Instrument applications

Authors: F.J. Bailén, D. Orozco Suárez, J.C. del Toro Iniesta

Comments: 10 pages, 5 figures

Journal-ref: The Astrophysical Journal Supplement Series,246:17(10pp), 2020 January

Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM)

The spectral, imaging, and polarimetric behavior of Fabry-P\'erot etalons have an influence on imaging vector magnetograph instruments based on these devices. The impact depends, among others, on the optical configuration (collimated or telecentric), on the relative position of the etalon with respect to the polarimeter, on the type of etalon (air-gapped or crystalline), and even on the polarimetric technique to be used (single-beam or dual-beam). In this paper we evaluate the artificial line-of-sight velocities and magnetic field strengths that arise in etalon-based instruments attending to the mentioned factors. We differentiate between signals that are implicit to telecentric mounts due to the wavelength dependence of the point-spread function and those emerging in both collimated and telecentric setups from the polarimetric response of birefringent etalons. For the anisotropic case we consider two possible locations of the etalon, between the modulator and the analyzer or after it, and we include the effect on different channels when dual-beam polarimetry is employed. We also evaluate the impact of the loss of symmetry produced in telecentric mounts due to imperfections in the illumination and/or to a tilt of the etalon relative to the incident beam.

[28]  arXiv:2002.00610 [pdf, ps, other]

Title: Tidal evolution of galaxies in IllustrisTNG-100 most massive cluster

Authors: Ewa L. Lokas

Comments: 13 pages, 11 figures, submitted to A&A

Subjects: Astrophysics of Galaxies (astro-ph.GA); Cosmology and Nongalactic Astrophysics (astro-ph.CO)

We study the tidal evolution of galaxies in the most massive cluster of the IllustrisTNG-100 simulation. For the purpose of this work we select 112 galaxies with the largest stellar masses at present and follow their properties in time. Using their orbital history we divide the sample into unevolved (infalling), weakly evolved (with one pericenter passage) and strongly evolved (with multiple pericenters). The samples are clearly separated by the value of the integrated tidal force from the cluster the galaxies experienced during their entire evolution and their properties depend strongly on this quantity. As a result of tidal stripping, the galaxies of the weakly evolved sample lost between 10 and 80% of their dark mass and less than 10% of stars, while those in the strongly evolved one more than 70% of dark and between 10 and 55% of stellar mass, and are significantly less or even not dark matter dominated. While 33% of the infalling galaxies do not contain any gas, this fraction increases to 67% for the weakly evolved and to 100% for the strongly evolved sample. The strongly evolved galaxies lose their gas earlier and faster (within 2-6 Gyr) but the process can take up to 4 Gyr from the first pericenter passage. These galaxies are redder and more metal rich, and at redshift z=0.5 the population of galaxies in the cluster becomes predominantly red. As a result of tidal stirring, the morphology of the galaxies evolves from oblate to prolate and their rotation is diminished thus the morphology-density relation is reproduced in the simulated cluster. The strongly evolved sample contains at least six convincing examples of tidally induced bars and six more galaxies that had their bars enhanced by their interaction with the cluster.

[29]  arXiv:2002.00637 [pdf, ps, other]

Title: The density maps of the HS47.5-22 field

Authors: Sergei N. Dodonov, Aleksandra Grokhovskaya

Comments: 13 pages, 7 figures, 1 Table

Journal-ref: https://www.ta3.sk/caosp/Eedition/Abstracts/2020/Vol_50/No_1/pp257-269_abstract.html

Subjects: Astrophysics of Galaxies (astro-ph.GA)

We study the reconstruction of overdensity maps of galaxies as function of redshift in the range $0 < \mathrm z < 0.8$ using data from 1-m Schmidt Telescope of Byurakan Astrophysical Observatory (Armenia) in 16 medium band $\sim 250$ A and four broad band (u,g,r,i) filters. The data used in this work homogeneously cover $2.39$ sq. deg with accurate photometric redshiftss, down to $\mathrm R < 23$ mag (AB). We reconstructed the density contrast maps for the whole galaxy sample of the HS 47.5-22 ROSAT field in narrow slices for full range of redshifts. We select groups and clusters of galaxies with adaptive kernel based on density peaks which are larger than two times the mean density. The reconstructed overdensity field of galaxies consists of cluster-like structures outlining void-like regions for full redshift range $0 \leq \mathrm z \leq 0.8$. We detect known galaxy clusters in this field with software specially developed for this project. This gives us a possibility to study how star formation properties and galaxy morphology depend on the environments of the galaxies in this field.

[30]  arXiv:2002.00659 [pdf, ps, other]

Title: Asteroid migration due to the Yarkovsky effect and the distribution of the Eos family

Authors: Yang-Bo Xu (1), Li-Yong Zhou (1), Christoph Lhotka (2), Wing-Huen Ip (3) ((1) Nanjing University (2) Austrian Academy of Sciences, (3) National Central University)

Comments: 15 pages, 7 figures

Subjects: Earth and Planetary Astrophysics (astro-ph.EP)

Based on a linearized model of the Yarkovsky effect, we investigate in this paper the dependence of the semimajor axis drift $\Delta a$ of a celestial body on its size, spinning obliquity, initial orbit and thermal parameters on its surface. With appropriate simplification and approximation, we obtain the analytical solutions to the perturbation equations for the motion of asteroids influenced by the Yarkovsky effect, and they are then verified by numerical simulations of the full equations of motion. These solutions present explicitly the dependencies of $\Delta a$ on the thermal and dynamical parameters of the asteroid. With these analytical formulae for $\Delta a$, we investigate the combined seasonal and diurnal Yarkovsky effects. The critical points where the migration direction reverses are calculated and the consequent selective effects according to the size and rotation state of asteroids are discussed. %Solely the Yarkovsky effect is found to be able to produce some ring structure in the aged circumstellar debris disk. Finally, we apply the analytical formulae to calculate the migration of Eos family members. The space distribution of asteroids is well reproduced. Our calculations suggest that statistically the orientations of spin axes of family members satisfy a random-obliquity distribution, and the rotation rate $\omega_{\rm rot}$ of asteroid depends on its size $R$ by $\omega_{\rm rot}\propto R^{-1}$.

[31]  arXiv:2002.00674 [pdf, other]

Title: Dynamical heating of the X-ray emitting intracluster medium: the roles of merger shocks and turbulence dissipation

Authors: Xun Shi, Daisuke Nagai, Han Aung, Andrew Wetzel

Comments: 11 pages, 11 figures, submitted to MNRAS

Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO)

The diffuse plasma inside clusters of galaxies has X-ray emitting temperatures of a few keV. The physical mechanisms that heat this intracluster medium (ICM) to such temperatures include the accretion shock at the periphery of a galaxy cluster, the shocks driven by merger events, as well as a somewhat overlooked mechanism -- the dissipation of intracluster turbulent motions. We study the relative role of these heating mechanisms using simulated galaxy clusters in a set of Lagrangian tracer particle re-simulations of the non-radiative run of the Omega500 cosmological simulation. We adopt a novel analysis method of decomposing the temperature increase at each time step into that associated with entropy increase and that caused by density variations, which enables separation of irreversible dissipative heating and adiabatic heating. The high time resolution and a large number of tracer particles allow a unique view of the spatial-temporal distribution of these heating rates, in which merger tracks are clearly visible, demonstrating the dominant role of merger events in heating the ICM. The dissipative heating contributed by each merger event is extended in time and occurs also in regions where the gas density is decreasing, suggesting the importance of heating by the dissipation of merger-induced turbulence. Quantitative analysis shows that turbulence heating, rather than direct heating at merger shocks, dominates the temperature increase of the ICM especially at inner radii $r < r_{\rm 500c}$. In addition, we find that many merger shocks can propagate with almost constant velocity to very large radii $r \gg r_{\rm 500c}$, some even reach and join with the accretion shock, becoming the outer boundary of the ICM. Altogether, these results suggest that the ICM is heated more in an `inside-out' fashion rather than `outside-in' as depicted in the classical smooth accretion picture.

