Date: Thu, 30 Jul 20 00:34:56 GMT Subject: astro-ph daily 64 new + 7 crosses received by eprepget ------------------------------------------------------------------------------ ------------------------------------------------------------------------------ Send any comments regarding submissions directly to submitter. ------------------------------------------------------------------------------ Archives at http://arxiv.org/ To unsubscribe, e-mail To: astro-ph@arXiv.org, Subject: cancel ------------------------------------------------------------------------------ received by eprepget from Tue 28 Jul 20 18:00:00 GMT to Wed 29 Jul 20 18:00:00 GMT ------------------------------------------------------------------------------ \\ arXiv:2007.14395 Date: Tue, 28 Jul 2020 18:00:00 GMT (164kb,D) Title: How to Build a Catalogue of Linearly-Evolving Cosmic Voids Authors: Stephen Stopyra, Hiranya V. Peiris, Andrew Pontzen Categories: astro-ph.CO Comments: 9 pages, 5 figures \\ Cosmic voids provide a powerful probe of the origin and evolution of structures in the Universe because their dynamics can remain near-linear to the present day. As a result they have the potential to connect large scale structure at late times to early-Universe physics. Existing "watershed"-based algorithms, however, define voids in terms of their morphological properties at low redshift. The degree to which the resulting regions exhibit linear dynamics is consequently uncertain, and there is no direct connection to their evolution from the initial density field. A recent void definition addresses these issues by considering "anti-halos". This approach consists of inverting the initial conditions of an $N$-body simulation to swap overdensities and underdensities. After evolving the pair of initial conditions, anti-halos are defined by the particles within the inverted simulation that are inside halos in the original (uninverted) simulation. In this work, we quantify the degree of non-linearity of both anti-halos and watershed voids using the Zel'dovich approximation. We find that non-linearities are introduced by voids with radii less than $5\,\mathrm{Mpc}\,h^{-1}$, and that both anti-halos and watershed voids can be made into highly linear sets by removing these voids. \\ ( https://arxiv.org/abs/2007.14395 , 164kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14398 Date: Tue, 28 Jul 2020 18:00:00 GMT (5326kb,D) Title: The Hubble constant from eight time-delay galaxy lenses Authors: Philipp Denzel, Jonathan P. Coles, Prasenjit Saha, Liliya L. R. Williams Categories: astro-ph.CO Comments: 19 pages, 11 figures, submitted to MNRAS \\ We present a determination of the Hubble constant from the joint, free-form analysis of 8 strongly, quadruply lensing systems. In the concordance cosmology, we find $H_0 = 71.8^{+3.9}_{-3.3}\,\mathrm{km}\,\mathrm{s}^{-1}\,\mathrm{Mpc}^{-1}$ with a precision of $4.97\%$. This is in agreement with the latest measurements from Supernovae Type Ia and Planck observations of the cosmic microwave background. Our precision is lower compared to these and other recent time-delay cosmography determinations, because our modelling strategies reflect the systematic uncertainties of lensing degeneracies. We furthermore are able to find reasonable lensed image reconstructions by constraining to either value of $H_0$ from local and early Universe measurements. This leads us to conclude that current lensing constraints on $H_0$ are not strong enough to break the "Hubble tension" problem of cosmology. \\ ( https://arxiv.org/abs/2007.14398 , 5326kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14401 Date: Tue, 28 Jul 2020 18:00:01 GMT (1616kb,D) Title: A coupled guiding center-Boris particle pusher for magnetized plasmas in compact-object magnetospheres Authors: Fabio Bacchini, Bart Ripperda, Alexander A. Philippov, Kyle Parfrey Categories: astro-ph.HE Comments: Submitted to ApJS \\ We present a novel numerical scheme for simulating the motion of relativistic charged particles in magnetospheres of compact objects, typically filled with highly magnetized collisionless plasmas. The new algorithm is based on a dynamic switch between the full system of equations of motion and a guiding center approximation. The switch between the two formulations is based on the magnetization of the plasma particles, such that the dynamics are accurately captured by the guiding center motion even when the gyro-frequency is under-resolved by the time step. For particles with a large gyro-radius, due to acceleration in, e.g., reconnecting current sheets, the algorithm adaptively switches to solve the full equations of motion instead. The new scheme is directly compatible with standard Particle-in-Cell codes, and is readily applicable in curved spacetimes via a dedicated covariant formulation. We test the performance of the coupled algorithm by evolving charged particles in electromagnetic configurations of reconnecting current sheets in magnetized plasma, obtained from special- and general-relativistic Particle-in-Cell simulations. The new coupled pusher is capable of producing highly accurate particle trajectories even when the time step is many orders of magnitude larger than the gyro-period, substantially reducing the restrictions of the temporal resolution. \\ ( https://arxiv.org/abs/2007.14401 , 1616kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14402 Date: Tue, 28 Jul 2020 18:00:01 GMT (14523kb,D) Title: Very high redshift quasars and the rapid emergence of super-massive black holes Authors: Pavel Kroupa (Bonn, Prague), Ladislav Subr (Prague), Tereza Jerabkova (GRANTECAN+), Long Wang (Tokyo) Categories: astro-ph.GA Comments: 34 pages, 18 figures, MNRAS, in press \\ The observation of quasars at very high redshift such as Poniuaena is a challenge for models of super-massive black hole (SMBH) formation. This work presents a study of SMBH formation via known physical processes in star-burst clusters formed at the onset of the formation of their hosting galaxy. While at the early stages hyper-massive star-burst clusters reach the luminosities of quasars, once their massive stars die, the ensuing gas accretion from the still forming host galaxy compresses its stellar black hole (BH) component to a compact state overcoming heating from the BH--BH binaries such that the cluster collapses, forming a massive SMBH-seed within about a hundred Myr. Within this scenario the SMBH--spheroid correlation emerges near-to-exactly. The highest-redshift quasars may thus be hyper-massive star-burst clusters or young ultra-compact dwarf galaxies (UCDs), being the precursors of the SMBHs that form therein within about 200 Myr of the first stars. For spheroid masses <10^9.6 Msun a SMBH cannot form and instead only the accumulated nuclear cluster remains. The number evolution of the quasar phases with redshift is calculated and the possible problem of missing quasars at very high redshift is raised. SMBH-bearing UCDs and the formation of spheroids are discussed critically in view of the high redshift observations. A possible tension is found between the high star-formation rates (SFRs) implied by downsizing and the observed SFRs, which may be alleviated within the IGIMF theory and if the downsizing times are somewhat longer. \\ ( https://arxiv.org/abs/2007.14402 , 14523kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14403 Date: Tue, 28 Jul 2020 18:00:01 GMT (2496kb,D) Title: Gravitational wave background from extreme mass ratio inspirals Authors: Matteo Bonetti, Alberto Sesana Categories: astro-ph.GA astro-ph.CO gr-qc Comments: 19 pages, 12 figures, to be submitted to PRD \\ Extreme mass ratio inspirals (EMRIs), i.e. binary systems comprised by a compact stellar-mass object orbiting a massive black hole, are expected to be among the primary gravitational wave (GW) sources for the forthcoming LISA mission. The astrophysical processes leading to the formation of such systems still remain poorly understood, resulting into large uncertainties in the predicted cosmic rate of these sources, spanning at least three orders of magnitude. As LISA can individually resolve mostly EMRIs up to $z\gtrsim1$, the ensemble of signals below its detection threshold will add up incoherently forming an unresolved confusion noise, which can be formally described as a stochastic background. We perform an extensive study of this background by considering a collection of astrophysically motivated EMRI formation scenarios, spanning current uncertainties. We find that in fiducial EMRI models -- predicting hundreds of EMRI detections during mission operations -- a significant background comparable to the LISA noise emerges, affecting the performance of the instrument around 3 mHz. In extreme cases, this background can even "erase" the whole LISA sensitivity bucket in the 2-10 mHz frequency range. This points to the need of a better understanding of EMRIs' astrophysics for a full assessment of the LISA mission potential. \\ ( https://arxiv.org/abs/2007.14403 , 2496kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14404 Date: Tue, 28 Jul 2020 18:00:02 GMT (3178kb,D) Title: Detection of 15 bursts from FRB 180916.J0158+65 with the uGMRT Authors: Visweshwar Ram Marthi, Tasha Gautam, Dongzi Li, Hsiu-Hsien Lin, Robert Main, Arun Kumar Naidu, Ue-Li Pen and Robert Wharton Categories: astro-ph.HE Comments: 5 pages, 4 figures, submitted to MNRAS Letters \\ We report the findings of a uGMRT observing campaign on FRB 180916.J0158+65, discovered recently to show a 16.35-day periodicity of its active cycle. We observed the source at 550-750 MHz for $\sim 2$ hours each during three successive cycles at the peak of its expected active period. We find 0, 12, and 3 bursts respectively, implying a highly variable bursting rate even within the active phase. We consistently detect faint bursts with spectral energies only an order of magnitude higher than the Galactic burst source SGR~1935+2154. The times of arrival of the detected bursts rule out many possible aliased solutions, strengthening the findings of the 16.35-day periodicity. A short-timescale periodicity search returned no highly significant candidates. Two of the beamformer-detected bursts were bright enough to be clearly detected in the imaging data, achieving sub-arcsecond localization, and proving as a proof-of-concept for FRB imaging with the GMRT. We provide a $3\sigma$ upper limit of the persistent radio flux density at 650 MHz of $66~\mu{\rm Jy}$ which, combined with the EVN and VLA limits at 1.6~GHz, further constrains any potential radio counterpart. These results demonstrate the power of uGMRT for targeted observations to detect and localize known repeating FRBs. \\ ( https://arxiv.org/abs/2007.14404 , 3178kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14405 Date: Tue, 28 Jul 2020 18:00:02 GMT (10635kb,D) Title: The Atacama Cosmology Telescope: Delensed Power Spectra and Parameters Authors: Dongwon Han, Neelima Sehgal, Amanda MacInnis, Alexander van Engelen, Blake D. Sherwin, Mathew S. Madhavacheril, Simone Aiola, Nicholas Battaglia, James A. Beall, Daniel T. Becker, Erminia Calabrese, Steve K. Choi, Omar Darwish, Edward V. Denison, Jo Dunkley, Simone Ferraro, Anna E. Fox, Matthew Hasselfield, J. Colin Hill, Gene C. Hilton, Matt Hilton, Ren\'ee Hlo\v{z}ek, Johannes Hubmayr, John P. Hughes, Arthur Kosowsky, Jeff Van Lanen, Thibaut Louis, Kavilan Moodley, Sigurd Naess, Toshiya Namikawa, Federico Nati, John P. Nibarger, Michael D. Niemack, Lyman A. Page, Bruce Partridge, Frank J. Qu, Alessandro Schillaci, David N. Spergel, Suzanne Staggs, Emilie Storer, Edward J. Wollack Categories: astro-ph.CO hep-ph Comments: 29 pages, 17 figures \\ We present LCDM cosmological parameter constraints obtained from delensed microwave background power spectra. Lensing maps from a subset of DR4 data from the Atacama Cosmology Telescope (ACT) are used to undo the lensing effect in ACT spectra observed at 150 and 98 GHz. At 150 GHz, we remove the lensing distortion with an effective efficiency of 30% (TT), 30% (EE), 26% (TE) and 20% (BB); this results in detections of the delensing effect at 8.7 sigma (TT), 5.1 sigma (EE), 2.6 sigma (TE), and 2.4 sigma (BB) significance. The combination of 150 and 98 GHz TT, EE, and TE delensed spectra is well fit by a standard LCDM model. We also measure the shift in best-fit parameters when fitting delensed versus lensed spectra; while this shift does not inform our ability to measure cosmological parameters, it does provide a three-way consistency check among the lensing inferred from the best-fit parameters, the lensing in the CMB power spectrum, and the reconstructed lensing map. This shift is predicted to be zero when fitting with the correct model since both lensed and delensed spectra originate from the same region of sky. Fitting with a LCDM model and marginalizing over foregrounds, we find that the shift in cosmological parameters is consistent with zero. Our results show that gravitational lensing of the microwave background is internally consistent within the framework of the standard cosmological model. \\ ( https://arxiv.org/abs/2007.14405 , 10635kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14407 Date: Tue, 28 Jul 2020 18:00:04 GMT (283kb,D) Title: Soft X-ray emission lines in the X-ray binary Swift J1858.6-0814 observed with XMM-Newton-RGS: disc atmosphere or wind? Authors: D. J. K. Buisson, D. Altamirano, M. D\'iaz Trigo, M. Mendez, M. Armas Padilla, N. Castro Segura, N. D. Degenaar, J. van den Eijnden, F. A. Fogantini, P. Gandhi, C. Knigge, T. Mu\~noz-Darias, M. \"Ozbey Arabac{\i} and F. M. Vincentelli Categories: astro-ph.HE Comments: 10 pages, 7 figures, MNRAS accepted \\ We find soft X-ray emission lines from the X-ray binary Swift J1858.6-0814 in data from XMM-Newton-RGS: N VII, O VII and O VIII, as well as notable residuals short of a detection at Ne IX and other higher ionisation transitions. These could be associated with the disc atmosphere, as in accretion disc corona sources, or with a wind, as has been detected in Swift J1858.6-0814 in emission lines at optical wavelengths. Indeed, the N VII line is redshifted, consistent with being the emitting component of a P-Cygni profile. We find that the emitting plasma has an ionisation parameter $\log(\xi)=1.35\pm0.2$ and a density $n>1.5\times10^{11}$ cm$^{-3}$. From this, we infer that the emitting plasma must be within $10^{13}$ cm of the ionising source, $\sim5\times10^{7}r_{\rm g}$ for a $1.4M_{\odot}$ neutron star, and from the line width that it is at least $10^4r_{\rm g}$ away ($2\times10^{9}(M/1.4M_{\odot})$ cm). We compare this with known classes of emission line regions in other X-ray binaries and active galactic nuclei. \\ ( https://arxiv.org/abs/2007.14407 , 283kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14408 Date: Tue, 28 Jul 2020 18:00:04 GMT (6597kb,D) Title: A Diffuse Metal-Poor Component of the Sagittarius Stream Revealed by the H3 Survey Authors: Benjamin D. Johnson, Charlie Conroy, Rohan P. Naidu, Ana Bonaca, Dennis Zaritsky, Yuan-Sen Ting, Phillip A. Cargile, Jiwon Jesse Han, Joshua S. Speagle Categories: astro-ph.GA Comments: 18 pages, 12 figures, 1 table. Submitted to ApJ \\ The tidal disruption of the Sagittarius dwarf galaxy has generated a spectacular stream of stars wrapping around the entire Galaxy. We use data from $Gaia$ and the H3 Stellar Spectroscopic Survey to identify 823 high-quality Sagittarius members based on their angular momenta. The H3 Survey is largely unbiased in metallicity, and so our sample of Sagittarius members is similarly unbiased. Stream stars span a wide range in [Fe/H] from $-0.2$ to $\approx -3.0$, with a mean overall metallicity of $\langle$[Fe/H]$\rangle=-0.99$. We identify a strong metallicity-dependence to the kinematics of the stream members. At [Fe/H]$\gt -0.8$ nearly all members belong to the well-known cold ($\sigma_v \lt 20$ km/s) leading and trailing arms. At intermediate metallicities ($-1.9 \lt$[Fe/H]$\lt -0.8$) a significant population (24$\%$) emerges of stars that are kinematically offset from the cold arms. These stars also appear to have hotter kinematics. At the lowest metallicities ([Fe/H]$\lesssim-2$), the majority of stars (69$\%$) belong to this kinematically-offset diffuse population. Comparison to simulations suggests that the diffuse component was stripped from the Sagittarius progenitor at earlier epochs, and therefore resided at larger radius on average, compared to the colder metal-rich component. We speculate that this kinematically diffuse, low metallicity, population is the stellar halo of the Sagittarius progenitor system. \\ ( https://arxiv.org/abs/2007.14408 , 6597kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14410 Date: Tue, 28 Jul 2020 18:00:11 GMT (10491kb,D) Title: Double-peak emission line galaxies in the SDSS catalogue. A minor merger sequence Authors: Daniel Maschmann, Anne-Laure Melchior, Gary A. Mamon, Igor V. Chilingarian and Ivan Yu. Katkov Categories: astro-ph.GA Comments: 30 pages, 27 figures, article accepted to A&A \\ Mergers can be detected as double-peak narrow emission line galaxies but they are difficult to disentangle from disc rotations and gas outflows. We aim to properly detect such galaxies and distinguish the underlying mechanisms. Relying on RCSED, we developed an automated selection procedure and found 5663 double-peak emission line galaxies at z<0.34 corresponding to 0.8% of the parent database. To characterise these galaxies, we built a single-peak no-bias control sample (NBCS) with the same redshift and stellar mass distributions as the double-peak sample (DPS). These two samples are indeed very similar in terms of absolute magnitude, [OIII] luminosity, colour-colour diagrams, age and specific star formation rate, metallicity, and environment. We find an important excess of S0 galaxies in the DPS, not observed in the NBCS, and which cannot be accounted for by the environment, as most of these galaxies are isolated or in poor groups. Similarly, we find a relative deficit of pure discs in the DPS late-type galaxies, that are preferentially of Sa type. In parallel, we observe a systematic central excess of star formation and extinction for DP galaxies. Finally, there are noticeable differences in the kinematics: the gas velocity dispersion is correlated with the galaxy inclination in the NBCS, whereas this relation does not hold for the DPS. Furthermore, the DP galaxies show larger stellar velocity dispersions and they deviate from the Tully-Fisher relation for both late-type and S0 galaxies. These discrepancies can be reconciled if one considers the two peaks as two different components. Considering the morphological biases in favour, bulge-dominated galaxies and star-formation central enhancement, we suggest a scenario of multiple sequential minor mergers driving the increase of the bulge size, leading to larger fractions of S0 galaxies and a deficit of pure disc galaxies. \\ ( https://arxiv.org/abs/2007.14410 , 10491kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14412 Date: Tue, 28 Jul 2020 18:00:17 GMT (5431kb,D) Title: High resolution tomography for galaxy spectroscopic surveys with Angular Redshift