adsabs/AstroCLIMB huggingface dataset:
Paper: Dust in Little Red Dots
Authors: Caitlin M. Casey, Hollis B. Akins, Vasily Kokorev, Jed McKinney, Olivia R. Cooper, Arianna S. Long, Maximilien Franco, Sinclaire M. Manning
Figure caption: The average rest-frame UV through radio SED of the 675 LRDs in this work. The raw OIR/near-IR photometry of all LRDs is shown in light-blue points, the median stack in dark-blue points, and best-fit BAGPIPES model to the median stack by the thin blue line. The purple shaded region denotes the 68th and 95th percentile confidence regions on the derived dust SED discussed in Section 3, and the best-matched ∼100 K (B. Draine & A. Li 2007) model is shown in dark purple. The matching radio synchrotron component, assuming the FIR/radio correlation holds to high-z (V. Smolčić et al. 2017), is shown in teal with ±0.5 dex. The expectation for AGN torus emission is shown in orange, matched to the same predicted L IR as the SED in Section 3. The total SED, summing optical/near-IR, dust, and synchrotron components, is shown in gray (using the Draine & Li star formation template) and black (using the Nenkova et al. torus template); both are made available. Measured 5σ limits in the mid/far-IR are shown in light-green triangles from A24 and from I. Labbe et al. (2023) in dark green. Vertical gray bars show the 5σ continuum depth achievable by ALMA in each of its observing bands with a 1 hr on-source integration time (as of ALMA Cycle 11 in 2024).
Paper: 2019 UO14: A Transient Trojan of Saturn
Authors: Man-To Hui, 文韜 許, Paul A. Wiegert, Robert Weryk, Marco Micheli, David J. Tholen, Sam Deen, Andrew J. Walker, Richard Wainscoat
Figure caption: Comparison of 2019 UO14 (plotted as a magenta star) to other Trojans and Centaurs, with active Centaurs highlighted (see the legends), in the space of (a) semimajor axis (a) vs. eccentricity (e) and (b) perihelion distance (q) vs. inclination (i). Other Trojans were queried from the MPC, and Centaurs were sourced from the JPL Small-Body Database Query with constraints on semimajor axes a J ≤ a ≤ a N, perihelion distances a J ≤ q ≤ a N, and exclusions of Trojans (a J and a N are the semimajor axes of Jupiter and Neptune, respectively). The list of active Centaurs was compiled using D. Jewitt (2009) and A. Guilbert-Lepoutre (2012), along with objects with cometary designations from the JPL Small-Body Database Query. The four labeled dashed curves in the left panel represent loci of orbits with perihelion distances equal to those of the four giant planets. The two vertical gray dotted lines in both panels mark the boundaries of the Centaur region at the semimajor axes of Jupiter and Neptune.
Paper: Dust in Little Red Dots
Authors: Caitlin M. Casey, Hollis B. Akins, Vasily Kokorev, Jed McKinney, Olivia R. Cooper, Arianna S. Long, Maximilien Franco, Sinclaire M. Manning
Figure caption: The dust mass volume density of the Universe placing LRDs (dark red) in context. Measurements presented in the literature are made from the FIR background directly (yellow; C. Thacker et al. 2013), galaxies with directly observable FIR SEDs (lavender; L. Dunne et al. 2011; R. A. Beeston et al. 2018; S. P. Driver et al. 2018; F. Pozzi et al. 2020), extrapolation from extinction/reddening of OIR SEDs (light red; B. Ménard et al. 2010; B. Ménard & M. Fukugita 2012), and neutral gas depletion (teal; C. Péroux & J. C. Howk 2020). We overplot the integrated contribution from IR luminous galaxies with L IR > 109 L ⊙ in brown, and specifically from ULIRGs (orange; L IR > 1012 L ⊙) and LIRGs (tan; 1011 < L IR < 1012 L ⊙) from the C. Casey et al. (2018) model, using the measured luminosity function parameters from J. A. Zavala et al. (2021). Despite their relatively high number density, LRDs are thought to only contribute ∼0.1% to the cosmic dust budget relative to the total, which is dominated by IR luminous galaxies.