[32]  arXiv:2002.00687 [pdf, other]

Title: A toy model for the electromagnetic output of neutron star merger prompt collapse to a black hole: magnetised neutron star collisions

Authors: Antonios Nathanail

Comments: 14 pages, 10 figures

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

We present a systematic study of magnetised neutron star head on collisions. We investigate the resulting magnetic field geometries as the two neutron stars merge. Furthermore, we analyze the luminosity produced in these collisions and monitor the evolution of the magnetic fields from the time of merger until the subsequent production of a black hole. At the time of black hole formation the luminosity peaks and rings-down following the decay of the electromagnetic fields. A comparison is presented for three different cases, one where the initial magnetic field in both neutron stars is aligned, one where they are anti-aligned and also one case where they have unequal magnetic field strength initially. We identify regions and set limits that pair creation and magnetic reconnection would occur in this scenario, and further discuss limits and differences in the radiated energy. This study should be regarded as a toy model of the case where the remnant, of a binary neutron star merger, undergoes a prompt collapse to a black hole with a negligible surrounding disk. We note that the generated electromagnetic pulses resembles the fast radio bursts phenomenology. We consider implications on the high mass mergers leading to a fast prompt collapse to a black hole and the expected flux to be observed in a distance similar to the binary neutron star gravitational wave detection GW190425.

[33]  arXiv:2002.00691 [pdf, other]

Title: $\texttt{triceratops}$: A Tool for Rapid Validation of $\textit{TESS}$ Objects of Interest and Application to 424 Planet Candidates

Authors: Steven Giacalone, Courtney D. Dressing

Comments: Submitted to AAS journals

Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Instrumentation and Methods for Astrophysics (astro-ph.IM); Solar and Stellar Astrophysics (astro-ph.SR)

We present a new tool, $\texttt{triceratops}$, that can be used to rapidly validate $\textit{TESS}$ Objects of Interest (TOIs). We test this procedure on 213 TOIs that have been previously confirmed as planets or rejected as astrophysical false positives. We find that our tool is generally able to distinguish bona fide planets from astrophysical false positives for TOIs with radii smaller than $8 R_\oplus$, and that it performs better when the candidate host is observed with a shorter cadence. We apply this procedure on 424 unclassified TOIs and identify 262 that have high probabilities of being bona fide planets and 61 that have high probabilities of being false positives. We discuss how this tool can be utilized for follow-up target prioritization and how it can be used in tandem with existing vetting tools to perform thorough validation analyses of planet candidates detected by $\textit{TESS}$.

[34]  arXiv:2002.00696 [pdf, other]

Title: From Stellar Coronæ to Gyrochronology: a theoretical and observational exploration

Authors: Jérémy Ahuir, Allan-Sacha Brun, Antoine Strugarek

Comments: 19 pages, 8 figures, accepted for publication in Astronomy & Astrophysics

Subjects: Solar and Stellar Astrophysics (astro-ph.SR)

Context. Stellar spin-down is the result of a complex process involving rotation, dynamo, wind and magnetism. Multi-wavelength surveys of solar-like stars have revealed the likely existence of relationships between their rotation, X-ray luminosity, mass-losses and magnetism. Those impose strong constraints on the corona and wind of cool stars.
Aims. We aim to provide power-law prescriptions of the mass-loss of stars, of their magnetic field, and of their base coronal density and temperature that are compatible with their observationally-constrained spin-down.
Methods. We link the magnetic field and the mass-loss rate from a wind torque formulation in agreement with the distribution of stellar rotation periods in open clusters and the Skumanich law. Given a wind model and an expression of the X-ray luminosity from radiative losses, we constrain the coronal properties by assuming different physical scenarii linking closed loops to coronal holes.
Results. We find that the magnetic field and the mass loss are involved in a one-to-one correspondence constrained from spin-down considerations. We show that a magnetic field depending on both the Rossby number and the stellar mass is required to keep a consistent spin-down model. The estimates of the magnetic field and the mass-loss rate obtained from our formalism are consistent with statistical studies as well as individual observations and give new leads to constrain the magnetic field-rotation relation. The set of scaling-laws we derived can be broadly applied to cool stars from the PMS to the end of the MS, and allow for a stellar wind modelling consistent with all the observational constraints available to date.

[35]  arXiv:2002.00723 [pdf, other]

Title: Impact of gravity waves on the middle atmosphere of Mars: a non-orographic gravity wave parameterization based on Global Climate modeling and MCS observations

Authors: G. Gilli, F. Forget, A. Spiga, T. Navarro, E. Millour, L. Montabone, A. Kleinböhl, D. M. Kass, D. J. McCleese, J. T. Schofield

Comments: JGR (Planets), accepted

Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Atmospheric and Oceanic Physics (physics.ao-ph)

The impact of gravity waves (GW) on diurnal tides and the global circulation in the middle/upper atmosphere of Mars is investigated using a General Circulation Model (GCM). We have implemented a stochastic parameterization of non-orographic GW into the Laboratoire de M\'et\'eorologie Dynamique (LMD) Mars GCM (LMD-MGCM) following an innovative approach. The source is assumed to be located above typical convective cells ($\sim$ 250 Pa) and the effect of GW on the circulation and predicted thermal structure above 1 Pa ($\sim$ 50 km) is analyzed. We focus on the comparison between model simulations and observations by the Mars Climate Sounder (MCS) on board Mars Reconnaissance Orbiter during Martian Year 29. MCS data provide the only systematic measurements of the Martian mesosphere up to 80 km to date. The primary effect of GW is to damp the thermal tides by reducing the diurnal oscillation of the meridional and zonal winds. The GW drag reaches magnitudes of the order of 1 m/s/sol above 10$^{-2}$ Pa in the northern hemisphere winter solstice and produces major changes in the zonal wind field (from tens to hundreds of m/s), while the impact on the temperature field is relatively moderate (10-20K). It suggests that GW induced alteration of the meridional flow is the main responsible for the simulated temperature variation. The results also show that with the GW scheme included, the maximum day-night temperature difference due to the diurnal tide is around 10K, and the peak of the tide is shifted toward lower altitudes, in better agreement with MCS observations.

[36]  arXiv:2002.00773 [pdf, other]

Title: Understanding and Mitigating Biases when Studying Inhomogeneous Emission Spectra with JWST

Authors: Jake Taylor, Vivien Parmentier, Patrick G.J. Irwin, Suzanne Aigrain, Graham K.H. Lee, Joshua Krissansen-Totton

Comments: 13 pages, 9 figures, submitted to MNRAS after addressing a second round of comments from reviewer

Subjects: Earth and Planetary Astrophysics (astro-ph.EP)

Exoplanet emission spectra are often modelled assuming that the hemisphere observed is well represented by a horizontally homogenised atmosphere. However this approximation will likely fail for planets with a large temperature contrast in the James Webb Space Telescope (JWST) era, potentially leading to erroneous interpretations of spectra. We first develop an analytic formulation to quantify the signal-to-noise ratio and wavelength coverage necessary to disentangle temperature inhomogeneities from a hemispherically averaged spectrum. We find that for a given signal-to-noise ratio, observations at shorter wavelengths are better at detecting the presence of inhomogeneities. We then determine why the presence of an inhomogeneous thermal structure can lead to spurious molecular detections when assuming a fully homogenised planet in the retrieval process. Finally, we quantify more precisely the potential biases by modelling a suite of hot Jupiter spectra, varying the spatial contributions of a hot and a cold region, as would be observed by the different instruments of JWST/NIRSpec. We then retrieve the abundances and temperature profiles from the synthetic observations. We find that in most cases, assuming a homogeneous thermal structure when retrieving the atmospheric chemistry leads to biased results, and spurious molecular detection. Explicitly modelling the data using two profiles avoids these biases, and is statistically supported provided the wavelength coverage is wide enough, and crucially also spanning shorter wavelengths. For the high contrast used here, a single profile with a dilution factor performs as well as the two-profile case, with only one additional parameter compared to the 1-D approach.

[37]  arXiv:2002.00783 [pdf, ps, other]

Title: $l=1$: Weinberg's weakly damped mode in an $N$-body model of a spherical stellar system

Authors: Douglas C. Heggie, Philip G. Breen, Anna Lisa Varri

Comments: 9 pages, 6 figures, Monthly Notices of the Royal Astronomical Society, Advance Access, this https URL

Subjects: Astrophysics of Galaxies (astro-ph.GA)

Spherical stellar systems such as King models, in which the distribution function is a decreasing function of energy and depends on no other invariant, are stable in the sense of collisionless dynamics. But Weinberg showed, by a clever application of the matrix method of linear stability, that they may be nearly unstable, in the sense of possessing {\sl weakly} damped modes of oscillation. He also demonstrated the presence of such a mode in an $N$-body model by endowing it with initial conditions generated from his perturbative solution. In the present paper we provide evidence for the presence of this same mode in $N$-body simulations of the King $W_0 = 5$ model, in which the initial conditions are generated by the usual Monte Carlo sampling of the King distribution function. It is shown that the oscillation of the density centre correlates with variations in the structure of the system out to a radius of about 1 virial radius, but anticorrelates with variations beyond that radius. Though the oscillations appear to be continually reexcited (presumably by the motions of the particles) we show by calculation of power spectra that Weinberg's estimate of the period (strictly, $2\pi$ divided by the real part of the eigenfrequency) lies within the range where the power is largest. In addition, however, the power spectrum displays another very prominent feature at shorter periods, around 5 crossing times.

