adsabs/WIESP2022-NER huggingface dataset:
Paper: 2017ApJ...835..113L (fulltext)
clarity only scales are shown. Left: total fraction of fake sources recovered as a function of input H 160 -band magnitude. Recovery of faint sources is improved with the wavelet subtraction method. Bright sources are lost as they are subtracted in the wavelet decomposition process; to ensure that we can detect bright as well as faint sources, we therefore use both the original and wavelet-subtracted images for source detection. Middle: recovered−input magnitudes of fake sources as a function of input magnitudes for sources detected in the original and wavelet-subtracted images, but all photometry measured in the original image. The accuracy of photometry is noticeably affected when the objects are detected in images subtracted to scale 3. Right: same as the middle panel, but with photometry measured in the wavelet-subtracted images. Here, we recover systematically fainter magnitudes, as part of the light of some of the galaxies is subtracted during the wavelet subtraction procedure. We also note that detection in the wavelet-subtracted images is hampered for bright galaxies as they get removed when we perform the subtraction to smaller scales. Although we do not expect to find any high-redshift galaxies in this regime, we nonetheless choose to combine catalogs from the wavelet-subtracted and original images in order to ensure that we include potential bright or extended sources. 4. Source Selection We detect galaxies in these fields using SExtractor in dual image mode, where one detection image is used to measure photometry in each of the seven available HST filters. In order to maximize our sensitivity to faint high-redshift galaxies at a range of different colors, we use 11 different detection images: each of the four HST /WFC3 filters , plus seven stacked combinations of these images: , , , , , , and . We carry out this process with detection in both the original PSF-matched images and the wavelet-subtracted ones, for a total of 22 detection images. In all cases, photometry is measured from the original, PSF-matched images in all seven filters, as well as from the wavelet-subtracted images. We use the wavelet-subtracted photometry where it is within 1 σ of the photometry from the original image in every band, because the signal-to-noise ratio is higher, especially in the central regions of the clusters. Where the photometry differs (i.e., where some part of the Galaxy has been subtracted in the wavelet decomposition process), we use the photometry from the original image. We also visually inspect every galaxy to ensure that no part of the Galaxy has been subtracted; we find that all partially subtracted galaxies have photometry that differs by between the original and wavelet-subtracted images, so the original image photometry is used. We then combine our 22 catalogs into a single master catalog, selecting unique sources within a matching radius of 02. We measure photometry in the small Kron aperture flux, with the SExtractor parameter
Paper: 2018MNRAS.481.2548G (acknowledgments)
ACKNOWLEDGEMENTS We would like to thank the anonymous referee and the journal’s editorial team for their work in improving the text. In addition, the authors would like to thank Simon Glover, Thomas Greif, Sacha Hony, Ben Keller, Eric Pellegrini, Daniel Rahner, and Stefan Reissl for their useful comments and discussions during the preparation of this work. This work was granted access to HPC resources of CINES under the allocation x2014047023 made by GENCI (Grand Equipement National de Calcul Intensif). The authors acknowledge support by the High Performance and Cloud Computing Group at the Zentrum für Datenverarbeitung of the University of Tübingen, the state of Baden-Württemberg through bwHPC and the German Research Foundation (DFG) through grant no INST 37/935-1 FUGG. This work has been funded by the European Research Council under the European Community’s Seventh Framework Programme (FP7/2007-2013). SG and RSK have received funding from grant agreement no. 339177 ( starlight ) of this programme. RSK further acknowledges support from the Deutsche Forschungsgemeinschaft in the Collaborative Research Centre SFB 881 ‘The Milky Way System’ (subprojects B1, B2, and B8) and in the Priority Program SPP 1573 ‘Physics of the Interstellar Medium’ (grant nos KL 1358/18.1 and KL 1358/19.2). PH has received funding from grant agreement no. 306483. JR acknowledges support from the ORAGE project from the Agence Nationale de la Recherche, grant ANR-14-CE33-0016-03.
