adsabs/AstroCLIMB huggingface dataset:
Paper: FORCASTing the Spectroscopic Dust Properties of the WC+O Binary WR 137 with SOFIA
Authors: Megan J. Peatt, Noel D. Richardson, Peredur M. Williams, Nicole Karnath, Victor I. Shenavrin, Ryan M. Lau, Anthony F. J. Moffat, Gerd Weigelt
Figure caption: The long-term IR light curve of WR 137. We show the archival photometry (references in Section 1) of WR 137 as well as our new measurements. When the binary nears periastron, the IR brightness increases due to increased dust production with the next periastron happening soon.(The data used to create this figure are available.)
Paper: FORCASTing the Spectroscopic Dust Properties of the WC+O Binary WR 137 with SOFIA
Authors: Megan J. Peatt, Noel D. Richardson, Peredur M. Williams, Nicole Karnath, Victor I. Shenavrin, Ryan M. Lau, Anthony F. J. Moffat, Gerd Weigelt
Figure caption: In the top panel, we show the spectrum from 2021 July with line identifications for He I, He II, C III, and C IV. We also show the region of the weak UIR feature at 6.3–6.4 μm. In the lower panel, we show the three spectra taken with SOFIA/FORCAST compared to a smoothed model of the binary without dust emission (Richardson et al. 2016). Note that the model only includes the stellar and wind flux, neglecting all dust emission. Some of these emission lines from the wind were not included in the model.
Paper: AMUSE-Antlia. I. Nuclear X-Ray Properties of Early-type Galaxies in a Dynamically Young Galaxy Cluster
Authors: Zhensong Hu, Yuanyuan Su, Zhiyuan Li, Kelley M. Hess, Ralph P. Kraft, William R. Forman, Paul E. J. Nulsen, Sarrvesh S. Sridhar, Andra Stroe, Junhyun Baek, Aeree Chung, Dirk Grupe, Hao Chen, Jimmy A. Irwin, Christine Jones, Scott W. Randall, Elke Roediger
Figure caption: The fundamental plane correlation of AGN mass, 5 GHz radio luminosity, and 2–10 keV hard X-ray luminosity. The nine Antlia galaxies hosting nuclear X-ray sources are shown as the black dots with 1σ error. Antlia 105 does not have a significant radio source, so here we use 3 times the rms background level as the radio term to calculate the black hole mass and present it with an open circle. The yellow dotted, green dashed, and purple dashed–dotted lines indicate black hole mass ﹩\mathrm{log}({M}_{\mathrm{BH}}/{M}_{\odot })﹩ from 6–8. As a result, if the galaxies do host AGN, the black hole masses fall in a reasonable range of ﹩6\lesssim \mathrm{log}({M}_{\mathrm{BH}}/{M}_{\odot })\lesssim 8﹩.
Paper: AMUSE-Antlia. I. Nuclear X-Ray Properties of Early-type Galaxies in a Dynamically Young Galaxy Cluster
Authors: Zhensong Hu, Yuanyuan Su, Zhiyuan Li, Kelley M. Hess, Ralph P. Kraft, William R. Forman, Paul E. J. Nulsen, Sarrvesh S. Sridhar, Andra Stroe, Junhyun Baek, Aeree Chung, Dirk Grupe, Hao Chen, Jimmy A. Irwin, Christine Jones, Scott W. Randall, Elke Roediger
Figure caption: The posterior probability P  i  of the weighted bootstrap method according to Equation (B1). The sum of the posterior probability is less than 1 because there are multiple galaxies in one bin. Each marker represents a galaxy hosting an AGN and its corresponding stellar mass. The five AMUSE-Antlia AGN with host stellar masses around 10.7 dex have higher posterior probabilities, which contributes to the increase of the resulting occupation fraction.
Paper: FORCASTing the Spectroscopic Dust Properties of the WC+O Binary WR 137 with SOFIA
Authors: Megan J. Peatt, Noel D. Richardson, Peredur M. Williams, Nicole Karnath, Victor I. Shenavrin, Ryan M. Lau, Anthony F. J. Moffat, Gerd Weigelt
Figure caption: The W-R lines can be seen decreasing in strength as the continuum increases, while the 6.4 μm feature’s strength grows, demonstrating a relation to the dust being produced during periastron. The error bars are the standard deviation from the mean of the measurements. 6.4 μm is shown with a black dot and the others are colored symbols, which match the symbols used in Figure 5.
