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New submissions for Fri, 27 Mar 20

[1]  arXiv:2003.11548 [pdf, other]

Title: Why is it so Cold in Here?: Explaining the Cold Temperatures Retrieved from Transmission Spectra of Exoplanet Atmospheres

Authors: Ryan J. MacDonald, Jayesh M. Goyal, Nikole K. Lewis

Comments: 16 pages, 4 figures. Accepted for publication in ApJL

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

Transmission spectroscopy is a powerful technique widely used to probe exoplanet terminators. Atmospheric retrievals of transmission spectra are enabling comparative studies of exoplanet atmospheres. However, the atmospheric properties inferred by retrieval techniques display a significant anomaly: most retrieved temperatures are far colder than expected. In some cases, retrieved temperatures are ~1000 K colder than T_eq. Here, we provide an explanation for this conundrum. We demonstrate that erroneously cold temperatures result when 1D atmospheric models are applied to spectra of planets with differing morning-evening terminator compositions. Despite providing an acceptable fit, 1D retrieval techniques artificially tune atmospheric parameters away from terminator-averaged properties. Retrieved temperature profiles are hundreds of degrees cooler and have weaker temperature gradients than reality. Retrieved abundances are mostly biased by > 1$\sigma$ and sometimes by > 3$\sigma$, with the most extreme biases for ultra-hot Jupiters. When morning-evening compositional differences manifest for prominent opacity sources, H$_2$O abundances retrieved by 1D models can be biased by over an order of magnitude. Finally, we demonstrate that these biases provide an explanation for the cold retrieved temperatures reported for WASP-17b and WASP-12b. To overcome biases associated with 1D atmospheric models, there is an urgent need to develop multidimensional retrieval techniques.

[2]  arXiv:2003.11549 [pdf, other]

Title: Age-chemical abundance structure of the Galaxy I: Evidence for a late accretion event in the outer disc at z ~ 0.6

Authors: Jianhui Lian (University of Utah), Daniel Thomas (University of Portsmouth), Claudia Maraston (University of Portsmouth), Olga Zamora, Jamie Tayar, Kaike Pan, Patricia Tissera, José G. Fernández-Trincado, Domingo Anibal Garcia-Hernandez

Comments: 17 pages, 11 figures, accepted for publication in MNRAS

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

We investigate the age-chemical abundance structure of the outer Galactic disc at a galactocentric distance of r > 10 kpc as recently revealed by the SDSS/APOGEE survey. Two sequences are present in the [alpha/Fe]-[Fe/H] plane with systematically different stellar ages. Surprisingly, the young sequence is less metal-rich, suggesting a recent dilution process by additional gas accretion. As the stars with the lowest iron abundance in the younger sequence also show an enhancement in alpha-element abundance, the gas accretion event must have involved a burst of star formation. In order to explain these observations, we construct a chemical evolution model. In this model we include a relatively short episode of gas accretion at late times on top of an underlying secular accretion over long timescales. Our model is successful at reproducing the observed distribution of stars in the three dimensional space of [alpha/Fe]-[Fe/H]-Age in the outer disc. We find that a late-time accretion with a delay of 8.2 Gyr and a timescale of 0.7 Gyr best fits the observed data, in particular the presence of the young, metal-poor sequence. Our best-fit model further implies that the amount of accreted gas in the late-time accretion event needs to be about three times the local gas reservoir in the outer disc at the time of accretion in order to sufficiently dilute the metal abundance. Given this large fraction, we interpret the late-time accretion event as a minor merger presumably with a gas-rich dwarf galaxy with a mass M_* < 10^9 M_Sun and a gas fraction of ~ 75 per cent.

[3]  arXiv:2003.11551 [pdf, other]

Title: Constraining VLBI-optical offsets in high redshift galaxies using strong gravitational lensing

Authors: C. Spingola, A. Barnacka

Comments: 16 pages, 7 figures; accepted for publication in MNRAS

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

We present a multi-wavelength analysis of two highly magnified strong gravitationally lensed galaxies, CLASS B0712+472 and CLASS B1608+656, at redshifts $1.34$ and $1.394$, respectively, using new VLBI and archival HST observations. We reconstruct the positions of the radio and optical emissions with their uncertainties using Monte Carlo sampling. We find that in CLASS B0712+472 the optical and radio emissions are co-spatial within $2\pm5$ mas ($17\pm 42$ pc at redshift of 1.34). But, in CLASS B1608+656, we reconstruct an optical-radio offset of $25\pm16$ mas ($214\pm137$ pc at redshift of 1.394), the smallest offset measured for an AGN at such high redshift. The spectral features indicate that CLASS B1608+656 is a post-merger galaxy, which, in combination with the optical-VLBI offset reported here, makes CLASS B1608+656 a promising candidate for a high-$z$ offset-AGN. Furthermore, the milliarcsecond angular resolution of the VLBI observations combined with the precise lens models allow us to spatially locate the radio emission at $0.05$ mas precision ($0.4$ pc) in CLASS B0712+472, and $0.009$ mas precision ($0.08$ pc) in CLASS B1608+656. The search for optical-radio offsets in high redshift galaxies will be eased by the upcoming synoptic all-sky surveys, including E-ELT and SKA, which are expected to find $\sim 10^5$ strongly lensed galaxies, opening an era of large strong lensing samples observed at high angular resolution.

[4]  arXiv:2003.11555 [pdf, other]

Title: Clusters Have Edges: The Projected Phase SpaceStructure of SDSS redMaPPer Clusters

Authors: Paxton Tomooka, Eduardo Rozo, Erika L. Wagoner, Han Aung, Daisuke Nagai, Sasha Safonova

Comments: 10 pages, 5 figures, submitted to MNRAS, companion paper to Aung et al. 2020

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

We study the distribution of line-of-sight velocities of galaxies in the vicinity of SDSS redMaPPer galaxy clusters. Based on their velocities, galaxies can be split into two categories: galaxies that are dynamically associated with the cluster, and random line-of-sight projections. Both the fraction of galaxies associated with the galaxy clusters, and the velocity dispersion of the same, exhibit a sharp feature as a function of radius. The feature occurs at a radial scale $R_{\rm edge} \approx 2.2R_{\rm{\lambda}}$, where $R_{\rm{\lambda}}$ is the cluster radius assigned by redMaPPer. We refer to $R_{\rm edge}$ as the "edge radius." These results are naturally explained by a model that further splits the galaxies dynamically associated with a galaxy cluster into a component of galaxies orbiting the halo and an infalling galaxy component. The edge radius $R_{\rm edge}$ constitutes a true "cluster edge", in the sense that no orbiting structures exist past this radius. A companion paper (Aung et al. 2020) tests whether the "halo edge" hypothesis holds when investigating the full three-dimensional phase space distribution of dark matter substructures in numerical simulations, and demonstrates that this radius coincides with a suitably defined splashback radius.

