adsabs/WIESP2022-NER huggingface dataset:
Paper: 2016ApJ...831..165V (acknowledgments)
This research was conducted as part of the Cerro Tololo Inter-American Observatory REU Program, which is supported by the National Science Foundation under grant AST-1062976 respectively. R.Z. acknowledges support from NSF grant AST-1108948. Support for S.D. is provided by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. This research is based in part on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministrio da Cincia, Tecnologia, e Inovao (MCTI) da Republica Federativa do Brasil, the US National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). It is also partly based on observations at Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the participating institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/ . SDSS-III is managed by the Astrophysical Research Consortium for the participating institutions of the SDSS-III Collaboration, including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, the University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, the Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. We thank the anonymous referee for useful comments. Facilities: WIYN (Hydra) , SOAR . Software: IRAF, Topcat.
Paper: 2019ApJ...881..139S (fulltext)
late times based on sophisticated simulations is presented in Mirizzi et al. ( 2016 ). In these studies the initial conditions have been prepared using other supernova models, thereby separating the PNS cooling from the explosion mechanism. In order to explore the connection between progenitors and compact objects using the neutrino signal, it is essential to study the long-term neutrino emission starting from the initial stellar model and include the thermal evolution of the PNS born in the resulting explosion. Evolution from the supernova explosion to the formation of a neutron star has been studied in 1D (Totani et al. 1998 ; Hüdepohl et al. 2010 ; Fischer et al. 2010 ) for selected progenitors and to a limited extent in 2D (Suwa 2014 ). 11 11 See Nakamura et al. ( 2015 ) and Horiuchi et al. ( 2018 ) for limitations of these models. Neutrino light curves in the 1D models by Totani et al. ( 1998 ) and Dalhed et al. ( 1999 ) have been routinely used to evaluate the total event number at neutrino detectors (see also Mirizzi et al. 2016 ). Due to limitations in the ability of these predictions and their focus on explosion dynamics, the expected number of neutrino events at underground neutrino detectors such as IceCube (Tamborra et al. 2013 ), Super-Kamiokande (Ikeda et al. 2007 ), and Hyper-Kamiokande (Abe et al. 2011 ; Hyper-Kamiokande Proto-Collaboration et al. 2018 ) has been estimated only for the dynamical phase using various models and numerical simulations to discuss these detectors’ ability to probe the physics of the supernova. As a result, the long-term behavior of the neutrino burst from the PNS has not been studied in detail with modern simulations covering a variety of progenitors. Our first aim in the current study is, therefore, to predict the basic features of the expected number of events at Super-Kamiokande for the full time sequence of supernova models. We utilize neutrino emission properties from a supernova neutrino database (Nakazato et al. 2013 ), which covers the complete dynamical evolution of the event from gravitational collapse to the cooling of the PNS. Through comparisons of event numbers for a set of progenitors systematically obtained from neutrino-radiation hydrodynamics (RHD) and PNS cooling simulations, we explore the differences in neutrino signals among models based on different progenitors. We discuss the time profile of the event rate for both early times around the bounce and the later phases of PNSs. We estimate the basic features of the event rate evolution for various models to assess whether one can extract information on the progenitor from future observations of a supernova neutrino burst. This is an important step in discussing the possibility of studying the progenitor’s mass, metallicity, and explosion timing, for instance, immediately after detection at Super-Kamiokande. Our second aim is to demonstrate the importance of the late phase of supernova neutrino emission. We study the long-term
Paper: 2021MNRAS.503.3759B (fulltext)
−1 . Observations of BG Ind were obtained simultaneously in two cameras on WASP-South over three observing seasons, from 2012 July 3 to 2014 December 6. Fluxes are measured in an aperture with a radius of 132 arcsec for the 85-mm data and instrumental trends are removed using the SYSRem algorithm (Tamuz, Mazeh Zucker 2005 ). Data points more than 5 standard deviations from a phase-binned version of the light curve were rejected and the entire night of data was rejected if more than one-fourth of the observations were identified as outliers based on this criterion. An 8-d section of the WASP measurements is shown in Fig. 2 . Note, we converted the original HJD(UTC) times of the WASP observations into BJD(TDT) for the forthcoming analyses. We also applied the same transformations for all the archival data that we describe below. Figure 2. An 8-d-long section of the WASP observations of BG Ind (blue circles). Red dots represent the best-fitting spectro-photodynamical model solution (see later, in Section 3 ) projected back to the epoch of each individual WASP measurement, while the black line shows the evenly phased model solution. The residuals curve is also shown below. 