Paper: FORCASTing the Spectroscopic Dust Properties of the WC+O Binary WR 137 with SOFIA
Authors: Megan J. Peatt, Noel D. Richardson, Peredur M. Williams, Nicole Karnath, Victor I. Shenavrin, Ryan M. Lau, Anthony F. J. Moffat, Gerd Weigelt
Figure caption: To compare the strengths of the lines, a ratio was taken of the 6.4 μm feature over each W-R line. Ratios are represented by the corresponding symbol from our previous plot. A clear trend is shown of the ratios steadily increasing over time, though the W-R line at 5.8 μm does so at a quicker rate, potentially related to colliding winds or the dust.
Paper: FORCASTing the Spectroscopic Dust Properties of the WC+O Binary WR 137 with SOFIA
Authors: Megan J. Peatt, Noel D. Richardson, Peredur M. Williams, Nicole Karnath, Victor I. Shenavrin, Ryan M. Lau, Anthony F. J. Moffat, Gerd Weigelt
Figure caption: Here we show the three spectra with the corresponding times in the IR evolution. Unfortunately, no IR photometry was able to be collected at times near the 2022 February observation, so the interpolated flux on a line plot is likely overestimated compared with the actual flux at that time.
Paper: On the Encounter between the GASP Galaxy JO36 and the Radio Plume of GIN 049
Authors: Alessandro Ignesti, Marisa Brienza, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Rory Smith, Martin J. Hardcastle, Andrea Botteon, Ian D. Roberts, Jacopo Fritz, Rosita Paladino, Myriam Gitti, Anna Wolter, Neven Tomičić, Sean McGee, Alessia Moretti, Marco Gullieuszik, Alexander Drabent
Figure caption: Radio luminosity at 144 MHz vs. SFR showing JO36 stellar disk (blue cross point) and extended region (blue star point), the GASP-LOFAR (gold, from Ignesti et al. 2022c), and LoTSS (silver, from Roberts et al. 2021b) samples. We report the empirical relations between L rad and SFR presented by Gürkan et al. (2018) (red) and Roberts et al. (2021b) (silver), the latter is fitted on the LoTSS sample. The shaded regions show the dispersion at 1σ around the corresponding best-fit relations.
Paper: On the Encounter between the GASP Galaxy JO36 and the Radio Plume of GIN 049
Authors: Alessandro Ignesti, Marisa Brienza, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Rory Smith, Martin J. Hardcastle, Andrea Botteon, Ian D. Roberts, Jacopo Fritz, Rosita Paladino, Myriam Gitti, Anna Wolter, Neven Tomičić, Sean McGee, Alessia Moretti, Marco Gullieuszik, Alexander Drabent
Figure caption: Radio continuum image at 144 MHz of the mandolin radio source with the contours at the 3, 6, 12, 24, 48 × rms (rms = 172 μJy beam−1, resolution = 17.7 × 11.4 arcsec2). The labels point out the mandolin (where headstock, neck, and body are, respectively, A1, A2, and A3), GIN 049 southern lobe (B), and WINGS J011319.77+152927.4 (C). In the top-left insert, we show the SDSS optical image of the headstock region (silver box).
Paper: On the Encounter between the GASP Galaxy JO36 and the Radio Plume of GIN 049
Authors: Alessandro Ignesti, Marisa Brienza, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Rory Smith, Martin J. Hardcastle, Andrea Botteon, Ian D. Roberts, Jacopo Fritz, Rosita Paladino, Myriam Gitti, Anna Wolter, Neven Tomičić, Sean McGee, Alessia Moretti, Marco Gullieuszik, Alexander Drabent
Figure caption: Left: LOFAR image, previously shown in Figure 1, central panels, with on top the 40 × 40 pixel2 sampling grid. Right: from top to bottom, 144 MHz flux density, 675 MHz flux density, and spectral index vs. the distance from GIN 049. We report northern and southern jets in, respectively, red and blue. The vertical dashed–dotted line indicates the position of JO36.