Fluctuations Authors: Louis Legrand, Carlos Hern\'andez-Monteagudo, Marian Douspis, Nabila Aghanim, Ra\'ul E. Angulo Categories: astro-ph.CO Comments: 14 pages, 21 figures, submitted to A&A \\ In the context of next generation spectroscopic galaxy surveys, new observables of the distribution of matter are currently being developed. Among these we investigate the angular redshift fluctuations (ARF), which probe the information contained in the projected redshift distribution of galaxies. Relying on the Fisher formalism, we show how ARF will provide complementary cosmological information compared to traditional angular galaxy clustering. We test both the standard $\Lambda$CDM model and the wCDM extension. We find that the cosmological and galaxy bias parameters express different degeneracies when inferred from ARF or from angular galaxy clustering. As such, combining both observables breaks these degeneracies and greatly decreases the marginalised uncertainties, by a factor of at least two on most parameters for the $\Lambda$CDM and wCDM model. We find that the ARF combined with angular galaxy clustering are a great probe of dark energy by increasing the figure of merit of the $w_0$-$w_{\rm a}$ parameter set by a factor of more than 10 compared to angular galaxy clustering alone. Finally we compare ARF to the CMB lensing constraints on the galaxy bias parameters. We show that a joint analysis of ARF and angular galaxy clustering improves constraints by $\sim 40\%$ on galaxy bias compared to a joint analysis of angular galaxy clustering and CMB lensing. \\ ( https://arxiv.org/abs/2007.14412 , 5431kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14413 Date: Tue, 28 Jul 2020 18:00:49 GMT (4395kb,D) Title: Laboratory Demonstration of Spatial Linear Dark Field Control For Imaging Extrasolar Planets in Reflected Light Authors: Thayne Currie, Eugene Pluzhnik, Olivier Guyon, Ruslan Belikov, Kelsey Miller, Steven Bos, Jared Males, Dan Sirbu, Charlotte Bond, Richard Frazin, Tyler Groff, Brian Kern, Julien Lozi, Benjamin Mazin, Bijan Nemati, Barnaby Norris, Hari Subedi, Scott Will Categories: astro-ph.IM astro-ph.EP Comments: 13 pages, 7 figures, accepted for publication in Publications of the Astronomical Society of the Pacific \\ Imaging planets in reflected light, a key focus of future NASA missions and ELTs, requires advanced wavefront control to maintain a deep, temporally correlated null of stellar halo -- i.e. a dark hole -- at just several diffraction beam widths. Using the Ames Coronagraph Experiment testbed, we present the first laboratory tests of Spatial Linear Dark Field Control (LDFC) approaching raw contrasts ($\sim$ 5$\times$10$^{-7}$) and separations (1.5--5.2 $\lambda$/D) needed to image jovian planets around Sun-like stars with space-borne coronagraphs like WFIRST-CGI and image exo-Earths around low-mass stars with future ground-based 30m class telescopes. In four separate experiments and for a range of different perturbations, LDFC largely restores (to within a factor of 1.2--1.7) and maintains a dark hole whose contrast is degraded by phase errors by an order of magnitude. Our implementation of classical speckle nulling requires a factor of 2--5 more iterations and 20--50 DM commands to reach contrasts obtained by spatial LDFC. Our results provide a promising path forward to maintaining dark holes without relying on DM probing and in the low-flux regime, which may improve the duty cycle of high-contrast imaging instruments, increase the temporal correlation of speckles, and thus enhance our ability to image true solar system analogues in the next two decades. \\ ( https://arxiv.org/abs/2007.14413 , 4395kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14414 Date: Tue, 28 Jul 2020 18:00:58 GMT (8267kb,D) Title: Bi-abundance photoionization models of planetary nebulae: determining the amount of Oxygen in the metal rich component Authors: V. G\'omez-Llanos and C. Morisset Categories: astro-ph.GA Comments: Accepted for publication in MNRAS Journal-ref: Monthly Notices of the Royal Astronomical Society, staa2157, published 25 July 2020 DOI: 10.1093/mnras/staa2157 \\ We study the hypothesis of high metallicity clumps being responsible for the abundance discrepancy found in planetary nebulae between the values obtained from recombination and collisionaly excited lines. We generate grids of photoionization models combining cold metal-rich clumps emitting the heavy element recombination lines, embedded in a normal metallicity region responsible for the forbidden lines. The two running parameters of the grid are the metallicity of the clumps and its volume fraction relative to the whole nebula. We determine the density and temperatures (from the Balmer jump and the [OIII] 5007/4363 A line ratio), and the ionic abundances from the collisional and recombination lines, as an observer would do. The metallicity of the near-to-solar region is recovered, while the metallicity of the clumps is systematically underestimated, by up to 2 orders of magnitude. This is mainly because most of the H$\beta$ emission is coming from the "normal" region, and only the small contribution emitted by the metal-rich clumps should be used. We find that a given ADF(O$^{++}$) can be reproduced by a small amount of rich clumps, or a bigger amount of less rich clumps. Finally, comparing with the observations of NGC 6153 we find 2 models that reproduce its ADF(O$^{++}$) and the observed electron temperatures. We determine the fraction of oxygen embedded in the metal-rich region (with a fraction of volume less than 1%) to be roughly between 25% and 60% of the total amount of oxygen in the nebula (a few 10$^{-3} M_\odot$). \\ ( https://arxiv.org/abs/2007.14414 , 8267kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14416 Date: Tue, 28 Jul 2020 18:05:01 GMT (42826kb,D) Title: Measuring accretion disk sizes of lensed quasars with microlensing time delay in multi-band light curves Authors: J.H.H. Chan, K. Rojas, M. Millon, F. Courbin, V. Bonvin, G. Jauffret Categories: astro-ph.GA Comments: 10 pages, 9 figures \\ Time-delay cosmography in strongly lensed quasars offer an independent way of measuring the Hubble constant, $H_0$. However, it has been proposed that the combination of microlensing and source-size effects, also known as microlensing time delay can potentially increase the uncertainty in time-delay measurements as well as lead to a biased time delay. In this work, we first investigate how microlensing time delay changes with assumptions on the initial mass function (IMF) and find that the more massive microlenses produce the sharper distributions of microlensing time delays. However, we also find that the magnification probability distributions for different IMFs are indistinguishable from each other. Second, we present a new method to measure the color-dependent source size in lensed quasars using the microlensing time delays inferred from multi-band light curves. In practice the relevant observable is the differential microlensing time delays between different bands. We show from simulation using the LSST-like facility that if this differential time delay between bands can be measured with a precision of $0.1$ days in any given lensed image, the disk size can be recovered to within a factor of $2$. If four lensed images are used, our method is able to achieve an unbiased source measurement within error of the order of $20\%$, which is comparable with other techniques. \\ ( https://arxiv.org/abs/2007.14416 , 42826kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14428 Date: Tue, 28 Jul 2020 18:27:58 GMT (18060kb) Title: An Eruptive Circular-ribbon Flare with Extended Remote Brightenings Authors: Chang Liu, Avijeet Prasad, Jeongwoo Lee, Haimin Wang Categories: astro-ph.SR Comments: 12 pages, 7 figures, Accepted to ApJ \\ We study an eruptive X1.1 circular-ribbon flare on 2013 November 10, combining multiwavelength observations with a coronal field reconstruction using a non-force-free field method. In the first stage, a filament forms via magnetic reconnection between two mildly twisted sheared arcades, which are embedded under the fan dome associated with a null point. This reconnection seems to be driven by photospheric shearing and converging flows around the inner two arcade footpoints, consistent with the flare-related changes of transverse field. The southern portion of the filament rises upward due to torus instability and pushes against the null point. The induced null point reconnection then generates the circular ribbon and the initial remote brightening in the west, as accelerated electrons precipitate along the fan and propagate outward along quasi-separatix surfaces with high values of the squashing factor (Q) in the envelope fields, which have a curtain-like shape here. In the second stage, the southern end of the flux rope breaks away from the surface, sequentially disrupts the dome and overlying fields, and erupts in a whipping-like fashion to become a partial halo coronal mass ejection. This leads to an enhanced flare emission and fast-moving remote brightenings at the footpoints of the magnetic curtain, which span a remarkably broad region and are also associated with coronal dimmings. This is a rare example of eruptive circular-ribbon flares, in which the evolution of a flux rope from its formation to successful eruption out of the dome and the resulting unusually extended remote brightenings are completely observed. \\ ( https://arxiv.org/abs/2007.14428 , 18060kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14439 Date: Tue, 28 Jul 2020 19:18:11 GMT (2803kb,D) Title: An analytic model for OIII fine structure emission from high redshift galaxies Authors: Shengqi Yang, Adam Lidz Categories: astro-ph.GA \\ Recent ALMA measurements have revealed bright OIII 88 micron line emission from galaxies during the Epoch of Reionization (EoR) at redshifts as large as $z \sim 9$. We introduce an analytic model to help interpret these and other upcoming OIII 88 micron measurements. Our approach sums over the emission from discrete Str$\ddot{\mathrm{o}}$mgren spheres and considers the total volume of ionized hydrogen in a galaxy of a given star-formation rate. We estimate the relative volume of doubly-ionized oxygen and ionized hydrogen and its dependence on the spectrum of ionizing photons. We then calculate the level populations of OIII ions in different fine-structure states for HII regions of specified parameters. In this simple model, a galaxy's OIII 88 micron luminosity is determined by: the typical number density of free electrons in HII regions ($n_e$), the average metallicity of these regions ($Z$), the rate of hydrogen ionizing photons emitted ($Q_{\mathrm{HI}}$), and the shape of the ionizing spectrum. We cross-check our model by comparing it with detailed CLOUDY calculations, and find that it works to better than 15$\%$ accuracy across a broad range of parameter space. Applying our model to existing ALMA data at $z \sim 6-9$, we derive lower bounds on the gas metallicity and upper bounds on the gas density in the HII regions of these galaxies. These limits vary considerably from galaxy to galaxy, with the tightest bounds indicating $Z \gtrsim 0.5 Z_\odot$ and $n_{\mathrm{H}} \lesssim 50$ cm$^{-3}$ at $2-\sigma$ confidence. \\ ( https://arxiv.org/abs/2007.14439 , 2803kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14473 Date: Tue, 28 Jul 2020 20:30:27 GMT (13650kb,D) Title: Architectures of Exoplanetary Systems: Eccentricity and Mutual Inclination Distributions of AMD-Stable Planetary Systems Authors: Matthias Y. He, Eric B. Ford, Darin Ragozzine, and Daniel Carrera Categories: astro-ph.EP Comments: Submitted to AAS Journals; 40 pages, 14 figures, plus supplemental online materials with 8 figures \\ The angular momentum deficit (AMD) of a planetary system is a measure of its orbital excitation and a predictor of long-term stability. We adopt the AMD-stability criteria to constrain the orbital architectures for exoplanetary systems. Previously, He, Ford, & Ragozzine (2019) (arXiv:1907.07773v2) showed through forward modelling (SysSim) that the observed multiplicity distribution can be well reproduced by two populations consisting of a low and a high mutual inclination component. Here, we show that a broad distribution of mutual inclinations arising from systems at the AMD-stability limit can also match the observed Kepler population. We show that distributing a planetary system's maximum AMD amongst its planets results in a multiplicity-dependent distribution of eccentricities and mutual inclinations. Systems with intrinsically more planets have lower median eccentricities and mutual inclinations, and this trend is well described by power-law functions of the intrinsic planet multiplicity ($n$): $\tilde{\mu}_{e,n} \propto n^{-1.74_{-0.07}^{+0.11}}$ and $\tilde{\mu}_{i,n} \propto n^{-1.73_{-0.08}^{+0.09}}$, where $\tilde{\mu}_{e,n}$ and $\tilde{\mu}_{i,n}$ are the medians of the eccentricity and inclination distributions. We also find that intrinsic single planets have higher eccentricities ($\sigma_{e,1} \sim 0.25$) than multi-planet systems, and that the trends with multiplicity appear in the observed distributions of period-normalized transit duration ratios. We show that the observed preferences for planet size orderings and uniform spacings are more extreme than what can be produced by the detection biases of the Kepler mission alone. Finally, we find that for systems with detected transiting planets between 5 and 10d, there is another planet with a greater RV signal $\simeq~53\%$ of the time. \\ ( https://arxiv.org/abs/2007.14473 , 13650kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14484 Date: Tue, 28 Jul 2020 21:05:44 GMT (1398kb,D) Title: Validation of Emission-Line Galaxies Target Selection Algorithms for the Dark Energy Spectroscopic Instrument Using the MMT Binospec Authors: Tanveer Karim (1), Jae H. Lee (2 and 3), Daniel J. Eisenstein (1), Etienne Burtin (4), John Moustakas (5), Anand Raichoor (6), Christophe Y\`eche (4) (for the DESI collaboration, (1) Department of Astronomy, Harvard University, (2) Department of Physics, Harvard University, (3) Vertex Pharmaceuticals, (4) IRFU, CEA, Universit\'e Paris-Saclay, (5) Department of Physics and Astronomy, Siena College, (6) Institute of Physics, Laboratory of Astrophysics, \'Ecole Polytechnique F\'ed\'erale de Lausanne) Categories: astro-ph.GA astro-ph.CO Comments: 16 pages, 9 figures, Accepted by the MNRAS on 2020 July 27 \\ The forthcoming Dark Energy Spectroscopic Instrument (DESI) experiment plans to measure the effects of dark energy on the expansion of the Universe and create a $3$D map of the Universe using galaxies up to $z \sim 1.6$ and QSOs up to $z \sim 3.5$. In order to create this map, DESI will obtain spectroscopic redshifts of over $30$ million objects; among them, a majority are \oii emitting star-forming galaxies known as emission-line galaxies (ELGs). These ELG targets will be pre-selected by drawing a selection region on the $g - r$ vs. $r - z$ colour-colour plot, where high redshift ELGs form a separate locus from the lower redshift ELGs and interlopers. In this paper, we study the efficiency of three ELG target selection algorithms -- the final design report (FDR) cut based on the DEEP2 photometry, Number Density Modelling and Random Forest -- to determine how the combination of these three algorithms can be best used to yield a simple selection boundary that will be best suited to meet DESI's science goals. To do this, we selected $17$ small patches in the DESI footprint where we run the three target selection algorithms to pre-select ELGs based on their photometry. We observed the pre-selected ELGs using the MMT Binospec, which is similar in functionality to the DESI instrument, to obtain their spectroscopic redshifts and fluxes of $1054$ ELGs. By analysing the redshift and fluxing distribution of these galaxies, we find that although NDM performed the best, simple changes in the FDR definition would also yield sufficient performance. \\ ( https://arxiv.org/abs/2007.14484 , 1398kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14493 Date: Tue, 28 Jul 2020 21:21:25 GMT (1564kb) Title: A Volatile-Poor Formation of LHS 3844b based on its Lack of Significant Atmosphere Authors: Stephen R. Kane, Rachael M. Roettenbacher, Cayman T. Unterborn, Bradford J. Foley, Michelle L. Hill Categories: astro-ph.EP Comments: 23 pages, 14 figures, accepted for publication in the Planetary Science Journal \\ Exoplanet discoveries have reached into the realm of terrestrial planets that are becoming the subject of atmospheric studies. One such discovery is LHS 3844b, a 1.3 Earth radius planet in a 0.46 day orbit around an M4.5-5 dwarf star. Follow-up observations indicate that the planet is largely devoid of substantial atmosphere. This lack of significant atmosphere places astrophysical and geophysical constraints on LHS 3844b, primarily the degree of volatile outgassing and the rate of atmosphere erosion. We estimate the age of the host star as $7.8\pm1.6$ Gyrs and find evidence of an active past comparable to Proxima Centauri. We use geodynamical models of volcanic outgassing and atmospheric erosion to show that the apparent lack of atmosphere is consistent with a volatile-poor mantle for LHS 3844b. We show the core is unlikely to host enough C to produce a sufficiently volatile-poor mantle, unless the bulk planet is volatile-poor relative to Earth. While we cannot rule out a giant impact stripping LHS 3844b's atmosphere, we show this mechanism would require significant mantle stripping, potentially leaving LHS 3844b as an Fe-rich "super-Mercury". Atmospheric erosion by smaller impacts is possible, but only if the planet has already begun degassing and is bombarded by $10^3$ impactors of radius 500-1000 km traveling at escape velocity. We discuss formation and migration scenarios that could account for a volatile poor origin, including the potential for an unobserved massive companion planet. A relatively volatile-poor composition of LHS 3844b suggests that the planet formed interior to the system snow-line. \\ ( https://arxiv.org/abs/2007.14493 , 1564kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14499 Date: Tue, 28 Jul 2020 21:55:14 GMT (7580kb,D) Title: Mitigating contamination in LSS surveys: a comparison of methods Authors: Noah Weaverdyck and Dragan Huterer Categories: astro-ph.CO Comments: 33 pages; Plan of work in Fig 1, key results in Figs. 10-11; Comments welcome \\ Future large scale structure surveys will measure the locations and shapes of billions of galaxies. The precision of such catalogs will require meticulous treatment of systematic contamination of the observed fields. We compare several existing methods for removing such systematics from galaxy clustering measurements. We show how all the methods, including the popular pseudo-$C_\ell$ Mode Projection and Template Subtraction methods, can be interpreted under a common regression framework and use this to suggest improved estimators. We show how methods designed to mitigate systematics in the power spectrum can be used to produce clean maps, which are