[38]  arXiv:2002.00805 [pdf, other]

Title: Systematic search for gamma-ray periodicity in active galactic nuclei detected by the Fermi Large Area Telescope

Authors: P. Peñil (UC Madrid), A. Domínguez (UC Madrid), S. Buson, M. Ajello, J. Otero-Santos, J. A. Barrio, R. Nemmen, S. Cutini, B. Rani, A. Franckowiak, E. Cavazzuti

Comments: 16 pages, 5 figures, 4 tables. Submitted to ApJ

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

We use nine years of gamma-ray data provided by the Fermi Large Area Telescope (LAT) to systematically study the light curves of more than two thousand active galactic nuclei (AGN) included in recent Fermi-LAT catalogs. Ten different techniques are used, which are organized in an automatic periodicity-search flow, in order to search for evidence of periodic emission in gamma rays. Understanding the processes behind this puzzling phenomenon will provide a better view about the astrophysical nature of these extragalactic sources. However, the observation of temporal patterns in gamma-ray light curves of AGN is still challenging. Despite the fact that there have been efforts on characterizing the temporal emission of some individual sources, a systematic search for periodicities that considers large samples of sources is missing. Our analysis finds 11 AGN, of which 9 are identified for the first time, showing periodicity at more than $4\sigma$ in at least four algorithms. These findings will help in solving questions related to the astrophysical origin of this periodic behavior.

[39]  arXiv:2002.00871 [pdf, ps, other]

Title: Orbital period dependent spatial scatter of Galactic Black Hole Transients

Authors: P. Gandhi, A. Rao, P.A. Charles (Univ. Southampton), K. Belczynski (Warsaw), T.J. Maccarone, K. Arur (TTU), J.M. Corral-Santana (ESO)

Comments: MNRAS Letters submitted. Comments welcome

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Astrophysics of Galaxies (astro-ph.GA); Solar and Stellar Astrophysics (astro-ph.SR)

There remain significant uncertainties in the origin and evolution of black holes in binary systems, in particular regarding their birth sites and the influence of natal kicks. These are long-standing issues, but their debate has been reinvigorated in the era of gravitational wave detections and the improving precision of astrometric measurements. Using recent and archival characterisation of Galactic black hole X-ray binaries (BHXBs), we report here an apparent anticorrelation between P{orb} (system orbital periods) and scatter in z (elevation above the Galactic plane). The absence of long period sources at high z is not an obvious observational bias, and two possible explanatory scenarios are qualitatively explored: (1) a disc origin for BHXBs followed by natal kicks producing the scatter in z, with only the tightest binaries preferentially surviving strong kicks; (2) a halo origin, with P{orb} shortening through dynamical interactions in globular clusters (GCs). For the latter case, we show a correspondence in z-scatter between BHXBs and the GCs with most compact core radii of <0.1pc. However, the known absence of outbursting BHXB transients within Galactic GCs remains puzzling in this case, in contrast to the multitude of known GC neutron star XRBs. These results provide an interesting observational constraint for any black hole binary evolutionary model to satisfy.

[40]  arXiv:2002.00898 [pdf, ps, other]

Title: CMB and BBN constraints on evaporating primordial black holes revisited

Authors: Sandeep Kumar Acharya, Rishi Khatri

Comments: Comments welcome

Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics - Phenomenology (hep-ph)

We derive new CMB anisotropy power spectrum and BBN constraints for evaporating primordial black holes by explicitly solving the electromagnetic particle cascades of emitted particles and the deposition of this emitted energy to the background baryon-photon plasma. We show that the CMB anisotropies can provide stronger constraints compared to BBN and CMB spectral distortions on black holes with masses as small as $M_{\rm BH}=1.1\times 10^{13}$g, a slightly smaller mass than what has been considered in literature until now. We also show that, with more up-to-date data on abundances of deuterium and helium-3, BBN constraints are strengthened significantly.

[41]  arXiv:2002.00906 [pdf, other]

Title: The CARMENES search for exoplanets around M dwarfs. Dynamical characterization of the multiple planet system GJ 1148 and prospects of habitable exomoons around GJ 1148 b

Authors: T. Trifonov, M. H. Lee, M. Kürster, Th. Henning, E. Grishin, S. Stock, J. Tjoa, J. A. Caballero, K. H. Wong, F. F. Bauer, A. Quirrenbach, M. Zechmeister, I. Ribas, S. Reffert, A. Reiners, P. J. Amado, D. Kossakowski, M. Azzaro, V. J. S. Béjar, M. Cortés-Contreras, S. Dreizler, A. P. Hatzes, S. V. Jeffers, A. Kaminski, M. Lafarga, D. Montes, J. C. Morales, A. Pavlov, C. Rodríguez-López, J. H. M. M. Schmitt, E. Solano, R. Barnes

Comments: Accepted for publication in A&A

Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Solar and Stellar Astrophysics (astro-ph.SR)

Context. GJ 1148 is an M-dwarf star hosting a planetary system composed of two Saturn-mass planets in eccentric orbits with periods of 41.38 and 532.02 days. Aims. We reanalyze the orbital configuration and dynamics of the GJ 1148 multi-planetary system based on new precise radial velocity (RV) measurements taken with CARMENES. Methods. We combined new and archival precise Doppler measurements from CARMENES with those available from HIRES for GJ 1148 and modeled these data with a self-consistent dynamical model. We studied the orbital dynamics of the system using the secular theory and direct N-body integrations. The prospects of potentially habitable moons around GJ 1148 b were examined. Results. The refined dynamical analyses show that the GJ 1148 system is long-term stable in a large phase-space of orbital parameters with an orbital configuration suggesting apsidal alignment, but not in any particular high-order mean-motion resonant commensurability. GJ 1148 b orbits inside the optimistic habitable zone (HZ). We find only a narrow stability region around the planet where exomoons can exist. However, in this stable region exomoons exhibit quick orbital decay due to tidal interaction with the planet. Conclusions. The GJ 1148 planetary system is a very rare M-dwarf planetary system consisting of a pair of gas giants, the inner of which resides in the HZ. We conclude that habitable exomoons around GJ 1148 b are very unlikely to exist.

[42]  arXiv:2002.00907 [pdf, ps, other]

Title: The infrared view of dust and molecules around V4334 Sgr (Sakurai's Object): a 20-year retrospective

Authors: A. Evans (Keele University, UK), R. D. Gehrz, C. E. Woodward (University of Minnesota, USA), D. P. K. Banerjee (Physical Research Laboratory, Ahmedabad, India), T. R. Geballe (Gemini Observatory), G. C. Clayton (Louisiana State University, USA), P. J. Sarre (University of Nottingham, UK), S. Starrfield (Arizona State University, USA), K. Hinkle, R. R. Joyce (NSF's National Optical-Infrared Astronomy Research Laboratory, USA), Foteini Lykou (The University of Hong Kong), L. A. Helton (USRA-SOFIA Science Center, USA), S. P. S. Eyres (University of South Wales, University of Central Lancashire, UK), H. Worters (SAAO, South Africa), E. J. Montiel (USRA-SOFIA Science Center, University of California Davis, USA), T. Liimets (Tartu Observatory, Estonia, Astronomický ústav, Czeck Republic), et al. (3 additional authors not shown)

Subjects: Solar and Stellar Astrophysics (astro-ph.SR); Astrophysics of Galaxies (astro-ph.GA)

We present an analysis of the evolution of circumstellar dust and molecules in the environment of the very late thermal pulse object V4334 Sgr (Sakurai's Object) over a $\sim20$-year period, drawing on ground-, airborne- and space-based infrared photometry and spectroscopy. The dust emission, which started in 1997, resembles a blackbody that cooled from $\sim1200$K in 1998 August to $\sim180$K in 2016 July. The dust mass, assuming amorphous carbon, was $\sim5\times10^{-10}$M$_\odot$ in 1998 August, and we estimate that the total dust mass was $\sim2\times10^{-5}$M$_\odot$ by $\sim2016$. The appearance of a near infrared excess in 2008 suggests a new episode of (or renewed) mass loss began then. We infer lower limits on the bolometric luminosity of the embedded star from that of the dust shell, which rose to $\sim16000$L$_\odot$ before declining to $\sim3000$L$_\odot$. There is evidence for weak 6-7$\mu$m absorption, which we attribute to hydrogenated amorphous carbon formed in material ejected by Sakurai's Object during a mass ejection phase that preceded the 1997 event. We detect small hydrocarbon and other molecules in the spectra, and trace the column densities in hydrogen cyanide (HCN) and acetylene (C$_2$H$_2$). We use the former to determine the $^{12}$C/$^{13}$C ratio to be $6.4\pm0.7$, 14 times smaller than the Solar System value.

