We gratefully acknowledge support from
the Simons Foundation and Leiden University.

Astrophysics

New submissions

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New submissions for Mon, 18 May 20

[1]  arXiv:2005.07199 [pdf, other]
Title: A Gas Giant Planet in the OGLE-2006-BLG-284L Stellar Binary System
Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Solar and Stellar Astrophysics (astro-ph.SR)

We present the analysis of microlensing event OGLE-2006-BLG-284, which has a lens system that consists of two stars and a gas giant planet with a mass ratio of $q_p = (1.26\pm 0.19) \times 10^{-3}$ to the primary. The mass ratio of the two stars is $q_s = 0.289\pm 0.011$, and their projected separation is $s_s = 2.1\pm 0.7\,$AU, while the projected separation of the planet from the primary is $s_p = 2.2\pm 0.8\,$AU. For this lens system to have stable orbits, the three-dimensional separation of either the primary and secondary stars or the planet and primary star must be much larger than that these projected separations. Since we do not know which is the case, the system could include either a circumbinary or a circumstellar planet. Because there is no measurement of the microlensing parallax effect or lens system brightness, we can only make a rough Bayesian estimate of the lens system masses and brightness. We find host star and planet masses of $M_{L1} = 0.35^{+0.30}_{-0.20}\,M_\odot$, $M_{L2} = 0.10^{+0.09}_{-0.06}\,M_\odot$, and $m_p = 144^{+126}_{-82}\,M_\oplus$, and the $K$-band magnitude of the combined brightness of the host stars is $K_L = 19.7^{+0.7}_{-1.0}$. The separation between the lens and source system will be $\sim 90\,$mas in mid-2020, so it should be possible to detect the host system with follow-up adaptive optics or Hubble Space Telescope observations.

[2]  arXiv:2005.07203 [pdf, other]
Title: TESS Data for Asteroseismology: Timing verification
Comments: 15 pages, 9 figures
Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Solar and Stellar Astrophysics (astro-ph.SR)

The Transiting Exoplanet Survey Satellite (TESS) is NASA's latest space telescope dedicated to the discovery of transiting exoplanets around nearby stars. Besides the main goal of the mission, asteroseismology is an important secondary goal and very relevant for the high-quality time series that TESS will make during its two year all-sky survey. Using TESS for asteroseismology introduces strong timing requirements, especially for coherent oscillators. Although the internal clock on board TESS is precise in its own time, it might have a constant drift and will thus need calibration, or offsets might inadvertently be introduced. Here we present simultaneously ground- and space-based observations of primary eclipses of several binary systems in the Southern ecliptic hemisphere, used to verify the reliability of the TESS timestamps. From twelve contemporaneous TESS/ground observations we determined a time offset equal to 5.8 +/- 2.5 sec, in the sense that the Barycentric time measured by TESS is ahead of real time. The offset is consistent with zero at 2.3-sigma level. In addition, we used 405 individually measured mid-eclipse times of 26 eclipsing binary stars observed solely by TESS to test the existence of a potential drift with a monotonic growth (or decay) affecting the observations of all stars. We find a drift corresponding to sigma_drift = 0.009 +/- 0.015 sec/day. We find that the measured offset is of a size that will not become an issue for comparing ground-based and space data for coherent oscillations for most of the targets observed with TESS.

[3]  arXiv:2005.07206 [pdf, other]
Title: The 21 cm-kSZ-kSZ Bispectrum during the Epoch of Reionization
Comments: 23 pages, 13 figures, submitted to ApJ
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO)

The high-redshift 21 cm signal from the Epoch of Reionization (EoR) is a promising observational probe of the early universe. Current- and next-generation radio interferometers such as the Hydrogen Epoch of Reionization Array (HERA) and Square Kilometre Array (SKA) are projected to measure the 21 cm auto power spectrum from the EoR. Another observational signal of this era is the kinetic Sunyaev-Zel'dovich (kSZ) signal in the cosmic microwave background (CMB), which will be observed by the upcoming Simons Observatory (SO) and CMB-S4 experiments. The 21 cm signal and the contribution to the kSZ from the EoR are expected to be anti-correlated, the former coming from regions of neutral gas in the intergalactic medium and the latter coming from ionized regions. However, the naive cross-correlation between the kSZ and 21 cm maps suffers from a cancellation that occurs because ionized regions are equally likely to be moving toward or away from the observer and so there is no net correlation with the 21 cm signal. We present here an investigation of the 21 cm-kSZ-kSZ bispectrum, which should not suffer the same cancellation as the simple two-point cross-correlation. We show that there is a significant and non-vanishing signal that is sensitive to the reionization history, suggesting the statistic may be used to confirm or infer the ionization fraction as a function of redshift. In the absence of foreground contamination, we forecast that this signal is detectable at high statistical significance with HERA and SO. The bispectrum we study suffers from the fact that the kSZ signal is sensitive only to Fourier modes with long-wavelength line-of-sight components, which are generally lost in the 21 cm data sets owing to foreground contamination. We discuss possible strategies for alleviating this contamination, including an alternative four-point statistic that may help circumvent this issue.

[4]  arXiv:2005.07208 [pdf, other]
Title: Effects of self-consistent rest-ultraviolet colours in semi-empirical galaxy formation models
Comments: 14+4 pages, 11+5 figures, submitted to MNRAS
Subjects: Astrophysics of Galaxies (astro-ph.GA)

Connecting the observed rest-ultraviolet (UV) luminosities of high-$z$ galaxies to their intrinsic luminosities (and thus star formation rates) requires correcting for the presence of dust. We bypass a common dust-correction approach that uses empirical relationships between infrared (IR) emission and UV colours, and instead augment a semi-empirical model for galaxy formation with a simple -- but self-consistent -- dust model and use it to jointly fit high-$z$ rest-UV luminosity functions (LFs) and colour-magnitude relations ($M_{\mathrm{UV}}$-$\beta$). In doing so, we find that UV colours evolve with redshift (at fixed UV magnitude), as suggested by observations, even in cases without underlying evolution in dust production, destruction, absorption, or geometry. The observed evolution in our model arises due to the reduction in the mean stellar age and rise in specific star formation rates with increasing $z$. The UV extinction, $A_{\mathrm{UV}}$, evolves similarly with redshift, though we find a systematically shallower relation between $A_{\mathrm{UV}}$ and $M_{\mathrm{UV}}$ than that predicted by IRX-$\beta$ relationships derived from $z \sim 3$ galaxy samples. Finally, assuming that high $1600 \r{A}$ transmission ($\gtrsim 0.6$) is a reliable LAE indicator, modest scatter in the effective dust surface density of galaxies can explain the evolution both in $M_{\mathrm{UV}}$-$\beta$ and LAE fractions. These predictions are readily testable by deep surveys with the James Webb Space Telescope.

[5]  arXiv:2005.07210 [pdf, other]
Title: LAMOST Medium-Resolution Spectroscopic Survey (LAMOST-MRS): Scientific goals and survey plan
Comments: 25 pages, 10 figues. Submitted to Reseach in Astronomy and Astrophysics
Subjects: Solar and Stellar Astrophysics (astro-ph.SR); Astrophysics of Galaxies (astro-ph.GA); Instrumentation and Methods for Astrophysics (astro-ph.IM)

Since September 2018, LAMOST starts a new 5-year medium-resolution spectroscopic survey (MRS) using bright/gray nights. We present the scientific goals of LAMOST-MRS and propose a near optimistic strategy of the survey. A complete footprint is also provided. Not only the regular medium-resolution survey, but also a time-domain spectroscopic survey is being conducted since 2018 and will be end in 2023. According to the detailed survey plan, we expect that LAMOST-MRS can observe about 2 million stellar spectra with ~7500 and limiting magnitude of around G=15 mag. Moreover, it will also provide about 200 thousand stars with averagely 60-epoch observations and limiting magnitude of G~14 mag. These high quality spectra will give around 20 elemental abundances, rotational velocities, emission line profiles as well as precise radial velocity with uncertainty less than 1 km/s. With these data, we expect that LAMOST can effectively leverage sciences on stellar physics, e.g. exotic binary stars, detailed observation of many types of variable stars etc., planet host stars, emission nebulae, open clusters, young pre-main-sequence stars etc.

