adsabs/WIESP2022-NER huggingface dataset:
Paper: 2017ApJ...845..132C (fulltext)
; Pierrehumbert et al. 2011 ; Rose 2015 ). The substellar point in our simulations was located over the pacific ocean. We also tried aquaplanet simulations and achieved similar results. It would be interesting to test whether locating the substellar point over a large land mass such as Asia would significantly affects our results. 5. Conclusions The main conclusions of this paper are as follows. 1. Tidally locked planets will not necessarily exhibit a snowball bifurcation. This is in contrast with planets with Earth-like rotation and orbit, which are required to exhibit a snowball bifurcation except in unrealistic edge cases. 2. The reason tidally locked planets are not required to exhibit a snowball bifurcation is that the insolation increases strongly as the substellar point is approached. 3. Whether a tidally locked planet actually does exhibit a snowball bifurcation depends on the heat transport and ice/ocean albedo contrast. Higher heat transport and a higher ice/ocean albedo contrast both favor a snowball bifurcation. 4. We performed GCM simulations that suggest that realistic tidally locked planets will not exhibit a snowball bifurcation. Although they should tend to have stronger heat transport, the top-of-atmosphere ice/ocean albedo contrast should tend to be smaller. 5. This work suggests that we will not find habitable tidally locked exoplanets with an active carbon cycle in a snowball state. This should be verified with a model incorporating an active carbon cycle. Appendix Artifact of Sea Ice Scheme Interestingly, and in contrast with Lucarini et al. ( 2013 ), we find a small separation between equilibrated states that were initialized from Warm and Cold Starts. The most likely reason Lucarini et al. ( 2013 ) did not observe this separation is that they started their Cold Start simulations from a significantly warmer climate state that was not globally glaciated. To further investigate this issue, we show global mean sea ice concentration for a series of simulations with a stellar flux of 1200 W m −2 and initial conditions representing equilibrated climate states with different amounts of sea ice (Figure 9 ). We find that states started within the apparent separation band are stable, rather than approaching separate stable warm and cold states at the upper and lower ends of the separation band. This means that the separation band actually represents a smeared state, which we can consider a continuum of states rather than two distinct “fixed points” with separate basins of attraction. This is clearly unrelated to a snowball bifurcation and does not alter our interpretation that there is no snowball bifurcation in PlaSim in the tidally locked configuration. Figure 9. Time series of global mean sea ice concentration for a series of simulations at a stellar flux of 1200 W m −2 with different initial conditions. This plot demonstrates that the solution is a continuum of states rather than two distinct fixed points. By further
Paper: 2017ApJ...835..260Z (acknowledgments)
We thank the referee for the very helpful suggestions that have significantly improved our manuscript. We acknowledge financial support from the 973 Program of China under grant 2013CB837000, the National Natural Science Foundation of China (No. 11573060), the Key Laboratory of Astroparticle Physics of Yunnan Province (No. 2016DG006), the Strategic Priority Research Program, and the Emergence of Cosmological Structure of the Chinese Academy of Sciences, Grant No. XDB09000000. The work of D.H.Y. is supported by CAS “Light of West China” Program.