necessary for cosmological analyses beyond the power spectrum, and we extend current methods to treat the next-order multiplicative contamination in observed maps and power spectra. Two new mitigation methods are proposed, which incorporate desirable features of current state-of-the-art methods while being simpler to implement. Investigating the performance of all the methods on a common set of simulated measurements from Year 5 of the Dark Energy Survey, we test their robustness to various analysis cases. Our proposed methods produce improved maps and power spectra when compared to current methods, while requiring almost no user tuning. We end with recommendations for systematics mitigation in future surveys, and note that the methods presented are generally applicable beyond the galaxy distribution to any field with spatial systematics. \\ ( https://arxiv.org/abs/2007.14499 , 7580kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14517 Date: Tue, 28 Jul 2020 22:59:48 GMT (237kb,D) Title: A Gravitational Redshift Measurement of the White Dwarf Mass-Radius Relation Authors: Vedant Chandra, Hsiang-Chih Hwang, Nadia L. Zakamska, Sihao Cheng Categories: astro-ph.SR astro-ph.GA Comments: 11 pages, 5 figures. Accepted to ApJ \\ The mass-radius relation of white dwarfs is largely determined by the equation of state of degenerate electrons, which causes the stellar radius to decrease as mass increases. Here we observationally measure this relation using the gravitational redshift effect, a prediction of general relativity that depends on the ratio between stellar mass and radius. Using observations of over three thousand white dwarfs from the Sloan Digital Sky Survey and the Gaia space observatory, we derive apparent radial velocities from absorption lines, stellar radii from photometry and parallaxes, and surface gravities by fitting atmospheric models to spectra. By averaging the apparent radial velocities of white dwarfs with similar radii and, independently, surface gravities, we cancel out random Doppler shifts and measure the underlying gravitational redshift. Using these results, we empirically measure the white dwarf mass-radius relation across a wide range of stellar masses. Our results are consistent with leading theoretical models, and our methods could be used with future observations to empirically constrain white dwarf core composition and evolution. \\ ( https://arxiv.org/abs/2007.14517 , 237kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14522 Date: Tue, 28 Jul 2020 23:18:41 GMT (376kb) Title: Orbits and Individual Masses of Some Visual Binaries Authors: Essam A. Elkholy, Waleed H. Elsanhoury and Mohamed I. Nouh Categories: astro-ph.SR Comments: 14 pages, 4 figures, 5 tables \\ The orbits of visual binary systems still attract many of the working groups in astronomy. These orbits are the most important and reliable source of the stellar masse. In the present paper, we are going to compute orbits and dynamical masses of some visual binaries using an independent code. We used Kowalsky method to compute the geometrical elements. The dynamical elements (the period and the time of the periastron passage) are computed by implementing the double areal constant. We used the developed code to calculate the orbits for the four visual binaries, WDS J02262+3428, WDS J14310-0548, WDS J17466-0354, and WDS J12422+2622. We introduced a new orbit of the neglected visual binary WDS J17466-0354 and modified orbits for the rest three binaries. Using the Gaia DR2 parallaxes we computed the total masses of the systems. Comparing the adopted total masses with those derived from the spectral type relation revealed good agreement. \\ ( https://arxiv.org/abs/2007.14522 , 376kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14530 Date: Wed, 29 Jul 2020 00:02:15 GMT (4489kb,D) Title: Implementing multi-wavelength fringe tracking for the Large Binocular Telescope Interferometer's phase sensor, PHASECam Authors: Erin R. Maier, Phil Hinz, Denis Defr\`ere, Paul Grenz, Elwood Downey, Steve Ertel, Katie Morzinski, and Ewan S. Douglas Categories: astro-ph.IM Comments: 22 pages, 11 figures, accepted for publication by JATIS Journal-ref: J. Astron. Telesc. Instrum. Syst. 6(3), 035001 (2020) DOI: 10.1117/1.JATIS.6.3.035001. \\ PHASECam is the fringe tracker for the Large Binocular Telescope Interferometer (LBTI). It is a near-infrared camera which is used to measure both tip/tilt and fringe phase variations between the two adaptive optics (AO) corrected apertures of the Large Binocular Telescope (LBT). Tip/tilt and phase sensing are currently performed in the $H$ (1.65 $\mu$m) and $K$ (2.2 $\mu$m) bands at 1 kHz, but only the $K$-band phase telemetry is used to send corrections to the system in order to maintain fringe coherence and visibility. However, due to the cyclic nature of the fringe phase, only the phase, modulo 360 deg, can be measured. PHASECam's phase unwrapping algorithm, which attempts to mitigate this issue, occasionally fails in the case of fast, large phase variations or low signal-to-noise ratio. This can cause a fringe jump, in which case the OPD correction will be incorrect by a wavelength. This can currently be manually corrected by the operator. However, as the LBTI commissions further modes which require robust, active phase control and for which fringe jumps are harder to detect, including multi-axial (Fizeau) interferometry and dual-aperture non-redundant aperture masking interferometry, a more reliable and automated solution is desired. We present a multi-wavelength method of fringe jump capture and correction which involves direct comparison between the $K$-band and $H$-band phase telemetry. We demonstrate the method utilizing archival PHASECam telemetry, showing it provides a robust, reliable way of detecting fringe jumps which can potentially recover a significant fraction of the data lost to them. \\ ( https://arxiv.org/abs/2007.14530 , 4489kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14547 Date: Wed, 29 Jul 2020 01:45:40 GMT (108kb) Title: An X-ray Luminosity-dependent "Changing-look" Phenomenon in UGC\,3223 Authors: J. Wang, D. W. Xu and J. Y. Wei Categories: astro-ph.GA Comments: 9 pages, 3 figures and 3 tables, accepted by ApJ \\ The nature of the rare "Changing-look" (CL) phenomenon in active galactic nuclei (AGNs) is still under debate at current stage. We here present \it Swift/\rm XRT and UVOT follow-up observations of UGC\,3223, a newly discovered repeat CL-AGN with type transitions of $\mathrm{S1.5\rightarrow S2 \rightarrow S1.8}$ occurring in a period of about 30 years. By comparing the values previously reported in the \it ROSAT \rm All-sky Survey and in the second Swift-XRT Point Source catalog, we clearly find that the X-ray flux tightly follows the optical spectral transition, in which a spectral type closer to a Seyfert 1 type is associated with a higher X-ray flux. An invariable X-ray spectral shape is, however, found in the CL phenomenon of the object. An extremely low Eddington ratio of $\sim2\times10^{-4}$ can be obtained from the X-ray luminosity for its Seyfert 2 state, which suggests a favor of the disk-wind broad-line region model in explaining the CL phenomenon. A variation of the total UV emission is not revealed when compared to the previous \it GALEX \rm NUV observation, since the UVOT images indicate that $\sim90$\% UV emission comes from the intensive star formation in the host galaxy. \\ ( https://arxiv.org/abs/2007.14547 , 108kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14559 Date: Wed, 29 Jul 2020 02:40:50 GMT (658kb) Title: Has LIGO Detected Primordial Black Hole Dark Matter? -- Tidal Disruption in Binary Black Hole Formation Authors: Yuan Gao, Xiaojia Zhang and Meng Su Categories: astro-ph.HE \\ The frequent detection of binary mergers of $\sim 30 M_{\odot}$ black holes (BHs) by the Laser Interferometer Gravitational-Wave Observatory (LIGO) rekindled researchers' interest in primordial BHs (PBHs) being dark matter (DM). In this work, we looked at PBHs distributed as DM with a monochromatic mass of $30 M_{\odot}$ and examined the encounter-capture scenario of binary formation, where the densest central region of DM halo dominates. Thus, we paid special attention to the tidal effect by the supermassive black hole (SMBH) present. In doing so, we discovered a necessary tool called loss zone that complements the usage of loss cone. We found that the tidal effect is not prominent in affecting binary formation, which also turned out insufficient in explaining the totality of LIGO's event rate estimation, especially due to a microlensing event constraining the DM fraction in PBH at the mass of interest from near unity to an order smaller. Meanwhile, early-universe binary formation scenario proves so prevailing that the LIGO signal in turn constrains the PBH fraction below one percent. Thus, people should put more faith in alternative PBH windows and other DM candidates. \\ ( https://arxiv.org/abs/2007.14559 , 658kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14571 Date: Wed, 29 Jul 2020 03:24:02 GMT (1076kb,D) Title: X-ray Observations of a [C II]-bright, z=6.59 Quasar/Companion System Authors: Thomas Connor, Eduardo Ba\~nados, Chiara Mazzucchelli, Daniel Stern, Roberto Decarli, Xiaohui Fan, Emanuele Paolo Farina, Elisabeta Lusso, Marcel Neeleman, and Fabian Walter Categories: astro-ph.GA astro-ph.HE Comments: 11 pages, 4 figures. Accepted for publication in ApJ \\ We present deep Chandra observations of PSO J231.6576$-$20.8335, a quasar at redshift z=6.59 with a nearby (${\sim}8$ proper kpc) companion galaxy. ALMA observed both the quasar and companion to be bright in [C II], and the system has significant extended Ly$\alpha$ emission around the quasar, suggesting that a galaxy merger is ongoing. Unlike previous studies of two similar systems, and despite observing the system with Chandra for 140 ks, we do not detect the companion in X-rays. The quasar itself is detected, but only $13.3^{+4.8}_{-3.7}$ net counts are observed. From a basic spectral analysis, the X-ray spectrum of the quasar is soft (hardness ratio of $\mathcal{HR} = -0.60_{-0.27}^{+0.17}$, power-law index of $\Gamma=2.6^{+1.0}_{-0.9}$), which results in a rest-frame X-ray luminosity comparable to other bright quasars ($L_{2-10} = 1.09^{+2.20}_{-0.70}\times 10^{45}\ \textrm{erg}\ \textrm{s}^{-1}$) despite the faint observed X-ray flux. We highlight two possible interpretations of this result: the quasar has a steep value of $\Gamma$ -- potentially related to observed ongoing Eddington accretion -- thereby pushing much of the emission out of our observed band, or the quasar has a more normal spectrum ($\Gamma{\sim}2$) but is therefore less X-ray luminous ($L_{2-10} \sim 0.6 \times 10^{45}\ \textrm{ erg}\ \textrm{ s}^{-1}$). \\ ( https://arxiv.org/abs/2007.14571 , 1076kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14577 Date: Wed, 29 Jul 2020 03:44:50 GMT (2014kb,D) Title: The tidal remnant of an unusually metal-poor globular cluster Authors: Zhen Wan, Geraint F. Lewis, Ting S. Li, Jeffrey D. Simpson, Sarah L. Martell, Daniel B. Zucker, Jeremy R. Mould, Denis Erkal, Andrew B. Pace, Dougal Mackey, Alexander P. Ji, Sergey E. Koposov, Kyler Kuehn, Nora Shipp, Eduardo Balbinot, Joss Bland-Hawthorn, Andrew R. Casey, Gary S. Da Costa, Prajwal Kafle, Sanjib Sharma and Gayandhi M. De Silva Categories: astro-ph.GA Comments: Authors' version of an Article published in Nature on July 29th, 2020 DOI: 10.1038/s41586-020-2483-6 \\ Globular clusters are some of the oldest bound stellar structures observed in the Universe. They are ubiquitous in large galaxies and are believed to trace intense star formation events and the hierarchical build-up of structure. Observations of globular clusters in the Milky Way, and a wide variety of other galaxies, have found evidence for a `metallicity floor', whereby no globular clusters are found with chemical (`metal') abundances below approximately 0.3 to 0.4 per cent of that of the Sun. The existence of this metallicity floor may reflect a minimum mass and a maximum redshift for surviving globular clusters to form, both critical components for understanding the build-up of mass in the universe. Here we report measurements from the Southern Stellar Streams Spectroscopic Survey of the spatially thin, dynamically cold Phoenix stellar stream in the halo of the Milky Way. The properties of the Phoenix stream are consistent with it being the tidally disrupted remains of a globular cluster. However, its metal abundance ([Fe/H] = -2.7) is substantially below that of the empirical metallicity floor. The Phoenix stream thus represents the debris of the most metal-poor globular cluster discovered so far, and its progenitor is distinct from the present-day globular cluster population in the local Universe. Its existence implies that globular clusters below the metallicity floor have probably existed, but were destroyed during Galactic evolution. \\ ( https://arxiv.org/abs/2007.14577 , 2014kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14600 Date: Wed, 29 Jul 2020 05:06:01 GMT (1093kb) Title: NuSTAR View of TeV Blazar Mrk 501 Authors: Ashwani Pandey Categories: astro-ph.HE Comments: 13 pages, 3 figures, 3 tables, published in special issue "X-Ray Flux and Spectral Variability of Blazars" of Galaxies journal Journal-ref: Galaxies 2020, 8(3), 55 DOI: 10.3390/galaxies8030055 \\ We report the results of flux and spectral variability studies of all seven {\it Nuclear Spectroscopic Telescope Array (NuSTAR)} observations of TeV $\gamma-$ray emitting blazar Markarian (or Mrk) 501. We found strong evidence of intraday variability in 3-79 keV X-ray light curves (LCs) of Mrk 501 during four out of these seven observations. We examined spectral variability using a model-independent hardness-ratio analysis and found a general "harder-when-brighter" behaviour in two observations. We also investigated the nature of 3-79 keV X-ray spectra of TeV blazar Mrk 501 and found that five out of seven spectra are well described by the curved log-parabola models with photon indices (at 10 keV) $\alpha \sim$ 2.12-2.32 and a curvature $\beta \sim$ 0.15-0.28. The two other spectra are somewhat better represented by simple power-law models with photon indices 2.70 and 2.75. We briefly discuss available physical models to explain our results. \\ ( https://arxiv.org/abs/2007.14600 , 1093kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14607 Date: Wed, 29 Jul 2020 05:21:30 GMT (4465kb,D) Title: The thermal-radiative wind in the neutron star low mass X-ray binary GX 13+1 Authors: Ryota Tomaru, Chris Done, Ken Ohsuga, Hirokazu Odaka, and Tadayuki Takahashi Categories: astro-ph.HE Comments: 12pages, 13 figures, accepted by MNRAS DOI: 10.1093/mnras/staa2254 \\ We fit the observed high ionisation X-ray absorption lines in the neutron star binary GX13+1 with a full simulation of a thermal-radiative wind. This uses a radiation hydrodynamic code coupled to Monte Carlo radiation transfer to compute the observed line profiles from Hydrogen and Helium-like iron and Nickel, including all strong K{\alpha} and K{\beta} transitions. The wind is very strong as this object has a very large disc and is very luminous. The absorption lines from Fe K{\alpha} are strongly saturated as the ion columns are large, so the line equivalent widths (EWs) depend sensitively on the velocity structure. We additionally simulate the lines including isotropic turbulence at the level of the azimuthal and radial velocities. We fit these models to the Fe xxv and xxvi absorption lines seen in the highest resolution Chandra third order HETGS data. These data already rule out the addition of turbulence at the level of the radial velocity of ~500 km/s. The velocity structure predicted by the thermal-radiative wind alone is a fairly good match to the observed profile, with an upper limit to additional turbulence at the level of the azimuthal velocity of ~100 km/s. This gives stringent constraints on any remaining contribution from magnetic acceleration. \\ ( https://arxiv.org/abs/2007.14607 , 4465kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14609 Date: Wed, 29 Jul 2020 05:29:06 GMT (4482kb) Title: Magnetic fields in late-stage proto-neutron stars Authors: S. K. Lander, P. Haensel, B. Haskell, J. L. Zdunik, M. Fortin Categories: astro-ph.HE astro-ph.SR Comments: 20 pages, 16 figures \\ We explore the thermal and magnetic-field structure of a late-stage proto-neutron star. We find the dominant contribution to the entropy in different regions of the star, from which we build a simplified equation of state for the hot neutron star. With this, we numerically solve the stellar equilibrium equations to find a range of models, including magnetic fields and rotation up to Keplerian velocity. We argue that the equation of state is effectively barotropic for this problem. For fixed magnetic-field strength, the induced ellipticity increases with temperature; we give quantitative formulae for this. The Keplerian velocity is considerably lower for hotter stars, which may set a de-facto maximum rotation rate for non-recycled NSs well below 1 kHz. The qualitative magnetic-field structure is similar for hot and cold stars, with the poloidal field component dominating over the toroidal one; we argue this result may be universal. We show that truncating magnetic-field solutions at low multipoles leads to serious inaccuracies, especially for models with rapid rotation or a strong toroidal-field component. \\ ( https://arxiv.org/abs/2007.14609 , 4482kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14624 Date: Wed, 29 Jul 2020 06:24:46 GMT (1543kb,D) Title: An efficient hybrid method to produce high resolution large volume dark matter simulations for semi-analytic models of reionisation Authors: Yisheng Qiu, Simon J. Mutch, Pascal J. Elahi, J. Stuart B. Wyithe Categories: astro-ph.GA Comments: 14 pages, 13 figures. Submitted to MNRAS \\ Resolving faint galaxies in large volumes is critical for accurate cosmic reionisation simulations. While less demanding than hydrodynamical simulations, semi-analytic reionisation models still require very large N-body simulations in order to resolve the atomic cooling limit across the whole reionisation history within box sizes $\gtrsim 100 h^{-1}\text{Mpc}$. To facilitate this, we extend the mass resolution of N-body simulations using a Monte Carlo algorithm. Our extended halo catalogues are designed for semi-analytic galaxy formation models that utilise halo positions for reionisation calculations. To illustrate, we present an extended halo catalogue that reaches a mass resolution of $M_\text{halo} = 3.2 \times 10^7 h^{-1}\text{M}_\odot$ in a $105 h^{-1}\text{Mpc}$ box, equivalent to an N-body simulation with $\sim 6800^3$ particles. The results are verified using smaller volume N-body simulations with higher resolution. The extended halo catalogues are applied to the Meraxes semi-analytic reionisation model, producing stellar mass functions, star formation rate densities and volume-weighted neutral fractions that are consistent with those based on direct N-body halo merger trees up to $z \sim 10$. Comparison