[43]  arXiv:2002.00908 [pdf, other]

Title: Infrared properties of Planetary Nebulae with [WR] and $wels$ central stars

Authors: C. Muthumariappan, M. Parthasarathy

Comments: Accepted for publication in MNRAS

Subjects: Solar and Stellar Astrophysics (astro-ph.SR); Astrophysics of Galaxies (astro-ph.GA)

We report the IR properties of planetary nebulae with WR type and $wels$ central stars known to date and compare them with the IR properties of a sample of PNe with H-rich central stars. We use near-, mid- and far-IR photometric data from archives to derive the IR properties of PNe. We have constructed IR colour-colour diagrams of PNe using measurements from $2MASS$, $IRAS$, $WISE$ and $Akari$ bands. [WR] PNe have a larger near-IR emission from the hot dust component and also show a tendency for stronger 12$\mu$m emission as compared to the other two groups. Cool AGB dust properties of all PNe are found to be similar. We derived the dust colour temperatures, dust masses, dust-to-gas mass ratios, IR luminosities and IR excess of PNe for these three groups. [WR] PNe and $wels$-PNe tend to have larger mean values for dust mass when compared to the third group. The average dust-to-gas mass ratio is found to be similar for the three groups of PNe. While there is a strong correlation of dust temperature and IR luminosity with the age for the three groups of PNe, the dust mass, dust-to-gas mass ratios and IR excess are found to be non-varying as the PNe evolve. [WR] PNe and $wels$-PNe show very similar distribution of excitation classes and also show similar distribution with Galactic latitude.

[44]  arXiv:2002.00929 [pdf, other]

Title: 3D propagation of relativistic solar protons through interplanetary space

Authors: S. Dalla, G. De Nolfo, A. Bruno, J. Giacalone, T. Laitinen, S. Thomas, M. Battarbee, M.S. Marsh

Comments: Submitted to A&A (9 pages, 6 figures)

Subjects: Solar and Stellar Astrophysics (astro-ph.SR); High Energy Astrophysical Phenomena (astro-ph.HE); Space Physics (physics.space-ph)

Context. Solar Energetic Particles (SEPs) with energy in the GeV range can propagate to Earth from their acceleration region near the Sun and produce Ground Level Enhancements (GLEs). The traditional approach to interpreting and modelling GLE observations assumes particle propagation only parallel to the magnetic field lines of interplanetary space, i.e. it is spatially 1D. Recent measurements by PAMELA have characterised SEP properties at 1 AU for the ~100 MeV-1 GeV range at high spectral resolution. Aims. We model the transport of GLE-energy solar protons through the Interplanetary Magnetic Field (IMF) using a 3D approach, to assess the effect of the Heliospheric Current Sheet (HCS) and drifts associated to the gradient and curvature of the Parker spiral. The latter are influenced by the IMF polarity. We derive 1 AU observables and compare the simulation results with data from PAMELA. Methods. We use a 3D test particle model including a HCS. Monoenergetic populations are studied first to obtain a qualitative picture of propagation patterns and numbers of crossings of the 1 AU sphere. Simulations for power law injection are used to derive intensity profiles and fluence spectra at 1 AU. A simulation for a specific event, GLE 71, is used to compare with PAMELA data. Results. Spatial patterns of 1 AU crossings and the average number of crossings are strongly influenced by 3D effects, with significant differences between periods of A+ and A- polarities. The decay time constant of 1 AU intensity profiles varies depending on the polarity and position of the observer, and it is not a simple function of the mean free path as in 1D models. Energy dependent leakage from the injection flux tube is particularly important for GLE energy particles, in many cases resulting in a roll-over in the fluence spectrum.

[45]  arXiv:2002.00936 [pdf]

Title: High-contrast Demonstration of an Apodized Vortex Coronagraph

Authors: Jorge Llop-Sayson, Garreth Ruane, Dimitri Mawet, Nemanja Jovanovic, Carl T. Coker, Jacques-Robert Delorme, Daniel Echeverri, Jason Fucik, A J Eldorado Riggs, J. Kent Wallace

Journal-ref: The Astronomical Journal, Volume 159, Number 3, year 2020

Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM)

High contrast imaging is the primary path to the direct detection and characterization of Earth-like planets around solar-type stars; a cleverly designed internal coronagraph suppresses the light from the star, revealing the elusive circumstellar companions. However, future large-aperture telescopes ($>$4~m in diameter) will likely have segmented primary mirrors, which causes additional diffraction of unwanted stellar light. Here we present the first high contrast laboratory demonstration of an apodized vortex coronagraph (AVC), in which an apodizer is placed upstream of a vortex focal plane mask to improve its performance with a segmented aperture. The gray-scale apodization is numerically optimized to yield a better sensitivity to faint companions assuming an aperture shape similar to the LUVOIR-B concept. Using wavefront sensing and control over a one-sided dark hole, we achieve a raw contrast of $2\times10^{-8}$ in monochromatic light at 775~nm, and a raw contrast of $4\times10^{-8}$ in a 10\% bandwidth. These results open the path to a new family of coronagraph designs, optimally suited for next-generation segmented space telescopes.

Cross-lists for Tue, 4 Feb 20

[46]  arXiv:2001.11910 (cross-list from hep-th) [pdf, other]

Title: Gravitating cosmic superconducting tubes in the Einstein gauged non-linear sigma-model in (3+1)-dimensions

Authors: Fabrizio Canfora, Alex Giacomini, Marcela Lagos, Seung Hun Oh, Aldo Vera

Comments: 26 pages, 9 figures

Subjects: High Energy Physics - Theory (hep-th); Cosmology and Nongalactic Astrophysics (astro-ph.CO); General Relativity and Quantum Cosmology (gr-qc)

In this paper we construct the first analytic examples of (3+1)-dimensional self-gravitating regular cosmic tube solutions which are superconducting, free of curvature singularities and with non trivial topological charge in the Einstein-SU(2) non-linear sigma-model. These gravitating topological solitons at large distance from the axis look like a (boosted) cosmic string with an angular defect given by the parameters of the theory, and near the axis the parameters of the solutions can be chosen so that the metric is singularity free and without angular defect. The curvature is concentrated on a tube around the axis. These solutions are similar to global strings but regular everywhere, and the non-linear sigma-model regularizes the global string in a similar way as a non-Abelian field regularizes the Dirac monopole. Also, these solutions can be promoted to self consistent solutions of the fully coupled Einstein Maxwell non-linear sigma-model in which the non-linear sigma model is minimally coupled both to the U(1) gauge field and to General Relativity. The analysis shows that these solutions behave as superconductors as they carry a persistent current even when the $U(1)$ field vanishes. Such persistent current cannot be continuously deformed to zero as it is tied to the topological charge of the solutions themselves. The peculiar features of the gravitational lensing of these gravitating solitons are shortly discussed.

[47]  arXiv:2002.00036 (cross-list from hep-ph) [pdf, other]

Title: Degenerate Sub-keV Fermion Dark Matter from a Solution to the Hubble Tension

Authors: Gongjun Choi, Motoo Suzuki, Tsutomu T. Yanagida

Comments: 7 pages, 2 figures

Subjects: High Energy Physics - Phenomenology (hep-ph); Cosmology and Nongalactic Astrophysics (astro-ph.CO); Astrophysics of Galaxies (astro-ph.GA)

We present a dark sector model addressing both the Hubble tension and the core-cusp problem. The model is based on a hidden Abelian gauge symmetry group with some chiral fermions required by the anomaly cancellation conditions, producing a candidate for the decaying fermion dark matter as a solution to the Hubble tension. Moreover, the sub-keV mass regime and the thermal history of the dark sector help the dark matter candidate resolve the core-cusp problem occurring in the standard $\Lambda$CDM cosmology.

