adsabs/AstroCLIMB huggingface dataset:
Paper: A Long Time Ago in a Galaxy Far, Far Away: A Candidate z ∼ 12 Galaxy in Early JWST CEERS Imaging
Authors: Steven L. Finkelstein, Micaela B. Bagley, Pablo Arrabal Haro, Mark Dickinson, Henry C. Ferguson, Jeyhan S. Kartaltepe, Casey Papovich, Denis Burgarella, Dale D. Kocevski, Marc Huertas-Company, Kartheik G. Iyer, Anton M. Koekemoer, Rebecca L. Larson, Pablo G. Pérez-González, Caitlin Rose, Sandro Tacchella, Stephen M. Wilkins, Katherine Chworowsky, Aubrey Medrano, Alexa M. Morales, Rachel S. Somerville, L. Y. Aaron Yung, Adriano Fontana, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Lisa J. Kewley, Allison Kirkpatrick, Peter Kurczynski, Jennifer M. Lotz, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Russell E. Ryan, Jonathan R. Trump, Guang Yang, Omar Almaini, Ricardo O. Amorín, Marianna Annunziatella, Bren E. Backhaus, Guillermo Barro, Peter Behroozi, Eric F. Bell, Rachana Bhatawdekar, Laura Bisigello, Volker Bromm, Véronique Buat, Fernando Buitrago, Antonello Calabrò, Caitlin M. Casey, Marco Castellano, Óscar A. Chávez Ortiz, Laure Ciesla, Nikko J. Cleri, Seth H. Cohen, Justin W. Cole, Kevin C. Cooke, M. C. Cooper, Asantha R. Cooray, Luca Costantin, Isabella G. Cox, Darren Croton, Emanuele Daddi, Romeel Davé, Alexander de la Vega, Avishai Dekel, David Elbaz, Vicente Estrada-Carpenter, Sandra M. Faber, Vital Fernández, Keely D. Finkelstein, Jonathan Freundlich, Seiji Fujimoto, Ángela García-Argumánez, Jonathan P. Gardner, Eric Gawiser, Carlos Gómez-Guijarro, Yuchen Guo, Kurt Hamblin, Timothy S. Hamilton, Nimish P. Hathi, Benne W. Holwerda, Michaela Hirschmann, Taylor A. Hutchison, Anne E. Jaskot, Saurabh W. Jha, Shardha Jogee, Stéphanie Juneau, Intae Jung, Susan A. Kassin, Aurélien Le Bail, Gene C. K. Leung, Ray A. Lucas, Benjamin Magnelli, Kameswara Bharadwaj Mantha, Jasleen Matharu, Elizabeth J. McGrath, Daniel H. McIntosh, Emiliano Merlin, Bahram Mobasher, Jeffrey A. Newman, David C. Nicholls, Viraj Pandya, Marc Rafelski, Kaila Ronayne, Paola Santini, Lise-Marie Seillé, Ekta A. Shah, Lu Shen, Raymond C. Simons, Gregory F. Snyder, Elizabeth R. Stanway, Amber N. Straughn, Harry I. Teplitz, Brittany N. Vanderhoof, Jesús Vega-Ferrero, Weichen Wang, Benjamin J. Weiner, Christopher N. A. Willmer, Stijn Wuyts, Jorge A. Zavala
Figure caption: Three-color images of Maisie’s Galaxy. The left image is a composite of HST/ACS F606W and F814W in blue, F115W and F150W in green, and F200W in red. This shows the galaxy candidate as red due to the very high redshift resulting in no detected flux in the filters assigned to the blue and green colors. The right image shows an approximated “true” rest-UV color image composed of F200W+F277W in blue, F356W in green, and F410M+F444W in red. As we discuss further in Section 5, intrinsically, this galaxy is quite blue. The scale bar corresponds to 1 (physical) kpc assuming z = 12 at a scale of 0.″37 kpc–1.
