adsabs/AstroCLIMB huggingface dataset:
Paper: The DECam Local Volume Exploration Survey Data Release 2
Authors: A. Drlica-Wagner, P. S. Ferguson, M. Adamów, M. Aguena, S. Allam, F. Andrade-Oliveira, D. Bacon, K. Bechtol, E. F. Bell, E. Bertin, P. Bilaji, S. Bocquet, C. R. Bom, D. Brooks, D. L. Burke, J. A. Carballo-Bello, J. L. Carlin, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, W. Cerny, C. Chang, Y. Choi, C. Conselice, M. Costanzi, D. Crnojević, L. N. da Costa, J. De Vicente, S. Desai, J. Esteves, S. Everett, I. Ferrero, M. Fitzpatrick, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, D. W. Gerdes, D. Gruen, R. A. Gruendl, J. Gschwend, W. G. Hartley, D. Hernandez-Lang, S. R. Hinton, D. L. Hollowood, K. Honscheid, A. K. Hughes, A. Jacques, D. J. James, M. D. Johnson, K. Kuehn, N. Kuropatkin, O. Lahav, T. S. Li, C. Lidman, H. Lin, M. March, J. L. Marshall, D. Martínez-Delgado, C. E. Martínez-Vázquez, P. Massana, S. Mau, M. McNanna, P. Melchior, F. Menanteau, A. E. Miller, R. Miquel, J. J. Mohr, R. Morgan, B. Mutlu-Pakdil, R. R. Muñoz, E. H. Neilsen, D. L. Nidever, R. Nikutta, J. L. Nilo Castellon, N. E. D. Noël, R. L. C. Ogando, K. A. G. Olsen, A. B. Pace, A. Palmese, F. Paz-Chinchón, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, J. Prat, A. H. Riley, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, M. Sako, J. D. Sakowska, E. Sanchez, F. J. Sánchez, D. J. Sand, L. Santana-Silva, B. Santiago, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, J. D. Simon, M. Smith, M. Soares-Santos, G. S. Stringfellow, E. Suchyta, D. J. Suson, C. Y. Tan, G. Tarle, K. Tavangar, D. Thomas, C. To, E. J. Tollerud, M. A. Troxel, D. L. Tucker, T. N. Varga, A. K. Vivas, A. R. Walker, J. Weller, R. D. Wilkinson, J. F. Wu, B. Yanny, E. Zaborowski, A. Zenteno
Figure caption: DELVE DR2 star/galaxy classification performance as a function of magnitude estimated from matched objects in the wide layer of HSC-SSP PDR3. (Left) Stellar efficiency and galaxy contamination for several stellar samples based on   extended_class_g. (Right) Galaxy efficiency and stellar contamination as a function of magnitude for several galaxy samples based on   extended_class_g.
