adsabs/AstroCLIMB huggingface dataset:
Paper: Mind the Kinematics Simulation of Planet–Disk Interactions: Time Evolution and Numerical Resolution
Authors: Kan Chen, Ruobing Dong
Figure caption: Successive channel maps of our disk model at 1000 orbits and with CPH = 20. Gray and blue dashed lines denote gap edges and the primary spirals, respectively. The location of the planet is indicated by the cyan marker. The disk rotation direction is marked in the lower left panel. The color bar is in a linear scale.
Paper: Mind the Kinematics Simulation of Planet–Disk Interactions: Time Evolution and Numerical Resolution
Authors: Kan Chen, Ruobing Dong
Figure caption: Similar to Figure 3 but for V  θ .
Paper: A NICER View of PSR J1231−1411: A Complex Case
Authors: Tuomo Salmi, Julia S. Deneva, Paul S. Ray, Anna L. Watts, Devarshi Choudhury, Yves Kini, Serena Vinciguerra, H. Thankful Cromartie, Michael T. Wolff, Zaven Arzoumanian, Slavko Bogdanov, Keith Gendreau, Sebastien Guillot, Wynn C. G. Ho, Sharon M. Morsink, Ismaël Cognard, Lucas Guillemot, Gilles Theureau, Matthew Kerr
Figure caption: Radius, mass, compactness, and inclination posterior distributions using the NICER and XMM-Newton data sets for the PDT-U model. The results with three different radius priors are shown, but the run with widest radius prior (R eq ∈ [8, 16] km) seems not to have converged because it finds only significantly worse fits to the data than the others. Dashed–dotted curves represent the marginal prior probability density functions (PDFs). The vertical dashed orange line shows R eq = 14 km to guide the eye. The shaded vertical bands show the 68.3% credible intervals (for the posteriors corresponding to the red curves), and the contours in the off-diagonal panels show the 68.3%, 95.4%, and 99.7% credible regions. See the captions of Figure 5 of T. E. Riley et al. (2021) for additional details about the figure elements.
Paper: A NICER View of PSR J1231−1411: A Complex Case
Authors: Tuomo Salmi, Julia S. Deneva, Paul S. Ray, Anna L. Watts, Devarshi Choudhury, Yves Kini, Serena Vinciguerra, H. Thankful Cromartie, Michael T. Wolff, Zaven Arzoumanian, Slavko Bogdanov, Keith Gendreau, Sebastien Guillot, Wynn C. G. Ho, Sharon M. Morsink, Ismaël Cognard, Lucas Guillemot, Gilles Theureau, Matthew Kerr
Figure caption: Bolometric pulse profiles (counts summed over energy channels) for the maximum-likelihood parameters (red-stepped curves) of the ST-U H T else (upper left-hand panel) and PDT-U H R eq ∈ [10, 14] km (upper right-hand panel) km models. See Table 1 and Section 4.2 for model explanations. The bolometric NICER data are shown with black-stepped curves. The differences (data − model) are shown in the bottom panels also with black-stepped curves. The expected Poisson fluctuation levels (for NICER data) are shown there with blue-dashed curves. We note that the model curves are rather similar between all the ST-U versions and between all the PDT-U versions.
Paper: A NICER View of PSR J1231−1411: A Complex Case
Authors: Tuomo Salmi, Julia S. Deneva, Paul S. Ray, Anna L. Watts, Devarshi Choudhury, Yves Kini, Serena Vinciguerra, H. Thankful Cromartie, Michael T. Wolff, Zaven Arzoumanian, Slavko Bogdanov, Keith Gendreau, Sebastien Guillot, Wynn C. G. Ho, Sharon M. Morsink, Ismaël Cognard, Lucas Guillemot, Gilles Theureau, Matthew Kerr
Figure caption: The phase-folded PSR J1231−1411 event data for two rotational cycles (for clarity). The top panel shows the pulse profile summed over the channels. The total number of counts is given by the sum over all phase-channel pairs (over both cycles). For the modeling, all the event data are grouped into a single rotational cycle instead, and thus each phase-channel bin has twice the number of counts shown here.