of high resolution large volume simulations with both small volume or low resolution simulations indicates that both low resolution and small volume simulations lead to reionisation ending too rapidly. Thus, both sufficient resolution and volume are required to correctly model the late stage of cosmic reionisation. \\ ( https://arxiv.org/abs/2007.14624 , 1543kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14648 Date: Wed, 29 Jul 2020 07:49:51 GMT (3207kb) Title: Radio Echo in the Turbulent Corona and Simulations of Solar Drift-Pair Radio Bursts Authors: Alexey A. Kuznetsov, Nicolina Chrysaphi, Eduard P. Kontar, and Galina Motorina Categories: astro-ph.SR physics.plasm-ph physics.space-ph Comments: 13 pages, 7 figures DOI: 10.3847/1538-4357/aba04a \\ Drift-pair bursts are an unusual type of solar low-frequency radio emission, which appear in the dynamic spectra as two parallel drifting bright stripes separated in time. Recent imaging spectroscopy observations allowed for the quantitative characterization of the drifting pairs in terms of source size, position, and evolution. Here, the drift-pair parameters are qualitatively analyzed and compared with the newly-developed Monte Carlo ray-tracing technique simulating radio-wave propagation in the inhomogeneous anisotropic turbulent solar corona. The results suggest that the drift-pair bursts can be formed due to a combination of the refraction and scattering processes, with the trailing component being the result of turbulent reflection (turbulent radio echo). The formation of drift-pair bursts requires an anisotropic scattering with the level of plasma density fluctuations comparable to that in type III bursts, but with a stronger anisotropy at the inner turbulence scale. The anisotropic radio-wave scattering model can quantitatively reproduce the key properties of drift-pair bursts: the apparent source size and its increase with time at a given frequency, the parallel motion of the source centroid positions, and the delay between the burst components. The trailing component is found to be virtually co-spatial and following the main component. The simulations suggest that the drift-pair bursts are likely to be observed closer to the disk center and below 100 MHz due to the effects of free-free absorption and scattering. The exciter of drift-pairs is consistent with propagating packets of whistlers, allowing for a fascinating way to diagnose the plasma turbulence and the radio emission mechanism. \\ ( https://arxiv.org/abs/2007.14648 , 3207kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14670 Date: Wed, 29 Jul 2020 08:33:29 GMT (3288kb,D) Title: Searching for misaligned active galactic nuclei among blazar candidates in the Fourth Fermi-LAT catalog Authors: G.Chiaro, G. La Mura, A. Dominguez, S. Bisogni Categories: astro-ph.GA astro-ph.HE \\ Radio-loud sources with blazar-like properties, but having a jet that does not directly point in the direction of the observer are among the most interesting classes of gamma-ray emitters. These sources are known as Misaligned Active Galactic Nuclei (MAGN). Understanding MAGN properties is useful to improve the knowledge of blazar energetics. We searched for new MAGN candidates among the remaining blazars of uncertain type detected by the Fermi Large Area Telescope (LAT) using a methodology based on characterizing their radio morphology. We identified seven new candidates associated with gamma-ray sources. Their features are consistent with a source with a misaligned relativistic jet consistent with the definition of MAGN. \\ ( https://arxiv.org/abs/2007.14670 , 3288kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14688 Date: Wed, 29 Jul 2020 09:07:21 GMT (893kb,D) Title: Reproductive Freeze-In of Self-Interacting Dark Matter Authors: John March-Russell, Hannah Tillim, Stephen M. West Categories: astro-ph.CO hep-ph Comments: 10 pages, 7 figures \\ We present a mechanism for dark matter (DM) production involving a self-interacting sector that at early times is ultra-relativistic but far-underpopulated relative to thermal equilibrium (such initial conditions often arise, e.g., from inflaton decay). Although elastic scatterings can establish kinetic equilibrium we show that for a broad variety of self-interactions full equilibrium is never established despite the DM yield significantly evolving due to $2\to k$ ($k>2$) processes (the DM carries no conserved quantum number nor asymmetry). During the active phase of the process, the DM to Standard Model temperature ratio falls rapidly, with DM kinetic energy being converted to DM mass, the inverse of the recently-discussed `cannibal DM mechanism'. Potential observables and applications include self-interacting DM signatures in galaxies and clusters, dark acoustic oscillations, the alteration of free-streaming constraints, and possible easing of $\sigma_8$ and Hubble tensions. \\ ( https://arxiv.org/abs/2007.14688 , 893kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14695 Date: Wed, 29 Jul 2020 09:24:35 GMT (5203kb,D) Title: Constraints on Primordial Power Spectrum from Galaxy Luminosity Functions Authors: Shintaro Yoshiura, Masamune Oguri, Keitaro Takahashi, Tomo Takahashi Categories: astro-ph.CO gr-qc hep-ph Comments: 20 pages, 24 figures, comments welcome \\ We derive constraints on primordial power spectrum, for the first time, from galaxy UV luminosity functions (LFs) at high redshifts. Since the galaxy LFs reflect an underlying halo mass function which depends on primordial fluctuations, one can constrain primordial power spectrum, particularly on small scales. We perform a Markov Chain Monte Carlo analysis by varying parameters for primordial power spectrum as well as those describing astrophysics. We adopt the UV LFs derived from Hubble Frontier Fields data at $z = 6 -10$, which enable us to probe primordial fluctuations on the scales of $k \sim 10 - 10^3~{\rm Mpc}^{-1}$. Our analysis also clarifies how the assumption on cosmology such as primordial power spectrum affects the determination of astrophysical parameters. \\ ( https://arxiv.org/abs/2007.14695 , 5203kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14704 Date: Wed, 29 Jul 2020 09:34:41 GMT (1328kb,D) Title: Re-observing the NLS1 Galaxy RE J1034+396. II. New Insights on the Soft X-ray Excess, QPO and the Analogy with GRS 1915+105 Authors: Chichuan Jin, Chris Done, Martin Ward Categories: astro-ph.HE astro-ph.GA Comments: 21 pages, 16 figures, 6 tables, submitted to MNRAS \\ RE J1034+396 displays the so far detected most significant X-ray Quasi-Periodic Oscillation (QPO) in AGN. We perform a detailed spectral-timing analysis on the data using recent simultaneous XMM-Newton, NuSTAR and Swift observations. We present the detailed energy dependence of the QPO's frequency, rms, coherence and phase lag. We construct various frequency-resolved variability spectra, which are modelled together with the time-averaged spectra. Our study shows that four components are required to fit all the spectra, including an inner disc component (diskbb), two warm corona components (CompTT-1 and CompTT-2) and a hot corona component (nthComp). An important discovery is that within the two warm corona components, CompTT-2 (the hotter, less luminous component) contains the QPO signal, while the stochastic variability is concentrated in CompTT-1. These components also allow us to fit the lag-energy spectra, as well as being able to describe the previous observation of a strong QPO in 2007, and the absent QPO observations, by varying only the relative normalizations of these components. Our multi-wavelength study shows that the QPO's detectability does not depend on the contemporaneous mass accretion rate through the outer disc as estimated from the UV flux. We do not detect a significant Iron K$\alpha$ line, nor any significant reflection component hump. Finally, we show that the rms and lag spectra of RE J1034+396 in the recent observation are very similar to the 67 Hz QPO in the micro-quasar GRS 1915+105. These new results reinforce the physical analogy between the two sources. We speculate that the QPO in both sources is due to expansion/contraction of the inner disc vertical structure. \\ ( https://arxiv.org/abs/2007.14704 , 1328kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14720 Date: Wed, 29 Jul 2020 10:12:42 GMT (5709kb,D) Title: The Uchuu Simulations: Data Release 1 and Dark Matter Halo Concentrations Authors: Tomoaki Ishiyama, Francisco Prada, Anatoly A. Klypin, Manodeep Sinha, R. Benton Metcalf, Eric Jullo, Bruno Altieri, Sof\'ia A. Cora, Darren Croton, Sylvain de la Torre, David E. Mill\'an-Calero, Taira Oogi, Jos\'e Ruedas, Cristian A. Vega-Mart\'inez Categories: astro-ph.CO Comments: 18 pages, 12 figures, We release various $N$-body products as data release 1 on http://skiesanduniverses.org/ such as subsets of simulation particles, matter power spectra, halo/subhalo catalogues, and their merger trees \\ We introduce the Uchuu suite of large high-resolution cosmological $N$-body simulations. The largest simulation, named Uchuu, consists of 2.1 trillion ($12800^3$) dark matter particles in a box of 2.0 Gpc/h, and the mass of each particle is $3.27 \times 10^{8}$ Msun/h. The highest resolution simulation, called Shin-Uchuu, consists of 262 billion ($6400^3$) particles in a box of 140 Mpc/h, with a particle mass of $8.97 \times 10^{5}$ Msun/h. Combining these simulations we can follow the evolution of dark matter haloes (and subhaloes) spanning from dwarf galaxies to massive galaxy cluster hosts. We present basic statistics, dark matter power spectra and halo (subhalo) mass function, to demonstrate the huge dynamic range and superb statistics of the Uchuu simulations. From the analysis of the evolution of the power spectra we conclude that our simulations are accurate enough from the Baryon Acoustic Oscillations up to very small scales. We also provide parameters of a mass-concentration model, which describes the evolution of halo concentrations, that reproduces our simulation data within 5% error. We make publicly available various $N$-body products, as part of Uchuu Data Release 1, on the Skies & Universes site. We also plan to release gravitational lensing maps, mock galaxy, X-ray cluster and active galactic nuclei catalogues in the near future. \\ ( https://arxiv.org/abs/2007.14720 , 5709kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14739 Date: Wed, 29 Jul 2020 10:58:51 GMT (2230kb,D) Title: Validating post-AGB candidates in the LMC and SMC using SALT spectra Authors: Ryszard Szczerba, Marcin Hajduk, Yakiv V. Pavlenko, Bruce J. Hrivnak, Bohdan Kaminsky, Kevin Volk, Natasz Si\'odmiak, IlknurI Gezer, Laimons Za\v{c}s, Wojtek Pych, Marek Sarna Categories: astro-ph.SR astro-ph.GA Comments: 19 pages, 19 figures, A&A in press DOI: 10.1051/0004-6361/201935392 \\ We selected a sample of post-AGB candidates in the Magellanic Clouds on the basis of their near- and mid-infrared colour characteristics. Fifteen of the most optically bright post-AGB candidates were observed with the South African Large Telescope in order to determine their stellar parameters and thus to validate or discriminate their nature as post-AGB objects in the Magellanic Clouds. The spectral types of absorption-line objects were estimated according to the MK classification, and effective temperatures were obtained by means of stellar atmosphere modelling. Emission-line objects were classified on the basis of the fluxes of the emission lines and the presence of the continuum. Out of 15 observed objects, only 4 appear to be genuine post-AGB stars (27\%). In the SMC, 1 out of 4 is post-AGB, and in the LMC, 3 out 11 are post-AGB objects. Thus, we can conclude that the selected region in the colour-colour diagram, while selecting the genuine post-AGB objects, overlaps severely with other types of objects, in particular young stellar objects and planetary nebulae. Additional classification criteria are required to distinguish between post-AGB stars and other types of objects. In particular, photometry at far-IR wavelengths would greatly assist in distinguishing young stellar objects from evolved ones. On the other hand, we showed that the low-resolution optical spectra appear to be sufficient to determine whether the candidates are post-AGB objects. \\ ( https://arxiv.org/abs/2007.14739 , 2230kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14742 Date: Wed, 29 Jul 2020 11:05:31 GMT (510kb) Title: A broadband X-ray spectral study of the Seyfert 1 galaxy ESO 141--G055 with XMM-Newton and NuSTAR Authors: Ritesh Ghosh and Sibasish Laha Categories: astro-ph.HE Comments: 10 pages, 4 tables and 4 figures. Accepted in MNRAS DOI: 10.1093/mnras/staa2259 \\ We have extensively studied the broadband X-ray spectra of the source ESO~141--G055 using all available \xmm{} and \nustar{} observations. We detect a prominent soft excess below 2 keV, a narrow Fe line and a Compton hump (>10 keV). The origin of the soft excess is still debated. We used two models to describe the soft excess: the blurred reflection from the ionized accretion disk and the intrinsic thermal Comptonisation model. We find that both of these models explain the soft excess equally well. We confirm that we do not detect any broad Fe line in the X-ray spectra of this source, although both the physical models prefer a maximally spinning black hole scenario (a$>$0.96). This may mean that either the broad Fe line is absent or blurred beyond detection. The Eddington rate of the source is estimated to be $\lambda_{Edd} \sim 0.31$. In the reflection model, the Compton hump has a contribution from both ionized and neutral reflection components. The neutral reflector which simultaneously describes the narrow Fe K$\alpha$ and the Compton hump has a column density of $\rm N_{H} \geq 7\times 10^{24} \rm cm^{-2} $. In addition, we detect a partially covering ionized absorption with ionization parameter $\log \xi/\rm erg cm s^{-1}$ = $0.1^{+0.1}_{-0.1}$ and column density $\rm N_{H} =20.6^{+1.0}_{-1.0}\times 10^{22} \rm cm^{-2}$ with a covering factor of $0.21^{+0.01}_{-0.01}$. \\ ( https://arxiv.org/abs/2007.14742 , 510kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14743 Date: Wed, 29 Jul 2020 11:10:06 GMT (906kb,D) Title: Prediction of the in situ coronal mass ejection rate for solar cycle 25: Implications for Parker Solar Probe in situ observations Authors: Christian M\"ostl, Andreas J. Weiss, Rachel L. Bailey, Martin A. Reiss, Ute V. Amerstorfer, Tanja Amerstorfer, J\"urgen Hinterreiter, Maike Bauer, Scott W. McIntosh, No\'e Lugaz, David Stansby Categories: astro-ph.SR astro-ph.EP physics.space-ph Comments: 11 pages, 6 figures, submitted to the Astrophysical Journal 2020 July 28 \\ The Parker Solar Probe (PSP) and Solar Orbiter missions are designed to make groundbreaking observations of the Sun and interplanetary space within this decade. We show that a particularly interesting in situ observation of an interplanetary coronal mass ejection (ICME) by PSP may arise during close solar flybys ($< 0.1$ AU). During these times, the same magnetic flux rope inside an ICME could be observed in situ by PSP twice, by impacting its frontal part as well as its leg. Investigating the odds of this situation, we forecast the ICME rate in solar cycle 25 based on 2 models for the sunspot number (SSN): (1) the consensus prediction of an expert panel in 2019 (maximum SSN = 115), and (2) a prediction by McIntosh et al. (2020, maximum SSN = 232). We link the SSN to the observed ICME rates in solar cycles 23 and 24 with the Richardson and Cane list and our own ICME catalog with a linear fit. We calculate that between 2 and 7 ICMEs will be observed by PSP at heliocentric distances $< 0.1$ AU until 2025, including 1$\sigma$ uncertainties. We then model the potential flux rope signatures of such a double-crossing event with the semi-empirical 3DCORE flux rope model, showing a telltale elevation of the radial magnetic field component $B_R$ and a sign reversal in the component $B_N$ normal to the solar equator, which is in contrast to the classic field rotation in the first encounter. This holds considerable promise to determine the structure of CMEs close to their origin in the solar corona. \\ ( https://arxiv.org/abs/2007.14743 , 906kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14744 Date: Wed, 29 Jul 2020 11:10:56 GMT (3454kb,D) Title: Solar observatory Einstein Tower -- Data release of the digitized solar full-disk photographic plate archive Authors: Partha S. Pal, M. Verma, J. Rendtel, S. J. Gonz\'alez Manrique, H. Enke, C. Denker Categories: astro-ph.SR astro-ph.IM \\ We present solar full-disk observations, which were recorded at the Einstein Tower during the years 1943 - 1991 (Solar Cycles 18 - 22). High-school students from Potsdam and Berlin digitized more than 3500 full-disk images during two- to three-week internships at AIP. The digital images cover a 15 cm $\times$ 15 cm region on photographic plates, which were scanned at a resolution of 7086 $\times$ 7086 pixels. The raw data are monochromatic 8-bit images in the Tagged Image File Format (TIFF). These images were calibrated and saved with improved photometric precision as 16-bit images with 2048 $\times$ 2048 pixels in the Flexible Image Transport System (FITS) format, which contains extensive headers describing the full-disk images and the observations. The various calibration steps include, for example, accurate measurements of the solar radius, determination of the limb-darkening function, and establishing an accurate coordinate system. The contrast-enhanced and limb-darkening corrected images as well as the raw data are freely available to researchers and the general public in publicly accessible repository. The data are published as a special data release of the Archives of Photographic PLates for Astronomical USE (APPLAUSE) project. \\ ( https://arxiv.org/abs/2007.14744 , 3454kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14779 Date: Wed, 29 Jul 2020 12:29:39 GMT (2814kb,D) Title: Shape of solar cycles and mid-term solar activity oscillations Authors: D.D. Sokoloff, A.S. Shibalova, V.N. Obridko and V.V. Pipin Categories: astro-ph.SR Comments: 8 pages, 8 figures, accepted in MNRAS \\ The evolution of the solar activity comprises, apart from the well-known 11-year cycle, various temporal scales ranging from months up to the secondary cycles known as mid-term oscillations. Its nature deserves a physical explanation. In this work, we consider the 5-to-6 year oscillations as derived both from sunspot and from solar magnetic dipole time series. Using the solar dynamo model, we deduced that these variations may be a manifestation of the dynamo nonlinearities and non-harmonic shape of the solar activity cycles. We conclude that the observed mid-term oscillations are related to the nonlinear saturation of the dynamo processes in the solar interior. \\ ( https://arxiv.org/abs/2007.14779 , 2814kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14815 Date: Wed, 29 Jul 2020 13:05:41 GMT (4560kb,D) Title: Relativistic AGN jets III. Synthesis of synchrotron emission from Double-Double Radio Galaxies Authors: S. Walg (1 and 2), A. Achterberg, (1) S. Markoff, (2) R. Keppens, (3) O. Porth (2) ((1) Department of Astrophysics/IMAPP, Radboud University, Nijmegen, The Netherlands, (2) Astronomical Institute "Anton Pannekoek", University of Amsterdam, Amsterdam, The Netherlands, (3) Centre for mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven, Heverlee, Belgium.) Categories: astro-ph.HE astro-ph.GA Comments: 24 pages, 8 figures DOI: 10.1093/mnras/staa2195 \\ The class of Double-Double Radio Galaxies (DDRGs) relates to episodic jet outbursts. How various regions and components add to the total intensity in radio images is less well known. In this paper we synthesize synchrotron images for DDRGs based on special relativistic hydrodynamic simulations, making advanced approximations for the magnetic fields. We study the synchrotron images for: Three different radial jet profiles; Ordered, entangled or mixed magnetic fields; Spectral ageing from synchrotron cooling; The contribution from different jet components; The viewing angle and Doppler (de-)boosting; The various epochs of the evolution of the DDRG. To link our results to observational data, we adopt to J1835+6204 as a reference source. In all cases the synthesized synchrotron images show two clear pairs of hotspots, in the inner and outer lobes. The best resemblance is obtained for the piecewise isochoric jet model, for a viewing angle of approximately $\vartheta \sim -71^{\circ}$, i.e. inclined with the lower jet towards the observer, with predominantly entangled ($\gtrsim 70$ per cent of the magnetic pressure) in turbulent, rather than ordered fields. The effects of spectral ageing become significant when the ratio of observation frequencies and cut-off frequency $\nu_{\rm obs}/\nu_{\infty,0} \gtrsim 10^{-3}$, corresponding to $\sim 3 \cdot 10^2$ MHz. For viewing angles $\vartheta \lesssim -30^{\circ}$, a DDRG morphology can no longer be recognized. The second jets must be injected within $\lesssim$ 4 per cent of the lifetime of the first jets for a DDRG structure to emerge, which is relevant for Active Galactic Nuclei feedback constraints. \\ ( https://arxiv.org/abs/2007.14815 , 4560kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14825 Date: Wed, 29 Jul 2020 13:24:11 GMT (381kb) Title: Gaia-DR2 extended kinematical maps. Part III: Rotation curves analysis, dark matter, and Modified Newtonian dynamics tests Authors: \v{Z}. Chrob\'akov\'a, M. L\'opez-Corredoira, F. Sylos Labini, H.