adsabs/AstroCLIMB huggingface dataset:
Paper: Hadronic Processes at Work in 5BZB J0630−2406
Authors: Gaëtan Fichet de Clairfontaine, Sara Buson, Leonard Pfeiffer, Stefano Marchesi, Alessandra Azzollini, Vardan Baghmanyan, Andrea Tramacere, Eleonora Barbano, Lenz Oswald
Figure caption: SED from the purely leptonic model of 5BZB J0630−2406 in the observer 							frame. The dotted–dashed curves represent synchrotron and inverse 							Compton from pair production due to γ–γ absorption. The black 							solid squares represent the contemporaneous MWL data used for the 							modeling. Archival data are shown by the gray solid dots. The red 							downward triangle represents the accretion-disk limit from (Ghisellini 							et al. 2012).
Paper: Hadronic Processes at Work in 5BZB J0630−2406
Authors: Gaëtan Fichet de Clairfontaine, Sara Buson, Leonard Pfeiffer, Stefano Marchesi, Alessandra Azzollini, Vardan Baghmanyan, Andrea Tramacere, Eleonora Barbano, Lenz Oswald
Figure caption: The same as Figure 5, with 							the leptohadronic solution of 5BZB J0630−2406 in the observer frame. The 							dashed curves represent hadronic processes (BH and photopion 							productions). The dotted–dashed blue curves represent the obtained muon 							neutrino flux, with associated uncertainties from the Poisson statistic 							assuming 3σ levels.
Paper: Hadronic Processes at Work in 5BZB J0630−2406
Authors: Gaëtan Fichet de Clairfontaine, Sara Buson, Leonard Pfeiffer, Stefano Marchesi, Alessandra Azzollini, Vardan Baghmanyan, Andrea Tramacere, Eleonora Barbano, Lenz Oswald
Figure caption: Schematic view of the model. 1: SMBH. 2: Accretion disk defined by a 							luminosity L disk and a temperature T disk. 3: Dust torus defined by a luminosity L torus and a temperature T torus. 4: BLR that scattered direct emission. 5: Relativistic 							jet (not modeled here). 6: Moving emission region (”blob”) situated at a 							distance R diss from the black hole. Direct (indirect) external photon 							fields are represented by continuous (dashed) arrows. Scheme not to 							scale.
Paper: Hadronic Processes at Work in 5BZB J0630−2406
Authors: Gaëtan Fichet de Clairfontaine, Sara Buson, Leonard Pfeiffer, Stefano Marchesi, Alessandra Azzollini, Vardan Baghmanyan, Andrea Tramacere, Eleonora Barbano, Lenz Oswald
Figure caption: Neutrino flux scaled according to the livetime shown in Aartsen et al. (2017b) derived for mixed 						leptohadronic modeling of 5BZB J0630−2406. The uncertainties are computed 						assuming Poisson statistics and 3σ levels. The 						dashed gray line represents the 7 yr IceCube sensitivity, assuming E −2 and δ = −24.°06.
Paper: Hadronic Processes at Work in 5BZB J0630−2406
Authors: Gaëtan Fichet de Clairfontaine, Sara Buson, Leonard Pfeiffer, Stefano Marchesi, Alessandra Azzollini, Vardan Baghmanyan, Andrea Tramacere, Eleonora Barbano, Lenz Oswald
Figure caption: Evolution of the number of observed events by the IceCube detector in time 						according to various string configurations and assuming a constant flux. The 						uncertainties are evaluated assuming Poisson statistics (3σ levels). The blue dashed line represents the 						integrated livetime used in Buson et al. (2022a).
Paper: Hadronic Processes at Work in 5BZB J0630−2406
Authors: Gaëtan Fichet de Clairfontaine, Sara Buson, Leonard Pfeiffer, Stefano Marchesi, Alessandra Azzollini, Vardan Baghmanyan, Andrea Tramacere, Eleonora Barbano, Lenz Oswald
Figure caption: Pre-analyzed observed SED showing the first peak, assumed to be due to 							synchrotron emission from relativistic electrons, and the second peak. 							Assuming a Doppler factor δ D and a magnetic field strength ﹩B^{\prime} ﹩ (and the source redshift z), one can derive characteristics of the electron 							distribution, including the minimum, break, and maximum energies, with 							both indexes being indicated in the legend.
