adsabs/WIESP2022-NER huggingface dataset:
Paper: 2018ApJ...865....9B (acknowledgments)
The Berger Time-Domain Group at Harvard is supported in part by the NSF under grant AST-1714498 and by NASA under grant NNX15AE50G. This paper is based upon work supported by the National Science Foundation Graduate Research Fellowship Program under Grant No. DGE1144152. We thank Pete Challis and Allyson Bieryla for assistance with some of the FLWO 48 inch observations. We thank Stephen Smartt and Ken Smith for providing access to the early PSST images. This work is based in part on observations obtained at the MDM Observatory, operated by Dartmouth College, Columbia University, Ohio State University, Ohio University, and the University of Michigan. This work is partially based on data acquired with the Swift GO program 1114109 (PI Margutti). R.M. acknowledges partial support from programs No. NNX16AT51G provided by NASA through Swift Guest Investigator Programs. Based on observations (Proposal ID GN-2016B-FT-28) obtained at the Gemini Observatory acquired through the Gemini Observatory Archive and processed using the Gemini IRAF package, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), and Ministério da Ciência, Tecnologia e Inovação (Brazil). This paper uses data products produced by the OIR Telescope Data Center, supported by the Smithsonian Astrophysical Observatory. Some observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. Based on observations made with the NASA/ESA Hubble Space Telescope , obtained from the data archive at the Space Telescope Science Institute. Support for program GO-15162 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.
Paper: 2017A&A...608A..57V (acknowledgments)
We thank Gijs Nelemans for useful discussions.
Paper: 2015MNRAS.451.3400B (acknowledgments)
MAB thanks Tomas Ruiz Lara, Mina Koleva, Ryan Leaman, John Beckman, Chris Flynn, Bradley Gibson and Marie Martig for useful discussions. This paper is based on observations made with the GTC, installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, on the island of La Palma. This research has made extensive use of the NED which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research also made use of aplpy , an open-source plotting package for python hosted at http://aplpy.github.com , NASA's Astrophysics Data System and iraf , which is distributed by the National Optical Astronomy Observatory and operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. The IAC researchers acknowledge financial support from the Spanish Ministry of Economy and Competitiveness (MINECO) under the 2011 Severo Ochoa Program MINECO SEV-2011-0187. CG and AA are partially funded by the Science and technology Ministry of Spain (grant AYA 2010-16717). MB acknowledges support from grant AYA2013-48226-C3-1-P from the Spanish Ministry of Economy and Competitiveness (MINECO).
Paper: 2019A&A...621A..96C (acknowledgments)
We wish to thank J. Blaizot, J. Devriendt, R. Teyssier and M. Trebitsch for useful suggestions. CC wishes to acknowledge the valuable feedback provided by R. Beckmann and P. Mitchell. CC is sponsored by the Institut Lagrange de Paris fellowship. This work has made use of the Horizon Cluster hosted by Institut d’Astrophysique de Paris. We thank Stephane Rouberol for running smoothly this cluster for us. It has also made use of the Occigen Cluster hosted by the CINES on the A0040406955 GENCI grant. This work has extensively used YT , the open-source analysis and visualisation toolkit. The source code of the new tracer particles is available upon request.