Paper: Dust in Little Red Dots
Authors: Caitlin M. Casey, Hollis B. Akins, Vasily Kokorev, Jed McKinney, Olivia R. Cooper, Arianna S. Long, Maximilien Franco, Sinclaire M. Manning
Figure caption: Top left: photometric redshift vs. visual magnitudes of extinction (A  V ) inferred through SED fitting presented in K24 and A24. On the right y-axis we show the mapping from A  V  to dust mass surface density using Equation (1). Top right: the estimated dust masses (M dust) and dust luminosities (L IR) for the sample. L IR is agnostic to the source of emission (whether AGN or star formation), while M dust depends on size and thus may be regarded as an upper limit. Bottom: reported size measurements for LRDs against the interpolated peak SED dust temperature, which is derived from the combination of M dust and L IR.
Paper: PKS 2254+074: A Blazar in Likely Association with the Neutrino Event IceCube-190619A
Authors: Shunhao Ji, Zhongxiang Wang
Figure caption: Left: 180 day binned γ-ray light curve of PKS 2254+074 in 0.1–500 GeV (upper), its optical Catalina V band and ZTF zg- and zr-band light curves (middle), and MIR WISE light curves (bottom). The orange line marks the arrival time of IC-190619A. In the upper panel, the red line represents the average flux, the cyan histograms mark the blocks, and the gray region marks the flare defined by the HOP algorithm. Right: 30 day binned γ-ray light curve during the time period marked by the two blue dashed lines in the upper left panel and the arrival times of ≥10 GeV photons with probability >68% (lower right panel; see Section 2.2.3). In both γ-ray light-curve panels, the downward triangles are the 95% C.L. flux upper limits, and red histograms indicate the TS values of the data points.
Paper: PKS 2254+074: A Blazar in Likely Association with the Neutrino Event IceCube-190619A
Authors: Shunhao Ji, Zhongxiang Wang
Figure caption: TS map of size 8° × 8° centered at IC-190619A in the energy of 0.1–500 GeV. The dashed cyan ellipse marks the uncertainty region with the systematic uncertainty (by scaling the major and minor axes of the 90% error ellipse with a factor of 1.3; P. Giommi et al. 2020a) included, and the pink ellipse marks the uncertainty region given in IceCat-1. In addition to PKS 2254+074 (4FGL J2257.5+0748), another Fermi-LAT source (4FGL J2306.6+0940) is also in the uncertainty region in IceCat-1.
Paper: PKS 2254+074: A Blazar in Likely Association with the Neutrino Event IceCube-190619A
Authors: Shunhao Ji, Zhongxiang Wang
Figure caption: Broadband SED of PKS 2254+074. The gray dots are the archival data from Firmamento. The Swift-XRT X-ray spectrum is plotted as the blue dots. The γ-ray spectrum in the flare and the model fit in the low state are plotted as red diamonds and cyan region, respectively. The estimated neutrino fluxes for two time intervals (see Section 3) are shown as the red and gray lines.
Paper: From Coasting to Energy-conserving: New Self-similar Solutions to the Interaction Phase of Strong Explosions
Authors: Eric R. Coughlin
Figure caption: A diagram of the relevant radii, being the RS, the CD, and the FS, as well as the ejecta radius R ej; the latter is the radius that the CD and RS would have in the limit that the ratio of the ambient to ejecta density were identically 0. The top right inset shows how the ejecta density declines with time as ﹩{R}_{{\rm{r}}}^{-m}﹩, where m = 2 for a steady wind and m = 3 for homologously expanding ejecta, as well as the power-law decline of the ambient density as ∝r −n  and the overall variation of the density throughout the shocked FS and RS shells. The inset on the bottom right shows a zoom-in on the RS–CD–FS structure, as well as the locations of the three discontinuities in the top right inset.
Paper: From Coasting to Energy-conserving: New Self-similar Solutions to the Interaction Phase of Strong Explosions
Authors: Eric R. Coughlin
Figure caption: The self-similar density (top), velocity (middle), and pressure (bottom) for a wind-driven explosion (m = 2; left) and that driven by homologous ejecta (m = 3; right) for the values of the ambient density power-law index n shown in the legend. In all cases, we set γ = 5/3.