[6]  arXiv:2005.07215 [pdf, other]
Title: The origin of the escape of Lyman alpha and ionizing photons in Lyman Continuum Emitters
Comments: Accepted for publication in A&A. 28 pages, 23 figures, 7 tables
Subjects: Astrophysics of Galaxies (astro-ph.GA); Cosmology and Nongalactic Astrophysics (astro-ph.CO)

Identifying the mechanisms driving the escape of Lyman Continuum (LyC) photons is crucial to find Lyman Continuum Emitter (LCE) candidates. To understand the physical properties involved in the leakage of LyC photons, we investigate the connection between the HI covering fraction, HI velocity width, the Lyman alpha (LyA) properties and escape of LyC photons in a sample of 22 star-forming galaxies including 13 LCEs. We fit the stellar continua, dust attenuation, and absorption lines between 920 and 1300 A to extract the HI covering fractions and dust attenuation. Additionally, we measure the HI velocity widths of the optically thick Lyman series and derive the LyA equivalent widths (EW), escape fractions (fesc), peak velocities and fluxes at the minimum of the LyA profiles. Overall, we highlight strong correlations between the presence of low HI covering fractions and (1) low LyA peak velocities; (2) more flux at the profile minimum; and (3) larger EW(LyA), fesc(LyA), and fesc(LyC). Hence, low column density channels are crucial ISM ingredients for the leakage of LyC and LyA photons. Additionally, galaxies with narrower HI absorption velocity widths have higher LyA equivalent widths, larger LyA escape fractions, and lower LyA peak velocity separations. This suggests that these galaxies have low HI column density. Finally, we find that dust regulates the amount of LyA and LyC radiation that actually escapes the ISM. Overall, the ISM porosity is one origin of strong LyA emission and enables the escape of ionizing photons in low-z leakers. However, this is not enough to explain the largest fesc(LyC) observed, which indicates that the most extreme LCEs are likely density-bounded along all lines of sight to the observer. Overall, the neutral gas porosity constrains a lower limit to the escape fraction of LyC and LyA photons, providing a key estimator of the leakage of ionizing photons.

[7]  arXiv:2005.07216 [pdf, ps, other]
Title: Bayesian Inference of the Symmetry Energy of Super-Dense Neutron-Rich Matter from Future Radius Measurements of Massive Neutron Stars
Comments: 18 pages with 9 figures
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Nuclear Experiment (nucl-ex); Nuclear Theory (nucl-th)

Using an explicitly isospin-dependent parametric Equation of State (EOS) for the core of neutron stars (NSs) within the Bayesian statistical approach, we infer the EOS parameters of super-dense neutron-rich nuclear matter from three sets of imagined mass-radius correlation data representing typical predictions by various nuclear many-body theories, i.e, the radius stays the same, decreases or increases with increasing NS mass within $\pm 15\%$ between 1.4 M$_{\odot}$ and 2.0 M$_{\odot}$. The corresponding average density increases quickly, slowly or slightly decreases as the NS mass increases from 1.4 M$_{\odot}$ to 2.0 M$_{\odot}$. Using the posterior probability distribution functions (PDFs) of EOS parameters inferred from GW170817 and NICER radius data for canonical NSs as references, we investigate how future radius measurements of massive NS will improve our knowledge about the EOS of super-dense neutron-rich nuclear matter, especially its symmetry energy term, compared to what people have already learned from analyzing the GW170817 and NICER data. While the EOS of symmetric nuclear matter (SNM) inferred from the three data sets are approximately the same, the corresponding high-density symmetry energies at densities above about $2\rho_0$ are very different, indicating that the radii of massive NSs carry reliable information about the high-density behavior of nuclear symmetry energy with little influence from the remaining uncertainties of the SNM EOS.

[8]  arXiv:2005.07218 [pdf, other]
Title: Comprehensive Multimessenger Modeling of the Extreme Blazar 3HSP J095507.9+355101 and Predictions for IceCube
Comments: 25 pages, 15 figures, 4 tables, submitted to ApJ
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

3HSP J095507.9+355101 is an extreme blazar to have been possibly associated with a high-energy neutrino, IceCube-200107A, which was detected one day before the blazar was observed and found to undergo a hard X-ray flare. Motivated by this observation, we perform a comprehensive study of the predicted multimessenger emission from 3HSP J095507.9+355101 during its recent X-ray flare, but also in the long term. We focus on single-zone leptohadronic models, where the broadband photon and high-energy neutrino emissions originate from same region of the jet, but we also explore alternative scenarios: (i) a blazar-core model, which considers neutrino production in the inner jet close to the accreting supermassive black hole, (ii) a hidden external-photon model, which considers neutrino production in the jet through interactions with photons from a possible weak broad line region, (iii) a one-zone proton synchrotron model, where high-energy protons produce $\gamma$-rays in the jet via synchrotron, and (iv) an intergalactic cascade scenario, where neutrinos are produced in the intergalactic medium by interactions of a high-energy cosmic-ray beam escaping the blazar jet. We find that the Poisson probability to detect one or more neutrinos in 8 years from 3HSP J095507.9+355101 is $\sim 2\%$ ($3\%$) when considering the most optimistic one-zone leptohadronic model (the multi-zone blazar-core model), while detection of one neutrino event during the X-ray flare is much less likely. If the association is real, then IceCube-Gen2 and other future detectors should be able to provide additional evidence for neutrino production in 3HSP J095507.9+355101 and other extreme blazars, assuming similar physical conditions.

[9]  arXiv:2005.07228 [pdf, other]
Title: Galaxy classification: deep learning on the OTELO and COSMOS databases
Authors: José A. de Diego (1, 2), Jakub Nadolny (2, 3), Ángel Bongiovanni (4, 5), Jordi Cepa (2, 5, 3), Mirjana Pović (6, 7), Ana María Pérez García (5, 8), Carmen P. Padilla Torres (2, 3, 9), Maritza A. Lara-López (10), Miguel Cerviño (8), Ricardo Pérez Martínez (5, 11), Emilio J. Alfaro (7), Héctor O. Castañeda (12), Miriam Fernández-Lorenzo (7), Jesús Gallego (13), J. Jesús González (1), J. Ignacio González-Serrano (14, 5), Irene Pintos-Castro (15), Miguel Sánchez-Portal (4, 5), Bernab? Cedrés (2, 3), Mauro González-Otero (2, 3), D. Heath Jones (16), Joss Bland-Hawthorn (17) ((1) Instituto de Astronomía UNAM, (2) Instituto de Astrofísica de Canarias, (3) Departamento de Astrofísica ULL, (4) Instituto de Radioastronomía Milimétrica, (5) Asociación Astrofísica para la Promoción de la Investigación Instrumentación y su Desarrollo, (6) Ethiopian Space Science and Technology Institute, (7) Instituto de Astrofísica de Andalucía CSIC, (8) Depto. Astrofísica Centro de Astrobiología CSIC, (9) Fundación Galileo Galilei Telescopio Nazionale Galileo, (10) DARK Niels Bohr Institute University of Copenhagen, (11) ISDEFE for European Space Astronomy Centre ESAC ESA, (12) Depto. de Física Escuela Superior de Física y Matemáticas Instituto Politécnico Nacional, (13) Depto. de Física de la Tierra y Astrofísica Facultad CC Físicas In stituto de Física de Partículas y del Cosmos, (14) Instituto de Física de Cantabria CSIC Universidad de Cantabria, (15) Dep. of Astronomy Astrophysics University of Toronto, (16) English Language and Foundation Studies Centre University of Newcastle, (17) Sydney Institute of Astronomy School of Physics Univ. of Sydney)
Comments: 20 pages, 10 tables, 14 figures, Astronomy and Astrophysics (in press)
Subjects: Astrophysics of Galaxies (astro-ph.GA)

Context. The accurate classification of hundreds of thousands of galaxies observed in modern deep surveys is imperative if we want to understand the universe and its evolution. Aims. Here, we report the use of machine learning techniques to classify early- and late-type galaxies in the OTELO and COSMOS databases using optical and infrared photometry and available shape parameters: either the Sersic index or the concentration index. Methods. We used three classification methods for the OTELO database: 1) u-r color separation , 2) linear discriminant analysis using u-r and a shape parameter classification, and 3) a deep neural network using the r magnitude, several colors, and a shape parameter. We analyzed the performance of each method by sample bootstrapping and tested the performance of our neural network architecture using COSMOS data. Results. The accuracy achieved by the deep neural network is greater than that of the other classification methods, and it can also operate with missing data. Our neural network architecture is able to classify both OTELO and COSMOS datasets regardless of small differences in the photometric bands used in each catalog. Conclusions. In this study we show that the use of deep neural networks is a robust method to mine the cataloged data

[10]  arXiv:2005.07231 [pdf, other]
Title: Prospects of Probing Dark Energy with eLISA: Standard versus Null Diagnostics
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO)

Gravitational waves from supermassive black hole binary mergers along with an electromagnetic counterpart has the potential to shed `light' on the nature of dark energy in the intermediate redshift regime. An accurate measurement of dark energy parameters at intermediate redshift is extremely essential to improve our understanding of dark energy, and to possibly resolve couple of tensions involving cosmological parameters. We present a Fisher matrix forecast analysis in the context of eLISA to predict the errors for three different cases: the non-interacting dark energy with constant and evolving equation of state (EoS), and interacting dark sectors with a generalized parametrization. In all three cases, we perform the analysis for two separate formalisms, namely, the standard EoS formalism and the model-independent null diagnostics using \textit{Om} parametrization for a wide range of fiducial values in both phantom and non-phantom regions, in order to make a comparative analysis between the prospects of these two diagnostics in eLISA. Our analysis reveals that it is wiser and more effective to probe null diagnostics instead of the standard EoS parameters for any possible signature of dark energy at intermediate redshift measurements like eLISA.

