adsabs/AstroCLIMB huggingface dataset:
Paper: Challenging the Active Galactic Nucleus Scenario for JWST/NIRSpec Little Red Dot and Non–Little Red Dot Broad Hα Emitters in Light of Nondetection of NIRCam Photometric Variability and X-Ray
Authors: Mitsuru Kokubo, Yuichi Harikane
Figure caption: kbol,X as a function of Lbol. The data points denote lower limits of kbol,X because none of them are X-ray detected. Filled circles denote the lower limits for the JWST broad Hα emitters studied in this work (assuming Γ = 1.7 power law for the X-ray spectral model): GLASS 150029, GLASS 160133, MSAID2008, MSAID4286, and MSAID38108 from left to right. Open circles denote the R. Maiolino et al. (2025) sample of the LRD and non-LRD broad Hα emitters at z > 4 discovered by the JADES and GA-NIFS surveys, and the open star symbol denotes the lower limit for the stacked X-ray data. Open triangles denote the T. T. Ananna et al. (2024) UNCOVER sample cross-matched with the J. E. Greene et al. (2024) sample of the LRD broad Hα emitters. The black lines show the best fit and dispersion (1σ) of the kbol,X–Lbol relation for broad-line AGNs from F. Duras et al. (2020).
Paper: Challenging the Active Galactic Nucleus Scenario for JWST/NIRSpec Little Red Dot and Non–Little Red Dot Broad Hα Emitters in Light of Nondetection of NIRCam Photometric Variability and X-Ray
Authors: Mitsuru Kokubo, Yuichi Harikane
Figure caption: Cutouts of the NIRCam single-epoch images of the non-LRD broad Hα emitter GLASS 160133. The first and second rows of each panel are the unconvolved epoch 1 and epoch 2/epoch 3 images (Mepoch 1, Mepoch 2, and Mepoch 3), and the third row corresponds to the cross-convolved difference images (D* in Equation (3)), respectively. The red circles indicate the circular aperture positions (r = 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩08 and 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩16 for short and long channels, respectively) used for the photometry given in Table 5. The gray scale is linear (from −0.05 to 0.05 counts, where 1 count = 28 mag).
Paper: Challenging the Active Galactic Nucleus Scenario for JWST/NIRSpec Little Red Dot and Non–Little Red Dot Broad Hα Emitters in Light of Nondetection of NIRCam Photometric Variability and X-Ray
Authors: Mitsuru Kokubo, Yuichi Harikane
Figure caption: Same as Figure 8, but for the LRD broad Hα emitter MSAID38108.
Paper: Challenging the Active Galactic Nucleus Scenario for JWST/NIRSpec Little Red Dot and Non–Little Red Dot Broad Hα Emitters in Light of Nondetection of NIRCam Photometric Variability and X-Ray
Authors: Mitsuru Kokubo, Yuichi Harikane
Figure caption: Same as Figure 6, but for the LRD broad Hα emitter MSAID2008. The upper panel shows the epoch 1 and epoch 2 images, and the lower panel shows the epoch 1 and epoch 3/epoch 4 images.
Paper: Challenging the Active Galactic Nucleus Scenario for JWST/NIRSpec Little Red Dot and Non–Little Red Dot Broad Hα Emitters in Light of Nondetection of NIRCam Photometric Variability and X-Ray
Authors: Mitsuru Kokubo, Yuichi Harikane
Figure caption: Same as Figure 6, but for the non-LRD broad Hα emitter GLASS 150029.
Paper: Challenging the Active Galactic Nucleus Scenario for JWST/NIRSpec Little Red Dot and Non–Little Red Dot Broad Hα Emitters in Light of Nondetection of NIRCam Photometric Variability and X-Ray
Authors: Mitsuru Kokubo, Yuichi Harikane
Figure caption: Same as Figure 8, but for the LRD broad Hα emitter MSAID4286.
