adsabs/AstroCLIMB huggingface dataset:
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: As in Figure 13, in terms of the total number of events rather than detection fraction, using ﹩{{ \mathcal R }}_{0,\mathrm{BNS}}=105.5\,{\mathrm{Gpc}}^{-3}{\mathrm{yr}}^{-1}﹩. Except for the panel showing the distribution of the S/N, only the events whose Fisher matrix could be reliably inverted are included.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Redshift distributions of the NSBHs observed at ET alone, selected on the basis of different thresholds for the S/N (left panel), or setting S/N ≥ 12 and applying further cuts on Δd  L /d  L  (central panel), or on ΔΩ90% (right panel). The black solid line corresponds to the total NSBH population in the astrophysical model that we have assumed. We set ﹩{{ \mathcal R }}_{0,\mathrm{NSBH}}=45\,{\mathrm{Gpc}}^{-3}\,{\mathrm{yr}}^{-1}﹩, and show the results for the detections in 1 yr (taking into account our assumptions of the duty cycle). Given the current uncertainly on ﹩{{ \mathcal R }}_{0,\mathrm{NSBH}}﹩, one should keep in mind that the absolute number can still change by a factor ﹩{ \mathcal O }\left(3\right)﹩. In each column, the upper panel shows the number of events per redshift bin, while the lower panel shows the corresponding cumulative distributions, normalized to the number of BNS events in our sample, N NSBH = 4.5 × 104.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Cumulative distributions of the event fraction for BNS signals as function of S/N (for LVK-O4, ET and ET+2CE) and as a function of parameter errors (for ET and ET+2CE), using the waveform model IMRPhenomD_NRTidalv2.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Scatter plots of the observed BNS population at 3G detectors. On the top row, we report the results for ET alone; and in the bottom, for the ET+2CE network. In each row, the left panel shows the distribution of errors on the luminosity distance and sky location as a function of redshift; the central panel, the distribution of errors on the luminosity distance and detector-frame chirp mass as a function of redshift; and the right panel, the distribution of errors on the source-frame chirp mass and adimensional tidal deformability as a function of the total source-frame mass. The numbers reported on the dashed lines refer to the fraction of observed events lying inside the corresponding region.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: As in Figure 20, for ET+2CE.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: As in Figure 15, for ET+2CE.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Cumulative distributions of the S/Ns (for LVK-O4, ET, and ET+2CE) and parameter errors (for ET and ET+2CE) for NSBH signals, using the waveform model IMRPhenomNSBH.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: As in Figure 18, in terms of the total number of events rather than detection fraction.
Paper: Constraining Sterile Neutrino Dark Matter in the Milky Way Halo with Swift-XRT
Authors: Dominic Sicilian, Dannell Lopez, Massimo Moscetti, Esra Bulbul, Nico Cappelluti
Figure caption: Constraints on the sin2(2θ) vs. ﹩{m}_{{\nu }_{s}}﹩ parameter space. The red “MW Sat.” region represents Dekker et al.'s (2021b) study of small-scale structure, the dark gray “XMM” region indicates Foster et al. (2021), and the green “NuSTAR” region represents Neronov et al. (2016a), Perez et al. (2017), Ng et al. (2019), Roach et al. (2020), and Roach et al. (2022). Dashed gold represents the conservative Sicilian et al. (2020) Chandra constraint, while solid gold is the more aggressive constraint, with the gap between them representing NFW uncertainty. As described in the text, our Swift constraints are plotted in a similar way, with the uncertainty region appearing translucent while the region above the dashed conservative limit is solid. Purple and cyan data points show notable ∼3.5 keV line detections. Adapted from Ng et al. (2019), Roach et al. (2020), and Sicilian et al. (2020).