Paper: 2020A&A...633A..21R (fulltext)
abundance of polycyclic aromatic hydrocarbons (PAHs; Geers et al. 2009 ). Because of these drawbacks and the chemical complexity, we restrict our model to EUV and X-ray dominated heating. 3 Numerical model All simulations of this paper are two-dimensional axisymmetric, including the toroidal velocity and magnetic field component (i.e., 2.5 dimensional). They were carried out with the PLUTO code (version 4.3) ( Mignone et al. 2007 , 2012 ), which allows solving the MHD equations on a spherical grid, including ohmic resistivity. Throughout this section, we present the basis of the numerical model, that is, the X-ray and EUV heating approach, disk structure, magnetic field, and dynamic treatment of ohmic diffusion. 3.1 MHD equations Relevant equations are the conservation of mass, the conservation of momentum, the energy equation, and the induction equation, where P is the thermal gas pressure, ρ the gas density, B the magnetic flux density vector, J the electric current density vector, η the ohmic diffusion coefficient, v the gas velocity vector, and the gravitational potential. To update the cells, the HLLD Riemann solver ( Miyoshi Kusano 2005 ) was used. To ensure the condition ∇ ⋅ B = 0, the divergence cleaning method ( Dedner et al. 2002 ) was applied. All simulations were evolved with an adiabatic equation of state, using an isentropic exponent of κ = 5∕3. Fig. 1 Ionization parameter–temperature relation based on the data in Picogna et al. (2019) . 3.2 Diagnostics The relativestrength of the magnetic field can be expressed with the dimensionless plasma parameter β : which is the ratio of thermal pressure over magnetic pressure. In order to evaluate the nonideal MHD effects (ohmic diffusion) on possible MRI activity, the notion of an ohmic Elsasser number Λ Ω ( Turner et al. 2007 ) is useful: Here v A is the Alfvén velocity and η the ohmic diffusion coefficient. Generally, MRI is considered to be suppressed for Λ Ω ≲ 1. The integrated mass-loss rate caused by the wind is computed by the expression and the disk region is excluded from the range in θ . Here, v R denotes the radial velocity component of the flow. 3.3 EUVand X-ray heating Following the approach of Owen et al. (2010 , 2012 , 2013 ), X-ray heating was provided by using a fitted ionization parameter - temperature relation T = f ( ξ ), taken from Picogna et al. (2019) . In addition to the previously studied models, the temperature curves depend on the local column density, as shown in Fig. 1 . Knowing the dependence of the temperature on the local variables, we traced rays from the inner simulation boundary radially outward up to column densities of 5 × 10 22 cm −2 . Within this range, the temperatures were set corresponding to the locally computed ionization parameter using the fitted relation f ( ξ ). With intermediate column densities, the temperature is linearly interpolated. The temperature adjustment was only invoked when the temperature computed by the ionization model was
Paper: 2019ApJ...875..130L (fulltext)
have a Ly α luminosity of . It was the first SMG detected in CO, revealing it to contain a massive reservoir of molecular gas ( M ⊙ , Frayer et al. 1998 ). This gas reservoir was later shown to cover a large volume and contain multiple, merging galaxies (Ivison et al. 2010 ), one of which is a dusty, broad-absorption-line (BAL) quasar (Villar-Martín et al. 1999a , 1999b ; Vernet Cimatti 2001 ; Frayer et al. 2018 , e.g., Genzel et al. 2003 ). The existence of a large reservoir of diffuse molecular gas has been recently inferred by observations of the CH + cation (E. Falgarone et al. 2019, in preparation), following the detections against several other SMGs (Falgarone et al. 2017 ). Inspired by these earlier results, we observed the system with KCWI tuned to the Ly α nebula and directed to cover it and its neighboring galaxies and quasar. To our surprise, the data reveal a new, luminous Ly α source—the primary focus of this paper, which is structured as follows. We describe our KCWI observation and data reduction process in Section 2 . In Section 3 , we present the detection of the ≳100 kpc Ly α nebula powered by this system and the discovery of a new dark cloud illuminated by the nearby BAL QSO. Finally, we discuss the Ly α nebula and the physical interpretations of the newly discovered dark galaxy in Section 4 , and give a brief summary in Section 5 . Throughout this paper, we assume a flat cosmological model with and , which implies the physical scale is ≈7.85 kpc per arcsec at the redshift of SMM J02399−0136. We follow the naming convention presented in Ivison et al. ( 2010 ): L1 marks the BAL quasar; L2 is a low-surface-brightness companion to the east of L1; L2SW is a massive, extremely luminous and dust-obscured starburst galaxy, east–south–east of L1 and south–west of L2; L1N is a faint, compact northern component, visible in post-SM2 HST imaging. 2. Observations and Data Reduction 2.1. KCWI Observations The KCWI observations of SMM J02399 were carried out on UT 2017 October 21 (seeing ∼15) using KCWI on the Keck II telescope of the W. M. Keck Observatory in Hawaii. We used the BM1 grating and the medium slicer (slice width ∼07), which yields an IFU datacube with FoV of 20′′ × 168 (pixel scale of 03 × 07) centered on J023951.88−013558.0, the quasar optical position given by Ivison et al. ( 1998 ). The grating was tilted to give a central wavelength of 4620 Å and provides a spectral resolution, R ≈ 4000. The good wavelength coverage is ∼4230–5010 Å. The total on-source exposure time is four 10-minute exposures, each dithered by ∼06. For sky observations, we used an “offset-target-field” to construct the sky datacube. The offset-target has a different redshift and is located ∼2 degrees from SMM J02399. It is a compact point source at the Ly α wavelength of SMM J02399. To convert the spectral images and calibration frames (arcs, flats, bias) to a calibrated datacube, we used the IDL-based KCWI data reduction pipeline. 11 11 Available at