Paper: 2017MNRAS.467.4264G (fulltext)
of a desert beyond. However, of the 382 stars in their sample, only 36 are solar-type (main-sequence with 5000 T eff 6000K) stars. Troup etal. ( 2016 ) argue that this result agrees with the work of Guillot etal. ( 2014 ) who find that the BD desert may not be as dry as initially thought when considering stars more massive than the Sun, as well as evidence that the BD desert is a special case for solar-mass stars (Duchne Kraus 2013 ). Duchne Kraus ( 2013 ) suggest tidal interaction with host stars may shape the brown dwarf desert. While assessing the characteristic time-scale for orbital decay, Damiani Daz ( 2016 ) find that F-type stars may host massive companions for a significantly longer time than G-type stars for orbital periods less than 5 d; however, they conclude that BD occurrence should largely be unaffected by tidal decay for orbital periods greater than 10 d, regardless of host mass. Debate continues on valid formation mechanisms of BDs and whether or not different formation mechanisms dominate in different mass, period and eccentricity regimes. Three main mechanisms are advocated in the field: (i) the ejection of protostellar embryos from their natal cloud cores (Boss 2001 ; Reipurth Clarke 2001 ), (ii) the fragmentation of protostellar discs (Stamatellos Whitworth 2009 ; Stamatellos etal. 2011 ) or (iii) collapsing molecular cloud cores (Hopkins 2012 ; Hennebelle Chabrier 2013 ), i.e. the same process as Sun-like stars. Through their statistical study, Ma Ge ( 2014 ) reported that BD companions with minimum masses below 42.5 M Jup have an eccentricity distribution consistent with that of massive planets, while those with masses above 42.5 M Jup have an eccentricity distribution consistent with that of binaries. Ma Ge ( 2014 ) also find that host stars of BD companions are not metal rich and have a significantly different metallicity distribution compared to host stars of giant planets, suggesting a formation mechanism different from the core-accretion (Ida Lin 2004 ) scenario. Ma Ge ( 2014 ) conclude that BD companions with minimum masses below 42.5 M Jup likely form in a protoplanetary disc through the disc gravitational instability scenario, and their eccentricity is excited through scattering, while BD companions with minimum masses above 42.5 M Jup likely form in the same way as stars, through molecular cloud fragmentation. Troup etal. ( 2016 ) find 14 candidate BD companions around metal-poor stars ([Fe/H]0.5), also challenging the core-accretion formation model for BDs, which they find unsurprising given that Carney etal. ( 2003 ) observed that lower metallicity populations generally have a higher number of binaries. Here, we present new BD candidate companions using data from the SDSS-III Multi-object APO Radial Velocity Exoplanet Large-area Survey (MARVELS; Ge etal. 2008 ). MARVELS observed 3300 stars with 10 RV measurements. Unlike APOGEE, MARVELS primarily targeted solar-like dwarfs, and thus, is complementary to the
Paper: 2018ApJ...868...33L (fulltext)
(pessimistic). The most pessimistic lower limit for the background is ≈1 × 10 −16 (Dvorkin Barausse 2017 ; Bonetti et al. 2018 ), though most estimates suggest that A SB will be at least several times larger (Ravi et al. 2015 ). We also looked at two different values of the total time span observed after the end of NG11, T + = 10 or 20 years, for calculating ρ . In Table 1 , we show our results in terms of the amount of time per pulsar per year allocated given different values of A SB and T + . Table 1 Optimal Pulsar Cadences for a Stochastic Background Note. We assumed β = 13/3. Added time span T + is in units of years. Dashed entries formally have values, but are too small to be reported. 3.1. Maintaining the PTA: The Time Allocation per Pulsar Table 1 shows that our best pulsars do not overwhelmingly dominate the stochastic-background time allocation. This makes sense when we consider a hypothetical PTA where we ignore all T ij and χ ij and only have pulsars with white noise. Following Siemens et al. ( 2013 ) but including the differences in white noise and cadences, we have . Then, one can easily show that the total ρ maximizes when the “quality” of each pulsar, the white-noise spectrum , is similar, and thus one should spend more time on pulsars with higher white-noise rms. Lee et al. ( 2012 ) reached a similar result. Since the optimization performed is over complex nonlinear equations (Equations ( 1 ), ( 2 )), the results we obtain for an individual pulsar can differ compared with that of the scaling relations. For real PTAs, one should consider red noise, varying time baselines, changes in the relative contributions of white-noise parameters over time, and sky positions, which will modify the results accordingly, though the basic principle still applies. We see that the time allocation is of similar magnitude for all pulsars, i.e., no pulsar overwhelmingly dominates the time allocation, though several pulsars do not contribute significantly for certain assumed parameters and thus are not listed (when c i 1 hr/year). Comparing against the value of ρ determined from a continuation of the NG11 observing strategy versus the optimizations found here, we see a ∼5% increase in ρ for , but a nearly ∼8%–10% increase for . NANOGrav’s general strategy of observing many high-precision pulsars with roughly equal time (along with high-cadence programs) therefore currently provides close to optimal stochastic-background sensitivity. 3.2. Trimming the PTA: Removing Pulsars to Improve Sensitivity Figure 1 shows the effect of removing a pulsar from the array and whether reallocating its observing time will increase or decrease sensitivity to the stochastic background. We find that all 45 pulsars contribute significantly for decades-long experiments and that the relative importance of continuing to time these pulsars also tends to improve. However, note in Table 1 where certain pulsars become significant for T + = 20 years, whereas they are unlisted for
Paper: 2017ApJ...834...74S (acknowledgments)
We acknowledge helpful discussions with John ZuHone and Mateusz Ruszkowski. This work was supported by Chandra Awards GO1-12160X and GO2-13125X issued by the Chandra X-ray Observatory Center which is operated by the Smithsonian Astrophysical Observatory under NASA contract NAS8-03060.