[5]  arXiv:2003.11557 [pdf, other]

Title: The Phase Space Structure of Dark Matter Halos

Authors: Han Aung, Daisuke Nagai, Eduardo Rozo, Rafael Garcia

Comments: 7 pages, 5 figures, submitted to MNRAS, companion paper to Tomooka et al. 2020

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

The phase space structure of dark matter halos can be used to measure the mass of the halo, infer mass accretion rates, and probe the effects of modified gravity. Previous studies showed that the splashback radius can be measured in position space using the slope of the density profile. Using N-body simulations, we show that the phase space structure of the dark matter halo does not end at this splashback radius. Instead, there exists a region where infalling, splashback, and virialized halos are mixed spatially. We model the distribution of the three kinematically distinct populations and show that there exists an "edge radius" beyond which a dark matter halo has no orbiting substructures. This radius is a fixed multiple of the splashback radius as defined in previous works, and can be interpreted as a radius which contains a fixed fraction of the apocenters of dark matter particles. Our results provide a firm theoretical foundation to the satellite galaxy model adopted in the companion paper by Tomooka et al., where we analyzed the phase space distribution of SDSS redMaPPer clusters.

[6]  arXiv:2003.11558 [pdf, other]

Title: Source Distributions of Cosmic Shear Surveys in Efficiency Space

Authors: Nicolas Tessore, Ian Harrison

Comments: 6 pages, 9 figures; notebook available at this https URL, comments welcome

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

We show that the lensing efficiency of cosmic shear generically has a simple shape, even in the case of a tomographic survey with badly behaved photometric redshifts. We argue that source distributions for cosmic shear can therefore be more effectively parametrised in "efficiency space". Using realistic simulations, we find that the true lensing efficiency of a current cosmic shear survey without disconnected outliers in the redshift distributions can be described to per cent accuracy with only two parameters, and the approach straightforwardly generalises to other parametric forms and surveys. The cosmic shear signal is thus largely insensitive to the details of the source distributions, and the features that matter can be summarised by a small number of suitable efficiency parameters. For the simulated survey, we show that prior knowledge at the ten per cent level, which is attainable e.g. from photometric redshifts, is enough to marginalise over the efficiency parameters without severely affecting the constraints on the cosmology parameters $\Omega_m$ and $\sigma_8$.

[7]  arXiv:2003.11574 [pdf, ps, other]

Title: Stellar Inclination Angles from Be Star H$α$ Emission-Line Profiles

Authors: T. A. A. Sigut, A. K. Mahjour, C. Tycner

Comments: 19 pages, 23 figures, accepted for publication in The Astrophysical Journal

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

We demonstrate that the angle between star's rotation axis and the observer's line-of-sight, usually called the inclination angle, can be reliably determined for Be stars via H$\alpha$ emission-line profile fitting. We test our method on a sample of 11 Be stars with available long-baseline interferometric data from the Navy Precision Optical Interferometer~(NPOI). We fit the H$\alpha$ emission line profile of each star to obtain a spectroscopic inclination angle $i_{\rm H\alpha}$. We then obtain an independent inclination angle estimate, $i_{\rm V^2}$, by fitting the observed interferometric visibilities with model visibilities based on a purely geometric representation of the light distribution on the sky. The sample differences, $\Delta i \equiv i_{\rm H\alpha} - i_{\rm V^2}$, are normally distributed with a mean of zero and a standard deviation of $6.7$ degrees, and the linear correlation coefficient between $i_{\rm H\alpha}$ and $i_{\rm V^2}$ is $r=0.93$. As Be stars comprise upwards of one fifth of all main-sequence B-type stars, this H$\alpha$ line profile fitting technique has the potential to provide an efficient method for detecting correlated stellar spin axes in young open clusters. Furthermore, if the orientation of the Be star circumstellar disk on the plane of the sky can be constrained by polarization measurements, it is possible to determine the full 3D stellar rotation vector of each Be star.

[8]  arXiv:2003.11585 [pdf, other]

Title: The role of wind driving in OB star bow nebulae

Authors: Curtis Struck (Iowa State)

Comments: 11 pages, 3 figures, accepted for MNRAS

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

Bow-shaped mid-infrared emission regions have been discovered in satellite observations of numerous late-type O and early-type B stars with moderate velocities relative to the ambient interstellar medium. Previously, hydrodynamical bow shock models have been used to study this emission. It appears that such models are incomplete in that they neglect kinetic effects associated with long mean free paths of stellar wind particles, and the complexity of Weibel instability fronts. Wind ions are scattered in the Weibel instability and mix with the interstellar gas. However, they do not lose their momentum and most ultimately diffuse further into the ambient gas like cosmic rays, and share their energy and momentum. Lacking other coolants, the heated gas transfers energy to interstellar dust grains, which radiate it. This process, in addition to grain photo-heating, provides the energy for the emission. A weak R-type ionization front, formed well outside the infrared emission region, generally moderates the interstellar gas flow into the emission region. The theory suggests that the infrared emission process is limited to cases of moderate stellar peculiar velocities, evidently in accord with the observations.

[9]  arXiv:2003.11590 [pdf, other]

Title: Transit Duration Variations in Multi-Planet Systems

Authors: Aaron C. Boley, Christa Van Laerhoven, Agueda Paula Granados Contreras

Comments: To appear in AJ

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

A planet's orbital orientation relative to an observer's line of sight determines the chord length for a transiting planet, i.e., the projected distance a transiting planet travels across the stellar disc. For a given circular orbit, the chord length determines the transit duration. Changes in the orbital inclination, the direction of the ascending node, or both, can alter this chord length and thus result in transit duration variations (TDVs). Variation of the full orbital inclination vector can even lead to de-transiting or newly transiting planets for a system. We use Laplace-Lagrange secular theory to estimate the fastest nodal eigenfrequencies for over 100 short-period planetary systems. The highest eigenfrequency is an indicator of which systems should show the strongest TDVs. We further explore five cases (TRAPPIST-1, Kepler-11, K2-138, Kepler-445, and Kepler-334) using direct N-body simulations to characterize possible TDVs and to explore whether de-transiting planets could be possible for these systems. A range of initial conditions are explored, with each realization being consistent with the observed transits. We find that tens of percent of multiplanet systems have fast enough eigenfrequencies to expect large TDVs on decade timescales. Among the directly integrated cases, we find that de-transiting planets could occur on decade timescales and TDVs of 10 minutes per decade should be common.

[10]  arXiv:2003.11609 [pdf, ps, other]

Title: Chemical abundance analysis of extremely metal-poor stars in the Sextans dwarf spheroidal galaxy

Authors: Misa Aoki, Wako Aoki, Patrick Francois

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

Metal-poor components of dwarf galaxies around the Milky Way could be remnants of the building blocks of the Galactic halo structure. Low-mass stars that are currently observed as metal-poor stars are expected to have formed in chemically homogeneous clusters in the early phases of galaxy formation. They should have already disintegrated and should exhibit large scatter in abundance ratios of some sets of elements (e.g., Sr/Ba) in the Milky Way field stars. However, chemical abundance ratios are expected to cluster in very metal-poor stars in dwarf galaxies because the number of clusters formed in individual galaxies in the very early phase is expected to be quite limited. We examine the possible clustering of abundance ratios of Sr and Ba in the Sextans dwarf galaxy to test for the clustering star formation scenario. We investigate a total of 11 elements (C, Mg, Ca, Sc, Ti, Cr, Mn, Ni, Zn, Sr, Ba) in five stars in the Sextans dwarf galaxy. Previous studies suggest that these have similar abundance ratios. In this study, we focus on the abundance ratio of Sr to Ba. The observations are based on high-resolution spectroscopy (R = 40 000) using the Subaru Telescope High Dispersion Spectrograph. The distribution of $\alpha$/Fe abundance ratios of the Sextans dwarf galaxy stars is slightly lower than the average of the values of stars in the Galactic halo. The Sr/Ba abundance ratios for the five metal-poor stars are in good agreement, and this clumping is distinctive compared to the [Sr/Ba] spread seen in the metal-poor halo stars. We find that the probability of such clumping is very small if the Sextans stars have distributions of Sr and Ba abundances similar to halo stars.

