adsabs/WIESP2022-NER huggingface dataset:
Paper: 2018ApJ...860..141H (fulltext)
becomes minimum at S, with the Lorentz factor reaching maximum, suggesting a highly Doppler boosting jet. Together with the fact that an active γ -ray flaring event in 1H 0323+342 coincided with the passage of a highly superluminal component through S (Doi et al. 2018 ), the recollimation shock S at the end of ACZ might be a potential site of γ -ray production as well as the jet base. The deprojected distance of this feature is ∼40–100 pc. The γ -ray production at such distances is much higher than those usually suggested in typical γ -ray blazars, while this situation is quite similar to HST-1 in the jet of M87. 6. We found that the core shift of the 1H 0323+342 jet is small between 1.4 and 43 GHz. This is consistent with the jet having a small viewing angle to our line of sight. We estimated a relative separation between the 43 GHz core and the central BH using the measured parabolic collimation profile of the inner jet, and obtained a deprojected separation of ∼(0.24–0.71)pc (or possibly shorter) for a viewing angle of 4°–12°. 7. We found various remarkable similarities in the parsec-scale jet structures between 1H 0323+342 and M87 (e.g., the collimation profile and recollimation shock). If M BH of 1H 0323+342 is ∼4 × 10 8 M ⊙ and thus follows the M BH – σ relation, we suggest that a common jet formation mechanism is at work in M87 and 1H 0323+342, where the external gas bound by the SMBH potential plays a role in collimating the jets. 8. If M BH of 1H 0323+342 is a few times (and thus close to or above the Eddington limit), which is proposed by several previous papers, the parabolic jet continues up to 10 7–8 R s from the black hole, suggesting additional large-scale structures that confine the jet. NLR outflows, which may be driven by super-Eddington accretion flows, could be responsible for the large-scale jet confinement. Appendix Calibrator 0329+3510 0329+3510 is a radio source separated by 136 on the sky from 1H 0323+342. This source is a candidate to be a high-frequency peaker, which is a subclass of young radio galaxies (Dallacasa et al. 2000 ). In Figure 9 we show self-calibrated images of 0329+3510 obtained at 15, 24, and 43 GHz. The source morphology significantly changes with frequency. At 43 GHz, where the highest angular resolution is available, the source is resolved into the core (the southernmost brightest region) and a strong knot. The core and the knot are also securely resolved at 24 GHz. However, the two features are mixed in a synthesized beam at 15 GHz and the lower frequencies. This is because the knot becomes brighter as frequency decreases (i.e., an optically thin steep spectrum), while the core spectrum is relatively flat or slightly inverted (i.e., optically thick), as well as the resolution effect. This prevents us from specifying a reliable reference position in the 0329+3510 images at ≤15 GHz. Figure 9. Self-calibrated VLBA images of 0329+3510. From left to right, the images are at 43, 24, and 15 GHz,
Paper: 2017MNRAS.467.4050M (fulltext)
to see if the hint for high redshift contributions to is sharpened by future CMB polarization data. We eagerly await upcoming results from the new Planck HFI large-scale polarization data which is still proprietary to see if these observations strengthen the hint seen in the LFI data. Alternatively, these may reflect remaining systematics in the LFI data that do not also apply to the HFI data. Based on Fig. 5 , we expect that a future CV-limited experiment should be able to confirm or refute the high redshift contribution to , although we postpone a more detailed investigation of these prospects to future work. It will be extremely challenging to test the hint for non-negligible ionization fractions at z 15 by other means. The best alternative is likely redshifted 21cm surveys but these face challenges at high redshift owing to the bright galactic emission at the frequencies of interest. However, these surveys may find that the average neutral fraction rises more slowly towards high redshift than expected in models with Pop-II stars alone (see Fig. 1 ). There may be differences in the sizes of the ionized regions in these scenarios as well, which may provide a potential signature (Koh Wise 2016 ). However, the possibility of a significant contribution from Pop-III stars at high redshift may also somewhat complicate the interpretation of the 21cm power spectrum measurements (e.g. Fialkov etal. 2013 ). Another possibility may be to extract signatures of early phases of patchy reionization using the Kinetic SunyaevZeldovich effect, but these will have to push to smaller angular scales, which is challenging given foreground contamination. An extended self-regulated phase likely evades current constraints (Zahn etal. 2012 ; George etal. 2015 ) on the duration of reionization (Park etal. 2013 ). Finally, it is worth commenting on the implications of our findings for the goal of determining from the ionization history inferred from redshifted 21cm observations (Liu etal. 2016 ). This is an appealing idea, because the optical depth is an important nuisance parameter that can limit, for instance, inferences regarding the sum of the neutrino masses from upcoming CMB lensing measurements. However, this prospect becomes difficult if there are significant high redshift contributions to the optical depth, as hinted at in the Planck LFI data, which will be hard to extract from upcoming redshifted 21cm surveys. We hope that this work will encourage reionization modellers to adopt this PC analysis methodology of Hu Holder ( 2003 ) and effective likelihood of Heinrich etal. ( 2016 ). Here we have considered rather simple models for the ionization history in an effort to explore the broad-brush implications of the Planck data, but it would be interesting to explore more detailed reionization models and to combine the full information content of the CMB data with other reionization observables. It will also be interesting to explore whether dark matter
