adsabs/AstroCLIMB huggingface dataset:
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: The rest-frame color–magnitude distribution of the HALO7D sample. HALO7D galaxies are colored according to their field, and the dwarf galaxies in the sample have colored outlines. The CANDELS galaxies from the same fields are shown as underlying shaded contours. The bottom panel shows the normalized probability density distribution of the rest-UB color in CANDELS, HALO7D, and the low-mass HALO7D sample. HALO7D galaxies overall have a comparable color distribution to CANDELS galaxies, and the dwarf sample predominantly features bluer UB color.
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption:  U − V color vs. V − J color distributions for galaxies in the four CANDELS fields observed in HALO7D (colored points) and in CANDELS (contours). The solid black lines separate the quiescent and star-forming galaxies, using the color selection criteria from Williams et al. (2009) for 0.5 < z < 1.0. The colors of each set of points are as in Figure 17.
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: Observed-frame color–magnitude distribution of galaxies in each field with 0.4 < z < 1.0, the redshift range where the most strong emission lines are likely to be detected in the DEIMOS optical spectra. HALO7D galaxies are colored points, with CANDELS galaxies shown in shaded contours. Dwarf galaxies in HALO7D are indicated by a colored border.
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: The F814W magnitude as a function of redshift for the HALO7D galaxies, colored by stellar mass.
Paper: The Optical Two- and Three-dimensional Fundamental Plane Correlations for Nearly 180 Gamma-Ray Burst Afterglows with Swift/UVOT, RATIR, and the Subaru Telescope
Authors: M. G. Dainotti, S. Young, L. Li, D. Levine, K. K. Kalinowski, D. A. Kann, B. Tran, L. Zambrano-Tapia, A. Zambrano-Tapia, S. B. Cenko, M. Fuentes, E. G. Sánchez-Vázquez, S. R. Oates, N. Fraija, R. L. Becerra, A. M. Watson, N. R. Butler, J. J. González, A. S. Kutyrev, W. H. Lee, J. X. Prochaska, E. Ramirez-Ruiz, M. G. Richer, S. Zola
Figure caption: The top left panel shows an LC with multiple bands and the upper right panel shows an LC including the Subaru data with the W07 function superimposed. The second row of panels show examples of LCs that present a peak of the prompt emission, indicated by an empty black circle and the end of the plateau emission with a filled black circle with the W07 function superimposed with a dark red curve. The third and fourth rows of panels show the same, but with the simple and smoothly BPL, respectively.
Paper: The Optical Two- and Three-dimensional Fundamental Plane Correlations for Nearly 180 Gamma-Ray Burst Afterglows with Swift/UVOT, RATIR, and the Subaru Telescope
Authors: M. G. Dainotti, S. Young, L. Li, D. Levine, K. K. Kalinowski, D. A. Kann, B. Tran, L. Zambrano-Tapia, A. Zambrano-Tapia, S. B. Cenko, M. Fuentes, E. G. Sánchez-Vázquez, S. R. Oates, N. Fraija, R. L. Becerra, A. M. Watson, N. R. Butler, J. J. González, A. S. Kutyrev, W. H. Lee, J. X. Prochaska, E. Ramirez-Ruiz, M. G. Richer, S. Zola
Figure caption: Top panels: 58 GRBs in the ﹩{L}_{\mathrm{opt}}^{(^{\prime} )}-{T}_{\mathrm{opt}}^{(* /^{\prime} )}-{L}_{\mathrm{opt}}^{(^{\prime} )}﹩ parameter space with the fitted plane parameters in Table 2, including LGRBs (black circles), SGRBs (red cuboids), GRB-SNe Ic (purple cones), XRFs and XRRs (blue spheres), and ULGRBs (green icosahedrons). The left and right panels display the 3D correlation with and without any correction for both redshift evolution and selection biases, respectively. Bottom panels: the distances of the GRB of each class indicated with different colors from the Gold fundamental plane, which is taken as a reference, with and without correction for redshift evolution and selection biases, respectively.