2.4 Other ground-based archive photometric data used for our analysis We downloaded publicly available Strömgren u, v, b, y photometric observations from the ESO archive (Manfroid et al. 1991 ; Sterken et al. 1993 ). These observations were carried out between JDs 2 446 581 and 2 447 069. The light curves in each bandpass contain 175 measurements. We used these data primarily to determine additional times of eclipses in binary A. Unfortunately, however, the majority of the nightly observations contain only a few measurements, and we were therefore able to determine the mid-times of only two primary eclipses (see below, in Section 2.6 ) from this data set. BG Ind was also observed by Jens Viggo Clausen and collaborators as part of their long-running observing programme to measure absolute dimensions for solar-type stars in eclipsing binaries, carried out since 1994 at the Strömgren Automatic Telescope at ESO, La Silla. Unpublished data and manuscripts that were in preparation from this observing programme have been made available to one of us (PM), from which we extracted five more eclipse times (see again, in Section 2.6 ). The observing procedures and data reduction for these observations are similar to those described in Clausen, Helt Olsen ( 2001 ). 2.5 Disentanglement of the light curves For the combined analysis of all the observational data, we used the original TESS time-series, i.e. the net light curve of the two binaries together. However, at the start of the analysis, we found it worthwhile to disentangle the light curves of the two binaries, so we could examine each one separately. We have described this process in substantial detail in Powell et al. ( 2021 ). Therefore, we review only the highlights here. First, we folded and binned the Sector 1 (i.e. Year 1) TESS SAP
Paper: 2016A&A...588A..48C (acknowledgments)
Laurent Chemin acknowledges the financial support from CNES. We are grateful to an anonymous referee whose suggestions led to clarify the discussion, content, and structure of the manuscript. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration ( http://ned.ipac.caltech.edu ). We acknowledge the usage of the HyperLeda database ( leda.univ-lyon1.fr ). The SDSS image is from cosmo.nyu.edu/hogg/rc3 , prepared by David W. Hogg, Michael R. Blanton, and the Sloan Digital Sky Survey Collaboration.
Paper: 2017MNRAS.470.1570H (fulltext)
observations for a sample of 14 luminous nearby QSO host galaxies that we interpret in conjunction with the available optical integral field observations. This data set significantly extends the sample of luminous unobscured QSOs with molecular gas mass estimates at low redshift. Our main results of this work can be summarized as follows: We detect the 12 CO(1–0) emission line in 8 of 14 targets (∼60 per cent) with a clear preference for disc-dominated and major merger systems with a detection rate of nearly 80 per cent. The integrated 12 CO(1–0) emission line matches the spatially integrated Hα line profile, indicating that both are tracing star formation regions when averaged over kpc scales. We also detect the 12 CO(2–1) emission line in 7 of 11 targets (∼60 per cent). The corresponding r 21 brightness temperature ratio is close to 1 and ranges between 0.5 and 1.3. Some of the lowest ratios may suggest that the CO emission is already sub-thermal at J = 2 in these systems. While the disc-dominated QSO host galaxies exhibit similar gas fractions and gas depletion time-scales compared to non-AGN host galaxies, we find that bulge-dominated QSO hosts have systematically smaller gas fractions but shorter gas depletion times, given their elevated SFRs. The two major mergers in our sample show high gas fractions and rather short gas depletion times as expected from simulations for strongly interacting systems. We report a positive correlation between BH accretion rate and total molecular gas mass for disc-dominated QSO host galaxies after combining our sample with literature data. We interpret this as an upper limit of BH accretion rate, given our initial selection for the most luminous QSO at the considered redshift. We can explain this trend using a simply toy model that links the circumnuclear gas surface density with the total gas mass through a simple scaling relation for discs. The BH accretion rate in bulge-dominated QSOs host galaxies is significantly higher given their molecular gas content compared to disc-dominated QSOs hosts. This may be explained either by a more compact or steeper gas surface density gradient, by removal of the outer envelope of gas through feedback or by a significantly higher gas temperature, leading to a different composition of the different phases of ISM. While we did not measure a higher CO line excitation based on the r 21 temperature brightness ratio, this needs to be investigated with more excitation-sensitive observations. Despite the relatively small sample size of this study, we can confirm that the molecular gas content and star formation efficiency, at least in disc-dominated QSO hosts and major mergers, are indistinguishable from the corresponding population of non-AGN galaxies. Negative AGN feedback that either reduces the star formation efficiency or significantly lowers the cold gas content through galactic outflows is an implausible scenario for the majority of QSO hosts studied in this work.