Paper: The DECam Local Volume Exploration Survey Data Release 2
Authors: A. Drlica-Wagner, P. S. Ferguson, M. Adamów, M. Aguena, S. Allam, F. Andrade-Oliveira, D. Bacon, K. Bechtol, E. F. Bell, E. Bertin, P. Bilaji, S. Bocquet, C. R. Bom, D. Brooks, D. L. Burke, J. A. Carballo-Bello, J. L. Carlin, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, W. Cerny, C. Chang, Y. Choi, C. Conselice, M. Costanzi, D. Crnojević, L. N. da Costa, J. De Vicente, S. Desai, J. Esteves, S. Everett, I. Ferrero, M. Fitzpatrick, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, D. W. Gerdes, D. Gruen, R. A. Gruendl, J. Gschwend, W. G. Hartley, D. Hernandez-Lang, S. R. Hinton, D. L. Hollowood, K. Honscheid, A. K. Hughes, A. Jacques, D. J. James, M. D. Johnson, K. Kuehn, N. Kuropatkin, O. Lahav, T. S. Li, C. Lidman, H. Lin, M. March, J. L. Marshall, D. Martínez-Delgado, C. E. Martínez-Vázquez, P. Massana, S. Mau, M. McNanna, P. Melchior, F. Menanteau, A. E. Miller, R. Miquel, J. J. Mohr, R. Morgan, B. Mutlu-Pakdil, R. R. Muñoz, E. H. Neilsen, D. L. Nidever, R. Nikutta, J. L. Nilo Castellon, N. E. D. Noël, R. L. C. Ogando, K. A. G. Olsen, A. B. Pace, A. Palmese, F. Paz-Chinchón, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, J. Prat, A. H. Riley, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, M. Sako, J. D. Sakowska, E. Sanchez, F. J. Sánchez, D. J. Sand, L. Santana-Silva, B. Santiago, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, J. D. Simon, M. Smith, M. Soares-Santos, G. S. Stringfellow, E. Suchyta, D. J. Suson, C. Y. Tan, G. Tarle, K. Tavangar, D. Thomas, C. To, E. J. Tollerud, M. A. Troxel, D. L. Tucker, T. N. Varga, A. K. Vivas, A. R. Walker, J. Weller, R. D. Wilkinson, J. F. Wu, B. Yanny, E. Zaborowski, A. Zenteno
Figure caption: (Left) Stellar density map created with the  extended_class_g = 0 (high-confidence stars) selection described in Section 4.7. (Right) Analogous galaxy counts map created with the  extended_class_G = 3 (high-confidence galaxies) selection. The region of lower galaxy density toward the northeast of the footprint can be attributed to higher interstellar extinction, which is not corrected for in this map. Color range units are number of objects per arcmin2. Both maps apply a magnitude threshold of  mag_auto_g < 22.
Paper: The DECam Local Volume Exploration Survey Data Release 2
Authors: A. Drlica-Wagner, P. S. Ferguson, M. Adamów, M. Aguena, S. Allam, F. Andrade-Oliveira, D. Bacon, K. Bechtol, E. F. Bell, E. Bertin, P. Bilaji, S. Bocquet, C. R. Bom, D. Brooks, D. L. Burke, J. A. Carballo-Bello, J. L. Carlin, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, W. Cerny, C. Chang, Y. Choi, C. Conselice, M. Costanzi, D. Crnojević, L. N. da Costa, J. De Vicente, S. Desai, J. Esteves, S. Everett, I. Ferrero, M. Fitzpatrick, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, D. W. Gerdes, D. Gruen, R. A. Gruendl, J. Gschwend, W. G. Hartley, D. Hernandez-Lang, S. R. Hinton, D. L. Hollowood, K. Honscheid, A. K. Hughes, A. Jacques, D. J. James, M. D. Johnson, K. Kuehn, N. Kuropatkin, O. Lahav, T. S. Li, C. Lidman, H. Lin, M. March, J. L. Marshall, D. Martínez-Delgado, C. E. Martínez-Vázquez, P. Massana, S. Mau, M. McNanna, P. Melchior, F. Menanteau, A. E. Miller, R. Miquel, J. J. Mohr, R. Morgan, B. Mutlu-Pakdil, R. R. Muñoz, E. H. Neilsen, D. L. Nidever, R. Nikutta, J. L. Nilo Castellon, N. E. D. Noël, R. L. C. Ogando, K. A. G. Olsen, A. B. Pace, A. Palmese, F. Paz-Chinchón, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, J. Prat, A. H. Riley, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, M. Sako, J. D. Sakowska, E. Sanchez, F. J. Sánchez, D. J. Sand, L. Santana-Silva, B. Santiago, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, J. D. Simon, M. Smith, M. Soares-Santos, G. S. Stringfellow, E. Suchyta, D. J. Suson, C. Y. Tan, G. Tarle, K. Tavangar, D. Thomas, C. To, E. J. Tollerud, M. A. Troxel, D. L. Tucker, T. N. Varga, A. K. Vivas, A. R. Walker, J. Weller, R. D. Wilkinson, J. F. Wu, B. Yanny, E. Zaborowski, A. Zenteno
Figure caption: Sky maps and histograms of the S/N = 5 magnitude limit computed from the statistical uncertainty in MAG_PSF. Dashed vertical lines indicate the median depth quoted in Table 1. Sky maps are plotted using an equal-area McBryde–Thomas flat polar quartic projection in celestial equatorial coordinates.