Paper: Expansion Properties of the Young Supernova Type Iax Remnant Pa 30 Revealed
Authors: Tim Cunningham, Ilaria Caiazzo, Nikolaus Z. Prusinski, James Fuller, John C. Raymond, S. R. Kulkarni, James D. Neill, Paul Duffell, Chris Martin, Odette Toloza, David Charbonneau, Scott J. Kenyon, Zeren Lin, Mateusz Matuszewski, Rosalie McGurk, Abigail Polin, Philippe Z. Yao
Figure caption: Left: WISE W4 (22 μm) image from the WISE image service (E. L. Wright et al. 2010). Because the inner infrared nebula in the WISE image is much brighter than the outer one, to show the location of both nebulae we superimpose two versions of the same image with different contrast levels, following the method of V. V. Gvaramadze et al. (2019), so that the outer nebula appears in uniform dark purple. For clarity, we also overlay contours of constant W4 infrared flux (thin white lines). The 14 contours plotted are evenly spaced in flux, with a separation of 8 μJy, from 5.44 to 5.54 mJy. The minimum and maximum flux in the image are 5.43 and 5.55 mJy, respectively. Right: the WISE image is the same as in the left plot. On top of the WISE image, we plot as white points the deprojected positions of the filaments using our best-fit value of the ballistic fraction, k. The deprojected positions have been reflected, as they are in Figure 6, and rotated by 90° toward the viewer, turning line-of-sight positions into sky positions, while preserving the angular size.
Paper: Stripped Helium Star and Compact Object Binaries in Coeval Populations: Predictions Based on Detailed Binary Evolution Models
Authors: Chen Wang, Julia Bodensteiner, Xiao-Tian Xu, Selma E. de Mink, Norbert Langer, Eva Laplace, Alejandro Vigna-Gómez, Stephen Justham, Jakub Klencki, Aleksandra Olejak, Ruggero Valli, Abel Schootemeijer
Figure caption: Predicted properties of OB-type MS star binaries containing a helium-burning star (reddish brown bars), an NS that remains bound after SN kicks (turquoise bars with circles), an NS that is kicked out of the binary during SN explosion (cyan bars with diagonal lines), or a BH (orange bars) at 15 Myr. In the second and fourth panels, we exclude disrupted binaries to focus on binary features. The first panel displays the number distribution as a function of magnitude in terms of the HST/WFC3 F814W band. The gray open bars denote binaries containing two OB-type MS stars, with values on the right y-axis. The vertical dashed line marks the cluster turnoff magnitude. The upper panel shows the fraction of evolved massive binaries relative to the total number of stellar models at corresponding magnitudes with (dark) and without (light) SN kicks. The second panel shows the semiamplitude orbital velocity distribution of the OB star within evolved binaries and OB+OB systems. The third panel illustrates the velocity distribution of OB star components in evolved massive binaries. Open gray bars denote the rotational velocities of the secondary stars in OB+OB binaries, shown on the right y-axis. The fourth panel presents the mass ratio distribution. For evolved massive binaries, the mass ratio is defined as the ratio of the post-MS component’s mass to the OB component’s mass. For OB+OB binaries, it is the ratio of the secondary star’s mass to the primary star’s mass.
Paper: Stripped Helium Star and Compact Object Binaries in Coeval Populations: Predictions Based on Detailed Binary Evolution Models
Authors: Chen Wang, Julia Bodensteiner, Xiao-Tian Xu, Selma E. de Mink, Norbert Langer, Eva Laplace, Alejandro Vigna-Gómez, Stephen Justham, Jakub Klencki, Aleksandra Olejak, Ruggero Valli, Abel Schootemeijer
Figure caption: Panel (a): predicted numbers of postinteraction binaries as a function of age in a coeval stellar population with a total mass of 1.3 × 105 M ⊙. The solid lines in reddish brown, orange, turquoise, and purple represent binaries with an OB star paired with a helium-burning star, BH, NS, and WD component, respectively, under the fiducial assumptions. The dashed blue line denotes the number of OB+NS binaries without including SN kicks. Additionally, we depict the number of OB+OB binaries with m F814W ≤ 20 with the dotted gray line, referring to the scale on the right y-axis for its values. The shaded areas show one standard deviation of the Poisson distribution. The inset provides a zoomed-in view of the results for OB+NS binaries, assuming fiducial kicks. Panel (b): fraction of W-R stars, which are identified according to the criterion in T. Shenar et al. (2020a), among helium-burning stars with OB companions. Panel (c): fraction of OBe stars among OB+BH binaries. Here, we treat stellar models whose surface rotational velocities are higher than 95% of their breakup values as OBe stars. Panel (d): fraction of OBe stars among OB+NS binaries. The solid and dashed lines correspond to results for OB+NS binaries with and without SN kicks.