Paper: 2020MNRAS.497..976K (fulltext)
spectral line, which is used to derive the information of the magnetic fields. In addition, Qiu Gary ( 2003 ) discussed the possibility of change in line profiles during a transient polarity reversal observed in the photospheric magnetic field measurements obtained from the MDI instrument aboard SOHO space mission. Wang ( 1992 ) and Wang et al. ( 1994 , 2002 ) reported abrupt and permanent changes in the evolution of magnetic fields in the flaring region during the different class of solar flares using the data from Big Bear Solar Observatory. Later on, extensive analysis done by Sudol Harvey ( 2005 ) and Petrie Sudol ( 2010 ) of X- and M-class solar flares using the line-of-sight (i.e. longitudinal) magnetic fields obtained from Global Oscillation Network Group (GONG; Harvey et al. 1996 ) instruments, showed abrupt and permanent changes in the magnetic fields in the flaring locations within 10-min duration with a median magnitude of 100 G. In addition, Kumar et al. ( 2016 ) also found abrupt and persistent changes in line-of-sight magnetic fields at different locations in active region during an M6.5 class solar flare using the data from Helioseismic and Magnetic Imager (HMI; Schou et al. 2012 ) instrument aboard the Solar Dynamics Observatory ( SDO ; Pesnell, Thompson Chamberlin 2012 ) space mission. Hudson et al. ( 2008 ) and Fisher et al. ( 2012 ) proposed that abrupt changes in the magnetic fields can lead to an impulsive change in Lorentz force, which is also known as ‘magnetic-jerk’, and this can induce seismic emission in the sunspots. However, Raja Bayanna et al. ( 2014 ) observed distortions in the two circular polarization states of light, the left (LCP) and the right circular polarization (RCP) observations in the flaring locations which showed transient changes in Doppler velocity and line-of-sight magnetic fields during an X-class flare, using the line profile observations from HMI instrument aboard the SDO space mission. They showed that observed transient changes in Doppler velocity and line-of-sight magnetic fields in flaring locations are prone to artefacts in the measurements. Therefore, in this paper, we present a detailed analysis of seismic emission in the sunspots, which are away from the flare ribbons and hard X-ray footpoints accompanying large solar flares. Such acoustic enhancements are supposed to be free from any flare related problems in the observational data. In the following sections, we first describe the observational data and selection criteria for choosing the active regions aimed for our analysis. This is followed by methods of analysis and the results obtained. We finally conclude with discussions concerning our results. 2 THE OBSERVATIONAL DATA We have extensively used observations from the HMI instrument aboard the SDO spacecraft, which is a solar space mission of the National Aeronautics and Space Administration (NASA). The HMI instrument observes the photosphere of the Sun in Fe i 6173 Å absorption
Paper: 2019A&A...623L..11G (acknowledgments)
GRAVITY was developed via a collaboration of the Max Planck Institute for Extraterrestrial Physics, LESIA of Paris Observatory and IPAG of Université Grenoble Alpes/CNRS, the Max Planck Institute for Astronomy, the University of Cologne, the Centro Multidisciplinar de Astrofisica Lisbon and Porto, and the European Southern Observatory. Part of this work was supported by the European Union under ERC grant 639248 LITHIUM. J.W. is supported by the Heising-Simons Foundation 51 Pegasi b postdoctoral fellowship. A.A., P.G., and N.A. acknowledge funding from Fundação para a Ciência e Tecnologia through grants PTDC/CTE-AST/116561/2010, SFRH/BD/52066/2012, COMPETE FCOMP-01-0124-FEDER-019965, UID/FIS/00099/2013, and SFRH/BSAB/142940/2018. R.G.L. acknowledges funding by H2020 Marie Curie fellowship 706320.
Paper: 2019MNRAS.485.3715B (acknowledgments)
ACKNOWLEDGEMENTS We thank the anonymous referee for useful comments and Pierre Bergeron for helpful discussions. The work of DMB, AVK, and DAZ (Sections 2 and 3 ) was supported by the Russian Foundation for Basic Research, project No. 18-32-00781 mol_a. AYuK and SVZ acknowledge PAPIIT grant IN-100617 for resources provided towards this research. The work is based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma. iraf is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. DAZ thanks Pirinem School of Theoretical Physics for hospitality.
Paper: 2019ApJ...879...24S (acknowledgments)
The authors thank Jacob Heerikhuisen for sharing the model of the heliosphere that allowed them to assess the distance to the heliospheric termination shock, and Charles Smith for encouraging them to publish the first ideas of the study developed here. J.M.S. thanks Marcin Szpanko for the help with preparation of Figure 17 and Duncan Pettengill (Wolfram Technology Group) for technical support with Wolfram Research Mathematica software. The presented study is supported by the Polish National Science Center grant No. 2015/19/B/ST9/01328.
