Astrophysics
New submissions
[ showing up to 2000 entries per page: fewer | more ]
New submissions for Thu, 30 Apr 20
- [1] arXiv:2004.13720 [pdf, other]
-
Title: How Consumption and Repulsion Set Planetary Gap Depths and the Final Masses of Gas GiantsComments: Submitted to MNRASSubjects: Earth and Planetary Astrophysics (astro-ph.EP)
Planets open gaps in discs. Gap opening is typically modeled by considering the planetary Lindblad torque which repels disc gas away from the planet's orbit. But gaps also clear because the planet consumes local material. We present a simple, easy-to-use, analytic framework for calculating how gaps deplete and how the disc's structure as a whole changes by the combined action of Lindblad repulsion and planetary consumption. The final mass to which a gap-embedded gas giant grows is derived in tandem. The analytics are tested against 1D numerical experiments and calibrated using published multi-dimensional simulations. In viscous alpha discs, the planet, while clearing a gap, initially accretes practically all of the gas that tries to diffuse past, rapidly achieving super-Jupiter if not brown dwarf status. By contrast, in inviscid discs---that may still accrete onto their central stars by, say, magnetized winds---planets open deep, repulsion-dominated gaps. Then only a small fraction of the disc accretion flow is diverted onto the planet, which grows to a fraction of a Jupiter mass. Transitional disc cavities might be cleared by families of such low-mass objects opening inviscid, repulsion-dominated, overlapping gaps which allow most of the outer disc gas to flow unimpeded onto host stars.
- [2] arXiv:2004.13722 [pdf, other]
-
Title: Debris Disk Results from the Gemini Planet Imager Exoplanet Survey's Polarimetric Imaging CampaignAuthors: Thomas M. Esposito, Paul Kalas, Michael P. Fitzgerald, Maxwell A. Millar-Blanchaer, Gaspard Duchene, Jennifer Patience, Justin Hom, Marshall D. Perrin, Robert J. De Rosa, Eugene Chiang, Ian Czekala, Bruce Macintosh, James R. Graham, Megan Ansdell, Pauline Arriaga, Sebastian Bruzzone, Joanna Bulger, Christine H. Chen, Tara Cotten, Ruobing Dong, Zachary H. Draper, Katherine B. Follette, Li-Wei Hung, Ronald Lopez, Brenda C. Matthews, Johan Mazoyer, Stan Metchev, Julien Rameau, Bin Ren, Malena Rice, Inseok Song, Kevin Stahl, Jason Wang, Schuyler Wolff, Ben Zuckerman, S. Mark Ammons, Vanessa P. Bailey, Travis Barman, Jeffrey Chilcote, Rene Doyon, Benjamin L. Gerard, Stephen J. Goodsell, Alexandra Z. Greenbaum, Pascale Hibon, Sasha Hinkley, Patrick Ingraham, Quinn Konopacky, Jerome Maire, Franck Marchis, et al. (16 additional authors not shown)Comments: Accepted for publication in AJ. 19 figures, 7 tablesSubjects: Earth and Planetary Astrophysics (astro-ph.EP); Instrumentation and Methods for Astrophysics (astro-ph.IM); Solar and Stellar Astrophysics (astro-ph.SR)
We report the results of a ${\sim}4$-year direct imaging survey of 104 stars to resolve and characterize circumstellar debris disks in scattered light as part of the Gemini Planet Imager Exoplanet Survey. We targeted nearby (${\lesssim}150$ pc), young (${\lesssim}500$ Myr) stars with high infrared excesses ($L_{\mathrm{IR}} / L_\star > 10^{-5}$), including 38 with previously resolved disks. Observations were made using the Gemini Planet Imager high-contrast integral field spectrograph in $H$-band (1.6 $\mu$m) coronagraphic polarimetry mode to measure both polarized and total intensities. We resolved 26 debris disks and three protoplanetary/transitional disks. Seven debris disks were resolved in scattered light for the first time, including newly presented HD 117214 and HD 156623, and we quantified basic morphologies of five of them using radiative transfer models. All of our detected debris disks but HD 156623 have dust-poor inner holes, and their scattered-light radii are generally larger than corresponding radii measured from resolved thermal emission and those inferred from spectral energy distributions. To assess sensitivity, we report contrasts and consider causes of non-detections. Detections were strongly correlated with high IR excess and high inclination, although polarimetry outperformed total intensity angular differential imaging for detecting low inclination disks (${\lesssim} 70 \deg$). Based on post-survey statistics, we improved upon our pre-survey target prioritization metric predicting polarimetric disk detectability. We also examined scattered-light disks in the contexts of gas, far-IR, and millimeter detections. Comparing $H$-band and ALMA fluxes for two disks revealed tentative evidence for differing grain properties. Finally, we found no preference for debris disks to be detected in scattered light if wide-separation substellar companions were present.
- [3] arXiv:2004.13724 [pdf, other]
-
Title: Probing Dark Matter Clumps, Strings and Domain Walls with Gravitational Wave DetectorsComments: 21 pages + appendix, 11 figuresSubjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Physics - Phenomenology (hep-ph)
Gravitational wave astronomy has recently emerged as a new way to study our Universe. In this work, we survey the potential of gravitational wave interferometers to detect macroscopic astrophysical objects comprising the dark matter. Starting from the well-known case of clumps we expand to cosmic strings and domain walls. We also consider the sensitivity to measure the dark matter power spectrum on small scales. Our analysis is based on the fact that these objects, when traversing the vicinity of the detector, will exert a gravitational pull on each node of the interferometer, in turn leading to a differential acceleration and corresponding Doppler signal, that can be measured. As a prototypical example of a gravitational wave interferometer, we consider signals induced at LISA. We further extrapolate our results to gravitational wave experiments sensitive in other frequency bands, including ground-based interferometers, such as LIGO, and pulsar timing arrays, such as SKA. Assuming moderate sensitivity improvements beyond the current designs, clumps, strings and domain walls may be within reach of these experiments.
- [4] arXiv:2004.13728 [pdf, other]
-
Title: Constraints on Metastable Helium in the Atmospheres of WASP-69b and WASP-52b with Ultra-Narrowband PhotometryAuthors: Shreyas Vissapragada, Heather A. Knutson, Nemanja Jovanovic, Caleb K. Harada, Antonija Oklopčić, James Eriksen, Dimitri Mawet, Maxwell A. Millar-Blanchaer, Samaporn Tinyanont, Gautam VasishtComments: 17 pages, 8 figures (figures 1 and 2 are rasterized for arXiv file size compliance), accepted to AJSubjects: Earth and Planetary Astrophysics (astro-ph.EP); Instrumentation and Methods for Astrophysics (astro-ph.IM)
Infrared observations of metastable 2$^3$S helium absorption with ground- and space-based spectroscopy are rapidly maturing, as this species is a unique probe of exoplanet atmospheres. Specifically, the transit depth in the triplet feature (with vacuum wavelengths near 1083.3 nm) can be used to constrain the temperature and mass loss rate of an exoplanet's upper atmosphere. Here, we present a new photometric technique to measure metastable 2$^3$S helium absorption using an ultra-narrowband filter (full-width at half-maximum of 0.635 nm) coupled to a beam-shaping diffuser installed in the Wide-field Infrared Camera (WIRC) on the 200-inch Hale Telescope at Palomar Observatory. We use telluric OH lines and a helium arc lamp to characterize refractive effects through the filter and to confirm our understanding of the filter transmission profile. We benchmark our new technique by observing a transit of WASP-69b and detect an excess absorption of $0.498\pm0.045$% (11.1$\sigma$), consistent with previous measurements after considering our bandpass. Then, we use this method to study the inflated gas giant WASP-52b and place a 95th-percentile upper limit on excess absorption in our helium bandpass of 0.47%. Using an atmospheric escape model, we constrain the mass loss rate for WASP-69b to be $5.25^{+0.65}_{-0.46}\times10^{-4}~M_\mathrm{J}/\mathrm{Gyr}$ ($3.32^{+0.67}_{-0.56}\times10^{-3}~M_\mathrm{J}/\mathrm{Gyr}$) at 7,000 K (12,000 K). Additionally, we set an upper limit on the mass loss rate of WASP-52b at these temperatures of $2.1\times10^{-4}~M_\mathrm{J}/\mathrm{Gyr}$ ($2.1\times10^{-3}~M_\mathrm{J}/\mathrm{Gyr}$). These results show that ultra-narrowband photometry can reliably quantify absorption in the metastable helium feature.
- [5] arXiv:2004.13730 [pdf, other]
-
Title: Runaway and walkaway stars from the ONC with Gaia DR2Comments: 19 pages, 7 figures, accepted for publication in MNRASSubjects: Solar and Stellar Astrophysics (astro-ph.SR); Astrophysics of Galaxies (astro-ph.GA)
Theory predicts that we should find fast, ejected (runaway) stars of all masses around dense, young star-forming regions. $N$-body simulations show that the number and distribution of these ejected stars could be used to constrain the initial spatial and kinematic substructure of the regions. We search for runaway and slower walkaway stars within 100 pc of the Orion Nebula Cluster (ONC) using $Gaia$ DR2 astrometry and photometry. We compare our findings to predictions for the number and velocity distributions of runaway stars from simulations that we run for 4 Myr with initial conditions tailored to the ONC. In $Gaia$ DR2, we find 31 runaway and 54 walkaway candidates based on proper motion, but not all of these are viable candidates in three dimensions. About 40 per cent are missing radial velocities, but we can trace back 9 3D-runaways and 24 3D-walkaways to the ONC, all of which are low/intermediate-mass (<8 M$_{\odot}$). Our simulations show that the number of runaways within 100 pc decreases the older a region is (as they quickly travel beyond this boundary), whereas the number of walkaways increases up to 3 Myr. We find fewer walkaways in $Gaia$ DR2 than the maximum suggested from our simulations, which may be due to observational incompleteness. However, the number of $Gaia$ DR2 runaways agrees with the number from our simulations during an age of $\sim$1.3-2.4 Myr, allowing us to confirm existing age estimates for the ONC (and potentially other star-forming regions) using runaway stars.
- [6] arXiv:2004.13731 [pdf, other]
-
Title: High-Resolution Spectral Discriminants of Ocean Loss for M Dwarf Terrestrial ExoplanetsComments: 14 pages, 11 figuresSubjects: Earth and Planetary Astrophysics (astro-ph.EP); Instrumentation and Methods for Astrophysics (astro-ph.IM); Solar and Stellar Astrophysics (astro-ph.SR)
In the near future, extremely-large ground-based telescopes may conduct some of the first searches for life beyond the solar system. High-spectral resolution observations of reflected light from nearby exoplanetary atmospheres could be used to search for the biosignature oxygen. However, while Earth's abundant O$_2$is photosynthetic, early ocean loss may also produce high atmospheric O$_2$ via water vapor photolysis and subsequent hydrogen escape. To explore how to use spectra to discriminate between these two oxygen sources, we generate high-resolution line-by-line synthetic spectra of both a habitable Earth-like, and post-ocean-loss Proxima Centauri b. We examine the strength and profile of four bands of O$_2$ from 0.63 to 1.27 $\mu$m, and quantify their relative detectability. We find that 10 bar O$_2$ post-ocean-loss atmospheres have strong suppression of oxygen bands, and especially the 1.27$\mu$m band. This suppression is due to additional strong, broad O$_2$-O$_2$ collisionally-induced absorption (CIA) generated in these more massive O$_2$atmospheres, which is not present for the smaller amounts of oxygen generated by photosynthesis. Consequently, any detection of the 1.27$\mu$m band in reflected light indicates lower Earth-like O$_2$ levels, which suggests a likely photosynthetic origin. However, the 0.69 $\mu$m O$_2$ band is relatively unaffected by O$_2$-O$_2$ CIA, and the presence of an ocean-loss high-O$_2$ atmosphere could be inferred via detection of a strong 0.69 $\mu$m O$_2$ band, and a weaker or undetected 1.27 $\mu$m band. These results provide a strategy for observing and interpreting O$_2$ in exoplanet atmospheres, that could be considered by future ground-based telescopes.
- [7] arXiv:2004.13732 [pdf, other]
-
Title: Concentrations of Dark Haloes Emerge from Their Merger HistoriesAuthors: Kuan Wang (1), Yao-Yuan Mao (2), Andrew R. Zentner (1), Johannes U. Lange (3, 4), Frank C. van den Bosch (5), Risa H. Wechsler (4, 6) ((1) U. Pittsburgh, (2) Rutgers, (3) UCSC, (4) Stanford, (5) Yale, (6) SLAC)Comments: 14 pages, 7 figures, to be submitted to MNRAS, comments welcomeSubjects: Astrophysics of Galaxies (astro-ph.GA); Cosmology and Nongalactic Astrophysics (astro-ph.CO)
The concentration parameter is a key characteristic of a dark matter halo that conveniently connects the halo's present-day structure with its assembly history. Using 'Dark Sky', a suite of cosmological $N$-body simulations, we investigate how halo concentration evolves with time and emerges from the mass assembly history. We also explore the origin of the scatter in the relation between concentration and assembly history. We show that the evolution of halo concentration has two primary modes: (1) smooth increase due to pseudo-evolution; and (2) intense responses to physical merger events. Merger events induce lasting and substantial changes in halo structures, and we observe a universal response in the concentration parameter. We argue that merger events are a major contributor to the uncertainty in halo concentration at fixed halo mass and formation time. In fact, even haloes that are typically classified as having quiescent formation histories experience multiple minor mergers. These minor mergers drive small deviations from pseudo-evolution, which cause fluctuations in the concentration parameters and result in effectively irreducible scatter in the relation between concentration and assembly history. Hence, caution should be taken when using present-day halo concentration parameter as a proxy for the halo assembly history, especially if the recent merger history is unknown.
- [8] arXiv:2004.13733 [pdf, other]
-
Title: Mass loss rate and local thermodynamic state of KELT-9 b thermosphere from the hydrogen Balmer seriesAuthors: A. Wyttenbach, P. Mollière, D. Ehrenreich, H. M. Cegla, V. Bourrier, C. Lovis, L. Pino, R. Allart, J. V. Seidel, H. J. Hoeijmakers, L. D. Nielsen, B. Lavie, F. Pepe, X. Bonfils, I. A. G. SnellenComments: 20 pages, 25 figures, accepted for publication in A&A (2020-04-25)Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Solar and Stellar Astrophysics (astro-ph.SR)
KELT-9 b, the hottest known exoplanet with $T_{eq}\sim4400$ K, is the archetype of the new planet class of ultra hot Jupiters. These exoplanets are thought to have an atmosphere dominated by neutral and ionized atomic species. Particularly, the H$\alpha$ and H$\beta$ Balmer lines have been detected in the KELT-9~b upper atmosphere, suggesting that the hydrogen is filling the planetary Roche lobe and escapes from the planet. In this work, after detecting $\delta$ Scuti-type stellar pulsation (with a period $P_{puls}=7.54\pm0.12$ h) and studying the Rossiter-McLaughlin effect (we find a spin-orbit angle $\lambda=-85.01^{\deg}\pm0.23^{\deg}$), we focus on the Balmer lines (H$\alpha$ to H$\zeta$) in the optical transmission spectrum of KELT-9 b. Our HARPS-N data show significant absorption for H$\alpha$ to H$\delta$. The precise line shapes of the H$\alpha$, H$\beta$, and H$\gamma$ absorptions allow us to put constraints on the thermospheric temperature. Moreover, the mass loss rate, and the excited hydrogen population of KELT-9 b are also constrained, thanks to a retrieval analysis performed with a new atmospheric model. We retrieve a thermospheric temperature of $T=13200^{+800}_{-720}$ K, and a mass loss rate $\dot{M}=10^{12.8\pm0.3}$ g s$^{-1}$, when the atmosphere is assumed to be in hydrodynamical expansion and in local thermodynamic equilibrium (LTE). Since the thermospheres of hot Jupiters are not expected to be in LTE, we explore atmospheric structures with non-Boltzmann equilibrium for the population of the excited hydrogen. We do not find strong statistical evidence in favor of a departure from LTE. However, our non-LTE scenario suggests that departure from the Boltzmann equilibrium may not be sufficient to explain the retrieved low number densities of the excited hydrogen. In non-LTE, Saha equilibrium departure, via photo-ionization, is probably also needed to explain the data.