Paper: A NICER View of PSR J1231−1411: A Complex Case
Authors: Tuomo Salmi, Julia S. Deneva, Paul S. Ray, Anna L. Watts, Devarshi Choudhury, Yves Kini, Serena Vinciguerra, H. Thankful Cromartie, Michael T. Wolff, Zaven Arzoumanian, Slavko Bogdanov, Keith Gendreau, Sebastien Guillot, Wynn C. G. Ho, Sharon M. Morsink, Ismaël Cognard, Lucas Guillemot, Gilles Theureau, Matthew Kerr
Figure caption: Posterior-expected pulse profiles for the joint NICER and XMM-Newton analysis using the PDT-U H R eq ∈ [10, 14] km model. The top and top-center panels show the signal incident on the telescopes, and the bottom-center and bottom panels show the signal registered by NICER after accounting for the instrument response. The blue-dashed curves show the posterior-expected signals generated by the two hot regions separately and the black-solid curves in combination. The conditional posterior distribution of the incident photon flux and the NICER count rate are also presented (purple contours in the top-center and bottom panels, respectively). See Figure 11 of T. E. Riley et al. (2021) for additional details about the figure elements.
Paper: A NICER View of PSR J1231−1411: A Complex Case
Authors: Tuomo Salmi, Julia S. Deneva, Paul S. Ray, Anna L. Watts, Devarshi Choudhury, Yves Kini, Serena Vinciguerra, H. Thankful Cromartie, Michael T. Wolff, Zaven Arzoumanian, Slavko Bogdanov, Keith Gendreau, Sebastien Guillot, Wynn C. G. Ho, Sharon M. Morsink, Ismaël Cognard, Lucas Guillemot, Gilles Theureau, Matthew Kerr
Figure caption: Inferred NICER background for the joint NICER and XMM-Newton analysis using the PDT-U H R eq ∈ [10, 14] km model. The blue solid stepped curve shows the total NICER count-rate spectrum. The orange stepped curves show the backgrounds that maximize the likelihood for 1000 equally weighted posterior samples. The red curve shows the corresponding background for the maximum-likelihood sample. The black-dashed (dotted–dashed) curve shows the highest (lowest) background when considering the model uncertainty, as explained in Section 2.1. The inferred backgrounds of the other presented models are very similar to those shown here.
Paper: A NICER View of PSR J1231−1411: A Complex Case
Authors: Tuomo Salmi, Julia S. Deneva, Paul S. Ray, Anna L. Watts, Devarshi Choudhury, Yves Kini, Serena Vinciguerra, H. Thankful Cromartie, Michael T. Wolff, Zaven Arzoumanian, Slavko Bogdanov, Keith Gendreau, Sebastien Guillot, Wynn C. G. Ho, Sharon M. Morsink, Ismaël Cognard, Lucas Guillemot, Gilles Theureau, Matthew Kerr
Figure caption: A 2D ﹩\cos i\unicode{8210}M﹩ prior distribution based on the radio timing measurements from T. Cromartie et al. (2024, in preparation). The color indicates the probability of a ﹩\cos i\unicode{8210}M﹩ cell.
Paper: Disk Turbulence and Star Formation Regulation in High-z Main-sequence Analog Galaxies
Authors: Laura Lenkić, Deanne B. Fisher, Alberto D. Bolatto, Peter J. Teuben, Rebecca C. Levy, Jiayi Sun, Rodrigo Herrera-Camus, Karl Glazebrook, Danail Obreschkow, Roberto Abraham
Figure caption: Radial distribution of beam-smearing-corrected velocity dispersion measurements in DYNAMO along beam-sized sightlines (blue data points). The black solid line corresponds to the median velocity dispersion in DYNAMO galaxies at radii larger than 1.5× the beam FWHM. The error bars in the top left corner of each panel indicates the beam FWHM and the channel size of the CO(3−2) observations used to measure velocity dispersions. For comparison, the black dashed and dotted–dashed lines mark the molecular gas and ionized gas velocity dispersion respectively from M. Girard et al. (2021), while the gray shaded region indicates their uncertainties. Within the size of the channel width, our beam-smearing-corrected velocity dispersions are consistent with those found by M. Girard et al. (2021). Finally, the yellow solid line is the radial profile of the median beam smearing correction we apply to each velocity dispersion measurement.