Paper: 2019A&A...627A..48H (acknowledgments)
Acknowledgements We thank Brad Foley for his constructive review, which greatly helped to improve this paper. D.H. has been supported through the NWA StartImpuls and N.T. has been supported by the Helmholtz Association (project VH−NG−1017) and by the German research foundation (DFG) through the priority programs 1922 “Exploring the diversity of extrasolar planets” (TO 704/3-1) and 1883 “Building a habitable Earth” (TO 704/2-1).
Paper: 2016MNRAS.463.3204R (acknowledgments)
This work is part of the research project entitled ‘Dynamical Analysis, Advanced Orbit Propagation and Simulation of Complex Space Systems’ (ESP2013-41634-P) supported by the Spanish Ministry of Economy and Competitiveness. The author has been funded by a ‘La Caixa’ Doctoral Fellowship for he is deeply grateful to Obra Social ‘La Caixa’. The present paper would not have been possible without the selfless help, support, and advice from Prof. Jesús Peláez. An anonymous reviewer made valuable contributions to the final version of the manuscript.
Paper: 2018ApJ...869...24I (fulltext)
especially when high consistency is required for large-scale surveys like DESI. Further discussion of the VPH grating physics is given by Barden et al. ( 1998 ). 2.1. Requirements and Specifications The DESI VPH gratings have physical dimensions of 180 × 160 mm 2 × 16 mm (thickness) with varying clear aperture areas. The incident field of view (FOV) of the grating is ±75 from the grating central axis, illustrated in Figure 2 , and is illuminated by a collimated beam of various pupil sizes. All DESI VPH gratings are optimized such that the +1 diffracted order efficiency is maximized. There were no specifications on off-axis FOV efficiency. The performance requirements and specifications for the DESI VPH gratings are detailed in Table 1 . These are driven by both science requirements and optical design limitations. Efficiency requirements listed are averaged over polarization and over the clear aperture. Since the actual measurements of the diffraction efficiency will include transmission losses from the VPH gelatin, glue, antireflection (AR) coating, and the substrate glasses, the “adjusted” efficiencies are used to compare results. A total of 36 full-size gratings (12 per channel) were produced by Kaiser Optical Systems Inc. (KOSI). A preliminary set of measurements was conducted by KOSI on a few points across the clear aperture (Figure 4 ), albeit in a less comprehensive manner compared to our measurements presented here. Based on our measurements, the top performing gratings in each channel with the best efficiencies are chosen for DESI integration. Table 1 DESI VPH Grating Specifications and Requirements for Unpolarized Incidence; Wavefront Specifications at 632 nm Notes. a Incidence angles are to be within an allowed installation range of ±10 from the specified α 0 (Edelstein et al. 2018 ). b Including glue and gelatin losses, not including AR coating and glass transmission losses. c Adjusted for glue, gelatin, AR coating, and glass transmission losses. We compare measurements to these values. 2.2. Preliminary Evaluation of Test Gratings Prior to the full production of the DESI VPH gratings, preliminary performance studies were conducted on full-size test VPH gratings for each bandpass, also produced by KOSI. Measurements were made in all three bandpasss to verify that the gratings met desired design specifications and also to prototype a set of reliable and efficient test procedures discussed in this paper. Efficiency performance at the specified incidence angle and the peak-to-valley (P-V) WFE for power and irregularity met the requirements (DESI Collaboration et al. 2016b ). Performance results of the test gratings were used to constrain the properties of the final DESI VPH gratings discussed in this paper. 3. Measurement Rig We built an automated optical test bench to measure the +1 order diffraction efficiency of the gratings. The design was motivated by the desire to conduct a comprehensive yet efficient performance
Paper: 2017A&A...600A..22M (acknowledgments)
Part of the calculations were performed with the high-performance computing facility MESOCENTRE, hosted by OCA. We are grateful to Nicolas Prantzos for useful suggestions that improved the content of this article. We thank the anonymous referee for her/his constructive comments. T. Masseron and B. Plez were particularly kind in providing us with some molecular data. We appreciate that D. Romano, C. I. Johnson, and C. Kobayashi kindly shared their model data. This work was partly supported (Š.M.) by the grant from the Research Council of Lithuania (LAT-16019).