- [9] arXiv:2004.13734 [pdf, other]
-
Title: Astrophysical Insights into Radial Velocity Jitter from an Analysis of 600 Planet-search StarsComments: 44 pages, 11 figures, published in The Astronomical JournalJournal-ref: The Astronomical Journal, 159,235 (2020)Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Solar and Stellar Astrophysics (astro-ph.SR)
Radial velocity (RV) detection of planets is hampered by astrophysical processes on the surfaces of stars that induce a stochastic signal, or "jitter", which can drown out or even mimic planetary signals. Here, we empirically and carefully measure the RV jitter of more than 600 stars from the California Planet Search (CPS) sample on a star-by-star basis. As part of this process we explore the activity-RV correlation of stellar cycles and include appendices listing every ostensibly companion-induced signal we removed and every activity cycle we noted. We then use precise stellar properties from Brewer et al. (2017) to separate the sample into bins of stellar mass and examine trends with activity and with evolutionary state. We find RV jitter tracks stellar evolution and that in general, stars evolve through different stages of RV jitter: the jitter in younger stars is driven by magnetic activity, while the jitter in older stars is convectively-driven and dominated by granulation and oscillations. We identify the "jitter minimum" -- where activity-driven and convectively-driven jitter have similar amplitudes -- for stars between 0.7 and 1.7 $M_{\odot}$ and find that more massive stars reach this jitter minimum later in their lifetime, in the subgiant or even giant phases. Finally, we comment on how these results can inform future radial velocity efforts, from prioritization of follow-up targets from transit surveys like TESS to target selection of future RV surveys.
- [10] arXiv:2004.13736 [pdf, other]
-
Title: Accretion driven turbulence in filaments II: Effects of self-gravitySubjects: Astrophysics of Galaxies (astro-ph.GA)
We extend our previous work on simulations with the code RAMSES on accretion driven turbulence by including self-gravity and study the effects of core formation and collapse. We show that radial accretion onto filaments drives turbulent motions which are not isotropic but radially dominated. In contrast to filaments without gravity, the velocity dispersion of self-gravitating filaments does not settle in an equilibrium. Despite showing similar amounts of driven turbulence, they continually dissipate their velocity dispersion until the onset of core formation. This difference is connected to the evolution of the radius as it determines the dissipation rate. In the non-gravitational case filament growth is not limited and its radius grows linearly with time. In contrast, there is a maximum extent in the self-gravitational case resulting in an increased dissipation rate. Furthermore, accretion driven turbulence shows a radial profile which is anti-correlated with density. This leads to a constant turbulent pressure throughout the filament. As the additional turbulent pressure does not have a radial gradient it does not contribute to the stability of filaments and does not increase the critical line-mass. However, this radial turbulence does affect the radius of a filament, adding to the extent and setting its maximum value. Moreover, the radius evolution also affects the growth timescale of cores which compared to the timescale of collapse of an accreting filament limits core formation to high line-masses.
- [11] arXiv:2004.13737 [pdf, other]
-
Title: The ALPINE-ALMA [CII] Survey: CGM pollution and gas mixing by tidal stripping in a merging system at z~4.57Authors: M. Ginolfi, G. C. Jones, M. Bethermin, A. Faisst, B. C. Lemaux, D. Schaerer, Y. Fudamoto, P. Oesch, M. Dessauges-Zavadsky, S. Fujimoto, S. Carniani, O. Le Fevre, P. Cassata, J. D. Silverman, P. Capak, Lin Yan, S. Bardelli, O. Cucciati, R. Gal, C. Gruppioni, N. P. Hathi, L. Lubin, R. Maiolino, L. Morselli, D. Pelliccia, M. Talia, D. Vergani, G. ZamoraniComments: 11 pages, 7 figures. Submitted to A&A, comments are welcomeSubjects: Astrophysics of Galaxies (astro-ph.GA); Cosmology and Nongalactic Astrophysics (astro-ph.CO)
We present ALMA observations of a merging system at z ~ 4.57, observed as a part of the ALMA Large Program to INvestigate [CII] at Early times (ALPINE) survey. Combining ALMA [CII] 158 micron and far-infrared continuum data with multi-wavelength ancillary data we find that the system is composed of two massive (Mstar >~ 10^10 Msun) star-forming galaxies experiencing a major merger (stellar mass ratio r_mass ~ 0.9) at close spatial (~13 kpc; projected) and velocity (delta_v < 300 km/s) separations, and two additional faint narrow [CII]-emitting satellites. The overall system belongs to a larger-scale protocluster environment and is coincident to one of its overdensity peaks. ALMA reveals also the presence of [CII] emission arising from a circumgalactic gas structure, extending out to ~30 kpc. Our morpho-spectral decomposition analysis shows that about 50% of the total flux resides between the individual galaxy components, in a metal-enriched gaseous envelope characterized by a disturbed morphology and complex kinematics. Similarly to observations of shock-excited [CII] emitted from tidal tails in local groups, our results can be interpreted as a possible signature of interstellar gas stripped by strong gravitational interactions, with a possible contribution from material ejected by galactic outflows and emission triggered by star formation in small faint satellites. Our findings suggest that mergers could be an efficient mechanism of gas mixing in the circumgalactic medium around high-z galaxies, and thus play a key role in the galaxy baryon cycle at early epochs.
- [12] arXiv:2004.13739 [pdf, other]
-
Title: A Detailed View of the Circumstellar Environment and Disk of the Forming O-star AFGL 4176Authors: K. G. Johnston, M. G. Hoare, H. Beuther, H. Linz, P. Boley, R. Kuiper, N. D. Kee, T. P. RobitailleComments: Accepted for publication in The Astrophysical Journal, 49 pages, 26 figuresSubjects: Solar and Stellar Astrophysics (astro-ph.SR); Astrophysics of Galaxies (astro-ph.GA)
We present a detailed analysis of the disk and circumstellar environment of the forming O-type star AFGL 4176 mm1, placing results from the Atacama Large Millimeter/submillimeter Array (ALMA) into context with multi-wavelength data. With ALMA, we detect seventeen 1.2 mm continuum sources within 5$''$ (21,000 au) of AFGL 4176 mm1. We find that mm1 has a spectral index of 3.4$\pm$0.2 across the ALMA band, with $>$87 percent of its 1.2 mm continuum emission from dust. The source mm2, projected 4200 au from mm1, may be a companion or a blueshifted knot in a jet. We also explore the morphological differences between the molecular lines with ALMA, detecting 203 lines from 25 molecules, which we categorize into several morphological types. Our results show that AFGL 4176 mm1 provides an example of a forming O-star with a large and chemically complex disk, which is mainly traced by nitrogen-bearing molecules. Lines that show strong emission on the blueshifted side of the disk are predominantly oxygen-bearing, which we suggest are tracing a disk accretion shock. The molecules C$^{34}$S, H$_2$CS and CH$_{3}$CCN trace a slow wide-angle wind or dense structures in the outflow cavity walls. With the Australia Telescope Compact Array (ATCA), we detect a compact continuum source ($<$2000 $\times$ 760 au) at 1.2 cm, associated with mm1, of which $>$96 percent is from ionized gas. The ATCA NH$_3$(1,1) and (2,2) emission traces a large-scale (r$\sim$0.5 pc) rotating toroid with the disk source mm1 in the blueshifted part of this structure offset to the NW.
- [13] arXiv:2004.13740 [pdf, other]
-
Title: The bivariate gas-stellar mass distributions and the mass functions of early- and late-type galaxies at $z\sim0$Authors: Aldo Rodriguez-Puebla (1), A. R. Calette (1), Vladimir Avila-Reese (1), Vicente Rodriguez-Gomez (2), Marc Huertas-Company (3) ((1) IA-UNAM, (2) IRyA-UNAM, (3) Obs. Paris)Comments: 37 pages, 17 figures. Submitted to PASA, this is the version after the first Referee reportSubjects: Astrophysics of Galaxies (astro-ph.GA)
We report the bivariate HI- and H$_2$-stellar mass distributions of local galaxies in addition of an inventory of galaxy mass functions, MFs, for HI, H$_2$, cold gas, and baryonic mass, separately into early- and late-type galaxies. The MFs are determined using the HI and H$_2$ conditional distributionsand the galaxy stellar mass function, GSMF. For the conditional distributions we use the compilation presented in Calette et al. 2018. For determining the GSMF from $M_{\ast}\sim3\times10^{7}$ to $3\times10^{12}$ $M_{\odot}$, we combine two spectroscopic samples from the SDSS at the redshift range $0.0033<z<0.2$. We find that the low-mass end slope of the GSMF, after correcting from surface brightness incompleteness, is $\alpha\approx-1.4$, consistent with previous determinations. The obtained HI MFs agree with radio blind surveys. Similarly, the H$_2$ MFs are consistent with CO follow-up optically-selected samples. We estimate the impact of systematics due to mass-to-light ratios and find that our MFs are robust against systematic errors. We deconvolve our MFs from random errors to obtain the intrinsic MFs. Using the MFs, we calculate cosmic density parameters of all the baryonic components. Baryons locked inside galaxies represent 5.4% of the universal baryon content, while $\sim96$% of the HI and H$_2$ mass inside galaxies reside in late-type morphologies. Our results imply cosmic depletion times of H$_2$ and total neutral H in late-type galaxies of $\sim 1.3$ and 7.2 Gyr, respectively, which shows that late type galaxies are on average inefficient in converting H$_2$ into stars and in transforming HI gas into H$_2$. Our results provide a fully self-consistent empirical description of galaxy demographics in terms of the bivariate gas--stellar mass distribution and their projections, the MFs. This description is ideal to compare and/or to constrain galaxy formation models.
- [14] arXiv:2004.13741 [pdf, ps, other]
-
Title: Simulations of ELT-GMCAO performance for deep field observationsAuthors: Elisa Portaluri, Valentina Viotto, Roberto Ragazzoni, Carmelo Arcidiacono, Maria Bergomi, Marco Dima, Davide Greggio, Jacopo Farinato, Demetrio MagrinComments: 18 pages, 10 figures, accepted for publication on PASPSubjects: Instrumentation and Methods for Astrophysics (astro-ph.IM); Astrophysics of Galaxies (astro-ph.GA)
The Global-Multi Conjugated Adaptive Optics (GMCAO) approach offers an alternative way to correct an adequate scientific Field of View (FoV) using only natural guide stars (NGSs) to extremely large ground-based telescopes. Thus, even in the absence of laser guide stars, a GMCAO-equipped ELT-like telescope can achieve optimal performance in terms of Strehl Ratio (SR), retrieving impressive results in studying star-poor fields, as in the cases of the deep field observations. The benefits and usability of GMCAO have been demonstrated by studying 6000 mock high redshift galaxies in the Chandra Deep Field South region. However, a systematic study simulating observations in several portions of the sky is mandatory to have a robust statistic of the GMCAO performance. Technical, tomographic and astrophysical parameters, discussed here, are given as inputs to GIUSTO, an IDL-based code that estimates the SR over the considered field, and the results are analyzed with statistical considerations. The best performance is obtained using stars that are relatively close to the Scientific FoV; therefore, the SR correlates with the mean off-axis position of NGSs, as expected, while their magnitude plays a secondary role. This study concludes that the SRs correlate linearly with the galactic latitude, as also expected. Because of the lack of natural guide stars needed for low-order aberration sensing, the GMCAO confirms as a promising technique to observe regions that can not be studied without the use of laser beacons. It represents a robust alternative way or a risk mitigation strategy for laser approaches on the ELTs.
- [15] arXiv:2004.13742 [pdf, other]
-
Title: Self-scattering of non-spherical dust grainsComments: Accepted by A&A. Author accepted manuscript. Accepted on 28/04/2020. Deposited on 28/04/2020. 11 pagesSubjects: Solar and Stellar Astrophysics (astro-ph.SR); Earth and Planetary Astrophysics (astro-ph.EP); Astrophysics of Galaxies (astro-ph.GA)
The understanding of (sub-)millimetre polarisation has made a leap forward since high-resolution imaging with ALMA came available. Amongst other effects, self-scattering (i.e., scattering of thermal dust emission on other grains) is thought to be the origin of millimetre polarisation. This opens the first window to a direct measurement of dust grain sizes in regions of optically thick continuum emission as it can be found in protoplanetary disks and star-forming regions. However, the newly derived values of grain sizes are usually around ${\sim}100\,\mu$m and thus one order of magnitude smaller than those obtained from more indirect measurements as well as those expected from theory (${\sim}1\,$mm). We see the origin of this contradiction in the applied dust model of today's self-scattering simulations: a perfect compact sphere. The aim of this study is to test our hypothesis by investigating the impact of non-spherical grain shapes on the self-scattering signal. We apply discrete dipole approximation simulations to investigate the influence of the grain shape on self-scattering polarisation in three scenarios: an unpolarised and polarised incoming wave under a fixed as well as a varying incident polarisation angle. We find significant deviations of the resulting self-scattering polarisation when comparing non-spherical to spherical grains, in particular outside the Rayleigh regime, i.e. for >100$\,\mu$m size grains observed at $870\,\mu$m wavelength. Self-scattering by oblate grains produces higher polarisation degrees compared to spheres which challenges the interpretation of the origin of observed millimetre polarisation. A (nearly) perfect alignment of the non-spherical grains is required to account for the observed millimetre polarisation in protoplanetary disks. Our findings point towards a necessary re-evaluation of the dust grain sizes derived from (sub-)mm polarisation.
- [16] arXiv:2004.13743 [pdf, other]
-
Title: Properties of F Stars with Stable Radial Velocity Timeseries: A Useful Metric for Selecting Low-jitter F StarsComments: 10 pages, 8 figures, published in The Astronomical JournalJournal-ref: The Astrophysical Journal, 159:236, 2020Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Solar and Stellar Astrophysics (astro-ph.SR)
In a companion paper, we have conducted an in-depth analysis of radial velocity jitter of over 600 stars, examining the astrophysical origins including stellar granulation, oscillation, and magnetic activity. In this paper, we highlight a subsample of those stars, specifically the main sequence and "retired" F stars -- which we refer to as "MSRF" stars -- that show low levels of RV jitter ($<10$ m/s). We describe the observational signatures of these stars that allow them to be identified in radial velocity planet programs, for instance those performing follow-up of transiting planets discovered by TESS. We introduce a "jitter metric" that combines the two competing effects of RV jitter with age: activity and convection. Using thresholds in the jitter metric, we can select both "complete" and "pure" samples of low jitter F stars. We also provide recipes for identifying these stars using only Gaia colors and magnitudes. Finally, we describe a region in the Gaia color-magnitude diagram where low jitter F stars are most highly concentrated. By fitting a 9th order polynomial to the Gaia main sequence, we use the height above the main sequence as a proxy for evolution, allowing for a crude selection of low jitter MSRF stars when activity measurements are otherwise unavailable.
- [17] arXiv:2004.13750 [pdf, other]
-
Title: Timescales for detection of super-Chandrasekhar white dwarfs by gravitational wave astronomyAuthors: Surajit Kalita (IISc), Banibrata Mukhopadhyay (IISc), Tushar Mondal (IISc), Tomasz Bulik (Warsaw)Comments: 10 pages including 3 figures and 5 tables; Accepted for publication in ApJSubjects: High Energy Astrophysical Phenomena (astro-ph.HE)
In about last couple of decades, the inference of the violation of the Chandrasekhar mass-limit of white dwarfs from indirect observation is probably a revolutionary discovery in astronomy. Various researchers have already proposed different theories to explain this interesting phenomenon. However, such massive white dwarfs usually possess very little luminosity, and hence they, so far, cannot be detected directly by any observations. We have already proposed that the continuous gravitational wave may be one of the probes to detect them directly, and in the future, various space-based detectors such as LISA, DECIGO, and BBO, should be able to detect many of those white dwarfs (provided they behave like pulsars). In this paper, we address various timescales related to the emission of gravitational as well as dipole radiations. This exploration sets a timescale for the detectors to observe the massive white dwarfs.