Paper: Spectroscopic and Imaging Observations of Spatially Extended Magnetic Reconnection in the Splitting of a Solar Filament Structure
Authors: Huidong Hu, Ying D. Liu, Lakshmi Pradeep Chitta, Hardi Peter, Mingde Ding
Figure caption: Magnetic reconnection in the filament splitting. (a) SDO/AIA 304 Å image showing the brightening region between the two filament branches. (b) SDO/HMI line-of-sight magnetogram of the active region. (c)–(e) Doppler map, nonthermal width, and intensity (in digital numbers, DN) derived from a single Gaussian fitting of Si IV 1393.755 Å line in the IRIS raster scan. Red contours in (a)–(b) and (e) are of 1 km s−1 redshift surrounding the brightening region. Cyan contours in (a)–(b) and (e), and white contours in (d) are of −1 km s−1 blueshift. The distance between the two crosses (“+”) in (e) is ∼20″ and represents the length of the reconnection region. In (a) the rectangle denotes the field of view (FOV) of the IRIS scan; “F1,” “F2,” and the arrows are similar to those in Figure 1(a). In (c) the two cyan slits “S1” and “S2” indicate where the spectra are displayed in Figure 3(a)–(b); the black dashes denote where on the slits the line profiles are plotted in Figure 3(c)–(d); the time range is the duration of the IRIS raster scan for the FOV; the arrow points to the scan slit whose observation time is the closest to that of the SDO/AIA image in (a). The horizontal line near −110″ in (c)-(e) is a fiducial line.
Paper: Spectroscopic and Imaging Observations of Spatially Extended Magnetic Reconnection in the Splitting of a Solar Filament Structure
Authors: Huidong Hu, Ying D. Liu, Lakshmi Pradeep Chitta, Hardi Peter, Mingde Ding
Figure caption: Spectra of the bidirectional outflows from the reconnection site. (a)–(b) Si IV 1393.755 Å line spectra on slits “S1–2” defined in Figure 2(c). The horizontal lines “i–iv” on each slit are corresponding to the dashes in Figure 2(c). (c)–(d) Line profiles in positions “i–iv” on “S1–2,” and their double Gaussian fits for “i–iii” (but single Gaussian fit for “S2-iii”). The zero velocities are set to the rest wavelengths of Si IV 1393.755 Å. The black curves are the observed profiles; the cyan curves represent the total fits; the red and blue curves plot the two Gaussian components; the component velocities and their 1σ errors are given in kilometers per second.
Paper: Spectroscopic and Imaging Observations of Spatially Extended Magnetic Reconnection in the Splitting of a Solar Filament Structure
Authors: Huidong Hu, Ying D. Liu, Lakshmi Pradeep Chitta, Hardi Peter, Mingde Ding
Figure caption: Differential emission measure (DEM) and emission measure (EM) of the reconnection region based on SDO/AIA observations. (a) The EM that is the zeroth moment of DEM. (b) The EM-weighted temperature, which is the first moment of DEM divided by EM. (c) The temporal changes in the DEM that is averaged over the four pixels specified by the square in (b). The field of view of (a)–(b) is similar to that of Figure 2(c)–(e). The contours in (a) are the same as those in Figure 2(b). In (c), the solid curve is the EM-weighted temperature corresponding to the DEM, the dashed line denotes the averaged background EM-weighted temperature (with its span representing the time range 22:41:03–22:43:27 UT), and the dotted line marks the peak time of the EM and EM-weighted temperature.
Paper: Spectroscopic and Imaging Observations of Spatially Extended Magnetic Reconnection in the Splitting of a Solar Filament Structure
Authors: Huidong Hu, Ying D. Liu, Lakshmi Pradeep Chitta, Hardi Peter, Mingde Ding
Figure caption: Sketch of the magnetic field lines associated with the reconnection in the filament splitting. (a) Before the reconnection the upper and lower filament branches (green lines) are tethered by the magnetic field lines (purple curves). (b) (enlarged view) Magnetic reconnection occurs at a series of “X” points between the two filament branches, where the blue and red arrows indicate the upward and downward outflows, respectively. (c) After the reconnection the tether magnetic field lines are cut and the filament structure is split.