[11]  arXiv:2003.11682 [pdf, other]

Title: Earth-size planet formation in the habitable zone of circumbinary stars

Authors: G. O. Barbosa, O. C. Winter, A. Amarante, A. Izidoro, R. C. Domingos, E. E. N. Macau

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

In this work is investigated the possibility of close-binary star systems having Earth-size planets within their habitable zones. First, we selected all known close-binary systems with confirmed planets (totaling 22 systems) to calculate the boundaries of their respective habitable zones (HZ). However, only eight systems had all the data necessary for the computation of the HZ. Then, we numerically explored the stability within the habitable zones for each one of the eight systems using test particles. From the results, we selected five systems that have stable regions inside the habitable zones (HZ), namely Kepler-34, 35, 38, 413 and 453. For these five cases of systems with stable regions in the HZ, we perform a series of numerical simulations for planet formation considering disks composed of planetary embryos and planetesimals, with two distinct density profiles, in addition to the stars and host planets of each system. We found that in the case of Kepler-34 and 453 systems no Earth-size planet is formed within the habitable zones. Although planets with Earth-like masses were formed in the Kepler-453, but they were outside the HZ. In contrast, for Kepler-35 and 38 systems, the results showed that potentially habitable planets are formed in all simulations. In the case of the Kepler-413 system, in just one simulation a terrestrial planet was formed within the habitable zone.

[12]  arXiv:2003.11725 [pdf, ps, other]

Title: Discovery of two nearby post-T Tauri stellar associations

Authors: Jiaming Liu, Chao Liu, Min Fang

Comments: 13pages, 8 figures, 2 tables, accepted for publishing in AJ

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

In this work we report the discovery of 2 new stellar associations in close vicinity of the Sun at roughly 180 and 150 pc. These two associations, named as u Tau assoc and e Tau assoc, were detected based on their clustering in a multi-dimensional parameter space including ${\alpha}$, ${\delta}$, ${\mu}_{\alpha}$ , ${\mu}_{\delta}$ and ${\pi}$ of Gaia. The fitting of pre-main-sequence model isochrones in their color-magnitude diagrams suggests that the two associations are of about 50 Myr old and the group members lower than ${\sim}$0.8 $M_{\odot}$ are at the stage of post-T Tauri.

[13]  arXiv:2003.11730 [pdf, ps, other]

Title: NuSTAR Detection of Quiescent Hard X-Ray Emission from SGR 0526-66 in the Large Magellanic Cloud

Authors: Sangwook Park, Jayant Bhalerao (University of Texas at Arlington), Oleg Kargaltsev (George Washington University), Patrick O. Slane (SAO)

Comments: 7 pages (ApJ emulator format), 1 table, 3 figures, accepted by ApJ

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

The soft gamma-ray repeater (SGR) 0526-66 is the first-identified magnetar, and is projected within the supernova remnant N49 in the Large Magellanic Cloud. Based on our ~50 ks NuSTAR observation, we detect the quiescent-state 0526-66 for the first time in the 10-40 keV band. Based on the joint analysis of our NuSTAR and the archival Chandra ACIS data, we firmly establish the presence of the nonthermal component in the X-ray spectrum of 0526-66 in addition to the thermal emission. In the best-fit blackbody (BB) plus power law (PL) model, the slope of the PL component (photon index Gamma = 2.1) is steeper than those (Gamma > ~1.5) for other magnetars. The soft part of the X-ray spectrum can be described with a BB component with the temperature of kT = 0.43 keV. The best-fit radius (R = 6.5 km) of the X-ray-emitting area is smaller than the canonical size of a neutron star. If we assume an underlying cool BB component with the canonical radius of R = 10 km for the neutron star in addition to the hot BB component (2BB + PL model), a lower BB temperature of kT = 0.24 keV is obtained for the passively cooling neutron star'ssurface, while the hot spot emission with kT = 0.46 keV dominates the thermal spectrum (~85% of the thermal luminosity in the 0.5-5 keV band). The nonthermal component (Gamma ~ 1.8) is still required.

[14]  arXiv:2003.11732 [pdf]

Title: Habitability of polar regions in tidally locked extrasolar planet near the M-Dwarf stars

Authors: Nishith Burman

Comments: 4 pages

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

Since the launch of Kepler and Hubble more than a decade ago, we have come a long way in the quest to find a potentially habitable exoplanet. To date, we have already discovered more than 4000 exoplanets most of which are not suitable for sustaining life. Of all those that can potentially sustain life, A large number has been found rotating synchronously around their parent star, mostly Red dwarf star. Due to their synchronous rotation, these planets receive very uneven stellar heating. Synchronous rotation of these planets causes one side of the planet to permanently face the parent star while the other side remains dark. This results in an extreme climatic condition that is not feasible for sustaining life. Although these theories about exoplanets are well known, a systemic study of habitability of polar regions within an exoplanet using different climate models has not been done yet. Here I review the current literature on tidal locking and its impact on habitability and introduce the concept of habitability in the poles of these exoplanets. I focus on my understanding of the climatic condition in the polar region of the earth and based on that I present the concept of habitability in the poles of these exoplanets.

[15]  arXiv:2003.11747 [pdf, ps, other]

Title: A White-light Flare Powered by Magnetic Reconnection in the Lower Solar Atmosphere

Authors: Yongliang Song, Hui Tian, Xiaoshuai Zhu, Yajie Chen, Mei Zhang, Jingwen Zhang

Comments: 14 pages,5 figures,accepted for publication by ApJL

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

White-light flares (WLFs), first observed in 1859, refer to a type of solar flares showing an obvious enhancement of the visible continuum emission. This type of enhancement often occurs in most energetic flares, and is usually interpreted as a consequence of efficient heating in the lower solar atmosphere through non-thermal electrons propagating downward from the energy release site in the corona. However, this coronal-reconnection model has difficulty in explaining the recently discovered small WLFs. Here we report a C2.3 white-light flare, which are associated with several observational phenomena: fast decrease in opposite-polarity photospheric magnetic fluxes, disappearance of two adjacent pores, significant heating of the lower chromosphere, negligible increase of hard X-ray flux, and an associated U-shaped magnetic field configuration. All these suggest that this white-light flare is powered by magnetic reconnection in the lower part of the solar atmosphere rather than by reconnection higher up in the corona.