- [18] arXiv:2004.13752 [pdf, other]
-
Title: Cosmic Filaments from Cosmic StringsComments: 12 pages, 12 figuresSubjects: 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)
Cosmic strings are generically predicted in many extensions of the Standard Model of particle physics. We propose a new avenue for detecting cosmic strings through their effect on the filamentary structure in the cosmic web. Using cosmological simulations of the density wake from a cosmic string, we examine a variety of filament structure probes. We show that the largest effect of the cosmic string is an overdensity in the filament distribution around the string wake. The signal from the overdensity is stronger at higher redshift, and more robust with a wider field. We analyze the spatial distribution of filaments from a publicly available catalog of filaments built from SDSS galaxies. With existing data, we find no evidence for the presence of a cosmic string wake with string tension parameter $G\mu$ above $\sim 5\times 10^{-6}$. However, we project WFIRST will be able to detect a signal from such a wake at the $99\%$ confidence level at redshift $z=2$, with significantly higher confidence and the possibility of probing lower tensions ($G\mu \sim 10^{-6}$), at $z=10$. The sensitivity of this method is not competitive with constraints derived from the CMB. However, it provides an independent discovery channel at low redshift, which could be a smoking-gun in scenarios where the CMB bound can be weakened.
- [19] arXiv:2004.13754 [pdf, ps, other]
-
Title: The eye of Gaia on globular clusters structure: tidal tailsAuthors: A. SollimaComments: 13 pages, 5 figures, accepted for publication by MNRASSubjects: Astrophysics of Galaxies (astro-ph.GA); Solar and Stellar Astrophysics (astro-ph.SR)
I analyse the projected density distribution of member stars over a wide area surrounding 18 Galactic globular clusters using the photometric and astrometric information provided by the second data release of the Gaia mission. A 5D mixture modelling technique has been employed to optimally isolate the signal of the cluster stellar population from the contamination of the Galactic field, taking advantage of its different distribution in the space formed by colours, magnitudes, parallaxes and proper motions. In 7 clusters I detect collimated overdensities at a >3 sigma level above the background density extending well beyond the cluster tidal radius, consistent with the distortion expected as a result of the tidal interaction with the Milky Way potential. In five of these clusters (NGC288, NGC2298, NGC5139, NGC6341 and NGC7099) spectacular tidal tails extend up to the border of the analysed field of view at 5 degrees from the centre. At large distances from the cluster centre, the orientation of the detected overdensities appears to be systematically aligned with the cluster orbital path, in agreement with the predictions of N-body simulations. The fraction of stars contained in the tidal tails of these clusters is also used to determine the first observational estimate of their present-day destruction rates.
- [20] arXiv:2004.13756 [pdf, ps, other]
-
Title: Particle acceleration in low-power hotspots: modelling the broad-band spectral energy distributionAuthors: G. Migliori (1,2), M. Orienti (2), L. Coccato (3), G. Brunetti (2), F. D'Ammando (2), K.-H. Mack (2), M.A. Prieto (4) ((1) DIFA, University of Bologna, (2) INAF-IRA Bologna, (3) ESO, (4) IAC)Comments: 16 pages, 10 figures, accepted for publication in MNRASSubjects: High Energy Astrophysical Phenomena (astro-ph.HE)
The acceleration and radiative processes active in low-power radio hotspots are investigated by means of new deep near-infrared (NIR) and optical VLT observations, complemented with archival, high-sensitivity VLT, radio VLA and X-ray Chandra data. For the three studied radio galaxies (3C 105, 3C 195 and 3C 227), we confirm the detection of NIR/optical counterparts of the observed radio hotspots. We resolve multiple components in 3C 227 West and in 3C 105 South and characterize the diffuse NIR/optical emission of the latter. We show that the linear size of this component ($\gtrsim$4 kpc) makes 3C 105 South a compelling case for particles' re-acceleration in the post-shock region. Modeling of the radio-to-X-ray spectral energy distribution (SED) of 3C 195 South and 3C 227 W1 gives clues on the origin of the detected X-ray emission. In the context of inverse Compton models, the peculiarly steep synchrotron curve of 3C 195 South sets constraints on the shape of the radiating particles' spectrum that are testable with better knowledge of the SED shape at low ($\lesssim$GHz) radio frequencies and in X-rays. The X-ray emission of 3C 227 W1 can be explained with an additional synchrotron component originating in compact ($<$100 pc) regions, such those revealed by radio observations at 22 GHz, provided that efficient particle acceleration ($\gamma\gtrsim$10$^7$) is ongoing. The emerging picture is that of systems in which different acceleration and radiative processes coexist.
- [21] arXiv:2004.13757 [pdf, ps, other]
-
Title: Jansky VLA observations of synchrotron emitting optical hotspots of 3C 227 and 3C 445 radio galaxiesAuthors: M. Orienti (1), G. Migliori (1,2), G. Brunetti (1), H. Nagai (3), F. D'Ammando (1), K.-H. Mack (1), M.A. Prieto (4) ((1) INAF-IRA Bologna, (2) DIFA, University of Bologna, (3) NAOJ, (4) IAC)Comments: 12 pages, 13 figures, published in MNRASJournal-ref: MNRAS, Vol 494, 2020, pp.2244-2253Subjects: High Energy Astrophysical Phenomena (astro-ph.HE)
We report results on deep Jansky Very Large Array A-configuration observations at 22 GHz of the hotspots of the radio galaxies 3C227 and 3C445. Synchrotron emission in the optical on scales up to a few kpc was reported for the four hotspots. Our VLA observations point out the presence of unresolved regions with upper limit to their linear size of about 100 pc. This is the first time that such compact components in hotspots have been detected in a mini-sample, indicating that they are not a peculiar characteristic of a few individual hotspots. The polarization may reach values up to 70 per cent in compact (about 0.1 kpc scale) regions within the hotspot, indicating a highly ordered magnetic field with size up to a hundred parsecs. On larger scales, the average polarization of the hotspot component is about 30-45 per cent, suggesting the presence of a significant random field component, rather than an ordered magnetic field. This is further supported by the displacement between the peaks in polarized intensity and in total intensity images that is observed in all the four hotspots. The electric vector position angle is not constant, but changes arbitrarily in the central part of the hotspot regions, whereas it is usually perpendicular to the total intensity contours of the outermost edge of the hotspot structure, likely marking the large-scale shock front. The misalignment between X-ray and radio-to-optical emission suggests that the former is tracing the current particle acceleration, whereas the latter marks older shock fronts.
- [22] arXiv:2004.13767 [pdf, other]
-
Title: Photometry as a proxy for stellar activity in radial velocity analysesComments: 10 pages, accepted in AJSubjects: Earth and Planetary Astrophysics (astro-ph.EP); Instrumentation and Methods for Astrophysics (astro-ph.IM); Solar and Stellar Astrophysics (astro-ph.SR)
Stellar activity remains a limiting factor in measuring precise planet parameters from radial velocity spectroscopy, not least in the search for Earth mass planets orbiting in the habitable zones of Sun-like stars. One approach to mitigate stellar activity is to use combined analyses of both radial velocity and time-series photometry. We present an analysis of simultaneous disk-integrated photometry and radial velocity data of the Sun in order to determine the useful limits of a combined analysis. We find that simple periodogram or autocorrelation analysis of solar photometry give the correct rotation period <50% of the time. We therefore use a Gaussian process to investigate the time variability of solar photometry and to directly compare simultaneous photometry with radial velocity data. We find that the hyperparameter posteriors are relatively stable over 70 years of solar photometry and the amplitude tracks the solar cycle. We observe good agreement between the hyperparameter posteriors for the simultaneous photometry and radial velocity data. Our primary conclusion is a recommendation to include an additional prior in Gaussian process fits to constrain the evolutionary timescale to be greater than the recurrence timescale (ie., the rotation period) to recover more physically plausible and useful results. Our results indicate that such simultaneous monitoring may be a useful tool in enhancing the precision of radial velocity surveys.
- [23] arXiv:2004.13768 [pdf, other]
-
Title: The rotation curve, mass distribution and dark matter content of the Milky Way from Classical CepheidsComments: 21 pages, 5 figures, 1 table. Accepted for publication in Astrophysical Journal LettersSubjects: Astrophysics of Galaxies (astro-ph.GA)
With the increasing numbers of large stellar survey projects, the quality and quantity of excellent tracers to study the Milky Way is rapidly growing, one of which is the classical Cepheids. Classical Cepheids are high precision standard candles with very low typical uncertainties ($<$ 3\%) available via the mid-infrared period-luminosity relation. About 3500 classical Cepheids identified from OGLE, ASAS-SN, Gaia, WISE and ZTF survey data have been analyzed in this work, and their spatial distributions show a clear signature of Galactic warp. Two kinematical methods are adopted to measure the Galactic rotation curve in the Galactocentric distance range of $4\lesssim R_{\rm GC} \lesssim 19$ kpc. Gently declining rotation curves are derived by both the proper motion (PM) method and 3-dimensional velocity vector (3DV) method. The largest sample of classical Cepheids with most accurate 6D phase-space coordinates available to date are modeled in the 3DV method, and the resulting rotation curve is found to decline at the relatively smaller gradient of ($-1.33\pm0.1$) ${\rm km\,s^{-1}\,kpc^{-1}}$. Comparing to results from the PM method, a higher rotation velocity (($232.5\pm0.9$) ${\rm km\,s^{-1}}$) is derived at the position of Sun in the 3DV method. The virial mass and local dark matter density are estimated from the 3DV method which is the more reliable method, $M_{\rm vir} = (0.822\pm0.052)\times 10^{12}\,M_\odot$ and $\rho_{\rm DM,\odot} = 0.33\pm0.03$ GeV ${\rm cm^{-3}}$, respectively.
- [24] arXiv:2004.13792 [pdf, other]
-
Title: Active red giants: close binaries versus single rapid rotatorsAuthors: Patrick Gaulme, Jason Jackiewicz, Federico Spada, Drew Chojnowski, Benoit Mosser, Jean McKeever, Anne Hedlund, Mathieu Vrard, Mansour Benbakoura, Cilia DamianiComments: Accepted in Astronomy & Astrophysics (18 pages, 18 figures, 3 tables)Subjects: Solar and Stellar Astrophysics (astro-ph.SR)
The objective of this work is to determine what fraction of red-giant (RG) stars shows photometric rotational modulation, and understand its origin. One of the underlying questions is the role of close binarity in this population, standing upon the fact that RGs in short-period binary systems (<150 days or so) have been observed to display strong rotational modulation. We select a sample of about 4500 relatively bright RGs observed by Kepler, and show that 370 of them (8%) display rotational modulation. Almost all have oscillation amplitudes below the median of the sample, while 30 of them are not oscillating at all. Of the 85 of these RGs with rotational modulation chosen for follow-up radial-velocity observation and analysis, 34 show clear evidence of spectroscopic binarity. Surprisingly, 26 of the 30 non-oscillators are in this group of binaries. To the contrary, about 85% of the active RGs with detectable oscillations are not part of close binaries. With the help of stellar masses and evolutionary states computed from the oscillation properties, it appears that low-mass red-giant branch stars tend to be magnetically inactive, while intermediate-mass ones tend to be highly active. The opposite trends are true for helium-core burning (red clump) stars, whereby the lower-mass clump stars are comparatively more active and the higher-mass ones less so. In other words, we find that low-mass red-giant branch stars gain angular momentum as they evolve to clump stars, while higher-mass ones lose angular momentum. The trend observed with low-mass stars leads to possible scenarios of planet engulfment or other merging events during the shell-burning phase. Regarding intermediate-mass stars, the rotation periods are long with respect to theoretical expectations reported in the literature, which reinforces the existence of an unidentified sink of angular momentum after the main sequence.
- [25] arXiv:2004.13794 [pdf, other]
-
Title: Chemistry of Temperate Super-Earth and Mini-Neptune Atmospheric Hazes from Laboratory ExperimentsAuthors: Sarah E. Moran, Sarah M. Hörst, Véronique Vuitton, Chao He, Nikole K. Lewis, Laurène Flandinet, Julianne I. Moses, Nicole North, François-Régis Orthous-Daunay, Joshua Sebree, Cédric Wolters, Eliza M.-R. Kempton, Mark S. Marley, Caroline V. Morley, Jeff A. ValentiComments: 22 pages, 8 figures, 9 tables, accepted for publication in the Planetary Science JournalSubjects: Earth and Planetary Astrophysics (astro-ph.EP); Instrumentation and Methods for Astrophysics (astro-ph.IM)
Very little experimental work has been done to explore the properties of photochemical hazes formed in atmospheres with very different compositions or temperatures than that of the outer solar system or of early Earth. With extrasolar planet discoveries now numbering thousands, this untapped phase space merits exploration. This study presents measured chemical properties of haze particles produced in laboratory analogues of exoplanet atmospheres. We used very high resolution mass spectrometry to measure the chemical components of solid particles produced in atmospheric chamber experiments. Many complex molecular species with general chemical formulas C$_w$H$_x$N$_y$O$_z$ were detected. We detect molecular formulas of prebiotic interest in the data, including those for the monosaccharide glyceraldehyde, a variety of amino acids and nucleotide bases, and several sugar derivatives. Additionally, the experimental exoplanetary haze analogues exhibit diverse solubility characteristics, which provide insight into the possibility of further chemical or physical alteration of photochemical hazes in super-Earth and mini-Neptune atmospheres. These exoplanet analogue particles can help us better understand chemical atmospheric processes and suggest a possible source of in situ atmospheric prebiotic chemistry on distant worlds.
- [26] arXiv:2004.13811 [pdf, other]
-
Title: Localizing merging black holes with gravitational-wave lensingComments: 19 pages, 5 figuresSubjects: High Energy Astrophysical Phenomena (astro-ph.HE); General Relativity and Quantum Cosmology (gr-qc)
We report here a method that can precisely localize a merging black hole. The current gravitational-wave localization methods rely mainly on merging neutron stars or other sources with electromagnetic counterparts. However, the scientific targets of merging black holes are entirely different and they allow us to probe exciting properties such as higher-order modes, high redshifts, and the strong field of gravity. Unfortunately, the lack of an electromagnetic counterpart and the poor sky localization accuracies of the current gravitational-wave detectors make it generally difficult to localize a merging black hole precisely. However, lensed gravitational waves, whose first observation is predicted in this decade, could allow us to search for the source through locating its similarly lensed host galaxy. Specifically, a dedicated follow-up of the sky localization of the lensed gravitational wave could allow us to identify the lensed host galaxy, and to reconstruct its lens profile. Unfortunately, uniquely identifying the correct host galaxy is challenging, because there are hundreds and sometimes thousands of other lensed galaxies within the sky area spanned by the gravitational-wave observation. However, by combining the gravitational-wave information with the lens reconstructions of all the lensed galaxy candidates, we show that one can localize quadruply lensed waves to one or at most a few galaxies with the LIGO/Virgo/Kagra network. Using simulated data, we demonstrate that once the lensed host is identified, the gravitational-wave source can be localized within the host galaxy, and the system can be used to measure the Hubble constant.