Paper: 2016A&A...585A..87S (fulltext)
for studies of the host galaxies of AGN ( Kauffmann et al. 2003 ). When using the Vanden Berk et al. (2001) template, it is important to know that it contains significant host galaxy contamination, in particular at redder wavelengths (e.g., Fynbo et al. 2013 , their Fig. 5). In this paper, we use data from the X-Shooter spectrograph to build a new QSO template that covers the full range from rest-frame Ly to 11 350 Å based on bright SDSS QSOs and observed with a single instrument over this spectral range. In Sect. 3 we describe the sample selection and provide details of the observations. Section 4 describes the construction of the composite spectrum, and Sect. 5 presents the resulting composite. In Sect. 6 we perform a comparison with existing composites and in Sect. 7 offer our conclusion. We use the cosmological parameters from Planck Collaboration XVI (2014) with km s Mpc, , and throughout the entire paper. 2. Issues with the currently most used template The currently most widely used QSO template is the SDSS template of Vanden Berk et al. (2001) . As described very clearly in that paper, the SDSS composite spectrum shows a significant change to a shallower spectral slope around 5000 Å. This is mainly attributed to contaminating light from the underlying host galaxies. Other effects also contribute, such as the emission from a hot dust component, but the dominating factor is probably the host contamination. Our main motivation for building a QSO template without this problem is the following: a search for dust-reddened QSOs using near-IR (NIR) selection of QSOs has been initiated ( Fynbo et al. 2013 ; Krogager et al. 2015 ). In the central southern SDSS footprint, Stripe 82 ( Annis et al. 2014 ), about 50 such candidate QSOs have been studied using the New Technology Telescope (NTT). Although the search was for QSOs reddened by foreground absorber galaxies, most systems turned out to be QSOs reddened by dust in their host galaxies. The optical spectra can be matched well by the SDSS template spectrum reddened by SMC-like extinction curve, but the NIR (rest frame optical) photometry from the UKIRT Infrared Deep Sky Survey (UKIDSS) cannot be simultaneously fitted. The problem is illustrated in Fig. 6 in Fynbo et al. (2013) , where they attempt to model the EFOSC2 spectrum of a dust-reddened QSO at observed in that survey. As seen, the SDSS spectrum and photometry can be matched well with the Vanden Berk template, but the photometry from UKIDSS is much too blue for even the unreddened template. This is not a unique case, but a problem that is seen for all the dust-reddened QSOs found in their search. In the SDSS composite, the QSOs which contribute to the spectrum at 5000 Å have to be at fairly low redshifts (). These QSOs have absolute magnitudes that are three to four magnitudes fainter than bright QSOs (e.g., Vanden Berk et al. 2001 , their Fig. 1). They are also likely to have the brightest rest frame optical host galaxies, so host
Paper: 2020A&A...638L..10S (fulltext)
by Proshina et al. (2020) . 2. Observations and the data involved Our long-slit spectral observations were made with a multi-mode focal reducer SCORPIO-2 ( Afanasiev Moiseev 2011 ) at the prime focus of the Russian 6 m telescope of the Special Astrophysical Observatory, Russian Academy of Sciences. UGC 5936 was observed on February 28, 2014. In these observations, the 1′′ slit was aligned with the major axis, PA(slit) = 83deg, and the total exposure time was 75 min; also the target was exposed in the orientation through the neighbouring dwarf galaxy, PA(slit) = 135deg, with the exposure time of 45 min. The seeing during these observations was mediocre, F W H M = 3′′. We used the VPHG1200@540 grism providing an intermediate spectral resolution F W H M ≈ 5 Å in the wavelength region from 3700 Å to 7200 Å. This spectral range includes a set of strong absorption and emission lines making it suitable to analyse both stellar and gaseous kinematics of the galaxy as well as the gas excitation and chemistry and properties of the stellar populations. The slit is 6′ in length, which allowed us to use the edge spectra for subtraction of the sky background. The CCD E2V CCD42-90, with a format of 2048 × 4600, using in the 1 × 2 binning mode provided a spatial scale of 0.357 ′′/px and a spectral sampling of 0.86 Å/px. The data reduction as well as kinematics and stellar population characteristics derivation were standard for our SCORPIO-2 data; see for example Sil’chenko et al. (2019) or Proshina et al. (2020) . We used the g r -band images from the SDSS/DR9 archive ( Ahn et al. 2012 ) to study the large-scale structure of the galaxy. 3. Photometric and dynamical structure of UGC 5936 The smooth lenticular galaxy UGC 5936 (see 2MASS J -band image, Fig. 1 , lower middle) possesses a large pseudo-ring which looks unclosed in the optical continuum bands (Fig. 1 , upper left). However Fig. 1 (lower right), which shows the WISE/W3 data in the 12 μ m band delineates a perfect closed ring; in this figure hot dust heated by star formation reveals its organisation in a typical S0 outer ring structure. The colour map (Fig. 1 , upper right), demonstrates the blue colour of the ring, which is narrow to the east and splits into two arcs to the west, as well as the red colour of the arc connecting the core and the western part of the ring. The western blue-ring structures correspond to the ring in the unsharp-masked image (Fig. 1 , upper middle). Interestingly, the GALEX near-ultraviolet (NUV) map (Fig. 1 , lower left), which also refers to young star concentration, shows UV flux excesses beyond the borders of the continuum-band pseudo-ring; the offset is seen especially well at the major axis. To the south-east from UGC 5936, a small satellite, SDSS J105009.10+362009.9 , is observed at 15 kpc projected onto the sky plane; this satellite is observed at 19 kpc if we suggest that it lies in the plane of the UGC 5936 disc. This small satellite is very blue. According to