Paper: Using Anisotropies as a Forensic Tool for Decoding Supernova Remnants
Authors: Abigail Polin, Paul Duffell, Dan Milisavljevic
Figure caption: Power spectrum associated with the s = 2, n = 7 Chevalier solution. Left: velocity power spectra at different computational resolutions. The dark line tracing the data is the data smoothed via a Gaussian smoothing process used throughout the rest of this work for visualization purposes. Right: the smoothed power spectra of density (green) and velocity (purple) for the high-resolution model. Dashed lines trace the slopes of the characteristic power laws and the solid vertical line denotes the dominant mode, l 0, at which they break. The secondary peak at high l is caused by the grid scale.
Paper: Polar Dust Emission in Quasar IR SEDs and Its Correlation with Narrow-line Regions
Authors: Jianwei Lyu, 建伟 吕, George H. Rieke
Figure caption: Luminosity dependence of the AGN narrow-line emission strength and IR excess emission. For each quasar, we have interpolated and smoothed the observed SEDs, subtracted a WDD AGN template with the normalization at rest-frame 3.3 μm, and computed the relative excess luminosity at 5–25 μm as (L obs − L WDD)/L WDD. The red lines show the linear regressions of the data points with the fitted relations reported in the top-right corner of each panel.
Paper: Using Anisotropies as a Forensic Tool for Decoding Supernova Remnants
Authors: Abigail Polin, Paul Duffell, Dan Milisavljevic
Figure caption: The power spectra associated with velocity for all models. When the x-axis is shifted by a factor of n all of the power spectra align, making sense of the chaos. The green line denotes the best-fit function (Equation (14)). In this plot it becomes clear that l 0 ∼ 3n.
Paper: Using Anisotropies as a Forensic Tool for Decoding Supernova Remnants
Authors: Abigail Polin, Paul Duffell, Dan Milisavljevic
Figure caption: Rayleigh–Taylor fingers extending between the forward and reverse shock as the ejecta expands into the surrounding medium. Shown is the RTI arising from the Chevalier s = 2, n = 7 self-similar solution at a resolution of 8192 × 8192 (r × θ). Velocity is shown on the left and density on the right. The color bar displays values in code units.
Paper: Using Anisotropies as a Forensic Tool for Decoding Supernova Remnants
Authors: Abigail Polin, Paul Duffell, Dan Milisavljevic
Figure caption: Four example slices of the 2048 × 2048 resolution models. Plotted is a passive scalar where light yellow indicates fluid that originally belonged to the SN ejecta and dark purple indicates the surrounding material. Scales here are normalized by the radius of the shock. The dominant angular mode θ 0 for each model is traced out by the dotted lines. This opening angle roughly traces the width of the Rayleigh–Taylor fingers.
Paper: Using Anisotropies as a Forensic Tool for Decoding Supernova Remnants
Authors: Abigail Polin, Paul Duffell, Dan Milisavljevic
Figure caption: Effect on the power spectra of varying perturbations in the surrounding medium of the n = 7, s = 2 case according to Equation (25). Each y-axis tilt represents one order in C  l . The clumpy medium does not change the character of the SNR power spectrum.
Paper: Polar Dust Emission in Quasar IR SEDs and Its Correlation with Narrow-line Regions
Authors: Jianwei Lyu, 建伟 吕, George H. Rieke
Figure caption: Redshifts and luminosity (traced by L W2) distribution of the subsamples used to compute AGN templates in Figure 2.
Paper: Polar Dust Emission in Quasar IR SEDs and Its Correlation with Narrow-line Regions
Authors: Jianwei Lyu, 建伟 吕, George H. Rieke
Figure caption: WISE colors vs. [O IV]25.89 μm/W2 luminosity ratio (left panels) and [O III] 5007 Å/Hβ EW ratio (right panels). The red dots are for the PG quasar sample, with the open circles indicating the cases where galaxy emission contributes over 50% of the IR output (from Lyu et al. 2017), the blue crosses are for the SDSS-Spitzer sample (left panels) and background gray contours are the distribution of the SDSS quasar sample (right panels). The typical 1σ uncertainties of these measurements are ≲5%–10%. The green dashed and blue solid lines are, respectively, the template colors of warm-dust-deficient and normal AGN templates at the average redshift of the sample. The Spearman’s rank correlation coefficients ρ of each sample are denoted in the corresponding color.