Paper: 2017ApJ...835..265W (fulltext)
own reradiated IR photons ( for the most favorable geometry), so we assume that this boosting is unimportant. NGC 253 has a total infrared luminosity of erg s −1 , about half of which originates within a diameter of ∼200 pc from its center (Leroy et al. 2015b ), i.e., R src = 100 pc. The SW streamer has a “minimum mass” , a projected size on the sky of pc 2 , and a typical distance to the center of the order of pc. If we assume that the geometry corresponds to a cylinder 60 pc in diameter () illuminated by erg s −1 , the force due to radiation pressure applied at the base of the streamer would be dyn, resulting in an estimated acceleration of cm s −2 . In the absence of gravity, the resulting velocity at pc would be km s −1 , lower than the observed velocity before projection correction (Figure 4 ). If we instead assume that the radiation is exerting pressure on the long side of the cylinder (the geometry with the maximum area), f rad would be five times larger, with a corresponding km s −1 . Note, however, that the ratio of gravity to radiation pressure for stars is , where erg s −1 g for a fully sampled IMF containing young stars, and is the surface density of the cloud (Ψ is the light-to-mass ratio of the stellar population, e.g., Equation (33) in Kim et al. 2016 ). For the end-on geometry g cm −2 , while for the side-on geometry g cm −2 , resulting in . So, for our assumed geometry and mass, the net acceleration is between 6% and 81% of a rad , which would result in km s −1 . From the above estimates, it appears that radiation can contribute maybe up to a few tens of percent of the momentum, but it is extremely unlikely to completely explain the observations. Doing so would require using the most favorable geometric assumption (maximal cloud area, which maximizes f rad and minimizes ) and also assuming that there is almost no projection correction to the measured velocity (which requires a contrived geometry). This suggests that radiation pressure is not the dominant mechanism for accelerating the streamer, though it is non-negligible. Note also that any increase in the mass of the streamer over its minimum mass (see discussion in Section 3.6.1 ), or accounting for the old stars in the galaxy disk outside the starburst (which would increase gravity), would also reduce the importance of radiation pressure. Much higher resolution observations of the SW streamer may help further elucidate these questions, in particular, which mechanisms are driving the molecular gas in the outflow. 4. Summary Our new ALMA band 3 observations (CO and dense gas tracers) of the central starburst region of NGC 253 give new insights on the properties of the molecular outflowing gas originally discussed in Bolatto et al. ( 2013 ). The most prominent outflow feature toward the south, which is the main subject of this paper, possesses a large intrinsic velocity dispersion. Its extent and dispersion are consistent with an ejection from the disk starting about ∼1 Myr
Paper: 2017A&A...601A..17B (acknowledgments)
This work is supported by NASA grant NNX16AC07G through the XMM-Newton Guest Observing Program, and through grants for HST program number 14054 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. The research at the Technion is supported by the I-CORE program of the Planning and Budgeting Committee (grant number 1937/12). N.A. is grateful for a visiting-professor fellowship at the Technion, granted by the Lady Davis Trust. E.B. received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No. 655324. S.B. and M.C. acknowledge financial support from the Italian Space Agency under grant ASI-INAF I/037/12/0. P.O.P. and F.U. acknowledge support from CNES and from PNHE of CNRS/INSU. G.P. acknowledges support by the Bundesministerium für Wirtschaft und Technologie/Deutsches Zentrum für Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OR 1408 and FKZ 50 OR 1604) and the Max Planck Society. We thank the referee for useful comments that have been implemented in the manuscript.
Paper: 2016MNRAS.461.3259G (acknowledgments)
The Australia Telescope Compact Array is part of the Australia Telescope National Facility, which is funded by the Australian Government for operation as a National Facility managed by CSIRO. JFG and LFM are partially supported by MINECO (Spain) grant AYA2014-57369-C3-3 (co-funded by FEDER). LU acknowledges support from grant PE9-1160 of the Greek General Secretariat for Research and Technology in the framework of the program Support of Postdoctoral Researchers.