Paper: 2018MNRAS.477..552B (acknowledgments)
ACKNOWLEDGEMENTS We are grateful to Peter Camps for code support, interesting discussion, and the development of skirt . We thank Ricardo Amorin, Ilse De Looze, Hiroyuki Hirashita, Roberto Maiolino for helpful discussion, and Nicolas Laporte for providing data. AF acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120. We acknowledge the use of the python programming language (Van Rossum de Boer 1991 ), and use of the numpy (van der Walt, Colbert Varoquaux 2011 ), ipython (Perez Granger 2007 ), jupyter (Kluyver et al. 2016 ), matplotlib (Hunter 2007 ), and pymses (Labadens et al. 2012 ) packages. This research made use of astropy , a community-developed core python package for Astronomy (Astropy Collaboration et al. 2013 ).
Paper: 2019MNRAS.484.3935D (fulltext)
map maximum. The variability period is illustrated by the red dashed line in the global spectra. A possible aliasing period is displayed in blue. Lower panel: Lomb–Scargle periodogram for the same LC. The main peak labelled ‘A’ corresponds to the period of 18.86 d, whereas ‘B’ indicates the 39 d period. 3.3 KIC 4829241, KIC 10420021 and KIC 11822535 The stars KIC 4829241, KIC 10420021 and KIC 11822535 were classified as non-periodic by Maoz et al. ( 2015 ). Instead, our study suggests a periodic or quasi-periodic modulation well describing a variability signature in the wavelet representations. We attribute to this variability periodicities ranging between 11 and 16 d, which is reasonable for WDs (e.g. Kawaler 2015 ; Valeev et al. 2017 ; Braker et al. 2017 ). In fact, these periodicities are more persistent in KIC 4829241 and KIC 10420021 than in KIC 11822535, even though also noticeable in the latter star. We do not expect to find magnetic cool-spot signatures for KIC 4829241 and KIC 11822535 considering their high T eff and their log g values (Tremblay et al. 2015 ). However, a transient signature for KIC 10420021 is conceivable in view of its T eff and log g being close to the limit value (Tremblay et al. 2015 ), so the presence of a convection zone at the WD surface can still be envisaged. Combining the surface gravities and the effective temperatures, derived spectroscopically by Hallakoun et al. ( 2018 ), with evolutionary grids (Benvenuto Althaus 1999 ), we are able to estimate the mass of these three WDs. KIC 4829241 is a WD of mass . The Lomb–Scargle periodogram for this WD shows a period of 16.68 d with an amplitude of 286 ppm, as indicated by the letter A in the upper-right panel of Fig. 5 . Following Maoz et al. ( 2015 ), given its mass, rotation combined with an accretion of gas from the interstellar medium (ISM) and the material carried on the magnetic poles generating hotspots, with an accretion luminosity of Δ L acc ∼ 1.4 × 10 29 erg s −1 , could explain the periodic modulation. Fig. 5 (upper-left panel) displays the wavelet analysis, from which we noticed a long-lasting periodicity of 16.04 d over the time observation. With a lower amplitude, we also found a 40-d period that could be considered as a possible aliasing period. The 16-d period characterizes the WD photometric modulation since it is the main period obtained in both Fourier- and wavelet-based techniques. Based on a rough FAP estimation (see Section 2 ), these periods likely lie above the confidence level. Figure 5. Left: light curves with additional treatment, wavelet local and global spectra of Kepler WDs (from top to bottom) KIC 4829241, KIC 10420021, and KIC 11822535. Contour levels are 90 , 80 , 70 , ..., 20 , and 10 of the map maximum. The variability periods are illustrated by the red dashed lines in the global spectra. Possible aliasing periods are displayed in blue. Right: respective Lomb–Scargle periodogram for the same WD. The main peak labelled 'A'
Paper: 2018ApJ...866..145H (acknowledgments)
We thank Peter Stetson for a copy of DAOPHOT as well as his helpful engagement on its usage. Support for this work was provided by NASA through Hubble Fellowship grant #51386.01 awarded to R.L.B. by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. M.G.L. and I.S.J. were supported by the National Research Foundation of Korea (NRF) grant funded by the Korea Government (MSIP) No. 2017R1A2B4004632. Support for program #13691 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. 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. Facility: HST (ACS/WFC). Software: DAOPHOT (Stetson 1987 ), ALLFRAME (Stetson 1994 ), TinyTim (Krist et al. 2011 ).
