adsabs/AstroCLIMB huggingface dataset:
Paper: The Luminosity Function of Tidal Disruption Flares for the ZTF-I Survey
Authors: Zheyu Lin, Ning Jiang, Xu Kong, Shifeng Huang, Zesen Lin, Jiazheng Zhu, Yibo Wang
Figure caption: The TDF LF based on 33 ZTF-I TDFs. The volumetric rates for r-band limiting magnitudes r = 19.5, 20.0, and 20.5 are shown in blue, orange, and green, respectively. The solid and dotted lines represent the fitting results to a power-law profile and a Schechter function, respectively. The error for volumetric rate in each bin is estimated based on bootstrapping. Left: LF for rest-frame g-band peak luminosity L  g . The sources are binned into eight bins separated by equivalent log L  g . The number of sources in these eight bins is {2, 0, 4, 6, 8, 8, 0, 5}. Right: LF for blackbody luminosity L bb. The sources are binned into seven bins separated by equivalent log L bb. The number of sources in these seven bins is {5, 7, 9, 6, 1, 2, 3}.
Paper: The Luminosity Function of Tidal Disruption Flares for the ZTF-I Survey
Authors: Zheyu Lin, Ning Jiang, Xu Kong, Shifeng Huang, Zesen Lin, Jiazheng Zhu, Yibo Wang
Figure caption: Light curves around the peak for ZTF-I TDFs.
Paper: JWST Sneaks a Peek at the Stellar Morphology of z ∼ 2 Submillimeter Galaxies: Bulge Formation at Cosmic Noon
Authors: Chian-Chou Chen, 建州 陳, Zhen-Kai Gao, Qi-Ning Hsu, Cheng-Lin Liao, Yu-Han Ling, Ching-Min Lo, Ian Smail, Wei-Hao Wang, Yu-Jan Wang
Figure caption: Left: stellar mass–SFR main sequence at z = 2 based on Speagle et al. (2014). Dashed lines show the range of ±0.3 dex scatter. The locations of the sample SMGs are marked as black data points. Our sample SMGs lie on the main sequence at z ∼ 2. Right: thumbnail images of our sample SMGs with their IDs shown at the top left corner and their redshifts at bottom right, where photometric redshifts are shown to two decimal points and three decimal points for spectroscopic redshifts. The RGB images with 40 kpc on a side are made with NIRCam F115W, F277W, and F444W filters, except for 850.019 where the blue image is made with the F150W filter. The images are made with a linear stretch between 1% and 99.9%. The dotted contours show the VLA 1.4 GHz emissions with [3, 4, 5, 6] × σ levels, the dashed contours show the MIPS 24 μm emissions with [10, 13, 16, 19] × σ levels, and finally the smaller solid contours show the ALMA 870 μm continuum emissions with [5, 10, 15, 20] × σ levels. The JWST counterparts of the sample SMGs are robustly identified by VLA, MIPS, or ALMA.
Paper: JWST Sneaks a Peek at the Stellar Morphology of z ∼ 2 Submillimeter Galaxies: Bulge Formation at Cosmic Noon
Authors: Chian-Chou Chen, 建州 陳, Zhen-Kai Gao, Qi-Ning Hsu, Cheng-Lin Liao, Yu-Han Ling, Ching-Min Lo, Ian Smail, Wei-Hao Wang, Yu-Jan Wang
Figure caption: Half-light radii in observed wavelengths of our sample SMGs are shown in gray points, where measurements of the same source are connected by lines and those from AS2UDS.125.0 are explicitly marked in red. The median values of each wave band are shown in larger black points with bootstrapped uncertainties. Empty circles show size measurements of our sample SMGs based on the published HST results in the J and H bands (van der Wel et al. 2014), empty squares show H-band sizes of SMGs reported by Chen et al. (2015), and empty diamonds show sizes measured by Lang et al. (2019), where the 870 μm sizes and stellar mass sizes are also shown. At the top we show cutout images with 4″ on a side from HST, Spitzer, and JWST of one of our sample SMGs confirmed by ALMA, AS2UDS.125.0, and these cutouts are aligned vertically roughly to the wavelengths shown in the x-axis below.