[11]  arXiv:2005.07244 [pdf, other]
Title: Low-frequency observations of giant pulses from ordinary pulsars
Comments: 20 pages, 18 figures
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

We present our results of investigation of the rate of emission of the giant radio pulses (GRPs) from several second period pulsars, observed with Large Phased Array radio telescope of Pushchino Radio Astronomy Observatory at 111 MHz. It was found that for all pulsars detected rate was not constant and changed with time significantly. Abrupt jumps in the rate of GRPs generation were detected for PSR B0950+08 and PSR B1112+50. We found that GRPs of all pulsars have demonstrated very different clustering properties. Finally, we have carried out the phase analysis of the time of arrival for GRPs and detected their phase with reference to the averaged pulse time of arrival.

[12]  arXiv:2005.07248 [pdf, other]
Title: The high-redshift Universe with Spitzer
Authors: Maruša Bradač (UC Davis)
Comments: Nature Astronomy Review Article
Journal-ref: Nature Astronomy volume 4, pages 478-485 (2020)
Subjects: Astrophysics of Galaxies (astro-ph.GA)

When did galaxies start forming stars? What is the role of distant galaxies in galaxy formation models and the epoch of reionization? What are the conditions in typical star-forming galaxies at redshifts >~4? Why is galaxy evolution dependent on environment? The Spitzer Space Telescope has been a crucial tool for addressing these questions. Accurate knowledge of stellar masses, ages and star formation rates requires measuring rest-frame optical (and ultraviolet) light, which only Spitzer can probe at high redshifts for a sufficiently large sample of typical galaxies. Many of these science goals are the main science drivers for the James Webb Space Telescope, and Spitzer afforded us their first exploration.

[13]  arXiv:2005.07256 [pdf]
Title: Possible evidence from the flaring activity of Sgr A* for a star at a distance of ~3.3 Schwarzscild radii from the blackhole
Authors: Elia Leibowitz
Comments: ApJ accepted
Subjects: Astrophysics of Galaxies (astro-ph.GA); High Energy Astrophysical Phenomena (astro-ph.HE)

The frequent flaring events in the X-ray and the NIR radiation of Sgr A* seem not to be periodic in time. However, statistical regularities, here termed "modulations by a pacemaker", are found in the recorded arrival times of both types of events. The characteristic time of the X-ray pacemaker is 149 min and that of the NIR pacemaker is 40 min. Their reality as derived from observed data can be accepted at larger than 4.6{\sigma} and 3.8{\sigma} levels of statistical confidence, respectively. These results can be interpreted as evidence for a star that revolves around the BH of Sgr A* in a slightly elliptical precessing orbit, at a distance of 3-3.5 Schwarzschild radii of the BH. The period of the X-ray pacemaker, which is not a periodicity of the flare occurrences themselves, is the epicyclic period of the star orbital motion. This is the time interval between 2 successive passages of the star through the peri-center of its orbit. The NIR pacemaker period is the sidereal binary period of the star revolution. The origin of the X-ray flares is in episodes of intense mass loss from the star that occur preferably near the pericenter phase of the binary revolution. The NIR flares originate or are triggered by processes that are internal to the star. The radiation emitted in the direction of Earth is slightly modulated by the changing aspect ratio of the two components of the BH\star binary to the line of sight from Earth at the sidereal binary frequency.

[14]  arXiv:2005.07270 [pdf]
Title: Broadband photometry of asteroid 6478 Gault: activity and morphology
Subjects: Earth and Planetary Astrophysics (astro-ph.EP)

We present the results of short observational program for asteroid 6478 Gault with using of V and R Johnson filters realized at the Kyiv Comet Station during January-April 2019. Color indices and distribution of brightness in the comet-like tail were calculated. We made a comparative analysis of circumstances of the asteroid 6478 Gault activity with others morphologically similar active Main Belt asteroids.

[15]  arXiv:2005.07273 [pdf, other]
Title: The SKA Particle Array Prototype: The First Particle Detector at the Murchison Radio-astronomy Observatory
Comments: 17 pages, 14 figures, 3 tables, Accepted for publication in Nuclear Instruments and Physics Research A
Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM); High Energy Astrophysical Phenomena (astro-ph.HE)

We report on the design, deployment, and first results from a scintillation detector deployed at the Murchison Radio-astronomy Observatory (MRO). The detector is a prototype for a larger array -- the Square Kilometre Array Particle Array (SKAPA) -- planned to allow the radio-detection of cosmic rays with the Murchison Widefield Array and the low-frequency component of the Square Kilometre Array. The prototype design has been driven by stringent limits on radio emissions at the MRO, and to ensure survivability in a desert environment. Using data taken from Nov.\ 2018 to Feb.\ 2019, we characterize the detector response while accounting for the effects of temperature fluctuations, and calibrate the sensitivity of the prototype detector to through-going muons. This verifies the feasibility of cosmic ray detection at the MRO. We then estimate the required parameters of a planned array of eight such detectors to be used to trigger radio observations by the Murchison Widefield Array.

[16]  arXiv:2005.07281 [pdf, other]
Title: Report from the Tri-Agency Cosmological Simulation Task Force
Comments: 36 pages, 3 figures. Delivered to NASA, NSF, and DOE in Dec 2018
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO)

The Tri-Agency Cosmological Simulations (TACS) Task Force was formed when Program Managers from the Department of Energy (DOE), the National Aeronautics and Space Administration (NASA), and the National Science Foundation (NSF) expressed an interest in receiving input into the cosmological simulations landscape related to the upcoming DOE/NSF Vera Rubin Observatory (Rubin), NASA/ESA's Euclid, and NASA's Wide Field Infrared Survey Telescope (WFIRST). The Co-Chairs of TACS, Katrin Heitmann and Alina Kiessling, invited community scientists from the USA and Europe who are each subject matter experts and are also members of one or more of the surveys to contribute. The following report represents the input from TACS that was delivered to the Agencies in December 2018.

[17]  arXiv:2005.07290 [pdf, other]
Title: The Value of Progenitor Radius Measurements for Explosion Modeling of Type II-Plateau Supernovae
Comments: 8 pages, 4 figures, accepted to the Astrophysical Journal Letters
Subjects: Solar and Stellar Astrophysics (astro-ph.SR); High Energy Astrophysical Phenomena (astro-ph.HE)

Using Modules for Experiments in Stellar Astrophysics (MESA)+STELLA, we show that very different physical models can adequately reproduce a specific observed Type II-Plateau Supernova (SN). We consider SN2004A, SN2004et, SN2009ib, SN2017eaw, and SN2017gmr, Nickel-rich ($M_\mathrm{Ni}>0.03M_\odot$) events with bolometric lightcurves and a well-sampled decline from the plateau. These events also have constraints on the progenitor radius, via a progenitor image, or, in the case of SN2017gmr, a radius from fitting shock-cooling models. In general, many explosions spanning the parameter space of progenitors can yield excellent lightcurve and Fe line velocity agreement, demonstrating the success of scaling laws in motivating models which match plateau properties for a given radius and highlighting the degeneracy between plateau luminosity and velocity in models and observed events, which can span over 50% in ejecta mass, radius, and explosion energy. This can help explain disagreements in explosion properties reported for the same event using different model calculations. Our calculations yield explosion properties when combined with pre-explosion progenitor radius measurements or a robust understanding of the outermost $<0.1\,M_\odot$ of material that quantifies the progenitor radius from SN observations a few days after explosion.

