adsabs/WIESP2022-NER huggingface dataset:
Paper: 2015A&A...576A..95I (acknowledgments)
It is a pleasure to thank Eve Ostriker for stimulating discussions and insightful suggestions, Anne Decourchelle and Jean Ballet for enlightening elements regarding the observations of supernovae remnants and Matthieu Gounelle for triggering our interest in supernova explosions. We thank the anonymous referee for a careful reading of the manuscript which has significantly improved the paper. This work was granted access to HPC resources of CINES under the allocation x2014047023 made by GENCI (Grand Equipement National de Calcul Intensif). P.H. acknowledges the financial support of the Agence Nationale pour la Recherche through the COSMIS project. This research has received funding from the European Research Council under the European Community’s Seventh Framework Programme (FP7/2007-2013 Grant Agreement No. 306483 and No. 291294).
Paper: 2020MNRAS.497.1619M (fulltext)
; Taddia et al. 2018 ; Prentice et al. 2019 ). Indeed, the previous studies on 56 Ni mixing in stripped-envelope SNe indicate that 56 Ni mixing can affect the photospheric velocity evolution in stripped-envelope SNe (e.g. Dessart et al. 2012 ). In this paper, we perform a systematic study of the effect of 56 Ni mixing on the photospheric velocity evolution in stripped-envelope SNe. The rest of this paper is organized as follows. We summarize how we get progenitor models, how we mix 56 Ni, and how we conduct radiation transfer simulations in Section 2 . Our results are presented in Section 3 . We discuss the results and conclude this paper in Section 4 . 2 METHODS 2.1 Progenitor models We obtain hydrogen-free progenitor models by using the public stellar evolution code mesa (Paxton et al. 2011 , 2013 , 2015 , 2018 , 2019 ). We assume a metallicity of Z = 0.02. We adopt the standard mixing-length theory for convection with a mixing-length parameter of 2.0 with the Schwarzschild criteria. Our focus in this paper is on hydrogen-free SNe. There are many mechanisms to remove the hydrogen-rich envelope from SN progenitors and the mass-loss mechanisms themselves are a well investigated field of research (Smith 2014 ). In this work, we artificially remove hydrogen-rich envelopes to obtain hydrogen-free SN progenitors. We first evolve massive stars from zero-age main sequence (ZAMS) to the end of helium burning without mass loss. The helium core mass does not change much after the helium burning. At this point, we stop the stellar evolution calculation and gradually reduce the mass from the surface through wind by using the relax_mass option in mesa . The maximum mass-loss rate allowed in this process is 10 −4 M ⊙ yr −1 ( lg_max_abs_mdot = -4 in mesa ). When the stellar mass reaches the desired mass, we resume the stellar evolution calculation without mass loss. The stellar evolution calculations are performed at least until the end of oxygen burning. The subsequent evolution would not affect the envelope structure of the progenitors significantly. Using the method described above, we obtain three hydrogen-free progenitor models: He3.85, CO3.85, and He4.90 (Table 1 ). The density structure of the progenitors is shown in Fig. 1 . He3.85 and CO3.85 have the same mass (3.85 M ⊙ ), but He3.85 is a helium star while CO3.85 is a carbon+oxygen star without helium. The ZAMS masses of He3.85 and CO3.85 are 14 M ⊙ and 20 M ⊙ , respectively. He4.90 is a 4.90 M ⊙ helium star progenitor with a ZAMS mass of 17 M ⊙ . These masses are determined to have the typical ejecta mass (≃2 M ⊙ ) in stripped-envelope SNe (e.g. Lyman et al. 2016 ). Figure 1. Density structure of the progenitor models in the mass coordinate (top) and radius coordinate (bottom). Table 1. Progenitor properties. When we explode these progenitors, we set a mass cut M cut below which is assumed to form a compact remnant that is not ejected. The mass cut is set at 1.35 M ⊙ (He3.85 and CO3.85) and 1.40
Paper: 2016MNRAS.459.2651P (acknowledgments)
The author wishes to thank Derek Ward-Thompson for valuable discussions, the anonymous referee for a detailed and constructive review which greatly improved the content of this paper, and Chris Powles for proof-reading the derivations. The author wishes to thank the Science and Technology Facilities Council for studentship support under grant number ST/K501943/1 and post-doctoral support under grant number ST/K002023/1 while this research was carried out. This research has made use of the NASA Astrophysics Data System.