Paper: 2018A&A...611A..53J (acknowledgments)
Acknowledgements We thank the referee for helpful comments and multiple suggestions that significantly improved this paper. This work is part of a thesis co-funded by the University Aix-Marseille and the Centre National d’Études Spatiales (CNES) in the context of the upcoming Euclid mission of the European Space Agency, as developed by the Euclid Consortium. The authorswould like to thank the members of the AMAZED team who provided helpful feedback and insightful discussions on this topic. This work benefitted from access to databases managed by the CESAM (Astrophysical Data Center of Marseille) in LAM (Laboratoire d’Astrophysique de Marseille). We would also like to express our thanks to all the contributors whose fruitful comments and revision of this manuscript helped us expand our understanding and improve the paper.
Paper: 2016MNRAS.458.2476S (acknowledgments)
This work is based on observations made with ESO telescopes at the La Silla Paranal Observatory under programs 74.C-0209(A), 75.C-0014(A) and 91.C-0768(A). We would like to thank the anonymous referee for their comments, Casey Deen for performing the CRIRES observations and reading the manuscript, Chris Koresko for providing Keck/NIRC photometry, Hongchi Wang for helpful analysis of NACO photometry, and Peter Abraham for helpful discussions. This research was funded under Deutsche Forschungsgemeinschaft (DFG) programme nos. WO 857/10-1 and WO 857/13-1. CFM gratefully acknowledges an ESA Research Fellowship. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica.
Paper: 2017ApJ...847L..10M (fulltext)
by supergiant shells. Simulations of supernova-driven turbulence in a representative section of a stratified galactic disk by Joung Mac Low ( 2006 ) came to a similar conclusion. Neglecting the action of self-gravity on the gas, they found that only 10% as much gas was swept up into regions able to gravitationally collapse as would have been required to maintain the star formation rate implied by the input supernova rate. 3. Toomre Instability Therefore, we now turn to large-scale gravitational instability in disks (Safronov 1960 ; Toomre 1964 ; Goldreich Lynden-Bell 1965 ), which offers an alternative mechanism to assemble gas dense enough to form molecules. Galactic dynamics appears to be driven by such instabilities, which at the largest scales drive spiral arm formation (Agertz et al. 2009 ; Wada et al. 2011 ). When these instabilities grow strongly enough because of gas infall or galaxy mergers they lead to the formation of giant clumps (Li et al. 2005 ) in what is called violent disk instability (Agertz et al. 2009 ; Dekel et al. 2009 ). (Those clumps may well themselves collapse into clusters of small clumps as shown by Behrendt et al. 2016 .) That molecular clouds can form more quickly by gravitational instability than collisional agglomeration was shown by Elmegreen ( 1990 ), despite their apparently having the same dependences on density and velocity dispersion. The Toomre instability criterion for gaseous disks (Goldreich Lynden-Bell 1965 ) iswhere Σ g is the surface density of the gas, σ g is its velocity dispersion including both thermal and nonthermal components, G is the gravitational constant, and κ 2 = −4 ωB is the square of the epicyclic frequency, with Oort’s constantIn a galaxy with a flat rotation curve, the second term in B can be neglected. In this case, , so that . The timescale for growth of a perturbation in an isothermal gas disk can be expressed in terms of Q g as (Wang Silk 1994 )At the solar circle, with r = 8 kpc, the rotational velocity ωr = 220 km s −1 , dropping only slowly to 170 km s −1 at a Galactic radius of 60 kpc (Xue et al. 2008 ). Thus, the epicyclic frequency κ = 1.26 × 10 −15 s −1 , and the growth time τ g = f ( Q ) κ −1 , where κ −1 ≃ 25 Myr and f ( Q ) is a function of Q with a value of order unity. If the diffuse gas with mass M d ∼ 4 M m (Ferrière 2001 ) forms into molecular clouds on the Toomre timescale, then the molecular gas formation rate would beIf the molecular gas is being dispersed on a timescale of the order of 10 Myr, this formation rate can replenish it at more than the required rate given in Equation ( 3 ). 4. Variation with Redshift We now consider how the timescale for molecular gas formation by gravitational instability varies with redshift. The Toomre timescale τ g ∝ ω −1 . The disk angular velocity of a galaxy ω can be characterized by its value at the exponential scale length of the disk ω ( R d ) = V c / R d , where V c is the roughly constant circular velocity of the disk