Paper: On the Encounter between the GASP Galaxy JO36 and the Radio Plume of GIN 049
Authors: Alessandro Ignesti, Marisa Brienza, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Rory Smith, Martin J. Hardcastle, Andrea Botteon, Ian D. Roberts, Jacopo Fritz, Rosita Paladino, Myriam Gitti, Anna Wolter, Neven Tomičić, Sean McGee, Alessia Moretti, Marco Gullieuszik, Alexander Drabent
Figure caption: SFH of JO36 derived by SINOPSIS from Fritz et al. (2017).
Paper: On the Encounter between the GASP Galaxy JO36 and the Radio Plume of GIN 049
Authors: Alessandro Ignesti, Marisa Brienza, Benedetta Vulcani, Bianca M. Poggianti, Antonino Marasco, Rory Smith, Martin J. Hardcastle, Andrea Botteon, Ian D. Roberts, Jacopo Fritz, Rosita Paladino, Myriam Gitti, Anna Wolter, Neven Tomičić, Sean McGee, Alessia Moretti, Marco Gullieuszik, Alexander Drabent
Figure caption: ACCEPT n  e  profile with the best-fit β model. The blue shaded area indicates the 95% confidence interval. The gray-dashed and red vertical lines point out the JO36 projected clustercentric distance and R 200, respectively.
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: The redshift distribution of bent radio AGNs in the cluster (red) and noncluster (blue) sample. While we have more cluster sources at 0.5< z < 1.5 than noncluster sources, each sample spans a similar redshift range (with the exception of the highest-redshift noncluster source).
Paper: The High-redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey: Investigating the Role of Environment on Bent Radio AGNs Using LOFAR
Authors: Emmet Golden-Marx, E. Moravec, L. Shen, Z. Cai, E. L. Blanton, M. L. Gendron-Marsolais, H. J. A. Röttgering, R. J. van Weeren, V. Buiten, R. D. P. Grumitt, J. Golden-Marx, S. Pinjarkar, H. Tang
Figure caption: Cutouts of the 20 bent, double-lobed radio sources in the COBRA cluster candidate sample observed by LoTSS DR2. While most are 1.′3 × 1.′3, some are slightly larger to encompass the extent of the entire radio source. The three red contours show 10σ, 20σ, and 50σ contours based on the measurement of the rms noise in each image. The blue lines show our estimate of the projected physical size of each radio lobe, and the filled blue circle shows the location of the AGN’s core identified from both the optical/IR host and the FIRST images (see Figure 18 for the optical/IR host galaxies). The black circle shows the beam size, and the black line shows 0.′5.
Paper: Estimating Ejecta Masses of Stripped-envelope Supernovae Using Late-time Light Curves
Authors: Annastasia Haynie, Anthony L. Piro
Figure caption: (Top) Two simulations of our M ZAMS = 14 M ⊙ model in which we vary the opacity floor, effectively controlling the amount of recombination that is allowed to happen in the outer layers of the ejecta. The blue light curve, which represents significant recombination, rises significantly faster and to a brighter peak than the red (no recombination) light curve, but the two begin declining together at 60 days. (Bottom) Two simulations of our M ZAMS = 14 M ⊙ model in which we vary the strength of 56Ni mixing. As expected, the stronger mixing light curve (green) rises faster and to a slightly brighter peak. While the two light curves do not totally decline together in the radioactive decay phase, the tails have nearly the same slope.
Paper: FORCASTing the Spectroscopic Dust Properties of the WC+O Binary WR 137 with SOFIA
Authors: Megan J. Peatt, Noel D. Richardson, Peredur M. Williams, Nicole Karnath, Victor I. Shenavrin, Ryan M. Lau, Anthony F. J. Moffat, Gerd Weigelt
Figure caption: The portion of the SOFIA grism spectroscopy around the UIR feature at 6.2–6.5 μm. The data from 2022 May were shifted downward by 2 Jy for clarity. The average peak position from our measurements is highlighted and the data are smoothed for clarity with the unsmoothed spectra shown in gray. We have overplotted a dotted line to guide the eye in the shift of the peak wavelength.