[18]  arXiv:2005.07312 [pdf, other]
Title: Evidence for a Supergalactic Structure of Magnetic Deflection Multiplets of Ultra-High Energy Cosmic Rays
Authors: Telescope Array Collaboration: R.U. Abbasi (1), M. Abe (2), T. Abu-Zayyad (1), M. Allen (1), R. Azuma (3), E. Barcikowski (1), J.W. Belz (1), D.R. Bergman (1), S.A. Blake (1), R. Cady (1), B.G. Cheon (4), J. Chiba (5), M. Chikawa (6), A. di Matteo (7), T. Fujii (8), K. Fujisue (9), K. Fujita (10), R. Fujiwara (10), M. Fukushima (9,11), G. Furlich (1), W. Hanlon (1), M. Hayashi (12), Y. Hayashi (10), N. Hayashida (13), K. Hibino (13), R. Higuchi (9), K. Honda (14), D. Ikeda (15), T. Inadomi (16), N. Inoue (2), T. Ishii (14), R. Ishimori (3), H. Ito (17), D. Ivanov (1), H. Iwakura (16), H.M. Jeong (18), S. Jeong (18), C.C.H. Jui (1), K. Kadota (19), F. Kakimoto (3), O. Kalashev (20), K. Kasahara (21), S. Kasami (22), H. Kawai (23), S. Kawakami (10), S. Kawana (2), K. Kawata (9), E. Kido (9), et al. (102 additional authors not shown)
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

Evidence for a large-scale supergalactic cosmic ray multiplet (arrival directions correlated with energy) structure is reported for ultra-high energy cosmic ray (UHECR) energies above 10$^{19}$ eV using seven years of data from the Telescope Array (TA) surface detector and updated to 10 years. Previous energy-position correlation studies have made assumptions regarding magnetic field shapes and strength, and UHECR composition. Here the assumption tested is that, since the supergalactic plane is a fit to the average matter density of the local Large Scale Structure (LSS), UHECR sources and intervening extragalactic magnetic fields are correlated with this plane. This supergalactic deflection hypothesis is tested by the entire field-of-view (FOV) behavior of the strength of intermediate-scale energy-angle correlations. These multiplets are measured in spherical cap section bins (wedges) of the FOV to account for coherent and random magnetic fields. The structure found is consistent with supergalactic deflection, the previously published energy spectrum anisotropy results of TA (the hotspot and coldspot), and toy-model simulations of a supergalactic magnetic sheet. The seven year data post-trial significance of this supergalactic structure of multiplets appearing by chance, on an isotropic sky, is found by Monte Carlo simulation to be 4.19$\sigma$. The ten years of data post-trial significance is 4.09$\sigma$. Furthermore, the starburst galaxy M82 is shown to be a possible source of the TA Hotspot, and an estimate of the supergalactic magnetic field using UHECR measurements is presented.

[19]  arXiv:2005.07339 [pdf, ps, other]
Title: Dust Reverberation Mapping of Type 2 AGN NGC 2110 Realized with X-ray and 3-5 $μ$m IR monitoring
Comments: 10 pages, 7 figures, 1 table, accepted for the publication in MNRAS
Subjects: Astrophysics of Galaxies (astro-ph.GA); High Energy Astrophysical Phenomena (astro-ph.HE)

The dust reverberation mapping is one of powerful methods to investigate the structure of the dusty tori in AGNs, and it has been performed on more than a hundred type 1 AGNs. However, no clear results have been reported on type 2 AGNs because their strong optical-UV extinction completely hides their accretion disc emission. Here we focus on an X-ray-bright type 2 AGN, NGC 2110, and utilize 2-20 keV X-ray variation monitored by MAXI to trace disc emission, instead of optical-UV variation. Comparing it with light curves in the WISE infrared (IR) W1 band ($\lambda = 3.4$ $\mu$m) and W2 band ($\lambda = 4.6$ $\mu$m) with cross-correlation analyses, we found candidates of the dust reverberation time lag at $\sim60$ days, $\sim130$ days, and $\sim1250$ days between the X-ray flux variation and those of the IR bands. By examining the best-fitting X-ray and IR light curves with the derived time lags, we found that the time lag of $\sim130$ days is most favoured. With this time lag, the relation between the time lag and luminosity of NGC 2110 is consistent with those in type 1 AGNs, suggesting that the dust reverberation in NGC 2110 mainly originates in hot dust in the torus innermost region, the same as in type 1 AGNs. As demonstrated by the present study, X-ray and IR simultaneous monitoring can be a promising tool to perform the dust reverberation mapping on type 2 AGNs.

[20]  arXiv:2005.07348 [pdf, ps, other]
Title: The Near-Infrared Polarization of the Pre-Planetary Nebula Frosty Leo
Comments: 5 figures, 9 pages, accepted in MNRAS
Subjects: Solar and Stellar Astrophysics (astro-ph.SR); Astrophysics of Galaxies (astro-ph.GA)

We present a near-infrared imaging polarimetric study of the pre-planetary nebula: Frosty Leo. The observations were carried out in J, H and K' bands using the new polarimeter POLICAN mounted on the 2.1m telescope of the Guillermo Haro Astrophysical Observatory, Sonora, Mexico. The most prominent result observed in the polarization maps is a large and well defined dusty envelope (35\arcsec\ diameter in H-band). The polarization position angles in the envelope are particularly well ordered and nearly parallel to the equator of the nebula (seen in J and H bands). The nebula presents a known bipolar outflow and the envelope completely wraps around it. Within the bipolar lobes, we find high polarization levels ranging from $60\%$ (J band) to $90\%$ (K' band) and the polarization angles trace a centrosymmetric pattern. We found the remnants of superwind shells at the edges of the bipolar lobes and the duration of this phase is around 600 yrs. The origin of polarization features in the nebula is most likely due to a combination of single and multiple scattering. Our results clearly demonstrate new structures that provide new hints on the evolution of Frosty Leo from its previous asymptotic giant branch phase.

[21]  arXiv:2005.07367 [pdf, other]
Title: Coherent Stellar Motion in Galactic Spiral Arms by Swing Amplification
Comments: 13 pages, 10 figures, accepted for publication in ApJ
Subjects: Astrophysics of Galaxies (astro-ph.GA)

We perform local $N$-body simulations of disk galaxies and investigate the evolution of spiral arms. We calculate the time autocorrelation of the surface density of spiral arms and find that the typical evolution timescale is described by the epicycle period. We investigate the distribution of the orbital elements of stars and find that in spiral arms the epicycle motions of stars are in phase while the spatial distribution of the guiding center is nearly uniform. These facts clearly show that the phase synchronization of the epicycle motion takes place, which is theoretically predicted by the swing amplification.

[22]  arXiv:2005.07375 [pdf, other]
Title: Photometric study of the young open clusters IC 1442, King 21, and Trumpler 7
Comments: This article is accepted for publication in MNRAS
Subjects: Solar and Stellar Astrophysics (astro-ph.SR); Astrophysics of Galaxies (astro-ph.GA)

We carried out UBVRcIc photometric study of three poorly studied young open clusters IC 1442, King 21, and Trumpler 7 (Tr 7). We obtained 263, 244, and 128 member stars using Gaia DR2 proper motions and parallaxes in IC 1442, King 21, and Tr 7, respectively. The reddening, E(B-V), was derived to be 0.54+/-0.04, 0.76+/-0.06, and 0.38+/-0.04 mag for these clusters. The comparison of observed colour-magnitude diagrams (CMDs) with solar metallicity isochrones yields log(Age) = 7.40+/-0.30, 7.70+/-0.20, and 7.85+/-0.25 yr and corresponding distances 2847+/-238, 2622+/-156, and 1561+/-74 pc for IC 1442, King 21, and Tr 7, respectively. The estimated mass function (MF) slopes are found to be -1.94+/-0.18, -1.54+/-0.32, and -2.31+/-0.29 for IC 1442, King 21, and Tr 7, respectively. The study of MF slopes determined separately in the inner and the outer regions of these clusters gives a steeper slope in outer region which suggests spatial variation in slope and mass segregation in the clusters. We found evidence of mass segregation after dynamical study in these clusters. The obtained relaxation time is 74, 26, and 34 Myr for the clusters IC 1442, King 21, and Tr 7, respectively. The mass segregation in IC 1442 may be caused by early dynamical relaxation. The estimated relaxation time is well below to the ages of King 21 and Tr 7 which indicates that these clusters are dynamically relaxed.

[23]  arXiv:2005.07387 [pdf, other]
Title: Bar rejuvenation in S0 galaxies?
Comments: 10 pages, 7 figures, accepted for publication in MNRAS
Subjects: Astrophysics of Galaxies (astro-ph.GA)

Based on the colour measurements from a multi-band, multi-component 2D decomposition's of S0 and spiral galaxies using SDSS images, we found that bars are bluer in S0 galaxies compared to the spiral galaxies. Most of the S0s in our sample have stellar masses $\sim L_{*}$ galaxies. The environment might have played an important role as most of the S0s with bluer bars are in the intermediate-density environment. The possibility of minor mergers and tidal interactions which occurs frequently in the intermediate-density environment might have caused either a bar to form and/or induce star formation in the barred region of S0 galaxies. The underlying discs show the usual behaviour being redder in S0s compared to spiral galaxies while the bulges are red and old for both S0 and spiral galaxies. The finding of bluer bars in S0 galaxies is a puzzling issue and poses an interesting question at numerical and theoretical studies most of which shows that the bars are long-lived structures with old stellar populations.