Paper: Constraining Sterile Neutrino Dark Matter in the Milky Way Halo with Swift-XRT
Authors: Dominic Sicilian, Dannell Lopez, Massimo Moscetti, Esra Bulbul, Nico Cappelluti
Figure caption: The Swift line intensity upper-limit profile plotted alongside existing constraints, prior detections, and two example NFW-predicted profiles for reference. The gray profile was computed by Cappelluti et al. (2018; using Nesti & Salucci’s 2013 parameters) while the green profile was computed by Boyarsky et al. (2018; using McMillan’s 2017 parameters). Shaded regions for both represent 2σ uncertainty ranges. Adapted from Sicilian et al. (2020).
Paper: Constraining Sterile Neutrino Dark Matter in the Milky Way Halo with Swift-XRT
Authors: Dominic Sicilian, Dannell Lopez, Massimo Moscetti, Esra Bulbul, Nico Cappelluti
Figure caption: Data points indicate line significances when fitted at the discrete energies analyzed across the continuum. Connecting lines are used to enhance visualization.
Paper: Radio Pulse Profiles and Polarization of the Terzan 5 Pulsars
Authors: Ashley R. Martsen, Scott M. Ransom, Megan E. DeCesar, Paulo C. C. Freire, Jason W. T. Hessels, Anna Y. Q. Ho, Ryan S. Lynch, Ingrid H. Stairs, Yuankun Wang
Figure caption: Calibrated flux densities at 1750 MHz for Ter5C, O, ae, and Z, shown on a log scale (see Section 2.5). Statistical errors, when visible, are shown by a vertical bar. There is no obvious correlation between the pulsars, including for Ter5ae and Ter5Z, which are the closest pair of pulsars in Terzan 5 on the sky, with a 0.″47 separation.
Paper: Radio Pulse Profiles and Polarization of the Terzan 5 Pulsars
Authors: Ashley R. Martsen, Scott M. Ransom, Megan E. DeCesar, Paulo C. C. Freire, Jason W. T. Hessels, Anna Y. Q. Ho, Ryan S. Lynch, Ingrid H. Stairs, Yuankun Wang
Figure caption: Pseudo-luminosity (L 1400) vs. cumulative number of pulsars with pseudo-luminosity greater than that luminosity. A line with slope of −1 (not a fit) has been plotted in orange to compare to the trend of the data. A turnover at low luminosity is evident below ∼1 mJy kpc2, implying incompleteness in our searches, and that additional pulsars likely exist in the cluster.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: We show a snapshot of the weakly magnetized (SANE) simulation at t = 1.3 × 105 r g/c. The top row shows a vertical slice of the gas density and the plasma-β (≡p gas/p mag), while the bottom row shows the midplane cross section. The black lines correspond to the velocity streamlines and the cyan lines denote the magnetic field lines. The disk exhibits laminar gas inflow in the midplane punctuated by small-scale turbulent eddies as seen from the plasma-β.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: Same as Figure 1, but for the MAD simulation at t = 2.9 × 105 r g/c. In contrast to that in the SANE model, the inflow is broken up by outgoing magnetic flux tubes and accretion occurs via interchange instabilities. We also see a wider polar vacuum region and a vertically thinner accretion flow near the BH due to the presence of strong vertical magnetic fields.
Paper: Constraints on Cosmological Parameters with a Sample of Type Ia Supernovae from JWST
Authors: Jia Lu, Lifan Wang, Xingzhuo Chen, David Rubin, Saul Perlmutter, Dietrich Baade, Jeremy Mould, Jozsef Vinko, Enikő Regős, Anton M. Koekemoer
Figure caption: From the upper left clockwise, the panels show the constraints on Ω m , w 0, and w  a  of the flat w 0 w  a CDM model with the statistical errors of the Pantheon binned data reduced by a factor of 1, ﹩\sqrt{8}﹩, 4, and 8. The gray contours show the confidence levels constrained by the Pantheon binned data only; the orange contours show those with the inclusion of the VHZ SNe Ia. The gray and orange vertical dashed lines show the 1σ confidence levels of the Pantheon binned data only and those of the combined data, respectively. The numbers of the image titles show the 1σ confidence of the combined data. The contour levels are 1σ, 2σ, and 3σ with decreasing color weight.