[16]  arXiv:2003.11770 [pdf, other]

Title: A Shining Death of Unequal Supermassive Black Hole Binaries

Authors: Xian Chen, D. N. C. Lin, Xiaojia Zhang

Comments: 6 pages, 2 figures, accepted for publication in ApJ Letters

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

In the $\Lambda$CDM scenario, small galaxies merge to produce larger entities. Since supermassive black holes (SMBHs) are found in galaxies of all sizes, SMBH binaries (SMBHBs) are generally expected to form during the amalgamation of galaxies. It is unclear what fraction of these binaries could eventually merge, but a general consensus is that initially the orbital decay is mediated by the surrounding gas and stars. In this Letter, we show that in active galactic nulcei (AGNs) the radiation field also causes the orbits of the accreting SMBHs to shrink. The corresponding mechanism, known as the "Poynting-Robertson drag" (PR drag), takes effect on a well-defined timescale $CT_{\rm Sal}$, where $T_{\rm Sal}$ is the Salpeter timescale of the AGN, presumably coincide with the primary SMBH, and $C=4\xi^{-1}\epsilon^{-1}q^{1/3}(1+q)^{2/3}(1-\epsilon)$ is a constant determined by the radiative efficiency $\epsilon$, the mass ratio $q$ of the two black holes, and a parameter $\xi$ characterizing the size of the circum-secondary accretion disk. We find that when $q\lesssim$a few$\times10^{-5}$, the PR drag is more efficient in shrinking the binary than many other mechanisms, such as dynamical friction and type-I migration. Our finding points to a possible new channel for the coalescence of unequal SMBHBs and the clearing of intermediate-massive black holes in AGNs.

[17]  arXiv:2003.11788 [pdf, other]

Title: A model exploration of NIR ro-vibrational CO emission as a tracer of inner cavities in protoplanetary disks

Authors: S. Antonellini, A. Banzatti, I. Kamp, W.-F. Thi, P. Woitke

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

Near-IR observations of protoplanetary disks provide information about the properties of the inner disk. High resolution spectra of abundant molecules such as CO can be used to determine the disk structure in the warm inner parts. The $v2/v1$ ro-vibrational ratio of $v_{1-0}$ and $v_{2-1}$ transitions has been recently observed to follow distinct trends with the CO emitting radius, in a sample of TTauri and Herbig disks; these trends have been empirically interpreted as due to inner disk depletion from gas and dust. In this work we use existing thermo-chemical disk models to explore the interpretation of these observed trends in ro-vibrational CO emission. We use the radiation thermo-chemical code ProDiMo, exploring a set of previously published models with different disk properties and varying one parameter at a time: the inner radius, the dust-to-gas mass ratio, the gas mass. In addition, we use models where we change the surface density power law index, and employ a larger set of CO ro-vibrational levels, including also fluorescence from the first electronic state. We investigate these models for both TTauri and Herbig star disks. Finally, we include a set of DIANA models for individual TTauri and Herbig disks which were constructed to reproduce a large set of multi-wavelength observations.

[18]  arXiv:2003.11819 [pdf, other]

Title: An underground Sagnac gyroscope with sub-prad/s rotation rate sensitivity: toward General Relativity tests on Earth

Authors: Angela D.V. Di Virgilio, Filippo Bosi, Umberto Giacomelli, Andrea Simonelli, Giuseppe Terreni, Andrea Basti, Nicolo' Beverini, Giorgio Carelli, Donatella Ciampini, Francesco Fuso, Enrico Maccioni, Paolo Marsili, Antonello Ortolan, Alberto Porzio

Comments: 7 pages, 5 figures

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

Measuring in a single location on Earth its angular rotation rate with respect to the celestial frame, with a sensitivity enabling access to the tiny Lense-Thirring effect is an extremely challenging task. GINGERINO is a large frame ring laser gyroscope, operating free running and unattended inside the underground laboratory of the Gran Sasso, Italy. The main geodetic signals, i.e., Annual and Chandler wobbles, daily polar motion and Length of the Day, are recovered from GINGERINO data using standard linear regression methods, demonstrating a sensitivity better than 1 prad/s, therefore close to the requirements for an Earth-based Lense-Thirring test.

[19]  arXiv:2003.11888 [pdf]

Title: Breakdown products of gaseous polycyclic aromatic hydrocarbons investigated with infrared ion spectroscopy

Authors: A. Petrignani, M. Vala, J.R. Eyler, A.G.G.M. Tielens, G. Berden, A.F.G. van der Meer, B. Redlich, J. Oomens

Journal-ref: The Astrophysical Journal, 826, 2016, 33

Subjects: Astrophysics of Galaxies (astro-ph.GA); Chemical Physics (physics.chem-ph)

We report on a common fragment ion formed during the electron-ionization-induced fragmentation of three different three-ring polycyclic aromatic hydrocarbons (PAHs), fluorene (C$_{13}$H$_{10}$), 9,10-dihydrophenanthrene (C$_{14}$H$_{12}$), and 9,10-dihydroanthracene (C$_{14}$H$_{12}$). The infrared spectra of the mass-isolated product ions with $m/z=165$ were obtained in a Fourier transform ion cyclotron resonance mass spectrometer whose cell was placed inside the optical cavity of an infrared free-electron laser, thus providing the high photon fluence required for efficient infrared multiple-photon dissociation. The infrared spectra of the $m/z=165$ species generated from the three different precursors were found to be similar, suggesting the formation of a single C$_{13}$H$_{9}^+$ isomer. Theoretical calculations using density functional theory (DFT) revealed the fragment's identity as the closed-shell fluorenyl cation. Decomposition pathways from each parent precursor to the fluorenyl ion are proposed on the basis of DFT calculations. The identification of a single fragmentation product from three different PAHs supports the notion of the existence of common decomposition pathways of PAHs in general and can aid in understanding the fragmentation chemistry of astronomical PAH species.

[20]  arXiv:2003.11889 [pdf, other]

Title: Side-On transition radiation detector: a detector prototype for TeV energy scale calibration of calorimeters in space

Authors: Bo Huang, Hongbang Liu, Xuefeng Huang, Ming Xu, Yongwei Dong, Xiaotong Wei, Xiwen Liu, Huanbo Feng, Qinhe Yang, Jianyu Gu, Shuai Chen, Xiaochuan Xie, Jin Zhang, Yongbo Huang, Enwei Liang

Comments: 13 pages, 10 figures, 2 tables

Journal-ref: Nuclear Inst. and Methods in Physics Research, A 962 (2020) 163723

Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM); Instrumentation and Detectors (physics.ins-det)

Transition Radiation (TR) plays an important role in particle identification in high-energy physics and its characteristics provide a feasible method of energy calibration in the energy range up to 10 TeV, which is of interest for dark matter searches in cosmic rays. In a Transition Radiation Detector (TRD), the TR signal is superimposed onto the ionization energy loss signal induced by incident charged particles. In order to make the TR signal stand out from the background of ionization energy loss in a significant way, we optimized both the radiators and the detector. We have designed a new prototype of regular radiator optimized for a maximal TR photon yield, combined with the Side-On TRD which is supposed to improve the detection efficiency of TR. We started a test beam experiment with the Side-On TRD at Conseil Europ\'{e}en pour la Recherche Nucl\'{e}aire (CERN), and found that the experimental data is consistent with the simulation results.