Paper: 2019MNRAS.486..843P (acknowledgments)
ACKNOWLEDGEMENTS HDP, HJR-P, and FA-F thank the Brazilian Agency CAPES (DS and PDSE programs) for the financial support of this research. Funding was also provided by the US National Science Foundation grant AST 16-15688, The Marvin Clan, Babette Josephs, Manit Limlamai, and the 2015 Crowd Funding Campaign to Support Milky Way Research, to CM and HJN. ARGJ thanks FAPESP proc. 2018/11239-8. 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 web site 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, 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, 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. The Pan-STARRS1 Surveys (PS1) have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, and the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation Grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), and the Los Alamos National Laboratory.
Paper: 2019A&A...624A..16R (fulltext)
profiles (azimuthally averaged) for the dust continuum and line images. Shown are profiles derived from images convolved with representative beam sizes for SPHERE (blue, FWHM = 0.031′′), ALMA (black, FWHM = 0.012′′), and ngVLA (red, FWHM = 0.004′′). The continuum non-detections of wide-orbit CPDs with ALMA indicate low dust masses or very compact optically thick disks ( r out ≲ 0.5 au, Wu et al. 2017a ). Compared to those non-detections, the 860 μ m disk in our reference model seems to be too large. We discuss this further in Sects 3.2 and 3.3 . In contrast to the dust emission the 12 CO J = 3 − 2 emission traces mostly the outer disk and can, in principle, be spatially resolved with ALMA even with larger beams. In the reference model the line is optically thick throughout the disk (see Fig. 4 ) and traces only the upper layers of the disk. Because of the high optical depths 12 CO J = 3 − 2 is very sensitive to the disk size (i.e. emitting area) and the temperature. The different apparent extents of the dust and line emission in our model is similar to observations of T Tauri disks (e.g. de Gregorio-Monsalvo et al. 2013 ; Ansdell et al. 2018 ). It is still unclear if this difference is only caused by optical depth effects or if radial dust migration also plays a role ( Woitke et al. 2016 ; Facchini et al. 2017 ). In our models the cause is solely the different dust and line optical depths. For ngVLA observations at 3 mm the situation is similar to the ALMA Band 7 at 860 μ m. The main difference is the possible higher spatial resolution of the ngVLA (0.004′′, 0.6 au at d = 150 au), which might allow us to also resolve the dust disk (see right panel of Fig. 3 ). Compared to the 860 μ m emission, the emission at 3 mm is weaker and the optically thick region of the dust and the gas are slightly smaller (see Fig. 4 ). 3.2 Exploring disk mass and size In Fig. 5 we compare the modelled fluxes for the dust continuum and gas lines to the 5 σ detection limits of ngVLA and ALMA (6 h on-source observing time, see Appendix C ). We report the peak(maximum) fluxes determined from the synthetic beam convolved continuum images and line cubes (see Appendix D ). If the peak flux of the model is above the reported sensitivity limit a 5 σ detection is possible in the case of the lines in at least one channel. Figure 5 shows the reference model and models with varying R tap (i.e. changing the radial extent of the disk) and with a factor of 10 lower disk mass. Indicated in Fig. 5 are also the 3 σ rms values reported by Wu et al. (2017a , Table 1 ) for their observations of five potential CPDs with ALMA in Band 6. The average on-source integration time for their sample is around 12 min. Fig. 4 Vertical optical depth τ for the dust and for 12 CO lines as a function of radius in the reference model (see also Fig. 3 ). The horizontal dark grey line indicates τ = 1. As Fig. 5 shows our reference model is easily detectable in the dust, also with significantly shorter
Paper: 2018ApJ...867...30E (acknowledgments)
The authors would like to thank Michele Fumagalli for sharing his composite spectrum of the LLSs, and Feige Wang, Jonathan Stern, Bram Venemans, and Roberto Decarli for very helpful discussions and feedback. Some of the data presented in this paper 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. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This paper contains data based on observations obtained at the Gemini Observatory, acquired through the Gemini Observatory Archive, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), and Ministério da Ciência, Tecnologia e Inovação (Brazil).