Paper: Stripped Helium Star and Compact Object Binaries in Coeval Populations: Predictions Based on Detailed Binary Evolution Models
Authors: Chen Wang, Julia Bodensteiner, Xiao-Tian Xu, Selma E. de Mink, Norbert Langer, Eva Laplace, Alejandro Vigna-Gómez, Stephen Justham, Jakub Klencki, Aleksandra Olejak, Ruggero Valli, Abel Schootemeijer
Figure caption: Predicted properties of OB+BH binaries as a function of cluster age. The color coding represents the number density of these binaries in each pixel. The left panels display the mass distribution of OB stars and BHs, whereas the right panels show the distribution of the semiamplitude orbital velocity of OB stars and current binary orbital periods. The gray line in the upper left panel depicts the turnoff mass as a function of cluster age. The step plots at the top and right margins of the main panels represent 1D projections. Notably, the 1D projection on the right side is normalized to unity, taking into account the duration of binaries possessing specific properties.
Paper: Stripped Helium Star and Compact Object Binaries in Coeval Populations: Predictions Based on Detailed Binary Evolution Models
Authors: Chen Wang, Julia Bodensteiner, Xiao-Tian Xu, Selma E. de Mink, Norbert Langer, Eva Laplace, Alejandro Vigna-Gómez, Stephen Justham, Jakub Klencki, Aleksandra Olejak, Ruggero Valli, Abel Schootemeijer
Figure caption: Similar to Figure 1 but for ages of 10, 30, 60, and 100 Myr.
Paper: ALMA Observations of Proper Motions of the Dust Clumps in the Protoplanetary Disk MWC 758
Authors: I-Hsuan Genevieve Kuo, Hsi-Wei Yen, Pin-Gao Gu
Figure caption: Azimuthal intensity distribution and displacement. (upper panel) ALMA 1.3 mm continuum maps deprojected in the polar coordinates. The azimuthal angle is defined counterclockwise from the minor axis of the disk. The color scale and contours present the 2021 and 2017 data, respectively. The contour levels are 5σ, 20σ, 30σ, 50σ, and 100σ. (middle panel) Intensity residuals (color) after subtracting the 2021 from 2017 maps presented in the upper panel. The contours present the 2021 continuum map with the contour levels the same as those in the upper panel. (lower panel) Azimuthal intensity profiles of the inner and outer clumps passing through the continuum peaks of the clumps extracted from the 2017 (blue) and 2021 (red) continuum maps. The inner clump is centered around 322°, and the outer clump is centered at 95°.
Paper: ALMA Observations of Proper Motions of the Dust Clumps in the Protoplanetary Disk MWC 758
Authors: I-Hsuan Genevieve Kuo, Hsi-Wei Yen, Pin-Gao Gu
Figure caption: Measured azimuthal velocity of the proper motions of the inner and outer clumps (green and blue data points, respectively), in comparison with the Keplerian rotational profile of MWC 758, a 2 M ⊙ star (cyan dots) with uncertainty of ±0.5 M ⊙ (shading). The error bars show the 1σ uncertainties of the measured azimuthal velocities. The inner clump peaks at a radius of 0.″32 and azimuthal angle of 320°, while the outer clump peaks at a radius of 0.″53 and azimuthal angle of 90°.