Paper: JWST Sneaks a Peek at the Stellar Morphology of z ∼ 2 Submillimeter Galaxies: Bulge Formation at Cosmic Noon
Authors: Chian-Chou Chen, 建州 陳, Zhen-Kai Gao, Qi-Ning Hsu, Cheng-Lin Liao, Yu-Han Ling, Ching-Min Lo, Ian Smail, Wei-Hao Wang, Yu-Jan Wang
Figure caption: Top panels show the NIRCam science images with 5″ on a side centered at the ALMA confirmed SMG AS2UDS.125.0, where the white ellipses mark the source masks within which GALFIT modeling is performed. Middle and bottom panels show the model and residual maps produced by GALFIT. Example results of the three filters, F115W, F200W, and F444W, are shown in each column. We find at least two components, a bulge and a disk, are required to produce adequate fitting results in almost all filters of our sample SMGs, especially for F444W in which all sources need two components (Figure A1), suggesting stellar bulges are often present in SMGs.
Paper: JWST Sneaks a Peek at the Stellar Morphology of z ∼ 2 Submillimeter Galaxies: Bulge Formation at Cosmic Noon
Authors: Chian-Chou Chen, 建州 陳, Zhen-Kai Gao, Qi-Ning Hsu, Cheng-Lin Liao, Yu-Han Ling, Ching-Min Lo, Ian Smail, Wei-Hao Wang, Yu-Jan Wang
Figure caption: Similar to Figure 2, but here we show the GALFIT results only in the F444W filter but on all sample SMGs.
Paper: JWST Sneaks a Peek at the Stellar Morphology of z ∼ 2 Submillimeter Galaxies: Bulge Formation at Cosmic Noon
Authors: Chian-Chou Chen, 建州 陳, Zhen-Kai Gao, Qi-Ning Hsu, Cheng-Lin Liao, Yu-Han Ling, Ching-Min Lo, Ian Smail, Wei-Hao Wang, Yu-Jan Wang
Figure caption: Cumulative fractions of integrated flux densities measured from NIRCam on all seven sample SMGs as well as those from ALMA band 7 on AS2UDS.0125.0. Vertical lines with corresponding colors mark the half-light radii in the major axis, and the dotted lines show the results of PSFs at F444W. In all cases, half-light radii are smaller at longer wavelengths. It is also evident that bulges, despite presenting in many sources, do not dominate the total flux densities.
Paper: VLBA Reveals the Absence of a Compact Radio Core in the Radio-intermediate Quasar J2242+0334 at z = 5.9
Authors: Yuanqi Liu, Ran Wang, Emmanuel Momjian, Yingkang Zhang, Tao An, Xiaolong Yang, Jeff Wagg, Eduardo Bañados, Alain Omont
Figure caption: Left panel: the intensity map of VLA observations at 1.4 GHz. The contour levels are at [−1, 2, 4, 6] times the corresponding 1σ rms noise level of 24.7 μJy beam−1. The synthesized beam with an FWHM of 1.″4 × 1.″2 is shown as an ellipse in the bottom left corner. Right panel: full-resolution VLBA image in 1″ × 1″ area, zooming into the central area in the VLA image. A synthesized beam with an FWHM of 10.7 mas × 4.5 mas is shown as the ellipse in the bottom left black square box. For both panels, the black plus denotes the optical position and the white cross represents the peak position in VLA 3 GHz observations (Liu et al. 2021), which is also the phase center of the VLBA observations.
Paper: Dust Temperature Uncertainties Hamper the Inference of Dust and Molecular Gas Masses from the Dust Continuum Emission of Quiescent High-redshift Galaxies
Authors: R. K. Cochrane, C. C. Hayward, D. Anglés-Alcázar
Figure caption: The impact of quenching star formation on a galaxy’s observed-frame SED. Upper panels: dark blue lines show the SED generated for a simulated star-forming galaxy at z = 2.0 (left) and z = 4.0 (right). Other lines show the impact of a controlled “quenching” event: the pale blue lines show the SED generated if the galaxy had no stars formed within 100 Myr of z = 2.0 (or z = 4.0); the pale and dark red lines show the same for no stars formed within the prior 500 Myr and 1 Gyr, respectively. We overlay (appropriately redshifted) data from stacked samples of observed color-selected massive quiescent galaxies at z ∼ 0.3–1.4 (Magdis et al. 2021) on the panel that shows the SED for the lower-redshift snapshot. The data are in qualitative agreement with our predicted SEDs. Lower panels show the ratio of emission at different wavelengths, relative to the fiducial case of the star-forming source. Dashed navy lines mark an observed-frame wavelength of 1.3 mm. For the quenched galaxies, the radiation field is softer due to the absence of young massive stars and the dust temperature is lower. At z = 2.0, 1.3 mm in the observed frame is near the R–J regime, where the flux depends linearly on dust temperature. Hence, the difference in dust temperature between star-forming and quenched sources does not result in a substantial reduction in observed 1.3 mm flux density. At z = 4, 1.3 mm probes a shorter rest-frame wavelength (260 μm), and modest temperature differences are amplified because of the superlinear dependence of flux density on dust temperature.