Paper: The Head-on Collision of a Neutron Star with a White Dwarf
Authors: Zong-kai Peng, He Gao, Xian-Fei Zhang
Figure caption: Evolution of the relative distance between the pseudo-WD and the NS after the collision for a WD mass of 1.0 M⊙. The solid lines represent the relative distance for seven different values of Cn, while the dashed line denotes the sum of the WD and NS radii. Due to the energy loss during the collision, all results consistently show that the NS ultimately sinks toward the center of the WD.
Paper: The Head-on Collision of a Neutron Star with a White Dwarf
Authors: Zong-kai Peng, He Gao, Xian-Fei Zhang
Figure caption: The temperature profile of the reaction region. The sharp drop in the curve corresponds to the NS traversing the WD. The black dashed line denotes a temperature of 1 × 109 K, which is the ignition temperature of carbon (X. Chen et al. 2014), while the pink dashed line represents 3 × 109 K, corresponding to the critical burning temperature of oxygen (C.-Y. Wu & B. Wang 2018). The red dashed line denotes the temperature at which the thermal pressure equals the electron degeneracy pressure.
Paper: Active Galactic Nucleus-driven Biconical Outflows as the Origin of the Double-peaked [O III] Doublet in SDSS J134733.36+121724.27
Authors: PeiZhen Cheng, XingQian Chen, GuiLin Liao, Qi Zheng, Ying Gu, MuLin Chen, XueGuang Zhang
Figure caption: The best-fitting results and the corresponding residuals to the emission lines around Hα (panels (a) and (b)), and around Hβ (panels (c) and (d)), and the bad-fitting results and the corresponding residuals to the emission lines around Hβ (panels (e) and (f)). In panels (a), (c), and (e), the solid dark green lines show the line spectrum, and the solid red lines show the best-fitting results. The horizontal dashed red line shows fλ = 0. In panel (a), the solid and dashed blue lines show the determined core and extended components in narrow Hα, and the solid magenta line shows the determined component in broad Hα. The solid and dashed purple lines show the determined core and extended components in the [N II] doublet. The solid and dashed cyan lines show the determined core and extended components in the [O I] doublet. The solid and dashed green lines show the determined core and extended components in the [S II] doublet. In panel (c), the solid and dashed green lines show the determined core and extended components in narrow Hβ. The solid blue and red lines show the determined blueshifted and redshifted emission profiles in the [O III] doublet. The dashed purple lines show the determined extended components in the [O III] doublet. In panel (e), the solid blue line shows the determined core components in the [O III] doublet. The other line styles have the same meanings as those in panel (c). In panels (b), (d), and (f), the corresponding residuals are shown in dark green, with the horizontal red lines showing residuals = 0, ±1.
Paper: Active Galactic Nucleus-driven Biconical Outflows as the Origin of the Double-peaked [O III] Doublet in SDSS J134733.36+121724.27
Authors: PeiZhen Cheng, XingQian Chen, GuiLin Liao, Qi Zheng, Ying Gu, MuLin Chen, XueGuang Zhang
Figure caption: Comparative analysis of the emission-line spectra of SDSS J1347+1217 between the SDSS and SP2 observations. The top left panel shows the best descriptions of the host galaxy contributions for the SP2 spectrum. The line styles have the same meanings as those in the top panel of Figure 1. The top right panel shows the comparison of the emission-line spectra after subtracting the host galaxy contributions and AGN continuum emissions between the SP2 (dark green) and SDSS (red; shifted upward by 80 along the y-axis for a clearer comparison). The middle panels show the detailed emission-line spectra within the top right panel between the SP2 (dark green) and SDSS (red) around Hβ and Hα, respectively. The bottom panels show the spectral differences (SP2 – SDSS) around Hβ and Hα, respectively. The horizontal solid red line shows fλ = 0. The red semitransparent regions in the middle left and bottom left panels highlight the significant differences between the SP2 and SDSS spectra, which may be attributed to poor observational quality. The solid blue line in the bottom right panel indicates that a single Gaussian function provides a good description of the difference between the SP2 and SDSS spectra.