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). III. The Southern SMUDGes Catalog
Authors: Dennis Zaritsky, Richard Donnerstein, Ananthan Karunakaran, C. E. Barbosa, Arjun Dey, Jennifer Kadowaki, Kristine Spekkens, Huanian Zhang, 华年 张
Figure caption: The color–magnitude diagram for UDGs with estimated redshifts. The distribution has been corrected using our completeness estimates. Upper left panel shows the binned distribution, while the right shows the smoothed distribution. The dashed line is the extrapolation of the red sequence derived for faint (L < L *) ellipticals (Schombert 2016). In the lower panel, we show the color distribution for UDGs with −15.0 < M  r  < 15.0, and take note of the color along the red sequence of possible progenitors of this population for two different mass-loss factors. The dotted vertical line is the position of the red sequence corresponding to M  r  = 15.25 mag.
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). III. The Southern SMUDGes Catalog
Authors: Dennis Zaritsky, Richard Donnerstein, Ananthan Karunakaran, C. E. Barbosa, Arjun Dey, Jennifer Kadowaki, Kristine Spekkens, Huanian Zhang, 华年 张
Figure caption: The distribution of candidates that are estimated to have r  e  < 1.5 kpc (upper panel) and those that have r  e  > 1.5 kpc and also have cz > 1800 km s−1 (lower panel), so that the estimated distances are more reliable. Ellipses highlight positions of two known nearby (cz < 1800 km s−1) clusters (Virgo, upper left; Fornax, lower right). Outside of nearby clusters, we do not find that a large fraction of our candidates are likely to have r  e  < 1.5 kpc, suggesting that most of our candidates (outside of nearby clusters) are likely to be UDGs (see text for numbers).
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). III. The Southern SMUDGes Catalog
Authors: Dennis Zaritsky, Richard Donnerstein, Ananthan Karunakaran, C. E. Barbosa, Arjun Dey, Jennifer Kadowaki, Kristine Spekkens, Huanian Zhang, 华年 张
Figure caption: The comparison of observed properties of the overall sample in gray, the sample of candidates for which we were able to estimate a redshift and the inferred size confirms the candidate as a UDG (r  e  > 1.5 kpc) in green (upper panels), and candidates with an estimated redshift that are rejected as UDGs (r  e  < 1.5 kpc) in red (lower panels). All distributions are normalized to sum to unity for comparison.
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). III. The Southern SMUDGes Catalog
Authors: Dennis Zaritsky, Richard Donnerstein, Ananthan Karunakaran, C. E. Barbosa, Arjun Dey, Jennifer Kadowaki, Kristine Spekkens, Huanian Zhang, 华年 张
Figure caption: The dependence of UDG color on environment. In the left panel, we plot UDG color, g − r, vs. the line-of-sight velocity dispersion of the associated overdensity (σ) for each UDG with an estimated redshift. In the right panel, we plot color vs. the number of galaxies with known redshift in the associated overdensity for each UDG with an estimated redshift. In each panel, the solid line is the rolling mean of 75 galaxies. The lightly shaded area shows the dispersion among measurements in each rolling bin, while the more heavily shaded area shows the dispersion in the mean.
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). III. The Southern SMUDGes Catalog
Authors: Dennis Zaritsky, Richard Donnerstein, Ananthan Karunakaran, C. E. Barbosa, Arjun Dey, Jennifer Kadowaki, Kristine Spekkens, Huanian Zhang, 华年 张
Figure caption: Examples of UDGs in the blue (0.2 < g − r < 0.45) and red (0.55 < g − r < 0.7) higher central surface (μ 0,g  < 24.5) populations. Blue galaxies in the upper two rows, red in the lower two. Some blue UDGs show more internal structure and irregularities. Some red UDGs show what appear to be nuclear star clusters.