Paper: Polar Dust Emission in Quasar IR SEDs and Its Correlation with Narrow-line Regions
Authors: Jianwei Lyu, 建伟 吕, George H. Rieke
Figure caption: Average infrared SEDs of the sample binned by L  O IV /L  W2 (left panels) and of EW([O III])/EW(Hβ) (right panels) without (top panels) and with host-galaxy subtraction (bottom panels). The top 1/3, middle 1/3, and low 1/3 of the population are plotted as orange, dark green, and blue solid lines. As a comparison, we also show the spectral template of the normal quasar population (thick gray line) and the broadband SED template of the warm-dust-deficient (WDD) quasar population (light green dotted line) constructed in Lyu et al. (2017). All the templates are normalized at 3 μm with common mid-IR emission features denoted.
Paper: Detection of GeV Emission from an Ultralong Gamma-Ray Burst with the Fermi Large Area Telescope
Authors: Yi-Yun Huang, Hai-Ming Zhang, Kai Yan, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: GBM and Large Area Telescope (LAT) light curves of GRB 220627A. The background subtracted light curves of NaI and BGO are extracted from the CSPEC type data, which use a 1024 ms time bin after the detector trigger and a 4096 ms time bin before the detector trigger. The blue solid line represents the Bayesian block light curve and the gray dashed line represents that the S/N is equal to 3. The last panel shows the LAT TRANSIENT class events for energies >100 MeV using 10 s time bins. The red points show the arrival time and corresponding energy of LAT photons. The vertical dashed lines indicate the time intervals for the time-resolved spectral analysis derived from the Bayesian block: T 0+(−3.08, 129.53, 195.07, 288.26, 907.15, 996.75, 1072.53) s.
Paper: Detection of GeV Emission from an Ultralong Gamma-Ray Burst with the Fermi Large Area Telescope
Authors: Yi-Yun Huang, Hai-Ming Zhang, Kai Yan, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Broadband spectrum of of GRB 220627A in the two emission episodes. Left panel: the time-integrated spectrum measured from T 0 − 3.08 s to T 0 + 288.53 s and the fitting with the CPL+PL model. The dotted and dashed lines represent the CPL component and the PL component, respectively, and the solid lines represent the sum of them. Right panel: the time-integrated spectrum measured from T 0 + 907.15 s to T 0 + 1072.53 s and the fitting with the CPL model.
Paper: Detection of GeV Emission from an Ultralong Gamma-Ray Burst with the Fermi Large Area Telescope
Authors: Yi-Yun Huang, Hai-Ming Zhang, Kai Yan, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Long-term Large Area Telescope (LAT) light curve of GRB 220627A. The black data points represent the GeV light curve of GRB 220627A, while the arrows show the upper limits when the TS value of the data points is less than nine. The blue line shows the TS value of the corresponding data points. The vertical dashed line represents the end of the first emission episode measured by GBM.
Paper: A New Era of Intracluster Light Studies with JWST
Authors: Mireia Montes, Ignacio Trujillo
Figure caption: Left panel: F277W−F444W radial color profile of the BCG+ICL of SMACS 0723. The features seen in the ICL are highlighted in the plot. The east color profile is in orange (squares), while the west profile is in pink (circles). Right panel: stellar mass density radial profile of the BCG+ICL of SMACS 0723. The solid line indicates the density profile derived using an M/L of 0.7, and the dashed line has an M/L of 0.18. The gray shaded area indicates the range of all possible stellar mass density profiles assuming an M/L ranging from 0.7 to 0.18. For illustrative purposes, this is applied in this figure for the east profile. The center of the profile is assumed to have an M/L of 0.7. Note that the X-axis in the right panel is in logarithmic scale.
Paper: A New Era of Intracluster Light Studies with JWST
Authors: Mireia Montes, Ignacio Trujillo
Figure caption: Cluster SMACS 0723. The top panel shows an RGB composite of the long-wavelength bands with a black-and-white background that is an average of the three filters. Some of the most prominent features in the ICL of the cluster are marked with arrows. The inset in the top panel is to better show the features in the center of the cluster. The bottom panel shows an average of the three long-wavelength bands with two isocontours overplotted: 25 (red) and 27.5 (orange) mag arcsec2. North is up, and east is left.