[24]  arXiv:2005.07467 [pdf, other]
Title: Primordial Black Hole Constraints with Large Extra Dimensions
Authors: George Johnson
Comments: 17 pages, 4 figures
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); General Relativity and Quantum Cosmology (gr-qc)

We study how the constraints on the primordial black hole density arising from the extragalactic photon background are modified in the scenario that there exist extra large spatial dimensions. We find that though the overall magnitude of the constraints is not substantially different, the mass ranges to which they apply are, and for some choices of mass it is possible for the black holes to constitute the entirety of the dark matter.

[25]  arXiv:2005.07480 [pdf, other]
Title: Zodiacal light observations and its link with cosmic dust: a review
Comments: Accepted for publication in Planetary and Space Science
Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Solar and Stellar Astrophysics (astro-ph.SR)

The zodiacal light is a night-glow mostly visible along the plane of the ecliptic. It represents the background radiation associated with solar light scattered by the tenuous flattened interplanetary cloud of dust particles surrounding the Sun and the planets. It is an interesting subject of study, as the source of the micrometeoroids falling on Earth, as a link to the activity of the small bodies of the Solar System, but also as a foreground that veils the low brightness extrasolar astronomical light sources.
In this review, we summarize the zodiacal light observations that have been done from the ground and from space in brightness and polarization at various wavelength ranges. Local properties of the interplanetary dust particles in some given locations can be retrieved from the inversion of the zodiacal light integrated along the light-of-sight. We show that the current community consensus favors that the majority of the interplanetary dust particles detected at 1 au originate from the activity of comets.
Our current understanding of the interplanetary dust particles properties is then discussed in the context of the recent results from the Rosetta rendezvous space mission with comet 67P/Churyumov-Gerasimenko.

[26]  arXiv:2005.07494 [pdf, ps, other]
Title: Close eclipsing binary BD And: a triple system
Comments: 23 pages, 6 figures, online data table, to be published in CoSka
Subjects: Solar and Stellar Astrophysics (astro-ph.SR)

BD And is a fairly bright (V = 10.8), active and close (P = 0.9258 days) eclipsing binary. The cyclic variability of the apparent orbital period as well as third light in the light curves indicate the presence of an additional late-type component. The principal aim is the spectroscopic testing of the third-body hypothesis and determination of absolute stellar parameters for both components of the eclipsing binary. First medium and high-resolution spectroscopy of the system was obtained. The broadening-function technique appropriate for heavily-broadened spectra of close binaries was used. The radial velocities were determined fitting the Gaussian functions and rotational profiles to the broadening functions. A limited amount of photometric data has also been obtained. Although the photometric observations were focused on the obtaining the timing information, a cursory light-curve analysis was also performed. Extracted broadening functions clearly show the presence of a third, slowly-rotating component. Its radial velocity is within error of the systemic velocity of the eclipsing pair, strongly supporting the physical bond. The observed systemic radial-velocity and third-component changes do not support the 9 year orbit found from the timing variability. Masses of the components of the eclipsing pair are determined with about 0.5% precision. Further characterization of the system would require long-term photometric and spectroscopic monitoring.

[27]  arXiv:2005.07526 [pdf, other]
Title: Chemical Composition of Bright Stars in the Continuous Viewing Zone of the TESS Space Mission
Comments: 15 pages, 12 figures, published in ApJS, 2020 May 12
Journal-ref: The Astrophysical Journal Supplement Series, 248:19 (11pp), 2020 May
Subjects: Solar and Stellar Astrophysics (astro-ph.SR); Earth and Planetary Astrophysics (astro-ph.EP); Astrophysics of Galaxies (astro-ph.GA)

Accurate atmospheric parameters and chemical composition of stars play a vital role in characterizing physical parameters of exoplanetary systems and understanding of their formation. A full asteroseismic characterization of a star is also possible if its main atmospheric parameters are known. The NASA Transiting Exoplanet Survey Satellite (TESS) space telescope will play a very important role in searching of exoplanets around bright stars and stellar asteroseismic variability research. We have observed all 302 bright (V < 8 mag) and cooler than F5 spectral class stars in the northern TESS continuous viewing zone with a 1.65 m telescope at the Moletai Astronomical Observatory of Vilnius University and the high-resolution Vilnius University Echelle Spectrograph. We uniformly determined the main atmospheric parameters, ages, orbital parameters, velocity components, and precise abundances of 24 chemical species ( C(C2), N(CN), [O I], Na I, Mg I, Al I, Si I, Si II, Ca I, Ca II, Sc I, Sc II, Ti I, Ti II, V I, Cr I, Cr II, Mn I, Fe I, Fe II, Co I, Ni I, Cu I, and Zn I) for 277 slowly rotating single stars in the field. About 83 % of the sample stars exhibit the Mg/Si ratios greater than 1.0 and may potentially harbor rocky planets in their systems.

[28]  arXiv:2005.07527 [pdf, ps, other]
Title: A glimpse of pre-inflationary dynamics in tensor-to-scalar ratio
Authors: Suratna Das
Comments: 4 pages, no figure
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); General Relativity and Quantum Cosmology (gr-qc); High Energy Physics - Phenomenology (hep-ph)

Pre-inflationary dynamics is known to have left observable imprints via the varied dynamics of the inflaton and the graviton fields during those epochs. It is highlighted here that other particle degrees of freedom, too, are capable of leaving their imprints on primordial observables if they transfer their entropies upon annihilation after becoming non-relativistic during a pre-inflationary epoch. Such annihilations of other particles would result in lowering of the tensor-to-scalar ratio at the pivot scale (and at scales lower to that) which would help bring those potentials back in accordance with current observations which are otherwise disfavoured for yielding large tensor-to-scalar ratios.

[29]  arXiv:2005.07533 [pdf, ps, other]
Title: Testing the Equivalence Principle with Strong Lensing Time Delay Variations
Comments: 12 pages, no figures, comments are welcome
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); General Relativity and Quantum Cosmology (gr-qc)

Strong lensing time delay measurements provide a valuable and almost model-independent tool for cosmological investigations. In this work we recognize that they also carry information on the strength of the gravitational coupling at the redshift of the lens, and thus could be in principle used to test the equivalence principle on extragalactic scales. For the case of an extended lens with a static mass distribution we explicitly derive an analytical relation between $\dot{G}/G$ and the relative variation of the time delay. For illustrative purpose, we apply our formula to the light curves of multiple images of the quasar WFI2033-4723 and simulated ones, which results in weak constraints on the variation of $\dot{G}/G$ of order $10^{-2} \, yr^{-1}$ in the best scenario. Finally we briefly discuss how those constraints can be improved in the next future.

[30]  arXiv:2005.07536 [pdf, other]
Title: Mergers of Equal-Mass Binaries with Compact Object Companions from Mass Transfer in Triple Star Systems
Comments: 15 pages, 7 figures; submitted for publication, comments welcome
Subjects: Solar and Stellar Astrophysics (astro-ph.SR)

In this paper, we consider triple systems composed of main-sequence (MS) stars, and their internal evolution due to stellar and binary evolution. Our focus is on triples that produce white dwarfs (WDs), where Roche lobe overflow of an evolving tertiary triggers accretion onto the inner binary via a circumbinary disk (CBD) driving it toward a mass ratio of unity. We present a combination of analytic- and population synthesis-based calculations performed using the \texttt{SeBa} code to constrain the expected frequency of such systems, given a realistic initial population of MS triples, and provide the predicted distributions of orbital periods. We identify the parameter space for triples that can accommodate a CBD, to inform future numerical simulations of suitable initial conditions. We find that $\lesssim$ 10\% of all MS triples should be able to accommodate a CBD around the inner binary, and compute lower limits for the production rates. This scenario broadly predicts mergers of near equal-mass binaries, producing blue stragglers (BSs), Type Ia supernovae, gamma ray bursts and gravitational wave-induced mergers, along with the presence of an outer WD tertiary companion. We compare our predicted distributions to a sample of field BS binaries, and argue that our proposed mechanism explains the observed range of orbital periods. Finally, the mechanism considered here could produce hypervelocity MS stars, WDs and even millisecond pulsars with masses close to the Chandrasekhar mass limit, and be used to constrain the maximum remnant masses at the time of any supernova explosion.