- [27] arXiv:2004.13877 [pdf, other]
-
Title: Classifying Image Sequences of Astronomical Transients with Deep Neural NetworksAuthors: Catalina Gómez, Mauricio Neira, Marcela Hernández Hoyos, Pablo Arbeláez, Jaime E. Forero-RomeroComments: 9 pages, 6 figures. Submitted. Comments are welcomeSubjects: Instrumentation and Methods for Astrophysics (astro-ph.IM); Computer Vision and Pattern Recognition (cs.CV)
Supervised classification of temporal sequences of astronomical images into meaningful transient astrophysical phenomena has been considered a hard problem because it requires the intervention of human experts. The classifier uses the expert's knowledge to find heuristic features to process the images, for instance, by performing image subtraction or by extracting sparse information such as flux time series in the form of light curves. We present a successful deep learning approach that learns directly from imaging data. Our method models explicitly the spatio-temporal patterns with Deep Convolutional Neural Networks and Gated Recurrent Units. We train these deep neural networks using 1.3 million real astronomical images from the Catalina Real-Time Transient Survey to classify the sequences into five different types of astronomical transient classes. The TAO-Net (for Transient Astronomical Objects Network) architecture achieves on the five-type classification task an average F1-score of 54.58$\pm$13.32, almost nine points higher than the F1-score of 45.49 $\pm$ 13.75 from the random forest classification on light curves. The achievement TAO-Net opens the possibility to develop new deep-learning architectures for early transient detection. We make available the training dataset and trained models of TAO-Net to allow for future extensions of this work.
- [28] arXiv:2004.13911 [pdf, ps, other]
-
Title: Dynamic evolution of major element chemistry in protoplanetary disks and its implications for chondrite formationComments: 16 pages, 6 figures, 1 tableSubjects: Earth and Planetary Astrophysics (astro-ph.EP); Geophysics (physics.geo-ph)
Chondrites are the likely building blocks of Earth, and identifying the group of chondrite that best represents Earth is a key to resolving the state of the early Earth. The origin of chondrites, however, remains controversial partly because of their puzzling major element compositions, some exhibiting depletions in Al, Ca, and Mg. Based on a new thermochemical evolution model of protoplanetary disks, we show that planetesimals with depletion patterns similar to ordinary and enstatite chondrites can originate at 1--2~AU just outside where enstatite evaporates. Around the "evaporation front" of enstatite, the large inward flow of refractory minerals, including forsterite, takes place with a high pebble concentration, and the loss of those minerals result in depletion in Al, Ca, and Mg. When evaporated solid grains re-condense onto pebbles, the concentration of pebbles is further enhanced, potentially triggering the streaming instability. Planetesimals with the composition of ordinary and enstatite chondrites can thus be naturally created in the terrestrial region. The preferential loss of forsterite also creates an enhancement of Mg/Si and heavy Si isotopes just inside the potential source region for ordinary and enstatite chondrites. Earth, which shows both features, may originate just inside where ordinary and enstatite chondrites were born.
- [29] arXiv:2004.13913 [pdf, other]
-
Title: Machine Learning the Cosmic Curvature in a Model-independent WayComments: 9 pages, 7 figures, and 2 tables. SubmittedSubjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); General Relativity and Quantum Cosmology (gr-qc)
In this work, we apply an algorithm of machine learning, the Artificial Neural Network (ANN), to determine the cosmic curvature in a cosmological model-independent way, by using the Hubble parameter measurements $H(z)$ and type Ia supernovae (SNe Ia). The code ReFANN \citep{Wanggj:2020}, a non-parametric approach that can reconstruct a function from observational data with ANN, is used to reconstruct $H(z)$ in our analysis. We find a spatially open universe is preferred by the current $H(z)$ and SNe Ia data, and the difference between our result and the value inferred from Planck CMB is $1.6\sigma$. Furthermore, we test the capability of the future gravitational waves (GW) standard sirens in the measurement of the cosmic curvature, and find that the error of $\Omega_K$ is $\sim0.186$ when 100 GW events with electromagnetic counterparts are detected, which is $\sim56\%$ smaller than that constrained from the Pantheon SNe Ia. In addition, we also test the performance of the ANN and the Gaussian process (GP) in the measurement of the cosmic curvature. We find that $\Omega_K$ based on the GP method can be greatly influenced by the prior of $H_0$, while the ANN method can overcome this to reduce the influence of the prior of $H_0$ on the measurement of the cosmic curvature. Therefore, the ANN method may have more advantages than GP in the measurement of the cosmic curvature.
- [30] arXiv:2004.13915 [pdf, other]
-
Title: HST survey of the Orion Nebula Cluster in the H$_2$O 1.4 $μ$m absorption band: I. A census of substellar and planetary mass objectsAuthors: Massimo Robberto, Mario Gennaro, Maria Giulia Ubeira Gabellini, Lynne A. Hillenbrand, Camilla Pacifici, Leonardo Ubeda, Morten Andersen, Travis Barman, Andrea Bellini, Nicola Da Rio, Selma E. de Mink, Giuseppe Lodato, Carlo Felice Manara, Imants Platais, Laurent Pueyo, Giovanni M. Strampelli, Jonathan C. Tan, Leonardo TestiComments: Accepted for publication in the Astrophysical Journal. The resolution of several figures has been downgraded to comply with the size limit of arXiv submissionsSubjects: Solar and Stellar Astrophysics (astro-ph.SR)
In order to obtain a complete census of the stellar and sub-stellar population, down to a few M$_{Jup}$ in the $\sim1$ Myr old Orion Nebula Cluster, we used the infrared channel of the Wide Field Camera 3 of the Hubble Space Telescope with the F139M and F130N filters. These bandpasses correspond to the $1.4 \mu$m H$_2$O absorption feature and an adjacent line-free continuum region. Out of $4,504$ detected sources, $3,352$ (about $75\%$) appear fainter than m$_{130}=14$ (Vega mag) in the F130N filter, a brightness corresponding to the hydrogen-burning limit mass (M$\simeq 0.072 M_\odot$) at $\sim 1$ Myr. Of these, however, only $742$ sources have a negative F130M-139N color index, indicative of the presence of H$_2$O vapor in absorption, and can therefore be classified as bona-fide M and L dwarfs, with effective temperatures T$\lesssim 2850$ K at an assumed $1$ Myr cluster age. On our color-magnitude diagram, this population of sources with H$_2$O absorption appears clearly distinct from the larger background population of highly reddened stars and galaxies with positive F130M-F139N color index, and can be traced down to the sensitivity limit of our survey, m$_{130}\simeq 21.5$, corresponding to a $1$ Myr old $\simeq 3 $M$_{Jup}$, planetary mass object under about 2 magnitudes of visual extinction. Theoretical models of the BT-Settl family predicting substellar isochrones of $1, 2$ and $3$ Myr (down to $\sim 1 $M$_{Jup}$) fail to reproduce the observed H$_2$O color index at M$\lesssim 20 $M$_{Jup}$. We perform a Bayesian analysis to determine extinction, mass and effective temperature of each sub-stellar member of our sample, together with its membership probability.
- [31] arXiv:2004.13917 [pdf, other]
-
Title: Effects of Dark Energy anisotropic stress on the matter power spectrumComments: 19 pages, 13 figures, 1 tableSubjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); General Relativity and Quantum Cosmology (gr-qc)
We study the effects of dark energy (DE) anisotropic stress on features of the matter power spectrum (PS). We employ the Parametrized Post-Friedmannian (PPF) formalism to emulate an effective DE, and model its anisotropic stress properties through a two-parameter equation that governs its overall amplitude ($g_0$) and transition scale ($c_g$). For the background cosmology, we consider different equations of state to model DE including a constant $w_0$ parameter, and models that provide thawing (CPL) and freezing (nCPL) behaviors. We first constrain these parameters by using the JLA, BAO, $H_0$ and CMB Planck data. Then, we analyze the role played by these parameters in the linear PS. In order for the anisotropic stress not to provoke deviations larger than $10\%$ and $5\%$ with respect to the $\Lambda$CDM PS at $k \sim 0.01 \,h/\text{Mpc}$, the parameters have to be in the range $-0.30< g_0 < 0.32$, $0 \leq c_g^2 < 0.01$ and $-0.15 < g_0 < 0.16$, $0 \leq c_g^2 < 0.01$, respectively. Additionally, we compute the leading nonlinear corrections to the PS using standard perturbation theory in real and redshift space, showing that the differences with respect to the $\Lambda$CDM are enhanced, especially for the quadrupole and hexadecapole RSD multipoles. %Additionally, we also compute the leading nonlinear corrections to the PS using standard perturbation theory in real and redshift space to understand how the linear anisotropic stress contributes to nonlinearities, showing that the differences with the $\Lambda$CDM are enhanced.
- [32] arXiv:2004.13920 [pdf, other]
-
Title: HST survey of the Orion Nebula Cluster in the H$_2$O 1.4 $μ$m absorption band: II. The substellar IMF down to planetary massesComments: Accepted for publication in the Astrophysical JournalSubjects: Solar and Stellar Astrophysics (astro-ph.SR); Astrophysics of Galaxies (astro-ph.GA)
We exploit the ability of the Hubble Space Telescope to probe near infrared water absorption present in the atmosphere of low-mass stars, brown dwarfs and planetary mass objects to create a very pure sample of Orion Nebula Cluster (ONC) members, not affected by contamination from background stars and galaxies which lack water absorption. Thanks to these data we infer the Initial Mass Function (IMF) of the ONC in the $0.005 - 1.4$M$_{\odot}$ regime, i.e. down to few Jupiter masses. The young age of the ONC, $\sim1$ Myr, provides a snapshot of the outcome of star formation for the present-day conditions (metallicity, temperature, pressure) of typical Milky Way disk molecular clouds. We demonstrate that the IMF of the ONC is well described by either a log-normal function or a broken power-law, with parameter values qualitatively in agreement with the canonical Chabrier or Kroupa forms for the Milky Way disk IMF. This continuity in the mass distribution provides clues to the fact that the same physical processes may be regulating formation of stars, brown dwarfs, and planetary mass objects. Both the canonical IMF forms under-predict the observed number of very low mass members (below $0.1$ M$_\odot$), a regime where our data allows more precise constraints. Nevertheless, we do not observe a rise or secondary peak in the brown dwarfs or planetary mass regimes. Our study thus contradicts findings based on broad-band near infrared ground-based photometry, which predict an extremely high number of free-floating planets, but likely suffer from unaccounted background contamination.
- [33] arXiv:2004.13924 [pdf, other]
-
Title: HST survey of the Orion Nebula Cluster in the H$_2$O 1.4 $μ$m absorption band: III. The population of sub-stellar binary companionsAuthors: Giovanni M. Strampelli, Jonathan Aguilar, Laurent Pueyo, Antonio Aparicio, Mario Gennaro, Leonardo Ubeda, Massimo RobbertoComments: Accepted for publication in the Astrophysical JournalSubjects: Solar and Stellar Astrophysics (astro-ph.SR); Astrophysics of Galaxies (astro-ph.GA)
We present new results concerning the sub-stellar binary population in the Orion Nebula Cluster (ONC). Using the Karhunen-Lo\`{e}ve Image Projection (KLIP) algorithm, we have reprocessed images taken with the IR channel of the Wide Field Camera 3 mounted on the Hubble Space Telescope to unveil faint close companions in the wings of the stellar PSFs. Starting with a sample of $1392$ bona-fide not saturated cluster members, we detect $39$ close-pairs cluster candidates with separation $0.16''-0.77''$. The primary masses span a range M$_p$ $\sim 0.015-1.27$ M$_{\odot}$ whereas for the companions we derive M$_c$ $\sim 0.004-0.54$ M$_{\odot}$. Of these $39$ binary systems, $18$ were already known while the remaining $21$ are new detections. Correcting for completeness and combining our catalog with previously detected ONC binaries, we obtain an overall binary fraction of $11.5\% \pm 0.9\%$. Compared to other star forming regions, our multiplicity function is $\sim 2$ smaller than e.g. Taurus, while compared to the binaries in the field we obtain comparable values. We analyze the mass function of the binaries, finding differences between the mass distribution of binaries and single stars and between primary and companion mass distributions. The mass ratio shows a bottom-heavy distribution with median value of $M_c/M_p \sim 0.25$. Overall our results suggest that ONC binaries may represent a template for the typical population of field binaries, supporting the hypothesis that the ONC may be regarded as a most typical star forming region in the Milky Way.
- [34] arXiv:2004.13946 [pdf, other]
-
Title: Probing the initial conditions of high-mass star formation -- IV. Gas dynamics and NH$_2$D chemistry in high-mass pre/protocluster clumpsAuthors: Chuan-Peng Zhang, Guang-Xing Li, Thushara Pillai, Timea Csengeri, Friedrich Wyrowski, Karl M. Menten, Michele R. PestalozziComments: 27 pages, 25 figures, 6 tables, accepted for publication in A&ASubjects: Astrophysics of Galaxies (astro-ph.GA); Solar and Stellar Astrophysics (astro-ph.SR)
The initial stage of star formation is very difficult to study because of its high density and low temperature. Under such conditions, many molecules become depleted from the gas phase by freezing out onto dust grains. However, the deuterated species could remain gaseous and are thus ideal tracers. We investigate the gas dynamics and NH$_2$D chemistry in eight massive pre/protocluster clumps. We present NH$_2$D 1$_{11}$-1$_{01}$ (at 85.926 GHz), NH$_3$ (1, 1) and (2, 2) observations in the eight clumps using the PdBI and the VLA, respectively. We find that the distribution between deuterium fractionation and kinetic temperature shows a number density peak at around $T_{\rm kin}=16.1$ K, and the NH$_2$D cores are mainly located at a temperature range of 13.0 to 22.0 K. We detect seven extremely high deuterium fractionation of $1.0 \leqslant D_{\rm frac} \leqslant 1.41$. We find that the NH$_2$D emission does not appear to coincide exactly with either dust continuum or NH$_3$ peak positions, but often surrounds the star-formation active regions. This suggests that the NH$_{2}$D has been destroyed by the central young stellar object (YSO) due to its heating. The detected NH$_2$D lines are very narrow with a median width of $\rm 0.98\pm0.02 km/s$. The extracted NH$_2$D cores are gravitationally bound ($\alpha_{\rm vir} < 1$), are likely prestellar or starless, and can potentially form intermediate-mass or high-mass stars. Using NH$_3$ (1, 1) as a dynamical tracer, we find very complicated dynamical movement, which can be explained by a combined process with outflow, rotation, convergent flow, collision, large velocity gradient, and rotating toroids. We find that high deuterium fractionation strongly depends on the temperature condition, and NH$_2$D is a poor evolutionary indicator of high-mass star formation in evolved stages, but a useful tracer in the starless and prestellar cores.
- [35] arXiv:2004.13951 [pdf]
-
Title: Near-infrared observations of active asteroid (3200) Phaethon reveal no evidence for hydrationAuthors: Driss Takir, Theodore Kareta, Joshua P. Emery, Josef Hanus, Vishnu Reddy, Ellen S. Howell, Andrew S. Rivkin, Tomoko AraiJournal-ref: Nat Commun 11, 2050 (2020)Subjects: Earth and Planetary Astrophysics (astro-ph.EP)
Asteroid (3200) Phaethon is an active near-Earth asteroid and the parent body of the Geminid Meteor Shower. Because of its small perihelion distance, Phaethon's surface reaches temperatures sufficient to destabilize hydrated materials. We conducted rotationally resolved spectroscopic observations of this asteroid, mostly covering the northern hemisphere and the equatorial region, beyond 2.5-micron to search for evidence of hydration on its surface. Here we show that the observed part of Phaethon does not exhibit the 3-micron hydrated mineral absorption (within 2-sigma). These observations suggest that Phaethon's modern activity is not due to volatile sublimation or devolatilization of phyllosilicates on its surface. It is possible that the observed part of Phaethon was originally hydrated and has since lost volatiles from its surface via dehydration, supporting its connection to the Pallas family, or it was formed from anhydrous material.