[21]  arXiv:2003.11899 [pdf, ps, other]

Title: Progress in the development of frequency domain multiplexing for the X-ray Integral Field Unit on board the Athena mission

Authors: H. Akamatsu, L. Gottardi, J. van der Kuur, C.P. de Vries, M.P. Bruijn, J.A. Chervenak, M. Kiviranta, A.J. van den Linden, B.D. Jackson, A. Miniussi, K. Ravensberg, K. Sakai, S.J. Smith, N. Wakeham

Comments: 7 pages, 5 figures. Published on Journal of Low Temperature Physics (2020)

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

Frequency domain multiplexing (FDM) is the baseline readout system for the X-ray Integral Field Unit (X-IFU) on board the Athena mission. Under the FDM scheme, TESs are coupled to a passive LC filter and biased with alternating current (AC bias) at MHz frequencies. Using high-quality factor LC filters and room temperature electronics developed at SRON and low-noise two-stage SQUID amplifiers provided by VTT, we have recently demonstrated good performance with the FDM readout of Mo/Au TES calorimeters with Au/Bi absorbers. We have achieved a performance requested for the demonstration model (DM) with the single pixel AC bias ($\Delta E=$1.8 eV) and 9 pixel multiplexing ($\Delta E=$2.6 eV) modes. We have also demonstrated 14-pixel multiplexing with an average energy resolution of 3.3 eV, which is limited by non-fundamental issues related to FDM readout in our lab setup.

[22]  arXiv:2003.11930 [pdf, other]

Title: An explanation of the repetition/pulse width relation in FRBs

Authors: L. Connor, M.C. Miller, D.W. Gardenier

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

It is currently not known if repeating fast radio bursts (FRBs) are fundamentally different from those that have not been seen to repeat. One striking difference between repeaters and apparent non-repeaters in the CHIME sample is that the once-off events are typically shorter in duration than sources that have been detected two or more times. We offer a simple explanation for this discrepancy based on a selection effect due to beamed mission, in which highly-beamed FRBs are less easily observed to repeat, but are abundant enough to detect often as once-off events. The explanation predicts that there is a continuous distribution of burst duration---not a bimodal one---with a correlation between repetition rate and width. Pulse width and opening angle may be related by relativistic effects in shocks, where short-duration bursts have small solid angles due to a large common Lorentz factor. Alternatively, the relationship could be a geometric effect where narrow beams sweep past the observer more quickly, as with pulsars. Our model has implications for the FRB emission mechanism and energy scale, volumetric event rates, and the application of FRBs to cosmology. It also provides a way of predicting which sources could be seen to repeat in the future.

[23]  arXiv:2003.11937 [pdf, ps, other]

Title: Rotation-activity relations and flares of M dwarfs with K2 long- and short-cadence data

Authors: St. Raetz, B. Stelzer, M. Damasso, A. Scholz

Comments: 23 pages, 26 figures, 7 tables

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

Using light curves obtained by the K2 mission, we study the relation between stellar rotation and magnetic activity with special focus on stellar flares. Our sample comprises 56 bright and nearby M dwarfs observed by K2 during campaigns C0-C18 in long- and short-cadence mode. We derive rotation periods for 46 M dwarfs and measure photometric activity indicators such as amplitude of the rotational signal, standard deviation of the light curves, and the basic flare properties (flare rate, flare energy, flare duration, and flare amplitude). We found 1662 short-cadence flares, 363 of which have a long-cadence counterpart with flare energies of up to $5.6\cdotp10^{34}$erg. The flare amplitude, duration, and frequency derived from the short-cadence light curves differ significantly from those derived from the long-cadence data. The analysis of the short-cadence light curves results in a flare rate that is 4.6 times higher than the long-cadence data. We confirm the abrupt change in activity level in the rotation-activity relation at a critical period of ~10d when photometric activity diagnostics are used. This change is most drastic in the flare duration and frequency for short-cadence data. Our flare studies revealed that the highest flare rates are not found among the fastest rotators and that stars with the highest flare rates do not show the most energetic flares. We found that the superflare frequency ($E\geq5\cdotp10^{34}$erg) for the fast-rotating M stars is twice higher than for solar like stars in the same period range. By fitting the cumulative FFD, we derived a power-law index of $\alpha=1.84 \pm 0.14$, consistent with previous M dwarf studies and the value found for the Sun.

[24]  arXiv:2003.11970 [pdf, ps, other]

Title: Efficient search of optimal Flower Constellations

Authors: Martín Avendaño, David Arnas, Richard Linares, Miles Lifson

Comments: 9 pages

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

We derive an analytical closed expression to compute the minimum distance (quantified by the angle of separation measured from the center of the Earth) between any two satellites located at the same altitude and in circular orbits. We also exploit several properties of Flower Constellations (FCs) that, combined with our formula for the distance, give an efficient method to compute the minimum angular distance between satellites, for all possible FCs with up to a given number of satellites.

[25]  arXiv:2003.11976 [pdf, ps, other]

Title: Does a solar filament barb always correspond to a prominence foot?

Authors: Y. Ouyang, P. F. Chen, S. Q. Fan, B. Li, A. A. Xu

Comments: 12 pages, 3 figures, accepted for publication in ApJ

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

Solar filaments are dark structures on the solar disk, with an elongated spine and several barbs extending out from the spine. When appearing above the solar limb, a filament is called a prominence, with with several feet extending down to the solar surface. It was generally thought that filament barbs are simply the prominence feet veering away from the spine and down to the solar surface. However, it was recently noticed that there might be another dynamic type of barbs, which were proposed to be due to filament thread longitudinal oscillation. If this is the case, the dynamic barbs would not extend down to the solar surface. With the quadrature observations of a filament barb on 2011 June 5 from the {\it Solar Dynamics Observatory} and the {\it STEREO} satellites, we confirm that the filament barb is due to filament thread longitudinal oscillations. Viewed from the side, the filament barb looks like an appendix along the spine of the prominence, and does not extend down to the solar surface as a foot.

[26]  arXiv:2003.11980 [pdf, other]

Title: The Planetary Luminosity Problem: "Missing Planets" and the Observational Consequences of Episodic Accretion

Authors: Sean D. Brittain, Joan R. Najita, Ruobing Dong, Zhaohuan Zhu

Comments: 17 pages, 2 figures, accepted by ApJ

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

The high occurrence rates of spiral arms and large central clearings in protoplanetary disks, if interpreted as signposts of giant planets, indicate that gas giants form commonly as companions to young stars ($<$ few Myr) at orbital separations of 10--300\,au. However, attempts to directly image this giant planet population as companions to more mature stars ($> 10$\, Myr) have yielded few successes. This discrepancy could be explained if most giant planets form "cold start," i.e., by radiating away much of their formation energy as they assemble their mass, rendering them faint enough to elude detection at later times. In that case, giant planets should be bright at early times, during their accretion phase, and yet forming planets are detected only rarely through direct imaging techniques. Here we explore the possibility that the low detection rate of accreting planets is the result of episodic accretion through a circumplanetary disk. We also explore the possibility that the companion orbiting the Herbig Ae star HD~142527 may be a giant planet undergoing such an accretion outburst.

[27]  arXiv:2003.12033 [pdf, ps, other]

Title: Properties of X-ray detected far-IR AGN in the green valley

Authors: Antoine Mahoro, Mirjana Pović, Petri Väisänen, Pheneas Nkundabakura, Beatrice Nyiransengiyumva, Kurt van der Heyden

Comments: Proceedings paper of the IAU symposium "Nuclear Activity in Galaxies Across Cosmic Time" (Ethiopia) accepted to be published under the Cambridge University Press, eds. M. Povic, P. Marziani, J. Masegosa, H. Netzer, S. H. Negu, and S. B. Tessema

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

In this study, we analysed active galactic nuclei in the "green valley" by comparing active and non-active galaxies using data from the COSMOS field. We found that most of our X-ray detected active galactic nuclei with far-infrared emission have star formation rates higher than the ones of normal galaxies of the same stellar mass range.