[31]  arXiv:2005.07559 [pdf, ps, other]
Title: Discovery of $β$ Cep pulsations in the eclipsing binary V453 Cygni
Comments: Accepted for publication as a Letter by MNRAS. 5 pages, 3 figures, 2 tables
Subjects: Solar and Stellar Astrophysics (astro-ph.SR)

V453 Cyg is an eclipsing binary containing 14 Msun and 11 Msun stars in an eccentric short-period orbit. We have discovered $\beta$ Cep-type pulsations in this system using TESS data. We identify seven significant pulsation frequencies, between 2.37 and 10.51 d$^{-1}$, in the primary star. These include six frequencies which are separated by yet significantly offset from harmonics of the orbital frequency, indicating they are tidally-perturbed modes. We have determined the physical properties of the system to high precision: V453 Cyg A is the first $\beta$ Cep pulsator with a precise mass measurement. The system is a vital tracer of the physical processes that govern the evolution of massive single and binary stars.

[32]  arXiv:2005.07563 [pdf, other]
Title: Energy distribution and equation of state of the early Universe: matching the end of inflation and the onset of radiation domination
Comments: 5 pages + references, 3 figures
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Physics - Phenomenology (hep-ph); High Energy Physics - Theory (hep-th)

We study the energy distribution and equation of state of the universe between the end of inflation and the onset of radiation domination (RD), considering observationally consistent single-field inflationary scenarios, with a potential 'flattening' at large field values, and a monomial shape $V(\phi) \propto |\phi|^p$ around the origin. We include a quadratic interaction $g^2\phi^2X^2$ between the inflaton $\phi$ and a light scalar 'daughter' field $X$, as a proxy for (p)reheating. We capture the non-perturbative and non-linear nature of the system dynamics with lattice simulations, obtaining that: $i)$ the final energy transferred to $X$ depends only on $p$, not on $g^2$; $ii)$ the final transfer of energy is always negligible for $2 \leq p < 4$, and of order $\sim 50\%$ for $p \geq 4$; $iii)$ the system goes at late times to matter-domination for $p = 2$, and always to RD for $p > 2$. In the latter case we calculate the number of e-folds until RD, significantly reducing the uncertainty in the inflationary observables $n_s$ and $r$.

[33]  arXiv:2005.07588 [pdf, other]
Title: Formation of the Large Nearby Galaxies
Authors: P. J. E. Peebles
Comments: 10 pages, 6 figures
Subjects: Astrophysics of Galaxies (astro-ph.GA); Cosmology and Nongalactic Astrophysics (astro-ph.CO)

Observations of the nearby large galaxies that can be examined in particularly close detail suggest that many have small stellar luminosity fractions in bulges and haloes. Simulations of galaxy formation tend to produce considerably larger fractions of the star particles in model bulges, stellar haloes, and more generally in orbits seriously different from circular. The situation might be improved by a prescription for non-Gaussian initial conditions on the scale of galaxies.

[34]  arXiv:2005.07622 [pdf]
Title: Some peculiarities of activity for comets with orbits on 2 - 5 AU
Comments: 5 pages, 3 figures
Journal-ref: Advances in Astronomy and Space Physics, 9, 3-7 (2019)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Solar and Stellar Astrophysics (astro-ph.SR)

Periodic comets of different dynamical groups with orbits at 2 - 5 AU still occasionally active. The observed dust activity of such objects can be connected with processes of water ice sublimation (MBCs) or crystallization of amorphous water ice (QHCs) as well as with external causes. No connections of cometary flares with cyclic variations of solar activity indexes were found. But some individual solar flares can affect the brightness of comets. Cometary objects in the main asteroid belt have a lower statistic of flares than comets at orbits like quasi-Hilda objects.

[35]  arXiv:2005.07630 [pdf, ps, other]
Title: Revisiting the Relationship between the Long GRB Rate and Cosmic Star Formation History Based on a Large Swift Sample
Comments: Published in ApJS
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

The exact relationship between the long gamma-ray burst (LGRB) rate and the cosmic star formation rate (CSFR) is essential for using LGRBs as cosmological probes. In this work, we collect a large sample composed of 371 Swift LGRBs with known redshifts and prompt emission properties. We first compare the rest-frame prompt properties of these bursts in different redshift bins, finding negligible redshift evolution of the luminosity of LGRBs with $L_{\mathrm{iso}}\gtrsim10^{51}\,\mathrm{erg\, s^{-1}}$ between $z\sim1$ and $z\sim4$. Then, by utilizing the CSFR obtained from the large-scale cosmological hydrodynamical simulation, the Illustris simulation, we calculate the cumulative redshift distribution of LGRBs under different metallicity thresholds. After comparing with our sample, we find that the predictions with a moderate threshold between $0.3\,Z_{\odot}\leqslant Z_{\mathrm{th}}\leqslant1.0\,Z_{\odot}$ are consistent with the sample between redshift $0<z<3$, while at higher redshifts between $3<z<5$, all metallicity thresholds fit the data well. When changing to an empirical model based on observations, the predictions show similar results as well. After comparing with the metallicity distribution of the observed LGRB host galaxies between $0<z<1$, we confirm that the production of LGRBs in galaxies with super-solar metallicity is suppressed. Nevertheless, considering that a significant fraction of stars are born in sub-solar metallicity environments at $z\gtrsim3$, we suggest that, as a first approximation, LGRBs can be used as direct tracers of the CSFR in this redshift range.

[36]  arXiv:2005.07634 [pdf, other]
Title: The Formation of Isolated Ultra-Diffuse Galaxies in Romulus25
Comments: 20 pages, 15 figures, 2 movies, submitted to MNRAS
Subjects: Astrophysics of Galaxies (astro-ph.GA)

We use the Romulus25 cosmological simulation volume to identify the largest-ever simulated sample of field ultra-diffuse galaxies (UDGs). At z=0, we find that isolated UDGs have average star formation rates, colors, and virial masses for their stellar masses and environment. Although they tend to have slightly elevated HI masses, UDGs are consistent with the general isolated dwarf galaxy population and make up ~20% of all field galaxies with 10$^7$<M$_\star$/M$_\odot$<10$^{9}$. The properties of our UDGs are consistent with existing observations of field UDGs, but we predict that many isolated UDGs have been missed by current surveys. Despite their isolation at z=0, the UDGs in our sample are the products of major mergers at z>1. Mergers are no more common in UDG than non-UDG progenitors, but mergers that create UDGs tend to happen earlier, produce a temporary boost in spin, and cause star formation to migrate to the outskirts of galaxies, resulting in lower central star formation rates. The centers of the galaxies fade as their central stellar populations age, but their global star formation rates are maintained through bursts of star formation at larger radii. This formation channel is unique relative to other proposals for UDG formation in isolated galaxies, or for UDGs in groups and clusters, demonstrating that UDGs can potentially be formed through multiple mechanisms.

[37]  arXiv:2005.07645 [pdf, other]
Title: Minutes-delayed jets from a neutron star companion in core collapse supernovae
Authors: Noam Soker (Technion, Israel)
Comments: Will be submitted in two days to allow comments by readers
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)

I study cases where a neutron star (NS; or a black hole) companion to a type Ib or type Ic (stripped-envelope) core collapse supernova (CCSN) accretes mass from the explosion ejecta and launches jets minutes to hours after explosion. The NS orbits at a pre-explosion radius of a=1-5Ro. I find that when the ejecta velocity drops to be <1000-1500km/s the ejecta gas that the NS accretes possesses sufficient specific angular momentum to form an accretion disk around the NS. The NS accretes a fraction of 3e-5 to 3e-4 of the ejecta mass through an accretion disk over a time period of 10min to few hours. If the jets carry about ten per cent of the accretion energy, then their total energy is a fraction of about 0.003-0.03 of the kinetic energy of the ejecta. The implications of these jets from a NS (or a black hole) companion to a CCSN are the shaping the inner ejecta to have a bipolar morphology, energising the light curve of the CCSN, and in some cases the possible enrichment of the inner ejecta with r-process elements.

[38]  arXiv:2005.07653 [pdf, other]
Title: Response to Comment on "A Non-Interacting Low-Mass Black Hole -- Giant Star Binary System"
Comments: 5 pages
Journal-ref: Science 08 May 2020. Vol. 368, Issue 6491, eaba4356
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Solar and Stellar Astrophysics (astro-ph.SR)

van den Heuvel & Tauris argue that if the red giant star in the system 2MASS J05215658+4359220 has a mass of 1 solar mass (M$_\odot$), then its unseen companion could be a binary composed of two 0.9 M$_\odot$ stars, making a triple system. We contend that the existing data are most consistent with a giant of mass $3.2^{+1.0}_{-1.0}$ M$_\odot$, implying a black hole companion of $3.3^{+2.8}_{-0.7}$ M$_\odot$.