Paper: Dust Temperature Uncertainties Hamper the Inference of Dust and Molecular Gas Masses from the Dust Continuum Emission of Quiescent High-redshift Galaxies
Authors: R. K. Cochrane, C. C. Hayward, D. Anglés-Alcázar
Figure caption: Upper: the M dust-to-S 1.3mm ratio (MSR) derived from our radiative transfer calculations, with predictions for the ratio at different dust temperatures overlaid (see Equation (2)). Middle: the predicted MSR for different quenching scenarios, divided by that calculated for the fiducial star-forming source, for each galaxy at a given redshift. Lower: the calculated MSR divided by the canonical ratio (Equation (2)), assuming a dust temperature of 25 K. For our fiducial sample of star-forming galaxies (dark blue), the true dust mass per unit flux density tends to be slightly lower than predicted, since the mass-weighted dust temperature is actually higher than 25 K. For the quenched galaxies, the true scaling between dust mass and 1.3mm flux density is higher than the canonical ratio by factors of a few. This effect is more pronounced at higher redshifts and can lead to an underestimation of dust (and gas) masses from continuum flux density measurements for galaxies with little or no recent star formation by as much as an order of magnitude.
Paper: Dust Temperature Uncertainties Hamper the Inference of Dust and Molecular Gas Masses from the Dust Continuum Emission of Quiescent High-redshift Galaxies
Authors: R. K. Cochrane, C. C. Hayward, D. Anglés-Alcázar
Figure caption: Mass-weighted dust temperature vs. the ratio of two rest-frame flux densities. Colors and symbols are the same as used and defined in Figure 2. The tight correlations show that measurements of two flux densities, or one measurement and an upper limit, can put constraints on the dust temperature, thereby enabling more accurate inference of the dust (and thus the gas) mass. We overplot the best-fitting relations derived for each wavelength combination (black dashed line; see Equation (5)). The shaded region shows the 1σ scatter between the true mass-weighted temperature and the best-fitting relation.
Paper: On the Sound Speed in Neutron Stars
Authors: Sinan Altiparmak, Christian Ecker, Luciano Rezzolla
Figure caption: PDF of the sound speed squared as function of the energy density. The purple region marks the 95% interval of maximum central energy densities, so that the vertical purple line represents an estimate for the largest possible energy density in a neutron star. The orange contour marks the region containing EOSs with ﹩{c}_{s}^{2}\lt 1/3﹩.
Paper: On the Sound Speed in Neutron Stars
Authors: Sinan Altiparmak, Christian Ecker, Luciano Rezzolla
Figure caption: Top: PDF of the mass–radius relation. The orange contour encloses EOSs with subconformal sound speed (see Figure 1). The dashed black line reports the lower bound for the radii as computed from considerations on the threshold mass (Koeppel et al. 2019). Bottom: PDF cuts for stars with mass M = 1.4 M ⊙ and M = 2 M ⊙; the dashed vertical lines mark the median of the distributions.
Paper: On the Sound Speed in Neutron Stars
Authors: Sinan Altiparmak, Christian Ecker, Luciano Rezzolla
Figure caption: Representative examples referring to a generic EOS (red solid line), a subconformal EOS (blue solid line), and monotonic sound speed inside neutron stars (green solid line). The left plot shows the sound speed as function of the energy density, with the kinks in the curves marking the matching points of the various segment used to construct the EOSs. The middle panel shows the corresponding EOSs, together with the BPS EOS (Baym et al. 1971; cyan solid line) that we use at low densities. The blue and green bands are the uncertainties from nuclear theory (Hebeler et al. 2013) and perturbative QCD (Fraga et al. 2014), respectively. Shown in gray is the outer envelope of all constraint-satisfying EOSs. The right panel reports the corresponding mass–radius curves, together with the outer envelope and various observational constraints.