Paper: Disk Turbulence and Star Formation Regulation in High-z Main-sequence Analog Galaxies
Authors: Laura Lenkić, Deanne B. Fisher, Alberto D. Bolatto, Peter J. Teuben, Rebecca C. Levy, Jiayi Sun, Rodrigo Herrera-Camus, Karl Glazebrook, Danail Obreschkow, Roberto Abraham
Figure caption: The same as Figure 5; however, we now include the DYNAMO velocity dispersion measurements with no beam smearing correction as gray circles. In this case, we fit the power law to these uncorrected data, and find steeper slopes and best-fit relations that are inconsistent with the best-fit relations presented in Table 2.
Paper: Disk Turbulence and Star Formation Regulation in High-z Main-sequence Analog Galaxies
Authors: Laura Lenkić, Deanne B. Fisher, Alberto D. Bolatto, Peter J. Teuben, Rebecca C. Levy, Jiayi Sun, Rodrigo Herrera-Camus, Karl Glazebrook, Danail Obreschkow, Roberto Abraham
Figure caption: The same as Figure 5; however, we now exclude all beam-smearing-corrected measurements that are within two beams of each galaxy center. When we refit the power laws to this subset of measurements we find results that are consistent with what is presented in Table 2.
Paper: The SAGA Survey. IV. The Star Formation Properties of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Marla Geha, Yao-Yuan Mao, Risa H. Wechsler, Yasmeen Asali, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, Yunchong Wang, John F. Wu
Figure caption: Gas-phase metallicity, 12+log(O/H), for SAGA satellites color-coded by sSFRNUV. White squares are binned SAGA medians and 16/84th percentile scatter. We compare to SDSS DR8 (gray) for galaxies with z < 0.035. All metallicities have been derived using the N2 index and Marino et al. (2013) calibration. Only individual satellites with line fluxes with S/N > 4 (circles) are included in the medians; SAGA satellites with line fluxes 3 > SN > 4 (triangles) are shown for comparison. We plot the LMC/SMC metallicities as stars (see Section 7.2 for references). SAGA satellites lie at slightly higher gas-phase metallicities as compared to the SDSS sample. Satellites with higher sSFRs lie at lower gas-phase metallicities for a given stellar mass.
Paper: The SAGA Survey. IV. The Star Formation Properties of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Marla Geha, Yao-Yuan Mao, Risa H. Wechsler, Yasmeen Asali, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, Yunchong Wang, John F. Wu
Figure caption: Literature measurements of atomic gas mass for 61 SAGA satellites: gas mass vs. stellar mass (left) and gas fraction vs. stellar mass (right). The LMC/SMC are shown as stars, with small gray bars indicating the addition of MC Stream gas. In the left panel, we plot the empirical relationship from Bradford et al. (2015) for isolated galaxies. The median SAGA bins (white squares) fall below the Bradford et al. relation. In both panels, we compute the minimum gas fraction observable based on the ALFALFA H I flux limit of the ALFALFA for satellite between 25 and 40 Mpc (gray region). In both panels, satellites are color-coded by sSFRNUV;  gas-poor satellites have lower sSFRNUV.
Paper: The SAGA Survey. IV. The Star Formation Properties of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Marla Geha, Yao-Yuan Mao, Risa H. Wechsler, Yasmeen Asali, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, Yunchong Wang, John F. Wu
Figure caption: The quenched fraction of SAGA satellite vs. projected distance from host. In all panels, we split the sample by host property, plotting the quenched fraction of systems above (green squares) and below (purple circles) the median value of (from left to right) group mass (a proxy for halo mass), host stellar mass, host g − r color, SFRNUV, and distance to nearest massive galaxy. The parenthetical numbers are the median values of these host properties. Because quenched fractions depend strongly on stellar mass, we plot separately satellites with stellar masses above 108.5 M ⊙ (top) and between 107.5−8.5 M ⊙ (bottom).