[39]  arXiv:2005.07664 [pdf, other]
Title: Bayesian Comparison of Interacting Modified Holographic Ricci Dark Energy Scenarios
Comments: 13 pages, 4 figures
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO)

We perform a Bayesian model selection analysis for interacting scenarios of dark matter and modified holographic Ricci dark energy (MHRDE) with linear interacting terms. We use a combination of some of the latest cosmological data such as type Ia supernovae, cosmic chronometers, cosmic microwave background and baryon acoustic oscillations measurements. We find strong evidence against all the MHRDE interacting scenarios studied with respect to $\Lambda$CDM when the full joint analysis is considered.

[40]  arXiv:2005.07693 [pdf, other]
Title: Galaxy properties as revealed by MaNGA. III. Kinematic profiles and stellar population gradients in S0s
Comments: Accepted for publication in MNRAS. 15 pages, 20 figures
Subjects: Astrophysics of Galaxies (astro-ph.GA); Cosmology and Nongalactic Astrophysics (astro-ph.CO)

This is the third paper of a series where we study the stellar population gradients (SP; ages, metallicities, $\alpha$-element abundance ratios and stellar initial mass functions) of early type galaxies (ETGs) at $z\le 0.08$ from the MaNGA-DR15 survey. In this work we focus on the S0 population and quantify how the SP varies across the population as well as with galactocentric distance. We do this by measuring Lick indices and comparing them to stellar population synthesis models. This requires spectra with high signal-to-noise which we achieve by stacking in bins of luminosity (L$_r$) and central velocity dispersion ($\sigma_0$). We find that: 1) There is a bimodality in the S0 population: S0s more massive than $3\times 10^{10}M_\odot$ show stronger velocity dispersion and age gradients (age and $\sigma_r$ decrease outwards) but little or no metallicity gradient, while the less massive ones present relatively flat age and velocity dispersion profiles, but a significant metallicity gradient (i.e. [M/H] decreases outwards). Above $2\times10^{11}M_\odot$ the number of S0s drops sharply. These two mass scales are also where global scaling relations of ETGs change slope. 2) S0s have steeper velocity dispersion profiles than fast rotating elliptical galaxies (E-FRs) of the same luminosity and velocity dispersion. The kinematic profiles and stellar population gradients of E-FRs are both more similar to those of slow rotating ellipticals (E-SRs) than to S0s, suggesting that E-FRs are not simply S0s viewed face-on. 3) At fixed $\sigma_0$, more luminous S0s and E-FRs are younger, more metal rich and less $\alpha$-enhanced. Evidently for these galaxies, the usual statement that 'massive galaxies are older' is not true if $\sigma_0$ is held fixed.

Cross-lists for Mon, 18 May 20

[41]  arXiv:2004.00339 (cross-list from astro-ph.CO) [pdf, other]
Title: Lorentzian Quintessential Inflation
Comments: This essay is awarded second prize in the 2020 Essay Competition of the Gravity Research Foundation
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); General Relativity and Quantum Cosmology (gr-qc); High Energy Physics - Theory (hep-th)

From the assumption that the slow roll parameter $\epsilon$ has a Lorentzian form as a function of the e-folds number $N$, a successful model of a quintessential inflation is obtained. The form corresponds to the vacuum energy both in the inflationary and in the dark energy epochs. The form satisfies the condition to climb from small values of $\epsilon$ to $1$ at the end of the inflationary epoch. At the late universe $\epsilon$ becomes small again and this leads to the Dark Energy epoch. The observables that the models predicts fits with the latest Planck data: $r \sim 10^{-3}, n_s \approx 0.965$. Naturally a large dimensionless factor that exponentially amplifies the inflationary scale and exponentially suppresses the dark energy scale appears, producing a sort of {\it{cosmological see saw mechanism}}. We find the corresponding scalar Quintessential Inflationary potential with two flat regions - one inflationary and one as a dark energy with slow roll behavior.

[42]  arXiv:2005.07200 (cross-list from hep-ph) [pdf, other]
Title: Visible Decay of Astrophysical Neutrinos at IceCube
Comments: 18 pages, 9 figures, comments welcome! Code available at this https URL
Subjects: High Energy Physics - Phenomenology (hep-ph); High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics - Experiment (hep-ex)

Neutrino decay modifies neutrino propagation in a unique way; not only is there flavor changing as there is in neutrino oscillations, there is also energy transport from initial to final neutrinos. The most sensitive direct probe of neutrino decay is currently IceCube which can measure the energy and flavor of neutrinos traveling over extragalactic distances. For the first time we calculate the flavor transition probability for the cases of visible and invisible neutrino decay, including the effects of the expansion of the universe, and consider the implications for IceCube. As an example, we demonstrate how neutrino decay addresses a tension in the IceCube data. We also provide a publicly available code to calculate the effect of visible decay.

[43]  arXiv:2005.07512 (cross-list from hep-ph) [pdf, ps, other]
Title: Particles and the Universe
Authors: George Lazarides
Comments: 23 pages, talk presented in the "Corfu Summer Institute 2019: School and Workshops on Elementary Particle Physics and Gravity (CORFU2019)", 31 August - 25 September 2019, Corfu, Greece, to appear in the proceedings. arXiv admin note: text overlap with arXiv:hep-ph/0607032, arXiv:hep-ph/0204294, arXiv:hep-ph/0111328
Subjects: High Energy Physics - Phenomenology (hep-ph); Cosmology and Nongalactic Astrophysics (astro-ph.CO)

The early stages of the universe evolution are discussed according to the hot big bang model and the grand unified theories. The shortcomings of big bang are summarized and their resolution by inflationary cosmology is sketched. Cosmological inflation, the subsequent oscillation and decay of the inflaton field, and the resulting reheating of the universe are studied in some detail. The density perturbations produced by inflation and the temperature fluctuations of the cosmic microwave background radiation are introduced. Baryogenesis via non-thermal leptogenesis is analyzed and dark energy and matter in the universe are presented. Quantum gravity and string theory are very briefly introduced. The problem of initial conditions for inflation is discussed in the light of string theory and the possibly detectable primordial gravity waves from inflation are mentioned.