Paper: On the Sound Speed in Neutron Stars
Authors: Sinan Altiparmak, Christian Ecker, Luciano Rezzolla
Figure caption: PDF of the pressure as function of the energy density. The blue and green regions mark the uncertainties in pressure in nuclear theory (Hebeler et al. 2013) and perturbative QCD (Fraga et al. 2014), respectively. The gray contour encloses all EOSs satisfying the astronomical constraints, while the purple regions and the orange contour are the same as in Figure 1.
Paper: On the Sound Speed in Neutron Stars
Authors: Sinan Altiparmak, Christian Ecker, Luciano Rezzolla
Figure caption: Top: PDF of the chirp mass as a function of the binary tidal deformability. Shown as black dashed lines are analytic fits for the minimum and maximum values of ﹩\tilde{{\rm{\Lambda }}}﹩ for a given chirp mass. Bottom: PDF cut for a binary with the same chirp mass as in GW170817, ﹩{{ \mathcal M }}_{\mathrm{chirp}}=1.186\,{M}_{\odot };﹩ the red dashed vertical line marks the median.
Paper: On the Sound Speed in Neutron Stars
Authors: Sinan Altiparmak, Christian Ecker, Luciano Rezzolla
Figure caption: Schematic representation of the various sets into which our total sample of EOSs can be decomposed, either when subject to the observational constraints (dark blue) or when not (light blue). The ratio between the two samples is shown with a stellar marker, while the hatched color coding reflects that used in Figure 1 and in the Appendix.
Paper: Investigating the [C II]-to-H I Conversion Factor and the H I Gas Budget of Galaxies at z ≈ 6 with Hydrodynamic Simulations
Authors: David Vizgan, Kasper E. Heintz, Thomas R. Greve, Desika Narayanan, Romeel Davé, Karen P. Olsen, Gergö Popping, Darach Watson
Figure caption: The evolution of the H I gas mass excess with stellar mass. Our simulations are color coded by star formation rate, and the y-axis is scaled logarithmically. The green stars represent galaxies from the ALPINE survey (Dessauges-Zavadsky et al. 2020). For the ALPINE data, we derive gas-phase metallicities from their M ⋆ and SFRs using the mass–metallicity relation in Curti et al. (2020). From there, we use Equation (2) to derive estimates of their H I gas mass content.
Paper: Cross-loop Propagation of a Quasiperiodic Extreme-ultraviolet Wave Train Triggered by Successive Stretching of Magnetic Field Structures during a Solar Eruption
Authors: Zheng Sun, Hui Tian, P. F. Chen, Shuo Yao, Zhenyong Hou, Hechao Chen, Linjie Chen
Figure caption: Magnetic field structure in the flare region. Panel (a) shows the linear force-free field extrapolation result of AR 12887 at ∼05:30 UT. The blue and red lines represent the overlying large-scale coronal loops and the postflare loops, respectively. Panels (b) and (c) are schematic representations of the evolution of magnetic field structures. The plus and minus signs represent different magnetic polarities. The red thick lines between the positive and negative polarities correspond to the erupting filament. The dashed lines and semitransparent solid lines represent the positions after and before the perturbation, respectively. The cyan wavy lines in panels (b) and (c) indicate multiple wave fronts.
Paper: Cross-loop Propagation of a Quasiperiodic Extreme-ultraviolet Wave Train Triggered by Successive Stretching of Magnetic Field Structures during a Solar Eruption
Authors: Zheng Sun, Hui Tian, P. F. Chen, Shuo Yao, Zhenyong Hou, Hechao Chen, Linjie Chen
Figure caption: Time–distance diagrams of AIA 171 Å running-difference images for the slice A–B (a) and slice C–D (b) in Figure 1. The green and cyan dashed lines in (b) indicate the propagation of the multiple wave fronts and the envelope, respectively. Speeds of the propagating features are printed in the figure.