- [36] arXiv:2004.13976 [pdf, other]
-
Title: Constraints on the Newton's Constant from Cosmological ObservationsComments: 7 pages, 2 figuresSubjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); General Relativity and Quantum Cosmology (gr-qc)
The Newton's constant have observational effects on both the CMB power spectra and the light curves of SNIa. We use the Planck data, BAO data and the SNIa measurement to constrain the Newton's constant $G$ during the CMB epoch and the redshift ranges of PANTHEON samples, and find no evidence indicating that $G$ is varying with redshift. By extending the $\Lambda$CDM model with a free parameter $G$, we get $H_0=70.54 \pm 0.95$ km s$^{-1}$ Mpc$^{-1}$ at 68$\%$ C.L. and alleviate the $H_0$ tension between R19 and Planck+BAO data slightly, to $2\sigma$.
- [37] arXiv:2004.13987 [pdf, other]
-
Title: The deep composition of Uranus and Neptune from in situ exploration and thermochemical modelingAuthors: Thibault Cavalié, Olivia Venot, Yamila Miguel, Leigh N. Fletcher, Peter Wurz, Olivier Mousis, Roda Bounaceur, Vincent Hue, Jérémy Leconte, Michel DobrijevicComments: Accepted for publication in Space Science ReviewsSubjects: Earth and Planetary Astrophysics (astro-ph.EP); Instrumentation and Methods for Astrophysics (astro-ph.IM)
The distant ice giants of the Solar System, Uranus and Neptune, have only been visited by one space mission, Voyager 2. The current knowledge on their composition remains very limited despite some recent advances. A better characterization of their composition is however essential to constrain their formation and evolution, as a significant fraction of their mass is made of heavy elements, contrary to the gas giants Jupiter and Saturn. An in situ probe like Galileo would provide us with invaluable direct ground-truth composition measurements. However, some of the condensibles will remain out of the grasp of a shallow probe. While additional constraints could be obtained from a complementary orbiter, thermochemistry and diffusion modeling can further help us to increase the science return of an in situ probe.
- [38] arXiv:2004.13996 [pdf, other]
-
Title: Simulations Show that Vortex Flows could Heat the Chromosphere in Solar PlageComments: 8 pages, 5 figures, accepted in ApJLSubjects: Solar and Stellar Astrophysics (astro-ph.SR)
The relationship between vortex flows at different spatial scales and their contribution to the energy balance in the chromosphere is not yet fully understood. We perform three-dimensional (3D) radiation-magnetohydrodynamic (MHD) simulations of a unipolar solar plage region at a spatial resolution of 10 km using the MURaM code. We use the swirling-strength criterion that mainly detects the smallest vortices present in the simulation data. We additionally degrade our simulation data to smooth-out the smaller vortices, so that also the vortices at larger spatial scales can be detected. Vortex flows at various spatial scales are found in our simulation data for different effective spatial resolutions. We conclude that the observed large vortices are likely clusters of much smaller ones that are not yet resolved by observations. We show that the vertical Poynting flux decreases rapidly with reduced effective spatial resolutions and is predominantly carried by the horizontal plasma motions rather than vertical flows. Since the small-scale horizontal motions or the smaller vortices carry most of the energy, the energy transported by vortices deduced from low resolution data is grossly underestimated. In full resolution simulation data, the Poynting flux contribution due to vortices is more than adequate to compensate for the radiative losses in plage, indicating their importance for chromospheric heating.
- [39] arXiv:2004.14011 [pdf, ps, other]
-
Title: Lagrangian-space Gaussian ansatz for the matter redshift-space power spectrum and correlation functionComments: 15 pagesSubjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
We study the predictions for the matter redshift-space power spectrum and correlation function of a Lagrangian-space Gaussian ansatz introduced in a previous work. This model is a natural extension of the Zeldovich approximation, where the displacement and velocity power spectra are determined by the equations of motion, instead of being set equal to the linear power spectrum. It does not contain any free parameter. As for the real-space statistics, we find that this Lagrangian-space approach is much more efficient for the correlation functions than for the power spectra. The damping of the BAO oscillations is well recovered but there is a large smooth drift from the simulations in the power spectra. The multipoles of the correlation functions are well recovered on BAO scales, with an accuracy of $2\%$ for $\xi^s_0$ down to $10 h^{-1}$ Mpc, and of $3\%$ for $\xi^s_2$ down to $26 h^{-1}$ Mpc, at $z \geq 0.35$.
- [40] arXiv:2004.14019 [pdf, other]
-
Title: A deep X-ray spectral imaging of the bow-shock pulsar wind nebula associated with PSR B1929+10Authors: Sangin Kim (1), C.Y. Hui (1), Jongsu Lee (1), Kwangmin Oh (1), L.C.C. Lin (2), J. Takata (3) ((1) Chungnam National University, (2) UNIST, (3) Huazhong University of Science and Technology)Comments: A&A Letter in press, 6 pages, 3 figures, 4 tablesSubjects: High Energy Astrophysical Phenomena (astro-ph.HE)
In this work, we study the X-ray bow-shock nebula powered by the mature pulsar PSR B1929+10 using data from XMM-Newton, with an effective exposure of $\sim$ 300 ks, offering the deepest investigation of this system thus far. We found the X-ray axial outflow extends as long as $\sim$ 8 arc minute behind the proper motion direction, which is a factor of two longer than the result reported in the previous study. Furthermore, we found evidence of two faint lateral outflows extending laterally with respect to the proper motion. We also found indications of spectral hardening along the axial outflow, suggesting that certain acceleration processes might occur along this feature.
- [41] arXiv:2004.14029 [pdf, ps, other]
-
Title: A Fast Radio Burst discovered in FAST drift scan surveyAuthors: Weiwei Zhu, Di Li, Rui Luo, Chenchen Miao, Bing Zhang, Laura Spitler, Duncan Lorimer, Michael Kramer, David Champion, Youling Yue, Andrew Cameron, Marilyn Cruces, Ran Duan, Yi Feng, Jun Han, George Hobbs, Chenhui Niu, Jiarui Niu, Zhichen Pan, Lei Qian, Dai Shi, Ningyu Tang, Pei Wang, Hongfeng Wang, Mao Yuan, Lei Zhang, Xinxin Zhang, Shuyun Cao, Li Feng, Hengqian Gan, Long Gao, Xuedong Gu, Minglei Guo, Qiaoli Hao, Lin Huang, Menglin Huang, Peng Jiang, Chengjin Jin, Hui Li, Qi Li, Qisheng Li, Hongfei Liu, Gaofeng Pan, Bo Peng, Hui Qian, Xiangwei Shi, Jinyuo Song, Liqiang Song, Caihong Sun, Jinghai Sun, Hong Wang, Qiming Wang, Yi Wang, Xiaoyao Xie, Jun Yan, Li Yang, Shimo Yang, Rui Yao, Dongjun Yu, Jinglong Yu, Chengmin Zhang, Haiyan Zhang, Shuxin Zhang, Xiaonian Zheng, Aiying Zhou, Boqin Zhu, et al. (4 additional authors not shown)Comments: 7 pages, 3 figures, accepted for publication in ApJLSubjects: High Energy Astrophysical Phenomena (astro-ph.HE)
We report the discovery of a highly dispersed fast radio burst, FRB~181123, from an analysis of $\sim$1500~hr of drift-scan survey data taken using the Five-hundred-meter Aperture Spherical radio Telescope (FAST). The pulse has three distinct emission components, which vary with frequency across our 1.0--1.5~GHz observing band. We measure the peak flux density to be $>0.065$~Jy and the corresponding fluence $>0.2$~Jy~ms. Based on the observed dispersion measure of 1812~cm$^{-3}$~pc, we infer a redshift of $\sim 1.9$. From this, we estimate the peak luminosity and isotropic energy to be $\lesssim 2\times10^{43}$~erg~s$^{-1}$ and $\lesssim 2\times10^{40}$~erg, respectively. With only one FRB from the survey detected so far, our constraints on the event rate are limited. We derive a 95\% confidence lower limit for the event rate of 900 FRBs per day for FRBs with fluences $>0.025$~Jy~ms. We performed follow-up observations of the source with FAST for four hours and have not found a repeated burst. We discuss the implications of this discovery for our understanding of the physical mechanisms of FRBs.
- [42] arXiv:2004.14040 [pdf, other]
-
Title: Rings and arcs around evolved stars. II. The Carbon Star AFGL 3068 and the Planetary Nebulae NGC 6543, NGC 7009 and NGC 7027Comments: 13 pages, 9 figures, accepted for publication in MNRASSubjects: Solar and Stellar Astrophysics (astro-ph.SR); Astrophysics of Galaxies (astro-ph.GA)
We present a detailed comparative study of the arcs and fragmented ring-like features in the haloes of the planetary nebulae (PNe) NGC 6543, NGC 7009, and NGC 7027 and the spiral pattern around the carbon star AFGL 3068 using high-quality multi-epoch HST images. This comparison allows us to investigate the connection and possible evolution between the regular patterns surrounding AGB stars and the irregular concentric patterns around PNe. The radial proper motion of these features, ~15 km/s, are found to be consistent with the AGB wind and their linear sizes and inter-lapse times (500-1900 yr) also agree with those found around AGB stars, suggesting a common origin. We find evidence using radiative-hydrodynamic simulations that regular patterns produced at the end of the AGB phase become highly distorted by their interactions with the expanding PN and the anisotropic illumination and ionization patterns caused by shadow instabilities. These processes will disrupt the regular (mostly spiral) patterns around AGB stars, plausibly becoming the arcs and fragmented rings observed in the haloes of PNe.
- [43] arXiv:2004.14041 [pdf, other]
-
Title: Electromagnetic induction heating as a driver of volcanic activity on massive rocky planetsComments: Five pages, three figures, accepted for publication in A&A lettersSubjects: Earth and Planetary Astrophysics (astro-ph.EP); Solar and Stellar Astrophysics (astro-ph.SR)
Aims. We investigate possible driving mechanisms of volcanic activity on rocky super-Earths with masses exceeding 3-4 Mearth. Due to high gravity and pressures in the mantles of these planets, melting in deep mantle layers can be suppressed, even if the energy releae due to tidal heating and radioactive decay is substantial. Here we investigate whether a newly identified heating mechanism, namely induction heating by the star's magnetic field, can drive volcanic activity on these planets due to its unique heating pattern in the very upper part of the mantle. In this region the pressure is not yet high enough to preclude the melt formation. Methods. Using the super-Earth HD 3167b as an example, we calculate induction heating in the planet's interiors assuming an electrical conductivity profile typical of a hot rocky planet and a moderate stellar magnetic field typical of an old inactive star. Then we use a mantle convection code (CHIC) to simulate the evolution of volcanic outgassing with time. Results. We show that although in most cases volcanic outgassing on HD 3167b is not very significant in the absence of induction heating, including this heating mechanism changes the picture and leads to a substantial increase in the outgassing from the planet's mantle. This result shows that induction heating combined with a high surface temperature is capable of driving volcanism on massive super-Earths, which has important observational implications.
- [44] arXiv:2004.14042 [pdf, other]
-
Title: The local and global properties of different types of supernova host galaxiesAuthors: Li Zhou, Yan-Chun Liang, Jun-Qiang Ge, Yi-Nan Zhu, Xu Shao, Hong Wu, Wei-Bin Shi, Li-Cai DengComments: 15 pages, 15 figuresSubjects: Astrophysics of Galaxies (astro-ph.GA)
By using Data Analysis Pipeline (DAP) products of Mapping Nearby Galaxies at Apache Point Observatory (MaNGA), which are publicly available from the SDSS Data Release 15, we analyze the local properties at the SN explosion sites and global properties of different types of SN host galaxies to explore the explosion environments of different types of SNe. In our sample, there are 67 SN host galaxies in the field of view of MaNGA, including 32 Type Ia, 29 CCSNe, 1 super-luminous SN (SLSN), 1 Type I and 4 unclassified type of SNe, with which we can perform the K-S test for analysis and derive statistically robust results. Due to the limited sample size, we couldn't remove the mass dependence in this work, which is likely the true driver of the trends for the properties presented in this work. The global star formation rate (SFR) and EW(H$\alpha$) for SN Ia hosts is slightly lower than that for CCSN hosts on average. SN Ia host galaxies are $\sim$ 0.3 dex more massive than CCSN hosts, which implies that the number ratio of CCSNe to Type Ia SNe will decrease with the increasing of stellar mass of host galaxies. The stellar population age of SN Ia host galaxies is older than that of CCSN hosts on average. There is no significant difference between different types of SN hosts for some properties, including local SFR density ($\Sigma \rm SFR$), local and global gas-phase oxygen abundance. For most galaxies in our sample, the global gas-phase oxygen abundance estimated from the integrated spectra of SN hosts can represent the local gas-phase oxygen abundance at the SN explosion sites with small bias.
- [45] arXiv:2004.14050 [pdf, other]
-
Title: A detailed analysis on the cloud structure and dynamics in Aquila RiftComments: 17 pages, 10 figuresSubjects: Solar and Stellar Astrophysics (astro-ph.SR); Astrophysics of Galaxies (astro-ph.GA)
We present maps in several molecular emission lines of a 1 square-degree region covering the W40 and Serpens South molecular clouds belonging to the Aquila Rift complex. The observations were made with the 45 m telescope at the Nobeyama Radio Observatory. We found that the $^{12}$CO and $^{13}$CO emission lines consist of several velocity components with different spatial distributions. The component that forms the main cloud of W40 and Serpens South, which we call the "main component", has a velocity of $V_{\rm LSR}\simeq 7$ km s$^{-1}$. There is another significant component at $V_{\rm LSR}\simeq 40$ km s$^{-1}$, which we call the "40 km s$^{-1}$ component". The latter component is mainly distributed around two young clusters: W40 and Serpens South. Moreover, the two components look spatially anti-correlated. Such spatial configuration suggests that the star formation in W40 and Serpens South was induced by the collision of the two components. We also discuss a possibility that the 40 km s$^{-1}$ component consists of gas swept up by superbubbles created by SNRs and stellar winds from the Scorpius-Centaurus Association.
- [46] arXiv:2004.14058 [pdf, other]
-
Title: Thermodynamic and Energetic Limits on Continental Silicate Weathering Strongly Impact the Climate and Habitability of Wet, Rocky WorldsComments: 27 pages excluding references, 8 figures. Submitted to ApJ, revised, resubmittedSubjects: Earth and Planetary Astrophysics (astro-ph.EP)
The "liquid water habitable zone" (HZ) concept is predicated on the ability of the silicate weathering feedback to stabilize climate across a wide range of instellations. However, representations of silicate weathering used in current estimates of the effective outer edge of the HZ do not account for the thermodynamic limit on concentration of weathering products in runoff set by clay precipitation, nor for the energetic limit on precipitation set by planetary instellation. We find that when the thermodynamic limit is included in an idealized coupled climate/weathering model, steady-state planetary climate loses sensitivity to silicate dissolution kinetics, becoming sensitive to temperature primarily through the effect of temperature on runoff and to pCO$_2$ through an effect on solute concentration mediated by pH. This increases sensitivity to land fraction, CO$_2$ outgassing, and geological factors such as soil age and lithology, all of which are found to have a profound effect on the position of the effective outer edge of the HZ. The interplay between runoff sensitivity and the energetic limit on precipitation leads to novel warm states in the outer reaches of the HZ, owing to the decoupling of temperature and precipitation. We discuss strategies for detecting the signature of silicate weathering feedback through exoplanet observations in light of insights derived from the revised picture of weathering.
