adsabs/WIESP2022-NER huggingface dataset:
Paper: 2018MNRAS.477.1258A (fulltext)
time varies with rigidity E / Z , with Z the charge number, as t res ∝ ( E / Z ) s with s ≃ 0.4–0.6. There are a number of codes that model Galactic CR propagation and the CR interactions (losses, spallation, decay of unstable nuclei, and re-acceleration) in the Galaxy, such as galprop , see Strong et al. ( 2010 ), dragon , see Evoli et al. ( 2008 ), and crpropa , see Alves Batista et al. ( 2016 ). In this paper, we do not take into account the effects of CR advection by the Galactic winds, energy losses, and re-acceleration. We also do not consider the network of nuclear reactions that leads to the production of secondary CRs. These effects will be considered in future work. However, in these codes one usually limits the calculations to models with cylindrical symmetry models with an effective diffusion coefficient D , thereby neglecting the influence of the geometry and strength of the GMF on CR diffusion. Recently, some efforts has been taken to consider anisotropic diffusion models for Galactic CRs, see Evoli et al. ( 2017 ). We will consider anisotropic diffusion of CRs inside the Galaxy. We note that a similar calculation, again employing stochastic differential equations, has been applied to the interplanetary transport and acceleration of solar energetic particles in the solar wind see Dröge et al. ( 2010 ) and the references therein. The outline of this paper is as follows: in Section 2 , we discuss the GMF and introduce the main features of the Jansson–Farrar. In Section 3 , we present our numerical solution method to the CR diffusion, based on the Itô formulation of stochastic differential equations, using relevant input, like the diffusion tensor and its connection to the GMF in Section 3.1 . The grammage calculation is discussed in Section 3.3 . In Section 4 , we present the spatial distribution of the CRs from a single source the associated residence time distribution, as well as the grammage of CR particles. We do this for various combinations of parallel and perpendicular diffusion. Section 5 discusses the implications of the results presented in this paper and summarizes our conclusions. 2 MODEL FOR THE GMF The magnetic field in the diffuse interstellar medium (ISM) has two distinct components: a large-scale () regular field, as well as a small-scale turbulent component. The strength of the total magnetic field in the Galaxy has been estimated of about 6±2 μG, see Beck ( 2001 ) and Haverkorn ( 2015 ), with the amplitude of the random field comparable to that of the large-scale field. The large-scale GMF affects the propagation of CRs (Strong et al. 2007 ), the dynamics of molecular clouds and star formation, see Hennebelle Falgarone ( 2012 ). In this paper, we use the GMF model of Jansson Farrar ( 2012a ) and Jansson Farrar ( 2012b ) for this large-scale (regular) field. This model matches the WMAP 7 22 GHz synchrotron intensity map and the Galactic Faraday rotation data obtained from polarization measurements of background
Paper: 2018MNRAS.478.1065C (acknowledgments)
ACKNOWLEDGEMENTS We thank James Bolton, Tirthankar Roy Choudhury, Harley Katz, Laura Keating, and Ewald Puchwein for helpful discussions. This work was supported by the ERC Advanced Grant 320596 ‘The Emergence of Structure During the Epoch of Reionization’. The ramses simulations presented in this paper were performed on the COSMOS Shared Memory system at DAMTP, University of Cambridge, operated on behalf of the STFC DiRAC HPC Facility. This equipment is funded by BIS National E-infrastructure capital grant ST/J005673/1 and STFC grants ST/H008586/1 and ST/K00333X/1. The aton radiative transfer simulations in this work were performed using the Wilkes GPU cluster at the University of Cambridge High Performance Computing Service ( http://www.hpc.cam.ac.uk/ ), provided by Dell Inc., NVIDIA, and Mellanox, and part funded by STFC with industrial sponsorship from Rolls Royce and Mitsubishi HeavyIndustries.
Paper: 2019A&A...630A..46H (acknowledgments)
Acknowledgements Rosetta is an ESA mission with contributions from its member states and NASA. We are indebted to the whole Rosetta Mission Team, LCC, SONC, SGS, and RMOC, for their outstanding efforts to make this mission possible. The contributions of the ROMAP and RPC-MAG teams were financially supported by the German Ministerium für Wirtschaft und Energie and the Deutsches Zentrum für Luft- und Raumfahrt under contract 50QP1401. The SPICE kernels used for this work are available as ROS-E/M/A/C-SPICE-6-V1.0 through PSA and PDS.