Paper: Cross-loop Propagation of a Quasiperiodic Extreme-ultraviolet Wave Train Triggered by Successive Stretching of Magnetic Field Structures during a Solar Eruption
Authors: Zheng Sun, Hui Tian, P. F. Chen, Shuo Yao, Zhenyong Hou, Hechao Chen, Linjie Chen
Figure caption: Variations of the intensities averaged over slice A–B in Figure 1(a). Normalized intensity variations (a) and normalized running difference of the intensity (b) in the 171, 193, and 211 Å channels (smoothed over 1 minute interval).
Paper: Optical–Radio Position Offsets Are Inversely Correlated with AGN Photometric Variability
Authors: Nathan J. Secrest
Figure caption: Gaia G BP–G RP color/spectral index α (S  ν  ∝ ν −α ) as a function of fractional variability. ICRF sources become progressively redder with increasing variability, reaching a plateau at F var ∼ 0.4, where they exhibit G BP–G RP color consistent with blazars (dotted line, showing the median color for all L  γ  = 1046−47 erg s−1 blazars, using the templates from Ghisellini et al. 2017). This sequence is consistent with the trend of α versus radio-loudness from Ivezić et al. (2002). Gaia magnitudes are in the Vega system.
Paper: Optical–Radio Position Offsets Are Inversely Correlated with AGN Photometric Variability
Authors: Nathan J. Secrest
Figure caption: Percentage of objects above the variability threshold identified as a Fermi blazar. The gray shaded region denotes the 90% confidence interval, determined using binomial statistics.
Paper: Investigating the [C II]-to-H I Conversion Factor and the H I Gas Budget of Galaxies at z ≈ 6 with Hydrodynamic Simulations
Authors: David Vizgan, Kasper E. Heintz, Thomas R. Greve, Desika Narayanan, Romeel Davé, Karen P. Olsen, Gergö Popping, Darach Watson
Figure caption: Top panel: histograms of scatter around the best-fit models for the C II-to-H I relation (this work, crimson) and for the C II–H2 relation (Vizgan et al. 2022, violet); the scatter around the former relation is tighter (0.39 dex) than for the C II–H2 relation (0.45 dex). Bottom figure: the C II luminosity vs. H I gas mass relation for our z ≃ 6 simulations. We find a very strong linear correlation between these two quantities, yielding a best-fit of ﹩\mathrm{log}{L}_{[{\rm{C}}\,{\rm\small{II}}]}=1.02\mathrm{log}{M}_{{\rm{H}}\,{\rm\small{I}}}-1.95﹩. The simulations are color coded by the star formation rate, further demonstrating a correlation between SFR and the log-linear C II–H I relation. When accounting only for the diffuse H I mass derived from CLOUDY, the relation changes to ﹩\mathrm{log}{L}_{[{\rm{C}}\,{\rm\small{II}}]}=0.84\mathrm{log}{M}_{{\rm{H}}\,{\rm\small{I}}}+0.55﹩ with a scatter of 0.22 dex.
Paper: Investigating the [C II]-to-H I Conversion Factor and the H I Gas Budget of Galaxies at z ≈ 6 with Hydrodynamic Simulations
Authors: David Vizgan, Kasper E. Heintz, Thomas R. Greve, Desika Narayanan, Romeel Davé, Karen P. Olsen, Gergö Popping, Darach Watson
Figure caption: The [C II]-to-H I conversion factor β [C II] vs. SFR-weighted metallicity. The blue dot is ﹩{\beta }_{[C\,{\rm\small{II}}]}={30}_{-7}^{+10}\,{M}_{\odot }/{L}_{\odot }﹩, the conversion factor at solar metallicities (Heintz et al. 2021). GRBs are taken from Selsing et al. (2019; see also Heintz et al. 2021), while the orange points are the galaxies from Cormier et al. (2015).