Paper: Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). III. The Southern SMUDGes Catalog
Authors: Dennis Zaritsky, Richard Donnerstein, Ananthan Karunakaran, C. E. Barbosa, Arjun Dey, Jennifer Kadowaki, Kristine Spekkens, Huanian Zhang, 华年 张
Figure caption: The 2D distribution of n vs. central surface brightness in the g band. The left panel shows the completeness-corrected binned distribution, while the right panel shows the smoothed distribution of the same data. A small number of candidates have μ 0,g  < 24 mag arcsec−2 once the measurement is bias corrected.
Paper: The COS Legacy Archive Spectroscopy Survey (CLASSY) Treasury Atlas 
Authors: Danielle A. Berg, Bethan L. James, Teagan King, Meaghan McDonald, Zuyi Chen, John Chisholm, Timothy Heckman, Crystal L. Martin, Dan P. Stark, Alessandra Aloisi, Ricardo O. Amorín, Karla Z. Arellano-Córdova, Matthew Bayliss, Rongmon Bordoloi, Jarle Brinchmann, Stéphane Charlot, Jacopo Chevallard, Ilyse Clark, Dawn K. Erb, Anna Feltre, Max Gronke, Matthew Hayes, Alaina Henry, Svea Hernandez, Anne Jaskot, Tucker Jones, Lisa J. Kewley, Nimisha Kumari, Claus Leitherer, Mario Llerena, Michael Maseda, Matilde Mingozzi, Themiya Nanayakkara, Masami Ouchi, Adele Plat, Richard W. Pogge, Swara Ravindranath, Jane R. Rigby, Ryan Sanders, Claudia Scarlata, Peter Senchyna, Evan D. Skillman, Charles C. Steidel, Allison L. Strom, Yuma Sugahara, Stephen M. Wilkins, Aida Wofford, Xinfeng Xu
Figure caption: Demonstrations of science that can be derived from model fits to the CLASSY spectra. Top row: the high-resolution coadded spectrum of J0036-3333 is well fit by a light-weighted combination of Starburst99 stellar population synthesis models (turquoise line). The regions of the continuum included in the fit are shown in purple, while masked regions are plotted in gray. The high S/N and spectral resolution of the CLASSY spectra allow both stellar wind (N V λλ1238,1242, Si IV λλ1393,1403, C IV λλ1548,1550) and stellar photospheric (C III λ1247, Si III λλ1295,1297,1299) features to be fit. Middle left: the Si II λ1260 interstellar absorption feature can be characterized in the high-resolution coadded spectrum of J1416+1223 using a double Gaussian fit. This total fit (solid green line) includes a static component (dashed blue line) that is matched to the line-spread function and an outflowing component (dotted–dashed gold line) that characterizes the kinematics of the low-ionization gas. Middle right: the Lyα profile in the very-high-resolution coadded spectrum of J1025+3622 is well fit by a tlac (Gronke & Dijkstra 2014) radiative transfer model. This model can be used to constrain the depth and kinematics of the neutral H gas. Bottom row: the high-resolution spectrum of J1044+0353 contains many high-ionization UV emission lines that are well fit by narrow, nebular Gaussian profiles. These lines, including the Si IV λλ1393,1403, O IV λλ1401,1405,1407, S IV λλ1405,1406,1417, C IV λλ1548,1550, He II λ1640, and O III] λλ1661,1666 lines shown, can be used as nebular diagnostics.