- [47] arXiv:2004.14083 [pdf, other]
-
Title: Standing kink waves in sigmoid solar coronal loops: implications for coronal seismologySubjects: Solar and Stellar Astrophysics (astro-ph.SR)
Using full three-dimensional magnetohydrodynamic numerical simulations, we study the effects of magnetic field sigmoidity or helicity on the properties of the fundamental kink oscillation of solar coronal loops. Our model consists of a single denser coronal loop, embedded in a plasma with dipolar force-free magnetic field with a constant alpha-parameter. For the loop with no sigmoidity, we find that the numerically determined oscillation period of the fundamental kink mode matches the theoretical period calculated using WKB theory. In contrast, with increasing sigmoidity of the loop, the actual period is increasingly smaller than the one estimated by WKB theory. Translated through coronal seismology, increasing sigmoidity results in magnetic field estimates which are increasingly shifting towards higher values, and even surpassing the average value for the highest alpha value considered. Nevertheless, the estimated range of the coronal magnetic field value lies within the mimimal/maximal limits, proving the robustness coronal seismology. We propose that the discrepancy in the estimations of the absolute value of the force-free magnetic field could be exploited seismologically to determine the free energy of coronal loops, if averages of the internal magnetic field and density can be reliably estimated by other methods.
- [48] arXiv:2004.14099 [pdf, other]
-
Title: Catalog of averaged magnetic phase curves of stars: the second editionAuthors: V.D. Bychkov (1), L.V. Bychkova (1), J. Madej (2) ((1) Special Astrophysical Observatory, RAS, Russia (2) Astronomical Observatory, Univ. of Warsaw, Poland)Comments: 136 pages, 511 figuresSubjects: Solar and Stellar Astrophysics (astro-ph.SR)
Magnetized stars exhibit periodic variations of their longitudinal global magnetic fields, $B_e$, owing to rotation. Here, we present the second catalog of averaged stellar magnetic rotational phase curves and their parameters derived from a compilation of the published observational data and personal communications for 350 stars of various spectral types, which were published up to the end of December 2019. Magnetic Ap and Bp stars constitute the most numerous subset in the catalog (215 objects). Phase curves were obtained by fitting either a sinusoid or a double sine wave to series of the observed $B_e$ measurements using the least squares method. For some stars, we present magnetic phase curves derived from time series of the surface magnetic field, $B_s$, or obtained improved values of the rotational period, $P_{\rm rot}$. We have also identified eight stars in our catalog that host planets or planetary systems.
- [49] arXiv:2004.14121 [pdf, other]
-
Title: Scattered light may reveal the existence of ringed exoplanetsAuthors: Mario Sucerquia, Jaime A. Alvarado-Montes, Jorge I. Zuluaga, Matías Montesinos, Amelia BayoComments: Accepted for publication in MNRAS Letters. 7 pages, 6 figuresSubjects: Earth and Planetary Astrophysics (astro-ph.EP); Instrumentation and Methods for Astrophysics (astro-ph.IM)
Rings around giant exoplanets (hereafter 'exorings') are still a missing planetary phenomenon among the vast number of discovered planets. Despite the fact there exist a large number of methods for identifying and characterizing these exorings, none of them has been successful to date. Most of those efforts focus on the photometric signatures produced by rings around transiting exoplanets; thus, little interest has been intended for the detectable signatures that non-transiting ringed planets might cause owing to the excess of scattered starlight from both their atmosphere and the considerably large surface of their (hypothetical) rings-system. This extra scattering produced by exorings would occur at an orbital location defined here as the `the summer solstice' of a stellar light curve. In this letter, we develop a first-order model to estimate the photometric signatures of non-transiting exorings and predict their detectability by using present and future facilities. We also show how, besides the discovery itself, our model can be used to constrain orbital and physical parameters of planet-rings systems.
- [50] arXiv:2004.14122 [pdf, other]
-
Title: Substructure Formation in a Protostellar Disk of L1527 IRSAuthors: Riouhei Nakatani, Hauyu Baobab Liu, Satoshi Ohashi, Yichen Zhang, Tomoyuki Hanawa, Claire Chandler, Yoko Oya, Nami SakaiSubjects: Solar and Stellar Astrophysics (astro-ph.SR); Earth and Planetary Astrophysics (astro-ph.EP); Astrophysics of Galaxies (astro-ph.GA)
We analyze multi-frequency, high-resolution continuum data obtained by ALMA and JVLA to study detailed structure of the dust distribution in the infant disk of a Class~0/I source, L1527 IRS. We find three clumps aligning in the north-south direction in the $7 {\rm \,mm}$ radio continuum image. The three clumps remain even after subtracting free-free contamination, which is estimated from the $1.3{\rm \,cm}$ continuum observations. The northern and southern clumps are located at a distance of $\sim 15{\rm \,au}$ from the central clump and are likely optically thick at $7{\rm \,mm}$ wavelength. The clumps have similar integrated intensities. The symmetric physical properties could be realized when a dust ring or spiral arms around the central protostar is projected to the plane of the sky. We demonstrates for the first time that such substructure may form even in the disk-forming stage, where the surrounding materials actively accrete toward a disk-protostar system.
- [51] arXiv:2004.14192 [pdf, ps, other]
-
Title: Searching for a Black Hole in the Outer Solar SystemAuthors: Edward WittenComments: 4 ppSubjects: Earth and Planetary Astrophysics (astro-ph.EP); High Energy Physics - Phenomenology (hep-ph); High Energy Physics - Theory (hep-th)
There are hints of a novel object ("Planet 9") with a mass $5-10$ $M_\oplus$ in the outer Solar System, at a distance of order 500 AU. If it is a relatively conventional planet, it can be found in telescopic searches. Alternatively, it has been suggested that this body might be a primordial black hole (PBH). In that case, conventional searches will fail. A possible alternative is to probe the gravitational field of this object using small, laser-launched spacecraft, like the ones envisioned in the Breakthrough Starshot project. With a velocity of order $.001~c$, such spacecraft can reach Planet 9 roughly a decade after launch and can discover it if they can report timing measurements accurate to $10^{-5}$ seconds back to Earth.
- [52] arXiv:2004.14207 [pdf, other]
-
Title: Orbital and super-orbital periods in ULX pulsars, disc-fed HMXBs, Be/X-ray binaries and double-periodic variablesAuthors: L. J. Townsend (1,2,3), P. A. Charles (4) ((1) South African Astronomical Observatory, (2) Southern African Large Telescope, (3) University of Cape Town, (4) University of Southampton)Comments: 5 pages, accepted for publication in MNRAS LettersSubjects: High Energy Astrophysical Phenomena (astro-ph.HE); Solar and Stellar Astrophysics (astro-ph.SR)
We present evidence for a simple linear relationship between the orbital period and super-orbital period in ultra-luminous X-ray (ULX) pulsars, akin to what is seen in the population of disc-fed neutron star super-giant X-ray binary and Be/X-ray binary systems. We argue that the most likely cause of this relationship is the modulation of precessing hot spots or density waves in an accretion or circumstellar disc by the binary motion of the system, implying a physical link between ULX pulsars and high-mass X-ray binary (HMXB) pulsars. This hypothesis is supported by recent studies of Galactic and Magellanic Cloud HMXBs accreting at super-Eddington rates, and the position of ULX pulsars on the spin period--orbital period diagram of HMXBs. An interesting secondary relationship discovered in this work is the apparent connection between disc-fed HMXBs, ULXs and a seemingly unrelated group of early-type binaries showing so-called "double-periodic" variability. We suggest that these systems are good candidates to be the direct progenitors of Be/X-ray binaries.
- [53] arXiv:2004.14232 [pdf, other]
-
Title: X-Shooter survey of disk accretion in Upper Scorpius I. Very high accretion rates at age>5 MyrAuthors: C.F. Manara, A. Natta, G.P. Rosotti, J.M. Alcala, B. Nisini, G. Lodato, L. Testi, I. Pascucci, L. Hillenbrand, J. Carpenter, A. Scholz, D. Fedele, A. Frasca, G. Mulders, E. Rigliaco, C. Scardoni, E. ZariComments: Under review on Astronomy & Astrophysics. Revised version after first positive referee reportSubjects: Solar and Stellar Astrophysics (astro-ph.SR); Earth and Planetary Astrophysics (astro-ph.EP); Astrophysics of Galaxies (astro-ph.GA)
Determining the mechanisms that drive the evolution of protoplanetary disks is a necessary step to understand how planets form. Here we measure the mass accretion rate for young stellar objects at age >5 Myr, a critical test for the current models of disk evolution. We present the analysis of the spectra of 36 targets in the ~5-10 Myr old Upper Scorpius region for which disk masses were measured with ALMA. We find that the mass accretion rates in this sample of old but still survived disks are similarly high as those of the younger (<3 Myr old) star-forming regions of Lupus and Cha I, when considering the dependence on stellar and disk mass. In particular, several disks show high mass accretion rates >10^-9 Msun/yr while having low disk masses. Furthermore, the median values of the measured mass accretion rates in the disk mass ranges where our sample is complete at a level ~60-80% are compatible in these three regions. At the same time, the spread of mass accretion rates at any given disk mass is still >0.9 dex even at age>5 Myr. These results are in contrast with simple models of viscous evolution, which would predict that the values of the mass accretion rate diminish with time, and a tighter correlation with disk mass at age>5 Myr. Similarly, simple models of internal photoevaporation cannot reproduce the observed mass accretion rates, while external photoevaporation might explain the low disk masses and high accretion rates. A partial possible solution to the discrepancy with the viscous models is that the gas-to-dust ratio of the disks at >5 Myr is significantly different and higher than the canonical 100, as suggested by some dust and gas disk evolution models. The results shown here require the presence of several inter-playing processes, such as detailed dust evolution, external photoevaporation and possibly MHD winds, to explain the secular evolution of protoplanetary disks.
- [54] arXiv:2004.14242 [pdf, other]
-
Title: Science with the TianQin observatory: Preliminary results on stellar-mass binary black holesComments: 20 pages, 8 figures, submitted to PRDSubjects: High Energy Astrophysical Phenomena (astro-ph.HE); General Relativity and Quantum Cosmology (gr-qc)
We study the prospect of using TianQin to detect stellar-mass binary black holes (SBBHs). We estimate the expected detection number as well as the precision of parameter estimation on SBBH inspirals, using five different population models. We note TianQin can possibly detect a few SBBH inspirals with signal to noise ratios greater than 12, lowering the threshold and combining multiple detectors can both boost the detection number. The source parameters can be recovered with good precision for most events above the detection threshold. For example, the precision of the merger time most likely occur near 1s, making it possible to guide the detection of the ground based detectors, the precision of the eccentricity $e_0$ most likely occur near $10^{-4}$, making it possible to distinguish the formation channels, and the precision of the mass parameter is better than $10^{-6}$ in general and most likely occur near $10^{-7}$. We note, in particular, that for a typical merger event, the error volume is likely to be small enough to contain only the host galaxy, which could greatly help the study of gravitational wave cosmology and relevant studies through the multi-messenger observation.
- [55] arXiv:2004.14260 [pdf, ps, other]
-
Title: Constraining the cosmological evolution of scalar-tensor theories with local measurements of the time variation of GComments: 19 pagesSubjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
We determine the conditions for which the constraints from lunar laser ranging on the time evolution of the local gravitational constant can be extrapolated to impose constraints on the time evolution of the cosmological gravitational constant in scalar-tensor theories of modified gravity. We allow for the possibility that the scalar-tensor theories are non-linear and contain a screening mechanism. This results in strong constraints on the running of the cosmological Planck mass described by the Horndeski function $|\alpha_M|\lesssim 0.002$. We find that our assumptions are valid for most Vainshtein and kinetic screening models, where the shift symmetry $\phi\rightarrow\phi + c$ holds, but are violated by some Chameleon and Symmetron screening models, where the macroscopic equivalence principle is broken.
- [56] arXiv:2004.14347 [pdf, other]
-
Title: A Machine Learning Classifier for Microlensing in Wide-Field SurveysSubjects: Instrumentation and Methods for Astrophysics (astro-ph.IM); Earth and Planetary Astrophysics (astro-ph.EP); Astrophysics of Galaxies (astro-ph.GA); Solar and Stellar Astrophysics (astro-ph.SR)
While microlensing is very rare, occurring on average once per million stars observed, current and near-future surveys are coming online with the capability of providing photometry of almost the entire visible sky to depths up to R ~ 22 mag or fainter every few days, which will contribute to the detection of black holes and exoplanets through follow-up observations of microlensing events. Based on galactic models, we can expect microlensing events across a vastly wider region of the galaxy, although the cadence of these surveys (2-3 per day ) is lower than traditional microlensing surveys, making efficient detection a challenge. Rapid advances are being made in the utility of time-series data to detect and classify transient events in real-time using very high data-rate surveys, but limited work has been published regarding the detection of microlensing events, particularly for when the data streams are of relatively low-cadence. In this research, we explore the utility of a Random Forest algorithm for identifying microlensing signals using time-series data, with the goal of creating an efficient machine learning classifier that can be applied to search for microlensing in wide-field surveys even with low-cadence data. We have applied and optimized our classifier using the OGLE-II microlensing dataset, in addition to testing with PTF/iPTF survey data and the currently operating ZTF, which applies the same data handling infrastructure that is envisioned for the upcoming LSST.
- [57] arXiv:2004.14349 [pdf, other]
-
Title: Scalar-tensor theories of gravity, neutrino physics, and the $H_0$ tensionAuthors: Mario Ballardini, Matteo Braglia, Fabio Finelli, Daniela Paoletti, Alexei A. Starobinsky, Caterina UmiltàComments: 25 pages, 12 figures, 8 tablesSubjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
We use $Planck$ 2018 data to constrain the simplest models of scalar-tensor theories characterized by a coupling to the Ricci scalar of the type $F(\sigma) R$ with $F(\sigma) = N_{pl}^2 + \xi \sigma^2$. We update our results with previous $Planck$ and BAO data releases obtaining the tightest constraints to date on the coupling parameters, that is $\xi < 5.5 \times 10^{-4}$ for $N_{pl}=0$ (induced gravity or equivalently extended Jordan-Brans-Dicke) and $(N_{pl} \sqrt{8 \pi G})-1 < 1.8 \times 10^{-5}$ for $\xi = -1/6$ (conformal coupling), both at 95% CL. Because of a modified expansion history after radiation-matter equality compared to the $\Lambda$CDM model, all these dynamical models accommodate a higher value for $H_0$ and therefore alleviate the tension between $Planck$/BAO and distance-ladder measurement from SNe Ia data from $4.4\sigma$ at best to $2.3\sigma$. We show that all these results are robust to changes in the neutrino physics. In comparison to the $\Lambda$CDM model, partial degeneracies between neutrino physics and the coupling to the Ricci scalar allow for smaller values $N_{\rm eff} \sim 2.8$, $1\sigma$ lower compared to the standard $N_{\rm eff} = 3.046$, and relax the upper limit on the neutrino mass up to 40%.
- [58] arXiv:2004.14350 [pdf, other]
-
Title: A Larger Extent for the Ophiuchus StreamAuthors: N. Caldwell (1), A. Bonaca (1), A. Price-Whelan (2), B. Sesar, M. Walker (3) ((1) CfA, (2) Princeton, (3) CMU)Comments: 17 pages, 10 figures, to appear in AJSubjects: Astrophysics of Galaxies (astro-ph.GA)
We present new kinematic data for the Ophiuchus stellar stream. Spectra have been taken of member candidates at the MMT telescope using Hectospec, Hectochelle and Binospec, which provide more than 1800 new velocities. Combined with proper motion measurements of stars in the field by the Gaia - DR2 catalog, we have derived stream membership probabilities, resulting in the detection of more than 200 likely members. These data show the stream extends to more than three times the length shown in the discovery data. A spur to the main stream is also detected. The high resolution spectra allow us to resolve the stellar velocity dispersion, found to be $1.6 \pm 0.3 $ km/sec.