Paper: Hadronic Processes at Work in 5BZB J0630−2406
Authors: Gaëtan Fichet de Clairfontaine, Sara Buson, Leonard Pfeiffer, Stefano Marchesi, Alessandra Azzollini, Vardan Baghmanyan, Andrea Tramacere, Eleonora Barbano, Lenz Oswald
Figure caption: 5BZB J0630−2406 NuSTAR FPMA (blue circles) and FPMB (red squares) light 							curves. Both data sets are fit with a constant, shown with a blue (red) 							dashed line. No trend is observed in the light curves, suggesting no 							significant intra-observation variability in the NuSTAR data.
Paper: Hadronic Processes at Work in 5BZB J0630−2406
Authors: Gaëtan Fichet de Clairfontaine, Sara Buson, Leonard Pfeiffer, Stefano Marchesi, Alessandra Azzollini, Vardan Baghmanyan, Andrea Tramacere, Eleonora Barbano, Lenz Oswald
Figure caption: Flow chart of the parameter-space research algorithm used in this study. 							A box labeled by a number represents a set of parameters for a given 							CPU.
Paper: Hadronic Processes at Work in 5BZB J0630−2406
Authors: Gaëtan Fichet de Clairfontaine, Sara Buson, Leonard Pfeiffer, Stefano Marchesi, Alessandra Azzollini, Vardan Baghmanyan, Andrea Tramacere, Eleonora Barbano, Lenz Oswald
Figure caption: Cutout region of the 7 yr IceCube L-value map 						(Aartsen et al. 2017b) 						centered at the position of the hotspot IC J0630−2353, displayed in 						celestial coordinates. The position of the associated blazar 5BZB J0630−2406 						is highlighted by a green cross. The black lines indicate the 1° × 1° 						coordinate grid.
Paper: Constraints on the Persistent Radio Source Associated with FRB 20190520B Using the European VLBI Network
Authors: Shivani Bhandari, Benito Marcote, Navin Sridhar, Tarraneh Eftekhari, Jason W. T. Hessels, Danté M. Hewitt, Franz Kirsten, Omar S. Ould-Boukattine, Zsolt Paragi, Mark P. Snelders
Figure caption: Top panel: comparison of the position of the check source (J1603-1007) measured from EM161A (orange) and EM161B (light orange) for all data (plus markers) and only high-elevation data (circles), all relative to the Astrogeo position at 3 GHz. Also plotted are the positional offsets measured from the CASA analysis (light purple) and AIPS analysis (violet) for the combined epoch EM161A/B data. The black-filled plus sign shows the average position derived from individual measurements at different epochs, using different analysis software, and different data selections. The gray ellipse shows the size of the synthesized beam for the combined EM161A/B data, centered at the average position. The individual measurements fall within the FWHM of the synthesized beam. Bottom panel: measured positional offsets for the PRS relative to the centroid of the published VLA position (Niu et al. 2022). We note that the uncertainty on this position is 100 and 50 mas in α and δ, respectively, which is larger than the extent of the image. Here the individual measurements show a scatter of a few mas with respect to the average PRS position shown by the dark black cross.
Paper: Constraints on the Persistent Radio Source Associated with FRB 20190520B Using the European VLBI Network
Authors: Shivani Bhandari, Benito Marcote, Navin Sridhar, Tarraneh Eftekhari, Jason W. T. Hessels, Danté M. Hewitt, Franz Kirsten, Omar S. Ould-Boukattine, Zsolt Paragi, Mark P. Snelders
Figure caption: Allowed parameter space for the age, t age, of a putative magnetar progenitor for FRB 20190520B and the radius R  n  of the synchrotron nebula responsible for powering the observed PRS emission, based on observational constraints. An upper limit on R  n  is obtained from our EVN observations, while a lower limit can be placed based on the lack of a clear self-absorption signature (SSA) below 1 GHz (Zhang 2018). An upper limit on the source age is obtained from the observed PRS luminosity and total available magnetic energy, while the date of discovery sets an approximate lower limit on the source age. Requiring that the size of the expanding supernova ejecta shell R ej is larger than the size of the magnetar-inflated nebula requires a minimum age of t age ≳ 900 yr. Gray-dashed curves correspond to the expansion velocity of the synchrotron nebula, R  n /t age.
