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New submissions for Thu, 16 Jan 20

[1]  arXiv:2001.04983 [pdf, other]

Title: A bound on the 12C/13C ratio in near-pristine gas with ESPRESSO

Authors: Louise Welsh, Ryan Cooke, Michele Fumagalli, Max Pettini

Comments: 13 pages, 8 figures, submitted to MNRAS

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

Using science verification observations obtained with ESPRESSO at the Very Large Telescope (VLT) in 4UT mode, we report the first bound on the carbon isotope ratio 12C/13C of a quiescent, near-pristine damped Ly-alpha (DLA) system at z=2.34. We recover a limit log10(12C/13C) > +0.37 (2 sigma). We use the abundance pattern of this DLA, combined with a stochastic chemical enrichment model, to infer the properties of the enriching stars, finding the total gas mass of this system to be log10(M_gas/M_sun)=6.3+1.4-0.9 and the total stellar mass to be log10(M_*/M_sun)=4.8+/-1.3. The current observations disfavour enrichment by metal-poor Asymptotic Giant Branch (AGB) stars with masses <2.4 Msun, limiting the epoch at which this DLA formed most of its enriching stars. Our modelling suggests that this DLA formed very few stars until >1 Gyr after the cosmic reionization of hydrogen and, despite its very low metallicity (~1/1000 of solar), this DLA appears to have formed most of its stars in the past few hundred Myr. Combining the inferred star formation history with evidence that some of the most metal-poor DLAs display an elevated [C/O] ratio at redshift z<3, we suggest that very metal-poor DLAs may have been affected by reionization quenching. Finally, given the simplicity and quiescence of the absorption features associated with the DLA studied here, we use these ESPRESSO data to place a bound on the possible variability of the fine-structure constant, Delta alpha/alpha=(-1.2 +/- 1.1)x10^-5.

[2]  arXiv:2001.04984 [pdf, other]

Title: Dynamical structure of small bulges reveals their early formation in ΛCDM paradigm

Authors: Luca Costantin, Jairo Méndez-Abreu, Enrico M. Corsini, Lorenzo Morelli, Adriana de Lorenzo-Cáceres, Ilaria Pagotto, Virginia Cuomo, J. Alfonso L. Aguerri, Michela Rubino

Comments: 7 pages, 1 figure, accepted for publication in ApJL

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

The {\Lambda} cold dark matter ({\Lambda}CDM) paradigm of galaxy formation predicts that dense spheroidal stellar structures invariably grow at early cosmic time. These primordial spheroids evolve toward a virialized dynamical status as they finally become today's elliptical galaxies and large bulges at the center of disk galaxies. However, observations reveal that small bulges in spiral galaxies are common in the nearby universe. The prevailing belief that all small bulges form at later times from internal processes occurring in the disk represents a challenge for the {\Lambda}CDM scenario. Notably, the coevolution of bulges and central supermassive black holes (SMBHs) at early phases of galaxy evolution is also at stake. However, observations have so far not provided conclusive evidence against their possible early origin. Here, we report new observations of small bulges showing that they follow the mass-velocity dispersion relation expected for virialized systems. Contrary to previous claims, small bulges bridge the gap between massive ellipticals and globular clusters. This dynamical picture supports a scenario where systems over seven orders of magnitude in stellar mass form at early cosmic time. These results alleviate the tension between {\Lambda}CDM simulations and observations at galactic scales. We hypothesize that these small bulges are actually the low-mass descendants of compact objects observed at high redshift, also known as red nuggets, which are consistently produced in cosmological {\Lambda}CDM simulations. Therefore, this also suggests that the established coevolution of SMBHs and large bulges naturally extends to spheroids in the low-mass regime.

[3]  arXiv:2001.04985 [pdf, other]

Title: Linking Macro, Meso, and Micro Scales in Multiphase AGN Feeding and Feedback

Authors: M. Gaspari, F. Tombesi, M. Cappi

Comments: Published in Nature Astronomy (authors' version after final referee iteration)

Journal-ref: Nat Astron 4, 10-13 (2020)

Subjects: Astrophysics of Galaxies (astro-ph.GA); Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Astrophysical Phenomena (astro-ph.HE); Plasma Physics (physics.plasm-ph)

Supermassive black hole (SMBH) feeding and feedback processes are often considered as disjoint and studied independently at different scales, both in observations and simulations. We encourage to adopt and unify three physically-motivated scales for feeding and feedback (micro - meso - macro ~ mpc - kpc - Mpc), linking them in a tight multiphase self-regulated loop. We pinpoint the key open questions related to this global SMBH unification problem, while advocating for the extension of novel mechanisms best observed in massive halos (such as chaotic cold accretion) down to low-mass systems. To solve such challenges, we provide a set of recommendations that promote a multiscale, multiwavelength, and interdisciplinary community.

[4]  arXiv:2001.04988 [pdf, other]

Title: The Pristine survey VIII: The metallicity distribution function of the Milky Way halo down to the extremely metal-poor regime

Authors: K. Youakim, E. Starkenburg, N. F. Martin, G. Matijevic, D. S. Aguado, C. Allende Prieto, A. Arentsen, P. Bonifacio, R. G. Carlberg, J. I. González Hernández, V. Hill, G. Kordopatis, C. Lardo, J. F. Navarro, P. Jablonka, R. Sánchez Janssen, F. Sestito, G. F. Thomas

Comments: 17 pages, 12 figures, 5 tables, accepted for publication in MNRAS

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

The Pristine survey uses narrow-band photometry to derive precise metallicities down to the extremely metal-poor regime ([Fe/H] < -3), and currently consists of over 4 million FGK-type stars over a sky area of $\sim 2~500\, \mathrm{deg}^2$. We focus our analysis on a subsample of $\sim 80~000$ main sequence turnoff stars with heliocentric distances between 6 and 20 kpc, which we take to be a representative sample of the inner halo. The resulting metallicity distribution function (MDF) has a peak at [Fe/H] = -1.6, and a slope of $\Delta$(LogN)/$\Delta[Fe/H] = 1.0 \pm 0.1$ in the metallicity range of -3.4 < [Fe/H] < -2.5. This agrees well with a simple closed-box chemical enrichment model in this range, but is shallower than previous spectroscopic MDFs presented in the literature, suggesting that there may be a larger proportion of metal-poor stars in the inner halo than previously reported. We identify the Monoceros/TriAnd/ACS/EBS/A13 structure in metallicity space in a low latitude field in the anticenter direction, and also discuss the possibility that the inner halo is dominated by a single, large merger event, but cannot strongly support or refute this idea with the current data. Finally, based on the MDF of field stars, we estimate the number of expected metal-poor globular clusters in the Milky Way halo to be 5.4 for [Fe/H] < -2.5 and 1.5 for [Fe/H] < -3, suggesting that the lack of low metallicity globular clusters in the Milky Way is not due simply to statistical undersampling.

[5]  arXiv:2001.04989 [pdf, other]

Title: A large, deep 3 deg$^2$ survey of H$α$, [OIII], and [OII] emitters from LAGER: constraining luminosity functions

Authors: Ali Ahmad Khostovan, Sangeeta Malhotra, James E. Rhoads, Chunyan Jiang, Junxian Wang, Isak Wold, Zhen-Ya Zheng, L. Felipe Barrientos, Alicia Coughlin, Santosh Harish, Weida Hu, Leopoldo Infante, Lucia A. Perez, John Pharo, Francisco Valdes, Alistair R. Walker, Huan Yang

Comments: 21 pages, 12 figures, 6 Tables. Accepted by MNRAS for publication on 6 Jan 2020

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

We present our measurements of the H$\alpha$, [OIII], and [OII] luminosity functions as part of the Lyman Alpha Galaxies at Epoch of Reionization (LAGER) survey using our samples of 1577 $z = 0.47$ H$\alpha$-, 3933 $z = 0.93$ [OIII]-, and 5367 $z = 1.59$ [OII]-selected emission line galaxies in a single 3 deg$^2$ CTIO/Blanco DECam pointing of the COSMOS field. Our observations reach 5$\sigma$ depths of $8.2\times10^{-18}$ erg s$^{-1}$ cm$^{-2}$ and comoving volumes of $(1-7)\times10^{5}$ Mpc$^3$ making our survey one of the deepest narrowband surveys. We measure the observed luminosity functions and find best-fits of $\phi^\star = 10^{-3.16\pm0.09}$ Mpc$^{-3}$ and $L^\star = 10^{41.72\pm0.09}$ erg s$^{-1}$ for H$\alpha$, $\phi^\star = 10^{-2.16^{+0.10}_{-0.12}}$ Mpc$^{-3}$ and $L^\star = 10^{41.38^{+0.07}_{-0.06}}$ erg s$^{-1}$ for [OIII], and $\phi^\star = 10^{-1.97^{+0.07}_{-0.07}}$ Mpc$^{-3}$ and $L^\star = 10^{41.66\pm0.03}$ erg s$^{-1}$ for [OII], with $\alpha$ fixed to $-1.75$, $-1.6$, and $-1.3$, respectively. An excess of bright $> 10^{42}$ erg s$^{-1}$ [OIII] emitters is observed and may be due to AGN contamination. Dust corrections are applied assuming $A_{\rm{H}\alpha} = 1$ mag. We also design our own empirical rest-frame $g - r$ calibration using SDSS DR12 data, test it against our $z = 0.47$ H$\alpha$ emitters with $z$COSMOS $1$D spectra, and calibrate it for $(g - r)$ between $-0.8$ and $1.3$ mag. Dust and AGN-corrected star formation rate densities (SFRDs) are measured as $\log_{10}\rho_{\rm{SFR}}/(\rm{M}_\odot\ \rm{yr}^{-1}\ \rm{Mpc}^{-3}) = -1.63\pm0.04$, $-1.07\pm0.06$, and $-0.90\pm0.10$ for H$\alpha$, [OIII], and [OII], respectively. We find our [OIII] and [OII] samples fully trace cosmic star formation activity at their respective redshifts in comparison to multi-wavelength SFRDs, while the H$\alpha$ sample traces $\sim 70$ percent of the total $z = 0.47$ SFRD.