- [59] arXiv:2004.14380 [pdf, other]
-
Title: Dynamics of Colombo's Top: Generating Exoplanet Obliquities from Planet-Disc InteractionsComments: 17 pages, 18 figures, 2 appendices. To be submittedSubjects: Earth and Planetary Astrophysics (astro-ph.EP)
Large planetary spin-orbit misalignments (obliquities) may strongly influence atmospheric circulation and tidal heating in the planet. A promising avenue to generate obliquities is via spin-orbit resonances, where the spin and orbital precession frequencies of the planet cross each other as the system evolves in time. One such mechanism involves a dissipating (mass-losing) protoplanetary disk that drives orbital precession of an interior planet. We study this scenario analytically in this paper, and obtain the mapping between the general initial spin orientation and the final obliquity. We show that (i) under adiabatic evolution (i.e. the disk dissipates at a sufficiently slow rate), the final planetary obliquity as a function of the initial spin orientation bifurcates into distinct tracks governed by interactions with the resonance; (ii) under nonadiabatic evolution, a broad range of obliquities can be excited. We obtain analytical expressions for the final obliquities for various regimes of parameter space. The dynamical system studied in this paper is an example of "Colombo's top", and our analysis and results can be adapted to other applications.
Cross-lists for Thu, 30 Apr 20
- [60] arXiv:2004.11681 (cross-list from physics.hist-ph) [pdf]
-
Title: The first attempts to measure light deflection by the SunComments: 8 pages, 8 figuresJournal-ref: Nature Astronomy 4 (2020) 6 9Subjects: History and Philosophy of Physics (physics.hist-ph); Solar and Stellar Astrophysics (astro-ph.SR); General Relativity and Quantum Cosmology (gr-qc)
Soon after Einstein's calculation of the effect of the Sun's gravitational field on the propagation of light in 1911, astronomers around the world tried to measure and verify the value. If the first attempts in Brazil in 1912 or Imperial Russia in 1914 had been successful, they would have proven Einstein wrong.
- [61] arXiv:2004.13186 (cross-list from cond-mat.stat-mech) [pdf, other]
-
Title: Simulations of Multi-Component Relativistic ThermalizationSubjects: Statistical Mechanics (cond-mat.stat-mech); Cosmology and Nongalactic Astrophysics (astro-ph.CO)
We report on the development and application of a multi dimensional relativistic Monte-Carlo code to explore the thermalization process in a relativistic multi-component environment. As an illustration we simulate the fully relativistic three dimensional Brownian-motion-like solution to the thermalization of a high mass particle in a bath of relativistic low-mass particles. We follow the thermalization and ultimate equilibrium distribution of the Brownian-like particle as can happen in the cosmic plasma during Big bang nucleosynthesis.
- [62] arXiv:2004.13706 (cross-list from hep-ph) [pdf, other]
-
Title: Boosting Ultraviolet Freeze-in in NO ModelsSubjects: High Energy Physics - Phenomenology (hep-ph); Cosmology and Nongalactic Astrophysics (astro-ph.CO)
We present a novel UV freeze-in mechanism for enhancing the dark matter abundance in cosmologies where inflation is followed by an epoch dominated by a fluid stiffer than radiation. In such scenarios, even a small radiation abundance, produced for instance by instantaneous preheating effects, will eventually dominate the total energy density of the Universe without the need for a complete inflaton decay. For the sake of concreteness, we focus in non-oscillatory (NO) quintessential inflation models, albeit our treatment is rather general and can be extended to other scenarios. The high temperature of the initial thermal bath together with the absence of subsequent entropy injections into the Standard Model plasma translates into a highly-effective UV DM freeze-in. In particular, we find that, during kination, an enhancement in the DM abundance is generically obtained for any production cross-section not-decreasing with temperature.
- [63] arXiv:2004.13729 (cross-list from gr-qc) [pdf, other]
-
Title: Interpreting gravitational-wave burst detections: constraining source properties without astrophysical modelsAuthors: Bence Bécsy, Peter Raffai, Kiranjyot Gill, Tyson B Littenberg, Margaret Millhouse, Marek J SzczepańczykComments: 19 pages, 4 figuresJournal-ref: Bence Becsy et al 2020 Class. Quantum Grav. 37 105011Subjects: General Relativity and Quantum Cosmology (gr-qc); High Energy Astrophysical Phenomena (astro-ph.HE)
We show that for detections of gravitational-wave transients, constraints can be given on physical parameters of the source without using any specific astrophysical models. Relying only on fundamental principles of general relativity, we can set upper limits on the size, mass, and distance of the source solely from characteristics of the observed waveform. If the distance of the source is known from independent (e.g. electromagnetic) observations, we can also set lower limits on the mass and size. As a demonstration, we tested these constraints on binary black hole signals observed by the LIGO and Virgo detectors during their first and second observing runs, as well as on simulated binary black hole and core-collapse supernova signals reconstructed from simulated detector data. We have found that our constraints are valid for all analyzed source types, but their efficiency (namely, how far they are from the true parameter values) strongly depends on the source type, ranging from being in the same order of magnitude to a several orders of magnitude difference. In cases when a gravitational-wave signal is reconstructed without waveform templates and no astrophysical model on the source is available, these constraints provide the only quantitative characterization of the source that can guide the astrophysical modeling process.
- [64] arXiv:2004.13755 (cross-list from hep-th) [pdf, other]
-
Title: Extra-Natural Inflation (De)constructedComments: 1+35 pages, 21 figure filesSubjects: High Energy Physics - Theory (hep-th); Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Physics - Phenomenology (hep-ph)
Extra-natural inflation is (de)constructed. Explicit models are compared with cosmological observations. The models successfully achieve trans-Planckian inflaton field excursions.
- [65] arXiv:2004.13782 (cross-list from gr-qc) [pdf, other]
-
Title: Common-envelope Dynamics of a Stellar-mass Black Hole: General Relativistic SimulationsComments: 16 pages, 27 figures. Accepted for publication in ApJSubjects: General Relativity and Quantum Cosmology (gr-qc); High Energy Astrophysical Phenomena (astro-ph.HE)
With the goal of providing more accurate and realistic estimates of the secular behavior of the mass accretion and drag rates in the "common-envelope" scenario encountered when a black hole or a neutron star moves in the stellar envelope of a red supergiant star, we have carried out the first general relativistic simulations of the accretion flow onto a nonrotating black hole moving supersonically in a medium with regular but different density gradients. The simulations reveal that the supersonic motion always rapidly reaches a stationary state and it produces a shock cone in the downstream part of the flow. In the absence of density gradients we recover the phenomenology already observed in the well-known Bondi--Hoyle--Lyttleton accretion problem, with super-Eddington mass accretion rate and a shock cone whose axis is stably aligned with the direction of motion. However, as the density gradient is made stronger, the accretion rate also increases and the shock cone is progressively and stably dragged toward the direction of motion. With sufficiently large gradients, the shock-cone axis can become orthogonal to the direction, or even move in the upstream region of the flow in the case of the largest density gradient. Together with the phenomenological aspects of the accretion flow, we have also quantified the rates of accretion of mass and momentum onto the black hole. Simple analytic expressions have been found for the rates of accretion of mass, momentum, drag force, and bremsstrahlung luminosity, all of which have been employed in the astrophysical modelling of the secular evolution of a binary system experiencing a common-envelope evolution...
- [66] arXiv:2004.13966 (cross-list from hep-ph) [pdf, other]
-
Title: Strongly-interacting massive particle and dark photon in the era of intensity frontierComments: 6 pages, 1 figureSubjects: High Energy Physics - Phenomenology (hep-ph); Cosmology and Nongalactic Astrophysics (astro-ph.CO)
A strongly interacting massive particle (SIMP) is an interesting candidate for dark matter (DM) because its self-interaction cross section can be naturally strong enough to address the astrophysical problem of small-scale structure formation. A simple model was proposed by assuming a monopole condensation, where composite SIMP comes from a "strongly interacting" U(1)$_{\rm d}$ gauge theory. In the original model, the DM relic abundance is determined by the $3\to2$ annihilation process via the Wess-Zumino-Witten term. In this letter, we discuss that the DM relic abundance is naturally determined also by a semi-annihilation process via a kinetic mixing between the hypercharge gauge boson and the dark U(1)$_{\rm d}$ gauge boson (dark photon). The dark photon can be discovered by LDMX-style missing momentum experiments in the near future.
- [67] arXiv:2004.14136 (cross-list from physics.ed-ph) [pdf]
-
Title: A collective insight into the cultural and academic journeys of Native Hawaiians while pursuing careers in physics and astronomyComments: Submitted to the National Academy of Sciences Decadal Survey on Astronomy and Astrophysics (Astro2020) Panel on the State of the Profession and Societal Impacts (SoP)Subjects: Physics Education (physics.ed-ph); Instrumentation and Methods for Astrophysics (astro-ph.IM)
In the field of astronomy, Maunakea is known as a prestigious site for observing and science. In Native Hawaiian culture, Maunakea is revered as the connection between past, present, and future generations and their ancestral lands of Hawai'i. We have reached a juncture at which it is necessary to allow and enable Native Hawaiians to pursue careers in astronomy, especially on Maunakea. This paper serves to tell the accounts of four Kanaka astronomers and raise awareness of the barriers they have faced while pursuing astronomy careers. The authors identify issues that the community faces due to the disconnect between astronomy and Hawai'i communities and propose resolutions to lead the way forward.
- [68] arXiv:2004.14156 (cross-list from gr-qc) [pdf, other]
-
Title: Analysis of the Topology of the Kerr MetricAuthors: Shatskiy AlexanderComments: 20 pages, 3 figuresJournal-ref: Journal of Experimental and Theoretical Physics, 2020, Vol. 130, N 3, p. 409Subjects: General Relativity and Quantum Cosmology (gr-qc); High Energy Astrophysical Phenomena (astro-ph.HE)
The equations of motion of a test particle are integrated for the field of a rotating Kerr black hole (BH). Due to the lack of analytical transformations for the Carter-Penrose diagrams (CPDs) for the Kerr metric, the topology of the Kerr BH is studied by analytical investigation of the equations of motion. Transformations for the CPDs for the Reisner-Nordstr\"om metric are analyzed. The problem of boundary conditions for the Reisner-Nordstr\"om topology is analyzed. A solution to this problem of boundary conditions is proposed. It is proved that, in the Reisner-Nordstr\"om topology, only one way to go to another universe is possible. For the Kerr topology, the possibility of the existence of an alternative transition to another universe that does not coincide with the universe for the ordinary transition is found. This alternative transition is performed through a surface with a zero radial coordinate (zero radius). Initial conditions for the falling particle are found that correspond to an alternative transition to another universe. The tidal forces acting on a falling body in the Kerr metric are estimated, and the possibility of the transition of the body to other universes without being destroyed by tidal forces is proved.
- [69] arXiv:2004.14234 (cross-list from physics.pop-ph) [pdf, other]
-
Title: The Lyapunov exponents and the neighbourhood of periodic orbitsComments: 5 pages, 1, figure. Accepted for publication in MNRASSubjects: Popular Physics (physics.pop-ph); Astrophysics of Galaxies (astro-ph.GA); Chaotic Dynamics (nlin.CD)
We show that the Lyapunov exponents of a periodic orbit can be easily obtained from the eigenvalues of the monodromy matrix. It turns out that the Lyapunov exponents of simply stable periodic orbits are all zero, simply unstable periodic orbits have only one positive Lyapunov exponent, doubly unstable periodic orbits have two different positive Lyapunov exponents and the two positive Lyapunov exponents of complex unstable periodic orbits are equal. We present a numerical example for periodic orbits in a realistic galactic potential. Moreover, the center manifold theorem allowed us to show that stable, simply unstable and doubly unstable periodic orbits are the mothers of families of, respectively, regular, partially and fully chaotic orbits in their neighbourhood.
- [70] arXiv:2004.14354 (cross-list from hep-ph) [pdf, other]
-
Title: Unveiling complex vector dark matter by magnetic fieldComments: 10 pages, 2 figuresSubjects: High Energy Physics - Phenomenology (hep-ph); High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics - Theory (hep-th)
We discuss the possibility that dark matter is made of a new complex massive vector field with a global $U(1)$-symmetry. The field interacts with the Standard Model via coupling to the gauge field of the hypercharge group. We study classical homogeneous configurations arising in the theory. Some of these configurations include magnetic components of the Standard Model electromagnetic field tensor. This opens a possibility to relate the origin of possible primordial magnetic fields to the cosmological evolution of vector dark matter condensates composed of magnetic bosons.
- [71] arXiv:2004.14377 (cross-list from nucl-th) [pdf, other]
-
Title: Mixed phase transition from hypernuclear matter to deconfined quark matter fulfilling mass-radius constraints of neutron starsComments: 19 pages, 5 figures, 2 tablesSubjects: Nuclear Theory (nucl-th); High Energy Astrophysical Phenomena (astro-ph.HE); High Energy Physics - Phenomenology (hep-ph)
A recent solution of the hyperon puzzle by a first order phase transition to color superconducting quark matter is revisited in order to replace the Maxwell construction by an interpolation method which describes a mixed phase. For the description of the hadronic phase the lowest order constrained variational method is used while for the quark phase the non local Nambu-Jona-Lasinio model with constant (model nlNJLA) and with density-dependent (model nlNJLB) parameters is employed. Applying the replacement interpolation method to both quark matter models results in a hybrid equation of state that allows a coexistence of nuclear matter, hypernuclear matter and quark matter in a mixed phase between the pure hadronic and quark phases which can also be realized in the structure of the corresponding hybrid star sequences. The predicted hybrid stars fulfill the constraints on the mass-radius relation for neutron stars obtained from recent observations.