Paper: Estimating Ejecta Masses of Stripped-envelope Supernovae Using Late-time Light Curves
Authors: Annastasia Haynie, Anthony L. Piro
Figure caption: (Top) Ejecta masses of each model at the onset of core collapse compared to their ZAMS mass, where ejecta mass refers to the mass of the model after completing mass transfer with its companion and iron core excision. (Bottom) Mass of the iron core excised from each model compared to ZAMS mass.
Paper: Estimating Ejecta Masses of Stripped-envelope Supernovae Using Late-time Light Curves
Authors: Annastasia Haynie, Anthony L. Piro
Figure caption: Correlations between the values of A, B, and C show that the value of A is heavily dependent on the values of both B and C, while B and C depend little on each other. This contributes to the large confidence interval around our best-fit value of A.
Paper: Estimating Ejecta Masses of Stripped-envelope Supernovae Using Late-time Light Curves
Authors: Annastasia Haynie, Anthony L. Piro
Figure caption: Snapshots of the ionization (top row) and opacity (bottom row) profiles of our fiducial model at 0.5, 5, 18, and 30 days beyond the explosion epoch. The bolometric luminosity of this model peaks at roughly 18 days, by which time a significant amount of the outer, helium-rich ejecta has recombined into neutral helium and the opacity continues to decrease. By day 30, the ejecta is entirely recombined, and the opacity profile has flattened out.
Paper: Estimating Ejecta Masses of Stripped-envelope Supernovae Using Late-time Light Curves
Authors: Annastasia Haynie, Anthony L. Piro
Figure caption: Ratio of calculated to true ejecta masses using Equation (8) with the A, B, and C values in Equation (12) for models that are fit over the time frame 0.5t thin to 100 days beyond the time of explosion. Similar to the 200 day fit, these results recover M ej values to within 20%.
Paper: Estimating Ejecta Masses of Stripped-envelope Supernovae Using Late-time Light Curves
Authors: Annastasia Haynie, Anthony L. Piro
Figure caption: Ratio of calculated to true ejecta masses using Equation (8) with the A, B, and C values in Equation (12) for models varying the 56Ni mixing and concentration. These values perform worse than the 200 day fit with varying the nickel parameters, particularly those of high mass.
Paper: Estimating Ejecta Masses of Stripped-envelope Supernovae Using Late-time Light Curves
Authors: Annastasia Haynie, Anthony L. Piro
Figure caption: Here we demonstrate our fitting procedure on our M ZAMS = 14 M ⊙ fiducial model, shown in blue. The black line shows the time over which we are fitting for T 0, and the red curve shows Equation (5) calculated with the best-fit value of T 0 = 115.464.
Paper: Estimating Ejecta Masses of Stripped-envelope Supernovae Using Late-time Light Curves
Authors: Annastasia Haynie, Anthony L. Piro
Figure caption: Ratio of ejecta mass calculated from Equation (8) utilizing our best-fit values of A, B, and C for cases varying the 56Ni mixing and concentration. We see that increasing the mixing strength tends to result in a slightly lower ejecta mass estimate but is still within a reasonable error.
Paper: Estimating Ejecta Masses of Stripped-envelope Supernovae Using Late-time Light Curves
Authors: Annastasia Haynie, Anthony L. Piro
Figure caption: Our fit of the bolometric light curve of SN 2011dh. As in Figure 4, the data are shown in blue, the best-fit modified heating equation is shown in red, and the black line indicates the fitting region from 57 to 200 days. We find that the data are best fit by T 0 = 100.64 days.
Paper: Estimating Ejecta Masses of Stripped-envelope Supernovae Using Late-time Light Curves
Authors: Annastasia Haynie, Anthony L. Piro
Figure caption: Ratio of mass calculated from Equation (11) utilizing our optimized values of A, B, and C in Equation (10). Calculated ejecta masses are within 20% of the true mass across our full grid of models.
