adsabs/AstroCLIMB huggingface dataset:
Paper: Probing Reflection from Aerosols with the Near-infrared Dayside Spectrum of WASP-80b
Authors: Bob Jacobs, Jean-Michel Désert, Peter Gao, Caroline V. Morley, Jacob Arcangeli, Saugata Barat, Mark S. Marley, Julianne I. Moses, Jonathan J. Fortney, Jacob L. Bean, Kevin B. Stevenson, Vatsal Panwar
Figure caption: Measured light curves of the WASP-80b secondary eclipse divided into three wavelength bins (columns) over five visits (rows) for the exponential-ramp method. In each cell, we show the normalized, telescope systematics-reduced data and split them into forward-scanned (dark), and reverse-scanned (light) data. We determined a unique eclipse depth for each bin and each visit. The fitted light curve is shown as a solid line and we denote the times of first, second, third, and fourth contact with vertical dashed lines. For each fit, we provide a residual histogram to the right of the light curve. We compare them to the expected photon noise (solid line). The residuals satisfy a Shapiro–Wilks test at the α = 0.1 level and they can thus be considered Gaussian. In Figure B2 we display the equivalent of this figure for the RECTE method. Note that for the exponential-ramp method, the first exposure of each orbit has been removed, whereas this exposure is kept for the RECTE method.
Paper: Probing Reflection from Aerosols with the Near-infrared Dayside Spectrum of WASP-80b
Authors: Bob Jacobs, Jean-Michel Désert, Peter Gao, Caroline V. Morley, Jacob Arcangeli, Saugata Barat, Mark S. Marley, Julianne I. Moses, Jonathan J. Fortney, Jacob L. Bean, Kevin B. Stevenson, Vatsal Panwar
Figure caption: Near-infrared secondary eclipse depth measurements of WASP-80b for the exponential-ramp method (blue) and the RECTE method (maroon). The right axis shows the geometric albedo if there were zero thermal emission. Left: near-infrared secondary eclipse spectrum. The transparent data points in the background denote the per-visit eclipse depths and the opaque data points in the foreground are the weighted averages thereof. The data are offset slightly in wavelength for visibility purposes. Right: posterior distributions of the “white light” eclipse depth for each visit. The median and 1σ levels of the posteriors are marked with a darker shade. The two methods agree within 1σ, except for the fifth visit, for which the methods differ by 1.2σ. However, the eclipse depths measured with the exponential-ramp method are larger for all but one visit. The mean white light eclipse depth is 34 ± 10 ppm for the exponential-ramp method and 22 ± 9 ppm for the RECTE method.
Paper: Probing Reflection from Aerosols with the Near-infrared Dayside Spectrum of WASP-80b
Authors: Bob Jacobs, Jean-Michel Désert, Peter Gao, Caroline V. Morley, Jacob Arcangeli, Saugata Barat, Mark S. Marley, Julianne I. Moses, Jonathan J. Fortney, Jacob L. Bean, Kevin B. Stevenson, Vatsal Panwar
Figure caption: Posterior distributions from MCMC fits to the dayside spectrum (orange) and the transmission spectrum (green). For each model, the x-axis shows the metallicity distribution. For the cloudy model, we plot the sedimentation efficiency f sed on the y-axis, and for the haze models, we plot the logarithm of the haze formation rate η (in g cm−2s−1) on the y-axis. The three isodensity lines denote the 1σ, 2σ, and 3σ limits of the posteriors. An extra monochromatic offset parameter was used to fit transmission spectra. Correlations with that parameter are not displayed here. None of the posterior samples here have ﹩{\chi }_{\nu }^{2}\lt 1.6﹩ for both spectra simultaneously.