Paper: 2018MNRAS.478.4851I (fulltext)
that all six galaxies are LyC leakers with f esc (LyC) ranging between 6 and 46 per cent. These values are much higher than f esc (LyC) of ∼0–4.5 per cent derived e.g. by Borthakur et al. ( 2014 ) and Chisholm et al. ( 2017 ) in SFGs with lower O 32 or with lower equivalent widths of the H β emission line (Hernandez et al. 2018 ). In this paper we present new HST /COS observations of the LyC in five compact SFGs with the highest O 32 ∼ 8–27 ever observed in order to detect ionizing radiation, and examine its behaviour over a wide range of O 32 . The properties of selected SFGs derived from observations in the optical range are presented in Section 2 . The HST observations and data reduction are described in Section 3 . The surface brightness (SB) profiles in the UV range are discussed in Section 4 . In Section 5 we compare the HST /COS spectra with the extrapolation of the modelled SEDs to the UV range. Lyα emission is considered in Section 6 . The escaping LyC emission is discussed in Section 7 together with the corresponding escape fractions. In Section 8 our results are compared with the LyC escape fractions for other galaxies obtained in some recent studies. We summarize our findings in Section 9 . 2 PROPERTIES OF SELECTED GALAXIES DERIVED FROM OBSERVATIONS IN THE OPTICAL RANGE 2.1 Emission-line diagnostic diagrams Our LyC leaker candidates were selected from the SDSS Data Release 12 (DR12) (Alam et al. 2015 ) by adopting the selection criteria described in Izotov et al. ( 2016a,c , 2018 ). All of them have a compact structure on SDSS images (Fig. 1 ) and high equivalent widths EW(H β) > 200 Å of the H β emission line in the SDSS spectra, indicating very recent star formation. These galaxies are located in the upper part of the SFG branch in the Baldwin–Phillips–Terlevich (BPT) diagram (filled stars in Fig. 2a ) implying the presence of high-excitation H ii regions. Izotov et al. ( 2016a,c ) discussed only galaxies with O 32 ∼ 5–7. In this paper and in Izotov et al. ( 2018 ) we report observations of galaxies with the considerably larger range of O 32 ∼ 8–27 (Table 1 ), aiming to study the applicability of the O 32 criterion to select galaxies with high escape fractions of ionizing radiation. It is seen in Fig. 2(b) that the selected galaxies have the highest O 32 ratios among all local LyC leaking galaxies observed so far. Figure 1. 25 arcsec × 25 arcsec SDSS composite images of selected galaxies. Figure 2. (a) The BPT diagram (Baldwin, Phillips Terlevich 1981 ) for SFGs. (b) The O 32 –R 23 diagram for SFGs where R 23 = ([O ii ]3727 + [O iii ]4959 + [O iii ]5007)/H β. The LyC leaking galaxies (this paper) and J1154+2443 (Izotov et al. 2018 ) are shown by filled stars in both panels. The location of LyC leaking galaxies by Borthakur et al. ( 2014 ) and Chisholm et al. ( 2017 ) are shown by open circles while LyC leaking galaxies by Izotov et al. ( 2016a,c ) are represented by open stars. The compact SFGs (Izotov et al. 2016b ) are
Paper: 2016A&A...585A..93R (acknowledgments)
We thank the Centre National d’Etudes Spatiales (CNES, France) and the French CNRS/INSU for continuous support for the preparation of the Gaia mission. This work benefited from travel support from the European Science Foundation through the GREAT Research Network Program. Some of the computations were done on the Mesocentre SIGAMM machine, hosted by the Observatoire de la Côte d’Azur. The first two authors would like to thank Naia for her numerous (and efficient) attempts to postpone the revision of this paper. We warmly thank C.A.L. Bailer-Jones for his constructive remarks, which helped to improve this article. We are also sincerely grateful to D. Katz for his help with regard to the in-flight RVS characteristics.
Paper: 2016ApJ...819...12B (acknowledgments)
This work received major support through an NSF grant NSF ANT-094513. We are thankful for the computing resources provided by the Minnesota Supercomputing Institute. EBEX is supported through NASA grants NNX08AG40G and NNX07AP36H. C. Bao acknowledges the support from the Doctoral Dissertation Fellowship from the University of Minnesota. C. Baccigalupi acknowledges the support from the INDARK INFN Grant.