Replacements for Thu, 30 Apr 20
- [72] arXiv:1605.02506 (replaced) [pdf, ps, other]
-
Title: Excited-state hydroxyl maser catalogue from the methanol multibeam survey -- I. Positions and VariabilityAuthors: A. Avison, L.J. Quinn, G.A. Fuller, J.L. Caswell, J.A. Green, S.L. Breen, S.P. Ellingsen, M.D. Gray, M. Pestalozzi, M. A. Thompson, M. A. VoronkovComments: 32 pages, 11 figures, 4 tables, accepted for publication in MNRAS; Typo in figure 5 caption corrected in 2nd version; Transposition error of words 'right' and 'left' in Figure 11 caption corrected in 3rd versionSubjects: Astrophysics of Galaxies (astro-ph.GA)
- [73] arXiv:1810.01995 (replaced) [pdf]
-
Title: Climate change via co2 drawdown from astrophysically initiated atmospheric ionization?Comments: Revised version to be published in the International Journal of Astrobiology. Expanded discussion of contributing processes, especially the effect of enhanced lightningSubjects: Earth and Planetary Astrophysics (astro-ph.EP); High Energy Astrophysical Phenomena (astro-ph.HE); Populations and Evolution (q-bio.PE)
- [74] arXiv:1812.03490 (replaced) [pdf, other]
-
Title: Modelling the SPARC galaxies using neo-MOND scaling relationships: the determination of distance scales and masses purely from disk dynamical dataAuthors: David RoscoeComments: 37 pages; 5 figuresSubjects: Astrophysics of Galaxies (astro-ph.GA)
- [75] arXiv:1907.11355 (replaced) [pdf, other]
-
Title: Improving Galaxy Clustering Measurements with Deep Learning: analysis of the DECaLS DR7 dataComments: 31 pages, 25 figures, accepted for publication in MNRAS. Moderate revision throughout the paper. The new version includes a quantitative evaluation of the remaining systematic effects in the DECaLS DR7 data in Summary and Discussion and in Conclusion. Pipeline available at this https URLSubjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); Instrumentation and Methods for Astrophysics (astro-ph.IM); Data Analysis, Statistics and Probability (physics.data-an)
- [76] arXiv:1909.12888 (replaced) [pdf, other]
-
Title: Cool-Core Cycles and PhoenixComments: 6 pages, 5 figures, Accepted for publication in MNRASSubjects: Astrophysics of Galaxies (astro-ph.GA); Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Astrophysical Phenomena (astro-ph.HE)
- [77] arXiv:1910.01285 (replaced) [pdf, other]
-
Title: Updated Constraints on Asteroid-Mass Primordial Black Holes as Dark MatterAuthors: Nolan Smyth, Stefano Profumo, Samuel English, Tesla Jeltema, Kevin McKinnon, Puragra GuhathakurtaComments: 8 pages, 6 figures, accepted to PRD. Moved supplemental section into main bodyJournal-ref: Phys. Rev. D 101, 063005 (2020)Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Physics - Theory (hep-th)
- [78] arXiv:1910.01651 (replaced) [pdf, other]
-
Title: On the stability of bimetric structure formationComments: 15 pages, 7 figures. v2 slight updates in accordance with the published versionJournal-ref: JCAP04(2020)046Subjects: General Relativity and Quantum Cosmology (gr-qc); Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Physics - Theory (hep-th)
- [79] arXiv:1910.04773 (replaced) [pdf, other]
-
Title: Mass Calibration of the CODEX Cluster Sample using SPIDERS Spectroscopy -- II. The X-ray Luminosity-Mass RelationAuthors: R. Capasso, J. J. Mohr, A. Saro, A. Biviano, N. Clerc, A. Finoguenov, M. Klein, S. Grandis, C. Collins, S. Damsted, C. Kirkpatrick, A. KukkolaComments: 12 pages, 8 figures, published in MNRASJournal-ref: Monthly Notices of the Royal Astronomical Society, Volume 494, Issue 2, May 2020, Pages 2736-2746Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
- [80] arXiv:1910.10927 (replaced) [pdf, other]
-
Title: Large Population of ALMA Galaxies at z>6 with Very High [OIII]88um to [CII]158um Flux Ratios: Evidence of Extremely High Ionization Parameter or PDR Deficit?Authors: Yuichi Harikane, Masami Ouchi, Akio K. Inoue, Yoshiki Matsuoka, Yoichi Tamura, Tom Bakx, Seiji Fujimoto, Kana Moriwaki, Yoshiaki Ono, Tohru Nagao, Ken-ichi Tadaki, Takashi Kojima, Takatoshi Shibuya, Eiichi Egami, Andrea Ferrara, Simona Gallerani, Takuya Hashimoto, Kotaro Kohno, Yuichi Matsuda, Hiroshi Matsuo, Andrea Pallottini, Yuma Sugahara, Livia ValliniComments: 20 pages, 18 figures, submitted to ApJSubjects: Astrophysics of Galaxies (astro-ph.GA)
- [81] arXiv:1911.06788 (replaced) [pdf, other]
-
Title: Two-component asymmetric dark matter via bound states and freeze-in decayComments: 19 pages plus appendices, 6 FiguresSubjects: High Energy Physics - Phenomenology (hep-ph); Cosmology and Nongalactic Astrophysics (astro-ph.CO)
- [82] arXiv:1911.07838 (replaced) [pdf, other]
-
Title: Dynamical evolution of axion condensates under stimulated decays into photonsAuthors: Pierluca Carenza (Bari U. & INFN Bari), Alessandro Mirizzi (Bari U. & INFN Bari), Günter Sigl (II Inst. Theor. Phys., Hamburg U.)Comments: 15 pages, 3 pdf figures. v2: 17 pages, 3 figures. Discussion enlarged. Added Appendix on axion instability in the expanding Universe. Matches the version accepted on PRDSubjects: High Energy Physics - Phenomenology (hep-ph); Cosmology and Nongalactic Astrophysics (astro-ph.CO)
- [83] arXiv:1912.03262 (replaced) [pdf, other]
-
Title: CODEX clusters. The Survey, the Catalog, and Cosmology of the X-ray Luminosity FunctionAuthors: A. Finoguenov, E. Rykoff, N. Clerc, M. Costanzi, S. Hagstotz, J. Ider Chitham, K. Kiiveri, C. C. Kirkpatrick, R. Capasso, J. Comparat, S. Damsted, R. Dupke, G. Erfanianfar, J. Patrick Henry, F. Kaefer, J-P. Kneib, V. Lindholm, E. Rozo, L. van Waerbeke, J. WellerComments: 10 pages, 11 figures, A&A in press, part of SDSS DR16 data releaseSubjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
- [84] arXiv:1912.03301 (replaced) [pdf, other]
-
Title: Two Ultra-Faint Milky Way Stellar Systems Discovered in Early Data from the DECam Local Volume Exploration SurveyAuthors: S. Mau, W. Cerny, A. B. Pace, Y. Choi, A. Drlica-Wagner, L. Santana-Silva, A. H. Riley, D. Erkal, G. S. Stringfellow, M. Adamów, J. L. Carlin, R. A. Gruendl, D. Hernandez-Lang, N. Kuropatkin, T. S. Li, C. E. Martínez-Vázquez, E. Morganson, B. Mutlu-Pakdil, E. H. Neilsen, D. L. Nidever, K. A. G. Olsen, D. J. Sand, E. J. Tollerud, D. L. Tucker, B. Yanny, A. Zenteno, S. Allam, W. A. Barkhouse, K. Bechtol, E. F. Bell, P. Balaji, D. Crnojević, J. Esteves, P. S. Ferguson, C. Gallart, A. K. Hughes, D. J. James, P. Jethwa, L. C. Johnson, K. Kuehn, S. Majewski, Y.-Y. Mao, P. Massana, M. McNanna, A. Monachesi, E. O. Nadler, N. E. D. Noël, A. Palmese, F. Paz-Chinchon, A. Pieres, J. Sanchez, N. Shipp, J. D. Simon, M. Soares-Santos, K. Tavangar, R. P. van der Marel, A. K. Vivas, et al. (2 additional authors not shown)Comments: 17 pages, 6 figures, 1 table; updated to match published versionJournal-ref: ApJ 890 2 (2020)Subjects: Astrophysics of Galaxies (astro-ph.GA)
- [85] arXiv:1912.04839 (replaced) [pdf, ps, other]
-
Title: Homogeneous Analysis of Globular Clusters from the APOGEE Survey with the BACCHUS Code. II. The Southern Clusters and OverviewAuthors: Szabolcs Mészáros, Thomas Masseron, D. A. García-Hernández, Carlos Allende Prieto, Timothy C. Beers, Dmitry Bizyaev, Drew Chojnowski, Roger E. Cohen, Katia Cunha, Flavia Dell'Agli, Garrett Ebelke, José G. Fernández-Trincado, Peter Frinchaboy, Doug Geisler, Sten Hasselquist, Fred Hearty, Jon Holtzman, Jennifer Johnson, Richard R. Lane, Ivan Lacerna, Penelopé Longa-Peña, Steven R. Majewski, Sarah L. Martell, Dante Minniti, David Nataf, David L. Nidever, Kaike Pan, Ricardo P. Schiavon, Matthew Shetrone, Verne V. Smith, Jennifer S. Sobeck, Guy S. Stringfellow, László Szigeti, Baitian Tang, John C. Wilson, Olga ZamoraComments: Published in MNRAS, 31 pages, 24 figures, 7 tables. Further typos are corrected, now identical in text, figures and tables to the published paperSubjects: Solar and Stellar Astrophysics (astro-ph.SR); Astrophysics of Galaxies (astro-ph.GA)
- [86] arXiv:2002.02961 (replaced) [pdf, other]
-
Title: From the Inner to Outer Milky Way: A Photometric Sample of 2.6 Million Red Clump StarsComments: 18 pages, 13 figures, 2 tables, submitted to MNRASSubjects: Solar and Stellar Astrophysics (astro-ph.SR); Astrophysics of Galaxies (astro-ph.GA)
- [87] arXiv:2002.04300 (replaced) [pdf, other]
-
Title: Shapes of stellar activity cyclesComments: Accepted to A&A; 12 pages, 12 figuresSubjects: Solar and Stellar Astrophysics (astro-ph.SR)
- [88] arXiv:2002.10357 (replaced) [pdf, other]
-
Title: Magnetic field configurations in neutron stars from MHD simulationsComments: Accepted for publication in MNRASSubjects: High Energy Astrophysical Phenomena (astro-ph.HE); Solar and Stellar Astrophysics (astro-ph.SR); General Relativity and Quantum Cosmology (gr-qc)
- [89] arXiv:2003.03596 (replaced) [pdf, other]
-
Title: Possible periodic activity in the repeating FRB 121102Authors: K. M. Rajwade, M. B. Mickaliger, B. W. Stappers, V. Morello, D. Agarwal, C. G. Bassa, R. P. Breton, M. Caleb, A. Karastergiou, E. F. Keane, D. R. LorimerComments: 9 pages, 6 Figures, 3 Tables. More detections added to the periodicity search. Updated period and activity period. Complete tables (Table 1 and Table 3) have been submitted as online supplementary materialsSubjects: High Energy Astrophysical Phenomena (astro-ph.HE)
- [90] arXiv:2003.10672 (replaced) [pdf, other]
-
Title: Frequency-Dependent Squeezed Vacuum Source for Broadband Quantum Noise Reduction in Advanced Gravitational-Wave DetectorsAuthors: Yuhang Zhao, Naoki Aritomi, Eleonora Capocasa, Matteo Leonardi, Marc Eisenmann, Yuefan Guo, Eleonora Polini, Akihiro Tomura, Koji Arai, Yoichi Aso, Yao-Chin Huang, Ray-Kuang Lee, Harald Lück, Osamu Miyakawa, Pierre Prat, Ayaka Shoda, Matteo Tacca, Ryutaro Takahashi, Henning Vahlbruch, Marco Vardaro, Chien-Ming Wu, Matteo Barsuglia, Raffaele FlaminioJournal-ref: Phys. Rev. Lett. 124, 171101 (2020)Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM); Instrumentation and Detectors (physics.ins-det)
- [91] arXiv:2004.01721 (replaced) [pdf, other]
-
Title: A joint SZ-Xray-optical analysis of the dynamical state of 288 massive galaxy clustersAuthors: A. Zenteno, D. Hernández-Lang, M. Klein, C. Vergara Cervantes, D. L. Hollowood, S. Bhargava, A. Palmese, V. Strazzullo, A. K. Romer, J. J. Mohr, T. Jeltema, A. Saro, C. Lidman, D. Gruen, V. Ojeda, A. Katzenberger, M. Aguena, S. Allam, S. Avila, M. Bayliss, E. Bertin, D. Brooks, E. Buckley-Geer, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, M. Costanzi, L. N. da Costa, J. De Vicente, S. Desai, H. T. Diehl, P. Doel, T. F. Eifler, A. E. Evrard, B. Flaugher, B. Floyd, P. Fosalba, J. Frieman, J. García-Bellido, D. W. Gerdes, J.R. Gonzalez, R. A. Gruendl, J. Gschwend, G. Gutierrez, W. G. Hartley, S. R. Hinton, K. Honscheid, D. J. James, K. Kuehn, O. Lahav, M. Lima, M. A. G. Maia, M. March, M. McDonald, P. Melchior, F. Menanteau, R. Miquel, R. L. C. Ogando, et al. (18 additional authors not shown)Comments: 21 pages, 12 Figures, 4 Tables. Accepted for publication in MNRASSubjects: Astrophysics of Galaxies (astro-ph.GA); Cosmology and Nongalactic Astrophysics (astro-ph.CO)
- [92] arXiv:2004.03135 (replaced) [pdf, other]
-
Title: GW Ori: Interactions Between a Triple-star System and its Circumtriple Disk in ActionAuthors: Jiaqing Bi, Nienke van der Marel, Ruobing Dong, Takayuki Muto, Rebecca G. Martin, Jeremy L. Smallwood, Jun Hashimoto, Hauyu Baobab Liu, Hideko Nomura, Yasuhiro Hasegawa, Michihiro Takami, Mihoko Konishi, Munetake Momose, Kazuhiro D. Kanagawa, Akimasa Kataoka, Tomohiro Ono, Michael L. Sitko, Sanemichi Z. Takahashi, Kengo Tomida, Takashi TsukagoshiComments: 17 pages, 3+3 figures, 2 tables; accepted by ApJL on 2020-04-29Subjects: Solar and Stellar Astrophysics (astro-ph.SR); Earth and Planetary Astrophysics (astro-ph.EP); Astrophysics of Galaxies (astro-ph.GA)
- [93] arXiv:2004.03824 (replaced) [pdf, other]
-
Title: X-ray variability analysis of a large series of XMM-Newton + NuSTAR observations of NGC 3227Comments: Accepted for publication in MNRAS; 19 pages, 13 figures, 4 tables; minor typographical errors corrected and reference list updatedSubjects: High Energy Astrophysical Phenomena (astro-ph.HE)
- [94] arXiv:2004.04506 (replaced) [pdf, ps, other]
-
Title: Crossing the Big Bang singularityAuthors: C. WetterichComments: new references,10 pagesSubjects: General Relativity and Quantum Cosmology (gr-qc); Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Physics - Theory (hep-th)
- [95] arXiv:2004.06728 (replaced) [pdf, other]
-
Title: The Massive and Distant Clusters of WISE Survey: SZ effect Verification with the Atacama Compact Array -- Localization and Cluster AnalysisAuthors: Luca Di Mascolo, Tony Mroczkowski, Eugene Churazov, Emily Moravec, Mark Brodwin, Anthony Gonzalez, Bandon B. Decker, Peter R. M. Eisenhardt, Spencer A. Stanford, Daniel Stern, Rashid Sunyaev, Dominika WylezalekComments: 19 pages (including appendices), 14 figures, and 4 tables; accepted for publication in A&ASubjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
- [96] arXiv:2004.06984 (replaced) [pdf, other]
-
Title: Broadband Electrical Action Sensing Techniques with conducting wires for low-mass dark matter axion detectionSubjects: Instrumentation and Detectors (physics.ins-det); Instrumentation and Methods for Astrophysics (astro-ph.IM); General Relativity and Quantum Cosmology (gr-qc); High Energy Physics - Experiment (hep-ex)
- [97] arXiv:2004.07744 (replaced) [pdf, other]
-
Title: Direct Astrophysical Tests of Chiral Effective Field Theory at Supranuclear DensitiesSubjects: High Energy Astrophysical Phenomena (astro-ph.HE); Nuclear Theory (nucl-th)
- [98] arXiv:2004.09288 (replaced) [pdf, other]
-
Title: An alternative interpretation of GW190412 as a binary black hole merger with a rapidly spinning secondaryComments: Updating to version accepted by ApJ LettersSubjects: High Energy Astrophysical Phenomena (astro-ph.HE); Solar and Stellar Astrophysics (astro-ph.SR); General Relativity and Quantum Cosmology (gr-qc)
- [99] arXiv:2004.10767 (replaced) [pdf, other]
-
Title: TESS unveils the phase curve of WASP-33b. Characterization of the planetary atmosphere and the pulsations from the starAuthors: C. von Essen, M. Mallonn, C. C. Borre, V. Antoci, K.G. Stassun, S. Khalafinejad, G. TautvaivsieneComments: 19 pages, 15 figuresSubjects: Earth and Planetary Astrophysics (astro-ph.EP); Solar and Stellar Astrophysics (astro-ph.SR)
- [100] arXiv:2004.11688 (replaced) [pdf, ps, other]
-
Title: Rotation Curve of the Milky Way and the Dark Matter DensityAuthors: Yoshiaki SofueComments: Invited review to appear in Galaxies, 28 pages, 4 figures, 8 tablesSubjects: Astrophysics of Galaxies (astro-ph.GA)
- [101] arXiv:2004.12907 (replaced) [pdf, other]
-
Title: Photometric Limits on the High Resolution Imaging of Exoplanets Using the Solar Gravity LensAuthors: Phil A. Willems (Jet Propulsion Laboratory, California Institute of Technology)Journal-ref: Acta Astronautica vol. 152, pp. 408-414 (2018)Subjects: Instrumentation and Methods for Astrophysics (astro-ph.IM); Earth and Planetary Astrophysics (astro-ph.EP); Solar and Stellar Astrophysics (astro-ph.SR); General Relativity and Quantum Cosmology (gr-qc)
[ showing up to 2000 entries per page: fewer | more ]
Disable MathJax (What is MathJax?)
Links to: arXiv, form interface, find, astro-ph, recent, 2004, contact, help (Access key information)