Paper: The SAGA Survey. IV. The Star Formation Properties of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Marla Geha, Yao-Yuan Mao, Risa H. Wechsler, Yasmeen Asali, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, Yunchong Wang, John F. Wu
Figure caption: Left: Cumulative number of star-forming satellites split into quartiles of sSFRHα  for the Gold+Silver sample. The shaded regions represent the contribution from incompleteness correction. The quartile with the lowest sSFR (lightest blue) follows the quenched population trend of being more concentrated toward the host. We indicate the radii that encloses half of each of the respective populations as vertical bars for the full SF sample (black), the least/most sSFR quartiles (light/dark blue), and the quenched population (red). Right: The sSFRHα  vs. projected radius for star-forming satellites color-coded by stellar mass. The median sSFR in bins of projected radius are shown for the Gold and Silver samples separately (squares).
Paper: The SAGA Survey. IV. The Star Formation Properties of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Marla Geha, Yao-Yuan Mao, Risa H. Wechsler, Yasmeen Asali, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, Yunchong Wang, John F. Wu
Figure caption: The BPT (left) and [S II]-BPT (right) diagram for SAGA satellites color-coded by stellar mass. The SAGA background sample (z < 0.035 and M ⋆ < 1010 M ⊙) is shown by the gray contour-scatter plots. We restrict both samples to galaxies with S/N > 4 in all lines, but also plot satellites with a lower threshold 3 > S/N > 4 for comparison (triangles). Regions of the BPT where emission is dominated by star formation (SF), AGN, or composite (Comp) are labeled. No high-S/N SAGA satellites fall within the AGN region as defined by Kewley et al. (2006, solid line) or Kauffmann et al. (2003, dotted line). The single SAGA satellite AGN confirmed via radio continuum does not fall in the optical AGN region (red circle). The SAGA satellite population roughly follows the background distribution.
Paper: The SAGA Survey. IV. The Star Formation Properties of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Marla Geha, Yao-Yuan Mao, Risa H. Wechsler, Yasmeen Asali, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, Yunchong Wang, John F. Wu
Figure caption: The SFRNUV (left) and sSFRNUV (right) as a function of stellar mass. SAGA star-forming satellites are plotted as gray circles. Triangles indicate NUV upper limits. Solid blue squares are binned medians, excluding upper limits. The SAGA background (SAGAbg) galaxy sample (z < 0.035) is plotted as dashed black line. The green line (Leroy et al. 2019) is fit at higher stellar mass and plotted down to the stellar mass where it is well-measured. An extrapolation to lower stellar mass would disagree with SAGA samples. The SAGA satellites and background sample agree well with the LVL sample (orange line) from Dale et al. (2023). These samples are all fit in the same stellar mass regime.
Paper: Estimating the Total Energy Content in Escaping Accelerated Solar Electron Beams
Authors: Alexander W. James, Hamish A. S. Reid
Figure caption: (a) Arched plasma structure seen in the AIA 131 Å channel (outlined with a red dashed line), interpreted as a hot magnetic flux rope signature. (b) Overlying loops (blue line) and two J-shaped flare ribbons (black dashed lines) seen in the AIA 171 Å channel. (c) Twin EUV dimmings seen in base-difference images in the AIA 211 Å channel (yellow arrows, base time at 12:00 UT on 2013 May 22). Overlying loops (blue arrow) dim and disappear from in this channel as they are deflected by the erupting CME. (d) Two J-shaped flare ribbons seen in the 195 Å channel of STEREO-A/EUVI, outlined with black dashed lines.
Paper: The SAGA Survey. IV. The Star Formation Properties of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Marla Geha, Yao-Yuan Mao, Risa H. Wechsler, Yasmeen Asali, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, Yunchong Wang, John F. Wu
Figure caption: Gas fraction plotted against projected distance from host, color-coded by the relative velocity separation between satellite and host. Satellites with low gas fractions are seen at all projected radii, but are more tightly bound to their hosts (smaller relative velocities) as compared to satellites with higher gas fractions.