[48]  arXiv:2002.00296 (cross-list from gr-qc) [pdf, other]

Title: Extracting the gravitational recoil from black hole merger signals

Authors: Vijay Varma, Maximiliano Isi, Sylvia Biscoveanu

Comments: 10 pages, including supplement

Subjects: General Relativity and Quantum Cosmology (gr-qc); High Energy Astrophysical Phenomena (astro-ph.HE)

Gravitational waves carry energy, angular momentum, and linear momentum. In generic binary black hole mergers, the loss of linear momentum imparts a recoil velocity, or a "kick", to the remnant black hole. We exploit recent advances in gravitational waveform and remnant black hole modeling to extract information about the kick from the gravitational wave signal. We find that, although little information can be gained about the kick for existing gravitational wave events, interesting measurements will soon become possible as detectors improve. We show that, once LIGO and Virgo reach their design sensitivities, we will reliably extract the kick velocity for generically precessing binaries--including the so-called superkicks, reaching up to 5000 km/s. Kick measurements such as these are astrophysically valuable, enabling independent constraints on the rate of second-generation mergers. Finally, we show that kicks must be factored into future ringdown tests of general relativity with third-generation gravitational wave detectors to avoid systematic biases.

[49]  arXiv:2002.00437 (cross-list from gr-qc) [pdf, other]

Title: Duel of cosmological screening lengths

Authors: Ezgi Canay, Maxim Eingorn

Comments: 17 pages, one nice figure

Subjects: General Relativity and Quantum Cosmology (gr-qc); Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Physics - Theory (hep-th)

Two distinct perturbative approaches have been recently formulated within General Relativity, arguing for the screening of gravity in the $\Lambda$CDM Universe. In this paper we compare them and show that the offered screening concepts, each characterized by its own interaction range, can peacefully coexist. Accordingly, we advance a united scheme, determining the gravitational potential at all scales, including regions of nonlinear density contrasts, by means of a simple Helmholtz equation with the effective cosmological screening length. In addition, we claim that cosmic structures may not grow at distances above this Yukawa range and confront its current value with dimensions of the largest known objects in the Universe.

[50]  arXiv:2002.00459 (cross-list from hep-ex) [pdf, other]

Title: Annual modulations from secular variations: relaxing DAMA?

Authors: Dario Buttazzo, Paolo Panci, Nicola Rossi, Alessandro Strumia

Comments: 19 pages, 9 figures, 1 table

Subjects: High Energy Physics - Experiment (hep-ex); Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Physics - Phenomenology (hep-ph)

The DAMA collaboration reported an annually modulated rate with a phase compatible with a Dark Matter induced signal. We point out that a slowly varying rate can bias or even simulate an annual modulation if data are analyzed in terms of residuals computed by subtracting approximately yearly averages starting from a fixed date, rather than a background continuous in time. In the most extreme case, the amplitude and phase of the annual modulation reported by DAMA could be alternatively interpreted as a decennial growth of the rate. This possibility appears mildly disfavoured by a detailed study of the available data, but cannot be safely excluded. In general, a decreasing or increasing rate could partially reduce or enhance a true annual modulation, respectively. The issue could be clarified by looking at the full time-dependence of the DAMA total rate, not explicitly published so far.

[51]  arXiv:2002.00594 (cross-list from nucl-th) [pdf, other]

Title: Effects of Dark Matter on Nuclear and Neutron Star Matter

Authors: Harish Chandra Das, Ankit Kumar, Bharat Kumar, Subrat Kumar Biswal, Takashi Nakatsukasa, Ang Li, S. K. Patra

Comments: 10 pages, 12 figures, comments are welcome

Subjects: Nuclear Theory (nucl-th); High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics - Phenomenology (hep-ph)

We study the dark matter (DM) effects on the nuclear matter (NM) parameters characterising the equation of states (EOS) of super dense neutron-rich nucleonic-matter. The observables of the NM, i.e. incompressibility, symmetry energy and its higher order derivatives in the presence DM for symmetric and asymmetric NM, are analysed with the help of relativistic mean field (RMF) model. The calculations are also extended to $\beta$-stable matter to explore the properties of the NS. We analyse the DM effects on symmetric NM, pure neutron matter and NS matter with the help of RMF model using NL3, G3 and IOPB-I forces. The binding energy and pressure are calculated with and without considering the DM interaction with the NM systems. The influences of DM are also analysed on the symmetry energy and its different coefficients. The incompressibility and the skewness parameters are affected considerably due to the presence of DM in the NM medium. We extend the calculations to NS and find its mass, radius and the moment of inertia for static and rotating NS with and without DM contribution. The mass of the NS is considerably changes due to rapid rotation with the frequency in the mass-shedding limit. The effects of DM are found to be important for some of the NM parameters, which are crucial for the properties of astrophysical objects.

[52]  arXiv:2002.00881 (cross-list from hep-ph) [pdf, other]

Title: FindBounce: package for multi-field bounce actions

Authors: Victor Guada, Miha Nemevšek, Matevž Pintar

Comments: 30 pages, 8 figures. Package homepage is available at this https URL

Subjects: High Energy Physics - Phenomenology (hep-ph); Cosmology and Nongalactic Astrophysics (astro-ph.CO)

We are launching FindBounce, a Mathematica package for the evaluation of the Euclidean bounce action that enters the decay rate of metastable states in quantum and thermal field theories. It is based on the idea of polygonal bounces, which is a semi-analytical approach to solving the bounce equation by discretizing the potential into piecewise linear segments. This allows for a fast and robust evaluation of arbitrary potentials with specified precision and any number of scalar fields. Time cost grows linearly with the number of fields and/or the number of segments. Computation with 20 fields takes $\sim 2$ seconds with $0.5\%$ accuracy of the action. The FindBounce function is simple to use with the native Mathematica look and feel, it is easy to install, and comes with detailed documentation and physical examples, such as the calculation of the nucleation temperature. We also provide timing benchmarks with comparisons to existing tools, where applicable.

Replacements for Tue, 4 Feb 20

[53]  arXiv:1505.01793 (replaced) [pdf, other]

Title: Implications of the observation of dark matter self-interactions for singlet scalar dark matter

Authors: Robyn Campbell, Stephen Godfrey, Heather E. Logan, Andrea D. Peterson, Alexandre Poulin (Carleton U.)

Comments: 9 pages, 3 figures. V4: We included the Higgs width in equation and modified the paragraph following eqn 11 to reflect this change. This modification had no effect on our subsequent conclusions. The revised paper subsumes the erratum submitted to the journal

Journal-ref: Phys. Rev. D 92, 055031 (2015)

Subjects: High Energy Physics - Phenomenology (hep-ph); Cosmology and Nongalactic Astrophysics (astro-ph.CO)

[54]  arXiv:1812.05760 (replaced) [pdf, ps, other]

Title: A Halo Occupation Interpretation Of Quasars At $z\sim1.5$ Using Very Small Scale Clustering Information

Authors: S. Eftekharzadeh, A. D. Myers, E. Kourkchi

Comments: Submitted to MNRAS. Please cross check with the published version when citing the content

Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO)

[55]  arXiv:1812.08910 (replaced) [pdf, other]

Title: Constraining nuclear matter parameters with GW170817

Authors: Zack Carson, Andrew W. Steiner, Kent Yagi

Comments: 15 pages, 14 figures; Updated the section on computing the EoS scattering uncertainty to include a more comprehensive error analysis; Fixed issue with incorrect EoSs plotted in Fig. 3; Fixed a small mistake on nuclear matter bounds

Journal-ref: Phys. Rev. D 99, 043010 (2019)

Subjects: General Relativity and Quantum Cosmology (gr-qc); High Energy Astrophysical Phenomena (astro-ph.HE)

[56]  arXiv:1901.03448 (replaced) [pdf, other]

Title: The Lazy Giants: APOGEE Abundances Reveal Low Star Formation Efficiencies in the Magellanic Clouds