Paper: Probing Reflection from Aerosols with the Near-infrared Dayside Spectrum of WASP-80b
Authors: Bob Jacobs, Jean-Michel Désert, Peter Gao, Caroline V. Morley, Jacob Arcangeli, Saugata Barat, Mark S. Marley, Julianne I. Moses, Jonathan J. Fortney, Jacob L. Bean, Kevin B. Stevenson, Vatsal Panwar
Figure caption: Temperature–pressure (TP) profiles for a selection of atmospheric models (described in Section 3.1) for a soot haze (left), tholin haze (middle), and clouds (right). These TP profiles are used to generate the spectra in Figure 2. Solid lines denote [M/H] = 0, dashed lines show [M/H] = 0.5 models, and dotted lines denote [M/H] = 1. As a reference, each panel also shows in green the TP profiles of the clear atmosphere models generated with the EGP radiative-convective-thermochemical equilibrium code (Morley et al. 2012).
Paper: Probing Reflection from Aerosols with the Near-infrared Dayside Spectrum of WASP-80b
Authors: Bob Jacobs, Jean-Michel Désert, Peter Gao, Caroline V. Morley, Jacob Arcangeli, Saugata Barat, Mark S. Marley, Julianne I. Moses, Jonathan J. Fortney, Jacob L. Bean, Kevin B. Stevenson, Vatsal Panwar
Figure caption: Best-fit models to the WASP-80b dayside (upper panel) and transmission (lower panel) spectra. Solid lines denote models fit to the dayside spectrum data. Spectra denoted with dashed lines were fit to the transmission spectrum data. All data, except for the WFC3 dayside data in blue, are adopted from Wong et al. (2022). All data in the left panels were taken with WFC3 and the data in the right panels were taken with Spitzer. We color the clear atmosphere model green, the soot haze model pink, the tholin haze model blue, and the cloudy model yellow. Diamonds denote the band-integrated eclipse/transit depths of the model fits to the dayside spectrum.
Paper: Jet Lorentz Factor Constraint for GRB 221009A Based on the Optical Depth of the TeV Photons
Authors: Duan-Yuan Gao, Yuan-Chuan Zou
Figure caption: The plot shows the optical depth for a photon with E T = 7 TeV as a function of t T when the Lorentz factor ΓT = 560. Different lines in different colors and line styles represent the optical depth as a function of t T for different methods. The black thick line represents the result obtained using the full formula, i.e., Equation (13). This is the most comprehensive and accurate calculation taking into account all relevant factors. The orange dashed line is obtained by neglecting changes in luminosity, power-law indices, and peak energy. In this method, we substitute the variables in Equation (7) with their time-averaged values, while using Equation (13) for other parts of the calculation. The green dashed–dotted line considers only changes in t T and neglects δ t R, i.e., δ t R = 0, instead of using the full expression from Equation (3). Other parts of the calculation use Equation (13). The purple dotted line omits the correction for the photon number density with the power-law index of the spectrum, i.e., ﹩{E}_{{\rm{P}}}^{* }={E}_{{\rm{P}}}﹩, instead of using the full expression from Equation (8). Other parts of the calculation use Equation (13). The red thin solid line is obtained using a simpler method, i.e., Equation (16).
Paper: PSR J1953+1844 Probably Being the Descendant of an Ultracompact X-Ray Binary
Authors: Z. L. Yang, J. L. Han, W. C. Jing, W. Q. Su
Figure caption: The probability distribution of the companion mass M c of M71E. Top panel: distribution of possible companion mass calculated for various inclination angle i and pulsar mass M psr. Here, ﹩\cos i﹩ should follow a uniform probability distribution if the orbital orientation is random in space. The probability density function (pdf) for the pulsar mass presented in the gray scale is taken from Özel & Freire (2016) for the recycled pulsars, following a Gaussian function centering at M 0 = 1.54 M ⊙ with a standard deviation of ±σ 0 = 0.23 M ⊙ as indicated by two dotted lines. Bottom panel: the pdf (in subpanel (a)) and the cumulative distribution function (CDF, in subpanel (b)) for the companion mass M  c  integrated from the pdf on the top panel, with a probability of ﹩\cos i﹩ uniformly distributed in the range of (0, 1). Two red dotted lines indicate the companion mass of 0.008 and 0.015 M ⊙ at the 16% and 84% probability (±1σ) of the CDF and the dashed line marked the 95% probability of the CDF at 0.026 M ⊙.