Paper: XUE: Molecular Inventory in the Inner Region of an Extremely Irradiated Protoplanetary Disk
Authors: María Claudia Ramírez-Tannus, Arjan Bik, Lars Cuijpers, Rens Waters, Christiane Göppl, Thomas Henning, Inga Kamp, Thomas Preibisch, Konstantin V. Getman, Germán Chaparro, Pablo Cuartas-Restrepo, Alex de Koter, Eric D. Feigelson, Sierra L. Grant, Thomas J. Haworth, Sebastián Hernández, Michael A. Kuhn, Giulia Perotti, Matthew S. Povich, Megan Reiter, Veronica Roccatagliata, Elena Sabbi, Benoît Tabone, Andrew J. Winter, Anna F. McLeod, Roy van Boekel, Sierk E. van Terwisga
Figure caption: Top: extinction A  K  for a sample of stars in Pis24, shown in colors. The position of XUE 1 in this diagram is indicated with a star. The O stars from the bottom panel are indicated with magenta borders. Bottom: radiation field toward XUE 1. The lines show the 2D distance from the massive stars to XUE 1 (indicated with the black star), and the colors of the circles show their temperature. The FUV radiation felt by XUE 1 from each massive star is shown by the color and width of the lines.
Paper: Constraints on the Persistent Radio Source Associated with FRB 20190520B Using the European VLBI Network
Authors: Shivani Bhandari, Benito Marcote, Navin Sridhar, Tarraneh Eftekhari, Jason W. T. Hessels, Danté M. Hewitt, Franz Kirsten, Omar S. Ould-Boukattine, Zsolt Paragi, Mark P. Snelders
Figure caption: EVN image of the PRS associated with FRB 20190520B, as seen in the combined EM161A/B observations. The source is compact on milliarcsecond scales: <2.3 mas at the 3σ level. This corresponds to a <9 pc transverse extent, given the known redshift of the host galaxy. A small bar in the top right of the image shows a representative 10 pc transverse extent, for scale. Contour levels start at two times the rms noise level of 16 μJy beam−1 and increase by factors of ﹩\sqrt{2}﹩. The synthesized beam is represented by the gray ellipse at the bottom left corner; it has a size of 3.8 × 5.9 mas2 and a position angle of 57°.
Paper: XUE: Molecular Inventory in the Inner Region of an Extremely Irradiated Protoplanetary Disk
Authors: María Claudia Ramírez-Tannus, Arjan Bik, Lars Cuijpers, Rens Waters, Christiane Göppl, Thomas Henning, Inga Kamp, Thomas Preibisch, Konstantin V. Getman, Germán Chaparro, Pablo Cuartas-Restrepo, Alex de Koter, Eric D. Feigelson, Sierra L. Grant, Thomas J. Haworth, Sebastián Hernández, Michael A. Kuhn, Giulia Perotti, Matthew S. Povich, Megan Reiter, Veronica Roccatagliata, Elena Sabbi, Benoît Tabone, Andrew J. Winter, Anna F. McLeod, Roy van Boekel, Sierk E. van Terwisga
Figure caption: Comparison between the gas line luminosities of XUE 1 and the Spitzer sample studied by Banzatti et al. (2020) and the CO emission from Banzatti et al. (2022) (black circles). The y-axis shows the 17 μm H2O luminosity. From left to right the x-axis shows the 12CO2, HCN, C2H2, and CO luminosities. The upper limits are indicated with gray arrows, and the open circles show the sources with upper limits in both the x- and y-axes. The yellow plus signs show the location of the MIRI spectra published to date: GW Lup (Grant et al. 2023) and EX Lup (Kóspál et al. 2023). The luminosities measured for the JWST spectrum of XUE 1 are shown with the orange stars.
Paper: Constraints on the Persistent Radio Source Associated with FRB 20190520B Using the European VLBI Network
Authors: Shivani Bhandari, Benito Marcote, Navin Sridhar, Tarraneh Eftekhari, Jason W. T. Hessels, Danté M. Hewitt, Franz Kirsten, Omar S. Ould-Boukattine, Zsolt Paragi, Mark P. Snelders
Figure caption: The burst profile (top panel) and dynamic spectrum (bottom panel) of the only burst detected from FRB 20190520B in our observations (in EK051C). The time and frequency resolution are 1.024 ms and 2 MHz, respectively. The data has been coherently de-dispersed using SFXC at the Heimdall-reported DM of 1177.2 pc cm−3.