Paper: Constraints on Cosmological Parameters with a Sample of Type Ia Supernovae from JWST
Authors: Jia Lu, Lifan Wang, Xingzhuo Chen, David Rubin, Saul Perlmutter, Dietrich Baade, Jeremy Mould, Jozsef Vinko, Enikő Regős, Anton M. Koekemoer
Figure caption: Clockwise from the upper left, contours showing cosmological constraints with (orange) and without (gray) the VHZ SN Ia data, for the ΛCDM, w 0 w  a CDM, and flat w 0 w  a CDM, wCDM models. The titles in each panel show the central values of the cosmological parameters and their 1σ uncertainties for the joint Pantheon and VHZ SN Ia data set. The contour levels are 1σ, 2σ, and 3σ with decreasing color weight.
Paper: Constraints on Cosmological Parameters with a Sample of Type Ia Supernovae from JWST
Authors: Jia Lu, Lifan Wang, Xingzhuo Chen, David Rubin, Saul Perlmutter, Dietrich Baade, Jeremy Mould, Jozsef Vinko, Enikő Regős, Anton M. Koekemoer
Figure caption: From the upper left clockwise, the panels show the constraints on Ω m  and ΩΛ of the ΛCDM model with the statistical errors of the Pantheon binned data reduced by a factor of 1, ﹩\sqrt{8}﹩, 4, and 8. The gray contours show the confidence levels constrained by the Pantheon binned data only, and the orange contours show those with the inclusion of the VHZ SNe Ia. The gray and orange vertical dashed lines show the 1σ confidence levels constrained by the Pantheon binned data only and those of the combined data, respectively. The numbers of the image titles show the 1σ confidence of the combined data. The contour levels are 1σ, 2σ, and 3σ with decreasing color weight.
Paper: Constraints on Cosmological Parameters with a Sample of Type Ia Supernovae from JWST
Authors: Jia Lu, Lifan Wang, Xingzhuo Chen, David Rubin, Saul Perlmutter, Dietrich Baade, Jeremy Mould, Jozsef Vinko, Enikő Regős, Anton M. Koekemoer
Figure caption: Top: Hubble diagram of the Pantheon unbinned and binned data and the mock VHZ SNe Ia , and the best-fit flat ΛCDM model of the Pantheon data. Bottom: the residuals of the Pantheon and VHZ SN Ia data after the subtraction of the best-fit flat ΛCDM cosmology.
Paper: Constraints on Cosmological Parameters with a Sample of Type Ia Supernovae from JWST
Authors: Jia Lu, Lifan Wang, Xingzhuo Chen, David Rubin, Saul Perlmutter, Dietrich Baade, Jeremy Mould, Jozsef Vinko, Enikő Regős, Anton M. Koekemoer
Figure caption: Redshift distribution of Pantheon SNe Ia and the mock VHZ Data.
Paper: Formation and Eruption of Hot Channels during an M6.5 Class Solar Flare
Authors: Yanjie Liu, Yingna Su, Rui Liu, Jialin Chen, Tie Liu, Haisheng Ji
Figure caption: Morphological evolution at the first flare precursor. (a)–(i) Multi-wavelength images acquired by SDO/AIA 131  and 304 Å, BBSO/GST Hα center line. The magenta dashed lines in panels (a)–(c) draw the outer edge of the seed hot channels during the first precursor. The yellow curve in panel (a) marks the main PIL of the active region. The white box in panel (d) represents the FOV of panels (g)–(i), the blue arrows mark the two filaments observed in AIA 304 Å, and the green dashed boxes frame the brightenings that appear on both sides of the PIL. The white and black contours in panel (f) show the photospheric positive and negative magnetic fields taken by SDO/HMI at 17:33:30 UT.