Paper: The COS Legacy Archive Spectroscopy Survey (CLASSY) Treasury Atlas 
Authors: Danielle A. Berg, Bethan L. James, Teagan King, Meaghan McDonald, Zuyi Chen, John Chisholm, Timothy Heckman, Crystal L. Martin, Dan P. Stark, Alessandra Aloisi, Ricardo O. Amorín, Karla Z. Arellano-Córdova, Matthew Bayliss, Rongmon Bordoloi, Jarle Brinchmann, Stéphane Charlot, Jacopo Chevallard, Ilyse Clark, Dawn K. Erb, Anna Feltre, Max Gronke, Matthew Hayes, Alaina Henry, Svea Hernandez, Anne Jaskot, Tucker Jones, Lisa J. Kewley, Nimisha Kumari, Claus Leitherer, Mario Llerena, Michael Maseda, Matilde Mingozzi, Themiya Nanayakkara, Masami Ouchi, Adele Plat, Richard W. Pogge, Swara Ravindranath, Jane R. Rigby, Ryan Sanders, Claudia Scarlata, Peter Senchyna, Evan D. Skillman, Charles C. Steidel, Allison L. Strom, Yuma Sugahara, Stephen M. Wilkins, Aida Wofford, Xinfeng Xu
Figure caption: The CLASSY sample properties, as measured from the optical spectra and UV+optical photometry described in Section 4, span a broad range of parameter space. Top row: star formation rate is plotted vs. stellar mass for both the entire galaxy (left) and in terms of surface density (right). The left plot shows a trend that extends to lower masses and star formation rates, but lies above the previous galaxy sample studies at z ∼ 0 (SDSS; Chang et al. 2015, blue dashed line and LMLVL; Berg et al. 2012 and Lee et al. 2009, cyan dotted–dashed lines) and z ∼ 1–2.5 (Whitaker et al. 2014, yellow lines). The total and intrinsic scatter of the observed trend are given as σ tot. and σ int., respectively. Middle row: specific star formation rate is plotted against gas-phase oxygen abundance, using the total stellar mass and SFR on the left and the aperture values on the right. Here, the majority of the CLASSY sample aligns with or extends from the Curti et al. (2020) relationships for 108 < M ⋆/M ⊙ < 1011 (red to yellow lines, respectively) star-forming SDSS galaxies, but lies well above the dwarf galaxies of the LMLVL (Berg et al. 2012; Lee et al. 2009). Bottom row: oxygen ionization ratio is plotted vs. density in the left-hand plot, showing the wide range in nebular conditions of the CLASSY sample. In the bottom right-hand plot, gas-phase oxygen abundance is plotted relative to total stellar mass, showing the well-known mass–metallicity relationship. The CLASSY sample seems to follow the same trend as other normal star-forming galaxies (e.g., Berg et al. 2012; Curti et al. 2020), but with larger scatter.
Paper: The COS Legacy Archive Spectroscopy Survey (CLASSY) Treasury Atlas 
Authors: Danielle A. Berg, Bethan L. James, Teagan King, Meaghan McDonald, Zuyi Chen, John Chisholm, Timothy Heckman, Crystal L. Martin, Dan P. Stark, Alessandra Aloisi, Ricardo O. Amorín, Karla Z. Arellano-Córdova, Matthew Bayliss, Rongmon Bordoloi, Jarle Brinchmann, Stéphane Charlot, Jacopo Chevallard, Ilyse Clark, Dawn K. Erb, Anna Feltre, Max Gronke, Matthew Hayes, Alaina Henry, Svea Hernandez, Anne Jaskot, Tucker Jones, Lisa J. Kewley, Nimisha Kumari, Claus Leitherer, Mario Llerena, Michael Maseda, Matilde Mingozzi, Themiya Nanayakkara, Masami Ouchi, Adele Plat, Richard W. Pogge, Swara Ravindranath, Jane R. Rigby, Ryan Sanders, Claudia Scarlata, Peter Senchyna, Evan D. Skillman, Charles C. Steidel, Allison L. Strom, Yuma Sugahara, Stephen M. Wilkins, Aida Wofford, Xinfeng Xu
Figure caption: Comparison of rest-frame spectra for J0337-0502 to demonstrate the improvement of CLASSY over previous FUV spectral atlases. The IUE spectrum is relatively low resolution (λ/Δλ ∼ 300) and consists of the integrated light within its large 10″ × 20″ aperture. In contrast, the CLASSY coadded spectral templates are characterized by an unrivaled combination of contiguous 1200–2000 Å FUV wavelength coverage, high spectral resolution (λ/Δλ = 15, 000), and high S/N (average S/N = 6.4 per resel) for much more compact regions that can be targeted with the 2.″5 COS aperture. Both spectra are normalized at 1450 Å. Note that the breaks in the CLASSY spectrum are due to chip gaps and that the geocoronal Lyα and O I emission have been whited-out. While few features are apparent in the IUE J0337-0502 spectra, the CLASSY spectrum reveals a significant number of absorption and emission features that enable simultaneous studies of the massive stellar population, ISM outflows, and nebular emission.