Paper: XUE: Molecular Inventory in the Inner Region of an Extremely Irradiated Protoplanetary Disk
Authors: María Claudia Ramírez-Tannus, Arjan Bik, Lars Cuijpers, Rens Waters, Christiane Göppl, Thomas Henning, Inga Kamp, Thomas Preibisch, Konstantin V. Getman, Germán Chaparro, Pablo Cuartas-Restrepo, Alex de Koter, Eric D. Feigelson, Sierra L. Grant, Thomas J. Haworth, Sebastián Hernández, Michael A. Kuhn, Giulia Perotti, Matthew S. Povich, Megan Reiter, Veronica Roccatagliata, Elena Sabbi, Benoît Tabone, Andrew J. Winter, Anna F. McLeod, Roy van Boekel, Sierk E. van Terwisga
Figure caption: Reduced χ 2 maps resulting from the fitting of LTE slab models to the MIRI MRS spectrum. The colors indicate the ﹩{\chi }_{\min }^{2}/{\chi }^{2}﹩ value, with 1 being the best-fit model. The white contours show the emitting radius in au, and the red, orange, and yellow contours show the 1σ, 2σ, and 3σ confidence intervals. The location of the best-fit models in the parameter space is shown by a black plus sign.
Paper: Accretion-modified Stars in Accretion Disks of Active Galactic Nuclei: The Low-luminosity Cases and an Application to Sgr A*
Authors: Jian-Min Wang, Jun-Rong Liu, Yan-Rong Li, Yu-Yang Songsheng, Ye-Fei Yuan, Luis C. Ho
Figure caption: Left: an sMBH embedded in SMBH-ADAFs is orbiting around the central SMBH. The sMBH is accreting with Bondi rates from the SMBH-ADAF, but outflows from the sMBH-ADAFs drive the formation of a cavity and quench the accretion. Such an accretion-feedback system exhibits quasi-periodic behaviors, showing quasi-periodic flickerings from relativistic jets produced through the Blandford–Znajek (BZ) mechanism of the sMBH-ADAF. Emissions of the jet constitute spectral energy distributions additional to the SMBH-ADAF. The jet may be partially choked by the SMBH-ADAF, giving rise to subrelativistic wisps from the SMBH-ADAF. The accumulating sMBH-outflows will trigger the viscosity instability of the SMBH-ADAF resulting in flares following a series of flickerings. The present model can explain the NIR quasi-periodic flickerings and flares of Sgr A*. Right: illustrated classifications of light curves. Type-A shows that flares and/or flickerings are superposed on a stationary state whereas type-B shows an upon-down mode. Flickerings are thin lines, and flares are thick lines.
Paper: Accretion-modified Stars in Accretion Disks of Active Galactic Nuclei: The Low-luminosity Cases and an Application to Sgr A*
Authors: Jian-Min Wang, Jun-Rong Liu, Yan-Rong Li, Yu-Yang Songsheng, Ye-Fei Yuan, Luis C. Ho
Figure caption: The overall spectral energy distribution of Sgr A* from radio to TeV bands. We get the accretion rates of the SMBH from the averaged SED. Curves are marked by the same color words. Syn: synchrotron radiation from the relativistic jet developed by the sMBH accretion. ADAF-EC: external IC (EC) of SMBH-ADAF photons. SSC: synchrotron self-Compton scattering. Narayan & Yi (1995) collected early radio data (we omit these references). INTEGRAL and Fermi data are from Malyshev et al. (2015). When m → 0, the inhomogeneous model becomes one-zone model.
Paper: Accretion-modified Stars in Accretion Disks of Active Galactic Nuclei: The Low-luminosity Cases and an Application to Sgr A*
Authors: Jian-Min Wang, Jun-Rong Liu, Yan-Rong Li, Yu-Yang Songsheng, Ye-Fei Yuan, Luis C. Ho
Figure caption: The overall spectral energy distributions of the SMBH-ADAF and the relativistic jets from the sMBH. The relativistic jet mainly contributes to the optical to soft X-ray bands. In these calculations, we take the same values of the magnetization parameter (β p,s) in the SMBH- and sMBH-ADAFs. See text for values of model parameters.