Paper: Formation and Eruption of Hot Channels during an M6.5 Class Solar Flare
Authors: Yanjie Liu, Yingna Su, Rui Liu, Jialin Chen, Tie Liu, Haisheng Ji
Figure caption: Morphological evolution at the second flare precursor. (a)–(i) Multi-wavelength images acquired by SDO/AIA 131 and 304 Å, BBSO/GST Hα center line. The magenta dashed lines in panels (a)–(c) draw the outer edge of the seed hot channels during the second precursor. The white box in panel (d) represents the FOV of panels (g)–(i). The green dashed boxes frame the brightenings that appear on both sides of the PIL.
Paper: A Red Giants’ Toy Story
Authors: Marcelo M. Miller Bertolami
Figure caption: Temperature stratification of the 1M ⊙ full evolutionary model (FEM) near the He flash. Green and cyan lines indicate the corresponding temperature stratification when the same chemical structure is fixed and the gravothermal energy release is relaxed to zero ϵ  g  = 0 (green), and when in addition to setting ϵ  g  = 0 neutrino energy losses are also set to zero.
Paper: A Red Giants’ Toy Story
Authors: Marcelo M. Miller Bertolami
Figure caption: Impact of very deep convection on the luminosity and radius of the star.
Paper: A Red Giants’ Toy Story
Authors: Marcelo M. Miller Bertolami
Figure caption: Density and temperature profiles of the 1M ⊙ model (Z = 0.02) for different core masses. Black dots indicate the location of the peak of the H-burning shell of each model.
Paper: A Red Giants’ Toy Story
Authors: Marcelo M. Miller Bertolami
Figure caption: Density profiles of the 1M ⊙ model (Z = 0.02) as a function of the Lagrangian coordinate m(r). Black dots indicate the location of the peak of the H-burning shell of each model.
Paper: A Red Giants’ Toy Story
Authors: Marcelo M. Miller Bertolami
Figure caption: Envelope integration for different values of ﹩{\mathbb{C}}﹩ and y +, for t + = 0.75 and for a Thomson scattering–like opacity.
Paper: A Red Giants’ Toy Story
Authors: Marcelo M. Miller Bertolami
Figure caption: Envelope integration for different values of ﹩{\mathbb{C}}﹩ and y +, for t + = 0.5 and for a Kramers’ opacity.
Paper: A Red Giants’ Toy Story
Authors: Marcelo M. Miller Bertolami
Figure caption: Envelope integration for different values of ﹩{\mathbb{C}}﹩ and y +, for t + = 1.5 and for a Kramers’ opacity.
Paper: A Red Giants’ Toy Story
Authors: Marcelo M. Miller Bertolami
Figure caption: Envelope integration for different values of ﹩{\mathbb{C}}﹩ and y +, for t + = 1 and for a Kramers’ opacity.
Paper: Optimal Spectral Lines for Measuring Chromospheric Magnetic Fields
Authors: P. Judge, P. Bryans, R. Casini, L. Kleint, D. Lacatus, A. Paraschiv, D. Schmit
Figure caption: The solar flux spectrum as measured on 2008 March 25–29 with various instruments, compiled by staff at LASP as part of the Whole Heliospheric Interval Campiagn, from http://lasp.colorado.edu/lisird/. The spectrum is from soft X-rays to near the atmospheric cutoff, highlighting emission and absorption features. The region has a number of deep absorption lines with emission in their core. Mg II is such an example, although the emission is not observable due to the modest spectral resolution. The transitions of H, He I, and He II, with Δn = 1 and labeled with asterisks are compared with Δn = 0 transitions of much more highly ionized species at similar wavelengths.