Paper: 2016MNRAS.462..352G (acknowledgments)
GA, RE, JMG, JFG, and JMT acknowledge support from MINECO (Spain) AYA2014-57369-C3 grant (co-funded with FEDER funds). JMG also acknowledges support from the MECD PRX15/00435 grant (Spain) and from the SI CGPS award, ‘Magnetic Fields and Massive Star Formation’. RE also acknowledges MDM-2014-0369 of ICCUB (Unidad de Excelencia ‘María de Maeztu’). SC acknowledges the support of DGAPA, UNAM, and CONACyT (Mexico).
Paper: 2019MNRAS.482.4528E (acknowledgments)
ACKNOWLEDGEMENTS We are grateful to Yu Lu for making public his implementation of the Parkinson Cole merger tree algorithm. We thank the anonymous referee for constructive comments that improved the paper. We also thank Mike Grudic, Charlie Conroy, Chris McKee, Joss Bland-Hawthorn, Aldo Rodriguez-Puebla, and Rohan Naidu for helpful discussions. Ideas for this project were developed in part at the Near/Far Globular Cluster Workshop in Napa in 2017 December. KE and DRW are grateful for the hospitality provided by the MPIA in Heidelberg during the writing of this paper. KE acknowledges support from an NSF Graduate Research Fellowship. EQ and KE are supported by a Simons Investigator Award from the Simons Foundation and by NSF grant AST-1715070. DRW is supported by fellowships provided by the Alfred P. Sloan Foundation and the Alexander von Humboldt Foundation. MBK acknowledges support from NSF grant AST-1517226 and CAREER grant AST-1752913 and from NASA grants NNX17AG29G and HST-AR-13888, HST-AR-13896, HST-AR-14282, HST-AR-14554, HST-AR-15006, HST-GO-12914, and HST-GO-14191 from STScI. The analysis in this paper relied on the python packages NumPy (Van Der Walt, Colbert Varoquaux 2011 ), Matplotlib (Hunter 2007 ), and AstroPy (Astropy Collaboration 2013 ).
Paper: 2019MNRAS.490.2200C (acknowledgments)
ACKNOWLEDGEMENTS We thank the anonymous referee for helpful suggestions in improving the text. We thank O. Bromberg, A. Philippov, O. Porth, and E. Sobacchi for helpful discussions. KC thanks M. Lucchini, T. Beuchert, F. Krauß, and T.D. Russell for providing useful insights for the background study. This research was made possible by National Science Foundation (NSF) PRAC award no. 1615281, OAC-1811605, NSF AST-1911080, AST-1910248, and AST-1910451 at the Blue Waters sustained-petascale computing project and supported in part under grant no. NSF PHY-1125915. KC and SM are supported by the Netherlands Organization for Scientific Research (NWO) VICI grant (no. 639.043.513), ML is supported by the NWO Spinoza Prize and AT by Northwestern University, the TAC and NASA Einstein (grant no. PF3-140131) postdoctoral fellowships and the NSF grant 1815304 and NASA grant 80NSSC18K0565. KC thanks the Leids Kerkhoven-Bosscha Fonds (LKBF) subsidy no. 17.2.100 for travel funding. The simulation data presented in this work are available on request to AT at atchekho@northwestern.edu.
Paper: 2021MNRAS.503.2902A (fulltext)
−12 with respect to H 2 (Quénard et al. 2017 ). The identification of this cation in various astrophysical environments may be attributed to its relatively large dipole moment (∼2.1 debye, Haese Woods 1980 , or ∼1.75 debye, Botschwina 1987 ). So far, protonated cyanoacetylene is the largest ion detected in space. For its formation in astrophysical media, Takagi et al. ( 1999 ) showed that the reaction of HCCH + with HNC followed by the protonation of HC 3 N leads to HC 3 NH + . They also established that the reaction between the N atom and cyclic C 3 H 3 + is not an efficient pathway for the production of HC 3 NH + in interstellar space (Takagi et al. 1999 ). HC 3 NH + may produce HCCCN and HNCCC species through a dissociative recombination reaction with electrons (Kawaguchi et al. 1994 ; Osamura et al. 1999 ). HC 3 NH + is suggested to play an important role in the production of cyanopolyynes (Turner, Amano Feldman 1990 ; Winstanley Nejad 1996 ; Quénard et al. 2017 ; Marcelino et al. 2020 ). Indeed, cyanopolyynes, HC 2 n +1 N, are widespread molecules in dark clouds. Molecular species up to HC 11 N have been identified in the ISM (Kawaguchi et al. 1994 ; Takagi et al. 1999 ; Sakai et al. 2008 ; Friesen et al. 2013 ; Loomis et al. 2016 ; Jaber Al-Edhari et al. 2017 ; Taniguchi et al. 2018 ). For their formation in astrophysical media, two pathways are proposed: (i) gas-phase neutral–neutral reactions between polyynes and CN or C 3 N radicals such as the reaction between C 2 H 2 and the CN radical, which leads to the formation of HCCCN molecules; and (ii) ion–molecule reactions involving HC 3 NH + , where the low temperature hinders the chemical reactions (e.g. at the so-called early times of less than 10 4 yr): In sum, the consideration of both neutral–neutral and ion–molecule reactions gives reasonable abundances of the cyanopolyyne species (Takagi et al. 1999 ; Wakelam et al. 2015 ; Agúndez et al. 2017 ; Yu et al. 2019 ). Moreover, the HC 3 NH + ion is involved in the chemistry of HCN and HNC, both of which are important species in the formation of larger and more complex nitrogen-containing molecules (Quénard et al. 2017 ) such as the building blocks of polycyclic aromatic nitrogen heterocycle molecules (PANHs) in protoplanetary disks (Mendoza et al. 2013 ). Collisional data represent an important input for the analysis of observed spectra emitted by molecular species in non-local thermodynamical equilibrium (non-LTE) interstellar medium and therefore for the derivation of more accurate molecular abundances (Sarrasin et al. 2010 ; Lique et al. 2015 ; Bop et al. 2019 ; Senent et al. 2019 ). These help astrochemists to propose new plausible routes and processes for the formation of complex molecular species. In particular, it is important to accurately estimate the abundances of HCCCNH + in astrophysical media to better understand the chemistry of complex nitrogen-bearing organic compounds such as cyanopolyynes. To the best of our knowledge,
Paper: 2017ApJ...836...90N (acknowledgments)
The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Support for this work was provided by the NSF through the Grote Reber Fellowship Program administered by Associated Universities, Inc./National Radio Astronomy Observatory. This research was also supported by the NASA Ames Research Center via Cooperative Agreements NNA09DB30A, NNX15AD20A, and NNX16AF59G to J.O. Burns. The authors like to especially thank J. Aguirre for his constructive feedback on the formalism of our approach and discussions on other aspects related to the foreground polarization. The authors would also like to thank R. Monsalve for his comments on the instrumental aspects of the approach. The authors gratefully acknowledge J. Mirocha for providing the simulated global 21 cm data using ARES. B.D. Nhan is also grateful to K. Tauscher and R. Monsalve for their assistance in utilizing the sky map data.
Paper: 2015ApJ...807...24B (acknowledgments)
The authors thank Geza Kovacs and Lynne Hillenbrand for suggesting that we take a closer look at the Hyades and Praesepe, and for helpful comments on the manuscript. We also thank Scott Tremaine for suggestions that made the statistical discussion much clearer. This work was performed in part under contract with the Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. This research has made use of the SIMBAD database and the VizieR catalog access tool, operated at CDS, Strasbourg, France.
Paper: 2018A&A...620A..64M (acknowledgments)
We acknowledge valuable contributions, useful discussions, and comments on the manuscript by Max-Niklas Newrzella, Martin Reinecke, Reimar Leike, Jakob Knollmüller, Björn Adebahr, Stefan Blex, and Alexander Becker. We also thank the anonymous referee for the insightful comments and suggestions. We thank Patricia Reich for providing the HEALPix map of the 1420 MHz radio continuum observations.