Paper: Rapid Premerger Localization of Binary Neutron Stars in Third-generation Gravitational-wave Detectors
Authors: Qian Hu, John Veitch
Figure caption: Multibanding scheme for this work. Left axis: an illustration of a chopped GW waveform that is alternately colored for different waveform bins and sampling frequencies. We use 2 minute segments with 256 Hz sampling frequency for waveforms from 60 minutes before merger to 2 minutes before merger, and 1 minute segments for the last 2 minutes with 1024 and 4096 Hz sampling frequencies, respectively. Right axis: the cumulative S/N of the signal, showing the contribution of S/N from each time segment.
Paper: Rapid Premerger Localization of Binary Neutron Stars in Third-generation Gravitational-wave Detectors
Authors: Qian Hu, John Veitch
Figure caption: Time cost of running SealGW and Bayestar for ET+2CE network on a 2.44 GHz processor with different number of threads, excluding the time costs of matched filtering and data conditioning. The two algorithms are tested with the same data, and sky maps are calculated to the same level of resolution (n side = 2048, finest pixel = 0.0008 deg2). The matched filtering speed (detection latency) depends on the efficiency of the detection pipeline, and data conditioning usually takes ∼0.1 s to read and preprocess the data from pipeline outputs.
Paper: Rapid Premerger Localization of Binary Neutron Stars in Third-generation Gravitational-wave Detectors
Authors: Qian Hu, John Veitch
Figure caption: Sky map evolution. Upper panel: an example sky map for a 1.4 + 1.4M ⊙ BNS at 1000 Mpc detected 30 minutes before merger with a network S/N of 12. The S/N increases to 17 at 20 minutes before merger, 31 at 10 minutes, 95 at 1 minute and 130 after merger. We show the 90% localization contours at different negative latencies. The injection sky location is marked with a cross. Lower panel: evolution of 90% confidence localization areas of early-warning events in our simulation. The example in upper panel is plotted in red line.
Paper: Rapid Premerger Localization of Binary Neutron Stars in Third-generation Gravitational-wave Detectors
Authors: Qian Hu, John Veitch
Figure caption: Cumulative number of detections and 90% confidence sky localization areas for the 68,000 BNS simulations (roughly one month of observation). The corresponding detection efficiency is labeled in the right y-axis. We choose 10 different negative latencies (from 50 minutes to postmerger) and the curves show the cumulative distribution of 90% areas of events that are detected at those times.
Paper: Rapid Premerger Localization of Binary Neutron Stars in Third-generation Gravitational-wave Detectors
Authors: Qian Hu, John Veitch
Figure caption: P–P plot of localizations in our simulation at different bands. For 50 minutes (light blue, sample size = 8), 40 minutes (brown, sample size = 18), and 30 minutes (orange, sample size = 53), error bars are plotted individually with their own colors. For other bands, we randomly select 150 events and plot their error bar in black. The error bar is calculated from a binomial distribution, and we note that it only converges to (0%, 0%) and (100%, 1%) when the sample size is sufficiently large.
Paper: Constraints on the Persistent Radio Source Associated with FRB 20190520B Using the European VLBI Network
Authors: Shivani Bhandari, Benito Marcote, Navin Sridhar, Tarraneh Eftekhari, Jason W. T. Hessels, Danté M. Hewitt, Franz Kirsten, Omar S. Ould-Boukattine, Zsolt Paragi, Mark P. Snelders
Figure caption: Radio luminosities (at 1 GHz) and physical sizes of multiple types of compact radio sources. These include measurement and constraints for the confirmed FRB PRSs (blue); the radio source potentially associated with FRB 20181030A (orange; Bhardwaj et al. 2021); the compact radio component of SNR SN 1986J (black); the orphan GRB afterglow, FIRST J141918.9+394036 (green); and wandering black hole candidates (magenta) obtained at the highest-possible angular resolutions (Marcote et al. 2017; Bietenholz & Bartel 2017; Marcote et al. 2019; Sargent et al. 2022). Teal points represent the PRS-like candidates identified in nearby dwarf galaxies by Vohl et al. (2023). Red data points show the inferred lower and upper limits on the size of the PWN candidate VT 1137-0337 (Dong & Hallinan 2023). Yellow and dark red points represent measurements from Galactic SNRs and PWNe, respectively (Ranasinghe & Leahy 2023; Green 2019), whereas cyan points represent SNRs in nearby galaxies (Urošević et al. 2005). The high-luminosity space is occupied by light green points showing low-luminosity AGNe (Radcliffe et al. 2018). Circles indicate a size measurement, while 1σ upper limits on size are shown as triangles. Overplotted dashed lines show the 3σ upper limits on radio luminosity for a sample of localized FRBs presented in Table 1.