Paper: Optimal Spectral Lines for Measuring Chromospheric Magnetic Fields
Authors: P. Judge, P. Bryans, R. Casini, L. Kleint, D. Lacatus, A. Paraschiv, D. Schmit
Figure caption: Intensities in the cores of the strongest lines are plotted, together with a blackbody spectrum at the solar effective temperature for reference. Also shown is a modest (typically 2 Å) resolution intensity spectrum from the Whole Heliosphere Interval campaign (https://lasp.colorado.edu/lisird/data/whi_ref_spectra), derived as 1/π of the irradiance spectrum scaled to the solar surface. Line core intensities (filled circles) used here and their sources are listed in Table 1.
Paper: Emission Line Galaxies in the SHARDS Hubble Frontier Fields. II. Limits on Lyman-continuum Escape Fractions of Lensed Emission Line Galaxies at Redshifts 2 < z < 3.5
Authors: Alex Griffiths, Christopher J. Conselice, Leonardo Ferreira, Daniel Ceverino, Pablo G. Pérez-González, Olga Vega, Daniel Rosa-González, Anton M. Koekemoer, Danilo Marchesini, José Miguel Rodríguez Espinosa, Lucía Rodríguez-Muñoz, Belén Alcalde Pampliega, Elena Terlevich
Figure caption: Example of the selection method for emission line candidates from the A0370 cluster and parallel field through the F913W medium-band filter. This process is repeated with all filter and field combinations in order to identify emission line candidates over all redshifts; for more detail, see Griffiths et al. (2021). The subsample used in this paper is selected based on the HST/UVIS filter and the redshift combination detailed in Table 1. Small gray points show all sources in the fields, while larger points are colored by redshift and represent candidates in which the selection criterion is met. Stars represent sources in which spectroscopic redshifts are available. Symbols that are in gray do not satisfy our selection criteria. The solid line represents the average Σ = 3 color significance, and the dotted horizontal line shows the observed EW = 25 Å.
Paper: Emission Line Galaxies in the SHARDS Hubble Frontier Fields. II. Limits on Lyman-continuum Escape Fractions of Lensed Emission Line Galaxies at Redshifts 2 < z < 3.5
Authors: Alex Griffiths, Christopher J. Conselice, Leonardo Ferreira, Daniel Ceverino, Pablo G. Pérez-González, Olga Vega, Daniel Rosa-González, Anton M. Koekemoer, Danilo Marchesini, José Miguel Rodríguez Espinosa, Lucía Rodríguez-Muñoz, Belén Alcalde Pampliega, Elena Terlevich
Figure caption: Average IGM transmission of UV light for an example galaxy at z ≈ 3. Light gray curves show the wavelength dependence of the IGM transmission for 100 individual runs of our Monte Carlo simulations, which are based on the models of Inoue et al. (2014). The green curve shows the average IGM transmission of all 1000 simulated sight lines, while the HST UVIS F336W filter throughput is denoted by the blue dashed line. An estimate for the value of IGM transmission is obtained through the convolution of the corresponding LyC filter response with the average IGM transmission.
Paper: Emission Line Galaxies in the SHARDS Hubble Frontier Fields. II. Limits on Lyman-continuum Escape Fractions of Lensed Emission Line Galaxies at Redshifts 2 < z < 3.5
Authors: Alex Griffiths, Christopher J. Conselice, Leonardo Ferreira, Daniel Ceverino, Pablo G. Pérez-González, Olga Vega, Daniel Rosa-González, Anton M. Koekemoer, Danilo Marchesini, José Miguel Rodríguez Espinosa, Lucía Rodríguez-Muñoz, Belén Alcalde Pampliega, Elena Terlevich
Figure caption: Transmission curves of the medium-band SHARDS filters (F517W17, F823W17, F883W35, F913W25, and F941W33) and broadband HST filters (F606W, F814W, and F105W) used for the selection of emission line galaxies. All curves have been individually normalized by their maximum transmission. We use the SHARDS medium-band filters to select our line emitter candidates in comparison to the broadband HST filters (F606W, F814W and F105W), whose filter transmission curves are also shown.