Paper: The Head-on Collision of a Neutron Star with a White Dwarf
Authors: Zong-kai Peng, He Gao, Xian-Fei Zhang
Figure caption: The relative displacement of the NS with the center of the WD for different parameters. For the purpose of visualization, a constant offset was applied to the relative distance such that the initial separation is normalized to zero. The light gray dashed line denotes the coincidence of the NS and WD centers of mass, while the black dashed line indicates the condition where the separation between the two centers of mass exceeds the sum of their radii, corresponding to the NS emerging from the WD.
Paper: Active Galactic Nucleus-driven Biconical Outflows as the Origin of the Double-peaked [O III] Doublet in SDSS J134733.36+121724.27
Authors: PeiZhen Cheng, XingQian Chen, GuiLin Liao, Qi Zheng, Ying Gu, MuLin Chen, XueGuang Zhang
Figure caption: The best descriptions of the host galaxy contributions in the SDSS spectrum of SDSS J1347+1217. In the top panel, in order to show clearer absorption features, the y-axis is plotted in logarithmic coordinates. The solid dark green line shows the SDSS spectrum, the solid blue line shows the SSP method-determined host galaxy contributions, the dashed blue line shows the determined AGN continuum emissions, and the solid red line shows the sum of the host galaxy contributions and the AGN continuum emissions. In the bottom panel, the line spectrum is shown as the SDSS spectrum minus the host galaxy contributions and the AGN continuum emissions.
Paper: Active Galactic Nucleus-driven Biconical Outflows as the Origin of the Double-peaked [O III] Doublet in SDSS J134733.36+121724.27
Authors: PeiZhen Cheng, XingQian Chen, GuiLin Liao, Qi Zheng, Ying Gu, MuLin Chen, XueGuang Zhang
Figure caption: The best-fitting results and the corresponding residuals to the emission lines around [O II] (panels (a) and (b)) and around Hγ (panels (c) and (d)). In panels (a) and (c), the solid dark green lines show the line spectrum, and the solid red lines show the best-fitting results. In panel (a), the solid and dashed purple lines show the determined core and extended components in [O II]λ3727 Å. The solid and dashed cyan lines show the determined core and extended components in Hϵ. The solid blue and red lines show the determined blueshifted and redshifted components in [Ne III]. The dashed green line shows the determined extended component in [Ne III]. In panel (c), the solid and dashed green lines show the determined core and extended components in Hγ. The solid and dashed purple lines show the determined core and extended components in narrow Hδ. The solid blue and red lines show the determined blueshifted and redshifted emission profiles in [O III]λ4363 Å. The solid and dashed cyan lines show the determined core and extended components in [S II]λ4070 Å. In panels (b) and (d), the corresponding residuals are shown, with the horizontal red lines showing residuals = 0, ±1.
Paper: Active Galactic Nucleus-driven Biconical Outflows as the Origin of the Double-peaked [O III] Doublet in SDSS J134733.36+121724.27
Authors: PeiZhen Cheng, XingQian Chen, GuiLin Liao, Qi Zheng, Ying Gu, MuLin Chen, XueGuang Zhang
Figure caption: The best-fitting results and the corresponding residuals to Hα and [N II] emission lines for Model_a (panels (a) and (b)), Model_c (panels (c) and (d)), and Model_d (panels (e) with the y-axis shown on a logarithmic scale and (f)). All line styles have the same meanings as those in panels (a) and (b) in Figure 2.
Paper: The Head-on Collision of a Neutron Star with a White Dwarf
Authors: Zong-kai Peng, He Gao, Xian-Fei Zhang
Figure caption: Taking the collision between the NS and WD as the initial moment, we measure the maximum separation between them during their relative motion over the subsequent 10 s. The red line indicates that the NS was just able to pierce through the WD.