Paper: Jet Lorentz Factor Constraint for GRB 221009A Based on the Optical Depth of the TeV Photons
Authors: Duan-Yuan Gao, Yuan-Chuan Zou
Figure caption: Minimal Lorentz factor ﹩{{\rm{\Gamma }}}_{{\rm{T}},\min }﹩ with E T = 7 TeV as a function of t T. Different lines and line style correspond to different methods. The black thick solid line is obtained by the full formula. The orange dashed line is obtained when we neglect change of luminosity, power-law indexes, and peak energy. We obtain the green dashed–dotted line when we neglect t R and only consider change of t T. The red thin solid one is obtained by the simple method. The purple dotted line omits the correction for photon number density with the power-law index of spectrum; that is to say, ﹩{E}_{{\rm{P}}}^{* }={E}_{{\rm{P}}}﹩.
Paper: Jet Lorentz Factor Constraint for GRB 221009A Based on the Optical Depth of the TeV Photons
Authors: Duan-Yuan Gao, Yuan-Chuan Zou
Figure caption: A schematic diagram illustrates the geometry of the difference in retarded time between MeV photons and TeV photons. When TeV photons collide with MeV photons at point A. the MeV photons will not reach Earth as the direction is not pointing to the Earth, but we can determine their number density from the photons arriving at Earth with the same retarded time. The MeV photons move radially at R, while the TeV photons move along the x-axis at ﹩x=R\cos \theta ﹩ when they are colliding.
Paper: Detecting High-energy Neutrino Minibursts from Local Supernovae with Multiple Neutrino Observatories
Authors: Ali Kheirandish, Kohta Murase
Figure caption: Left: expected neutrino signal events from SNe II with CCSM in IceCube, assuming that the source resides in the Northern sky. Here, we showcase the expected number of neutrino events between 100 GeV and 10 PeV for three different values of D * and s cr = 2.0. Right: expected neutrino signal event from SN IIn in IceCube, assuming that the source resides in the Northern sky.
Paper: Detecting High-energy Neutrino Minibursts from Local Supernovae with Multiple Neutrino Observatories
Authors: Ali Kheirandish, Kohta Murase
Figure caption: Detection probability for high-energy neutrinos from CCSNe in IceCube and IceCube-Gen2, assuming the CR spectral index s cr = 2.2. Left: detection probability of at least a singlet (solid), doublet (dotted), and triplet (dashed) event from SNe II with CCSM as a function of distance for D * = 1. Right: same as the left panel for SNe IIn. The expected rate of each SNe type is also shown in blue.
Paper: Detecting High-energy Neutrino Minibursts from Local Supernovae with Multiple Neutrino Observatories
Authors: Ali Kheirandish, Kohta Murase
Figure caption: Left: prospects for the identification of SNe II with CCSM in IceCube-Gen2 at different distances. The shaded band shows the p-values for D * ranging from 0.01 to 1. Right: same as left but for SN IIn in IceCube (dashed) and IceCube-Gen2 (solid).
Paper: Detecting High-energy Neutrino Minibursts from Local Supernovae with Multiple Neutrino Observatories
Authors: Ali Kheirandish, Kohta Murase
Figure caption: Neutrino fluences for SN 2023ixf, identified in a relatively nearby galaxy M101. The solid (dashed) line shows the fluence for D * = 0.003 (0.1), where s cr = 2.0 is used.
Paper: Detecting High-energy Neutrino Minibursts from Local Supernovae with Multiple Neutrino Observatories
Authors: Ali Kheirandish, Kohta Murase
Figure caption: Projected p-values for the detection of neutrinos from SN IIn at a distance of 2 Mpc in IceCube (red), IceCube and KM3NeT (orange), and a combination of IceCube, KM3NeT, and GVD.
Paper: Dissonance in Harmony: The UV/Optical Periodic Outbursts of ASASSN-14ko Exhibit Repeated Bumps and Rebrightenings
Authors: Shifeng Huang, Ning Jiang, Rong-Feng Shen, Tinggui Wang, Zhenfeng Sheng
Figure caption: Evolution of UV/optical bands. Here, to reduce the impact of the large data error in the v band, we excluded this band and fitted the remaining data to derive the results. The top panel plots the evolution of host-subtracted UV/optical bolometric luminosity. The evolution of the blackbody temperature and radius are shown on the middle and bottom panels.