Authors: David L. Nidever, Sten Hasselquist, Christian R. Hayes, Keith Hawkins, Joshua Povick, Steven R. Majewski, Verne V. Smith, Borja Anguiano, Guy S. Stringfellow, Jennifer S. Sobeck, Katia Cunha, Timothy C. Beers, Joachim M. Bestenlehner, Roger E. Cohen, D. A. Garcia-Hernandez, D. A. Garcia-Hernandez, Henrick Jonsson, Christian Nitschelm, Matthew Shetrone, Ivan Lacerna, Carlos Allende Prieto, Rachael L. Beaton, Flavia Dell'Agli, Jose G. Fernandez-Trincado, Diane Fuillet, Carme Gallart, Fred R. Hearty, Jon Holtzman, Arturo Manchado, Ricardo R. Munoz, Robert O'Connell, Margarita Rosado

Comments: 22 pages, 20 figues, 1 table, accepted for publication in ApJ

Subjects: Astrophysics of Galaxies (astro-ph.GA)

[57]  arXiv:1903.11083 (replaced) [pdf, other]

Title: Probing the extragalactic fast transient sky at minute timescales with DECam

Authors: Igor Andreoni, Jeffrey Cooke, Sara Webb, Armin Rest, Tyler A. Pritchard, Manisha Caleb, Seo-Won Chang, Wael Farah, Amy Lien, Anais Möller, Maria Edvige Ravasio, Timothy M. C. Abbott, Shivani Bhandari, Antonino Cucchiara, Christopher M. Flynn, Fabian Jankowski, Evan F. Keane, Takashi J. Moriya, Christopher Onken, Aditya Parthasarathy, Daniel C. Price, Emily Petroff, Stuart Ryder, Dany Vohl, Christian Wolf

Comments: Published in MNRAS

Journal-ref: Monthly Notices of the Royal Astronomical Society (2020), Volume 491, Issue 4, p.5852-5866

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Astrophysics of Galaxies (astro-ph.GA); Instrumentation and Methods for Astrophysics (astro-ph.IM); Solar and Stellar Astrophysics (astro-ph.SR)

[58]  arXiv:1904.01699 (replaced) [pdf, other]

Title: Resolution Study for Three-dimensional Supernova Simulations with the Prometheus-Vertex Code

Authors: Tobias Melson, Daniel Kresse, H.-Thomas Janka (MPI Astrophysics, Garching)

Comments: 37 pages, 14 figures, 4 tables; revised version with neutrino drag discussion extended for numerical evaluation; accepted by ApJ

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

[59]  arXiv:1905.08890 (replaced) [pdf, other]

Title: GRAMSES: a new route to general relativistic $N$-body simulations in cosmology. Part I. Methodology and code description

Authors: Cristian Barrera-Hinojosa, Baojiu Li

Comments: 40 pages, 11 figures. Matches published version

Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); General Relativity and Quantum Cosmology (gr-qc)

[60]  arXiv:1906.00997 (replaced) [pdf, other]

Title: The Effective Field Theory of Large Scale Structure at Three Loops

Authors: Thomas Konstandin, Rafael A. Porto, Henrique Rubira

Comments: 25 pages, 15 figs

Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); General Relativity and Quantum Cosmology (gr-qc); High Energy Physics - Theory (hep-th)

[61]  arXiv:1906.07209 (replaced) [pdf, other]

Title: POEMMA's Target of Opportunity Sensitivity to Cosmic Neutrino Transient Sources

Authors: Tonia M. Venters, Mary Hall Reno, John F. Krizmanic, Luis A. Anchordoqui, Claire Guépin, Angela V. Olinto

Comments: 33 pages (17.5 main + 15.5 appendices and references), 15 figures; submitted to Phys. Rev. D

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics - Phenomenology (hep-ph)

[62]  arXiv:1907.04145 (replaced) [pdf, other]

Title: Feasibility of Cosmic Microwave Background Observations using Radiometers based on Whispering Gallery Mode Resonators

Authors: Javier De Miguel-Hernández, Roger J. Hoyland

Comments: 24 pages, 5 figs

Journal-ref: Early acces; New Astronomy 2020 (NEWAST)

Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM); Optics (physics.optics)

[63]  arXiv:1908.01622 (replaced) [pdf, other]

Title: The HiSPARC Experiment

Authors: K. van Dam, B. van Eijk, D.B.R.A. Fokkema, J.W. van Holten, A.P.L.S. de Laat, N.G. Schultheiss, J.J.M. Steijger, J.C. Verkooijen

Comments: Accepted for publication in NIM A

Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM); High Energy Astrophysical Phenomena (astro-ph.HE)

[64]  arXiv:1908.02326 (replaced) [pdf, other]

Title: Pileups and Migration Rates for Planets in Low Mass Disks

Authors: Adam M. Dempsey, Wing-Kit Lee, Yoram Lithwick

Comments: 27 pages, 17 figures, accepted to ApJ

Subjects: Earth and Planetary Astrophysics (astro-ph.EP)

[65]  arXiv:1908.05042 (replaced) [pdf, ps, other]

Title: Understanding CMB physics through the exploration of exotic cosmological models: a classroom study using CLASS

Authors: Tanja Rindler-Daller

Comments: Proof-read, final version; accepted by European Journal of Physics; 21 pages, 5 figures

Subjects: Physics Education (physics.ed-ph); Cosmology and Nongalactic Astrophysics (astro-ph.CO)

[66]  arXiv:1908.07099 (replaced) [pdf, ps, other]

Title: The Third Data Release of the Beijing-Arizona Sky Survey

Authors: Hu Zou, Xu Zhou, Xiaohui Fan, Tianmeng Zhang, Zhimin Zhou, Xiyan Peng, Jundan Nie, Linhua Jiang, Ian McGreer, Zheng Cai, Guangwen Chen, Xinkai Chen, Arjun Dey, Dongwei Fan, Joseph R. Findlay, Jinghua Gao, Yizhou Gu, Yucheng Guo, Boliang He, Zhaoji Jiang, Junjie Jin, Xu Kong, Dustin Lang, Fengjie Lei, Michael Lesser, Feng Li, Zefeng Li, Zesen Lin, Jun Ma, Moe Maxwell, Xiaolei Meng, Adam D. Myers, Yuanhang Ning, David Schlegel, Yali Shao, Dongdong Shi, Fengwu Sun, Jiali Wang, Shu Wang, Yonghao Wang, Peng Wei, Hong Wu, Jin Wu, Xiaohan Wu, Jinyi Yang, Qian Yang, Qirong Yuan, Minghao Yue

Comments: published in ApJS

Subjects: Astrophysics of Galaxies (astro-ph.GA); Instrumentation and Methods for Astrophysics (astro-ph.IM)

[67]  arXiv:1908.09599 (replaced) [pdf, ps, other]

Title: The ExoTETHyS package: Tools for Exoplanetary Transits around Host Stars

Authors: Giuseppe Morello, Antonio Claret, Marine Martin-Lagarde, Christophe Cossou, Angelos Tsiaras, Pierre-Olivier Lagage

Comments: published on the AJ

Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Instrumentation and Methods for Astrophysics (astro-ph.IM); Solar and Stellar Astrophysics (astro-ph.SR)

[68]  arXiv:1909.03116 (replaced) [pdf, ps, other]

Title: Photometric imaging with the solar gravitational lens

Authors: Slava G. Turyshev, Viktor T. Toth

Comments: 11 pages, 4 figures

Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM); General Relativity and Quantum Cosmology (gr-qc); Optics (physics.optics)

[69]  arXiv:1909.10523 (replaced) [pdf, other]

Title: Rapid Transients Originating from Thermonuclear Explosions in Helium White Dwarf Tidal Disruption Events

Authors: Kojiro Kawana, Keiichi Maeda, Naoki Yoshida, Ataru Tanikawa

Comments: 9 pages, 5 figures, accepted to ApJL

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

[70]  arXiv:1909.11094 (replaced) [pdf, other]

Title: How sound are our ultra-light axion approximations?