Paper: Testing the Nature of GW200105 by Probing the Frequency Evolution of Eccentricity
Authors: Avinash Tiwari, Sajad A. Bhat, Md Arif Shaikh, Shasvath J. Kapadia
Figure caption: Same as Figure 1, but for a GW200105-like injection. Left: violins of eccentricity deviation δe at different reference frequencies. The horizontal line at δe = 0 represents zero deviation from GR. Right: individual eobs (right side) and eGR (left side) posteriors at different reference frequencies for the same. In both panels, the dashed and the dotted lines represent the 90% and 68% credible intervals, respectively. The vertical dashed–dotted gray lines between 30 and 35 Hz indicate the onset of eobs posteriors (35 and 40 Hz ones) that fail the zero-exclusion criterion described in Section 2.
Paper: Testing the Nature of GW200105 by Probing the Frequency Evolution of Eccentricity
Authors: Avinash Tiwari, Sajad A. Bhat, Md Arif Shaikh, Shasvath J. Kapadia
Figure caption: Left: violins of the eccentricity deviation δe at different reference frequencies. The horizontal line at δe = 0 represents zero deviation from GR. Right: individual eobs (right side) and eGR (left side) posteriors at different reference frequencies for the same. In both panels, the dashed and the dotted lines represent the 90% and 68% credible intervals, respectively.
Paper: Testing the Nature of GW200105 by Probing the Frequency Evolution of Eccentricity
Authors: Avinash Tiwari, Sajad A. Bhat, Md Arif Shaikh, Shasvath J. Kapadia
Figure caption: Detector-frame chirp mass posteriors recovered at different reference frequencies.
Paper: Testing the Nature of GW200105 by Probing the Frequency Evolution of Eccentricity
Authors: Avinash Tiwari, Sajad A. Bhat, Md Arif Shaikh, Shasvath J. Kapadia
Figure caption: Corner plot of posteriors recovered at 18 Hz (blue) and 25 Hz (maroon) for GW200105.
Paper: The Photometric Analysis of the Environment Around Two Dusty Star-forming Galaxies at z ∼ 2
Authors: Joe Bhangal, Allison W. S. Man, Tom J. L. C. Bakx, Darko Donevski, Pierre Cox, Helmut Dannerbauer, Stephen Serjeant, Masato Hagimoto, Pluto Jiang, Wenxiao Liu
Figure caption: A subset of the SPOTLESS sample of Herschel DSFGs with available line FWHM measurements from the literature. Redshifts are determined via targeted, mostly interferometric, submillimeter CO line observations. The y-axis shows the FWHM of the line, serving as a proxy for the galaxy’s internal kinematics. Red markers indicate galaxies at 2.1 ≲ z ≲ 2.3, where prominent spectral features fall within the K-band for MOS follow-up. Green and yellow markers highlight the two DSFGs studied in this paper: SDP.17b and HELMS-55, respectively. Blue markers denote the rest of the SPOTLESS sample. This plot is zoomed in to redshifts 1.5 ≲ z ≲ 4 and FWHM ≤ 1450 km s−1 to highlight the bulk population of the sample.
Paper: The Photometric Analysis of the Environment Around Two Dusty Star-forming Galaxies at z ∼ 2
Authors: Joe Bhangal, Allison W. S. Man, Tom J. L. C. Bakx, Darko Donevski, Pierre Cox, Helmut Dannerbauer, Stephen Serjeant, Masato Hagimoto, Pluto Jiang, Wenxiao Liu
Figure caption: The CIGALE fit values for instantaneous SFR [M⊙ yr−1] and total stellar mass [M⊙] of the maximum-likelihood companion galaxies (no magnitude cut applied) within dz = 0.2 of the central DSFG zspec, and the respective 1σ error bars. The main sequence at z = 2.3 from C. Schreiber et al. (2015) is shown in black, with shaded regions indicating  ±0.3, 0.6, and 0.9 dex scatter in increasing transparency. We define quiescent galaxies as sources that fall below or are consistent with the red dotted line (sSFR < 10−11 yr−1). The published SFR and M⋆ values of SDP.17b and HELMS-55 are also shown. For HELMS-55, we show a range of assumed magnification factors (μ = 1 and μ = 4) to account for the currently unconstrained lensing correction. For comparison, we plot published SFR and M⋆ values of known protoclusters from the literature: the Spiderweb protocluster (J. M. Pérez-Martínez et al. 2024; z = 2.16), PHz G237.01+42.50 (M. Polletta et al. 2021; z = 2.16), and PLCK G073.4-57.5 (R. Hill et al. 2025; z = 2.3). Additionally, we plot field galaxies from the COSMOS survey (J. R. Weaver et al. 2022) within dz = 0.2 of z = 2.3 as hexagonal density bins, where the darker blue indicates higher source density.