Paper: 2020ApJ...905L..31G (fulltext)
within the time span of 21–39 days after the latest outburst onset (in the absence of intense bursts), Younes et al. ( 2020b ) precisely measured a much higher spin-down rate of 3.9 × 10 −11 s s −1 . This might suggest a hysteresis in the dynamical response in these highly magnetized systems that is accompanied by changes in burst activation. The polar magnetic field strength inferred for a vacuum dipole approximation (i.e., ) of SGR J1935+2154 is about 4.4 × 10 14 G. However, our X-ray spectral modeling of the persistent emission with the STEMS3D model, which includes radiative propagation in extremely magnetized settings, yielded a local surface magnetic field strength of 9.6 × 10 14 G. This difference is not surprising since the spin-down estimate applies to the global field configuration, and can be modified by plasma loading of the magnetosphere (Harding et al. 1999 ). Nevertheless, the surface magnetic field strength being considerably larger than the inferred value suggests that there may be multipolar magnetic topology, where local field strengths are much larger than the dipolar ones. Such a circumstance was observed in SGR 0418+5729, the first “low-dipole field” magnetar. Its magnetic field strength inferred from its spin parameters is 6 × 10 12 G (Rea et al. 2010 ). Güver et al. ( 2011 ) modeled the XMM-Newton spectrum of SGR 0418−5729 with the STEMS atmospheric emission model and obtained ∼ 10 14 G for the surface magnetic field strength. They proposed a dominant nondipolar magnetic field structure for SGR 0418−5729, a picture that is consistent with the discovery of a variable proton cyclotron absorption feature in later XMM-Newton observations (Tiengo et al. 2013 ). A significant multipolar magnetic configuration for SGR J1935+2154 is also supported by the complexity of its energy-dependent pulse profiles. Its low-energy X-ray pulse profile is dominated by a broad structure with a phase width of around 0.7–0.8. However, minor structures become pronounced above ∼3 keV, in the absence of bright persistent X-ray emission ( kT = 0.5 keV) from the surface of the neutron star. The BB+BB spectral fits indicate that this putatively hotter portion emanates from smaller regions, less than ∼0.2 km in size, and perhaps analogous to multipolar field components that are observed from small regions on the Sun. These structured pulse profiles contrast the comparatively simple two-peaked forms observed for active outburst phases in another magnetar, 1RXS J170849.0−400910, which can be attributed to antipodal polar hot zones in a dipole field configuration (Younes et al. 2020a ). Extension of the pulse profile analysis of Younes et al. ( 2020a ) to treat broader surface temperature profiles in magnetic colatitude is unlikely to generate the abrupt rises and falls in consecutive phase bins evident above ∼3 keV in Figure 1 . We suggest that strong temperature gradients in magnetic longitude are also required to reproduce the observed
Paper: 2015MNRAS.451L..70M (acknowledgments)
We thank the referee, Hiroyuki Hirashita, for his insightful comments, Laura Pentericci and Daniel Schaerer for their kind clarifications. The research leading to these results has received funding from the European Research Council under the European Union (FP/2007-2013)/ERC Grant Agreement no. 306476. PD acknowledges the support of the Addison Wheeler Fellowship awarded by the Institute of Advanced Study at Durham University. UM has been funded through a Marie Curie fellowship by the European Union (FP/2007-2013), grant agreement no. 267251.
Paper: 2015ApJ...803....1N (acknowledgments)
We thank the HET resident astronomers and telescope operators for continuous support. A.N., M.o.A., B.D.-S., M.i.A. and K.K. are currently supported by NCN grant 2012/07/B/ST9/04415. M.o.A. also acknowledges the “Mobility + III” fellowship from the Polish Ministry of Science and Higher Education. A.W. was supported by the NASA grant NNX09AB36G. G.M. acknowledges the financial support from the Polish Ministry of Science and Higher Education through the Iuventus Plus grant IP2011 031971. The HET is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universität München, and Georg-August-Universität Göttingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University and the Eberly College of Science. This research has made extensive use of the SIMBAD database, operated at CDS (Strasbourg, France) and NASA’s Astrophysics Data System Bibliographic Services.