Paper: Dissonance in Harmony: The UV/Optical Periodic Outbursts of ASASSN-14ko Exhibit Repeated Bumps and Rebrightenings
Authors: Shifeng Huang, Ning Jiang, Rong-Feng Shen, Tinggui Wang, Zhenfeng Sheng
Figure caption: Multiwavelength light curves of ASASSN-14ko. In panel (a), the historical X-ray light curve, hardness ratio, and UV/optical light curves are shown. In panel (b), we plot the details of the multiwavelength light curves of the new observations. For comparison, the light curves of epochs 2 and 3 are also plotted. The early bumps and rebrightenings are marked by a color shadow region. The magnitudes are host-subtracted. The triangles represent the 3σ upper limit.
Paper: Dissonance in Harmony: The UV/Optical Periodic Outbursts of ASASSN-14ko Exhibit Repeated Bumps and Rebrightenings
Authors: Shifeng Huang, Ning Jiang, Rong-Feng Shen, Tinggui Wang, Zhenfeng Sheng
Figure caption: 0.3–2.0 keV X-ray spectra in different epochs of ASASSN-14ko. All three spectra are fitted with the absorb power-law model tbabs∗zashift∗powerlw.
Paper: Dissonance in Harmony: The UV/Optical Periodic Outbursts of ASASSN-14ko Exhibit Repeated Bumps and Rebrightenings
Authors: Shifeng Huang, Ning Jiang, Rong-Feng Shen, Tinggui Wang, Zhenfeng Sheng
Figure caption: SED fitting results of epochs 10 and 11. The time in the legend is relative to the UV peak. The X-ray data points at 2 keV are plotted, but are not included in the fitting.
Paper: Dissonance in Harmony: The UV/Optical Periodic Outbursts of ASASSN-14ko Exhibit Repeated Bumps and Rebrightenings
Authors: Shifeng Huang, Ning Jiang, Rong-Feng Shen, Tinggui Wang, Zhenfeng Sheng
Figure caption: The star is tidally stripped by the black hole, creating a debris stream that orbits around it. The stream crashes into the accretion disk twice in every cycle. These collisions produce flares in the UV/optical bands. The first flare occurs when the front stream hits the disk, creating an early bump in the light curves. The second flare occurs when the trailing stream collides with the disk, causing a rebrightening of the emission. The main outburst is powered by the accretion of the stripped material onto the black hole.
Paper: Dissonance in Harmony: The UV/Optical Periodic Outbursts of ASASSN-14ko Exhibit Repeated Bumps and Rebrightenings
Authors: Shifeng Huang, Ning Jiang, Rong-Feng Shen, Tinggui Wang, Zhenfeng Sheng
Figure caption: (a) The correlation between α ox and the luminosity of 2500 Å in different epochs. (b) The distribution of α ox at different epochs.
Paper: The Supersonic Project: Star Formation in Early Star Clusters without Dark Matter
Authors: William Lake, Smadar Naoz, Federico Marinacci, Blakesley Burkhart, Mark Vogelsberger, Claire E. Williams, Yeou S. Chiou, Gen Chiaki, Yurina Nakazato, Naoki Yoshida
Figure caption: Evolution of a star-forming SIGO. In the left panel, we show the evolution of the R 200 of the companion halo to the SIGO in Figure 1 (defined as the nearest halo to the SIGO as a function of the halo’s R 200). We also show the separation between the centers of mass of the SIGO and companion halo. In the right panel, we show the evolution of the total mass of the SIGO and the companion halo. The SIGO is indicated with stars in this panel. It begins forming stars at z ∼ 16.5. The black dots and lines in this panel indicate the mass evolution of the halo most closely associated with this SIGO at each redshift. The colors show the mass fraction of stars and gas within the SIGO compared to its total mass, showing that it maintains a high gas fraction throughout its evolution. Just after redshift 15, the companion halo that had previously been closest to the SIGO as a function of its R 200 is supplanted by a slightly more distant but significantly larger halo. This transition is marked with a blue horizontal line labeled “Companion Halo Switches” in both panels.