-F. Wang, R. Nagy Categories: astro-ph.GA Comments: 11 pages, 8 figures, accepted to be published in A&A \\ Recent statistical deconvolution methods have produced extended kinematical maps in a range of heliocentric distances that are a factor of two to three larger than those analysed in the Gaia Collaboration based on the same data. In this paper, we use such maps to derive the rotation curve both in the Galactic plane and in off-plane regions and to analyse the density distribution. By assuming stationary equilibrium and axisymmetry, we used the Jeans equation to derive the rotation curve. Then we fit it with density models that include both dark matter and predictions of the MOND (Modified Newtonian dynamics) theory. Since the Milky Way exhibits deviations from axisymmetry and equilibrium, we also considered corrections to the Jeans equation. To compute such corrections, we ran N-body experiments of mock disk galaxies where the departure from equilibrium becomes larger as a function of the distance from the centre. The rotation curve in the outer disk of the Milky Way that is constructed with the Jeans equation exhibits very low dependence on $R$ and $z$ and it is well-fitted both by dark matter halo and MOND models. The application of the Jeans equation for deriving the rotation curve, in the case of the systems that deviate from equilibrium and axisymmetry, introduces systematic errors that grow as a function of the amplitude of the average radial velocity. In the case of the Milky Way, we can observe that the amplitude of the radial velocity reaches $\sim 10\%$ that of the azimuthal one at $R\approx 20$ kpc. Based on this condition, using the rotation curve obtained from the Jeans equation to calculate the mass may overestimate its measurement. \\ ( https://arxiv.org/abs/2007.14825 , 381kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14830 Date: Wed, 29 Jul 2020 13:40:08 GMT (5056kb,D) Title: How do different spiral arm models impact the ISM and GMC population? Authors: Alex R. Pettitt, Clare L. Dobbs, Junichi Baba, Dario Colombo, Ana Duarte-Cabral, Fumi Egusa, Asao Habe Categories: astro-ph.GA Comments: 18 pages, 17 figures. Accepted for publication in MNRAS \\ The nature of galactic spiral arms in disc galaxies remains elusive. Regardless of the spiral model, arms are expected to play a role in sculpting the star-forming interstellar medium. As such, different arm models may result in differences in the structure of the interstellar medium and molecular cloud properties. In this study we present simulations of galactic discs subject to spiral arm perturbations of different natures. We find very little difference in how the cloud population or gas kinematics vary between the different grand-design spirals, indicting that the interstellar medium on cloud scales cares little about where spiral arms come from. We do, however, see a difference in the interarm/arm mass spectra, {and minor differences in tails of the distributions of cloud properties} (as well as radial variations in the stellar/gaseous velocity dispersions). These features can be attributed to differences in the radial dependence of the pattern speeds between the different spiral models, and could act as a metric of the nature of spiral structure in observational studies. \\ ( https://arxiv.org/abs/2007.14830 , 5056kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14843 Date: Tue, 28 Jul 2020 03:35:07 GMT (306kb,D) Title: Pulsar Candidate Sifting Using Multi-input Convolution Neural Networks Authors: Haitao Lin, Xiangru Li, Qingguo Zeng Categories: astro-ph.IM Comments: 13 pages,7 figures, 4 tables MSC-class: 85-11 ACM-class: I.5 \\ Pulsar candidate sifting is an essential process for discovering new pulsars. It aims to search for the most promising pulsar candidates from an all-sky survey, such as High Time Resolution Universe (HTRU), Green Bank Northern Celestial Cap (GBNCC), Five-hundred-meter Aperture Spherical radio Telescope (FAST), etc. Recently, machine learning (ML) is a hot topic in pulsar candidate sifting investigations. However, one typical challenge in ML for pulsar candidate sifting comes from the learning difficulty arising from the highly class-imbalance between the observation numbers of pulsars and non-pulsars. Therefore, this work proposes a novel framework for candidate sifting, named multi-input convolutional neural networks (MICNN). The MICNN is an architecture of deep learning with four diagnostic plots of a pulsar candidate as its inputs. To train our MICNN in a highly class-imbalanced dataset, a novel image augment technique, as well as a three-stage training strategy, is proposed. Experiments on observations from HTRU and GBNCC show the effectiveness and robustness of these proposed techniques. In the experiments on HTRU, our MICNN model achieves a recall of 0.962 and a precision rate of 0.967 even in a highly class-imbalanced test dataset. \\ ( https://arxiv.org/abs/2007.14843 , 306kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14849 Date: Wed, 29 Jul 2020 14:05:45 GMT (6552kb,D) Title: Einstein@Home Discovery of Gamma-ray Pulsations Confirms the Redback Nature of 3FGL J2039.6-5618 Authors: C. J. Clark, L. Nieder, G. Voisin, B. Allen, C. Aulbert, O. Behnke, R. P. Breton, C. Choquet, A. Corongiu, V. S. Dhillon, H. B. Eggenstein, H. Fehrmann, L. Guillemot, A. K. Harding, M. R. Kennedy, B. Machenschalk, T. R. Marsh, D. Mata S\'anchez, R. P. Mignani, J. Stringer, Z. Wadiasingh, J. Wu Categories: astro-ph.HE Comments: 21 pages, 11 figures, submitted to MNRAS \\ The Fermi Large Area Telescope gamma-ray source 3FGL J2039.6$-$5618 contains a periodic optical and X-ray source that was predicted to be a "redback" millisecond pulsar (MSP) binary system. However, the conclusive identification required the detection of pulsations from the putative MSP. To better constrain the orbital parameters for a directed search for gamma-ray pulsations, we obtained new optical light curves in 2017 and 2018, which revealed long-term variability from the companion star. The resulting orbital parameter constraints were used to perform a targeted gamma-ray pulsation search using the Einstein@Home distributed volunteer computing system. This search discovered pulsations with a period of 2.65 ms, confirming the source as a binary MSP now known as PSR J2039$-$5617. The pulsar's orbital Doppler shift indicates a companion mass of 0.15 to 0.22 $M_{\odot}$, confirming the redback classification. Optical light curve modelling is complicated by variability, but we find an inclination $i > 70{\deg}$, for a low pulsar mass between $1.1 M_{\odot} < M_{\rm psr} < 1.35 M_{\odot}$. Timing the gamma-ray pulsations also revealed significant variability in the orbital period, which we find to be consistent with quadrupole moment variations in the companion star, suggestive of convective activity. We also find that the pulsed flux is modulated at the orbital period, potentially due to inverse Compton scattering between high-energy leptons in the pulsar wind and the companion star's optical photon field. \\ ( https://arxiv.org/abs/2007.14849 , 6552kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14853 Date: Wed, 29 Jul 2020 14:11:41 GMT (1796kb,D) Title: The effect of tides on near-core rotation: analysis of 35 Kepler $\gamma$ Doradus stars in eclipsing and spectroscopic binaries Authors: Gang Li, Zhao Guo, Jim Fuller, Timothy R. Bedding, Simon J. Murphy, Isabel L. Colman, Daniel R. Hey Categories: astro-ph.SR Comments: 13 pages, 10 figures, accepted by MNRAS. Email me if you want the online appendix \\ We systematically searched for gravity- and Rossby-mode period spacing patterns in Kepler eclipsing binaries with $\gamma$ Doradus pulsators. These stars provide an excellent opportunity to test the theory of tidal synchronisation and angular momentum transport in F- and A-type stars. We discovered 35 systems that show clear patterns, including the spectroscopic binary KIC 10080943. Combined with 45 non-eclipsing binaries with $\gamma$ Dor components that have been found using pulsation timing, we measured their near-core rotation rates and asymptotic period spacings. We find that many stars are tidally locked if the orbital periods are shorter than 10 days, in which the near-core rotation periods given by the traditional approximation of rotation (TAR) are consistent with the orbital period. Compared to the single stars, $\gamma$ Dor stars in binaries tend to have slower near-core rotation rates, likely a consequence of tidal spin-down. We also find three stars that have extremely slow near-core rotation rates. To explain these, we hypothesise that unstable tidally excited oscillations can transfer angular momentum from the star to the orbit, and slow the star below synchronism, a process we refer to as `inverse tides'. \\ ( https://arxiv.org/abs/2007.14853 , 1796kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14869 Date: Wed, 29 Jul 2020 14:38:33 GMT (4526kb) Title: Space Project for Astrophysical and Cosmological Exploration (SPACE), an ESA stand-alone mission and a possible contribution to the Origins Space Telescope Authors: Denis Burgarella, Andrew Bunker, Rychard Bouwens, Laurent Pagani, Jose Afonso, Hakim Atek, Marc Audard, Sylvie Cabrit, Karina Caputi, Laure Ciesla, Christopher Conselice, Asantha Cooray, Giovanni Cresci, Mirko Curti, Marc Ferrari, Chiaki Kobayashi, Nadege Lagarde, Jesus Gallego Maestro, Roberto Maiolino, Katarzyna Malek, Jose Miguel Rodriguez Espinosa, Filippo Mannucci, Julien Montillaud, Pascal Oesch, Chris Pearson, Agnieszka Pollo, David Rosario, Itsuki Sakon, Daniel Schaerer, Ray Sharples, David Sobral, Frederic Zamkotsian Categories: astro-ph.IM astro-ph.CO astro-ph.GA Comments: Submitted to Experimental Astronomy as one of the proposals for the European Space Agency Voyage 2050 Programme \\ We propose a new mission called Space Project for Astrophysical and Cosmological Exploration (SPACE) as part on the ESA long term planning Voyage 2050 programme. SPACE will study galaxy evolution at the earliest times, with the key goals of charting the formation of the heavy elements, measuring the evolution of the galaxy luminosity function, tracing the build-up of stellar mass in galaxies over cosmic time, and finding the first super-massive black holes (SMBHs) to form. The mission will exploit a unique region of the parameter space, between the narrow ultra-deep surveys with HST and JWST, and shallow wide-field surveys such as Roman Space Telescope and EUCLID, and should yield by far the largest sample of any current or planned mission of very high redshift galaxies at z > 10 which are sufficiently bright for detailed follow-up spectroscopy. Crucially, we propose a wide-field spectroscopic near-IR + mid-IR capability which will greatly enhance our understanding of the first galaxies by detecting and identifying a statistical sample of the first galaxies and the first SMBH, and to chart the metal enrichment history of galaxies in the early Universe - potentially finding signatures of the very first stars to form from metal-free primordial gas. The wide-field and wavelength range of SPACE will also provide us a unique opportunity to study star formation by performing a wide survey of the Milky Way in the near-IR + mid-IR. This science project can be enabled either by a stand-alone ESA-led M mission or by an instrument for an L mission (with ESA and/or NASA, JAXA and other international space agencies) with a wide-field (sub-)millimetre capability at wavelength > 500 microns. \\ ( https://arxiv.org/abs/2007.14869 , 4526kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14876 Date: Wed, 29 Jul 2020 14:52:46 GMT (15274kb,D) Title: Reducing scattered light in LIGO's third observing run Authors: S Soni, C Austin, A Effler, R M S Schofield, G Gonzalez, V V Frolov, J C Driggers, A Pele, A L Urban, G Valdes, R. Abbott, C. Adams, R. X. Adhikari, A. Ananyeva, S. Appert, K. Arai, J. S. Areeda, Y. Asali, S. M. Aston, A. M. Baer, M. Ball, S. W. Ballmer, S. Banagiri, D. Barker, L. Barsotti, J. Bartlett, B. K. Berger, J. Betzwieser, D. Bhattacharjee, G. Billingsley, S. Biscans, C. D. Blair, R. M. Blair, N. Bode, P. Booker, R. Bork, A. Bramley, A. F. Brooks, D. D. Brown, A. Buikema, C. Cahillane, K. C. Cannon, X. Chen, A. A. Ciobanu, F. Clara, S. J. Cooper, K. R. Corley, S. T. Countryman, P. B. Covas, D. C. Coyne, L. E. H. Datrier, D. Davis, C. Di Fronzo, K. L. Dooley, P. Dupej, S. E. Dwyer, T. Etzel, M. Evans, T. M. Evans, J. Feicht, A. Fernandez-Galiana, P. Fritschel, P. Fulda, M. Fyffe, J. A. Giaime, et al. (133 additional authors not shown) Categories: astro-ph.IM Comments: 24 pages, 15 figures, 1 table Report-no: LIGO-P2000172 \\ Noise due to scattered light has been a frequent disturbance in the Advanced LIGO gravitational wave detectors, hindering the detection of gravitational waves. The non stationary scatter noise caused by low frequency motion can be recognized as arches in the time-frequency plane of the gravitational wave channel. In this paper, we characterize the scattering noise for LIGO's third observing run O3 from April, 2019 to March, 2020. We find at least two different populations of scattering noise and we investigate the multiple origins of one of them as well as its mitigation. We find that relative motion between two specific surfaces is strongly correlated with the presence of scattered light and we implement a technique to reduce this motion. We also present an algorithm using a witness channel to identify the times this noise can be present in the detector. \\ ( https://arxiv.org/abs/2007.14876 , 15274kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14888 Date: Wed, 29 Jul 2020 15:04:58 GMT (11462kb,D) Title: Incoherent Solar Radio Emission Authors: A. Nindos Categories: astro-ph.SR Comments: Frontiers in Astronomy and Space Sciences, accepted for publication \\ Incoherent solar radio radiation comes from the free-free, gyroresonance, and gyrosynchrotron emission mechanisms. Free-free is primarily produced from Coulomb collisions between thermal electrons and ions. Gyroresonance and gyrosynchrotron result from the acceleration of low-energy electrons and mildly relativistic electrons, respectively, in the presence of a magnetic field. In the non-flaring Sun, free-free is the dominant emission mechanism with the exception of regions of strong magnetic fields which emit gyroresonance at microwaves. Due to its ubiquitous presence, free-free emission can be used to probe the non-flaring solar atmosphere above temperature minimum. Gyroresonance opacity depends strongly on the magnetic field strength and orientation; hence it provides a unique tool for the estimation of coronal magnetic fields. Gyrosynchrotron is the primary emission mechanism in flares at frequencies higher than 1-2 GHz and depends on the properties of both the magnetic field and the accelerated electrons, as well as the properties of the ambient plasma. In this paper we discuss in detail the above mechanisms and their diagnostic potential. \\ ( https://arxiv.org/abs/2007.14888 , 11462kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14889 Date: Wed, 29 Jul 2020 15:05:15 GMT (4211kb,D) Title: Radio pulsations from the $\gamma$-ray millisecond pulsar PSR J2039-5617 Authors: A. Corongiu, R.P. Mignani, A.S. Seyffert, C. J. Clark, C. Venter, L. Nieder, A. Possenti, M. Burgay, A. Belfiore, A. De Luca, A. Ridolfi, Z. Wadiasingh Categories: astro-ph.HE astro-ph.SR Comments: 18 pages, submitted to MNRAS \\ The predicted nature of the candidate redback pulsar 4FGL J2039.5-56.17 was recently confirmed by the discovery of $\gamma$-ray millisecond pulsations (Clark et al. 2020, hereafter Paper I), which identify this $\gamma$-ray source as PSR J2039-5617. We observed 4FGL 2039.5-5617 with the Parkes radio telescope in 2016 and 2019. We detect radio pulsations at 1.4 GHz and 3.1 GHz, at the 2.6 ms period discovered in $\gamma$-rays, and also at 0.7 GHz in one 2015 archival observation. In all bands, the radio pulse profile is characterised by a single relatively broad peak which leads the main $\gamma$-ray peak. At 1.4 GHz we found clear evidence of eclipses of the radio signal for about half of the orbit, a characteristic phenomenon in redback systems, which we associate with the presence of intra-binary gas. From the dispersion measure DM$=24.57\pm0.03$\,pc\,cm$^{-3}$ we derive a pulsar distance of $0.9\pm 0.2$kpc or $1.7\pm0.7$kpc, depending on the assumed Galactic electron density model. Both the 1.4 GHz Parkes observations obtained in 2016 and 2019 and Swift monitoring campaign (2017-2018) show no obvious long-term changes in the pulsar radio and X-ray emission. The modelling of the radio and $\gamma$-ray light curves leads to an