Paper: Emission Line Galaxies in the SHARDS Hubble Frontier Fields. II. Limits on Lyman-continuum Escape Fractions of Lensed Emission Line Galaxies at Redshifts 2 < z < 3.5
Authors: Alex Griffiths, Christopher J. Conselice, Leonardo Ferreira, Daniel Ceverino, Pablo G. Pérez-González, Olga Vega, Daniel Rosa-González, Anton M. Koekemoer, Danilo Marchesini, José Miguel Rodríguez Espinosa, Lucía Rodríguez-Muñoz, Belén Alcalde Pampliega, Elena Terlevich
Figure caption: Photometric redshift distribution of line emitter candidates from our sample of photometrically selected sources at 2 < z < 3.5. Photometric redshifts are obtained with EAZY with the inclusion of all SHARDS medium-band photometry with HFF-DeepSpace catalogs.
Paper: Emission Line Galaxies in the SHARDS Hubble Frontier Fields. II. Limits on Lyman-continuum Escape Fractions of Lensed Emission Line Galaxies at Redshifts 2 < z < 3.5
Authors: Alex Griffiths, Christopher J. Conselice, Leonardo Ferreira, Daniel Ceverino, Pablo G. Pérez-González, Olga Vega, Daniel Rosa-González, Anton M. Koekemoer, Danilo Marchesini, José Miguel Rodríguez Espinosa, Lucía Rodríguez-Muñoz, Belén Alcalde Pampliega, Elena Terlevich
Figure caption: Demagnified stellar mass distribution of the line emitter candidates from our sample. Stellar masses have been corrected for lensing magnification and are obtained using our updated photometric redshifts and FAST SPS modeling, implementing all SHARDS medium-band photometry.
Paper: Near-infrared Spectroscopy of a Massive Young Stellar Object in the Direction toward the Galactic Center: XCN and Aromatic C–D Features
Authors: Takashi Onaka, Itsuki Sakon, Takashi Shimonishi
Figure caption: Spatial variations of the column densities, abundances, intensities, and temperatures along the slit. All the intensities of the emission features are corrected for the foreground extinction. (a) The abundances of the column densities of XCN, CO2 ice, CO ice, and red-wing component are shown by the red circles, black diamonds, blue triangles, and green squares, respectively. (b) The column densities of H2O ice and CO gas are indicated by the red circles and black diamonds, respectively (left axis), while the extinction at Brα is shown by the blue triangles (right axis). (c) The column density of XCN is shown by the red circles (left axis), and the intensity of Brα is indicated by the black diamonds (right axis). (d) The intensities of the 3.3 and 4.4 μm emissions are indicated by the red circles and black diamonds, respectively. (e) The best-fit temperature of H2O ice is shown by the red circles, and that of CO gas is indicated by the black diamonds.
Paper: Near-infrared Spectroscopy of a Massive Young Stellar Object in the Direction toward the Galactic Center: XCN and Aromatic C–D Features
Authors: Takashi Onaka, Itsuki Sakon, Takashi Shimonishi
Figure caption: The black lines show IRC spectra extracted at every 4.″38 in the slit. Figures (a), (b), (c), ..., and (g) correspond to +3, +2, , ..., and −3 in the slit position shown in Figure 1, respectively. In the left column, the red lines indicate the best fits, while the light blue lines show the assumed continua. The blue and orange lines show the absorption features of H2O ice and CO gas, respectively. The purple lines show the absorption of the red wing at around 3.4 μm and XCN at 4.62 μm, while the gray lines indicate those of CO2 ice at 4.26 μm and CO ice at 4.67 μm. The green lines show the emission features of PAH at 3.3 μm and H I recombination lines of Brα, Brβ, and predicted Pfβ (see the text). The right column shows the optical depth of each component for 4.5–4.8 μm. The line colors are the same as in the left column. See the text for details.