Paper: The Supersonic Project: Star Formation in Early Star Clusters without Dark Matter
Authors: William Lake, Smadar Naoz, Federico Marinacci, Blakesley Burkhart, Mark Vogelsberger, Claire E. Williams, Yeou S. Chiou, Gen Chiaki, Yurina Nakazato, Naoki Yoshida
Figure caption: SIGO flux as a function of redshift of initial star formation and JWST detectability. We consider the possibility of observing a lensed SIGO beginning star formation at later redshifts, similar to the observation of a faint lensed source in Welch et al. (2022). Solid lines show the modeled 1500 Å flux adopting the star formation rate estimate directly from our simulation (i.e., Figure 5, in Appendix). However, as discussed in Lake et al. (2023), larger SIGOs more readily form stars; therefore, we also consider a more massive, larger SIGO with a gas mass of ∼107 M ⊙. We scale the star formation rate linearly as a function of mass (as implied from the star formation rate–mass relation; e.g., Lada et al. 2012). This example is shown with dotted–dashed lines labeled as “Bright SIGO.” For the two examples, we show three possible magnifications of 10 (blue), 100 (orange), and 1000 (red), from bottom to top. The light (dark) shadowed region shows characteristic JWST sensitivity after 104 (106) s exposure time with a signal-to-noise ratio of about 10, in agreement with the JWST Exposure Time Calculator (Pontoppidan et al. 2016).
Paper: The Supersonic Project: Star Formation in Early Star Clusters without Dark Matter
Authors: William Lake, Smadar Naoz, Federico Marinacci, Blakesley Burkhart, Mark Vogelsberger, Claire E. Williams, Yeou S. Chiou, Gen Chiaki, Yurina Nakazato, Naoki Yoshida
Figure caption: Formation of a SIGO-derived GC. Here we show successive snapshots of a SIGO (yellow ellipse) becoming a star cluster interacting with DM halos (white circles) in our 2σ streaming velocity run. Stars are marked in the zoom-in panel (right) of each snap with black crosses. In the top panels, at z = 17, the SIGO is outside any DM halo and has not formed stars. By z = 15, in the middle panels, the SIGO is undergoing star formation. In the bottom panels, at z = 12, the SIGO (indicated by a white arrow) is no longer identified as an independent gas object caught on the edges of a protogalaxy merger. This SIGO’s fate is likely as a bound star cluster in this newborn galaxy (marked as “Background Galaxy” and also referred to as a protogalaxy in the text). Two other smaller halos are also present in the bottom panels.
Paper: The Supersonic Project: Star Formation in Early Star Clusters without Dark Matter
Authors: William Lake, Smadar Naoz, Federico Marinacci, Blakesley Burkhart, Mark Vogelsberger, Claire E. Williams, Yeou S. Chiou, Gen Chiaki, Yurina Nakazato, Naoki Yoshida
Figure caption: Gas density field around a star-forming SIGO (marked with a cyan ellipse) and local DM halos (marked with white circles) in our simulations at z = 15. The color scale shows the column mass density of matter in the box to a depth of 3 kpc, centered on the center of mass of the SIGO in run 2v. From left to right, we consider (a) gas density without the streaming velocity (0v), (b) gas density with the streaming velocity (2v), and (c) DM density with the streaming velocity (2v). All three panels show the same region. As can be seen in the middle panel, a SIGO is embedded in a larger shock (the high-density region of gas) and has a central high-density region/star formation site. The central SIGO here has a first generation of about 2 × 104 M ⊙ of stars by z = 15 in run 2v. The SIGO does not exist in run 0v (left).
Paper: The Force-freeness of the Solar Photosphere: Revisit with New Approach and Large Data Sets
Authors: Mei Zhang, Haocheng Zhang
Figure caption: From top to bottom, the panels present the magnetogram of NOAA 11739, F  x /F  p , F  y /F  p , and F  z /F  p  values. The left panels are of the HMI/SDO data, the middle panels are of the SP/Hinode “flux density” data, and the right panels are of the SP/Hinode “true field strength” data. The x-axis in the bottom nine panels is the resolution-index R. The green filled diamond points are of the NOAA 11739. The blue filled circle points present the corresponding mean values in each sample (those also shown in Figures 4–6). See the main text for more details.