Authors: Jonathan Cookmeyer, Daniel Grin, Tristan L. Smith

Comments: 22 pages, 16 figures, comments are welcome, updated to align all language with version published in Phys. Rev. D. Results unchanged, additional details on numerical methods provided

Journal-ref: Phys. Rev. D 101, 023501 (2020)

Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); General Relativity and Quantum Cosmology (gr-qc); High Energy Physics - Phenomenology (hep-ph)

[71]  arXiv:1909.12149 (replaced) [pdf, ps, other]

Title: First detection of the Crab Nebula at TeV energies with a Cherenkov telescope in a dual-mirror Schwarzschild-Couder configuration: the ASTRI-Horn telescope

Authors: S. Lombardi, O. Catalano, S. Scuderi, L. A. Antonelli, G. Pareschi, E. Antolini, L. Arrabito, G. Bellassai, K. Bernloehr, C. Bigongiari, B. Biondo, G. Bonanno, G. Bonnoli, G. M. Bottcher, J. Bregeon, P. Bruno, R. Canestrari, M. Capalbi, P. Caraveo, P. Conconi, V. Conforti, G. Contino, G. Cusumano, M. de Gouveia Dal Pino, A. Distefano, G. Farisato, C. Fermino, M. Fiorini, A. Frigo, S. Gallozzi, C. Gargano, S. Garozzo, F. Gianotti, S. Giarrusso, R. Gimenes, E. Giro, A. Grillo, D. Impiombato, S. Incorvaia, N. La Palombara, V. La Parola, G. La Rosa, G. Leto, F. Lucarelli, M. C. Maccarone, D. Marano, E. Martinetti, A. Micciche, R. Millul, T. Mineo, G. Nicotra, G. Occhipinti, I. Pagano, M. Perri, G. Romeo, F. Russo, F. Russo, B. Sacco, P. Sangiorgi, F. G. Saturni, A. Segreto, G. Sironi, G. Sottile, et al. (30 additional authors not shown)

Comments: 6 pages, 2 figures

Journal-ref: A&A 634, A22 (2020)

Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM); High Energy Astrophysical Phenomena (astro-ph.HE)

[72]  arXiv:1910.00016 (replaced) [pdf, other]

Title: Binary white dwarfs and decihertz gravitational wave observations: From the Hubble constant to supernova astrophysics

Authors: Andrea Maselli, Stefania Marassi, Marica Branchesi

Comments: Results updated to match the version in press on A&A

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); General Relativity and Quantum Cosmology (gr-qc)

[73]  arXiv:1910.10226 (replaced) [pdf, other]

Title: Joint analysis of EDGES $21$-cm line observations with standard candles and rulers in $Λ$CDM and non-adiabatic gCg models

Authors: C. Pigozzo, S. Carneiro, J. C. Fabris

Comments: Revised version to appear in Physics of the Dark Universe

Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); General Relativity and Quantum Cosmology (gr-qc)

[74]  arXiv:1910.13326 (replaced) [pdf, other]

Title: Gravitational wave propagation beyond geometric optics

Authors: Giulia Cusin, Macarena Lagos

Comments: Version accepted for publication

Subjects: General Relativity and Quantum Cosmology (gr-qc); Cosmology and Nongalactic Astrophysics (astro-ph.CO)

[75]  arXiv:1910.13654 (replaced) [pdf, other]

Title: Layered Uncertainty in Planetary Thermal History Models: Implications for Hypotheses Discrimination and Habitability Modeling

Authors: Johnny Seales, Adrian Lenardic

Comments: Preprint

Subjects: Earth and Planetary Astrophysics (astro-ph.EP)

[76]  arXiv:1911.05105 (replaced) [pdf, ps, other]

Title: Large-scale dynamo action of magnetized Taylor-Couette flows

Authors: G. Rüdiger, M. Schultz

Comments: 12 pages, 12 figures

Subjects: Solar and Stellar Astrophysics (astro-ph.SR); Fluid Dynamics (physics.flu-dyn)

[77]  arXiv:1911.05230 (replaced) [pdf, other]

Title: Structure of Multicomponent Coulomb Crystals

Authors: M. E. Caplan

Comments: 10 pages, 8 figures, accepted to PRE

Subjects: Soft Condensed Matter (cond-mat.soft); High Energy Astrophysical Phenomena (astro-ph.HE); Materials Science (cond-mat.mtrl-sci); Nuclear Theory (nucl-th)

[78]  arXiv:1911.08092 (replaced) [pdf, ps, other]

Title: Emergence of life in an inflationary universe

Authors: Tomonori Totani

Comments: 9 pages, 1 figure. matches the published version from Scientific Reports

Subjects: Populations and Evolution (q-bio.PE); Cosmology and Nongalactic Astrophysics (astro-ph.CO); Earth and Planetary Astrophysics (astro-ph.EP); Biomolecules (q-bio.BM)

[79]  arXiv:1911.09555 (replaced) [pdf, ps, other]

Title: A Case Study of the May 30th, 2017 Italian Fireball

Authors: A. Carbognani, D. Barghini, D. Gardiol, M. di Martino, G. B. Valsecchi, P. Trivero, A. Buzzoni, S. Rasetti, D. Selvestrel, C. Knapic, E. Londero, S. Zorba, C. A. Volpicelli, M. Di Carlo, J. Vaubaillon, C. Marmo, F. Colas, D. Valeri, F. Zanotti, M. Morini, P. Demaria, B. Zanda, S. Bouley, P. Vernazza, J. Gattacceca, J.-L. Rault, L. Maquet, M. Birlan

Comments: 19 pages, 17 figures. Accepted for publication in The European Physical Journal PLUS

Subjects: Earth and Planetary Astrophysics (astro-ph.EP)

[80]  arXiv:1911.11975 (replaced) [pdf, other]

Title: Inclination Dependence of The Time-Lag -- Photon-Index Correlation in BHXRBs and its Explanation with a Simple Jet Model

Authors: N. Kylafis (Univ of Crete, Inst. of Astrophysics-FORTH), P. Reig (Inst. of Astrophysics-FORTH, Univ of Crete)

Comments: Work presented at: High Energy Phenomena in Relativistic Outflows VII - HEPRO VII, 9-12 July 2019 Facultat de F\'isica, Universitat de Barcelona, Spain

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

[81]  arXiv:1911.12621 (replaced) [pdf, other]

Title: Real-time flare prediction based on distinctions between flaring and non-flaring active region spectra

Authors: Brandon Panos, Lucia Kleint

Subjects: Solar and Stellar Astrophysics (astro-ph.SR)

[82]  arXiv:1912.01653 (replaced) [pdf, other]

Title: Primordial black holes and gravitational waves in non-standard cosmologies

Authors: Sukannya Bhattacharya, Subhendra Mohanty, Priyank Parashari

Comments: 17 pages, 7 figures

Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Physics - Phenomenology (hep-ph)

[83]  arXiv:1912.02599 (replaced) [pdf, other]

Title: The mass of our Milky Way

Authors: Wenting Wang, Jiaxin Han, Marius Cautun, Zhaozhou Li, Miho N. Ishigaki

Comments: invited review to appear in Science China Physics, Mechanics & Astronomy

Subjects: Astrophysics of Galaxies (astro-ph.GA); Cosmology and Nongalactic Astrophysics (astro-ph.CO)

[84]  arXiv:2001.00055 (replaced) [pdf, other]

Title: Deflating Super-Puffs: Impact of Photochemical Hazes on the Observed Mass-Radius Relationship of Low Mass Planets

Authors: Peter Gao, Xi Zhang

Comments: 32 pages, 25 figures, and 2 tables. Accepted for publication in ApJ

Subjects: Earth and Planetary Astrophysics (astro-ph.EP)

[85]  arXiv:2001.02358 (replaced) [pdf, other]

Title: Characterization of unresolved and unclassified sources detected in radio continuum surveys of the Galactic plane

Authors: Arnab Chakraborty, Nirupam Roy, Y.Wang, Abhirup Datta, H. Beuther, S.-N.X. Medina, K. M. Menten, J. S. Urquhart, A. Brunthaler, S. A. Dzib

Comments: There are 6 pages and 3 figures. The paper is accepted for publication in MNRAS (DOI : 10.1093/mnras/stz3621)

Subjects: Astrophysics of Galaxies (astro-ph.GA); Cosmology and Nongalactic Astrophysics (astro-ph.CO)

[86]  arXiv:2001.03595 (replaced) [pdf, other]