Cross-lists for Fri, 27 Mar 20

[28]  arXiv:2003.11748 (cross-list from gr-qc) [pdf, other]

Title: On arrival time difference between lensed gravitational waves and light

Authors: Teruaki Suyama

Comments: 3 pages

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

It is known that geometrical optics no longer applies to the gravitational lensing if the wavelength of a propagating wave becomes comparable to or larger than the Schwarzshild radius of a lensing object. We investigate the propagation of gravitational waves in wave optics, particularly focusing on the difference between their arrival time and the arrival time of light. We argue that, contrary to the observation in the previous work, gravitational waves never arrive at an observer earlier than light when both gravitational waves and light are emitted from a same source simultaneously.

[29]  arXiv:2003.11831 (cross-list from gr-qc) [pdf, ps, other]

Title: Massive gravity with non-minimal coupling

Authors: A. Emir Gumrukcuoglu, Rampei Kimura, Kazuya Koyama

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

We propose new massive gravity theories with 5 dynamical degrees of freedom. We evade uniqueness theorems regarding the form of the kinetic and potential terms by adopting the "generalized massive gravity" framework, where a global translation invariance is broken. By exploiting the rotation symmetry in the field space, we determine two novel classes of theories. The first one is an extension of generalized massive gravity with a non-minimal coupling. On the other hand, the second theory produces a mass term that is different from de Rham, Gabadadze, Tolley construction and trivially has 5 degrees of freedom. Both theories allows for stable cosmological solutions without infinite strong coupling, which are free of ghost and gradient instabilities.

[30]  arXiv:2003.11901 (cross-list from gr-qc) [pdf, other]

Title: Gravitational waves and mass ejecta from binary neutron star mergers: Effect of the spin orientation

Authors: Swami Vivekanandji Chaurasia, Tim Dietrich, Maximiliano Ujevic, Kai Hendriks, Reetika Dudi, Francesco Maria Fabbri, Wolfgang Tichy, Bernd Brügmann

Comments: 17 pages, 15 figures

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

We continue our study of the binary neutron star parameter space by investigating the effect of the spin orientation on the dynamics, gravitational wave emission, and mass ejection during the binary neutron star coalescence. We simulate seven different configurations using multiple resolutions to allow a reasonable error assessment. Due to the particular choice of the setups, five configurations show precession effects, from which two show a precession (`wobbling') of the orbital plane, while three show a `bobbing' motion, i.e., the orbital angular momentum does not precess, while the orbital plane moves along the orbital angular momentum axis. Considering the ejection of mass, we find that precessing systems can have an anisotropic mass ejection, which could lead to a final remnant kick of about $\sim 40 \rm km/s$ for the studied systems. Furthermore, for the chosen configurations, anti-aligned spins lead to larger mass ejecta than aligned spins, so that brighter electromagnetic counterparts could be expected for these configurations. Finally, we compare our simulations with the precessing, tidal waveform approximant IMRPhenomPv2_NRTidalv2 and find good agreement between the approximant and our numerical relativity waveforms with phase differences below 1.2 rad accumulated over the last $\sim$ 16 gravitational wave cycles.

[31]  arXiv:2003.11983 (cross-list from physics.optics) [pdf, other]

Title: A vignetting advantage for thin-film filter arrays in hyperspectral cameras

Authors: Thomas Goossens, Bert Geelen, Andy Lambrechts, Chris Van Hoof

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

Vignetting in camera lenses is generally seen as something to avoid. For spectral cameras with thin-film interference filters, however, we argue that vignetting can be an advantage. When illuminated by focused light, the bandwidth of interference filters increases with the chief-ray angle, causing position-dependent smoothing of the spectra. We show that vignetting can be used to reduce smoothing and preserve important spectral features. Furthermore, we demonstrate that by adding additional vignetting to a lens, measurements can be made more consistent across the scene. This makes vignetting a useful parameter during spectral camera design.

[32]  arXiv:2003.12057 (cross-list from hep-ph) [pdf, other]

Title: Resolving Hubble Tension by Self-Interacting Neutrinos with Dirac Seesaw

Authors: Hong-Jian He, Yin-Zhe Ma, Jiaming Zheng

Comments: 23 pages

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

Self-interacting neutrinos that begin to free-stream at close to matter-radiation equality can reduce the physical size of photon sound horizon at last scattering surface. This can be the reason why standard $\Lambda$CDM cosmology sees a lower value of Hubble constant than local measurements from distance ladder. We propose a new realization of self-interacting Dirac neutrinos (SID$\nu$) with light dark photon mediator for a viable interaction mechanism. Our model is UV completed by a Dirac seesaw with anomaly-free dark $U(1)_X^{}$ gauge group which charges the right-handed neutrinos. This naturally generates small masses for Dirac neutrinos and induces self-scattering of right-handed neutrinos. The scattering with left-handed neutrinos is suppressed by a chirality-flip mass insertion when the neutrino energy is much larger than its mass. The resultant neutrino self-scattering is not operative for $E_{\nu}\gtrsim O(\text{keV})$, which avoids the cosmological and laboratory constraints. By evolving Boltzmann equations for left- and right-handed neutrino number densities, we show that about $2/3$ of the left-handed neutrinos are converted into right-handed neutrinos in a short epoch between the Big-Bang Nucleosynthesis and the recombination, and interact with each other efficiently afterwards. The resultant neutrino non-free-streaming is the key ingredient to shrink down the comoving sound horizon at drag epoch, which can reconcile the Hubble tension between early and late time measurements.

Replacements for Fri, 27 Mar 20

[33]  arXiv:1902.10488 (replaced) [pdf, other]

Title: Ghostly Galaxies as Solitons of Bose-Einstein Dark Matter

Authors: Tom Broadhurst, Ivan de Martino, Hoang Nhan Luu, George F. Smoot, S.-H. Henry Tye

Comments: 9 pages, 5 figure. Accepted for publication on Physical Review D

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

[34]  arXiv:1903.02159 (replaced) [pdf, other]

Title: Track length measurement of $^{19}$F$^+$ ions with the MIMAC Dark Matter directional detector prototype

Authors: Y. Tao, C. Beaufort, I. Moric, C. Tao, D. Santos, N. Sauzet, C. Couturier, O. Guillaudin, J.F. Muraz, F. Naraghi, N. Zhou, J. Busto

Comments: 17 pages, 10 figures

Subjects: Instrumentation and Detectors (physics.ins-det); Instrumentation and Methods for Astrophysics (astro-ph.IM); High Energy Physics - Experiment (hep-ex)

[35]  arXiv:1904.07504 (replaced) [pdf, other]

Title: Nebular Line Emission During the Epoch of Reionization

Authors: Stephen M. Wilkins, Christopher C. Lovell, Ciaran Fairhurst, Yu Feng, Tiziana Di Matteo, Rupert Croft, Jussi Kuusisto, Aswin P. Vijayan, Peter Thomas