Paper: 2018MNRAS.477.4454H (acknowledgments)
ACKNOWLEDGEMENTS The authors thank the anonymous referee for a careful reading and for useful and detailed comments which improved the quality of the paper. PHB thanks the Institut Universitaire de France for its support. DRF acknowledges support from STFC (ST/L00075X/1), including provision of local computing resources. This work has been supported by the Agence Nationale de la Recherche (ANR-HYDRIDES), contract ANR-12-BS05-0011-01.
Paper: 2018MNRAS.476.2918K (acknowledgments)
Acknowledgements This research was supported in part by the Polish Ministry of Science and Higher Education under grant 0149/DIA/2013/42 within the Diamond Grant Programme for years 2013–2017 and by the Polish National Science Centre under grant 2013/10/A/ST9/00023. MV acknowledges support from HST-AR-13890.001, NSF awards AST-0908346, AST-1515001, NASA-ATP award NNX15AK79G.
Paper: 2019MNRAS.482L..60W (acknowledgments)
ACKNOWLEDGEMENTS We thank M. Begelman, A. Beloborodov, E. Quataert, K. Parfrey, L. Sironi, A. Spitkovsky, and V. Zhdankin for fruitful discussions. This work was supported by DOE grant DE-SC0008409, NASA grants NNX17AK57G and NNX16AB28G, NSF grant AST-1411879, and NASA through Einstein Postdoctoral Fellowship grant PF7-180165 awarded to AP by the Chandra X-ray Center, operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS803060. The simulations presented in this paper used computational resources of the NASA/Ames HEC Program and XSEDE/Stampede2 (allocation PHY140041) (Towns et al. 2014 ). DAU gratefully acknowledges the hospitality of the Inst. for Advanced Study and support from the Ambrose Monell Foundation.