Paper: A New Era of Intracluster Light Studies with JWST
Authors: Mireia Montes, Ignacio Trujillo
Figure caption: Left panel: RGB color-composite image using the original calibrated coadds of the long-wavelength channels. Right panel: RGB color-composite image using the rereduced coadd images created in this work. Note the huge improvement of correcting the strong light gradient toward the east side on the NIRCam.
Paper: A New Era of Intracluster Light Studies with JWST
Authors: Mireia Montes, Ignacio Trujillo
Figure caption: Surface brightness profiles as a function of radius for the BCG + ICL of SMACS 0723 for the F277W (yellow), F356W (orange), and F444W (red) bands. The left panel shows the profiles toward the west, while the right panel shows the profiles toward the east. The insets in both panels indicate the regions where the profiles were extracted.
Paper: A New Era of Intracluster Light Studies with JWST
Authors: Mireia Montes, Ignacio Trujillo
Figure caption: Example of a single frame background correction. Left panel: calibrated F277W frame (jw02736001001_02101_00003_nrcblong_cal.fits). A gradient across the image can be seen toward the upper right corner. Middle panel: second-degree polynomial plane fitted to the (masked) calibrated frame to correct the gradient. Right panel: final frame after subtracting the plane.
Paper: A New Era of Intracluster Light Studies with JWST
Authors: Mireia Montes, Ignacio Trujillo
Figure caption: Zoom-ins to the different tidal features of SMACS 0723. The left panels show the RGB composite images, while the right panels show the F277W−F444W color maps. The upper panels show the giant west loop, and the lower panels show the east streams. The width of the different features is indicated with arrows.
Paper: A New Era of Intracluster Light Studies with JWST
Authors: Mireia Montes, Ignacio Trujillo
Figure caption: Left panel: original calibrated F090W coadd. Right panel: final coadd after the data rereduction.
Paper: Early Results from GLASS-JWST. VII. Evidence for Lensed, Gravitationally Bound Protoglobular Clusters at z = 4 in the Hubble Frontier Field A2744 
Authors: E. Vanzella, M. Castellano, P. Bergamini, T. Treu, A. Mercurio, C. Scarlata, P. Rosati, C. Grillo, A. Acebron, G. B. Caminha, M. Nonino, T. Nanayakkara, G. Roberts-Borsani, M. Bradac, X. Wang, G. Brammer, V. Strait, B. Vulcani, U. Meštrić, M. Meneghetti, F. Calura, Alaina Henry, A. Zanella, M. Trenti, K. Boyett, T. Morishita, A. Calabrò, K. Glazebrook, D. Marchesini, S. Birrer, L. Yang, T. Jones
Figure caption: Left panel: GALFIT modeling of the compact knots in images 3a and 3b performed in the HST/ACS F814W (left column) and JWST/NIRISS F200W (right column) bands. The fraction of light the compact sources contribute to the total underlying region is reported in blue in the middle panels (fluxes are measured within circular apertures of 2 × FWHMPSF). Right panel: SED fitting is shown for three of the knots (best-fit parameters are reported in Table 1). The F814W and F200W bands are indicated with vertical transparent stripes; magnitudes on the left (right) y-axis are observed (intrinsic).
Paper: Early Results from GLASS-JWST. VII. Evidence for Lensed, Gravitationally Bound Protoglobular Clusters at z = 4 in the Hubble Frontier Field A2744 
Authors: E. Vanzella, M. Castellano, P. Bergamini, T. Treu, A. Mercurio, C. Scarlata, P. Rosati, C. Grillo, A. Acebron, G. B. Caminha, M. Nonino, T. Nanayakkara, G. Roberts-Borsani, M. Bradac, X. Wang, G. Brammer, V. Strait, B. Vulcani, U. Meštrić, M. Meneghetti, F. Calura, Alaina Henry, A. Zanella, M. Trenti, K. Boyett, T. Morishita, A. Calabrò, K. Glazebrook, D. Marchesini, S. Birrer, L. Yang, T. Jones
Figure caption: The collection of JWST/NIRISS, HST ACS, and WFC3 filters, along with the VLT/HAWKI Ks band are shown superimposed with four examples of z = 4 star-forming templates extracted from Starburst99 library (Leitherer et al. 2014). JWST/NIRISS F200W and VLT/HAWKI Ks bands probe the Blamer break at z = 4. HST F105W and F125W filters bracket NIRISS/F115W; similarly, HST/F140W and HST/F160W bracket NIRISS/F150W.