[6]  arXiv:2001.04992 [pdf, other]

Title: A redshift-dependent IRX-$β$ dust attenuation relation for TNG50 galaxies

Authors: Sebastian Schulz, Gergö Popping, Annalisa Pillepich, Dylan Nelson, Mark Vogelsberger, Federico Marinacci, Lars Hernquist

Comments: The paper has been submitted to MNRAS and is currently undergoing review. Comments are welcome

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

We study the relation between the UV-slope, $\beta$, and the ratio between the IR and UV luminosities of galaxies, IRX, using TNG50, the latest installment of the IllustrisTNG galaxy formation simulations. We select 7280 TNG50 star-forming galaxies with stellar mass above $10^9M_\odot$ at selected redshifts, $0 \leq z \leq 4$, and perform radiative transfer calculations with SKIRT to model the effects of ISM dust on the simulated stellar light. We adopt a Milky Way (MW) type dust and a fixed dust-to-metal ratio of 0.3 throughout and find that TNG50 star-forming main-sequence galaxies agree with the empirically-derived reference IRX-$\beta$ relations at $z \lesssim 1$. There appears to be a redshift-dependent systematic offset with respect to the reference relations, with the TNG50 IRX-$\beta$ median relation steepening towards higher redshifts. This is to first order driven by variations in intrinsic UV-slopes due to different star-formation histories of galaxies selected at different cosmic epochs. Once differences in the intrinsic UV-slope are corrected for, TNG50 galaxies exhibit a scatter of 0.3 dex in IRX at fixed $\beta$ at all studied redshifts. These galaxy-to-galaxy variations are correlated with intrinsic galaxy properties, such that at fixed UV-slope galaxies with higher star--formation rates, star--formation efficiencies, gas metallicities, and stellar masses exhibit larger IRX values. We additionally demonstrate a degeneracy between stellar age and dust type. The combination of young stellar population age with a SMC type of dust for high-redshift ($z=4$) TNG50 galaxies can result in an IRX-$\beta$ relation similar to what is found for low-redshift galaxies with MW dust. This hampers the use of the IRX-$\beta$ relation as a proxy for dust type. We provide a redshift-dependent fitting function for the IRX-$\beta$ relation with MW dust based on our numerical models.

[7]  arXiv:2001.04994 [pdf, other]

Title: Bounds on secret neutrino interactions from high-energy astrophysical neutrinos

Authors: Mauricio Bustamante, Charlotte Amalie Rosenstroem, Shashank Shalgar, Irene Tamborra (Bohr Inst. & U. Copenhagen (main) & DARK)

Comments: 8 pages, 5 figures, technical appendix

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

Neutrinos offer a window to physics beyond the Standard Model. In particular, high-energy astrophysical neutrinos, with TeV-PeV energies, may provide evidence of new, "secret" neutrino-neutrino interactions that are stronger than ordinary weak interactions. During their propagation over cosmological distances, high-energy neutrinos could interact with the cosmic neutrino background via secret interactions, developing characteristic energy-dependent features in their observed energy distribution. For the first time, we look for signatures of secret neutrino interactions in the diffuse flux of high-energy astrophysical neutrinos, using 6 years of publicly available IceCube High Energy Starting Events (HESE). We find no significant evidence for secret neutrino interactions, but place competitive upper limits on the coupling strength of the new mediator through which they occur, in the mediator mass range of 1-100 MeV.

[8]  arXiv:2001.04997 [pdf, other]

Title: Detection of Irregular, Sub-mm Opaque Structures in the Orion Molecular Clouds: Protostars within 10000 years of formation?

Authors: Nicole Karnath, S. T. Megeath, John Tobin, Amelia Stutz, Zhi-Yun Li, Patrick Sheehan, Nick Reynolds, Sarah Sadavoy, Ian Stephens, Mayra Osorio, Guillem Anglada, Ana Diaz-Rodriguez, Eric Cox

Comments: accepted by ApJ, 22 pages, 11 figures, 5 tables

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

We report ALMA and VLA continuum observations that potentially identify the four youngest protostars in the Orion Molecular Clouds taken as part of the Orion VANDAM program. These are distinguished by bright, extended, irregular emission at 0.87 mm and 8 mm and are optically thick at 0.87 mm. These structures are distinct from the disk or point-like morphologies seen toward the other Orion protostars. The 0.87 mm emission implies temperatures of 41-170 K, requiring internal heating. The bright 8 mm emission implies masses of 0.5 to 1.2 M_sun assuming standard dust opacity models. One source has a Class 0 companion, while another exhibits substructure indicating a companion-candidate. Three compact outflows are detected, two of which may be driven by companions, with dynamical times of ~300 to ~400 years. The slowest outflow may be driven by a first hydrostatic core. These protostars appear to trace an early phase when the centers of collapsing fragments become optically thick to their own radiation and compression raises the gas temperature. This phase is thought to accompany the formation of hydrostatic cores. A key question is whether these structures are evolving on free fall times of ~100 years, or whether they are evolving on Kelvin-Helmholtz times of several thousand years. The number of these sources imply a lifetime of ~6000 years, in closer agreement with the Kelvin-Helmholtz time. In this case, rotational and/or magnetic support could be slowing the collapse.

[9]  arXiv:2001.05002 [pdf, other]

Title: CHAOS IV: Gas-Phase Abundance Trends From The First Four CHAOS Galaxies

Authors: Danielle A. Berg, Richard W. Pogge, Evan D. Skillman, Kevin V. Croxall, John Moustakas, Noah S.J. Rogers, Jiayi Sun

Comments: Accepted for publication in ApJ

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

The chemical abundances of spiral galaxies, as probed by HII regions across their disks, are key to understanding the evolution of galaxies over a wide range of environments. We present LBT/MODS spectra of 52 HII regions in NGC3184 as part of the CHemical Abundances Of Spirals (CHAOS) project. We explore the direct-method gas-phase abundance trends for the first four CHAOS galaxies, using temperature measurements from one or more auroral line detections in 190 individual HII regions. We find the dispersion in Te-Te relationships is dependent on ionization, as characterized by F_5007/F_3727, and so recommend ionization-based temperature priorities for abundance calculations. We confirm our previous results that [NII] and [SIII] provide the most robust measures of electron temperature in low-ionization zones, while [OIII] provides reliable electron temperatures in high-ionization nebula. We measure relative and absolute abundances for O, N, S, Ar, and Ne. The four CHAOS galaxies marginally conform with a universal O/H gradient, as found by empirical IFU studies when plotted relative to effective radius. However, after adjusting for vertical offsets, we find a tight universal N/O gradient of alpha_N/O = -0.33 dex/Re with sigma_tot. = 0.08 for Rg/Re < 2.0, where N is dominated by secondary production. Despite this tight universal N/O gradient, the scatter in the N/O-O/H relationship is significant. Interestingly, the scatter is similar when N/O is plotted relative to O/H or S/H. The observable ionic states of S probe lower ionization and excitation energies than O, which might be more appropriate for characterizing abundances in metal-rich HII regions.

[10]  arXiv:2001.05003 [pdf, other]

Title: The ALMaQUEST Survey: II. What drives central starbursts at z~0?

Authors: Sara L. Ellison, Mallory D. Thorp, Hsi-An Pan, Lihwai Lin, Jillian M. Scudder, Asa F. L. Bluck, Sebastian F. Sanchez, Mark Sargent

Comments: Accepted for publication in MNRAS

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

Starburst galaxies have elevated star formation rates (SFRs) for their stellar mass. In Ellison et al. (2018) we used integral field unit (IFU) maps of star formation rate surface density (Sigma_SFR) and stellar mass surface density (Sigma_*) to show that starburst galaxies in the local universe are driven by SFRs that are preferentially boosted in their central regions. Here, we present molecular gas maps obtained with the Atacama Large Millimeter Array (ALMA) observatory for 12 central starburst galaxies at z~0 drawn from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey. The ALMA and MaNGA data are well matched in spatial resolution, such that the ALMA maps of molecular gas surface density (Sigma_H2) can be directly compared with MaNGA maps at kpc-scale resolution. The combination of Sigma_H2, Sigma_* and Sigma_SFR at the same resolution allow us to investigate whether central starbursts are driven primarily by enhancements in star formation efficiency (SFE) or by increased gas fractions. By computing offsets from the resolved Kennicutt-Schmidt relation (Sigma_H2 vs. Sigma_SFR) and the molecular gas main sequence (Sigma_* vs. Sigma_H2), we conclude that the primary driver of the central starburst is an elevated SFE. We also show that the enhancement in Sigma_SFR is accompanied by a dilution in O/H, consistent with a triggering that is induced by metal poor gas inflow. These observational signatures are found in both undisturbed (9/12 galaxies in our sample) and recently merged galaxies, indicating that both interactions and secular mechanisms contribute to central starbursts.

[11]  arXiv:2001.05004 [pdf, other]

Title: The Observational Anatomy of Externally Photoevaporating Planet-Forming Discs I: Atomic Carbon

Authors: Thomas J. Haworth, James E. Owen

Comments: 12 pages, accepted for publication in MNRAS

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

We demonstrate the utility of CI as a tracer of photoevaporative winds that are being driven from discs by their ambient UV environment. Commonly observed CO lines only trace these winds in relatively weak UV environments and is otherwise dissociated in the wind at the intermediate to high UV fields that most young stars experience. However, CI traces unsubtle kinematic signatures of a wind in intermediate UV environments ($\sim1000$G$_0$) and can be used to place constraints on the kinematics and temperature of the wind. In CI position-velocity diagrams external photoevaporation results in velocities that are faster than those from Keplerian rotation alone, as well as emission from quadrants of position-velocity space in which there would be no Keplerian emission. This is independent of viewing angle because the wind has components that are perpendicular to the azimuthal rotation of the disc. At intermediate viewing angles ($\sim 30-60^\circ$) moment 1 maps also exhibit a twisted morphology over large scales (unlike other processes that result in twists, which are typically towards the inner disc). CI is readily observable with ALMA, which means that it is now possible to identify and characterise the effect of external photoevaporation on planet-forming discs in intermediate UV environments.

[12]  arXiv:2001.05007 [pdf, other]

Title: Observations of Protoplanetary Disk Structures

Authors: Sean M. Andrews

Comments: invited review to be published in Annual Reviews of Astronomy and Astrophysics; 43 pages, 13 figures

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

The disks that orbit young stars are the essential conduits and reservoirs of material for star and planet formation. Their structures, meaning the spatial variations of the disk physical conditions, reflect the underlying mechanisms that drive those formation processes. Observations of the solids and gas in these disks, particularly at high resolution, provide fundamental insights on their mass distributions, dynamical states, and evolutionary behaviors. Over the past decade, rapid developments in these areas have largely been driven by observations with the Atacama Large Millimeter/submillimeter Array (ALMA). This review highlights the state of observational research on disk structures, emphasizing three key conclusions that reflect the main branches of the field: (1) Relationships among disk structure properties are also linked to the masses, environments, and evolutionary states of their stellar hosts; (2) There is clear, qualitative evidence for the growth and migration of disk solids, although the implied evolutionary timescales suggest the classical assumption of a smooth gas disk is inappropriate; and (3) Small-scale substructures with a variety of morphologies, locations, scales, and amplitudes -- presumably tracing local gas pressure maxima -- broadly influence the physical and observational properties of disks. The last point especially is reshaping the field, with the recognition that these disk substructures likely trace active sites of planetesimal growth or are the hallmarks of planetary systems at their formation epoch.