Paper: 2018A&A...609A..62B (fulltext)
broadband SEDs, 19 with GROND and 3 with optical and NIR data from different instruments. For the rest of the GRBs at , we collected measurements from the literature if available; these measurements are listed in Table 3 . 4. Results The results, i.e., the best-fit models and parameters, from fitting the combined NIR, optical, and X-ray SEDs with the local extinction curves are summarized in the top portion of Table 2 and a plot containing all the SEDs is shown in Fig. 7 . As mentioned above, the SEDs of the 10 GRBs that show evidence for a small to medium amount of dust ( mag) were also fitted with the SN extinction curve. These SEDs are additionally plotted in Fig. 8 , in comparison to the best results from the local extinction curves (zoomed into the optical and NIR regime; the full plot is displayed in Fig. C.1 ). The corresponding parameters are given in the bottom portion of Table 2 . With these measurements we increase the number of determined values for GRBs at by a factor of 2–3. As previously observed for GRBs at lower redshift, the local extinction curves provide a good fit to the data, with the featureless SMC extinction curve usually best describing the observed magnitudes ( Greiner et al. 2011 ; Zafar et al. 2011a ). We find that from the 22 modeled GRBs at , 16 are best fit with the SMC and only 6 are best fit with the LMC or MW extinction curve. In contrast to other samples with GRBs at mostly , however, we find that all of the GRBs are only behind small to medium dust column densities ( mag) within their host galaxies line of sight, which is also true for the values collected from the literature (see Table 3 ). The distribution of our best-fit values compared to those from the unbiased samples from Greiner et al. (2011) and Covino et al. (2013) and the data from Zafar et al. (2011a) , based on the GRB sample from Fynbo et al. (2009) , is shown in Fig. 9 . While all of these samples include a % of GRBs with mag (and 3–5% with mag), only % of our GRBs at redshift have a visual extinction of mag and the remaining % have mag. A two-sample Kolmogorov-Smirnov test returns a rejection probability of % for the null hypothesis that the values from our GRBs at and those from Greiner et al. (2011) are drawn from the same sample. Considering the 10 SEDs that were also fitted with the SN extinction curve, we find that, besides GRB 090205 and 090516, the goodness of fit is comparable to the result from the local extinction curves, while for two of the bursts, GRB 140428A and 151027B, the SN extinction curve provides a better fit to the data. In case of GRB 140428A, the somewhat flat SED between the and band can be identified with the flattening between (rest-frame) 3000 and 1700 Å of the SN extinction curve () or as a small (rest-frame) 2175 Å feature when fitting the MW extinction curve (). This result is consistent with that from fitting the GROND SED to determine a photometric redshift, where we also find that the SN extinction curve is
Paper: 2020ApJ...901..156N (fulltext)
for a realistic simulated pulsar. Apart from different f - and -scales, the corresponding plot for the semicoherent mismatch looks very similar. The mismatch agrees well with its metric approximation for mismatch m ≤ 0.5, which is typical: in Appendix B , we show that the highest sensitivity at given computing cost for an elliptical search is obtained with an average mismatch (see Table B1 ). Figure 3. Comparison of the coherent metric approximation to the actual mismatch, for parameters of a simulated eccentric orbit binary pulsar in 4FGL J0523.3−2527. Blue contours show the actual mismatch and red contours the metric approximation, at m = 0.25 and 0.5. The sky position parameters { n x , n y } are not shown in Figure 3 because we assume that for spider pulsars they are known to high precision from optical observations. A partially informed search for binary pulsars in elliptic orbits, without exact information about the sky position and constraints on the orbital parameters, is computationally impossible. There are too many parameter space dimensions—even for circular orbits with reasonable parameter ranges, the grid has too many points. To make a search possible, one needs tight constraints derived from optical/X-ray observations of the pulsar’s companion star. In the next section, we will discuss constraints and the search design for the probable eccentric orbit binary gamma-ray pulsar in 4FGL J0523.3−2527 (Strader et al. 2014 ; Saz Parkinson et al. 2016 ). 4.2. Search Design for Low-eccentricity Binary In this section, we discuss how to reduce the search parameter space using orbital constraints for the gamma-ray source 4FGL J0523.3−2527, presumed to be a pulsar in an eccentric binary orbit. The source is named 3FGL J0523.3−2528, 2FGL J0523.3−2530, or 1FGL J0523.5−2529 in previous LAT source catalogs. This is similar to the circular example of Section 3.2 . The gamma-ray source itself was investigated by Saz Parkinson et al. ( 2016 ) and ranked ninth highest in a list of most significant 3FGL unassociated sources predicted to be pulsars. It shows typical pulsar-like properties: the photon flux is stable over time, and the spectrum is fit by an exponential cutoff power law. The source is not in the Galactic disk, which increases the odds that it hosts an MSP. Earlier optical observations identified a likely companion and indicate an orbit with small, but not negligible, eccentricity of (Strader et al. 2014 ). In contrast to the previous paragraph, this suggests that the pulsar is a YP, because binary MSPs tend to have rather circular orbits (Phinney 1992 ). The frequency and spin-down search ranges are chosen following the logic of the previous search design (Section 3.2 ). For YPs we search f ∈ [0, 44] Hz and . For MSPs we search f ∈ [44, 1500] Hz and . The f -dimension is efficiently searched using FFTs with bandwidth f BW = 8 Hz, and the -dimension is covered by a uniformly spaced lattice. The sky position search range of the probable