Paper: 2019MNRAS.486.5231H (acknowledgments)
ACKNOWLEDGEMENTS I appreciate discussions with Hanno Rein, Dan Tamayo, Scott Tremaine, Ed Bertschinger, Walter Dehnen, Matt Payne, and Marie-Claude Arnaud. I appreciate feedback from the anonymous referee.
Paper: 2016ApJ...833...96L (fulltext)
et al. 2014 )—have positions on the IR CMD consistent with the field locus (e.g., Figure 14 ). Finally, the AB Dor member SDSS J1110+0116 (T5.5; Gagné et al. 2015a ) also coincides with the field locus. Thus, for L/T objects as young as ≈100 Myr, while the temperatures for a given spectral type may be age dependent, the IR absolute magnitudes across the L/T transition do not seem to strongly depend on age. Figure 25. Absolute magnitudes vs. spectral type for our sample with an expanded range of spectral types, in order to highlight the latest-type objects. The L/T objects are shown as green squares, with the measurement errors comparable to the symbol size. Normal field objects (small gray triangles) are the same as in Figure 12 . The thick black lines are the polynomial fits from Dupuy Liu ( 2012 ), and the gray region shows the rms about the fits. See Figure 6 caption for further details. The two latest-type red objects in our sample, WISE J0206+2640 (L9 (red)) and WISE J0754+7909 (T2p (red)), may be illuminating landmarks for the transition. Their spectra are unusual compared to most field objects of similar type, especially WISE J0754+7909 (see details in Appendix ). And yet their absolute magnitudes are largely consistent with field objects, with the largest discrepancy being WISE J0206+2640 having ≈0.5 mag fainter magnitudes at Y and J bands compared to the field. Even given its very peculiar spectrum, WISE J0754+7909 has absolute magnitudes and color–magnitude positions in accord with the field. Thus, while the spectral peculiarities of these two objects may not be due to low gravity (indeed both have old field kinematics; Table 15 ), their consistency with field objects may be circumstantial evidence that the IR magnitudes of the L/T transition are robust over a range of physical properties. One interesting question that we can address is whether the J -band flux reversal that is a hallmark of L/T transition binaries in the field population (e.g., Liu et al. 2006 ) would appear different at lower gravities. The most extreme such flux-reversal binaries known are 2MASS J1404−3159AB (Δ J = −0.54 ± 0.08 mag, Δ K = 1.33 ± 0.05 mag; Looper et al. 2008a ) and SDSS J1052+4422AB (Δ J = −0.45 ± 0.09 mag, Δ K = 0.52 ± 0.05 mag; Dupuy et al. 2015 ). SDSS J1052+4422AB has a very precise evolutionary-model-based age derived from its dynamical masses and luminosities, clearly demonstrating that it is field age and gravity ( Gyr and = 5.0–5.2 dex; Dupuy et al. 2015 ). Now that we have parallaxes for members of YMGs that span the L/T transition, we can imagine hypothetical L/T transition binaries composed of these coeval objects. For example, if the AB Dor members WISEP J0047+6803 (L7 int-g ) and SDSS J1110+0116 (T5.5) were paired together in a binary, they would have Δ J = −0.37 ± 0.11 mag, Δ K = 2.04 ± 0.09 mag. If the primary were instead 2MASS J2244+2043 (L6 vl-g ), the flux ratios would be Δ J = −0.47 ± 0.09 mag, Δ K = 1.89 ±0.09 mag. Thus, it
Paper: 2018MNRAS.478.5410D (acknowledgments)
ACKNOWLEDGEMENTS This work has been funded by a French Doctoral Contract. The authors are also grateful to Google for the unrestricted gift given to the University of Santa Cruz to carry out the project: “Deep Learning for Galaxies”.