Paper: The COS Legacy Archive Spectroscopy Survey (CLASSY) Treasury Atlas 
Authors: Danielle A. Berg, Bethan L. James, Teagan King, Meaghan McDonald, Zuyi Chen, John Chisholm, Timothy Heckman, Crystal L. Martin, Dan P. Stark, Alessandra Aloisi, Ricardo O. Amorín, Karla Z. Arellano-Córdova, Matthew Bayliss, Rongmon Bordoloi, Jarle Brinchmann, Stéphane Charlot, Jacopo Chevallard, Ilyse Clark, Dawn K. Erb, Anna Feltre, Max Gronke, Matthew Hayes, Alaina Henry, Svea Hernandez, Anne Jaskot, Tucker Jones, Lisa J. Kewley, Nimisha Kumari, Claus Leitherer, Mario Llerena, Michael Maseda, Matilde Mingozzi, Themiya Nanayakkara, Masami Ouchi, Adele Plat, Richard W. Pogge, Swara Ravindranath, Jane R. Rigby, Ryan Sanders, Claudia Scarlata, Peter Senchyna, Evan D. Skillman, Charles C. Steidel, Allison L. Strom, Yuma Sugahara, Stephen M. Wilkins, Aida Wofford, Xinfeng Xu
Figure caption: This moderate-resolution coadded CLASSY spectrum for J1323-0132 (black line) is strikingly different than that of J0036-3333 in Figure 5, highlighting some of the emission lines that are observed at varying strengths for a subset of the CLASSY sample. The spectrum has particularly strong emission features from Lyα, C IV, He II, O III], and C III]; additional weak detections from the high-ionization O IV, S IV, and N IV] lines; but minimal absorption features. Note the high S/N of this spectrum is shown by the gray flux ± error spectrum, while the spectrum/black line is not shown for regions contaminated by geocoronal and Milky Way features.
Paper: The COS Legacy Archive Spectroscopy Survey (CLASSY) Treasury Atlas 
Authors: Danielle A. Berg, Bethan L. James, Teagan King, Meaghan McDonald, Zuyi Chen, John Chisholm, Timothy Heckman, Crystal L. Martin, Dan P. Stark, Alessandra Aloisi, Ricardo O. Amorín, Karla Z. Arellano-Córdova, Matthew Bayliss, Rongmon Bordoloi, Jarle Brinchmann, Stéphane Charlot, Jacopo Chevallard, Ilyse Clark, Dawn K. Erb, Anna Feltre, Max Gronke, Matthew Hayes, Alaina Henry, Svea Hernandez, Anne Jaskot, Tucker Jones, Lisa J. Kewley, Nimisha Kumari, Claus Leitherer, Mario Llerena, Michael Maseda, Matilde Mingozzi, Themiya Nanayakkara, Masami Ouchi, Adele Plat, Richard W. Pogge, Swara Ravindranath, Jane R. Rigby, Ryan Sanders, Claudia Scarlata, Peter Senchyna, Evan D. Skillman, Charles C. Steidel, Allison L. Strom, Yuma Sugahara, Stephen M. Wilkins, Aida Wofford, Xinfeng Xu
Figure caption: Example SED fits for two of the CLASSY galaxies, one local dwarf galaxy (J0944-0038, left) and one emission-line galaxy at z ≈ 0.1 (J1416+1223, right). The fits to host galaxies are shown in the top row while the aperture fits are in the bottom. Blue triangles are the measured fluxes from broadband photometry, and red circles give BEAGLE predictions. The median BEAGLE SED and 16th and 84th percentiles of posterior distribution are shown in black line and gray-shaded area, respectively. The significant excess to the broadband flux in the gr bands of J0944-0038 and r band of J1416+1223 is due to strong nebular emission lines, which are accounted for by BEAGLE.