Paper: Observations of Locally Generated Whistler-mode Waves in the Martian Magnetotail Current Sheet
Authors: Xiao Ma, Anmin Tian, Shichen Bai, Ruilong Guo, Quanqi Shi, Mengmeng Wang, Xiaochen Shen
Figure caption: Whistler instability analyses. (a) Magnetic field intensity; (b) energy spectrum of the electron differential energy flux; (c) electron temperature anisotropy T e⊥/T e∥; pitch angle distributions of the (d) 30.9–98.9 eV and (e) 111.2–905.4 eV electrons; (f) magnetic power spectrum; (g) wave amplitude above the low hybrid frequency; (h) linear growth rate of whistler-mode waves according to Kennel & Petschek (1966) theory. The black line in (b) represents the electron minimum resonant energy of 0.05 f ce whistler-mode waves. The black lines in (d) and (e) represent the loss cone angle calculated by arcsin(﹩B/{B}_{\max }﹩)1/2 and 180°− arcsin(﹩B/{B}_{\max }﹩)1/2, where ﹩{B}_{\max }﹩ is the maximum value during the time interval. The white line in (f) and the black line in (h) represent the low hybrid frequency. Light red shaded rectangles denote where the whistler-mode waves are observed.
Paper: Observations of Locally Generated Whistler-mode Waves in the Martian Magnetotail Current Sheet
Authors: Xiao Ma, Anmin Tian, Shichen Bai, Ruilong Guo, Quanqi Shi, Mengmeng Wang, Xiaochen Shen
Figure caption: MAVEN orbit in (a) X MSO–Y MSO and (b) X MSO–Z MSO planes. Blue and red bold lines are for time intervals of 09:32:00–09:46:00 UT and 09:37:30–09:41:00 UT on 2016 March 31, respectively. MAVEN observations of (c) Bx (blue), By (green), Bz (red) components in MSO coordinates, and total magnetic field intensity (black); (d) ion energy spectrum provided by SWIA; (e) electron energy spectrum provided by SWEA; (f) magnetic field during 09:37:30–09:41:00 UT, with the same format of (c); magnetic power spectra for (g) transverse and (h) compressional components; (i) wave normal angle; (j) degree of polarization; and (k) ellipticity spectra obtained by Means’ method (Means 1972). Blue and red bars correspond to the blue and red orbits in (a) and (b). White lines in (g)–(h) and black lines in (i)–(k) represent the low hybrid frequency. The solid and dashed lines in (a) and (b) represent the empirical locations of the bow shock and magnetic pileup boundary (Trotignon et al. 2006).
Paper: Observations of Locally Generated Whistler-mode Waves in the Martian Magnetotail Current Sheet
Authors: Xiao Ma, Anmin Tian, Shichen Bai, Ruilong Guo, Quanqi Shi, Mengmeng Wang, Xiaochen Shen
Figure caption: Mirror instability analyses. (a) The magnetic field in MSO coordinates with the same format of Figure 1(c); (b) number density and (c) temperature of O+ (green), O2 + (orange), and electron (black); (d) electron temperature anisotropy T e⊥/T e∥; (e) electron (red), O+ (green), O2 + (orange) thermal pressure, magnetic pressure (blue), and total pressure (black); (f) plasma beta; (g) condition of the mirror instability 1+β ⊥(1-T ⊥/T ∥) (Hasegawa 1969), smaller than 0 represents the instability is satisfied. Light red shaded rectangles denote where the whistler-mode waves are observed.
Paper: Observations of Locally Generated Whistler-mode Waves in the Martian Magnetotail Current Sheet
Authors: Xiao Ma, Anmin Tian, Shichen Bai, Ruilong Guo, Quanqi Shi, Mengmeng Wang, Xiaochen Shen
Figure caption: Overview of the current sheet. (a) The magnetic field in LMN coordinates using the MVA method (Sonnerup & Cahill 1967); (b) ion mass spectrum provided by STATIC; energy spectrum of (c) a.m.u. < 10 and (d) a.m.u. > 10 ions; (e) H+, (f) O+, and (g) O2 + bulk velocity in LMN coordinates; (h) H+ bulk speed V H+ (black), (m O+/m H+)1/2  V O+ (green), and (m O2+/m H+)1/2  V O2+ (orange). LMN coordinates are labeled in (a).