Paper: 2019A&A...630A.151P (acknowledgments)
This work has made use of the C2PAP cluster at the Leibniz-Rechenzentrum. NP is supported by the DFG cluster of excellence “Origin and Structure of the Universe”. GL acknowledges financial support from the ILP LABEX (under reference ANR-10-LABX-63) and from “Programme National de Cosmologie et Galaxies” (PNCG) of CNRS/INSU, France, and the ANR BIG4, under reference ANR-16-CE23-0002. This work was carried out within the Aquila Consortium.
Paper: 2021ApJ...911L..30M (fulltext)
pCO 2 case for a single multi-epoch case. 1 σ and 2 σ contours are included. 5. Atmospheric Retrievals To perform our retrievals we use the open-source radiative transfer and retrieval framework CHIMERA (Line Yung 2013 ; Line et al. 2013 ). It previously has been used to study the atmosphere of TRAPPIST-1e to determine the resolution that a future instrument needs to have in order to detect and constrain the abundances of molecules in the atmospheres of temperate terrestrial planets to high precision (Tremblay et al. 2020 ). Our retrieval setup is similar to that presented in Tremblay et al. ( 2020 ). For each of the combined spectra we fit for six parameters: an isothermal temperature profile ( T iso ), a radius scaling factor (x R p ), the cloud top pressure (), the mean molecular weight of the atmosphere, and the volume mixing ratio of H 2 O and CO 2 . We use the mean molecular weight (MMW) as a proxy to effectively fill the rest of the atmosphere with N 2 as this molecule is inert. 6. Results Each spectra that we retrieved had a different underlying cloud configuration, hence we wanted to determine if these physical processes impact the retrieved CO 2 abundance. The histograms presented in Figure 5 show that the retrieved abundances are consistent for each of the combined spectra, suggesting that the impact of cloud variability is not detectable with the resolution provided by JWST NIRSpec PRISM. This is further verified by the third panel, which shows consistent retrieved cloud top pressure for each spectra. While the cloud top pressure can be seen to vary in our models, this consistency in the retrieved cloud top pressures demonstrates that the precision of JWST NIRSpec PRISM will not be able to differentiate variable cloud spectra at any level of confidence. It can be seen from Figure 5 that for the CO 2 partial pressure greater than 10 −1 bars the posterior tends toward the upper prior, which is set by the physical limit of the volume mixing ratio, with the true value lying outside 1 σ . The lower partial pressures are not prior dominated and we are able to retrieve the correct volume mixing ratios within 1 σ . Further, the 10 cases for each partial pressure are consistent, suggesting that the variable clouds are not affecting the retrieved values. We are unable to constrain a water abundance due to its lack of strong spectral features in our models. Figure 5. Retrieved posterior distributions for four of the key parameters explored in this study. From top to bottom the four panels are: CO 2 abundance, H 2 O abundance, cloud top pressure, and temperature. Each colored histogram represents the retrieved parameter for one of the combined spectra (representing 10 different “observed” epochs), for a total 10 different combined spectra, each with different underlying cloud assumption. The thick solid vertical lines show the terminator-average abundance of CO 2 and H 2 O from the input models, while the dotted vertical lines represent
Paper: 2016MNRAS.463.4331D (acknowledgments)
MVdV acknowledges CNPq / Twas for financial support. EMdGDP acknowledges partial support from the Brazilian agencies FAPESP (grant no. 2013/10559-5 ) and CNPq (grant no. 300083/94-7 ). GK acknowledges support from FAPESP (grants no. 2013/04073-2 and 2013/18815-0 ) and PNPD/CAPES (grant no. 1475088 ). MVdV thanks Reinaldo Santos-Lima for fruitful discussions on different topics addressed in this paper. The authors also acknowledge the anonymous referee for a careful review. This work has made use of the computing facilities of the Laboratory of Astroinformatics (IAG/USP, NAT/Unicsul), whose purchase was made possible by the Brazilian agency FAPESP (grant 2009/54006-4 ) and the INCT-A. MVdV is grateful for the great hospitality of the Instituto de Astronomia, Geofísica e Ciências Atmosféricas (São Paulo University), where part of this work was developed.
Paper: 2018MNRAS.480..879M (acknowledgments)
ACKNOWLEDGEMENTS Part of this work is based on archival data, software, or online services provided by the Space Science Data Center – ASI. We would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, and CSD2009-00064), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia ‘Severo Ochoa’ SEV-2012-0234 and SEV-2015-0548, and Unidad de Excelencia ‘María de Maeztu’ MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382, and by the Brazilian MCTIC, CNPq, and FAPERJ. The Fermi -LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT and scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l’Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucléaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK), and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Études Spatiales in France. This work performed in part under DOE Contract DEAC02-76SF00515. The OVRO 40-m monitoring program is supported in part by NASA grants NNX08AW31G, NNX11A043G, and NNX14AQ89G, and NSF grants AST-0808050 and AST-1109911.