Paper: 2019ApJ...885...62T (acknowledgments)
We thank the anonymous referee for his/her constructive comments that helped improve the paper. P.T. acknowledges support from NASA grant 80NSSC18K0408 (solicitation NNH17ZDA001N-ADAP). This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by the National Aeronautics and Space Administration. This research made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). Facilities: Suzaku , NuSTAR .
Paper: 2019MNRAS.487..168P (acknowledgments)
ACKNOWLEDGEMENTS This research has used 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.
Paper: 2016MNRAS.460...44P (acknowledgments)
We thank the referee for useful comments that helped to improve the manuscript. We also thank Prof. R. A. Chevalier and Dr D. Caprioli for critically reading the manuscript. MP acknowledges support for this work by NASA through Einstein Post-doctoral Fellowship grant number PF3 140113 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060.
Paper: 2017MNRAS.469S.443B (fulltext)
that the outburst ejecta are comprising small and bright particles. The decrease of the colour temperature and colour shortly after the peak brightness suggests an increase of the mean particle size with time for the particles crossing VIRTIS FOV. The presence of silicatic grains devoid of organic material could be explained by the high grain temperatures causing sublimation of the organics. Quantitatively, the September 13 outburst data are consistent with the silicatic grain hypothesis. However, large colour temperatures (>600 K) are measured at the peak brightness of the September 14 outburst, whereas computed temperatures are 530 K for olivine grains. Several explanations are possible. First, we did not consider grains smaller than 100 nm in radius, whereas we cannot exclude their presence. These grains might reach higher temperatures than 100 nm grains, though this is not expected from model calculations (Lasue et al. 2007 ). In our model, 100 nm grains are compact ( P = 0). Considering instead that these grains are aggregates, their temperature would be higher than the temperature of the equivalent sphere (Xing Hanner 1997 ). Another possibility is that the spectral indices of amorphous olivine differ significantly from those of the refractory material of cometary grains. We performed Mie calculations with inclusions of FeS within an olivine matrix. For a volume fraction of 6 per cent of FeS consistent with the suggestion of Fulle et al. ( 2016a ) for 67P grains, the colour temperature reaches 575 K (Fig. 12 ), which is not far from the extremum values measured during the September 14 outburst. Could fractal agglomerates explain the outburst spectra? For carbon/amorphous olivine mixtures, the colour and colour temperature of their infrared spectrum match the measurement, but this is not the case for the bolometric albedo (Fig. 10 ). Calculations made for units of amorphous olivine provide a bolometric albedo 0.4, i.e. a factor of 2 below the measured values. During 67P outbursts, MIDAS collected a high amount of micrometric grains (Bentley, personal communication), in agreement with an ejecta population dominated by compact grains rather than aggregates. We performed calculations setting the maximum size of the fractal aggregates to a max = 1 μm, and the bolometric albedo is still 0.4. Finally, the main contributors to the scattered and thermal parts of the spectrum could be distinct populations of grains. Cold and bright grains would essentially contribute to scattered light, whereas this is the opposite for warm and dark grains made of strongly absorbing material. These two populations of grains were found in the outburst ejecta of the extraordinary outburst of comet 17P/Holmes in 2007 October ( r h = 2.45 au) (Yang et al. 2009 ). The near-IR spectra of the outburst ejectas showed strong absorption bands at 2 and 3 μm related to water ice (Yang et al. 2009 ). Infrared signatures of ice are not detected in the VIRTIS-H outburst
Paper: 2015MNRAS.447..598S (acknowledgments)
NS thanks J. S. Gallagher for discussions regarding binary evolution and LBVs, and in particular for drawing our attention to previous work by N. King. We benefitted from discussion about SN host environments with P. Crowther, J. Anderson, and P. Kelly, and from further discussions concerning binary evolution with S. de Mink. We also thank the referee (J. Eldridge) for a careful reading and thoughtful comments that improved the paper. Partial support was provided by NSF award AST-1312221. This research has made use of the SIMBAD data base, operated at CDS, Strasbourg, France.