Paper: 2016MNRAS.462.1882K (acknowledgments)
We thank Seshadri Nadathur, Shaun Hotchkiss, David Alonso, Airam Marcos-Caballero, Fabio Finelli, Francesco Paci, István Szapudi, and the anonymous referee for useful comments that improved the paper. We also thank Krishna Naidoo, Ofer Lahav, and Aurelien Benoit-Lévy for informative discussions. AK thanks Márton Vargyas, and JGB the Theory Division at CERN, for their hospitality, where the main ideas of the project were discussed. Funding for this project was provided by the Spanish Ministerio de Economía y Competitividad (MINECO) under projects FPA2012-39684, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234 and SEV-2012-0249.
Paper: 2018A&A...617A...7R (fulltext)
model assumes a temperature of 10 K for the gas, whichis up to 40% higher than the values found for the central parts of the cores (6–7 K). However, further calculations have shown that lowering the temperature by 2–3 K does not produce significant differences in the results (Roueff, priv. comm.). Visser et al. (2018) highlighted how isotope-selective photodissociation is a key mechanism to understand the nitrogen isotopic chemistry in protoplanetary disks. We can speculate that different levels of selective photodissociation in different environments could reproduce the variety of N-isotopic ratios that are observed. Further investigation of this point from both an observational and a theoretical point of view is merited. From the L1544 and L694-2 results, there seems to be tentative evidence that N 15 NH + is more abundant than 15 NNH + . This can be explained by the theory according to which the proton transfer reaction, tends to shift the relative abundance of the two isotopologues, slightly favouring N 15 NH + due to the fact that N 15 NH + zero-point energy is lower than that of 15 NNH + by 8.1 K (see reaction RF2 in Wirström Charnley 2018 ). It is interesting that the same trend is found also in a very different environment such as OMC-2 FIR4, a young protocluster hosting several protostellar objects. In this source, Kahane et al. (2018) measured lower values for the isotopic ratio, but in agreement with our result found that 15 NNH + is less abundant than N 15 NH + . However, we emphasise that higher-quality observations and those with better statistics are needed to confirm this point. 6. Conclusions We have analysed the diazenylium isotopologues’ spectra in three prestellar cores, L183, L429 and L694-2 in order to derive nitrogen isotopic ratios. Since LTE conditions are not fulfilled, especially for the N 2 H + (1–0) transition, we have used a fully non-LTE radiative transfer approach, implemented in the numerical code MOLLIE. We have carefully derived the physical models of the sources, computing their volume density and dust temperature profiles. With these, we were able to produce synthetic spectra to be compared with our observations, in order to derive the best-fit values for the molecular abundances and column densities. Using the same method, we have also recomputed the isotopic ratio of L1544. The difference with the literature value of Bizzocchi et al. (2013) , due to changes in the molecular collisional rates, is well within the uncertainties. In our sample of four cores, we derived 14 N/ 15 N values in the range 580–1000. Within the confidence range given by our uncertainties estimation, all our results are inconsistent with the value ≈400, predicted by the current theoretical models. L1544 still presents higher depletion levels than the other sources, but in general all the cores are anti-fractionated. The theoretical bases of such a trend are at the moment not understood. A deep revision of our knowledge of the
Paper: 2021MNRAS.500.5479B (fulltext)