independent determination of the orbital inclination, and to a determination of the pulsar mass, qualitatively consistent to the results in Paper I. \\ ( https://arxiv.org/abs/2007.14889 , 4211kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14899 Date: Wed, 29 Jul 2020 15:16:41 GMT (540kb) Title: Volatile Sample Return in the Solar System Authors: Stefanie N. Milam, Jason P. Dworkin, Jamie E. Elsila, Daniel P. Glavin, Perry A. Gerakines, Julie L. Mitchell, Keiko Nakamura-Messenger, Marc Neveu, Larry Nittler, James Parker, Elisa Quintana, Scott A. Sandford, Joshua E. Schlieder, Rhonda Stroud, Melissa G. Trainer, Meenakshi Wadhwa, Andrew J. Westphal, Michael Zolensky, Dennis Bodewits, Simon Clemett Categories: astro-ph.IM astro-ph.EP Comments: White paper submitted to the Planetary Science and Astrobiology Decadal Survey 2023-2032 \\ We advocate for the realization of volatile sample return from various destinations including: small bodies, the Moon, Mars, ocean worlds/satellites, and plumes. As part of recent mission studies (e.g., Comet Astrobiology Exploration SAmple Return (CAESAR) and Mars Sample Return), new concepts, technologies, and protocols have been considered for specific environments and cost. Here we provide a plan for volatile sample collection and identify the associated challenges with the environment, transit/storage, Earth re-entry, and curation. Laboratory and theoretical simulations are proposed to verify sample integrity during each mission phase. Sample collection mechanisms are evaluated for a given environment with consideration for alteration. Transport and curation are essential for sample return to maximize the science investment and ensure pristine samples for analysis upon return and after years of preservation. All aspects of a volatile sample return mission are driven by the science motivation: isotope fractionation, noble gases, organics and prebiotic species; plus planetary protection considerations for collection and for the sample. The science value of sample return missions has been clearly demonstrated by previous sample return programs and missions. Sample return of volatile material is key to understanding (exo)planet formation, evolution, and habitability. Returning planetary volatiles poses unique and potentially severe technical challenges. These include preventing changes to samples between (and including) collection and analyses, and meeting planetary protection requirements. \\ ( https://arxiv.org/abs/2007.14899 , 540kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14905 Date: Wed, 29 Jul 2020 15:24:03 GMT (2511kb,D) Title: Retention of Long-Period Gas Giant Planets: Type II Migration Revisited Authors: Yi-Xian Chen, Xiaojia Zhang, Ya-Ping Li, Hui Li, and Douglas N. C. Lin Categories: astro-ph.EP Comments: 21 pages, 12 figures, accepted by ApJ \\ During their formation, emerging protoplanets tidally interact with their natal disks. Proto-gas-giant planets, with Hills radius larger than the disk thickness, open gaps and quench gas flow in the vicinity of their orbits. It is usually assumed that their type II migration is coupled to the viscous evolution of the disk. Although this hypothesis provides an explanation for the origin of close-in planets, it also encounter predicament on the retention of long-period orbits for most gas giant planets. Moreover, numerical simulations indicate that planets migrations are not solely determined by the viscous diffusion of their natal disk. Here we carry out a series of hydrodynamic simulations combined with analytic studies to examine the transition between different paradigms of type II migration. We find a range of planetary mass for which gas continues to flow through a severely depleted gap so that the surface density distribution in the disk region beyond the gap is maintained in a quasi-steady state. The associated gap profile modifies the location of corotation \& Lindblad resonances. In the proximity of the planet's orbit, high-order Lindblad \& corotation torque are weakened by the gas depletion in the gap while low-order Lindblad torques near the gap walls preserves their magnitude. Consequently, the intrinsic surface density distribution of the disk determines delicately both pace and direction of planets' type II migration. We show that this effect might stall the inward migration of giant planets and preserve them in disk regions where the surface density is steep. \\ ( https://arxiv.org/abs/2007.14905 , 2511kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14950 Date: Wed, 29 Jul 2020 16:47:02 GMT (10344kb,D) Title: Characterising the target selection pipeline for the Dark Energy Spectroscopic Instrument Bright Galaxy Survey Authors: Omar Ruiz-Macias, Pauline Zarrouk, Shaun Cole, Carlton M. Baugh, Peder Norberg, John Lucey, Arjun Dey, Daniel J. Eisenstein, Peter Doel, Enrique Gazta\~naga, ChangHoon Hahn, Robert Kehoe, Ellie Kitanidis, Martin Landriau, Dustin Lang, John Moustakas, Adam D. Myers, Francisco Prada, Michael Schubnell, David H. Weinberg, M. J. Wilson Categories: astro-ph.GA Comments: 24 pages, 19 Figures \\ We present the steps taken to produce a reliable and complete input galaxy catalogue for the Dark Energy Spectroscopic Instrument (\uppercase{desi}) Bright Galaxy Sample (\uppercase{bgs}) using the photometric Legacy Survey \uppercase{dr8} \uppercase{dec}am. We analyze some of the main issues faced in the selection of targets for the \uppercase{desi} \uppercase{bgs}, such as star-galaxy separation, contamination by fragmented stars and bright galaxies, and completeness at low surface brightness. Our pipeline utilizes a new way to select \uppercase{bgs} galaxies using {\it Gaia} photometry and we implement geometrical and photometric masks that reduce the number of spurious objects. The resulting catalogue is cross-matched with the Galaxy and Mass Assembly (\uppercase{gama}) survey to assess the completeness of the galaxy catalogue and the performance of the target selection. We also validate the clustering of our \uppercase{bgs} catalogue by comparing with mock catalogues and \uppercase{sdss} data and we include a simple linear correction to the target density to mitigate the effects of stellar density systematics. The systematic variations are at most $7$ per cent before applying any weighting correction and less than $3$ per cent after a linear weight correction. Eventually, the \uppercase{bgs} selection criteria is also assessed by measuring the correlation of the target galaxy density field with systematic properties of the imaging. \\ ( https://arxiv.org/abs/2007.14950 , 10344kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14962 Date: Wed, 29 Jul 2020 17:10:16 GMT (655kb,D) Title: Hybrid-basis inference for large-scale galaxy clustering: combining spherical and Cartesian Fourier analyses Authors: Mike Shengbo Wang, Santiago Avila, Davide Bianchi, Robert Crittenden and Will J. Percival Categories: astro-ph.CO Comments: submitted to JCAP, 39 pages, 12 figures and 1 table; public code available at http://github.com/MikeSWang/Harmonia \\ Future precision cosmology from large-scale structure experiments including the Dark Energy Spectroscopic Instrument (DESI) and Euclid will probe wider and deeper cosmic volumes than those covered by previous surveys. The Cartesian power spectrum analysis of anisotropic galaxy clustering based on the Fourier plane wave basis makes a number of assumptions, including the local plane-parallel approximation, that will no longer be valid on very large scales and may degrade cosmological constraints. We propose an approach that utilises a hybrid basis: on the largest scales, clustering statistics are decomposed into spherical Fourier modes which respect the natural geometry of both survey observations and physical effects along the line of sight, such as redshift-space distortions, the Alcock--Paczy\'nsky and light-cone effects; on smaller scales with far more clustering modes, we retain the computational benefit of the power spectrum analysis aided by fast Fourier transforms. This approach is particularly suited to the likelihood analysis of local primordial non-Gaussianity $f_\textrm{NL}$ through the scale-dependent halo bias, and we demonstrate its applicability with $N$-body simulations. We also release our public code Harmonia (https://github.com/MikeSWang/Harmonia) for galaxy clustering likelihood inference in spherical Fourier or hybrid-basis analyses. \\ ( https://arxiv.org/abs/2007.14962 , 655kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14969 Date: Wed, 29 Jul 2020 17:27:47 GMT (2073kb,D) Title: A survey for variable young stars with small telescopes: III -- Warm spots on the active star V1598Cyg Authors: Dirk Froebrich, Aleks Scholz, Jochen Eisl\"offel, Bringfried Stecklum Categories: astro-ph.SR Comments: 13 pages, 10 figures, 1 table, accepted for publication in MNRAS \\ Magnetic spots on low-mass stars can be traced and characterised using multi-band photometric light curves. Here we analyse an extensive data set for one active star, V1598Cyg, a known variable K dwarf which is either pre-main sequence and/or in a close binary system. Our light curve contains 2854 photometric data points, mostly in $V$, $R_c$, $I_c$, but also in $U$, $B$ and $H\alpha$, with a total baseline of about 4yr, obtained with small telescopes as part of the HOYS project. We find that V1598Cyg is a very fast rotator with a period of 0.8246 days and varying amplitudes in all filters, best explained as a signature of strong magnetic activity and spots. We fit the photometric amplitudes in $V$, $R_c$, $I_c$ and use them to estimate spot properties, using a grid-based method that is also propagating uncertainties. We verify the method on a partial data set with high cadence and all five broad-band filters. The method yields spot temperatures and fractional spot coverage with typical uncertainties of 100K and 3-4%, respectively. V1598Cyg consistently exhibits spots that are a few hundred degrees warmer than the photosphere, most likely indicating that the light curve is dominated by chromospheric plage. The spot activity varies over our observing baseline, with a typical time scale of 0.5-1yr, which we interpret as the typical spot lifetime. Combining our light curve with archival data, we find a six year cycle in the average brightness, that is probably a sign of a magnetic activity cycle. \\ ( https://arxiv.org/abs/2007.14969 , 2073kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14970 Date: Wed, 29 Jul 2020 17:29:18 GMT (5454kb,D) Title: maxsmooth: Rapid maximally smooth function fitting with applications in Global 21-cm cosmology Authors: H. T. J. Bevins, W. J. Handley, A. Fialkov, E. de Lera Acedo, L. J. Greenhill, D. C. Price Categories: astro-ph.CO astro-ph.IM Comments: 19 pages, 15 figures \\ Maximally Smooth Functions (MSFs) are a form of constrained functions in which there are no inflection points or zero crossings in high order derivatives. Consequently, they have applications to signal recovery in experiments where signals of interest are expected to be non-smooth features masked by larger smooth signals or foregrounds. They can also act as a powerful tool for diagnosing the presence of systematics. However, the constrained nature of MSFs makes fitting these functions a non-trivial task. Here, we introduce maxsmooth, an open source package that uses quadratic programming to rapidly fit MSFs. We demonstrate the efficiency and reliability of maxsmooth by comparison to commonly used fitting routines. We show that by using quadratic programming we can reduce the fitting time by approximately two orders of magnitude. maxsmooth features a built-in library of MSF models and allows the user to define their own. We also introduce and implement with maxsmooth Partially Smooth Functions, which are useful for describing elements of non-smooth structure in foregrounds. This work has been motivated by the problem of foreground modelling in 21-cm cosmology for which MSFs have been shown to be a viable alternative to polynomial models. We discuss applications of maxsmooth to 21-cm cosmology and highlight this with examples using data from the Experiment to Detect the Global Epoch of Reionization Signature (EDGES) and the Large-aperture Experiment to Detect the Dark Ages (LEDA) experiments. MSFs are applied to data from LEDA for the first time in this paper. maxsmooth is pip installable and available for download at: https://github.com/htjb/maxsmooth \\ ( https://arxiv.org/abs/2007.14970 , 5454kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14973 Date: Wed, 29 Jul 2020 17:32:39 GMT (13300kb) Title: Transient Jupiter Co-orbitals from Solar System Sources Authors: Sarah Greenstreet, Brett Gladman, and Henry Ngo Categories: astro-ph.EP Comments: Accepted at AJ \\ We demonstrate dynamical pathways from main-belt asteroid and Centaur orbits to those in co-orbital motion with Jupiter, including the retrograde (inclination $i>90^o$) state. We estimate that at any given time, there should be $\sim1$ kilometer-scale or larger escaped asteroid in a transient direct (prograde) orbit with semimajor axis near that of Jupiter's ($a\simeq a_J$), with proportionally more smaller objects as determined by their size distribution. Most of these objects would be in the horseshoe dynamical state, which are hard to detect due to their moderate eccentricities (spending most of their time beyond 5 AU) and longitudes relative to Jupiter being spread nearly all over the sky. We also show that $\approx$1% of the transient asteroid co-orbital population is on retrograde orbits with Jupiter. This population, like the recently identified asteroid (514107) 2015 BZ$_{509}$, can spend millions of years with $a\simeq a_J$ including tens or hundreds of thousands of years formally in the retrograde 1:-1 co-orbital resonance. Escaping near-Earth asteroids (NEAs) are thus likely the precursors to the handful of known high-inclination objects with $a\simeq a_J$. We compare the production of jovian co-orbitals from escaping NEAs with those from incoming Centaurs. We find that temporary direct co-orbitals are likely dominated by Centaur capture, but we only find production of (temporary) retrograde jovian co-orbitals (including very long-lived ones) from the NEA source. We postulate that the primordial elimination of the inner Solar System's planetesimal population could provide a supply route for a metastable outer Solar System reservoir for the high-inclination Centaurs. \\ ( https://arxiv.org/abs/2007.14973 , 13300kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14977 Date: Wed, 29 Jul 2020 17:43:36 GMT (1291kb,D) Title: Powerful ionized gas outflows in the interacting radio galaxy 4C +29.30 Authors: Guilherme S. Couto, Thaisa Storchi-Bergmann, Aneta Siemiginowska, Rogemar A. Riffel, Raffaella Morganti Categories: astro-ph.GA Comments: 17 pages, 10 figures, 2 tables, accepted by MNRAS. Comments are welcome \\ We investigate the ionized gas excitation and kinematics in the inner $4.3 \times 6.2$ kpc$^{2}$ of the merger radio galaxy 4C +29.30. Using optical integral field spectroscopy with the Gemini North Telescope, we present flux distributions, line-ratio maps, peak velocities and velocity dispersion maps as well as channel maps with a spatial resolution of $\approx 955$ pc. We observe high blueshifts of up to $\sim -650$ km s$^{-1}$, in a region $\sim 1''$ south of the nucleus (the southern knot, SK), which also presents high velocity dispersions ($\sim 250$ km s$^{-1}$), which we attribute to an outflow. A possible redshifted counterpart is observed north from the nucleus (the northern knot, NK). We propose that these regions correspond to a bipolar outflow possibly due to the interaction of the radio jet with the ambient gas. We estimate a total ionized gas mass outflow rate of $\dot{M}_{out} = 25.4 \substack{+11.5 \\ -7.5}$ M$_\odot$ yr$^{-1}$ with a kinetic power of $\dot{E} = 8.1 \substack{+10.7 \\ -4.0} \times 10^{42}$ erg s$^{-1}$, which represents $5.8 \substack{+7.6 \\ -2.9} \%$ of the AGN bolometric luminosity. These values are higher than usually observed in nearby active galaxies with the same bolometric luminosities and could imply a significant impact of the outflows in the evolution of the host galaxy. The excitation is higher in the NK (that correlates with extended X-ray emission, indicating the presence of hotter gas) than in the SK, supporting a scenario in which an obscuring dust lane is blocking part of the AGN radiation to reach the southern region of the galaxy. \\ ( https://arxiv.org/abs/2007.14977 , 1291kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14984 Date: Wed, 29 Jul 2020 17:52:11 GMT (4812kb,D) Title: Cosmological Model Parameter Dependence of the Matter Power Spectrum Covariance from the DEUS-PUR $Cosmo$ Simulations Authors: Linda Blot, Pier-Stefano Corasaniti, Yann Rasera, Shankar Agarwal Categories: astro-ph.CO Comments: 10 pages, 8 figures, submitted to MNRAS. Data available at https://cosmo.obspm.fr/public-datasets/ \\ Future galaxy surveys will provide accurate measurements of the matter power spectrum across an unprecedented range of scales and redshifts. The analysis of these data will require to accurately model the imprint of non-linearities on the matter density field, which induces a non-Gaussian contribution to the data covariance. As the imprint of non-linearities is cosmology dependent, a further complication arises from accounting for the cosmological dependence of the non-Gaussian part of the covariance. Here, we study this using a dedicated suite of N-body simulations, the Dark Energy Universe Simulation - Parallel Universe Runs (DEUS-PUR) $Cosmo$. These consist of 512 realizations for 10 different cosmologies where we vary the matter density $\Omega_m$, the amplitude of density fluctuations $\sigma_8$, the reduced Hubble parameter $h$ and a constant dark energy equation of state $w$ by approximately $10\%$. We use these data to evaluate the first and second derivatives of the power spectrum covariance with respect to a fiducial $\Lambda$CDM cosmology. We find that the variations can be as large as $150\%$ depending on the scale, redshift and model parameter considered. Using a Fisher matrix approach, we evaluate the impact of using a covariance estimated at a fiducial model rather than the true underlying cosmology. We find that the estimated $1\sigma$ errors are affected at approximately $5\%$, $20\%$, $50\%$ and $120\%$ level when assuming non-fiducial values of $h$, $w$, $\Omega_m$ and $\sigma_8$ respectively. These results suggest that the use of cosmology-dependent covariances is key for precision cosmology. \\ ( https://arxiv.org/abs/2007.14984 , 4812kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14988 Date: Wed, 29 Jul 2020 17:59:02 GMT (347kb,D) Title: The EFT Likelihood for Large-Scale Structure in Redshift Space Authors: Giovanni Cabass Categories: astro-ph.CO astro-ph.GA Comments: 32 pages (27+5), 1 figure \\ We study the EFT likelihood for biased tracers in redshift space, for which the bias expansion of the galaxy velocity field $\mathbf{v}_g$ plays a fundamental role. The equivalence principle forbids stochastic contributions to $\mathbf{v}_g$ to survive at small $k$. Therefore, at leading order in derivatives the form of the likelihood ${\cal P}[\tilde{\delta}_g|\delta,\!