Paper: 2018ApJ...855..100S (fulltext)
of linking lengths is somewhat generous compared to previous studies. We use the FoF algorithm only as a basis for an X-ray-detected cluster catalog in the HectoMAP region. We would rather include false candidates than exclude real ones. We next show that this approach recovers the relevant set of X-ray clusters in a separate densely surveyed region with essentially full X-ray coverage (Starikova et al. 2014 ). We test the FoF on the SHELS survey (Geller et al. 2010 , 2012 , 2014 , 2016 ), a dense complete redshift survey with no color selection and covering two well-separated 4 deg 2 fields (F1 and F2) of the Deep Lens Survey (DLS, Wittman et al. 2002 ). We use the F2 survey alone for this investigation because it has essentially complete X-ray coverage of all of the possible massive systems in the appropriate redshift range. The F2 survey is ∼95% complete to R ≤ 20.6 with a number density of ∼3200 galaxies deg −2 . In total, there are 26 X-ray-extended sources detected based on Chandra and XMM X-ray data (Starikova et al. 2014 ); 18 of these X-ray sources are in the redshift range 0.2 z ≤ 0.6 of interest for testing our approach to HectoMAP X-ray clusters. Here, we select 12 X-ray sources within 0.2 z ≤ 0.5 for testing our cluster identification procedure because the F2 magnitude limit R ≤ 20.6 is ∼0.4 mag brighter than the HectoMAP limit. The brighter F2 limit precludes FoF cluster detection at z ≳ 0.5. The X-ray flux limit for the 12 X-ray-extended sources with z 0.5 is 4.3 × 10 −15 erg cm −2 s −1 within 0.5–2.0 keV energy band. This X-ray flux limit is nearly two orders of magnitude fainter than the one we reach for the HectoMAP systems. Starikova et al. ( 2014 ) showed that 10 of these sources have optical counterparts identified as clusters in the SHELS spectroscopic survey (Geller et al. 2010 ) or in the DLS weak lensing analysis (Wittman et al. 2006 ). Here, we examine the number of F2 X-ray extended sources recovered by the FoF algorithm with the HectoMAP choice of linking lengths. Figure 4 shows the cone diagram of the subset of F2 galaxies selected according to the HectoMAP red galaxy prescription within 0.2 z ≤ 0.5. In Figure 4 , the cyan circles display the locations of seven X-ray-extended sources with spectroscopically identified counterparts from Geller et al. ( 2010 ). We also show the X-ray extended sources (yellow circles in Figure 4 ) matched with weak lensing peaks (Wittman et al. 2006 ) or with optical concentrations on the sky in the DLS images (Starikova et al. 2014 ). The redshifts of these X-ray sources with photometrically identified counterparts may not be accurate because they are based on photometric redshifts. Figure 4. Cone diagram for the SHELS F2 survey subsample with R ≤ 20.6, ( g − r ) fiber,0 > 1.0, ( r − i ) fiber,0 > 0.5 projected in the R.A. direction. The cyan and yellow circles indicate extended X-ray sources in F2 with spectroscopic counterparts (Geller et al. 2010 ) and photometric counterparts
Paper: 2016ApJ...826..109C (fulltext)
of . The magnetic field strength B and fitted values translate to a radiative lifetime of ∼100 years, which is difficult to explain without distributed in situ acceleration—this requirement can be relaxed by using a lower value of B . Figure 9. Representative models for the SED of the high-energy synchrotron component along with our binned X-ray data for K61 (top) and the NHS (bottom). Dashed vertical lines represent the boundaries of the energy range that NuSTAR is capable of observing. Varying several of the input parameters can have a large effect on the shape of the curve above 7 keV for K61 and especially in the case of the NHS. The bottom of Figure 9 shows several representative models for the SED of the NHS near the NuSTAR energy band. Unlike K61, the low-energy tail of the second emission component of the NHS is not constrained by the radio or near-IR data. The models shown here vary wildly in emission above 7 keV, where the magnetic field strengths ranges over G, with , and , with a comoving luminosity of . Future observations using NuSTAR would allow us to constrain the SED up to ∼ 80 keV. If the X-ray emission is due only to EC/CMB, then an estimate of the magnetic field strength can be made using (Felten Morrison 1966 ), where is the apparent energy density of the CMB at redshift z , erg cm −3 is the local CMB energy density, the apparent temperature of the CMB is , and the temperature of the CMB is . This calculation gives a value of G. While this is comparable to that quoted for other jets where the EC/CMB model is used to model their X-ray emission, in this case a comoving luminosity of is required to fit the model to our X-ray data. We feel this is unrealistic, as it would violate the Eddington limit by many orders of magnitude. For that reason, we have not shown it in any figure. Additionally, assuming an equipartition magnetic field, a Doppler factor of is required for EC/CMB to explain the observed X-ray/radio NHS flux even for the case of using standard formulae (Harris Krawczynski 2002 ). The required beaming is highly unlikely given the observed properties of the 3C 111 jet, e.g., the observed brightness of the SHS and the lack of obvious blazar properties. We do not have many data points with which to constrain the model of the low-energy synchrotron component, especially in K30 and K61. We expect to be able model its SED well in a follow-up paper using JVLA observations of the jet. As well, additional HST and Chandra observations would help to better constrain the near-IR to optical and X-ray spectral indices of the components, and perhaps also constrain the X-ray emission mechanism of additional components. 5. CONCLUSIONS We have presented new Chandra and HST observations of 3C 111 that reveal that its jet has eight X-ray and near-IR/optical emitting components, which extend for 121 arcsec (355 kpc deprojected length) from its AGN nucleus in the approaching jet, and also reveal the hotspot emission on the