Paper: First AI for Deep Super-resolution Wide-field Imaging in Radio Astronomy: Unveiling Structure in ESO 137-006
Authors: A. Dabbech, M. Terris, A. Jackson, M. Ramatsoku, O. M. Smirnov, Y. Wiaux
Figure caption: ESO 137-006: CLEAN reconstructions (flip pages to visualize differences at a glance with uSARA in Figure 1 and AIRI in Figure 2). First and second rows: recovered convolved model images (Jy pixel−1, displayed in log10 scale) at the high and low bands (panels (a) and (d)), respectively, overlaid with zooms on the core (panels (b) and (e)), a region with compact sources from the imaged FoV (panels (c) and (c′)), and a zoom on ESO 137-007, a radio galaxy north of ESO 137-006 (panels (f) and (f′)). Third row: estimated spectral index map of ESO 137-006 (displayed in linear scale; panel (g)), overlaid with a zoom on its core (panel (h), same region as in panels (b), (b′), and (e)). First, regarding the central region, the first side lobe of the dirty beam is highlighted with a dashed circle. Unlike the uSARA and AIRI reconstructions, only one new filament, T2, has clearly emerged south of the core at the high band. The previously detected filament, T0, is recovered at both bands. The filamentary structure S is an example of what mostly likely is a calibration residual artifact, as it moves with the geometry of the dirty beam. Inspection of the zooms on the core from CLEAN model images (panels (c′) and (e′)) confirms these findings. Second, looking at the zooms on the compact sources, one can see that some faint sources are not recovered in the CLEAN model image (panel (c)). Instead, they are left in the residual and so only visible in the CLEAN restored image (panel (c′)). Finally, a close look at ESO 137-007 in the convolved model image (panel (f)) indicates that much of the filamentary structure is not captured and is only visible on the CLEAN restored image (panel (f′)).
Paper: First AI for Deep Super-resolution Wide-field Imaging in Radio Astronomy: Unveiling Structure in ESO 137-006
Authors: A. Dabbech, M. Terris, A. Jackson, M. Ramatsoku, O. M. Smirnov, Y. Wiaux
Figure caption: ESO 137-006: uSARA reconstructions (flip pages to visualize differences at a glance with AIRI in Figure 2 and CLEAN in Figure 3). First and second rows: recovered model images (Jy pixel−1, displayed in log10 scale) at the high and low bands (panels (a) and (d)), respectively, overlaid with zooms on the core of ESO 137-006 (panels (b) and (e)), a region with compact sources from the imaged FoV (panel (c)), and a zoom on ESO 137-007, a radio galaxy north of ESO 137-006 (panel (f)). Third row: spectral index map of ESO 137-006 (displayed in linear scale; panel (g)), overlaid with a zoom on its core (panel (h), same region as in panels (b) and (e)). Focusing on the central region (panels (b) and (e)), the first side lobe of the dirty beam is highlighted with a dashed circle. One can see three filaments emerging: T1 and T2, located north and south of the inner core, seen at both bands, and T3, located further south, recovered only at low band. A fourth filament, T0, detected previously, is also recovered. The filamentary structure S is an example of what mostly likely is a calibration residual artifact, as it moves with the geometry of the dirty beam. The spectral index values of the newly formed filaments (panel (h)) are inconclusive.
Paper: First AI for Deep Super-resolution Wide-field Imaging in Radio Astronomy: Unveiling Structure in ESO 137-006
Authors: A. Dabbech, M. Terris, A. Jackson, M. Ramatsoku, O. M. Smirnov, Y. Wiaux
Figure caption: ESO 137-006: AIRI reconstructions (flip pages to visualize differences at a glance with uSARA in Figure 1 and CLEAN in Figure 3). First and second rows: recovered model images (Jy pixel−1, displayed in log10 scale) at the high and low bands (panels (a) and (d)), respectively, overlaid with zooms on the core of ESO 137-006 (panels (b) and (e)), a region with compact sources from the imaged FoV (panel (c)), and a zoom on ESO 137-007, a radio galaxy north of ESO 137-006 (panel (f)). Third row: spectral index map of ESO 137-006 (displayed in linear scale; panel (g)), overlaid with a zoom on its core (panel (h), same region as in panels (b) and (e)). Focusing on the central region (panels (b) and (e)), the first side lobe of the dirty beam is highlighted with a dashed circle. Similarly to uSARA reconstructions, one can see three filaments emerging: T1 and T2, located north and south of the inner core, seen at both bands, and T3, located further south, recovered only at low band. A fourth filament, T0, detected previously, is also recovered. The filamentary structure S is an example of what mostly likely is a calibration residual artifact, as it moves with the geometry of the dirty beam. The spectral index values of the newly formed filaments (panel (h)) are inconclusive.