Paper: Is a Recently Discovered H I Cloud near M94 a Starless Dark Matter Halo?
Authors: Alejandro Benitez-Llambay, Julio F. Navarro
Figure caption: Identical to Figure 2, but assuming RELHICs are embedded within gNFW halos with γ = 0. See Equation (1). The solid line in the bottom panel shows the family of models that provide a good fit to the second innermost isocontour.
Paper: Is a Recently Discovered H I Cloud near M94 a Starless Dark Matter Halo?
Authors: Alejandro Benitez-Llambay, Julio F. Navarro
Figure caption: Mean DM density profile of the best-fit ΛCDM RELHIC model at the fiducial distance of M94 (gray dashed line) compared with the best-fit gNFW RELHIC model. The DM content between the models differs by more than a factor of 2 below ∼6 kpc (vertical line).
Paper: Is a Recently Discovered H I Cloud near M94 a Starless Dark Matter Halo?
Authors: Alejandro Benitez-Llambay, Julio F. Navarro
Figure caption: Top panel: CL-9's observed column density profile (circles), including 3σ  uncertainties, together with mock-observed RELHICs (lines) at the distance of M94 and convolved with the FAST Gaussian beam. RELHICs were chosen to bracket CL-9's observations while following the ΛCDM mass–concentration relation. The thick line highlights the best-fit model (see text for discussion), and the labels indicate the total H I mass of the model immediately below. Middle panel: intrinsic column density profiles of the models shown in the top panel. The vertical line indicates the radial extent of the FAST beam. Bottom panel: mass–concentration relation of the models, together with the Ludlow et al. (2016) mass–concentration relation (line) and scatter (shaded region). The orange and green squares indicate examples with lower-than-average concentrations that also match observations (see the lines of the same color in the middle and top panels).
Paper: Is a Recently Discovered H I Cloud near M94 a Starless Dark Matter Halo?
Authors: Alejandro Benitez-Llambay, Julio F. Navarro
Figure caption: CL-9's observed column density isocontours (taken from Z23) superimposed on a DESI LS color image of the same field. The white circle indicates the FAST beam size. We approximate the observed isocontours with the dashed circles to construct the observed column density profile displayed in the bottom panel. The error bars indicate 3σ  uncertainties. The coordinates are relative to the origin, ﹩(\alpha ,\delta )=({12}^{{\rm{h}}}{51}^{{\rm{m}}}{52}^{{\rm{s}}},+40^\circ 17^{\prime} 29^{\prime\prime} )﹩.
Paper: Is a Recently Discovered H I Cloud near M94 a Starless Dark Matter Halo?
Authors: Alejandro Benitez-Llambay, Julio F. Navarro
Figure caption: Identical to Figure 2, but assuming CL-9 is at a distance d = 500 kpc.
Paper: Atmospheric Effects on Neutron Star Parameter Constraints with NICER
Authors: Tuomo Salmi, Serena Vinciguerra, Devarshi Choudhury, Anna L. Watts, Wynn C. G. Ho, Sebastien Guillot, Yves Kini, Bas Dorsman, Sharon M. Morsink, Slavko Bogdanov
Figure caption: Effect of the atmosphere model on the posterior distributions of radius, compactness, mass, and temperatures for both primary and secondary hot regions, using the PSR J0740+6620 NICER data set conditional on the ST-U model. Six types of posterior distribution are shown with five different atmosphere tables used in the analysis (see Table 1 for definitions), and one fully ionized hydrogen NSX model with a free beaming correction limited to 10% deviation at most (ST-U-nsxH-beam10). The credible intervals and the Kullback–Leibler (KL) divergence D KL are reported for the fully ionized hydrogen NSX case: ST-U-nsxH (see Table 2 for mass and radius values in other cases). The prior distributions are shown by the dashed–dotted functions. The 1D intervals (shaded in red) contain 68.3% of the posterior mass, and the contours in the 2D panels contain 68.3%, 95.4%, and 99.7% of the posterior mass. For more details of the figure elements, see Figure 5 of Riley et al. (2021) and Figure 5 of Salmi et al. (2022). Posterior distributions for the other parameters are shown in Figure 8 of the Appendix.