[13]  arXiv:2001.05020 [pdf, ps, other]

Title: NuSTAR Observations and multi-wavelength modeling of the high-redshift BL Lac Object 4FGL J2146.5-1344

Authors: M. Rajagopal (1 and 2), L. Marcotulli (1), M. Ajello (1), A. Kaur (3), V. Paliya (4), D. Hartmann (1 and 2) ((1) Department of Physics and Astronomy, Clemson University (2) Southeastern Association for Research in Astronomy (SARA), (3) Department of Astronomy and Astrophysics, Pennsylvania State University (4) Deutsches Elektronen-Synchrotron DESY, Germany)

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

High synchrotron peak (HSP; $\nu_{sy}^{pk} > 10^{15}$\,Hz) BL Lacs are some of the most extreme accelerators in the Universe. Those found at high redshifts ($z>1$) challenge our understanding of blazar evolution models and are crucial for cosmological measurements of the Extragalactic Background Light. In this paper, we study a high-$z$ BL Lac, 4FGL J2146.5-1344, detected to be at $z$=1.34 using the photometric dropout technique. We collected multi-wavelength data for this source from optical up to $\gamma$-rays, in order to study its spectral energy distribution (SED). In particular, this source was observed for the first time with {\it NuSTAR}, which accurately measures the synchrotron emission of this blazar up to 50\,keV. Despite being classified as an HSP BL Lac object, the modeling of the SED reveals that this source likely belongs to the ``masquerading BL Lac" class, which comprises of FSRQs appearing as disguised BL Lac objects.

[14]  arXiv:2001.05025 [pdf]

Title: A unified theory of cataclysmic variables from self-consistent numerical simulations

Authors: Yael Hillman, Michael M. Shara, Dina Prialnik, Attay Kovetz

Comments: 23 pages, 4 figures, submitted to Nature Astronomy

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

The hydrogen-rich envelopes accreted by white dwarf stars from their red dwarf companions lead to thermonuclear runaways observed as classical nova eruptions peaking at up to 1 Million solar luminosities. Virtually all nova progenitors are novalike binaries exhibiting high rates of mass transfer to their white dwarfs before and after an eruption. It is a puzzle that binaries indistinguishable from novalikes, but with much lower mass transfer rates, and resulting dwarf nova outbursts, co-exist at the same orbital periods. Nova shells surrounding several dwarf novae demonstrate that at least some novae become dwarf novae between successive nova eruptions, though the mechanisms and timescales governing mass transfer rate variations are poorly understood. Here we report simulations of the multiGyr evolution of novae which self-consistently model every eruption's thermonuclear runaway, mass and angular momentum losses, feedback due to irradiation and variable mass transfer, and orbital size and period changes. The simulations reproduce the observed wide range of mass transfer rates at a given orbital period, with large and cyclic changes in white dwarf-red dwarf binaries emerging on kyr to Myr timescales. They also demonstrate that deep hibernation, (complete stoppage of mass transfer for long periods), occurs only in short-period binaries; that initially very different binaries converge to become nearly identical systems; that while almost all prenovae should be novalike binaries, dwarf novae should also occasionally be observed to give rise to novae; and that the masses of white dwarfs decrease only slightly while their red dwarf companions are consumed.

[15]  arXiv:2001.05030 [pdf, other]

Title: Peter Pan Disks: Long-lived Accretion Disks Around Young M Stars

Authors: Steven M. Silverberg, John P. Wisniewski, Marc J. Kuchner, Kellen D. Lawson, Alissa S. Bans, John H. Debes, Joseph R. Biggs, Milton K.D. Bosch, Katharina Doll, Hugo A. Durantini Luca, Alexandru Enachioaie, Joshua Hamilton, Jonathan Holden, Michiharu Hyogo, the Disk Detective Collaboration

Comments: 25 pages, 17 figures. Accepted for publication in the Astrophysical Journal

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

WISEA J080822.18-644357.3, an M star in the Carina association, exhibits extreme infrared excess and accretion activity at an age greater than the expected accretion disk lifetime. We consider J0808 as the prototypical example of a class of M star accretion disks at ages $\gtrsim 20$ Myr, which we call ``Peter Pan'' disks, since they apparently refuse to grow up. We present four new Peter Pan disk candidates identified via the Disk Detective citizen science project, coupled with \textit{Gaia} astrometry. We find that WISEA J044634.16-262756.1 and WISEA J094900.65-713803.1 both exhibit significant infrared excess after accounting for nearby stars within the 2MASS beams. The J0446 system has $>95\%$ likelihood of Columba membership. The J0949 system shows $>95\%$ likelihood of Carina membership. We present new GMOS optical spectra of all four objects, showing possible accretion signatures on all four stars. We present ground-based and \textit{TESS} lightcurves of J0808 and 2MASS J0501-4337, including a large flare and aperiodic dipping activity on J0808, and strong periodicity on J0501. We find Pa$\beta$ and Br$\gamma$ emission indicating ongoing accretion in near-IR spectroscopy of J0808. Using observed characteristics of these systems, we discuss mechanisms that lead to accretion disks at ages $\gtrsim20$ Myr, and find that these objects most plausibly represent long-lived CO-poor primordial disks, or ``hybrid'' disks, exhibiting both debris- and primordial-disk features. The question remains: why have gas-rich disks persisted so long around these particular stars?

[16]  arXiv:2001.05037 [pdf, other]

Title: An accurate, extensive, and practical line list of methane for the HITEMP database

Authors: Robert J. Hargreaves, Iouli E. Gordon, Michael Rey, Andrei V. Nikitin, Vladimir G. Tyuterev, Roman V. Kochanov, Laurence S. Rothman

Comments: 25 pages, 12 figures, submitted to the Astrophysical Journal Supplement Series

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

A methane line list for the HITEMP spectroscopic database, covering 0-13,400 cm$^{-1}$ ($>$746 nm), is presented. To create this compilation, ab initio line lists of $^{12}$CH$_{4}$ from Rey et al. (2017) ApJ, 847, 105 (provided at separate temperatures in the TheoReTS information system), are now combined with HITRAN2016 methane data to produce a single line list suitable for high-temperature line-by-line calculations up to 2000 K. An effective-temperature interpolation model was created in order to represent continuum-like features at any temperature of interest. This model is advantageous to previously-used approaches that employ so-called ``super-lines'', which are suitable only at a given temperature and require separate line lists for different temperatures. The resultant HITEMP line list contains $\sim$32 million lines and is significantly more flexible than alternative line lists of methane, while accuracy required for astrophysical or combustion applications is retained. Comparisons against experimental observations of methane absorption at high temperatures have been used to demonstrate the accuracy of the new work. The line list includes both strong lines and quasi-continuum features and is provided in the common user-friendly HITRAN/HITEMP format, making it the most practical methane line list for radiative transfer modeling at high-temperature conditions.

[17]  arXiv:2001.05047 [pdf, other]

Title: [CI](1-0) and [CI](2-1) in resolved local galaxies

Authors: Alison F. Crocker, Eric Pellegrini, J.-D. T. Smith, Bruce T. Draine, Christine D. Wilson, Mark Wolfire, Lee Armus, Elias Brinks, Daniel A. Dale, Brent Groves, Rodrigo Herrera-Camus, Leslie K. Hunt, Robert C. Kennicutt, Eric J. Murphy, Karin Sandstrom, Eva Schinnerer, Dimitra Rigopoulou, Erik Rosolowsky, Paul van der Werf

Comments: 15 pages, 10 figures, published in ApJ

Journal-ref: The Astrophysical Journal 887 (2019) 105

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

We present resolved [CI] line intensities of 18 nearby galaxies observed with the SPIRE FTS spectrometer on the Herschel Space Observatory. We use these data along with resolved CO line intensities from $J_\mathrm{up} = 1$ to 7 to interpret what phase of the interstellar medium the [CI] lines trace within typical local galaxies. A tight, linear relation is found between the intensities of the CO(4-3) and [CI](2-1) lines; we hypothesize this is due to the similar upper level temperature of these two lines. We modeled the [CI] and CO line emission using large velocity gradient models combined with an empirical template. According to this modeling, the [CI](1-0) line is clearly dominated by the low-excitation component. We determine [CI] to molecular mass conversion factors for both the [CI](1-0) and [CI](2-1) lines, with mean values of $\alpha_{\mathrm{[CI](1-0)}} = 7.3$ M$_{\mathrm{sun}}$ K$^{-1}$ km$^{-1}$ s pc$^{-2}$ and $\alpha_{\mathrm{[CI](2-1)}} = 34 $ M$_{\mathrm{sun}}$ K$^{-1}$ km$^{-1}$ s pc$^{-2}$ with logarithmic root-mean-square spreads of 0.20 and 0.32 dex, respectively. The similar spread of $\alpha_{\mathrm{[CI](1-0)}}$ to $\alpha_{\mathrm{CO}}$ (derived using the CO(2-1) line) suggests that [CI](1-0) may be just as good a tracer of cold molecular gas as CO(2-1) in galaxies of this type. On the other hand, the wider spread of $\alpha_{\mathrm{[CI](2-1)}}$ and the tight relation found between [CI](2-1) and CO(4-3) suggest that much of the [CI](2-1) emission may originate in warmer molecular gas.

[18]  arXiv:2001.05048 [pdf, other]

Title: Limits on Mode Coherence in Pulsating DA White Dwarfs Due to a Non-static Convection Zone

Authors: M. H. Montgomery, J. J. Hermes, D. E. Winget, B. H. Dunlap, K. J. Bell

Comments: 11 pages, 11 figures, accepted for publication in ApJ

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

The standard theory of pulsations deals with the frequencies and growth rates of infinitesimal perturbations in a stellar model. Modes which are calculated to be linearly driven should increase their amplitudes exponentially with time; the fact that nearly constant amplitudes are usually observed is evidence that nonlinear mechanisms inhibit the growth of finite amplitude pulsations. Models predict that the mass of convection zones in pulsating hydrogen-atmosphere (DAV) white dwarfs is very sensitive to temperature (i.e., $M_{\rm CZ} \propto T_{\rm eff}^{-90}$), leading to the possibility that even low-amplitude pulsators may experience significant nonlinear effects. In particular, the outer turning point of finite-amplitude g-mode pulsations can vary with the local surface temperature, producing a reflected wave that is out of phase with what is required for a standing wave. This can lead to a lack of coherence of the mode and a reduction in its global amplitude. In this paper we show that: (1) whether a mode is calculated to propagate to the base of the convection zone is an accurate predictor of its width in the Fourier spectrum, (2) the phase shifts produced by reflection from the outer turning point are large enough to produce significant damping, and (3) amplitudes and periods are predicted to increase from the blue edge to the middle of the instability strip, and subsequently decrease as the red edge is approached. This amplitude decrease is in agreement with the observational data while the period decrease has not yet been systematically studied.

