6 research outputs found

    Model-based cross-correlation search for gravitational waves from the low-mass X-ray binary Scorpius X-1 in LIGO O3 data

    Get PDF

    CALIFA, the Calar Alto Legacy Integral Field Area survey: IV. Third public data release

    Get PDF
    This paper describes the third public data release (DR3) of the Calar Alto Legacy Integral Field Area (CALIFA) survey. Science-grade quality data for 667 galaxies are made public, including the 200 galaxies of the second public data release (DR2). Data were obtained with the integral-field spectrograph PMAS/PPak mounted on the 3.5 m telescope at the Calar Alto Observatory. Three different spectral setups are available: i) a low-resolution V500 setup covering the wavelength range 3745-7500 Å (4240-7140 Å unvignetted) with a spectral resolution of 6.0 Å (FWHM) for 646 galaxies, ii) a medium-resolution V1200 setup covering the wavelength range 3650-4840 Å (3650-4620 Å unvignetted) with a spectral resolution of 2.3 Å (FWHM) for 484 galaxies, and iii) the combination of the cubes from both setups (called COMBO) with a spectral resolution of 6.0 Å and a wavelength range between 3700-7500 Å (3700-7140 Å unvignetted) for 446 galaxies. The Main Sample, selected and observed according to the CALIFA survey strategy covers a redshift range between 0.005 and 0.03, spans the color-magnitude diagram and probes a wide range of stellar masses, ionization conditions, and morphological types. The Extension Sample covers several types of galaxies that are rare in the overall galaxy population and are therefore not numerous or absent in the CALIFA Main Sample. All the cubes in the data release were processed using the latest pipeline, which includes improved versions of the calibration frames and an even further improved image reconstruction quality. In total, the third data release contains 1576 datacubes, including ~1.5 million independent spectra.Fil: Sánchez, S. F.. Universidad Nacional Autónoma de México; MéxicoFil: Garciá Benito, R.. Instituto de Astrofísica de Andalucía; EspañaFil: Zibetti, S.. Osservatorio Astrofisico di Arcetri; ItaliaFil: Walcher, C. J.. Leibniz-Institut für Astrophysik Potsdam; AlemaniaFil: Husemann, B.. European Southern Observatory; AlemaniaFil: Mast, Damian. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; ArgentinaFil: López Fernández, R.. Instituto de Astrofísica de Andalucía; EspañaFil: López Sánchez, A. R.. Sydney Institute for Astronomy; AustraliaFil: Lyubenova, M.. University of Groningen. Kapteyn Astronomical Institute; Países BajosFil: Marino, R.. Institut für Astronomie; SuizaFil: Márquez, I.. Instituto de Astrofísica de Andalucía; EspañaFil: Mendez Abreu, J.. University of St. Andrews. School of Physics and Astronomy; Reino UnidoFil: Mollá, M.. Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas; EspañaFil: Monreal Ibero, A.. Université Paris Diderot. Observatoire de Paris; FranciaFil: Ortega Minakata, R.. Universidade Federal do Rio de Janeiro. Observatorio do Valongo; BrasilFil: Torres Papaqui, J. P.. Universidad de Guanajuato. Departamento de Astronomía; MéxicoFil: Pérez, E.. Instituto de Astrofísica de Andalucía; EspañaFil: Rosales Ortega, F. F.. Instituto Nacional de Astrofísica, Óptica y Electrónica; MéxicoFil: Roth, M. M.. Leibniz-Institut für Astrophysik Potsdam; AlemaniaFil: Sánchez Blázquez, P.. Universidad Autónoma de Madrid. Facultad de Ciencias. Departamento de Física Teórica; EspañaFil: Schilling, U.. Ruhr-Universität Bochum. Astronomisches Institut; AlemaniaFil: Spekkens, K.. Royal Military College of Canada. Department of Physics; CanadáFil: Vale Asari, N.. Universidade Federal de Santa Catarina. Departamento de Física; BrasilFil: Van Den Bosch, R. C. E.. Max-Planck-Institut für Astronomie; AlemaniaFil: Van De Ven, G.. Max-Planck-Institut für Astronomie; AlemaniaFil: Vilchez, J. M.. Instituto de Astrofísica de Andalucía; EspañaFil: Wild, V.. University of St. Andrews. School of Physics and Astronomy; Reino UnidoFil: Wisotzki, L.. Leibniz-Institut für Astrophysik Potsdam; AlemaniaFil: Ylldlrlm, A.. Max-Planck-Institut für Astronomie; AlemaniaFil: Ziegler, B.. Department of Astrophysics. University of Vienna; Austri

    Factors Influencing Phenolic Compounds in Table Olives (Olea europaea)

    No full text

    GW190425: Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M o

    Get PDF
    On 2019 April 25, the LIGO Livingston detector observed a compact binary coalescence with signal-to-noise ratio 12.9. The Virgo detector was also taking data that did not contribute to detection due to a low signal-to-noise ratio, but were used for subsequent parameter estimation. The 90% credible intervals for the component masses range from to if we restrict the dimensionless component spin magnitudes to be smaller than 0.05). These mass parameters are consistent with the individual binary components being neutron stars. However, both the source-frame chirp mass and the total mass of this system are significantly larger than those of any other known binary neutron star (BNS) system. The possibility that one or both binary components of the system are black holes cannot be ruled out from gravitational-wave data. We discuss possible origins of the system based on its inconsistency with the known Galactic BNS population. Under the assumption that the signal was produced by a BNS coalescence, the local rate of neutron star mergers is updated to 250-2810. © 2020. The Author(s). Published by the American Astronomical Society.

    Search for gravitational waves associated with fast radio bursts detected by CHIME/FRB during the LIGO-Virgo observing run O3a

    No full text
    We search for gravitational-wave (GW) transients associated with fast radio bursts (FRBs) detected by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst Project, during the first part of the third observing run of Advanced LIGO and Advanced Virgo (2019 April 1 15:00 UTC–2019 October 1 15:00 UTC). Triggers from 22 FRBs were analyzed with a search that targets both binary neutron star (BNS) and neutron star– black hole (NSBH) mergers. A targeted search for generic GW transients was conducted on 40 FRBs. We find no significant evidence for a GW association in either search. Given the large uncertainties in the distances of our FRB sample, we are unable to exclude the possibility of a GW association. Assessing the volumetric event rates of both FRB and binary mergers, an association is limited to 15% of the FRB population for BNS mergers or 1% for NSBH mergers. We report 90% confidence lower bounds on the distance to each FRB for a range of GW progenitor models and set upper limits on the energy emitted through GWs for a range of emission scenarios. We find values of order 1051–1057 erg for models with central GW frequencies in the range 70–3560 Hz. At the sensitivity of this search, we find these limits to be above the predicted GW emissions for the models considered. We also find no significant coincident detection of GWs with the repeater, FRB 20200120E, which is the closest known extragalactic FRB
    corecore