Paper: Constraints on the Persistent Radio Source Associated with FRB 20190520B Using the European VLBI Network
Authors: Shivani Bhandari, Benito Marcote, Navin Sridhar, Tarraneh Eftekhari, Jason W. T. Hessels, Danté M. Hewitt, Franz Kirsten, Omar S. Ould-Boukattine, Zsolt Paragi, Mark P. Snelders
Figure caption: Direct convolution (the so-called dirty map) of the interferometric data from the single FRB 20190520B burst detected in our EVN-PRECISE observations (EK051C). The synthesized beam, with a size of 62 × 18 mas2 and a position angle of 17°, is shown as the gray ellipse at the bottom-left corner of each of the two top panels. Also, in both top panels, the red solid and dotted ellipses represent the position and 2σ uncertainty of the PRS and bursting source, respectively, as measured by Niu et al. (2022) using the VLA. Top left: A ∼2″ × 2″ image of the field. The fringe pattern with strong peaks is due to the limited UV-coverage resulting from only four available antennas and a few milliseconds of integration (meaning negligible Earth rotation during this time). Top right: zoom-in on the white square shown in the left panel. The cross represents the centroid of the strongest peak in the whole ∼2″ × 2″ field. The EVN position of the PRS along with the 1σ (solid), 2σ, and 3σ (dotted) uncertainties are represented by white ellipses. The PRS position is ∼20 mas offset from the centroid of the brightest and closest peak. Bottom: a CDF of the pixel values in the ∼2″ × 2″ field. The black-dotted line shows the pixel value at the position of the PRS centroid, while the shaded region represents pixel values within 1σ of the nominal PRS position. The data are consistent with the PRS and burst source being positionally coincident to within ≲20 mas (i.e., to within a transverse distance of ≲80 pc).
Paper: Estimating Coronal Mass Ejection Mass and Kinetic Energy by Fusion of Multiple Deep-learning Models
Authors: Khalid A. Alobaid, Yasser Abduallah, Jason T. L. Wang, Haimin Wang, Shen Fan, Jialiang Li, Huseyin Cavus, Vasyl Yurchyshyn
Figure caption: Distributions of the mass and kinetic energy values of the CMEs used in this study.
Paper: Estimating Coronal Mass Ejection Mass and Kinetic Energy by Fusion of Multiple Deep-learning Models
Authors: Khalid A. Alobaid, Yasser Abduallah, Jason T. L. Wang, Haimin Wang, Shen Fan, Jialiang Li, Huseyin Cavus, Vasyl Yurchyshyn
Figure caption: Illustration of the DeepCME architecture. The fusion model begins with three component models, namely ResNet50, InceptionV3, and InceptionResNetV2, each of which is succeeded by a 2D convolutional layer, followed by five convolutional blocks, followed by two dense layers with 1024 neurons and 1 neuron, respectively. The fusion model concludes with a concatenation layer, which produces the output (i.e., the estimated CME mass or kinetic energy value) for the input base-difference image (CME event).
Paper: Estimating Coronal Mass Ejection Mass and Kinetic Energy by Fusion of Multiple Deep-learning Models
Authors: Khalid A. Alobaid, Yasser Abduallah, Jason T. L. Wang, Haimin Wang, Shen Fan, Jialiang Li, Huseyin Cavus, Vasyl Yurchyshyn
Figure caption: Construction of the base-difference image for the CME event that occurred on 2004 September 12 at 00:36:06 UT. The left panel shows the pre-event image of the CME. The middle panel shows the CME appearing as a full-grown structure. The right panel shows the base-difference image of the CME obtained by subtracting the image in the left panel from the image in the middle panel.