[19]  arXiv:2001.05077 [pdf, other]

Title: STARE2: Detecting Fast Radio Bursts in the Milky Way

Authors: Christopher D. Bochenek, Daniel L. McKenna, Konstantin V. Belov, Jonathon Kocz, Shri R. Kulkarni, James Lamb, Vikram Ravi, David Woody

Comments: 7 pages, 9 figures, accepted to PASP

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

There are several unexplored regions of the short-duration radio transient phase space. One such unexplored region is the luminosity gap between giant pulses (from pulsars) and cosmologically located fast radio bursts (FRBs). The Survey for Transient Astronomical Radio Emission 2 (STARE2) is a search for such transients out to 7 Mpc. STARE2 has a field of view of 3.6 steradians and is sensitive to one-millisecond transients above $\sim300$ kJy. With a two-station system we have detected and localized a solar burst, demonstrating that the pilot system is capable of detecting short duration radio transients. We found no convincing transients with duration between 65 $\mu$s and 34 ms in 200 days of observing, limiting with 95% confidence the all-sky rate of transients above $\sim300$ kJy to $< 40$ ${\rm sky^{-1} year^{-1}}$. If the luminosity function of FRBs could be extrapolated down to 300 kJy for a distance of 10 kpc, then one would expect the rate to be $\sim2$ ${\rm sky^{-1} year^{-1}}$.

[20]  arXiv:2001.05081 [pdf, other]

Title: Inner-Heliosphere Signatures of Ion-Scale Dissipation and Nonlinear Interaction

Authors: Trevor A. Bowen, Alfred Mallet, Stuart D. Bale, J. W. Bonnell, Anthony W. Case, Benjamin D. G. Chandran, Alexandros Chasapis, Christopher H. K. Chen, Die Duan, Thierry Dudok de Wit, Keith Goetz, Jasper Halekas, Peter R. Harvey, J. C. Kasper, Kelly E. Korreck, Davin Larson, Roberto Livi, Robert J. MacDowall, David M. Malaspina, Marc Pulupa, Michael Stevens, Phyllis Whittlesey

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

We perform a statistical study of the turbulent power spectrum at inertial and kinetic scales observed during the first perihelion encounter of Parker Solar Probe. We find that often there is an extremely steep scaling range of the power spectrum just above the ion-kinetic scales, similar to prior observations at 1 AU, with a power-law index of around $-4$. Based on our measurements, we demonstrate that either a significant ($>50\%$) fraction of the total turbulent energy flux is dissipated in this range of scales, or the characteristic nonlinear interaction time of the turbulence decreases dramatically from the expectation based solely on the dispersive nature of nonlinearly interacting kinetic Alfv\'en waves.

[21]  arXiv:2001.05092 [pdf, ps, other]

Title: Constraints on a special running vacuum model

Authors: Chao-Qiang Geng, Chung-Chi Lee, Lu Yin

Comments: 16 pages, 6 figures, accepted for publication in EPJC

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

We study a special running vacuum model (RVM) with $\Lambda = 3 \alpha H^2+3\beta H_0^4 H^{-2}+\Lambda_0$, where $\alpha$, $\beta$ and $\Lambda_0$ are the model parameters and $H$ is the Hubble one. This RVM has non-analytic background solutions for the energy densities of matter and radiation, which can only be evaluated numerically. From the analysis of the CMB power spectrum and baryon acoustic oscillation along with the prior of $\alpha>0$ to avoid having a negative dark energy density, we find that $\alpha<2.83\times 10^{-4}$ and $\beta=(-0.2^{+3.9}_{-4.5})\times 10^{-4}$ (95$\%$ C.L.). We show that the RVM fits the cosmological data comparably to the $\Lambda$CDM. In addition, we relate the fluctuation amplitude $\sigma_8$ to the neutrino mass sum $\Sigma m_\nu$.

[22]  arXiv:2001.05103 [pdf, other]

Title: Generalised Emergent Dark Energy Model: Confronting $Λ$ and PEDE

Authors: Xiaolei Li, Arman Shafieloo

Comments: 8 pages, 4 figures, Comments welcome

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

We introduce a generalised form of an emergent dark energy model with one degree of freedom for the dark energy sector that has the flexibility to include both $\Lambda$CDM as well as the PEDE model (Phenomenologically Emergent Dark Energy) proposed by Li & Shafieloo (2019) as two of its special limits. This allows us to compare statistically these models in a straightforward way and following conventional Bayesian approach. The free parameter for the dark energy sector, namely $\Delta$, has the value of $0$ for the case of the $\Lambda$ and $1$ for the case of PEDE and its posterior fitting the generalised parametric form to different data can directly show the consistency of the models to the data. Fitting the introduced parametric form to Planck CMB data and most recent $H_0$ results from local observations of Cepheids and Supernovae (Riess et al. 2019), we show that the $\Delta=0$ associated with the $\Lambda$CDM model would fall out of 4$\sigma$ confidence limits of the derived posterior of the $\Delta$ parameter. In contrast, PEDE model can satisfy the combination of the observations. This is another support for the case of PEDE model with respect to the standard $\Lambda$CDM model if we trust the reliability of both Planck CMB data and local $H_0$ observations.

[23]  arXiv:2001.05151 [pdf, other]

Title: DESHIMA on ASTE: On-sky Responsivity Calibration of the Integrated Superconducting Spectrometer

Authors: Tatsuya Takekoshi, Kenichi Karatsu, Junya Suzuki, Yoichi Tamura, Tai Oshima, Akio Taniguchi, Shin'ichiro Asayama, Tom J. L. C. Bakx, Jochem J. A. Baselmans, Sjoerd Bosma, Juan Bueno, Kah Wuy Chin, Yasunori Fujii, Kazuyuki Fujita, Robert Huiting, Soh Ikarashi, Tsuyoshi Ishida, Shun Ishii, Ryohei Kawabe, Teun M. Klapwijk, Kotaro Kohno, Akira Kouchi, Nuria Llombart, Jun Maekawa, Vignesh Murugesan, Shunichi Nakatsubo, Masato Naruse, Kazushige Ohtawara, Alejandro Pascual Laguna, Koyo Suzuki, David J. Thoen, Takashi Tsukagoshi, Tetsutaro Ueda, Pieter J. de Visser, Paul P. van der Werf, Stephen J. C. Yates, Yuki Yoshimura, Ozan Yurduseven, Akira Endo

Comments: Accepted for publication in the Journal of Low Temperature Physics for LTD-18 special issue

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

We are developing an ultra-wideband spectroscopic instrument, DESHIMA (DEep Spectroscopic HIgh-redshift MApper), based on the technologies of an on-chip filter-bank and Microwave Kinetic Inductance Detector (MKID) to investigate dusty star-burst galaxies in the distant universe at millimeter and submillimeter wavelength. An on-site experiment of DESHIMA was performed using the ASTE 10-m telescope. We established a responsivity model that converts frequency responses of the MKIDs to line-of-sight brightness temperature. We estimated two parameters of the responsivity model using a set of skydip data taken under various precipitable water vapor (PWV, 0.4-3.0 mm) conditions for each MKID. The line-of-sight brightness temperature of sky is estimated using an atmospheric transmission model and the PWVs. As a result, we obtain an average temperature calibration uncertainty of $1\sigma=4$%, which is smaller than other photometric biases. In addition, the average forward efficiency of 0.88 in our responsivity model is consistent with the value expected from the geometrical support structure of the telescope. We also estimate line-of-sight PWVs of each skydip observation using the frequency response of MKIDs, and confirm the consistency with PWVs reported by the Atacama Large Millimeter/submillimeter Array.

[24]  arXiv:2001.05154 [pdf, other]

Title: Generation of Solenoidal Modes and Magnetic Fields in Turbulence Driven by Compressive Driving

Authors: Jeonghoon Lim, Jungyeon Cho, Heesun Yoon

Comments: 20 pages, 23 figures, 1 table

Subjects: Astrophysics of Galaxies (astro-ph.GA); Cosmology and Nongalactic Astrophysics (astro-ph.CO); Solar and Stellar Astrophysics (astro-ph.SR); Fluid Dynamics (physics.flu-dyn)

We perform numerical simulations of hydrodynamic (HD) and magnetohydrodynamic (MHD) turbulence driven by compressive driving to study generation of solenoidal velocity component and small-scale magnetic field. We mainly focus on the effects of mean magnetic field ($B_0$) and the sonic Mach number ($M_s$). We also consider two different driving schemes in terms of correlation timescale of forcing vectors: a finite-correlated driving and a delta-correlated driving. The former has a longer correlation timescale of forcing vectors, which is comparable to large-eddy turnover time, than the latter. Our findings are as follows. First, when we fix the value of $B_0$, the level of solenoidal velocity component after saturation increases as $M_s$ increases. A similar trend is observed for generation of magnetic field when $B_0$ is small. Second, when we fix the value of $M_s$, HD and MHD simulations result in similar level of the solenoidal component when $B_0$ $\lesssim$ 0.2 (or Alfven Mach number of $\sim$ 5). However, the level increases when $B_0$ $\gtrsim$ 0.2. Roughly speaking, the magnetic energy density after saturation is a linearly increasing function of $B_0$ irrespective of $M_s$. Third, generation of solenoidal velocity component is not sensitive to numerical resolution, but that of magnetic energy density is mildly sensitive. Lastly, when initial conditions are same, the finite-correlated driving always produces more solenoidal velocity and small-scale magnetic field components than the delta-correlated driving. We additionally analyze the vorticity equation to understand why higher $M_s$ and $B_0$ yield larger quantity of the solenoidal velocity component.

[25]  arXiv:2001.05156 [pdf, ps, other]

Title: Decay of Turbulence in Fluids with Polytropic Equations of State

Authors: Jeonghoon Lim, Jungyeon Cho

Comments: 9 pages, 9 figures, 1 table

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

We present numerical simulations of decaying hydrodynamic turbulence initially driven by solenoidal (divergence-free) and compressive (curl-free) driving. Most previous numerical studies for decaying turbulence assume an isothermal equation of state (EOS). Here we use a polytropic EOS, $P$ $\propto$ $\rho^{\gamma}$, with polytropic $\gamma$ ranging from 0.7 to 5/3. We mainly aim at determining the effects of polytropic $\gamma$ and driving schemes on the decay law of turbulence energy, E $\propto$ $t^{-\alpha}$. We additionally study probability density function (PDF) of gas density and skewness of the distribution in polytropic turbulence driven by compressive driving. Our findings are as follows. First of all, we find that even if polytropic $\gamma$ does not strongly change scaling relation of the decay law, the driving schemes weakly change the relation; in our all simulations, turbulence decays with $\alpha$ $\approx$ 1, but compressive driving yields smaller $\alpha$ than solenoidal driving at the same sonic Mach number. Second, we calculate compressive and solenoidal velocity components separately and compare their decay rates in turbulence initially driven by compressive driving. We find that the former decays much faster so that it ends up having a smaller fraction than the latter. Third, the density PDF of compressively driven turbulence with polytropic $\gamma$ $>$ 1 deviates from log-normal distribution: it has a power-law tail at low density as in the case of solenoidally driven turbulence. However, as it decays, the density PDF becomes approximately log-normal. We discuss why decay rates of compressive and solenoidal velocity components are different in compressively driven turbulence and astrophysical implication of our findings.