Comments: 17 pages, accepted to MNRAS, significant modification from v1.0 data available at this https URL

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

[36]  arXiv:1905.05769 (replaced) [pdf, other]

Title: The Photon Spectrum of Asymmetric Dark Stars

Authors: Andrea Maselli, Chris Kouvaris, Kostas D. Kokkotas

Comments: New results. Improved analysis on the photon spectrum production

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

[37]  arXiv:1908.08404 (replaced) [pdf, ps, other]

Title: ALMA CO Observations of a Giant Molecular Cloud in M33: Evidence for High-Mass Star Formation Triggered by Cloud-Cloud Collisions

Authors: Hidetoshi Sano, Kisetsu Tsuge, Kazuki Tokuda, Kazuyuki Muraoka, Kengo Tachihara, Yumiko Yamane, Mikito Kohno, Shinji Fujita, Rei Enokiya, Gavin Rowell, Nigel Maxted, Miroslav D. Filipovic, Jonathan Knies, Manami Sasaki, Toshikazu Onishi, Paul P. Plucinsky, Yasuo Fukui

Comments: 13 pages, 10 figures, 1 table, submitted to the Publications of the Astronomical Society of Japan (PASJ)

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

[38]  arXiv:1908.08477 (replaced) [pdf, other]

Title: Using SPTpol, Planck 2015, and non-CMB data to constrain tilted spatially-flat and untilted non-flat $Λ$CDM, XCDM, and $φ$CDM dark energy inflation cosmologies

Authors: Chan-Gyung Park, Bharat Ratra

Comments: 26 pages, 14 figures, 7 tables. Accepted for publication in Physical Review D

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

[39]  arXiv:1909.04681 (replaced) [pdf, other]

Title: Interferometric Closure Phase Uncertainties in the Low Signal-to-Noise Ratio Regime

Authors: Pierre Christian, Dimitrios Psaltis

Comments: Matches accepted version

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

[40]  arXiv:1909.08016 (replaced) [pdf, other]

Title: Validating the methodology for constraining the linear growth rate from clustering anisotropies

Authors: Jorge Enrique García-Farieta, Federico Marulli, Lauro Moscardini, Alfonso Veropalumbo, Rigoberto A. Casas-Miranda

Comments: 17 pages, 14 figures, 1 table

Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); Instrumentation and Methods for Astrophysics (astro-ph.IM)

[41]  arXiv:1909.09212 (replaced) [pdf, other]

Title: RELICS: Spectroscopy of gravitationally-lensed $z\simeq 2$ reionization-era analogs and implications for CIII] detections at $z>6$

Authors: Ramesh Mainali, Daniel P Stark, Mengtao Tang, Jacopo Chevallard, Stéphane Charlot, Keren Sharon, Dan Coe, Brett Salmon, Larry D. Bradley, Traci L. Johnson, Brenda Frye, Roberto J. Avila, Sara Ogaz, Adi Zitrin, Maruša Bradač, Brian C. Lemaux, Guillaume Mahler, Rachel Paterno-Mahler, Victoria Strait, Felipe Andrade-Santos

Comments: Accepted for publication in MNRAS

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

[42]  arXiv:1911.00323 (replaced) [pdf, other]

Title: Swampland, Axions and Minimal Warm Inflation

Authors: Suratna Das, Gaurav Goswami, Chethan Krishnan

Comments: v2: Improved model, all constraints now comfortably satisfied. Semi-analytic arguments double-checked using explicit numerical evolution. Refs and discussions added

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

[43]  arXiv:1911.08070 (replaced) [pdf, other]

Title: Constraints on Lorentz invariance violation from HAWC observations of gamma rays above 100 TeV

Authors: HAWC Collaboration: A. Albert, R. Alfaro, C. Alvarez, J.R. Angeles Camacho, J.C. Arteaga-Velázquez, K.P. Arunbabu, D. Avila Rojas, H.A. Ayala Solares, V. Baghmanyan, E. Belmont-Moreno, S.Y. BenZvi, C. Brisbois, K.S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, C. de León, B.L. Dingus, M.A. DuVernois, J.C. Díaz-Vélez, R.W. Ellsworth, K. Engel, C. Espinoza, H. Fleischhack, N. Fraija, A. Galván-Gámez, D. Garcia, J.A. García-González, F. Garfias, M.M. González, J.A. Goodman, J.P. Harding, S. Hernandez, B. Hona, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, W.H. Lee, H. León Vargas, J.T. Linnemann, A.L. Longinotti, et al. (44 additional authors not shown)

Comments: Accepted for publication in Physical Review Letters

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

[44]  arXiv:1911.13296 (replaced) [pdf, other]

Title: The SOPHIE search for northern extrasolar planets. XVI. HD 158259: A compact planetary system in a near-3:2 mean motion resonance chain

Authors: N. C. Hara, F. Bouchy, M. Stalport, I. Boisse, J. Rodrigues, J-. B. Delisle, A. Santerne, G. W. Henry, L. Arnold, N. Astudillo-Defru, S. Borgniet, X.Bonfils, V. Bourrier, B. Brugger, B. Courcol, S. Dalal, M. Deleuil, X. Delfosse, O. Demangeon, R. F. D'iaz, X. Dumusque, T. Forveille, G. Hébrard, M. Hobson, F. Kiefer, T. Lopez, L. Mignon, O. Mousis, C. Moutou, F. Pepe, J. Rey, N. C. Santos, D. Ségransan, S. Udry, P. A. Wilson

Comments: Accepted for publication in Astronomy & Astrophysics

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

[45]  arXiv:1912.01518 (replaced) [pdf, ps, other]

Title: Effects of the general relativistic spin precessions on the habitability of rogue planets orbiting supermassive black holes

Authors: Lorenzo Iorio

Comments: LaTex2e, 19 pages, 7 figures, no tables. Changes suggested by a referee implemented

Subjects: Earth and Planetary Astrophysics (astro-ph.EP); General Relativity and Quantum Cosmology (gr-qc); Popular Physics (physics.pop-ph); Space Physics (physics.space-ph)

[46]  arXiv:1912.08301 (replaced) [pdf, other]

Title: The PDFI_SS Electric Field Inversion Software

Authors: George H. Fisher, Maria D. Kazachenko, Brian T. Welsch, Xudong Sun, Erkka Lumme, David J. Bercik, Marc L. DeRosa, Mark C. M. Cheung

Comments: 67 pages, 28 figures, 3 tables. Accepted for publication in the Astrophysical Journal Supplements Series

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

[47]  arXiv:1912.09726 (replaced) [pdf, other]

Title: TeV Scale Leptogenesis with Dark Matter in Non-standard Cosmology

Authors: Devabrat Mahanta, Debasish Borah

Comments: 45 pages, 22 figures, matches version accepted for publication in JCAP

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

[48]  arXiv:1912.13208 (replaced) [pdf, other]

Title: Cosmological consequences of a scalar field with oscillating equation of state: A possible solution to the fine-tuning and coincidence problems

Authors: S. X. Tián

Comments: 7 pages, 3 figures, matches published version

Journal-ref: Phys. Rev. D 101, 063531 (2020)

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

[49]  arXiv:2001.00394 (replaced) [pdf, other]

Title: Viable Gauge Choices in Cosmologies with Non-Linear Structures

Authors: Timothy Clifton, Christopher S. Gallagher, Sophia Goldberg, Karim A. Malik