\mathbf{v}]$ to observe a redshift-space galaxy overdensity $\tilde{\delta}_g(\tilde{\mathbf{x}})$ given a rest-frame matter and velocity fields $\delta(\mathbf{x})$, $\mathbf{v}(\mathbf{x})$ is fixed by the rest-frame noise. If this noise is Gaussian with constant power spectrum, ${\cal P}[\tilde{\delta}_g|\delta,\!\mathbf{v}]$ is also a Gaussian in the difference between $\tilde{\delta}_g(\tilde{\mathbf{x}})$ and its bias expansion: redshift-space distortions only make the covariance depend on $\delta(\mathbf{x})$ and $\mathbf{v}(\mathbf{x})$. We then show how to match this result to perturbation theory, and that one can consistently neglect the field-dependent covariance if the bias expansion is stopped at second order in perturbations. We discuss qualitatively how this affects numerical implementations of the EFT-based forward modeling, and how the picture changes when the survey window function is taken into account. \\ ( https://arxiv.org/abs/2007.14988 , 347kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14989 Date: Wed, 29 Jul 2020 17:59:06 GMT (2126kb,D) Title: Analytic marginalization of $N(z)$ uncertainties in tomographic galaxy surveys Authors: Boryana Hadzhiyska, David Alonso, Andrina Nicola, An\v{z}e Slosar Categories: astro-ph.CO Comments: 26 pages, 7 figures \\ We present a new method to marginalize over uncertainties in redshift distributions, $N(z)$, within tomographic cosmological analyses applicable to current and upcoming photometric galaxy surveys. We allow for arbitrary deviations from the best-guess $N(z)$ governed by a general covariance matrix describing the uncertainty in our knowledge of redshift distributions. In principle, this is marginalization over hundreds or thousands of new parameters describing potential deviations as a function of redshift and tomographic bin. However, by linearly expanding the theory predictions around a fiducial model, this marginalization can be performed analytically, resulting in a modified data covariance matrix that effectively downweights the modes of the data vector that are more sensitive to redshift distribution variations. We showcase this method by applying it to the galaxy clustering measurements from the Hyper Suprime-Cam first data release. We illustrate how to marginalize over sample-variance of the calibration sample and a large general systematic uncertainty in photometric estimation methods, and explore the impact of priors imposing smoothness in the redshift distributions. \\ ( https://arxiv.org/abs/2007.14989 , 2126kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14992 Date: Wed, 29 Jul 2020 17:59:54 GMT (4563kb,D) Title: A First-Principle Model for Polarization Swings during Reconnection-Powered Flares Authors: David N. Hosking and Lorenzo Sironi Categories: astro-ph.HE physics.plasm-ph Comments: 8 pages, 4 figures. Submitted to ApJL \\ We show that magnetic reconnection in a magnetically-dominated fast-cooling plasma can naturally produce bright flares accompanied by rotations in the synchrotron polarization vector. With particle-in-cell simulations of reconnection, we find that flares are powered by efficient particle acceleration at the interface of merging magnetic flux ropes, or "plasmoids". The accelerated particles stream through the post-merger plasmoid towards the observer, thus progressively illuminating regions with varying plane-of-sky field direction, and so leading to a rotation in the observed polarization vector. Our results provide evidence for magnetic reconnection as the physical cause of high-energy flares from the relativistic jets of blazars (which recent observations have shown to be frequently associated with polarization rotations), and provide a first-principle physical mechanism for such flares. \\ ( https://arxiv.org/abs/2007.14992 , 4563kb) %-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%-%- ------------------------------------------------------------------------------ \\ arXiv:2007.13165 (*cross-listing*) Date: Sun, 26 Jul 2020 16:18:29 GMT (657kb,D) Title: Evolution of the universe during the inflationary epoch Authors: Gabriel German Categories: gr-qc astro-ph.CO Comments: 14 pages, 13 figures \\ We often find in the literature solutions to the Friedmann and fluid equations for simple cosmological models during the matter, radiation or cosmological constant dominated epochs. However no solutions appear for the inflationary era dominated by the potential energy of a scalar field due, perhaps, to the fact that we do not have as yet a strongly favored model of inflation; there are, of course, very well motivated models which fit the data. The purpose of this article is to study with some detail the evolution of the Universe during inflation in the slow-roll approximation. Taking the Starobinsky model as an example, we display exact solutions for the time evolution of the scalar field $\phi(t)$, scale factor $a(t)$, Hubble function $H(t)$, equation of state parameter $\omega(t)$ and acceleration of the scale factor $\ddot{a}(t)$ among other quantities of interest. \\ ( https://arxiv.org/abs/2007.13165 , 657kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14605 (*cross-listing*) Date: Wed, 29 Jul 2020 05:18:25 GMT (140kb,D) Title: Signal from sterile neutrino dark matter in extra $U(1)$ model at direct detection experiment Authors: Osamu Seto and Takashi Shimomura Categories: hep-ph astro-ph.CO Comments: 11 pages, 2 figures Report-no: UME-PP-013, EPHOU-20-009 \\ We examine the possibility that direct dark matter detection experiments find decay products from sterile neutrino dark mater in $U(1)_{B-L}$ and $U(1)_R$ models. This is possible if the sterile neutrino interacts with a light gauge boson and decays into a neutrino and the light gauge boson with a certain lifetime. This decay produces energetic neutrinos scattering off nuclei with a large enough recoil energy in direct dark matter detection experiments. We stress that direct dark matter detection experiments can explore not only WIMP but also sterile neutrino dark matter. \\ ( https://arxiv.org/abs/2007.14605 , 140kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14705 (*cross-listing*) Date: Wed, 29 Jul 2020 09:35:36 GMT (2315kb,D) Title: Detecting the Diffuse Supernova Neutrino Background in the future Water-based Liquid Scintillator Detector Theia Authors: Julia Sawatzki, Michael Wurm and Daniel Kresse Categories: physics.ins-det astro-ph.IM hep-ex hep-ph \\ A large-scale neutrino observatory based on Water-based Liquid Scintillator (WbLS) will be excellently suited for a measurement of the Diffuse Supernova Neutrino Background (DSNB). The WbLS technique offers high signal efficiency and effective suppression of the otherwise overwhelming background from neutral-current interactions of atmospheric neutrinos. To illustrate this, we investigate the DSNB sensitivity for two configurations of the future Theia detector by developing the expected signal and background rejection efficiencies along a full analysis chain. Based on a statistical analysis of the remaining signal and background rates, we find that a rather moderate exposure of 150 kt$\cdot$yrs will be sufficient to claim a ($5\sigma$) discovery of the faint DSNB signal for standard model assumptions. We conclude that, in comparison with other experimental techniques, WbLS offers the highest signal efficiency of more than 80% and best signal significance over background. \\ ( https://arxiv.org/abs/2007.14705 , 2315kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14733 (*cross-listing*) Date: Wed, 29 Jul 2020 10:43:38 GMT (397kb) Title: Gauging scale symmetry and inflation: Weyl versus Palatini gravity Authors: D. M. Ghilencea Categories: hep-th astro-ph.CO gr-qc hep-ph Comments: 17 pages, 7 figures, LaTeX \\ We present a comparative study of inflation in two theories of quadratic gravity with {\it gauged} scale symmetry: 1) the original Weyl quadratic gravity and 2) the theory defined by a similar action but in the Palatini approach, obtained by replacing the Weyl connection by its Palatini counterpart. These theories have different vectorial non-metricity induced by the gauge field ($\omega_\mu$) of this symmetry. In both theories, the Einstein-Proca action (of $\omega_\mu$), Planck scale and metricity emerge in the broken phase of this symmetry when $\omega_\mu$ acquires mass by Stueckelberg mechanism and decouples. The scalar potential in the presence of non-minimally coupled matter ($\phi_1$) is similar in both theories up to couplings and field rescaling. For small field values the potential is Higgs-like while for large fields inflation is possible. Due to an $R^2$ term in their action, both theories have a small but different tensor-to-scalar ratio ($r\sim 10^{-3}$), larger in the Palatini case. In both Weyl and Palatini theory with a fixed $n_s$, reducing the non-minimal coupling ($\xi_1$) increases $r$ which in Weyl theory is bounded from above by that of Starobinsky inflation. For a small enough $\xi_1\leq 10^{-3}$, unlike the Palatini case, Weyl quadratic gravity gives a dependence $r(n_s)$ on the spectral index ($n_s$) similar to that in Starobinsky inflation, while also protecting $r$ against higher dimensional operators corrections. \\ ( https://arxiv.org/abs/2007.14733 , 397kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14881 (*cross-listing*) Date: Wed, 29 Jul 2020 14:58:17 GMT (209kb,D) Title: Probing Massive Scalar/Vector Fields with Binary Pulsars Authors: Brian C. Seymour, Kent Yagi Categories: gr-qc astro-ph.HE Comments: 12 pages, 3 figures \\ Precision tests of general relativity can be conducted by observing binary pulsars. Theories with massive fields exist to explain a variety of phenomena from dark energy to the strong CP problem. Existing pulsar binaries, such as the white dwarf-pulsar binary J1738+0333, have been used to place stringent bounds on the scalar dipole emission, and radio telescopes may detect a pulsar orbiting a black hole in the future. In this paper, we study the ability of pulsar binaries to probe theories involving massive scalar and vector fields through the measurement of the orbital decay rate. With a generic framework, we describe corrections to orbital decay rate due to (a) modification of GR quadrupolar radiation and (b) dipolar radiation of a massive field. We then consider three concrete examples: (i) massive Brans-Dicke theory, (ii) general relativity with axions, and (iii) general relativity with bound dark matter and a dark force. Finally, we apply direct observations of J1738 and simulations of a black hole-pulsar binary to bound theory parameters such as field's mass and coupling constant. We find new constraints on bound dark matter interactions with PSR J1738, and a black hole-pulsar discovery would likely improve these further. Such bounds are complementary to future gravitational-wave bounds. Regarding other theories, we find similar constraints to previous pulsar measurements for massive Brans-Dicke theory and axions. These results show that new pulsar binaries will continue to allow for more stringent tests of gravity. \\ ( https://arxiv.org/abs/2007.14881 , 209kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14956 (*cross-listing*) Date: Wed, 29 Jul 2020 17:01:24 GMT (30kb,D) Title: Effective anisotropic stresses of the relic gravitons Authors: Massimo Giovannini Categories: hep-th astro-ph.CO gr-qc hep-ph Comments: 31 pages \\ The effective anisotropic stresses induced by the scalar modes of the geometry depend on the coordinate system so that the comparison of the competing results is ultimately determined by the evolution of the pivotal variables in each particular gauge. After arguing that the only reasonable physical coordinate systems for this problem are the ones where the gauge freedom is completely fixed (like the longitudinal and the uniform curvature gauges), we propose a novel gauge-invariant strategy for the comparison of gauge-dependent results. Instead of employing the pivotal variables of a given coordinate system, the effective anisotropic stress is solely expressed in terms of the gravitating normal modes of the plasma and in terms of their conformal time derivatives. The new approach is explicitly gauge-invariant and when the wavelengths of the normal modes are either shorter or larger than the sound horizon, the physical limits of the anisotropic stresses are determined without relying on the specific details of the background evolution. The relevance of the proposed strategy is discussed in the general situation where the scalar anisotropic stress and the non-adiabatic pressure fluctuations are simultaneously present. We finally argue that the anisotropic stress can be most efficiently obtained from the second-order effective action of the curvature inhomogeneities. \\ ( https://arxiv.org/abs/2007.14956 , 30kb) ------------------------------------------------------------------------------ \\ arXiv:2007.14978 (*cross-listing*) Date: Wed, 29 Jul 2020 17:45:13 GMT (2618kb,D) Title: Higgs inflation in Einstein-Cartan gravity Authors: Mikhail Shaposhnikov, Andrey Shkerin, Inar Timiryasov, Sebastian Zell Categories: hep-ph astro-ph.CO gr-qc hep-th Comments: 25 pages, 8 figures, 1 appendix \\ We study inflation driven by the Higgs field in the Einstein-Cartan formulation of gravity. In this theory, the presence of the Holst and Nieh-Yan terms with the Higgs field non-minimally coupled to them leads to three additional coupling constants. For a broad range of parameters, we find that inflation is both possible and consistent with observations. In most cases, the spectral index is given by $n_s=1-2/N_\star$ (with $N_\star$ the number of e-foldings) whereas the tensor-to-scalar ratio $r$ can vary between about $10^{-10}$ and $1$. Thus, there are scenarios of Higgs inflation in the Einstein-Cartan framework for which the detection of gravitational waves from inflation is possible in the near future. In certain limits, the known models of Higgs inflation in the metric and Palatini formulations of gravity are reproduced. Finally, we discuss the robustness of inflationary dynamics against quantum corrections due to the scalar and fermion fields. \\ ( https://arxiv.org/abs/2007.14978 , 2618kb) %%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%%--%% ------------------------------------------------------------------------------ \\ arXiv:1906.00913 (*cross-listing*) replaced with revised version Wed, 29 Jul 2020 13:58:57 GMT (117kb,D) Title: Compact binary coalescences: Constraints on waveforms Authors: Abhay Ashtekar, Tommaso De Lorenzo and Neev Khera Categories: gr-qc astro-ph.HE Comments: 19 pages, 1 figure. The main results are the same as in V1. Focus of the article improved by expanding the material addressed to the waveform community and dropping the one primarily addressed to mathematical relativists. Discussion section improved with preliminary new results. Typos corrected \\ ( https://arxiv.org/abs/1906.00913 , 117kb) ------------------------------------------------------------------------------ \\ arXiv:1906.11388 replaced with revised version Tue, 28 Jul 2020 23:37:02 GMT (2725kb,D) Title: Constraining Radio Mode Feedback in Galaxy Clusters with the Cluster Radio AGN Properties to z$\sim$1 Authors: N. Gupta, M. Pannella, J. J. Mohr, M. Klein, E. S. Rykoff, J. Annis, S. Avila, F. Bianchini, D. Brooks, E. Buckley-Geer, E. Bulbul, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, I. Chiu, M. Costanzi, L. N. da Costa, J. De Vicente, S. Desai, J. P. Dietrich, P. Doel, S. Everett, A. E. Evrard, J. Garc\'ia-Bellido, E. Gaztanaga, R. A. Gruendl, J. Gschwend, G. Gutierrez, D. L. Hollowood, K. Honscheid, D. J. James, T. Jeltema, K. Kuehn, C. Lidman, M. Lima, M. A. G. Maia, J. L. Marshall, M. McDonald, F. Menanteau, R. Miquel, R. L. C. Ogando, A. Palmese, F. Paz-Chinch\'on, A. A. Plazas, C. L. Reichardt, E. Sanchez, B. Santiago, A. Saro, V. Scarpine, R. Schindler, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, X. Shao, M. Smith, J. P. Stott, V. Strazzullo, E. Suchyta, M. E. C. Swanson, V. Vikram, et al. (1 additional author not shown) Categories: astro-ph.GA astro-ph.CO Comments: 20 pages, 15 figures Replaced with published version DOI: 10.1093/mnras/staa832 \\ ( https://arxiv.org/abs/1906.11388 , 2725kb) ------------------------------------------------------------------------------ \\ arXiv:1907.06545 replaced with revised version Wed, 29 Jul 2020 09:07:35 GMT (113kb) Title: Predictions for solar flares activity in solar cycle 25 Authors: Eleni Petrakou Categories: astro-ph.SR Comments: 5 pages, 2 figures; updated taking into account the start date for cycle 25 \\ ( https://arxiv.org/abs/1907.06545 , 113kb) ------------------------------------------------------------------------------ \\ arXiv:1907.10088 replaced with revised version Wed, 29 Jul 2020 13:26:34 GMT (1230kb) Title: New Insights into Uncertainties in the Relic Neutrino Background and Effects from the Nuclear Equation of State Authors: Grant J. Mathews, Luca Boccioli, Jun Hidaka, Toshitaka Kajino Categories: astro-ph.HE Comments: 19 pages, 9 figures, accepted to IJMPA. arXiv admin note: text overlap with arXiv:1405.0458 \\ ( https://arxiv.org/abs/1907.10088 , 1230kb) ------------------------------------------------------------------------------ \\ arXiv:1911.03856 replaced with revised version Wed, 29 Jul 2020 05:56:13 GMT (1755kb,D) Title: The hydroxyl satellite-line `flip' as a tracer of expanding HII regions Authors: Anita Petzler, Joanne R Dawson, Mark Wardle Categories: astro-ph.GA Comments: Accepted to MNRAS with significant revisions to the version previously uploaded to arXiv \\ ( https://arxiv.org/abs/1911.03856 , 1755kb) ------------------------------------------------------------------------------ \\ arXiv:1911.04465 replaced with revised version Wed, 29 Jul 2020 12:27:15 GMT (13135kb,D) Title: The Origin of Massive Stars: The Inertial-Inflow Model Authors: Paolo Padoan, Liubin Pan, Mika Juvela, Troels Haugb{\o}lle, {\AA}ke Nordlund Categories: astro-ph.GA astro-ph.SR Comments: 35 pages, 30 figures, ApJ in press \\ ( https://arxiv.org/abs/1911.04465 , 13135kb) ------------------------------------------------------------------------------ \\ arXiv:1912.11677 (*cross-listing*) replaced with revised version Wed, 29 Jul 2020 08:32:14 GMT (258kb,D) Title: Cosmic event horizons and the light-speed limit for relative radial motion Authors: Markus P\"ossel Categories: gr-qc astro-ph.CO Comments: 15 pages, 4 figures \\ ( https://arxiv.org/abs/1912.11677 , 258kb) ------------------------------------------------------------------------------ \\ arXiv:2001.03178 replaced with revised version Tue, 28 Jul 2020 22:07:46 GMT (5920kb,D) Title: The Formation Times and Building Blocks of Milky Way-mass Galaxies in the FIRE Simulations Authors: Isaiah B. Santistevan, Andrew Wetzel, Kareem El-Badry, Joss Bland-Hawthorn, Michael Boylan-Kolchin, Jeremy Bailin, Claude-Andre Faucher-Giguere, Samantha Benincasa Categories: astro-ph.GA astro-ph.CO Comments: 