Paper: 2017MNRAS.467.1222H (fulltext)
the component CO lines in a merger model, measured in km s 1 . The HST images (Rix etal. 2004 ) show various clumps that indicate ALESS 122.1 and ALESS 67.1 could be mergers (Fig. 3 ). Taking the merger model and R to be 0.5arcsec (4.2kpc at z 2), which is the approximate separation of the clumps in HST optical counterparts (Fig. 3 ), the dynamical mass, M dyn sin 2 i , is 510 11 M for both ALESS 122.1 and ALESS 67.1. Figure 3. The CO(10) velocity structure of ALESS 122.1 (left) and ALESS 67.1 (right), overlaid on HST z band ( F 850 LP ) images from Rix etal. ( 2004 ) 3 . Both optical counterparts are clumpy or complex in the rest-frame UV, indicating either structured dust or a possible merging system. Blue contours indicate the CO(10) emission integrated from 300 to 0kms 1 at 3, 5, 7.... Red contours indicate the CO(10) emission integrated from 0 to 300kms 1 at 3, 5, 7.... Red and blue crosses mark the centroid of the blueshifted and redshifted emission, respectively. The images are 2020arcsec. However, the HST image does not reveal whether or not the systems contain a gaseous disc. In the presence of a gas disc, the dynamical mass can be estimated from the CO line kinematics, by comparing the spatial offset between the redshifted and blueshifted components of the CO line. This was determined by making 300kms 1 wide channel maps centred at 300 to 0kms 1 and 0 to 300kms 1 (Fig. 3 ). The centroid of the CO emission was determined for the maps, and we derive a spatial offset between the redshifted and blueshifted emissions of 1.20.6arcsec (10.25.1kpc) and 1.8 0.5arcsec (15.24.2kpc) for ALESS 122.1 and ALESS 67.1, respectively. This is comparable to CO(10) sizes observed in other SMGs by Ivison etal. ( 2011 ). Assuming this spatial offset represents rotating gas, then the dynamical mass M dyn sin 2 i = (2.11.1)10 11 M and (3.20.9)10 11 M for ALESS 122.1 and ALESS 67.1, respectively. These estimates are consistent with the dynamical masses derived from using the CO line FWHM and optical size from HST imaging. For a rotating model, Bothwell etal. ( 2013 ) found their sample of SMGs to have a median dynamical mass of (1.60.3)10 10 R M , where radius R is in kpc. Using the measured spatial offsets of 10 and 15kpc for R , the dynamical masses of ALESS 122.1 and ALESS 67.1 are consistent with the median dynamical mass of their SMG sample. The total baryonic mass can be calculated by combining the gas and stellar mass estimates for the SMGs. The stellar masses of ALESS 122.1 and ALESS 67.1 have been estimated by Simpson etal. ( 2014 ), who used absolute rest-frame H -band magnitudes from best-fitting SEDs to multiband photometry and a model mass-to-light ratio. They estimate ALESS 122.1 has a stellar mass of 5.210 10 M and ALESS 67.1 has a stellar mass of 4.410 10 M . These estimates are uncertain by a factor of at least a few, due to the difficulty in distinguishing between different model SF histories to predict an accurate mass-to-light ratio
Paper: 2018ApJ...854...52S (acknowledgments)
We thank Tony Piro for his encouragement, Stefan Taubenberger for providing access to data, and Carles Badenes, Stéphane Blondin, Hector Martínez-Rodríguez, Alison Miller, Rüdiger Pakmor, Stuart Sim, and Frank Timmes for helpful discussions. K.J.S., D.M.T., and B.J.M. received support from the NASA Astrophysics Theory Program (NNX15AB16G and NNX17AG28G). D.K. is supported in part by a DOE Office of Nuclear Physics Early Career Award, and by the Director, Office of Energy Research, Office of High Energy and Nuclear Physics, Divisions of Nuclear Physics, of the US DOE under Contract No. DE-AC02-05CH11231. This research used the Savio computational cluster resource provided by the Berkeley Research Computing program at the University of California, Berkeley (supported by the UC Berkeley Chancellor, Vice Chancellor of Research, and Office of the CIO), high-performance computing resources provided by the University of Alabama, and resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the US DOE under Contract No. DE-AC02-05CH11231. Software: MESA (v8845; Paxton et al. 2011 , 2013 , 2015 ), FLASH (v4.2.2; Fryxell et al. 2000 ; Dubey et al. 2009 ), SEDONA (Kasen et al. 2006 ).