Comments: 15 pages, 2 figures

Journal-ref: Phys. Rev. D 101, 063530 (2020)

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

[50]  arXiv:2001.08770 (replaced) [pdf, ps, other]

Title: Wind-reprocessed Transients

Authors: Anthony L. Piro (Carnegie Observatories), Wenbin Lu (Caltech)

Comments: 13 pages, 7 figures, version accepted for publication in ApJ, added panel to Figure 7 and short discussion on the X-ray production efficiency of AT2018cow

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

[51]  arXiv:2001.10852 (replaced) [pdf, other]

Title: All-inclusive interacting dark sector cosmologies

Authors: Weiqiang Yang, Eleonora Di Valentino, Olga Mena, Supriya Pan, Rafael C. Nunes

Comments: 15 pages, 8 Tables, 8 captioned Figures, accepted for publication in PRD

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

[52]  arXiv:2002.02840 (replaced) [pdf, other]

Title: Occurrence and Architecture of Kepler Planetary Systems as Functions of Stellar Mass and Effective Temperature

Authors: Jia-Yi Yang (Nanjing), Ji-Wei Xie (Nanjing), Ji-Lin Zhou (Nanjing)

Comments: 25 pages, 21 figures, 2 tables, accepted for publication in AJ

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

[53]  arXiv:2002.10364 (replaced) [pdf, ps, other]

Title: Revisiting the 2PN pericentre precession in view of possible future measurements of it

Authors: Lorenzo Iorio

Comments: Latex2e, 25 pages, 2 figures, no tables. Some equations for expressing E,h in terms of a,e to the PN level added

Subjects: General Relativity and Quantum Cosmology (gr-qc); Earth and Planetary Astrophysics (astro-ph.EP); Space Physics (physics.space-ph)

[54]  arXiv:2003.03390 (replaced) [pdf, other]

Title: Most Stars (and Planets?) Are Born in Intense Radiation Fields

Authors: Eve J. Lee, Philip F. Hopkins

Comments: MNRAS Letters in press

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

[55]  arXiv:2003.03634 (replaced) [pdf, other]

Title: The redshift and the host galaxy of the neutrino candidate 4FGL J0955.1+3551 (3HSP J095507.9+355101)

Authors: Simona Paiano, Renato Falomo, Paolo Padovani, Paolo Giommi, Adriana Gargiulo, Michela Uslenghi, Andrea Rossi, Aldo Treves

Comments: 4 pages, 4 figures, accepted to MNRAS

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

[56]  arXiv:2003.04304 (replaced) [pdf, ps, other]

Title: Canonical Analysis of Brans-Dicke Theory Addresses Hamiltonian Inequivalence between Jordan and Einstein Frames

Authors: Gabriele Gionti, S.J

Comments: 12 pages, letter, latex. Minor corrections and some references added

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

[57]  arXiv:2003.04783 (replaced) [pdf, other]

Title: Probing the inflationary background of gravitational waves from large to small scales

Authors: William Giarè, Alessandro Melchiorri

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

[58]  arXiv:2003.08508 (replaced) [pdf, other]

Title: An Application of Gaussian Process Modeling for High-order Accurate Adaptive Mesh Refinement Prolongation

Authors: Steven I. Reeves, Dongwook Lee, Adam Reyes, Carlo Graziani, Petros Tzeferacos

Subjects: Numerical Analysis (math.NA); Instrumentation and Methods for Astrophysics (astro-ph.IM); Fluid Dynamics (physics.flu-dyn)

[59]  arXiv:2003.09659 (replaced) [pdf]

Title: Narrowband large amplitude whistler-mode waves in the solar wind and their association with electrons: STEREO waveform capture observations

Authors: C. A. Cattell, B. Short, A.W. Breneman, P.Grul

Comments: astro-ph.EP - Earth and Planetary Astrophysics

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

[60]  arXiv:2003.09776 (replaced) [pdf, ps, other]

Title: Characteristic masses in galaxy quenching: environmental versus internal effects

Authors: Pengfei Li, Huiyuan Wang, H.J. Mo, Enci Wang, Hui Hong

Comments: 7 pages, 4 figures, submitted to AAS

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

[61]  arXiv:2003.10035 (replaced) [pdf, ps, other]

Title: Time Variability of Nonthermal X-ray Stripes in Tycho's Supernova Remnant with Chandra

Authors: Tomoyuki Okuno, Takaaki Tanaka, Hiroyuki Uchida, Felix A. Aharonian, Yasunobu Uchiyama, Takeshi Go Tsuru, Masamune Matsuda

Comments: 8 pages, 3 figures, 2 tables, accepted for publication in ApJ

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

[62]  arXiv:2003.10135 (replaced) [pdf, ps, other]

Title: The path to Z And-type outbursts: The case of V426 Sagittae (HBHA 1704-05)

Authors: A. Skopal, S. Yu. Shugarov, U. Munari, N. Masetti, E. Marchesini, R. M. Komzik, E. Kundra, N. Shagatova, T. N. Tarasova, C. Buil, C. Boussin, V. I. Shenavrin, F.-J. Hambsch, S. Dallaporta, A. Frigo, O. Garde, A. Zubareva, P. A. Dubovský, P. Kroll

Comments: 19 pages, 12 figures, 9 tables, 2 appendices, accepted for A&A, Tables A.1, A.2 and A.3 are only available at the CDS, added references for section 1

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

[63]  arXiv:2003.10516 (replaced) [pdf, ps, other]

Title: Global asymptotic dynamics of Cosmological Einsteinian Cubic Gravity

Authors: Israel Quiros, Ricardo García-Salcedo, Tame Gonzalez, Jorge Luis Morales Martínez, Ulises Nucamendi

Comments: 9 pages, 3 figures. A figure and several bibliographic references added. Acknowledgments modified

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

[64]  arXiv:2003.10912 (replaced) [pdf, ps, other]

Title: On the Angular Momentum History of Galactic Disks

Authors: Alvio Renzini

Comments: % pages, 0 figures, to appear on MNRAS

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

[65]  arXiv:2003.11085 (replaced) [pdf, other]

Title: Detailed abundances in the Galactic center: Evidence of a metal-rich alpha-enhanced stellar population

Authors: B. Thorsbro, N. Ryde, R. M. Rich, M. Schultheis, F. Renaud, E. Spitoni, T. K. Fritz, A. Mastrobuono-Battisti, L. Origlia, F. Matteucci, R. Schödel

Comments: 13 pages, 10 figures, accepted for publication in ApJ, Figure 7 corrected

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

[66]  arXiv:2003.11138 (replaced) [pdf, other]

Title: Apparent radio transients mapping the near-Earth plasma environment

Authors: Mark J. Kuiack, Ralph A.M.J. Wijers, Aleksandar Shulevski, Antonia Rowlinson

Comments: 12 pages, 13 figures. Submitted to MNRAS

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

[67]  arXiv:2003.11447 (replaced) [pdf, ps, other]

Title: The M dwarf problem: Fe and Ti abundances in a volume-limited sample of M dwarf stars

Authors: Vincent M. Woolf, George Wallerstein

Comments: 10 pages, 3 figures. Accepted for publication in MNRAS. Corrected typos in Abstract

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

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