Paper: The COS Legacy Archive Spectroscopy Survey (CLASSY) Treasury Atlas 
Authors: Danielle A. Berg, Bethan L. James, Teagan King, Meaghan McDonald, Zuyi Chen, John Chisholm, Timothy Heckman, Crystal L. Martin, Dan P. Stark, Alessandra Aloisi, Ricardo O. Amorín, Karla Z. Arellano-Córdova, Matthew Bayliss, Rongmon Bordoloi, Jarle Brinchmann, Stéphane Charlot, Jacopo Chevallard, Ilyse Clark, Dawn K. Erb, Anna Feltre, Max Gronke, Matthew Hayes, Alaina Henry, Svea Hernandez, Anne Jaskot, Tucker Jones, Lisa J. Kewley, Nimisha Kumari, Claus Leitherer, Mario Llerena, Michael Maseda, Matilde Mingozzi, Themiya Nanayakkara, Masami Ouchi, Adele Plat, Richard W. Pogge, Swara Ravindranath, Jane R. Rigby, Ryan Sanders, Claudia Scarlata, Peter Senchyna, Evan D. Skillman, Charles C. Steidel, Allison L. Strom, Yuma Sugahara, Stephen M. Wilkins, Aida Wofford, Xinfeng Xu
Figure caption: Aperture fraction of optical flux vs. redshift for the CLASSY sample. The points are color coded by the optical half-light radii in arcseconds.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: Top panel: The velocity-integrated intensity map of 13CO(1–0) emission in the second Galactic quadrant with 104.°75 < l < 150.°25 and ∣b∣ < 5.°25. This map is derived by integrating the 13CO emission over the velocity range between −95 and 25 km s−1. The distribution of noise rms for the spectrum in each pixel is presented in Figure A1; the mean noise rms is about 0.25 K. The sensitivity for this velocity-integrated map can be calculated as ﹩\sigma \times \sqrt{N}\times {dv}﹩ = 1.2 K km s−1, where σ is the mean noise rms (0.25 K), dv represents the velocity resolution, its value is 0.17 km s−1, and N = 760 is the number of velocity channels. Bottom panel: The latitude-integrated intensity map of 13CO(1–0) emission. This map is derived by integrating the 13CO emission over the latitude range from −5.°25 to 5.°25. The white dashed line at V LSR = −30 km s−1 divides the molecular clouds into two groups, i.e., the near and far groups, as described in Section 4.1. The velocity-integrated intensity maps and the latitude-integrated maps for the 13CO emission in the near and far velocity ranges are shown in Figures A2 and A3, respectively.
Paper: Wavelengths and Energy Levels of Singly Ionized Nickel (Ni II) Measured Using Fourier Transform Spectroscopy
Authors: Christian P. Clear, Juliet C. Pickering, Gillian Nave, Peter Uylings, Ton Raassen
Figure caption: The singly excited (normal) system 3d 8( M  L)nl of Ni II. The upper region of the diagram, above the dotted line indicating the ionization energy of Ni II, displays the ( M L) parent terms of the 3d8 configuration of Ni III against level energy. Vertical lines connect each of the parent terms to boxes representing Ni II levels in their daughter subconfigurations. The height of the boxes indicate the maximum energy range of the levels in each subconfiguration. The terms of the 3d9 configuration are also shown.