[26]  arXiv:2001.05183 [pdf, other]

Title: On the possibility of Baryon Acoustic Oscillation measurements at redshift $z>7.6$ with WFIRST

Authors: Siddharth Satpathy, Zhaozhou An, Rupert A. C. Croft, Tiziana Di Matteo, Ananth Tenneti, Yu Feng, Katrin Heitmann, Graziano Rossi

Comments: 17 pages, 16 figures

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

The Wide Field Infrared Survey Telescope (WFIRST), with its field of view and high sensitivity will make surveys of cosmological large-scale structure possible at high redshifts. We investigate the possibility of detecting Baryon Acoustic Oscillations (BAO) at redshifts $z>7.6$ for use as a standard ruler. We use data from the hydrodynamic simulation \textsc{BlueTides} in conjunction with the gigaparsec-scale Outer Rim simulation and a model for patchy reionization to create mock WFIRST High Latitude Survey grism data for \lya\ emission line selected galaxies at redshifts $z=7.4$ to $z=10$, covering 2280 square degrees. We measure the monopoles of galaxies in the mock catalogues and fit the BAO features. We find that for a line flux of $L = 7\times 10^{-17} \ {\rm erg/s/cm}^{2}$, the $5 \sigma$ detection limit for the current design, the BAO feature is partially detectable (measured in three out of four survey quadrants analysed independently). The resulting root mean square error on the angular diameter distance to $z=7.7$ is 7.9$\%$. If we improve the detection sensitivity by a factor of two (i.e. $L = 3.5\times 10^{-17} \ {\rm erg/s/cm}^{2}$), the distance error reduces to $1.4\%$. We caution that many more factors are yet to be modelled, including dust obscuration, the damping wing due to the intergalactic medium, and low redshift interlopers. If these issues do not strongly affect the results, or different observational techniques (such as use of multiple lines) can mitigate them, WFIRST or similar instruments may be able to constrain the angular diameter distance to the high redshift Universe.

[27]  arXiv:2001.05190 [pdf, other]

Title: Corona-Australis DANCe. I. Revisiting the census of stars with Gaia-DR2 data

Authors: P.A.B. Galli, H. Bouy, J. Olivares, N. Miret-Roig, L.M. Sarro, D. Barrado, A. Berihuete, W. Brandner

Comments: 17 pages, 11 figures, online data. Abridged abstract. Accepted for publication in A&A (in press)

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

Corona-Australis is one of the nearest regions to the Sun with recent and ongoing star formation, but the current picture of its stellar (and substellar) content is not complete yet. We take advantage of the second data release of the Gaia space mission to revisit the stellar census and search for additional members of the young stellar association in Corona-Australis. We applied a probabilistic method to infer membership probabilities based on a multidimensional astrometric and photometric data set over a field of 128 deg$^{2}$ around the dark clouds of the region. We identify 313 high-probability candidate members to the Corona-Australis association, 262 of which had never been reported as members before. Our sample of members covers the magnitude range between $G\gtrsim5$ mag and $G\lesssim20$ mag, and it reveals the existence of two kinematically and spatially distinct subgroups. There is a distributed `off-cloud' population of stars located in the north of the dark clouds that is twice as numerous as the historically known `on-cloud' population that is concentrated around the densest cores. By comparing the location of the stars in the HR-diagram with evolutionary models, we show that these two populations are younger than 10 Myr. Based on their infrared excess emission, we identify 28 Class II and 215 Class III stars among the sources with available infrared photometry, and we conclude that the frequency of Class II stars (i.e. `disc-bearing' stars) in the on-cloud region is twice as large as compared to the off-cloud population. The distance derived for the Corona-Australis region based on this updated census is $d=149.4^{+0.4}_{-0.4}$ pc, which exceeds previous estimates by about 20 pc.In this paper we provide the most complete census of stars in Corona-Australis available to date that can be confirmed with Gaia data.

[28]  arXiv:2001.05302 [pdf, other]

Title: Testing tidal alignment models for anisotropic correlations of halo ellipticities with N-body simulations

Authors: Teppei Okumura, Atsushi Taruya, Takahiro Nishimichi

Comments: 9 pages, 6 figures

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

There is a growing interest of using the intrinsic alignment (IA) of galaxy images as a tool to extract cosmological information complimentary to galaxy clustering analysis. Recently, Okumura & Taruya derived useful formulas for the intrinsic ellipticity--ellipticity correlation, the gravitational shear--intrinsic ellipticity correlation, and the velocity--intrinsic ellipticity correlation functions based on the linear alignment (LA) model. In this paper, using large-volume $N$-body simulations, we measure these alignment statistics in real and redshift space and compare them to the LA and nonlinear alignment model predictions. We find that anisotropic features of baryon acoustic oscillations in the IA statistics can be accurately predicted by our models. The anisotropy due to redshift-space distortions (RSDs) is also well described in the large-scale limit. Our results indicate that one can extract the cosmological information encoded in the IA through the Alcock-Paczynski and RSD effects.

[29]  arXiv:2001.05355 [pdf, ps, other]

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

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

Comments: 7 pages, 1 table, and 4 figures, accepted for publication in ApJ

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

The observed internal plateau of X-ray emission in some short GRBs suggests the formation of a remnant supra-massive magnetar following a double neutron star (NS) merger. In this paper, we assume that the rotational energy is lost mainly via gravitational-wave (GW) radiation instead of magnetic dipole (MD) radiation, and present further constraints on the NS nuclear equation of state (EoS) via mass quadrupole deformation and r-mode fluid oscillations of the magnetar. We present two short GRBs with measured redshifts, 101219A and 160821B, whose X-ray light curves exhibit an internal plateau. This suggests that a supra-massive NS may survive as the central engine. By considering twelve NS EoSs, within the mass quadrupole deformation scenario we find that the GM1, DD2, and DDME2 models give an $M_{\rm p}$ band falling within the 2$\sigma$ region of the proto-magnetar mass distribution for $\varepsilon=0.01$. This is consistent with the constraints from the MD radiation dominated model of rotational energy loss. However, for an r-mode fluid oscillation model with $\alpha=0.1$ the data suggest that the NS EOS is close to the Shen and APR models, which is obviously different from the MD radiation dominated and mass quadrupole deformation cases.

[30]  arXiv:2001.05392 [pdf, ps, other]

Title: Gravitational radiation by magnetic field: application to millisecond magnetars

Authors: Elham Nazari, Mahmood Roshan

Comments: 3 figures, Comments welcome!

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

We investigate the direct effect of magnetic fields on gravitational waves. To do so, we study the post-Newtonian energy-momentum tensor of the magnetized fluid and the post-Newtonian expansion of the gravitational potential in the wave zone. We show that the magnetic field appears even in the first post-Newtonian order of the multipole moment tensor. Then, we derive an explicit relativistic correction containing the magnetic field contribution to the well-known quadrupole formula. As an application of this derivation, we explicitly prove that the magnetic field of millisecond magnetars can be a promising source of the gravitational waves. We show that this type of gravitational wave is strong enough to be detected by the next generation of the detectors.

[31]  arXiv:2001.05393 [pdf, other]

Title: Forecast for cosmological parameter estimation with gravitational-wave standard siren observation from the Cosmic Explorer

Authors: Shang-Jie Jin, Dong-Ze He, Yidong Xu, Jing-Fei Zhang, Xin Zhang

Comments: 13 pages, 4 figures

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

The third-generation ground-based gravitational-wave (GW) detector, Cosmic Explorer (CE), is scheduled to start its observation in the 2030s. In this paper, we make a forecast for cosmological parameter estimation with gravitational-wave standard siren observation from the CE. We use the simulated GW standard siren data of CE to constrain the $\Lambda$CDM, $w$CDM and CPL models. We combine the simulated GW data with the current cosmological electromagnetic observations including the latest cosmic microwave background (CMB) anisotropies data from Planck, the optical baryon acoustic oscillation (BAO) measurements, and the type Ia supernovae (SN) observation (Pantheon compilation) to do the analysis. We find that the future standard siren observation from CE will improve the cosmological parameter estimation to a great extent, since the future GW standard siren data can well break the degeneracies generated by the optical observations between various cosmological parameters. We also find that the CE's constraining capability on the cosmological parameters is slightly better than that of the same-type GW detector, the Einstein Telescope (ET). In addition, the synergy between the GW standard siren observation from CE and the 21 cm emission observation from SKA is also discussed.

[32]  arXiv:2001.05405 [pdf]

Title: Heterogeneous accretion of Earth inferred from Mo-Ru isotope systematics

Authors: Timo Hopp, Gerrit Budde, Thorsten Kleine

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

The Mo and Ru isotopic compositions of meteorites and the bulk silicate Earth (BSE) hold important clues about the provenance of Earth's building material. Prior studies have argued that non-carbonaceous (NC) and carbonaceous (CC) meteorite groups together define a Mo-Ru 'cosmic' correlation, and that the BSE plots on the extension of this correlation. These observations were taken as evidence that the final 10-15% of Earth's accreted material derived from a homogeneous inner disk reservoir with an enstatite chondrite-like isotopic composition. Here, using new Mo and Ru isotopic data for previously uninvestigated meteorite groups, we show that the Mo-Ru correlation only exists for NC meteorites, and that both the BSE and CC meteorites fall off this Mo-Ru correlation. These observations indicate that the final stages of Earth's accretion were heterogeneous and consisted of a mixture of NC and CC materials. The Mo-Ru isotope systematics are best accounted for by either an NC heritage of the late veneer combined with a CC heritage of the Moon-forming giant impactor, or by mixed NC-CC compositions for both components. The involvement of CC bodies in the late-stage accretionary assemblage of Earth is consistent with chemical models for core-mantle differentiation, which argue for the addition of more oxidized and volatile-rich material toward the end of Earth's formation. As such, this study resolves the inconsistencies between homogeneous accretion models based on prior interpretations of the Mo-Ru systematics of meteorites and the chemical evidence for heterogeneous accretion of Earth.

[33]  arXiv:2001.05433 [pdf, ps, other]

Title: Cyclic variations in the main components of the solar large-scale magnetic field

Authors: V. N. Obridko (1), D. D. Sokoloff (1 and 2), B. D. Shelting (1), A. S. Shibalova (1 and 2), I. M. Livshits (1 and 3) ((1) IZMIRAN, Troitsk, Moscow, Russia, (2) Department of Physics, Moscow State University, Moscow, Russia, (3) Sternberg State Astronomical Institute, Lomonosov Moscow State University, Moscow, Russia)

Comments: 10 pages, 14 figures. Accepted to Monthly Notices of the Royal Astronomical Society

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

We considered variations the dipole and the quadrupole components of the solar large-scale magnetic field. Both the axial and the equatorial dipoles exhibit a systematic decrease in the past four cycles in accordance with the general decrease of solar activity. The transition of the pole of a dipole from the polar region to mid latitudes occurs rather quickly, so that the longitude of the pole changes little. With time, however, this inclined dipole region shifts to larger longitudes, which suggests an acceleration of the dipole rotation. The mean rotation rate exceeds the Carrington velocity by 0.6%. The behavior of the quadrupole differs dramatically. Its decrease over last four cycles was much smaller than that of the dipole moment. The ratio of the quadrupole and dipole moments has increased for four cycles more than twice in contrast to the sunspot numbers, which displayed a twofold decrease for the same time interval. What about quadrupole rotation, the mean longitude of the poles of one sign decreased by 600 degrees over four cycles, which suggests that the mean rotation rate was lower than the Carrington velocity by 0.28%. We do not see however any conclusive evidence that, in the period under discussion, a mode of quadrupole symmetry was excited on the Sun along with the dipole mode.