20 pages, 8 figures, accepted for publication in MNRAS \\ ( https://arxiv.org/abs/2001.03178 , 5920kb) ------------------------------------------------------------------------------ \\ arXiv:2002.01756 (*cross-listing*) replaced with revised version Wed, 29 Jul 2020 06:23:22 GMT (1166kb) Title: N=2 PNGB Quintessence Dark Energy Authors: Keunsu Cheon, Jungjai Lee Categories: gr-qc astro-ph.CO hep-ph hep-th Comments: 6 pages, 2 figures, minor revision \\ ( https://arxiv.org/abs/2002.01756 , 1166kb) ------------------------------------------------------------------------------ \\ arXiv:2003.02776 replaced with revised version Tue, 28 Jul 2020 21:09:22 GMT (320kb,D) Title: Does the mean-field alpha effect have any impact on the memory of the solar cycle? Authors: Soumitra Hazra, Allan Sacha Brun, Dibyendu Nandy Categories: astro-ph.SR Comments: Accepted in Astronomy and Astrophysics, 12 pages, 5 figures \\ ( https://arxiv.org/abs/2003.02776 , 320kb) ------------------------------------------------------------------------------ \\ arXiv:2003.05137 replaced with revised version Tue, 28 Jul 2020 20:18:04 GMT (661kb,D) Title: Relating the structure of dark matter halos to their assembly and environment Authors: Yangyao Chen, H.J. Mo, Cheng Li, Huiyuan Wang, Xiaohu Yang, Youcai Zhang, Kai Wang Categories: astro-ph.GA astro-ph.CO Comments: 22 pages, 11 figures, 2 tables. ApJ accepted. Comments are welcomed \\ ( https://arxiv.org/abs/2003.05137 , 661kb) ------------------------------------------------------------------------------ \\ arXiv:2003.08510 replaced with revised version Wed, 29 Jul 2020 00:44:05 GMT (3997kb,D) Title: An improved analysis framework for axion dark matter searches Authors: D. A. Palken, B. M. Brubaker, M. Malnou, S. Al Kenany, K. M. Backes, S. B. Cahn, Y. V. Gurevich, S. K. Lamoreaux, S. M. Lewis, R. H. Maruyama, N. M. Rapidis, J. R. Root, M. Simanovskaia, T. M. Shokair, Sukhman Singh, D. H. Speller, I. Urdinaran, K. van Bibber, L. Zhong and K. W. Lehnert Categories: astro-ph.IM hep-ex physics.data-an Comments: 22 pages, 5 figures Journal-ref: Phys. Rev. D 101, 123011 (2020) DOI: 10.1103/PhysRevD.101.123011 \\ ( https://arxiv.org/abs/2003.08510 , 3997kb) ------------------------------------------------------------------------------ \\ arXiv:2003.09325 replaced with revised version Wed, 29 Jul 2020 10:32:01 GMT (4269kb,D) Title: The changing-type SN 2014C may come from an 11-$M_\odot$ star stripped by binary interaction and violent eruption Authors: Ning-Chen Sun, Justyn R. Maund and Paul A. Crowther Categories: astro-ph.SR astro-ph.GA Comments: 19 pages, 13 figures, minor revision, accepted for publication in MNRAS \\ ( https://arxiv.org/abs/2003.09325 , 4269kb) ------------------------------------------------------------------------------ \\ arXiv:2004.00863 replaced with revised version Wed, 29 Jul 2020 11:37:12 GMT (8329kb,D) Title: First Structure Formation under the Influence of Gas-Dark Matter Streaming Velocity and Density: Impact of the Baryons-trace-dark matter Approximation Authors: Hyunbae Park, Kyungjin Ahn, Naoki Yoshida, Shingo Hirano Categories: astro-ph.CO astro-ph.GA Comments: Submitted to ApJ \\ ( https://arxiv.org/abs/2004.00863 , 8329kb) ------------------------------------------------------------------------------ \\ arXiv:2005.00440 replaced with revised version Wed, 29 Jul 2020 02:51:30 GMT (1122kb) Title: Rotating Convective Core Excites Non-Radial Pulsations to Cause Rotational Modulations in Early-Type Stars Authors: Umin Lee, Hideyuki Saio Categories: astro-ph.SR Comments: accepted for publication in MNRAS; 12 pages, 15 figures \\ ( https://arxiv.org/abs/2005.00440 , 1122kb) ------------------------------------------------------------------------------ \\ arXiv:2005.03034 replaced with revised version Tue, 28 Jul 2020 19:07:57 GMT (1875kb,D) Title: Modeling Radial Velocity Data of Resonant Planets to Infer Migration Histories Authors: Sam Hadden and Matthew J. Payne Categories: astro-ph.EP Comments: Revised in response to referee report and accepted to AJ; Code for RV fitting available online at https://github.com/shadden/ResonantPlanetPairsRVModeling \\ ( https://arxiv.org/abs/2005.03034 , 1875kb) ------------------------------------------------------------------------------ \\ arXiv:2005.06838 replaced with revised version Wed, 29 Jul 2020 11:44:39 GMT (7098kb,D) Title: Optimal Stereoscopic Angle for Reconstructing Solar Wind Inhomogeneous Structures Authors: Shaoyu Lyu, Xiaolei Li, Yuming Wang Categories: astro-ph.SR physics.space-ph Comments: 19 pages, 13 figures \\ ( https://arxiv.org/abs/2005.06838 , 7098kb) ------------------------------------------------------------------------------ \\ arXiv:2005.07710 replaced with revised version Wed, 29 Jul 2020 14:26:48 GMT (4237kb,D) Title: Flare Statistics for Young Stars from a Convolutional Neural Network Analysis of $\textit{TESS}$ Data Authors: Adina D. Feinstein, Benjamin T. Montet, Megan Ansdell, Brian Nord, Jacob L. Bean, Maximilian N. G\"unther, Michael A. Gully-Santiago, Joshua E. Schlieder Categories: astro-ph.SR astro-ph.IM Comments: 21 pages, 17 figures, 1 table, AJ accepted \\ ( https://arxiv.org/abs/2005.07710 , 4237kb) ------------------------------------------------------------------------------ \\ arXiv:2005.08010 (*cross-listing*) replaced with revised version Wed, 29 Jul 2020 16:55:26 GMT (37kb,D) Title: Gravitational Landau Damping for massive scalar modes Authors: Fabio Moretti, Flavio Bombacigno and Giovanni Montani Categories: gr-qc astro-ph.CO astro-ph.GA astro-ph.HE physics.plasm-ph Comments: 5 pages, 1 figure. Submitted to PRL \\ ( https://arxiv.org/abs/2005.08010 , 37kb) ------------------------------------------------------------------------------ \\ arXiv:2005.14175 replaced with revised version Wed, 29 Jul 2020 11:07:06 GMT (4309kb,D) Title: High-resolution observations of the solar photosphere, chromosphere and transition region. A database of coordinated IRIS and SST observations Authors: L.H.M. Rouppe van der Voort, B. De Pontieu, M. Carlsson, J. de la Cruz Rodriguez, S. Bose, G. Chintzoglou, A. Drews, C. Froment, M. Gosic, D.R. Graham, V.H. Hansteen, V.M.J. Henriques, S. Jafarzadeh, J. Joshi, L. Kleint, P. Kohutova, T. Leifsen, J. Martinez-Sykora, D. Nobrega-Siverio, A. Ortiz, T.M.D. Pereira, A. Popovas, C. Quintero Noda, A. Sainz Dalda, G.B. Scharmer, D. Schmit, E. Scullion, H. Skogsrud, M. Szydlarski, R. Timmons, G.J.M. Vissers, M.M. Woods, P. Zacharias Categories: astro-ph.SR Comments: Accepted for publication in Astronomy & Astrophysics (July 21, 2020) \\ ( https://arxiv.org/abs/2005.14175 , 4309kb) ------------------------------------------------------------------------------ \\ arXiv:2005.14208 replaced with revised version Tue, 28 Jul 2020 21:43:38 GMT (2275kb,D) Title: The landscape of disk outflows from black hole - neutron star mergers Authors: Rodrigo Fern\'andez, Francois Foucart, Jonas Lippuner Categories: astro-ph.HE astro-ph.SR gr-qc nucl-th Comments: Accepted by MNRAS with minor revisions DOI: 10.1093/mnras/staa2209 \\ ( https://arxiv.org/abs/2005.14208 , 2275kb) ------------------------------------------------------------------------------ \\ arXiv:2006.03582 replaced with revised version Wed, 29 Jul 2020 14:14:12 GMT (396kb,D) Title: The one that got away: A unique eclipse in the young brown dwarf Roque 12 Authors: Aleks Scholz (University of St Andrews, UK), Dirk Froebrich (University of Canterbury, UK), Koraljka Muzic (Universidade de Lisboa, Portugal), Jochen Eisl\"offel (TLS Tautenburg, Germany) Categories: astro-ph.SR astro-ph.EP Comments: 7 pages, 5 figures, 1 table, accepted for publication in Open Journal of Astrophysics DOI: 10.21105/astro.2006.03582 \\ ( https://arxiv.org/abs/2006.03582 , 396kb) ------------------------------------------------------------------------------ \\ arXiv:2006.04362 replaced with revised version Wed, 29 Jul 2020 00:52:09 GMT (733kb,D) Title: Narrow-Band Signal Localization for SETI on Noisy Synthetic Spectrogram Data Authors: Bryan Brzycki, Andrew P. V. Siemion, Steve Croft, Daniel Czech, David DeBoer, Julia DeMarines, Jamie Drew, Vishal Gajjar, Howard Isaacson, Brian Lacki, Matthew Lebofsky, David H. E. MacMahon, Imke de Pater, Danny C. Price, S. Pete Worden Categories: astro-ph.IM Comments: 12 pages, 10 figures, 1 table, submitted to PASP \\ ( https://arxiv.org/abs/2006.04362 , 733kb) ------------------------------------------------------------------------------ \\ arXiv:2006.08340 (*cross-listing*) replaced with revised version Tue, 28 Jul 2020 18:48:20 GMT (4661kb) Title: Lessons learned from (and since) the Voyager 2 flybys of Uranus and Neptune Authors: Heidi B. Hammel Categories: physics.pop-ph astro-ph.EP astro-ph.IM Comments: 13 pages, 6 figures, 1 table; to be published in Phil. Trans. R. Soc. A \\ ( https://arxiv.org/abs/2006.08340 , 4661kb) ------------------------------------------------------------------------------ \\ arXiv:2006.09795 replaced with revised version Wed, 29 Jul 2020 08:18:45 GMT (7437kb,D) Title: Herschel-PACS photometry of Uranus' five major moons Authors: \"O. H. Detre, T. G. M\"uller, U. Klaas, G. Marton, H. Linz and Z. Balog Categories: astro-ph.EP astro-ph.IM Comments: 25 pages, 10 figures, 7 tables, plus appendices. Accepted for publication on A&A \\ ( https://arxiv.org/abs/2006.09795 , 7437kb) ------------------------------------------------------------------------------ \\ arXiv:2006.10470 replaced with revised version Wed, 29 Jul 2020 03:08:36 GMT (319kb,D) Title: Awakening of two $\gamma$-ray high redshift flat-spectrum radio quasars in the southern hemisphere Authors: Shang Li, Lu-Ming Sun, Neng-Hui Liao and Yi-Zhong Fan Categories: astro-ph.HE Comments: 12 pages, 6 figures. Accepted for publication in ApJ \\ ( https://arxiv.org/abs/2006.10470 , 319kb) ------------------------------------------------------------------------------ \\ arXiv:2006.12984 replaced with revised version Wed, 29 Jul 2020 09:15:06 GMT (1636kb) Title: Hall cascade with fractional magnetic helicity in neutron star crusts Authors: Axel Brandenburg Categories: astro-ph.HE physics.flu-dyn Comments: 14 pages, 17 figures, 5 tables, submitted to ApJ Report-no: NORDITA-2020-063 \\ ( https://arxiv.org/abs/2006.12984 , 1636kb) ------------------------------------------------------------------------------ \\ arXiv:2006.14322 replaced with revised version Wed, 29 Jul 2020 11:26:56 GMT (2487kb,D) Title: Radiative cooling rates, ion fractions, molecule abundances and line emissivities including self-shielding and both local and metagalactic radiation fields Authors: Sylvia Ploeckinger, Joop Schaye Categories: astro-ph.GA Comments: Accepted for publication in MNRAS; 29 pages, 24 figures; for data files and more info see: https://www.sylviaploeckinger.com/radcool; minor changes to match published version \\ ( https://arxiv.org/abs/2006.14322 , 2487kb) ------------------------------------------------------------------------------ \\ arXiv:2006.14577 (*cross-listing*) replaced with revised version Wed, 29 Jul 2020 03:48:06 GMT (253kb,D) Title: Mirror Dark Matter and Electronic Recoil Events in XENON1T Authors: Lei Zu, Guan-Wen Yuan, Lei Feng, Yi-Zhong Fan Categories: hep-ph astro-ph.HE Comments: 4 pages, 3 figures \\ ( https://arxiv.org/abs/2006.14577 , 253kb) ------------------------------------------------------------------------------ \\ arXiv:2007.00847 replaced with revised version Tue, 28 Jul 2020 18:01:56 GMT (452kb,D) Title: Formation of mass gap objects in highly asymmetric mergers Authors: Mohammadtaher Safarzadeh, Abraham Loeb Categories: astro-ph.HE gr-qc Comments: Accepted for publication in ApJ Letters \\ ( https://arxiv.org/abs/2007.00847 , 452kb) ------------------------------------------------------------------------------ \\ arXiv:2007.01873 (*cross-listing*) replaced with revised version Wed, 29 Jul 2020 13:38:31 GMT (224kb,D) Title: Constraints on Axion-Lepton coupling from Big Bang Nucleosynthesis Authors: Diptimoy Ghosh, Divya Sachdeva Categories: hep-ph astro-ph.CO Comments: Minor improvement in the bounds; references and some more existing bounds added \\ ( https://arxiv.org/abs/2007.01873 , 224kb) ------------------------------------------------------------------------------ \\ arXiv:2007.04980 replaced with revised version Wed, 29 Jul 2020 14:30:25 GMT (1310kb,AD) Title: Dynamical Evidence of a Spiral Arm--Driving Planet in the MWC 758 Protoplanetary Disk Authors: Bin Ren, Ruobing Dong, Rob G. van Holstein, Jean-Baptiste Ruffio, Benjamin A. Calvin, Julien H. Girard, Myriam Benisty, Anthony Boccaletti, Thomas M. Esposito, \'Elodie Choquet, Dimitri Mawet, Laurent Pueyo, Tomas Stolker, Eugene Chiang, Jozua de Boer, John H. Debes, Antonio Garufi, Carol A. Grady, Dean C. Hines, Anne-Lise Maire, Fran\c{c}ois M\'enard, Maxwell Millar-Blanchaer, Marshall D. Perrin, Charles A. Poteet, Glenn Schneider Categories: astro-ph.EP astro-ph.SR Comments: 9 pages, 3 figures, published in ApJ Letters. Data files and gif movie of Figure 1ab in ancillary folder Journal-ref: ApJL 898 (2020) L38 DOI: 10.3847/2041-8213/aba43e \\ ( https://arxiv.org/abs/2007.04980 , 1310kb) ------------------------------------------------------------------------------ \\ arXiv:2007.06593 replaced with revised version Tue, 28 Jul 2020 21:25:34 GMT (782kb,D) Title: Exploring the origin of ultra-diffuse galaxies in clusters from their primordial alignment Authors: Yu Rong, Pavel E. Mancera Pi\~na, Elmo Tempel, Thomas H. Puzia, Sven De Rijcke Categories: astro-ph.GA Comments: Accepted for publication in MNRAS Letter DOI: 10.1093/mnrasl/slaa129 \\ ( https://arxiv.org/abs/2007.06593 , 782kb) ------------------------------------------------------------------------------ \\ arXiv:2007.06905 replaced with revised version Wed, 29 Jul 2020 15:12:10 GMT (552kb,D) Title: Gravitational Wave mergers as tracers of Large Scale Structures Authors: S. Libanore, M. C. Artale, D. Karagiannis, M. Liguori, N. Bartolo, Y. Bouffanais, N. Giacobbo, M. Mapelli, S. Matarrese Categories: astro-ph.CO Comments: 30 pages, 12 figures. Rewied version: author list updated; details on sky localization provided and included in the results discussion \\ ( https://arxiv.org/abs/2007.06905 , 552kb) ------------------------------------------------------------------------------ \\ arXiv:2007.08029 (*cross-listing*) replaced with revised version Wed, 29 Jul 2020 02:45:59 GMT (204kb,D) Title: Renormalization in gravitational leptogenesis with pseudo-scalar-tensor coupling Authors: Kohei Kamada, Jun'ya Kume, Yusuke Yamada Categories: hep-ph astro-ph.CO gr-qc hep-th Comments: 22 pages, 3 figures; v2: references are added Report-no: RESCEU-12/20 \\ ( https://arxiv.org/abs/2007.08029 , 204kb) ------------------------------------------------------------------------------ \\ arXiv:2007.08685 replaced with revised version Tue, 28 Jul 2020 23:53:15 GMT (4486kb) Title: Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs). IX. Identification of Two Red Quasars at z > 5.6 Authors: Nanako Kato, Yoshiki Matsuoka, Masafusa Onoue, Shuhei Koyama, Yoshiki Toba, Masayuki Akiyama, Seiji Fujimoto, Masatoshi Imanishi, Kazushi Iwasawa, Takuma Izumi, Nobunari Kashikawa, Toshihiro Kawaguchi, Chien-Hsiu Lee, Takeo Minezaki, Tohru Nagao, Akatoki Noboriguchi, and Michael A. Strauss Categories: astro-ph.GA Comments: Accepted for publication in PASJ \\ ( https://arxiv.org/abs/2007.08685 , 4486kb) ------------------------------------------------------------------------------ \\ arXiv:2007.11438 replaced with revised version Wed, 29 Jul 2020 13:44:34 GMT (1165kb,D) Title: A New Method For Studying Exoplanet Atmospheres Using Planetary Infrared Excess Authors: Kevin B. Stevenson Categories: astro-ph.EP astro-ph.IM Comments: Minor edits, Published in ApJL, 12 pages, 6 figures Journal-ref: ApJL 898 L35 (2020) DOI: 10.3847/2041-8213/aba68c \\ ( https://arxiv.org/abs/2007.11438 , 1165kb) ------------------------------------------------------------------------------ \\ arXiv:2007.12103 replaced with revised version Wed, 29 Jul 2020 12:24:25 GMT (1499kb) Title: An APEX survey of outflow and infall toward the youngest protostars in Orion Authors: Z. Nagy, A. Menechella, S. T. Megeath, J. J. Tobin, J. J. Booker, W. J. Fischer, P. Manoj, T. Stanke, A. Stutz, and F. Wyrowski Categories: astro-ph.GA Comments: Accepted for publication in A&A \\ ( https://arxiv.org/abs/2007.12103 , 1499kb) ------------------------------------------------------------------------------ \\ arXiv:2007.12193 replaced with revised version Wed, 29 Jul 2020 09:00:06 GMT (5961kb,D) Title: The impact of unresolved magnetic spots on high precision radial velocity measurements Authors: Maksym Lisogorskyi, Sudeshna Boro Saikia, Sandra V. Jeffers, Hugh R. A. Jones, Julien Morin, Matthew Mengel, Ansgar Reiners, Aline A. Vidotto, Pascal Petit Categories: astro-ph.EP astro-ph.SR Comments: Main text: 7 pages, 3 figures. Appendix: 6 pages, 6 figures. Author name typo corrected. Accepted for publication in MNRAS \\ ( https://arxiv.org/abs/2007.12193 , 5961kb) ------------------------------------------------------------------------------ \\ arXiv:2007.12705 replaced with revised version Wed, 29 Jul 2020 15:48:59 GMT (749kb,D) Title: Strong bound on canonical ultra-light axion dark matter from the Lyman-alpha forest Authors: Keir K. Rogers and Hiranya V. Peiris Categories: astro-ph.CO hep-ph Comments: 9 pages, 4 figures. Cross-references added \\ ( https://arxiv.org/abs/2007.12705 , 749kb) ------------------------------------------------------------------------------ \\ arXiv:2007.12712 replaced with revised version Tue, 28 Jul 2020 22:11:44 GMT (9115kb,D) Title: Lessons on Star-forming Ultra-diffuse Galaxies from The Stacked Spectra of Sloan Digital Sky Survey Authors: Yu Rong, Kai Zhu, Evelyn J. Johnston, Hong-Xin Zhang, Tianwen Cao, Thomas H. Puzia, Gaspar Galaz Categories: astro-ph.GA Comments: Accepted for publication in ApJL \\ ( https://arxiv.org/abs/2007.12712 , 9115kb) ------------------------------------------------------------------------------ \\ arXiv:2007.13751 replaced with revised version Wed, 29 Jul 2020 15:47:26 GMT (2708kb,D) Title: General framework for cosmological dark matter bounds using $N$-body simulations Authors: Keir K. Rogers and Hiranya V. Peiris Categories: astro-ph.CO Comments: 21 pages, 10 figures. Cross-references added \\ ( https://arxiv.org/abs/2007.13751 , 2708kb) ------------------------------------------------------------------------------ \\ arXiv:2007.13937 replaced with revised version Wed, 29 Jul 2020 03:19:50 GMT (11711kb,D) Title: Magnetic field fluctuations in anisotropic, supersonic turbulence Authors: James R. Beattie, Christoph Federrath, Amit Seta Categories: astro-ph.GA astro-ph.SR physics.flu-dyn Comments: 19 pages, 9 figures. Accepted for publication in MNRAS \\ ( https://arxiv.org/abs/2007.13937 , 11711kb) %%%---%%%---%%%---%%%---%%%---%%%---%%%---%%%---%%%---%%%---%%%---%%%---%%%--- For subscribe options to combined physics archives, e-mail To: physics@arxiv.org, Subject: subscribe ----------------------------------------------------------------------------- For help on viewing and making submissions, see http://arxiv.org/help/