Title: Nine New Repeating Fast Radio Burst Sources from CHIME/FRB

Authors: E. Fonseca, B. C. Andersen, M. Bhardwaj, P. Chawla, D. C. Good, A. Josephy, V. M. Kaspi, K. W. Masui, R. Mckinven, D. Michilli, Z. Pleunis, K. Shin, S. P. Tendulkar, K. M. Bandura, P. J. Boyle, C. Brar, T. Cassanelli, D. Cubranic, M. Dobbs, F. Q. Dong, B. M. Gaensler, G. Hinshaw, T. L. Landecker, C. Leung, D. Z. Li, H.-H. Lin, J. Mena-Parra, M. Merryfield, A. Naidu, C. Ng, C. Patel, U. Pen, M. Rafiei-Ravandi, M. Rahman, S. M. Ransom, P. Scholz, K. M. Smith, I. H. Stairs, K. Vanderlinde, P. Yadav, A. V. Zwaniga

Comments: Accepted for publication in ApJL

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

[87]  arXiv:2001.05355 (replaced) [pdf, ps, other]

Title: Constraining the nuclear equation of state via gravitational-wave radiation of short gamma-ray burst remnants

Authors: Lin Lan, Hou-Jun Lü, Jared Rice, En-Wei Liang

Comments: 7 pages, 1 table, and 4 figures. ApJ in press, matched the published version

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics - Phenomenology (hep-ph)

[88]  arXiv:2001.06501 (replaced) [pdf, other]

Title: The better half -- Asymmetric star-formation due to ram pressure in the EAGLE simulations

Authors: P. Troncoso-Iribarren, N. Padilla, C. Santander, C.D.P. Lagos, D. García-Lambas, S. Rodriguez, S. Contreras

Subjects: Astrophysics of Galaxies (astro-ph.GA)

[89]  arXiv:2001.08790 (replaced) [pdf, other]

Title: The MUSE-Faint survey: I. Spectroscopic evidence for a star cluster in Eridanus 2 and constraints on MACHOs as a constituent of dark matter

Authors: Sebastiaan L. Zoutendijk (1), Jarle Brinchmann (2 and 1), Leindert A. Boogaard (1), Madusha L. P. Gunawardhana (1), Tim-Oliver Husser (3), Sebastian Kamann (4), Andrés Felipe Ramos Padilla (1), Martin M. Roth (5), Roland Bacon (6), Mark den Brok (5), Stefan Dreizler (3), Davor Krajnović (5) ((1) Leiden Observatory, Leiden University, Leiden, The Netherlands, (2) Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Porto, Portugal, (3) Institute for Astrophysics, Georg-August-University, Göttingen, Germany, (4) Astrophysics Research Institute, Liverpool John Moores University, Liverpool, United Kingdom, (5) Leibniz-Institut für Astrophysik Potsdam (AIP), Potsdam, Germany, (6) Univ. Lyon, Univ. Lyon1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon, Saint-Genis-Laval, France)

Comments: 17 pages, 12 figures, 3 tables. 1 electronic table included in source. Accepted for publication in A&A. New in this version: correction to author list

Subjects: Astrophysics of Galaxies (astro-ph.GA)

[90]  arXiv:2001.09829 (replaced) [pdf, other]

Title: Common-Envelope Episodes that lead to Double Neutron Star formation

Authors: Alejandro Vigna-Gómez, Morgan MacLeod, Coenraad J. Neijssel, Floor S. Broekgaarden, Stephen Justham, George Howitt, Selma E. de Mink, Ilya Mandel

Comments: 20 pages, 9 figures, submitted version. Figure two updated. Email address fixed

Subjects: Solar and Stellar Astrophysics (astro-ph.SR); High Energy Astrophysical Phenomena (astro-ph.HE)

[91]  arXiv:2001.10011 (replaced) [pdf, other]

Title: LISA parameter estimation and source localization with higher harmonics of the ringdown

Authors: Vishal Baibhav, Emanuele Berti, Vitor Cardoso

Comments: 19 pages, 15 figures, 2 tables. v2: references added, replaced Fig. 1

Subjects: General Relativity and Quantum Cosmology (gr-qc); High Energy Astrophysical Phenomena (astro-ph.HE)

[92]  arXiv:2001.10275 (replaced) [pdf, other]

Title: Periodic activity from a fast radio burst source

Authors: The CHIME/FRB Collaboration, M. Amiri, B. C. Andersen, K. M. Bandura, M. Bhardwaj, P. J. Boyle, C. Brar, P. Chawla, T. Chen, J. F. Cliche, D. Cubranic, M. Deng, N. T. Denman, M. Dobbs, F. Q. Dong, M. Fandino, E. Fonseca, B. M. Gaensler, U. Giri, D. C. Good, M. Halpern, J. W. T. Hessels, A. S. Hill, C. Höfer, A. Josephy, J. W. Kania, R. Karuppusamy, V. M. Kaspi, A. Keimpema, F. Kirsten, T. L. Landecker, D. A. Lang, C. Leung, D. Z. Li, H. -H. Lin, B. Marcote, K. W. Masui, R. Mckinven, J. Mena-Parra, M. Merryfield, D. Michilli, N. Milutinovic, A. Mirhosseini, A. Naidu, L. B. Newburgh, C. Ng, K. Nimmo, Z. Paragi, C. Patel, U. -L. Pen, T. Pinsonneault-Marotte, Z. Pleunis, M. Rafiei-Ravandi, M. Rahman, S. M. Ransom, A. Renard, P. Sanghavi, P. Scholz, J. R. Shaw, K. Shin, S. R. Siegel, S. Singh, et al. (11 additional authors not shown)

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

[93]  arXiv:2001.10697 (replaced) [pdf, ps, other]

Title: Estimating the Jet Power of Mrk\,231 During the 2017-2018 Flare

Authors: Cormac Reynolds, Brian Punsly, Giovanni Miniutti, Christopher P. O'Dea, Natasha Hurley-Walker

Comments: Accepted version for ApJ

Subjects: Astrophysics of Galaxies (astro-ph.GA)

[94]  arXiv:2001.10879 (replaced) [pdf, other]

Title: 2MASS J15491331-3539118: a new low-mass wide companion of the GQ Lup system

Authors: J. M. Alcalá, F. Z. Majidi, S. Desidera, A. Frasca, C. F. Manara, E. Rigliaco, R. Gratton, M. Bonnefoy, E. Covino, G. Chauvin, R. Claudi, V. D'Orazi, M. Langlois, C. Lazzoni, D. Mesa, J.E. Schlieder, A. Vigan

Comments: 8 pages, 8 figures

Subjects: Solar and Stellar Astrophysics (astro-ph.SR); Earth and Planetary Astrophysics (astro-ph.EP); Astrophysics of Galaxies (astro-ph.GA)

[95]  arXiv:2001.10952 (replaced) [pdf, other]

Title: Concerns about ground based astronomical observations: a step to safeguard the astronomical sky

Authors: Stefano Gallozzi (1), Marco Scardia (2), Michele Maris (3) ((1) INAF-Osservatorio Astronomico di Roma, (2) INAF-Osservatorio Astronomico di Brera, (3) INAF-Osservatorio Astronomico di Trieste)

Comments: 16 pages, 6 figures, 2 tables

Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM)

[96]  arXiv:2001.11199 (replaced) [pdf, ps, other]

Title: Gaia's Detectability of Black Hole-Main Sequence Star Binaries Formed in Open Clusters

Authors: Minori Shikauchi, Jun Kumamoto, Ataru Tanikawa, Michiko S. Fujii

Comments: 10 pages, 9 figures, submitted to PASJ

Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Astrophysics of Galaxies (astro-ph.GA); Solar and Stellar Astrophysics (astro-ph.SR)

[97]  arXiv:2001.11378 (replaced) [pdf, other]

Title: Site testing campaign for the Large Optical/infrared Telescope of China: Overview

Authors: Lu Feng, Jin-Xin Hao, Zi-Huang Cao, Jin-Min Bai, Ji Yang, Xu Zhou, Yong-Qiang Yao, Jin-Liang Hou, Yong-Heng Zhao, Yu Liu, Teng-Fei Song, Li-Yong Liu, Jia Yin, Hua-Lin Chen, Chong Pei, Ali Esamdin, Lu Ma, Chun-Hai Bai, Peng Wei, Jing Xu, Guang-Xin Pu, Guo-Jie Feng, Xuan Zhang, Liang Ming, Abudusaimaitijiang Yisikandee, Jian-Rong Shi, Jian Li, Yuan Tian, Zheng Wang, Xia Wang, Xiao-Jun Jiang, Jian-Feng Wang, Jian-Feng Tian, Yan-Jie Xue, Jian-Sheng Chen, Jing-Yao Hu, Zhi-Xia Shen, Yun-Ying Jiang

Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM)

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