Paper: 2018ApJ...863...48C (acknowledgments)
We are very grateful for the warm reception and skillful help we have received from the staff of the Dominion Radio Astrophysical Observatory, which is operated by the National Research Council Canada. The CHIME/FRB Project is funded by a grant from the Canada Foundation for Innovation 2015 Innovation Fund (Project 33213), as well as by the Provinces of British Columbia and Quebec. Additional support was provided by the Canadian Institute for Advanced Research (CIFAR) Gravity Extreme Universe Program, McGill University and the McGill Space Institute, University of British Columbia, and University of Toronto Dunlap Institute. The Dunlap Institute is funded by an endowment established by the David Dunlap family and the University of Toronto. Research at Perimeter Institute is supported by the Government of Canada through Industry Canada and by the Province of Ontario through the Ministry of Research Innovation. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. J.C. was supported by a Natural Sciences and Engineering Research Council of Canada (NSERC) Undergraduate Student Research Award. P.C. is supported by a Mitacs Globalink Graduate Fellowship. M.D. is supported by an NSERC Discovery Grant, CIFAR, and Fonds de Recherche du Québec—Nature et technologies Centre de Recherche en Astrophysique du Québec (FRQNT/CRAQ). B.M.G. is supported by an NSERC Discovery Grant and the Canada Research Chairs program. M.H. and G.H. are supported by CIFAR. V.M.K. is supported by a Lorne Trottier Chair in Astrophysics Cosmology, a Canada Research Chair, CIFAR, an NSERC Discovery Grant and Herzberg Award, and FRQNT/CRAQ. U.-L.P. is supported by CIFAR. K.W.M. is supported by the Canadian Institute for Theoretical Astrophysics National Fellows program. S.M.R. is supported by CIFAR and the NSF Physics Frontiers Center award 1430284. I.H.S. is supported by CIFAR and an NSERC Discovery Grant. P.S. is supported by a DRAO Covington Fellowship from the National Research Council Canada. Software: CHIME/FRB pipeline, alpenhorn (Hincks et al. 2015 ), bonsai (K. M. Smith et al. 2018, in preparation), Grafana ( grafana.com ), Prometheus ( prometheus.io ), RRATTrap (Karako-Argaman et al. 2015 ), PRESTO ( github.com/scottransom/presto ).
Paper: 2018A&A...614A.110Z (acknowledgments)
Acknowledgements The authors thank the anonymous referee for his or her thorough review and comments, which contributed to improving the manuscript. The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013) / ERC Grant agreement No. 291058. This research was supported by the Research Council of Norway through the grant “Solar Atmospheric Modelling”. This research was supported in part with computational resources at NTNU provided by NOTUR, http://www.sigma2.no . Some computations were performed on resources provided by the Swedish National Infrastructure for Computing (SNIC) at the High Performance Computing Center North at Umeå University and the PDC Centre for High Performance Computing (PDC-HPC) at the Royal Institute of Technology in Stockholm. CHIANTI is a collaborative project involving George Mason University, the University of Michigan (USA) and the University of Cambridge (UK).