[34]  arXiv:2001.05436 [pdf, other]

Title: Limits on the Electromagnetic Counterpart to S190814bv

Authors: Alan M. Watson, Nathaniel R. Butler, William H. Lee, Rosa L. Becerra, Margarita Pereyra, Fernando Angeles, Alejandro Farah, Liliana Figueroa, Diego González-Buitrago, Fernando Quirós, Jaime Ruíz-Díaz-Soto, Carlos Tejada de Vergas, Silvio J. Tinoco, Tanner Wolfram

Comments: Accepted by MNRAS. 6 pages

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

We derive limits on any electromagnetic counterpart to the compact binary merger S190814bv, whose parameters are consistent with the merger of a black hole and a neutron star. We present observations with the new wide-field optical imager DDOTI and also consider Swift/BAT observations reported by Palmer et al. (2019). We show that Swift/BAT would have detected a counterpart with similar properties to a typical on-axis short GRB at the 98 per cent confidence level, whereas our DDOTI observations only rule out such a counterpart at the 27 per cent confidence level. Neither have sufficient sensitivity to rule out an off-axis counterpart like GW 170817. We compare the efficiency of Swift/BAT and DDOTI for future observations, and show that DDOTI is likely to be about twice as efficient as Swift/BAT for off-axis events up to about 100 Mpc.

[35]  arXiv:2001.05455 [pdf, other]

Title: Gaia-DR2 extended kinematical maps. Part II: Dynamics in the Galactic disk explaining radial and vertical velocities

Authors: M. Lopez-Corredoira, F. Garzon, H.-F. Wang, F. Sylos Labini, R. Nagy, Z. Chrobakova, J. Chang, B. Villarroel

Comments: 15 pages, 14 figures, accepted to be published in A&A

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

Context: In our Paper I, by using statistical deconvolution methods, extended kinematics maps of Gaia-DR2 data have been produced in a range of heliocentric distances that are a factor of two to three larger than those analyzed previously by the Gaia Collaboration with the same data. It added the range of Galactocentric distances between 13 kpc and 20 kpc to the previous maps.
Aims: Here, we investigate the dynamical effects produced by different mechanisms that can explain the radial and vertical components of these extended kinematic maps, including a decomposition of bending and breathing of the vertical components. This paper as a whole tries to be a compendium of different dynamical mechanisms whose predictions can be compared to the kinematic maps.
Methods: Using analytical methods or simulations, we are able to predict the main dynamical factors and compare them to the predictions of the extended kinematic maps of Gaia-DR2.
Results: The gravitational influence of Galactic components that are different from the disk, such as the long bar or bulge, the spiral arms, or a tidal interaction with Sagittarius dwarf galaxy, may explain some features of the velocity maps, especially in the inner parts of the disk. However, they are not sufficient in explaining the most conspicuous gradients in the outer disk. Vertical motions might be dominated by external perturbations or mergers, although a minor component may be due to a warp whose amplitude evolves with time. Here, we show with two different methods, which analyze the dispersion of velocities, that the mass distribution of the disk is flared. Despite these partial explanations, the main observed features can only be explained in terms of out-of-equilibrium models, which are either due to external perturbers or to the fact that the disk has not had time to reach equilibrium since its formation.

[36]  arXiv:2001.05456 [pdf, other]

Title: Star-disk alignment in the protoplanetary disks: SPH simulation of the collapse of turbulent molecular cloud cores

Authors: Daisuke Takaishi, Yusuke Tsukamoto, Yasushi Suto

Comments: Accepted for publication in MNRAS (16 pages, 16 figures, 2 tables)

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

We perform a series of three-dimensional smoothed particle hydrodynamics (SPH) simulations to study the evolution of the angle between the protostellar spin and the protoplanetary disk rotation axes (the star-disk angle $\psi_{\rm sd}$) in turbulent molecular cloud cores. While $\psi_{\rm sd}$ at the protostar formation epoch exhibits broad distribution up to $\sim 130^{\circ}$, $\psi_{\rm sd}$ decreases ($\lesssim 20^{\circ}$) in a timescale of $\sim 10^{4}$ yr. This timescale of the star-disk alignment, $t_{\rm alignment}$, corresponds basically to the mass doubling time of the central protostar, in which the protostar forgets its initial spin direction due to the mass accretion from the disk. Values of $\psi_{\rm sd}$ both at $t=10^2$ yr and $t=10^5$ yr after the protostar formation are independent of the ratios of thermal and turbulent energies to gravitational energy of the initial cloud cores: $\alpha=E_{\rm thermal}/|E_{\rm gravity}|$ and $\gamma_{\rm turb}=E_{\rm turbulence}/|E_{\rm gravity}|$. We also find that a warped disk is possibly formed by the turbulent accretion flow from the circumstellar envelope.

[37]  arXiv:2001.05465 [pdf, ps, other]

Title: Evolution of Stokes V area asymmetry related to a quiet Sun cancelation observed with GRIS/IFU

Authors: Anjali. J. Kaithakkal, J. M. Borrero, C. E. Fischer, C. Dominguez-Tagle, M. Collados

Comments: 8 pages, 9 figures, accepted for publication in A&A

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

A quiet Sun magnetic flux cancelation event at the disk centre was recorded using the Integral Field Unit (IFU) mounted on the GREGOR Infrared Spectrograph (GRIS). GRIS sampled the event in the photospheric Si I 10827 {\AA} spectral line. The cancelation is preceded by a significant rise in line core intensity and excitation temperature, which is inferred from Stokes inversions under local thermodynamic equilibrium (LTE). The opposite polarity features seem to undergo reconnection above the photosphere. We also found that the border pixels neighboring the polarity inversion line of one of the polarities exhibit a systematic variation of area asymmetry. Area asymmetry peaks right after the line core intensity enhancement and gradually declines thereafter. Analyzing Stokes profiles recorded from either side of the polarity inversion line could therefore potentially provide additional information on the reconnection process related to magnetic flux cancelation. Further analysis without assuming LTE will be required to fully characterize this event.

[38]  arXiv:2001.05469 [pdf, other]

Title: Cosmological constraints on dark energy in light of gravitational wave bounds

Authors: Johannes Noller

Comments: 16 pages, 4 figures, 1 table

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

Gravitational wave (GW) constraints have recently been used to significantly restrict models of dark energy and modified gravity. New bounds arising from GW decay and GW-induced dark energy instabilities are particularly powerful in this context, complementing bounds from the observed speed of GWs. We discuss the associated linear cosmology for Horndeski gravity models surviving these combined bounds and compute the corresponding cosmological parameter constraints, using CMB, redshift space distortion, matter power spectrum and BAO measurements from the Planck, SDSS/BOSS and 6dF surveys. The surviving theories are strongly constrained, tightening previous bounds on cosmological deviations from $\Lambda{}$CDM by over an order of magnitude. We also comment on general cosmological stability constraints and the nature of screening for the surviving theories, pointing out that a raised strong coupling scale can ensure compatibility with gravitational wave constraints, while maintaining a functional Vainshtein screening mechanism on solar system scales. Finally, we discuss the quasi-static limit as well as (constraints on) related observables for near-future surveys.

[39]  arXiv:2001.05473 [pdf, other]

Title: Metal enrichment in the circumgalactic medium and Lyα haloes around quasars at z $\sim$3

Authors: Yucheng Guo (KIAA-PKU, KICC-Cambrige), Roberto Maiolino (KICC-Cambridge), Linhua Jiang (KIAA-PKU), Kenta Matsuoka, Tohru Nagao, Oli Luiz Dors Junior, Michele Ginolfi, Nick Henden, Jake Bennett, Debora Sijacki, Ewald Puchwein

Comments: 24 pages, 17 figures, submitted to the AAS journals

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

Deep observations have detected extended Ly{\alpha} emission nebulae surrounding tens of QSOs at redshift 2 to 6. However, the metallicity of such extended haloes is still poorly understood. We perform a detailed analysis on a large sample of 80 quasars at z$\sim$3 based on MUSE-VLT data. We find clear evidence of extended emission of the UV nebular lines C IV {\lambda}1549 and He II {\lambda}1640 for about 18$\%$ of the sample, while C III] {\lambda}1909 is only marginally detected in a few objects. By stacking the cubes we detect emission of C IV, He II and C III] out to a radius of about 45 kpc. C IV and He II show a radial decline much steeper than Ly{\alpha}, while C III] shows a shallower profile similar to Ly{\alpha} in the inner 45 kpc. We infer that the average metallicity of the circumgalactic gas within the central 30-50 kpc is $\sim$0.5 solar, or even higher. However, we also find evidence of a component of the Ly{\alpha} haloes, which has much weaker metal emission lines relative to Ly{\alpha}. We suggest that the high metallicity of the circumgalactic medium within the central 30-50 kpc is associated with chemical pre-enrichment by past quasar-driven outflows and that there is a more extended component of the CGM that has much lower metallicity and likely associated with near-pristine gas accreted from the intergalactic medium. We show that our observational results are in good quantitative agreement with the expectations of the FABLE cosmological simulations.

[40]  arXiv:2001.05487 [pdf, other]

Title: SOFIA/FORCAST Galactic Center Legacy Survey: Overview

Authors: Matthew J. Hankins, Ryan M. Lau, James T. Radomski, Angela S. Cotera, Mark R. Morris, Elisabeth A. C. Mills, Daniel L. Walker, Ashley T. Barnes, Janet P. Simpson, Terry L. Herter, Steven N. Longmore, John Bally, Mansi M. Kasliwal, Nadeen B. Sabha, Macarena Garcia-Marin

Comments: 20 pages, 11 figures, Submitted to ApJ

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

The Galactic Center contains some of the most extreme conditions for star formation in our Galaxy as well as many other phenomena that are unique to this region. Given our relative proximity to the Galactic Center, we are able to study details of physical processes to a level that is simply not yet possible for more distant galaxies, yielding an otherwise inaccessible view of the nuclear region of a galaxy. We recently carried out a targeted imaging survey of mid-infrared bright portions of the Galactic Center at 25 and 37 $\mu$m using the FORCAST instrument on SOFIA. This survey was one of the inaugural Legacy Programs from SOFIA cycle 7, observing a total area of 403 arcmin$^2$ (2180 pc$^2$), including the Sgr A, B, and C complexes. Here we present an overview of the survey strategy, observations, and data reduction as an accompaniment to the initial public release of the survey data. We discuss interesting regions and features within the data including extended features near the circumnuclear disk, structures in the Arched Filaments and Sickle H II regions, and signs of embedded star formation in Sgr B2 and Sgr C. We also feature a handful of less well studied mid-infrared sources located between Sgr A and Sgr C that could be sites of relatively isolated star formation activity. Last, we discuss plans for subsequent publications and future data releases from the survey.