Paper: The Photometric Analysis of the Environment Around Two Dusty Star-forming Galaxies at z ∼ 2
Authors: Joe Bhangal, Allison W. S. Man, Tom J. L. C. Bakx, Darko Donevski, Pierre Cox, Helmut Dannerbauer, Stephen Serjeant, Masato Hagimoto, Pluto Jiang, Wenxiao Liu
Figure caption: Summary of the photometric data for each target environment, including companion galaxies associated with the central DSFGs. Gemini South F2 Ks-band footprints are shown as RGB images: Ks (red), i (green), and g (blue). Gaps in the F2 circular FOV arise from masking the on-Instrument wave front sensor probe shadows during observations. The HSC optical grizy footprint (grayscale) extends beyond the F2 coverage, and HST F110W/F160W footprints are shown as white ﹩\sim 2\mathop{.}\limits^{{\rm{^{\prime} }}}05\times 2\mathop{.}\limits^{{\rm{^{\prime} }}}27﹩ rectangles. Companion galaxies are marked with cyan circles, while the central DSFG is highlighted in green for SDP.17b and yellow for HELMS-55. Example companion galaxies are displayed in 5″ × 5″ RGB cutouts, with their object ID indicated. Central DSFGs are shown in larger 10″ × 10″ cutouts. SDP.17a is circled in magenta in SDP.17b’s cutout.
Paper: The Photometric Analysis of the Environment Around Two Dusty Star-forming Galaxies at z ∼ 2
Authors: Joe Bhangal, Allison W. S. Man, Tom J. L. C. Bakx, Darko Donevski, Pierre Cox, Helmut Dannerbauer, Stephen Serjeant, Masato Hagimoto, Pluto Jiang, Wenxiao Liu
Figure caption: Overdensity significances as a function of redshift for galaxy cluster and protocluster candidates photometrically identified in the literature. The overdensity significances of the SDP.17b and HELMS-55 environments are plotted in comparison as green and yellow triangles, respectively. Symbols represent different studies: gray circles for G. Castignani et al. (2014a), light blue squares for G. Castignani et al. (2014b), blue plus signs for G. Castignani et al. (2019), and purple diamonds for R. Calvi et al. (2023). However, these papers do not report error bars on their overdensity significance. Spectroscopically confirmed protoclusters are marked with magenta crosses. The median value of the overdensity significance, assuming the number of companion galaxies in a given realization is equal to the number of field galaxies drawn from the COSMOS control sample (Ntarget,i = NCOSMOS,i), is shown as gray and black crosses at the Ks-band magnitude cuts of the SDP.17b and HELMS-55 environments, respectively.
Paper: The Photometric Analysis of the Environment Around Two Dusty Star-forming Galaxies at z ∼ 2
Authors: Joe Bhangal, Allison W. S. Man, Tom J. L. C. Bakx, Darko Donevski, Pierre Cox, Helmut Dannerbauer, Stephen Serjeant, Masato Hagimoto, Pluto Jiang, Wenxiao Liu
Figure caption: Example EAZY-PY SED fits of the maximum-likelihood companion galaxies. The left and right panels correspond to a companion galaxy from the SDP.17b and HELMS-55 target environments, respectively. Each panel shows the SED plot on the left and the probability distribution function of the photometric redshift, p(z), with respect to the redshift on the right. The zspec value of the central DSFG is shown in red in the p(z) plots, and the maximum-likelihood zphot estimate, zml, is used to compute the best-fit SEDs, which are plotted in blue, with the 1σ error shaded around them. Template fluxes are shown as blue circles, while observed fluxes and their error bars are shown in black (SNR > 0) and gray (SNR  ≤ 0). Open markers at the bottom of the SED panels mark bands without flux measurements (e.g., HST F110W and F160W). For each source, cutouts measuring 10″ by 10″ are shown in the available filters, with 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 in diameter apertures overlaid, and filter names shown in yellow (e.g., grizy, Ks).