only the two-point statistic is insufficient to probe all the effects of different cosmological parameters on the evolution of the overall cosmological field. This motivates the need for considering other summary statistics in the analysis of clustering on smaller scales. Since the total information available in a survey scales with the number of independent modes (Tegmark 1997 ), and given that there are many more independent modes on small scales, it is important to develop these new statistical methods, that better extract information from small scales, to make optimal use of data from ongoing and future cosmological surveys. Various approaches towards harnessing information beyond that contained in the two-point statistics have been explored in the literature. One method is consider the higher N -point functions in the analysis – the three-point function and its Fourier transform, the bispectrum (e.g. Scoccimarro et al. 1998 ; Takada Jain 2004 ; Sefusatti et al. 2006 ), or the four-point function and its Fourier transform, the trispectrum (e.g. Verde Heavens 2001 ). While these additional statistics can be highly informative about small-scale clustering, and promise to yield significantly tighter constraints on some cosmological parameters (Coulton et al. 2019 ; Hahn et al. 2020 ), one drawback is that they generally entail much higher computational costs to measure either from simulations, or from data. The computational complexity rises with N – the order of the highest connected correlation function considered, while keeping the data size fixed. Further, the noise properties for these higher order estimators often make it difficult to obtain good signal-to-noise ratio (SNR) over a wide range of scales. In spite of these issues, analyses including higher order correlations, especially the bispectrum, have successfully been applied to certain cosmological data sets (Gil-Marín et al. 2015 ; Slepian et al. 2017 ; Gualdi et al. 2019 ). In this context, there also exist approaches which attempt to undo the non-linear effects of gravitational clustering on various cosmological fields. Once this procedure is applied, the analysis proceeds with the measurement of the two-point function of the linearized field. This approach has already been applied specifically to the reconstruction of the Baryon Acoustic Oscillation (BAO) signal (Eisenstein et al. 2007 ; Padmanabhan, White Cohn 2009 ; Padmanabhan et al. 2012 ). Schmittfull et al. ( 2015 ) showed that the reconstruction process can be interpreted as the transfer of information from the higher connected N -point functions in the observed field into the reconstructed two-point function. More recently, methods have been proposed for the full reconstruction of the initial linear modes from non-linear observables at low redshift (Baldauf et al. 2010 ; Seljak et al. 2017 ; Modi, Feng Seljak 2018 ; Horowitz, Seljak Aslanyan 2019 ). There is also a large body of literature investigating the one point
Paper: 2019MNRAS.489.3827B (acknowledgments)
ACKNOWLEDGEMENTS EZ and AV acknowledge funding from the Swedish National Space Board. AKI and TH acknowledge the financial support from the National Astronomical Observatory of Japan (NAOJ) ALMA Scientific Research Grant number 2016-01 A. AKI also acknowledges the support from the Japan Society for the Promotion of Science (JSPS) KAKENHI 17H01114. TH acknowledges the JSPS Grant-inAid for Scientific Research 19J01620. Numerical simulations of S16 have been performed with Cray XC30, XC50 at the Center for Computational Astrophysics at NAOJ and with Cray XC40 at the Yukawa Institute for Theoretical Physics at Kyoto University. DC is a DAWN fellow. This research has made use of NASAs Astrophysics Data System.
Paper: 2017A&A...599A..12Z (acknowledgments)
We gratefully acknowledge support by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics (MAS), by Fondecyt Regular 1150345 and by the BASAL-CATA Center for Astrophysics and Associated Technologies PFB-06. This work was finalized at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1066293. M.Z. and D.M. were partially supported by a grant from the Simons Foundation, during their stay in Aspen.