Cross-lists for Thu, 16 Jan 20

[41]  arXiv:2001.04795 (cross-list from gr-qc) [pdf, ps, other]

Title: Predictive Physics of Inflation and Grand Unification for and from the CMB observations

Authors: Norma G. Sanchez (CNRS, LERMA PSL University Observatoire de Paris, Sorbonne University)

Comments: White Paper presented at the CNRS IN2P3 Prospectives 2020, GT05 Steering Group {\guillemotleft} Physics of Inflation and Dark Energy {\guillemotright}, and the GT05 IN2P3 Topical Meeting held on 9-10 December 2019 in Grenoble, France. 12 pages, no figures

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

This White Paper for the CNRS IN2P3 Prospective 2020 focuses on realistic and timely situations of inflation in connection with the CMB, gravitational and particle physics, adding inter-disciplinarity and unification values within a strongly predictive physical approach. The formulation of inflation in the Ginsburg-Landau approach developed by de Vega and Sanchez [1] and by Boyanovsky, de Vega, Sanchez and Destri [2]-[4] clarifies and places inflation in the setting of the effective field theories of particle physics. In addition, it sets up a clean way to directly confront the inflationary predictions with the available and forthcoming CMB data and select a definitive model. All CMB + LSS data until now show how powerful is the Ginsburg-Landau effective theory of inflation in predicting observables in agreement with observations including the inflation energy scale and the inflaton potential, and which has much more to provide in the future. It paves the way to discoveries, new learning and understanding.

[42]  arXiv:2001.04978 (cross-list from gr-qc) [pdf, other]

Title: Scale-Invariant Dynamics of Galaxies, MOND, Dark Matter, and the Dwarf Spheroidals

Authors: Andre Maeder, Vesselin G. Gueorguiev

Comments: 12 pages, 3 figures

Subjects: General Relativity and Quantum Cosmology (gr-qc); Astrophysics of Galaxies (astro-ph.GA)

The Scale-Invariant Vacuum (SIV) theory is based on Weyl's Integrable Geometry, endowed with a gauge scalar field. The main difference between MOND and the SIV theory is that the first considers a global dilatation invariance of space and time, where the scale factor $\lambda$ is a constant, while the second opens the likely possibility that $\lambda$ is a function of time. The key equations of the SIV framework are used here to study the relationship between the Newtonian gravitational acceleration due to baryonic matter $g_{\mathrm{bar}}$ and the observed kinematical acceleration $g_{\mathrm{obs}}$. The relationship is applied to galactic systems of the same age where the Radial Acceleration Relation (RAR), between the $g_{\mathrm{obs}}$ and $g_{\mathrm{bar}}$ accelerations, can be compared with observational data. The SIV theory shows an excellent agreement with observations and with MOND for baryonic gravities $g_{\mathrm{bar}}>10^{-11.5}$ m s$^{-2}$. Below this value, SIV still fully agrees with the observations, as well as with the horizontal asymptote of the RAR for dwarf spheroidals, while this is not the case for MOND. These results support the view that there is no need for dark matter and that the RAR and related dynamical properties of galaxies can be interpreted by a modification of gravitation.

[43]  arXiv:2001.05125 (cross-list from physics.plasm-ph) [pdf, ps, other]

Title: On the temperature of the solar wind

Authors: Stanislav Boldyrev, Cary Forest, Jan Egedal

Comments: 9 pages, 3 figures

Subjects: Plasma Physics (physics.plasm-ph); Astrophysics of Galaxies (astro-ph.GA)

Solar wind provides an example of a weakly collisional plasma expanding from a thermal source in the presence of spatially diverging magnetic field lines. Observations show that in the inner heliosphere, the electron temperature declines with the distance approximately as $T_{e}(r)\sim r^{-0.3} \dots r^{-0.7}$, which is significantly slower than the adiabatic expansion law $ \sim r^{-4/3}$. Motivated by such observations, we propose a kinetic theory that addresses the non-adiabatic evolution of a nearly collisionless plasma expanding from a central thermal source. We concentrate on the dynamics of energetic electrons propagating along a radially diverging magnetic flux tube. Due to the conservation of their magnetic moments, the electrons form a beam collimated along the magnetic field lines. Due to weak energy exchange with the background plasma, the beam population slowly loses its energy and heats the background plasma. We propose that no matter how weak the collisions are, at large enough distances from the source a universal regime of expansion is established where the electron temperature declines as $T_e(r)\propto r^{-2/5}$. This is close to the observed scaling of the solar wind temperature in the inner heliosphere. Our first-principle kinetic derivation may thus provide an explanation for the slower-than-adiabatic temperature decline in the solar wind. More broadly, it may be useful for describing magnetized winds from G-type stars.

[44]  arXiv:2001.05225 (cross-list from physics.optics) [pdf]

Title: C-RED 3: A SWIR camera for FSO applications

Authors: J.L. Gach, David Boutolleau, Cecile Brun, Thomas Carmignani, Fabien Clop, Philippe Feautrier, Stephane Lemarchand, Eric Stadler, Yann Wanwanscappel

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

Free space communications (FSO) is interesting for distant applications where high bandwidth is needed while using a fiber is not possible. However these links have to face several issues, and the most important one is the beam scintillation due to the propagation through a turbulent media, the atmosphere. Several mitigation strategies have been developed, but the best way to suppress scintillation is to use adaptive optics, widely used now in astronomy. The main difficulty for FSO is to probe the wavefront fast enough to have a good turbulence correction. This was not possible due to the lack of wavefront sensors working in the SWIR. C-RED 3 is a 640x512 SWIR camera running at 600FPS full frame and has the legacy of all the developments of astronomical infrared fast wavefront sensors on top of specific features for FSO (Low SWaP, Low Cost). We will present the performances of this new camera and demonstrate how it fulfills the needs of FSO adaptive optics.

[45]  arXiv:2001.05327 (cross-list from hep-ph) [pdf, ps, other]

Title: Precision calculation of the axion-nucleon coupling in chiral perturbation theory

Authors: Thomas Vonk, Feng-Kun Guo, Ulf-G. Meißner

Comments: 20 pages

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

We derive the axion-nucleon interaction Lagrangian in heavy baryon chiral perturbation theory up to next-to-next-to-leading order. The effective axion-nucleon coupling is calculated to a few percent accuracy.

[46]  arXiv:2001.05359 (cross-list from physics.atom-ph) [pdf, ps, other]

Title: Comment on "Energy levels, oscillator strengths, and transition probabilities for sulfur-like scandium, Sc~VI" by El-Maaref et al.\, [Indian J. Phys. {\bf 91} 1029 (2017)]

Authors: K M Aggarwal

Comments: This Comment of 7 pages will appear in the 2020 issue of Indian Journal of Physics

Subjects: Atomic Physics (physics.atom-ph); Solar and Stellar Astrophysics (astro-ph.SR)

In this comment, through our independent calculations, we assess that the recently reported results of El-Maaref et al. [{\em Indian J. Phys.} {\bf 91} 1029 (2017)] for energy levels, oscillator strengths, radiative rates, and lifetimes are inaccurate and unreliable for several levels and transitions of S-like Sc~VI.

Replacements for Thu, 16 Jan 20

[47]  arXiv:1807.10034 (replaced) [pdf, other]

Title: Is it Mixed dark matter or neutrino masses?

Authors: Julia Stadler, Celine Bœhm, Olga Mena

Comments: 10 pages, 7 figures

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

[48]  arXiv:1810.05001 (replaced) [pdf, other]

Title: A Modified Dynamical Model of Cosmology I. Theory

Authors: Hossein Shenavar, Kurosh Javidan

Comments: The model is discussed in more details. Data analysis of the model will be presented in future. Includes 48 pages and 9 figures

Journal-ref: Universe 2020, 6(1), 1

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

[49]  arXiv:1903.06717 (replaced) [pdf, other]

Title: A new method to constrain the origins of dark matter-free galaxies and their unusual globular clusters

Authors: Nathan Leigh, Giacomo Fragione

Comments: 10 pages, 5 figures, 2 table

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

[50]  arXiv:1903.07813 (replaced) [pdf, other]

Title: What GW170729's exceptional mass and spin tells us about its family tree

Authors: Chase Kimball, Christopher P L Berry, Vicky Kalogera

Comments: Results updated to match published version (conclusions unchanged); 3 pages, 1 figure

Journal-ref: RNASS; 4(1):2; 2020

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

[51]  arXiv:1904.03314 (replaced) [pdf, ps, other]

Title: Dissecting the Phase Space Snail Shell

Authors: Zhao-Yu Li, Juntai Shen (Shanghai Jiao Tong Univ. & Shanghai Astronomical Obs.)

Comments: Accepted for publication on ApJ. Compared to the previous version, the strategy of Vr-Vphi phase space dissection is further improved to be more quantitative and objective (as shown in Fig. 1). The main conclusions are not affected by this new strategy

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

[52]  arXiv:1904.09297 (replaced) [pdf, other]

Title: The mean gauges in bimetric relativity

Authors: Francesco Torsello

Comments: 16 pages plus appendices. It matches with the published version. The ancillary files include the colored version of the paper

Journal-ref: Classical and Quantum Gravity 36.23 (Nov. 2019), p. 235010

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

[53]  arXiv:1904.10464 (replaced) [pdf, ps, other]

Title: $\mathtt{bimEX}$: A Mathematica package for exact computations in $3+1$ bimetric relativity

Authors: Francesco Torsello

Comments: 9 pages. It matches with the published version. GitHub repository at this https URL Program files doi: this http URL

Journal-ref: Computer Physics Communications 247 (2020) 106948

Subjects: Symbolic Computation (cs.SC); Cosmology and Nongalactic Astrophysics (astro-ph.CO); Mathematical Software (cs.MS); General Relativity and Quantum Cosmology (gr-qc)

[54]  arXiv:1906.01112 (replaced) [pdf, other]

Title: Robustness of Gaian Feedbacks to Climate Perturbations

Authors: Olivia D. N. Alcabes, Stephanie Olson, Dorian S. Abbot

Comments: 6 pages, 6 figures; accepted for publication in MNRAS

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

[55]  arXiv:1907.07777 (replaced) [pdf, other]

Title: The Intrinsic Temperature and Radiative-Convective Boundary Depth in the Atmospheres of Hot Jupiters

Authors: Daniel P. Thorngren, Peter Gao, Jonathan J. Fortney

Comments: 6 pages, 4 figures, accepted to ApJ Letters. This version corrects the constants in equation 3; our calculations used the form in equation 2, so none of our other results are changed. An corresponding erratum has been submitted to ApJ Letters

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

[56]  arXiv:1909.07395 (replaced) [pdf, other]

Title: Cusp-to-core transition in low-mass dwarf galaxies induced by dynamical heating of cold dark matter by primordial black holes

Authors: Pierre Boldrini, Yohei Miki, Alexander Y. Wagner, Roya Mohayaee, Joseph Silk, Alexandre Arbey