Paper: ALMA Observations of Proper Motions of the Dust Clumps in the Protoplanetary Disk MWC 758
Authors: I-Hsuan Genevieve Kuo, Hsi-Wei Yen, Pin-Gao Gu
Figure caption: Radial intensity distribution and displacement. (upper panel) Intensity residuals (color) after correcting for the measured azimuthal proper motions and subtracting the 2017 from 2021 maps in the polar coordinates. The contours present the 2017 continuum map with the contour levels the same as those in Figure 2. (lower panel) Radial intensity profiles of the inner and outer clumps passing through the continuum peaks of the clumps extracted from the 2017 (blue) and 2021 (red) continuum maps after correcting for the measured azimuthal proper motions.
Paper: ALMA Observations of Proper Motions of the Dust Clumps in the Protoplanetary Disk MWC 758
Authors: I-Hsuan Genevieve Kuo, Hsi-Wei Yen, Pin-Gao Gu
Figure caption: ALMA 1.3 mm continuum maps of the MWC 758 disk from the 2017 (left) and (right) 2021 data. The two maps have the same beam size of 0.″071, shown as white ellipses at the bottom left corners, and are generated with similar UV coverages. The contour levels are 5σ, 20σ, 30σ, 50σ, and 100σ.
Paper: ALMA Observations of Proper Motions of the Dust Clumps in the Protoplanetary Disk MWC 758
Authors: I-Hsuan Genevieve Kuo, Hsi-Wei Yen, Pin-Gao Gu
Figure caption: ALMA 1.3 mm continuum maps of the inner disk of MWC 758 from the 2017 (left) and (right) 2021 data. The two maps have the same beam size of 0.″071, shown as white ellipses at the bottom left corners, and are generated with similar UV coverages. The contour levels are 5σ and 10σ.
Paper: ALMA Observations of Proper Motions of the Dust Clumps in the Protoplanetary Disk MWC 758
Authors: I-Hsuan Genevieve Kuo, Hsi-Wei Yen, Pin-Gao Gu
Figure caption: Same as the Figure 3 but for the angular velocity.
Paper: Hints of New Physics for the Hubble Tension: Violation of Cosmological Principle
Authors: J. P. Hu, X. D. Jia, J. Hu, F. Y. Wang
Figure caption: Location distributions of different cutoff redshift SNe Ia in the galactic coordinate system. Panels (a)–(e) correspond to the redshift intervals (0, 0.10), (0.10, 0.20), (0.20, 0.30), (0.30, 0.50), and (0.50, 2.26), respectively. Panel (f) gives the location distribution of the Pantheon+ sample.
Paper: Hints of New Physics for the Hubble Tension: Violation of Cosmological Principle
Authors: J. P. Hu, X. D. Jia, J. Hu, F. Y. Wang
Figure caption: Redshift distribution of the Pantheon+ sample and the latest H(z) observation.
Paper: Expansion Properties of the Young Supernova Type Iax Remnant Pa 30 Revealed
Authors: Tim Cunningham, Ilaria Caiazzo, Nikolaus Z. Prusinski, James Fuller, John C. Raymond, S. R. Kulkarni, James D. Neill, Paul Duffell, Chris Martin, Odette Toloza, David Charbonneau, Scott J. Kenyon, Zeren Lin, Mateusz Matuszewski, Rosalie McGurk, Abigail Polin, Philippe Z. Yao
Figure caption: Deprojection fit with the assumptions outlined in the caption of Figure 5. The measured Doppler shift is converted into a line-of-sight distance using Equation (1), and plotted against the measured sky radius, which is defined as the distance from the central star on the sky in parsec. The central star is located at the origin of the graph. The data is reflected across the plane defined by r sky = 0 to enable an elliptical regression. The best-fit deprojection contour (solid) is found using the linear least-squares Levenberg–Marquardt algorithm to fit for the five parameters of the ellipse: a, b, x 0, y 0, and θ, which represent the semimajor axis, semiminor axis, x–y origin, and angle. The ballistic fraction, k, is then given by k = b/a. This yields a best-fit value of ﹩k={0.97}_{-0.08}^{+0.09}﹩, where the 1σ uncertainties also account for the uncertainty on the Gaia distance. The fitted values for the center of the ellipse are x 0 = 0.00 ± 0.05 pc and y 0 = 0.05 ± 0.03 pc. Right: posterior distribution of a and b from the elliptical regression shown in the left panel.