Paper: Directly Tracing Cool Filamentary Accretion over >100 kpc into the Interstellar Medium of a Quasar Host at z = 1
Authors: Sean D. Johnson, Joop Schaye, Gregory L. Walth, Jennifer I-Hsiu Li, Gwen C. Rudie, Hsiao-Wen Chen, Mandy C. Chen, Benoît Epinat, Massimo Gaspari, Sebastiano Cantalupo, Wolfram Kollatschny, Zhuoqi (Will) Liu, Sowgat Muzahid
Figure caption: Top panels: continuum-subtracted, narrowband images around the [O II] doublet with wavelength ranges chosen to highlight nebulae in the environment of TXS 0206−048. The wavelength range and corresponding approximate [O II] line-of-sight velocity relative to the quasar systemic are labeled in the top right corner of each panel. In each panel, the locations of galaxies in the quasar host environment are marked with black circles and the quasar position is marked by a star. Bottom left panel: [O II] surface brightness contours overlaid on the HST ACS/F814W image of the field marking surface brightness levels of 0.15, 0.3, 0.6, 1.2, and ﹩2.4\times {10}^{-17}\ \mathrm{erg}\,{{\rm{s}}}^{-1}\,{\mathrm{cm}}^{-2}\,{\mathrm{arcsec}}^{-2}﹩ after smoothing with a 1″ × 1″ boxcar. The [O II] contours are formed by summing the three images in the top panels. Bottom middle and right panels: [O II] line-of-sight velocity and line-of-sight velocity dispersion maps of the nebulae around TXS 0206−048 calculated with doublet fitting as described in the text. The locations of group members (quasar) are marked by black circles (black star) in the middle panel and the color interior to the symbols shows the objects systemic line-of-sight velocity relative to the quasar, Δv. The approximate luminosity-weighted group center is marked with an asterisk in all panels.
Paper: Directly Tracing Cool Filamentary Accretion over >100 kpc into the Interstellar Medium of a Quasar Host at z = 1
Authors: Sean D. Johnson, Joop Schaye, Gregory L. Walth, Jennifer I-Hsiu Li, Gwen C. Rudie, Hsiao-Wen Chen, Mandy C. Chen, Benoît Epinat, Massimo Gaspari, Sebastiano Cantalupo, Wolfram Kollatschny, Zhuoqi (Will) Liu, Sowgat Muzahid
Figure caption: Summary of emitting and absorbing gas kinematics near the nucleus. The image in the center panel displays the [O II] surface brightness map zoomed in and scaled to highlight structures near the nucleus. The quasar position is marked by a blue star and pixels touching the star are subject to large uncertainties in quasar light subtraction. The top right panel shows normalized flux of [Ne III] vs. line-of-sight velocity from the quasar while the three panels on the left display [Ne III] emission for circular apertures offset from the quasar centroid. The regions corresponding to each spectrum are shown in black circles and connected to the corresponding spectral panel by a dashed black line. The bottom two panels on the right display O V (middle right) and N IV (bottom right) narrow, associated absorption from the COS FUV spectrum of TXS 0206−048. The COS spectrum reveals both outflowing (blueshifted) and inflowing (redshifted) absorption and photoionization analysis of the absorbers from Finn et al. (2014), indicating that the absorbing gas arises at distances of 2−6 pkpc from the nucleus. For reference, the velocity ranges of the outflowing and inflowing material observed in the quasar absorption spectrum are shown in blue and red highlighting, respectively. The inflowing component exhibits a line-of-sight velocity of ≈+200 km s−1 that is consistent with the velocity field seen in [Ne III] emission seen at 5–10 kpc from the quasar in the panels on the left. The outflowing absorbing gas shows velocities that are comparable to the nuclear [Ne III] but exceed the blueshifts seen in emission at d = 5–10 kpc seen in the left three panels.