Comments: 8 pages, 7 figures, Accepted by MNRAS

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

[57]  arXiv:1909.08791 (replaced) [pdf, other]

Title: Prospects for Life on Temperate Planets Around Brown Dwarfs

Authors: Manasvi Lingam, Idan Ginsburg, Abraham Loeb

Comments: Published in The Astrophysical Journal; 13 pages; 9 figures

Journal-ref: The Astrophysical Journal, Vol. 888, 102 (2020)

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

[58]  arXiv:1909.11271 (replaced) [pdf, ps, other]

Title: Neutrino decoherence in a fermion and scalar background

Authors: Jose F. Nieves, Sarira Sahu

Comments: 21 pages, 3 figures

Journal-ref: Phys. Rev. D 100, 115049 (2019)

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

[59]  arXiv:1909.11534 (replaced) [pdf, other]

Title: A search for pulsars in subdwarf B binary systems and discovery of giant-pulse emitting PSR J0533-4524

Authors: L. C. Oostrum, J. van Leeuwen, Y. Maan, T. Coenen, C.H. Ishwara-Chandra

Comments: 12 pages, 8 figures. Accepted for publication in MNRAS

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

[60]  arXiv:1910.03340 (replaced) [pdf, other]

Title: Ray tracing the integrated Sachs-Wolfe effect through the light cones of the Dark Energy Universe Simulation -- Full Universe Runs

Authors: Julian Adamek, Yann Rasera, Pier Stefano Corasaniti, Jean-Michel Alimi

Comments: 13 pages, 8 figures; v2: minor revision, matches accepted version

Journal-ref: Phys. Rev. D 101, 023512 (2020)

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

[61]  arXiv:1910.04535 (replaced) [pdf, ps, other]

Title: Spectral and temporal properties of Compton scattering by mildly relativistic thermal electrons

Authors: Andrzej A. Zdziarski, Michal Szanecki, Juri Poutanen, Marek Gierlinski, Pawel Biernacki

Comments: MNRAS, in press, 13 pages

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

[62]  arXiv:1910.04591 (replaced) [pdf, other]

Title: A relativistic particle pusher for ultra-strong electromagnetic fields

Authors: J. Pétri

Comments: References added, submitted to Journal of Plasma Physics

Subjects: Computational Physics (physics.comp-ph); High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics - Theory (hep-th)

[63]  arXiv:1910.06176 (replaced) [pdf, other]

Title: Fast collective neutrino oscillations inside the neutrino sphere in core-collapse supernovae

Authors: Milad Delfan Azari, Shoichi Yamada, Taiki Morinaga, Hiroki Nagakura, Shun Furusawa, Akira Harada, Hirotada Okawa, Wakana Iwakami, Kohsuke Sumiyoshi

Comments: 12 pages, 12 figures, accepted for publication in PRD

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

[64]  arXiv:1910.11393 (replaced) [pdf, other]

Title: Gravitational antiscreening in stellar interiors

Authors: Alfio Bonanno, Roberto Casadio, Alessia Platania

Comments: 19 pages, 3 figures. V2: minor changes, references added. Matches published version

Journal-ref: JCAP 2001 (2020) no.01, 022

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

[65]  arXiv:1911.04510 (replaced) [pdf, other]

Title: Global axisymmetric simulations of photoevaporation and magnetically driven protoplanetary disk winds

Authors: Peter J. Rodenkirch, Hubert Klahr, Christian Fendt, Cornelis P. Dullemond

Comments: Published in A&A 633, A21 (2020)

Journal-ref: A&A 633, A21 (2020)

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

[66]  arXiv:1911.05432 (replaced) [pdf, other]

Title: Optimising gravitational waves follow-up using galaxies stellar mass

Authors: J.-G. Ducoin, D. Corre, N. Leroy, E. Le Floch

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

[67]  arXiv:1911.05744 (replaced) [pdf, other]

Title: Zodiacal Exoplanets in Time (ZEIT) IX: a flat transmission spectrum and a highly eccentric orbit for the young Neptune K2-25b as revealed by Spitzer

Authors: Pa Chia Thao, Andrew W. Mann, Marshall C. Johnson, Elisabeth R. Newton, Xueying Guo, Isabel J. Kain, Aaron C. Rizzuto, David Charbonneau, Paul A. Dalba, Eric Gaidos, Jonathan M. Irwin, Adam L. Kraus

Comments: v2 updated for proofs

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

[68]  arXiv:1911.12068 (replaced) [pdf, ps, other]

Title: Tidal disruption of planetary bodies by white dwarfs I: A hybrid SPH-analytical approach

Authors: Uri Malamud, Hagai Perets

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

[69]  arXiv:1911.12184 (replaced) [pdf, ps, other]

Title: Tidal disruption of planetary bodies by white dwarfs II: Debris disc structure and ejected interstellar asteroids

Authors: Uri Malamud, Hagai Perets

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

[70]  arXiv:1912.00737 (replaced) [pdf, ps, other]

Title: Brownian motion approach to anomalous rotation of galaxies

Authors: Alexander Jurisch

Comments: 8 pages, 4 figures

Subjects: Statistical Mechanics (cond-mat.stat-mech); Astrophysics of Galaxies (astro-ph.GA)

[71]  arXiv:1912.00885 (replaced) [pdf, other]

Title: Scalar Induced Gravitational Waves in Different Gauges

Authors: Chen Yuan, Zu-Cheng Chen, Qing-Guo Huang

Comments: 2 figures, 8 pages; errors in I(u,v) corrected; version accepted for publication

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

[72]  arXiv:1912.05572 (replaced) [pdf, other]

Title: Getting a THUMP from a WIMP

Authors: Hooman Davoudiasl, Gopolang Mohlabeng

Comments: 7 pages, 3 figures, Expanded and clarified the discussion on the light scalar evolution and impact on early universe cosmology. The original results and main conclusions remain unchanged

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

[73]  arXiv:1912.05749 (replaced) [pdf, ps, other]

Title: Do the TRAPPIST-1 Planets Have Hydrogen-rich Atmospheres?

Authors: Yasunori Hori, Masahiro Ogihara

Comments: 10 pages, 3 figures, accepted for publication in ApJ

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

[74]  arXiv:1912.08806 (replaced) [pdf, other]

Title: Cosmological parameter estimation via iterative emulation of likelihoods

Authors: Marcos Pellejero-Ibañez, Raul E. Angulo, Giovanni Aricó, Matteo Zennaro, Sergio Contreras, Jens Stücker

Comments: 12 pages, 5 figures

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

[75]  arXiv:2001.00095 (replaced) [pdf, other]

Title: Creation and Evolution of Impact-generated Reduced Atmospheres of Early Earth

Authors: Kevin Zahnle, Roxana Lupu, David Catling, Nick Wogan

Comments: Submitted 12/30/2019 to "The Planetary Science Journal"

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

[76]  arXiv:2001.00941 (replaced) [pdf, other]

Title: The LSST DESC Data Challenge 1: Generation and Analysis of Synthetic Images for Next Generation Surveys

Authors: F. Javier Sánchez, Chris W. Walter, Humna Awan, James Chiang, Scott F. Daniel, Eric Gawiser, Tom Glanzman, David P. Kirkby, Rachel Mandelbaum, Anže Slosar, W. Michael Wood-Vasey, Yusra AlSayyad, Colin J. Burke, Seth W. Digel, Mike Jarvis, Tony Johnson, Heather Kelly, Simon Krughoff, Robert H. Lupton, Phil J. Marshall, John R. Peterson, Paul A. Price, Glenn Sembroski, Brian Van Klaveren, Matthew P. Wiesner, Bo Xin (for the LSST Dark Energy Science Collaboration)

Comments: 20 pages, 22 figures. Submitted to MNRAS

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

[77]  arXiv:2001.02666 (replaced) [pdf, other]

Title: The evolution of dust-disk sizes from a homogeneous analysis of 1-10 Myr-old stars

Authors: Nathanial Hendler, Ilaria Pascucci, Paola Pinilla, Marco Tazzari, John Carpenter, Renu Malhotra, Leonardo Testi

Comments: ApJ accepted, 38 pages, 16 figures, 68k compatible

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

[78]  arXiv:2001.03234 (replaced) [pdf, other]

Title: Tidal Disruptions of Main Sequence Stars -- V. The Varieties of Disruptions

Authors: Julian Krolik, Tsvi Piran, Taeho Ryu

Comments: 10 pages, 2 figures, comments welcome!

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

[79]  arXiv:2001.03501 (replaced) [pdf, other]

Title: Tidal Disruptions of Main Sequence Stars -- I. Observable Quantities and their Dependence on Stellar and Black Hole Mass

Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble

Comments: 14 pages, 7 figures, comments welcome! Supersedes arXiv:1907.08205

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

[80]  arXiv:2001.03502 (replaced) [pdf, other]

Title: Tidal disruptions of main sequence stars -- II. Simulation methodology and stellar mass dependence of the character of full tidal disruptions

Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble

Comments: 19 pages, 10 figures, 3 tables, comments welcome! Supersedes arXiv:1907.11883

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

[81]  arXiv:2001.03503 (replaced) [pdf, other]

Title: Tidal disruptions of main sequence stars -- III. Stellar mass dependence of the character of partial disruptions

Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble

Comments: 14 pages, 8 figures, comments welcome! Supersedes arXiv:1909.04041

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

[82]  arXiv:2001.03504 (replaced) [pdf, other]

Title: Tidal disruptions of main sequence stars -- IV. Relativistic effects and dependence on black hole mass

Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble

Comments: 13 pages, 10 figures, 2 tables, comments welcome!

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

[83]  arXiv:2001.04081 (replaced) [pdf, other]

Title: An investigation on the factors affecting machine learning classifications in $γ$-ray astronomy

Authors: Shengda Luo (1), Alex P. Leung (1), C. Y. Hui (2), K.L. Li (2,3,4) ((1) Macau University of Science and Technology, (2) Chungnam National University, (3) UNIST, (4) National Tsing Hua University)

Comments: 15 pages, 10 figures, 11 tables, accepted for publication in MNRAS

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

[84]  arXiv:2001.04354 (replaced) [pdf, ps, other]

Title: The AGORA high-resolution galaxy simulations comparison project: Public data release

Authors: Santi Roca-Fàbrega, Ji-hoon Kim, Joel R. Primack, Michael J. Butler, Daniel Ceverino, Jun-Hwan Choi, Robert Feldmann, Ben W. Keller, Alessandro Lupi, Kentaro Nagamine, Thomas R. Quinn, Yves Revaz, Romain Teyssier, Spencer C. Wallace (for the AGORA Collaboration)

Comments: AGORA links: this http URL and this http URL

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

[85]  arXiv:2001.04741 (replaced) [pdf, other]

Title: Gravitational Waves from first-order phase transition and domain wall

Authors: Ruiyu Zhou, Jing Yang, Ligong Bian

Comments: 21 pages, 9 figures, comments welcome

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

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