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: PSF-subtracted, collapsed-cube images of η Tel, in which the PSF was scaled to the photosphere of the star to reveal the total flux contribution from the disk. The images are linearly scaled from 0 to 104 MJy sr−1 and zoom in on the disk. The contour lines indicate regions at 3σ, 5σ, 20σ, and 50σ detection thresholds for each subband image. The location of the primary is marked with a blue star, and the white arrow indicates the direction of the brown dwarf companion. The wavelength labels give the central wavelengths of each subband to which each image has been collapsed. Note that the radial extent of the disk appears to increase with wavelength.
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: Similar to Figure 6, except the PSF has been scaled to the peak flux of the science image before being subtracted, in order to reveal the spatially resolved dust component. The images are displayed with a linear scaling from 0 to 1.15 × 103 MJy sr−1. We observe that the disk appears largely axisymmetric across all wavelengths and that there appears to be a slight offset in PA between the disk and the position of η Tel B. We also note the apparent increase in the radial extent and inner cavity size of the disk with wavelength. The latter only appears in this scaling and is likely an artifact introduced by PSF subtraction.
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: Projected orbits of η Tel B from orbital derivation. Center: on-sky depiction of a sample of 100 potential orbits. The blue star marks the location of the primary and the maroon point marks the current location of the companion from MRS astrometry. Left: close-up of relative astrometry points clustered in the center image. The orange points indicate literature values. Right: separation and PA vs. epoch for the companion with respect to the primary. Due to the long-period nature of the orbit, it is likely that any significant change in separation/PA will not be observable for another few decades.
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: Top: transmission profiles for each photometric filter, indicating flux density throughput versus bandwidth on a normalized scale, where 1 is full flux transmitted and 0 is no flux transmitted. Middle: the full 0.85–21 μm spectral energy distribution of η Tel B, showing existing spectra and photometry along with the new MIRI MRS 11–20 μm spectrum. The black line shows the best-fit atmosphere model for the companion, which was calculated by fitting the spectroscopic and photometric data to a BT-SETTL (CIFIST) model grid using species (T. Stolker et al. 2020). The T eff, ﹩\mathrm{log}g﹩, and R values are consistent with expectations for a M7/8-type brown dwarf (see Table 1). Bottom: residual flux density for each data point from the literature compared to the best-fit model in σ. All residuals are within ± 5σ, indicating that the model is a good fit to the data.
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: Photosphere-subtracted spectrum of η Tel A, clearly showing the 10 μm feature weakly detected by Spitzer IRS, as well as a broad 20 μm feature detected for the first time in this disk. The best-fit model for the total contribution from the continuum is shown in black; the continuum is best fit by two blackbody components corresponding to a warm dust population with T  w  = 319 ± 59 K and a cool population with T  c  = 127 ± 25 K. This two-component structure is consistent with previous modeling of the disk (C. H. Chen et al. 2006; R. Smith et al. 2009).
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: MIRI MRS spectrum of η Tel B, compared to the atmosphere model from Section 4.1. The extracted spectrum is consistent with the model, showing no IR excess. The data set used to create this figure is available for download from the online journal.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: Left: 18 μm slice of MIRI MRS data, following peak-scaled PSF subtraction. Both lobes appear similar in brightness. Center: model of disk with e  f  = 0.1 that has been convolved with the MIRI MRS PSF at 18 μm, then PSF-subtracted. The pericenter lobe appears slightly brighter. Right: residuals after subtracting the MIRI MRS data slice from the model image, showing remnant structure in the pericenter lobe.
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: Photosphere + continuum-subtracted spectrum of the η Tel A disk, binned by a factor of 10. There is a firm detection of the 10 and 20 μm dust component features. Modeling indicates the presence of large amorphous olivine and pyroxene grains, as well as some silica, in the disk. The model’s difficulty with fitting the tail end of the broad 20 μm feature may be due to the presence of additional components that we do not account for; more detailed modeling outside the scope of this work may help to identify these components.