Replacements for Mon, 18 May 20

[44]  arXiv:1702.04255 (replaced) [pdf, other]
Title: Ionized gaseous nebulae chemical abundance determination using the direct method
Comments: 27 pages, 9 figures. Accepted for publication as invited tutorial in PASP. Equation (3.5) relating t(OII) with RO2 corrected. Equation (4.20) for Ne2+ corrected
Subjects: Astrophysics of Galaxies (astro-ph.GA)
[45]  arXiv:1903.09049 (replaced) [pdf, other]
Title: TARDIS Paper I: A Constrained Reconstruction Approach to Modeling the z~2.5 Cosmic Web Probed by Lyman-alpha Forest Tomography
Comments: 18 pages, 14 figures
Journal-ref: The Astrophysical Journal 887.1 (2019): 61
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); Astrophysics of Galaxies (astro-ph.GA)
[46]  arXiv:1904.04074 (replaced) [pdf, ps, other]
Title: Alternative approach to gravity and MOND
Authors: Jozef Klačka
Subjects: Astrophysics of Galaxies (astro-ph.GA); Cosmology and Nongalactic Astrophysics (astro-ph.CO)
[47]  arXiv:1905.13744 (replaced) [pdf, other]
Title: Detecting Light Dark Matter with Magnons
Comments: 9 pages, 2 figures, 1 table; v2: clarification added, matches journal version
Subjects: High Energy Physics - Phenomenology (hep-ph); Cosmology and Nongalactic Astrophysics (astro-ph.CO); Materials Science (cond-mat.mtrl-sci); High Energy Physics - Experiment (hep-ex)
[48]  arXiv:1906.03998 (replaced) [pdf, other]
Title: Multi-waveform cross-correlation search method for intermediate-duration gravitational waves from gamma-ray bursts
Authors: Eric Sowell (TTU), Alessandra Corsi (TTU), Robert Coyne (URI)
Comments: 20 pages, 11 figures, 2 tables, submitted to Phys. Rev. D
Journal-ref: Phys. Rev. D 100, 124041 (2019)
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); General Relativity and Quantum Cosmology (gr-qc)
[49]  arXiv:1906.08909 (replaced) [pdf, other]
Title: Forecasting the Interaction in Dark Matter-Dark Energy Models with Standard Sirens From the Einstein Telescope
Comments: 19 pages, 6 figures. Version accepted for publication in JCAP
Journal-ref: JCAP(2020)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
[50]  arXiv:1908.03013 (replaced) [pdf, other]
Title: Application of the independent component analysis to the iKAGRA data
Comments: 27 pages, 12 figures : accepted version by PTEP with added discussion about the relation between ICA and Wiener filtering
Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM); General Relativity and Quantum Cosmology (gr-qc)
[51]  arXiv:1912.00997 (replaced) [pdf, other]
Title: On bubble collisions in strongly supercooled phase transitions
Comments: 8 pages, 5 figures
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Physics - Phenomenology (hep-ph)
[52]  arXiv:1912.12262 (replaced) [pdf, other]
Title: What Could be the Observational Signature of Dark Matter in Globular Clusters?
Comments: 18 pages, 2 figures
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics - Phenomenology (hep-ph)
[53]  arXiv:2001.01106 (replaced) [pdf, other]
Title: Long-term evolution of the Galilean satellites: the capture of Callisto into resonance
Comments: 22 pages, 13 figures, 6 sections. Accepted for publication in Astronomy & Astrophysics
Subjects: Earth and Planetary Astrophysics (astro-ph.EP)
[54]  arXiv:2001.02696 (replaced) [pdf, other]
Title: The Bolometric Quasar Luminosity Function at z = 0-7
Comments: Accepted by MNRAS. The code and data are available at this https URL
Subjects: Astrophysics of Galaxies (astro-ph.GA); Cosmology and Nongalactic Astrophysics (astro-ph.CO)
[55]  arXiv:2001.10003 (replaced) [pdf, other]
Title: Evolution of fractality and rotation in embedded star clusters
Comments: 12 pages, 11 figures, accepted on MNRAS
Subjects: Astrophysics of Galaxies (astro-ph.GA)
[56]  arXiv:2001.11517 (replaced) [pdf, ps, other]
Title: Detecting Helium Reionization with Fast Radio Bursts
Authors: Eric V. Linder
Comments: 8 pages, 8 figures; v2 minor clarifications in text and Fig. 3, matches PRD version
Journal-ref: Phys. Rev. D 101, 103019 (2020)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Astrophysical Phenomena (astro-ph.HE)
[57]  arXiv:2002.06924 (replaced) [pdf, other]
Title: New constraints on the magnetization of the cosmic web using LOFAR Faraday rotation observations
Comments: 13 pages, 8 figures, 2 tables. Accepted to MNRAS. Full version of Table 2 available at this https URL
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); Astrophysics of Galaxies (astro-ph.GA)
[58]  arXiv:2002.12382 (replaced) [pdf, other]
Title: Evidence for Cosmic Acceleration is Robust to Observed Correlations Between Type Ia Supernova Luminosity and Stellar Age
Comments: 9 pages, 3 figures, 3 tables. Accepted for publication in ApJL
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); Astrophysics of Galaxies (astro-ph.GA)
[59]  arXiv:2003.00685 (replaced) [pdf, other]
Title: The Multi-INstrument Burst ARchive (MINBAR)
Authors: D. K. Galloway (1), J. J. M. in 't Zand (2), J. Chenevez (3), H. Wörpel (4), L. Keek (5), L. Ootes (6), A. L. Watts (6), L. Gisler (1), C. Sanchez-Fernandez (7), E. Kuulkers (8) ((1) Monash University, (2) SRON, (3) DTU Space, (4) AIP Potsdam, (5) University of Maryland, (6) University of Amsterdam, (7) ESAC, Madrid (8) ESTEC, Noordwijk)
Comments: 108 pages, 34 figures, 18 tables; machine-readable sample data tables available via this https URL; web interface to sample data available via this http URL Added 2 new sources to burst table, other minor changes in response to referee report. Accepted by ApJS
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)
[60]  arXiv:2003.06405 (replaced) [pdf, other]
Title: 3HSP J095507.9+355101: a flaring extreme blazar coincident in space and time with IceCube-200107A
Comments: Submitted to A&A Letters, 5 pages, 4 figures
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)
[61]  arXiv:2003.08287 (replaced) [pdf, other]
Title: Magmatic intrusions control Io's crustal thickness
Comments: Accepted to JGR:Planets. 24 pages inc appendices and references. 7 figures
Subjects: Geophysics (physics.geo-ph); Earth and Planetary Astrophysics (astro-ph.EP)
[62]  arXiv:2004.00339 (replaced) [pdf, other]
Title: Lorentzian Quintessential Inflation
Comments: This essay is awarded second prize in the 2020 Essay Competition of the Gravity Research Foundation
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); General Relativity and Quantum Cosmology (gr-qc); High Energy Physics - Theory (hep-th)
[63]  arXiv:2004.01666 (replaced) [pdf, other]
Title: The Post-Limber Weak Lensing Bispectrum, Reduced Shear Correction, and Magnification Bias Correction
Comments: 12 pages, 4 figures. Accepted for publication in Phys. Rev. D
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
[64]  arXiv:2004.06841 (replaced) [pdf, other]
Title: On the Energy Coupling Efficiency of AGN Outbursts in Galaxy Clusters
Comments: 20 pages, 12 figures, slightly revised version, Accepted for publication in ApJ
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE); Astrophysics of Galaxies (astro-ph.GA)
[65]  arXiv:2004.07604 (replaced) [pdf, other]
Title: The XMM deep survey in the CDFS XI. X-ray properties of 185 bright sources
Comments: Accepted for publication in Astronomy & Astrophysics. Table 1 and Fig. 2 are available in electronic form the CDS. Typos corrected and some language editing and references added
Subjects: Astrophysics of Galaxies (astro-ph.GA); High Energy Astrophysical Phenomena (astro-ph.HE)
[66]  arXiv:2004.09513 (replaced) [pdf, other]
Title: PLATON II: New Capabilities And A Comprehensive Retrieval on HD 189733b Transit and Eclipse Data
Comments: replying to second referee report, fixed error in Figure 1
Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Instrumentation and Methods for Astrophysics (astro-ph.IM)
[67]  arXiv:2005.00801 (replaced) [pdf, other]
Title: The Physics of Star Cluster Formation and Evolution
Comments: 53 pages, 7 figures, preprint of a review to appear in Space Science Reviews Topical collection "Star formation". Changes in this version: updated comments line to to acceptance of the paper by the journal
Subjects: Astrophysics of Galaxies (astro-ph.GA); Solar and Stellar Astrophysics (astro-ph.SR)
[68]  arXiv:2005.04866 (replaced) [pdf, ps, other]
Title: Insights into the Formation and Evolution History of the Galactic Disk System
Comments: 17 pages, 12 figures, 3 tables, accepted for publication in ApJ
Subjects: Astrophysics of Galaxies (astro-ph.GA)
[69]  arXiv:2005.06479 (replaced) [pdf, other]
Title: Living with Neighbors. III. Scrutinizing the Spin$-$Orbit Alignment of Interacting Dark Matter Halo Pairs
Comments: 19 pages, 7 figures, and 7 tables, accepted for publication in ApJ
Subjects: Astrophysics of Galaxies (astro-ph.GA); Cosmology and Nongalactic Astrophysics (astro-ph.CO)
[70]  arXiv:2005.06535 (replaced) [pdf, other]
Title: The impact of non-Gaussianity on the Epoch of Reionization parameter forecast using 21-cm power spectrum measurements
Authors: Abinash Kumar Shaw (IIT KGP), Somnath Bharadwaj (IIT KGP), Rajesh Mondal (Sussex)
Comments: 16 pages, 7 figures, 3 tables, Comments are welcome
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
[71]  arXiv:2005.06603 (replaced) [pdf, other]
Title: OH level populations and accuracies of Einstein-A coefficients from hundreds of measured lines
Comments: 37 single-column pages and 14 figures, replacement due to publication of final paper in Atmos. Chem. Phys., changes related to DOI and journal reference
Journal-ref: Atmos.Chem.Phys. 20 (2020) 5269-5292
Subjects: Atmospheric and Oceanic Physics (physics.ao-ph); Earth and Planetary Astrophysics (astro-ph.EP)
[72]  arXiv:2005.07112 (replaced) [pdf, other]
Title: See Change: VLT spectroscopy of a sample of high-redshift Type Ia supernova host galaxies
Comments: Accepted for publication in MNRAS, corrected for repeated figure and minor text changes
Subjects: Astrophysics of Galaxies (astro-ph.GA); Cosmology and Nongalactic Astrophysics (astro-ph.CO)
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