Paper: The Photometric Analysis of the Environment Around Two Dusty Star-forming Galaxies at z ∼ 2
Authors: Joe Bhangal, Allison W. S. Man, Tom J. L. C. Bakx, Darko Donevski, Pierre Cox, Helmut Dannerbauer, Stephen Serjeant, Masato Hagimoto, Pluto Jiang, Wenxiao Liu
Figure caption: Molecular gas masses (﹩{M}_{{{\rm{H}}}_{2}}﹩) of our target DSFGs compared with the R. Calvi et al. (2023) DSFGs, assuming ﹩{\alpha }_{\,\rm{CO}\,}=4.0\,{M}_{\odot }\,{({\rm{K}}\,\mathrm{km}\,{{\rm{s}}}^{-1}\,{\mathrm{pc}}^{2})}^{-1}﹩. SDP.17b is shown in green and HELMS-55 in yellow. For HELMS-55, we show estimates assuming different lensing magnifications (μ = 4 and μ = 10) since no lensing model currently exists in the literature. The shaded blue region marks the threshold below which overdensity significances are considered protocluster candidates. For the R. Calvi et al. (2023) DSFGs, average overdensity significances were adopted; their colors correspond to their spectroscopic redshifts as indicated by the color bar, and marker shapes distinguish the individual DSFGs listed in the figure, where DSFGs near each other were grouped.
Paper: A NICER View of the 1.4 M⊙ Edge-on Pulsar PSR J0614-3329
Authors: Lucien Mauviard, Sebastien Guillot, Tuomo Salmi, Devarshi Choudhury, Bas Dorsman, Denis González-Caniulef, Mariska Hoogkamer, Daniela Huppenkothen, Christine Kazantsev, Yves Kini, Jean-Francois Olive, Pierre Stammler, Anna L. Watts, Melissa Mendes, Nathan Rutherford, Achim Schwenk, Isak Svensson, Slavko Bogdanov, Matthew Kerr, Paul S. Ray, Lucas Guillemot, Ismaël Cognard, Gilles Theureau
Figure caption: Reduced and phase-folded NICER event data for PSR J0614−3329 duplicated over two rotational cycles for visualization purpose. The top panel displays the 0.3–2.0 keV bolometric pulse profile with its associated Poisson uncertainty. The bottom panel shows the energy resolved pulse profile. Phases are separated into 32 regular sized bins and energy by registered PI channel, as used for the inference. Energy resolved pulse profiles in previous publications had their number of counts per bin divided by the number of cycles shown, which is not the case here.
Paper: The Photometric Analysis of the Environment Around Two Dusty Star-forming Galaxies at z ∼ 2
Authors: Joe Bhangal, Allison W. S. Man, Tom J. L. C. Bakx, Darko Donevski, Pierre Cox, Helmut Dannerbauer, Stephen Serjeant, Masato Hagimoto, Pluto Jiang, Wenxiao Liu
Figure caption: The description is the same as Figure 3, except the sources are SDP.17b’s maximum-likelihood companion galaxies. SDP.17b’s zspec is shown in red.
Paper: The Photometric Analysis of the Environment Around Two Dusty Star-forming Galaxies at z ∼ 2
Authors: Joe Bhangal, Allison W. S. Man, Tom J. L. C. Bakx, Darko Donevski, Pierre Cox, Helmut Dannerbauer, Stephen Serjeant, Masato Hagimoto, Pluto Jiang, Wenxiao Liu
Figure caption: The description is the same as Figure 7, except the sources are HELMS-55 maximum-likelihood companion galaxies. HELMS-55’s zspec is shown in red.