Paper: 2019MNRAS.484.2433S (acknowledgments)
ACKNOWLEDGEMENTS This material is based upon work supported by the National Science Foundation under Grant No. 1411943. Part of the work presented herein is supported by NASA Grant No. NNX15AK92G. P.F.W. acknowledges funding through the Horizon 2020 European Research Council Consolidator Grant No. 683184. We thank the Stanislav S. Shabala as the referee for a constructive report that greatly improved the paper. This study is based on data taken with the Karl G. Jansky VLA that is operated by the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work is based, in part, on data collected at the Subaru Telescope and obtained from the SMOKA, which is operated by the Astronomy Data centre, National Astronomical Observatory of Japan; observations made with the Spitzer Space Telescope , which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA; and data collected at UKIRT that is supported by NASA and operated under an agreement among the University of Hawaii, the University of Arizona, and Lockheed Martin Advanced Technology centre; operations are enabled through the cooperation of the East Asian Observatory. When the data reported here were acquired, UKIRT was operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK. This study is also based, in part, on observations obtained with WIRCam, a joint project of CFHT, Taiwan, Korea, Canada, France, and the Canada–France–Hawaii Telescope that is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawai’i. The scientific results reported in this article are based in part on observations made by the Chandra X-ray Observatory and data obtained from the Chandra Data Archive. The spectrographic data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. We wish to thank the indigenous Hawaiian community for allowing us to be guests on their sacred mountain, a privilege, without with, this work would not have been possible. We are most fortunate to be able to conduct observations from this site.
Paper: 2016MNRAS.460L..89K (fulltext)
thick discs. We observed (see Table 1 ) the mid-plane of NGC 4111 with the SCORPIO in the wavelength range 4800–5600 Å with the spectral resolution ∼2.2 Å =55 km s −1 . The remaining five data sets were obtained using SCORPIO-2 at slightly lower spectral resolution (∼3.8 Å =95 km s −1 at 5100 Å) at the broader wavelength range (3600–7070 Å). Table 1. Long-slit spectroscopy of the sample galaxies. We reduced our spectroscopic observations with our own idl -based reduction pipeline. We estimated the night sky background from outer slit regions not covered by our target galaxies and an optimized sky subtraction technique that takes into account spectral resolution variations along the slit (Katkov Chilingarian 2011 ; Katkov, Sil'chenko Afanasiev 2014 ). All three galaxies were observed with the Infrared Array Camera (IRAC) at Spitzer Space Telescope in the imaging mode at wavelengths 3.6 μm and 4.5 μm. We fetched fully reduced 3.6 μm images from the Spitzer Heritage Archive. 1 2.3 Data analysis Van der Kruit Searle ( 1981 ) have shown that in case an isothermal disc in the equilibrium state the vertical disc density profiles are described by the law I = I 0 sech 2 ( z / z 0 ), where I 0 is the central intensity and z 0 is the disc scale-height. We fitted vertical profiles obtained by averaging Spitzer IRAC images along the radius using models including one and two components. We set central positions of both components to be the same in the case of two-component fitting but left the position itself a free parameter. Our results for NGC 4111 and NGC 5422 quantitatively agree with those presented in the S4G survey (Salo et al. 2015 ), however the results for NGC 4710 decomposition were not presented there. To derive internal kinematics and stellar population properties (mean ages and metallicities [Fe/H]) of thick and thin discs we first binned our long slit spectra in the spatial direction with the adaptive binning algorithm in order to reach the minimal signal-to-noise ratio S / N = 30 per bin per spectral pixel in the middle of the wavelength range. Then, in every bin we applied the nbursts full spectral fitting technique (Chilingarian et al. 2007a , b ) with a grid of high resolution stellar pegase.hr (Le Borgne et al. 2004 ) simple stellar population (SSP) models based on the ELODIE3.1 empirical stellar library (Prugniel et al. 2007 ). The nbursts technique implements a pixel space χ 2 minimization algorithm where observed spectrum is approximated by a stellar population model broadened with parametric line-of-sight velocity distribution (LOSVD) and multiplied by polynomial continuum (10th degree in our case) to take into account dust attenuation and/or possible flux calibration imperfections in both observations and models. We used Gaussian parametrization of the stellar LOSVD, except our higher resolution mid-plane spectra of NGC 4111 where we exploited the standard Gaussian–Hermite parametrization (van der Marel Franx 1993 ). The [Mg/Fe]