Paper: Expansion Properties of the Young Supernova Type Iax Remnant Pa 30 Revealed
Authors: Tim Cunningham, Ilaria Caiazzo, Nikolaus Z. Prusinski, James Fuller, John C. Raymond, S. R. Kulkarni, James D. Neill, Paul Duffell, Chris Martin, Odette Toloza, David Charbonneau, Scott J. Kenyon, Zeren Lin, Mateusz Matuszewski, Rosalie McGurk, Abigail Polin, Philippe Z. Yao
Figure caption: Top: histogram of the measured Doppler shift for all detected [S II] doublets, weighted by the measured flux in each doublet. The four peaks are fit with four Gaussians, finding two high-velocity broad peaks centered on −778 and +932 km s−1, and two narrower, lower-velocity features centered on −177 and +303 km s−1. The peak-to-peak distance between symmetric peaks is shown with the horizontal lines, while the vertical dashed line shows the mean velocity between each Gaussian pair. Assuming a spherically symmetric ejecta, this mean velocity provides an estimate of the total radial velocity of the system, which we find to be v s = 70 ± 7 km s−1. In this figure, all velocities are given in the rest frame of Earth. The heliocentric correction is found to be v H = +8.08 km s−1, yielding a total system line-of-sight velocity in the rest frame of the Sun to be v sys = 78 ± 4 km s−1. Bottom: velocity distribution for the deprojected velocities computed via Equations (2) and (7). The distribution becomes almost fully bimodal, with peaks at ±1000 km s−1. The fitted central velocities are ﹩\overline{{v}_{{\rm{b}}}}=-927\pm 4﹩ and ﹩\overline{{v}_{{\rm{r}}}}=1022\pm 2﹩ km s−1, for the blue and redshifted components, respectively. The vertical dashed lines indicate the 99% confidence interval on the filament velocities.
Paper: Expansion Properties of the Young Supernova Type Iax Remnant Pa 30 Revealed
Authors: Tim Cunningham, Ilaria Caiazzo, Nikolaus Z. Prusinski, James Fuller, John C. Raymond, S. R. Kulkarni, James D. Neill, Paul Duffell, Chris Martin, Odette Toloza, David Charbonneau, Scott J. Kenyon, Zeren Lin, Mateusz Matuszewski, Rosalie McGurk, Abigail Polin, Philippe Z. Yao
Figure caption: Lower panel: narrowband image obtained from stacking all the KCWI-red channel cubes and integrating over the wavelength range 6680–6750 Å, covering the maximally blue- and redshifted [S II] emission features. Upper panel: the black and white image shows the [S II] narrowband data from R. A. Fesen et al. (2023), obtained with the Hiltner telescope at Kitt Peak. Superimposed in orange and with a large transparency, we show for comparison the same KCWI-red image as in the lower panel. The zoomed-in panel shows in red the contours of the filaments in the KCWI-red image: the same filaments are detected in the two images, but the KCWI-red image is deeper, allowing the detection of fainter features.
Paper: Expansion Properties of the Young Supernova Type Iax Remnant Pa 30 Revealed
Authors: Tim Cunningham, Ilaria Caiazzo, Nikolaus Z. Prusinski, James Fuller, John C. Raymond, S. R. Kulkarni, James D. Neill, Paul Duffell, Chris Martin, Odette Toloza, David Charbonneau, Scott J. Kenyon, Zeren Lin, Mateusz Matuszewski, Rosalie McGurk, Abigail Polin, Philippe Z. Yao
Figure caption: Deprojection of the measured line-of-sight velocities and sky position. The x-axis parameter, sky radius, describes the distance between the central star and any given point on the sky, collapsing the 2D sky positions into one dimension only. The parameter k, increasing from left to right, indicates the fraction of the ballistic velocity used in the deprojection. Under the assumptions that all material was ejected in the year 1181 and that the nebula has approximately spherical symmetry (as implied by the existing narrowband imaging; R. A. Fesen et al. 2023), we can see qualitatively that k should be close to unity, and therefore that the velocities in the ejecta are close to the ballistic free-expansion velocity. The contours show the predicted spatial location for material ejected at different velocities, from 700 km s−1 at the inner edge, to 1300 km s−1 at the outer edge.