Paper: The Force-freeness of the Solar Photosphere: Revisit with New Approach and Large Data Sets
Authors: Mei Zhang, Haocheng Zhang
Figure caption: The histograms of the F  x /F  p  (left panels), F  y /F  p  (middle panels), and F  z /F  p  (right panels) values of the 547 HMI/SDO magnetograms. From top to bottom, the panels are of the R = 0, 1, 2, 3, and 4 magnetograms, respectively. Blue shows the portion of active regions in the northern hemisphere and green the portion of active regions in the southern hemisphere. The mean value and the NF (non-force-free percentage) value are also listed in each panel. The vertical purple line in each panel shows where the mean value lies.
Paper: The Force-freeness of the Solar Photosphere: Revisit with New Approach and Large Data Sets
Authors: Mei Zhang, Haocheng Zhang
Figure caption: From top to bottom, the panels present the F  x /F  p , F  y /F  p , and F  z /F  p  values for the analytical force-free magnetic field (left panels) and non-force-free magnetic field (right panels). The x-axis is the noise level in the vertical field (﹩{\sigma }_{z}^{0}﹩). Values obtained from magnetograms with different spatial resolutions are presented in different colors, black for R = 0, blue for R = 1, red for R = 2, green for R = 3, and yellow for R = 4. See the main text for more details.
Paper: The Force-freeness of the Solar Photosphere: Revisit with New Approach and Large Data Sets
Authors: Mei Zhang, Haocheng Zhang
Figure caption: From top to bottom, the panels present the magnetogram, F  x /F  p , F  y /F  p , and F  z /F  p  values for the analytical force-free magnetic field (left panels) and non-force-free magnetic field (right panels). The x-axis in the bottom six panels is the resolution-index R, with R = 0 of the original spatial resolution. See the main text for more details.
Paper: The Force-freeness of the Solar Photosphere: Revisit with New Approach and Large Data Sets
Authors: Mei Zhang, Haocheng Zhang
Figure caption: Same as Figure 4 but for the sample of the 138 SP/Hinode “true field strength” magnetograms.
Paper: The Force-freeness of the Solar Photosphere: Revisit with New Approach and Large Data Sets
Authors: Mei Zhang, Haocheng Zhang
Figure caption: Same as Figure 4 but for the sample of the 144 SP/Hinode “flux density” magnetograms.
Paper: A SPectroscopic Survey of Biased Halos in the Reionization Era (ASPIRE): JWST Discovers an Overdensity around a Metal Absorption-selected Galaxy at z ∼ 5.5
Authors: Yunjing Wu, Feige Wang, Zheng Cai, Xiaohui Fan, Kristian Finlator, Jinyi Yang, Joseph F. Hennawi, Fengwu Sun, Jaclyn B. Champagne, Xiaojing Lin, Zihao Li, Zuyi Chen, Eduardo Bañados, George D. Becker, Sarah E. I. Bosman, Gustavo Bruzual, Stephane Charlot, Hsiao-Wen Chen, Jacopo Chevallard, Anna-Christina Eilers, Emanuele Paolo Farina, Xiangyu Jin, Hyunsung D. Jun, Koki Kakiichi, Mingyu Li, Weizhe Liu, Maria A. Pudoka, Wei Leong Tee, Zhang-Liang Xie, Siwei Zou
Figure caption: Number excess of galaxies around Mg II absorbers at z ≃ 5, ﹩{\xi }_{\mathrm{gal}-\mathrm{abs}}(r)=\tfrac{1}{{n}_{0}}\tfrac{N}{{\rm{\Delta }}V}-1﹩. The red dots are the measurements obtained from our observations. Error bars are estimated by assuming Poissonian uncertainties in the 84% confidence level (Gehrels 1986). The blue solid line indicates simulation-predicted values obtained from Doughty & Finlator (2023). The observed values are consistent with that predicted from cosmological simulations.