Paper: The Optical Two- and Three-dimensional Fundamental Plane Correlations for Nearly 180 Gamma-Ray Burst Afterglows with Swift/UVOT, RATIR, and the Subaru Telescope
Authors: M. G. Dainotti, S. Young, L. Li, D. Levine, K. K. Kalinowski, D. A. Kann, B. Tran, L. Zambrano-Tapia, A. Zambrano-Tapia, S. B. Cenko, M. Fuentes, E. G. Sánchez-Vázquez, S. R. Oates, N. Fraija, R. L. Becerra, A. M. Watson, N. R. Butler, J. J. González, A. S. Kutyrev, W. H. Lee, J. X. Prochaska, E. Ramirez-Ruiz, M. G. Richer, S. Zola
Figure caption: An overview of 3D fundamental plane best-fit parameters, where a, b, and C 0 are color coded according to the GRB class, with darker colors denoting correction. The x-axis displays the 1σ intervals for each parameter. The color coding is as follows: gray for LGRBs, gold for the Gold sample, light blue for XRFs, blue for XRRs, bright green for ULGRBs, purple for SNe Ic, red for SNe ABC, cyan for short and Type I (since both samples are identical), and orange for Type II. The same colors, but darker are for the corrected class. Exact values for each parameter can be found in Table 2.
Paper: The Optical Two- and Three-dimensional Fundamental Plane Correlations for Nearly 180 Gamma-Ray Burst Afterglows with Swift/UVOT, RATIR, and the Subaru Telescope
Authors: M. G. Dainotti, S. Young, L. Li, D. Levine, K. K. Kalinowski, D. A. Kann, B. Tran, L. Zambrano-Tapia, A. Zambrano-Tapia, S. B. Cenko, M. Fuentes, E. G. Sánchez-Vázquez, S. R. Oates, N. Fraija, R. L. Becerra, A. M. Watson, N. R. Butler, J. J. González, A. S. Kutyrev, W. H. Lee, J. X. Prochaska, E. Ramirez-Ruiz, M. G. Richer, S. Zola
Figure caption: The three top left panels show the observed ﹩{L}_{\mathrm{opt}}^{(^{\prime} )}﹩–﹩{T}_{\mathrm{opt}}^{(* /^{\prime} )}﹩ correlations uncorrected for biases and evolution with all classes (first row), the total and Gold samples (second row), and plateau angles (third row), respectively. Panels on the left for the first three rows show the correlation without any correction, on the right with correction. The bottom left panel shows Type I and Type II GRBs. The bottom right shows the GRB-SNe Ic and GRB-SNe ABC classes before and after correction.
Paper: The Optical Two- and Three-dimensional Fundamental Plane Correlations for Nearly 180 Gamma-Ray Burst Afterglows with Swift/UVOT, RATIR, and the Subaru Telescope
Authors: M. G. Dainotti, S. Young, L. Li, D. Levine, K. K. Kalinowski, D. A. Kann, B. Tran, L. Zambrano-Tapia, A. Zambrano-Tapia, S. B. Cenko, M. Fuentes, E. G. Sánchez-Vázquez, S. R. Oates, N. Fraija, R. L. Becerra, A. M. Watson, N. R. Butler, J. J. González, A. S. Kutyrev, W. H. Lee, J. X. Prochaska, E. Ramirez-Ruiz, M. G. Richer, S. Zola
Figure caption: An overview of 2D fundamental plane best-fit parameters, where a and C 0 are color coded according to the GRB class, with darker colors denoting correction. The x-axis displays the 1σ parameter intervals. The color coding is as follows: gray for LGRBs, gold for the Gold sample, light blue for XRFs, blue for XRR, bright green for ULGRBs, purple for SNe Ic, red for SNe ABC, and cyan for both short and Type I (since both samples are identical), and orange for Type II. Exact values for each parameter can be found in Table 2.
Paper: The Optical Two- and Three-dimensional Fundamental Plane Correlations for Nearly 180 Gamma-Ray Burst Afterglows with Swift/UVOT, RATIR, and the Subaru Telescope
Authors: M. G. Dainotti, S. Young, L. Li, D. Levine, K. K. Kalinowski, D. A. Kann, B. Tran, L. Zambrano-Tapia, A. Zambrano-Tapia, S. B. Cenko, M. Fuentes, E. G. Sánchez-Vázquez, S. R. Oates, N. Fraija, R. L. Becerra, A. M. Watson, N. R. Butler, J. J. González, A. S. Kutyrev, W. H. Lee, J. X. Prochaska, E. Ramirez-Ruiz, M. G. Richer, S. Zola
Figure caption: Flow chart summarizing all the steps of the analysis.
Paper: The Optical Two- and Three-dimensional Fundamental Plane Correlations for Nearly 180 Gamma-Ray Burst Afterglows with Swift/UVOT, RATIR, and the Subaru Telescope
Authors: M. G. Dainotti, S. Young, L. Li, D. Levine, K. K. Kalinowski, D. A. Kann, B. Tran, L. Zambrano-Tapia, A. Zambrano-Tapia, S. B. Cenko, M. Fuentes, E. G. Sánchez-Vázquez, S. R. Oates, N. Fraija, R. L. Becerra, A. M. Watson, N. R. Butler, J. J. González, A. S. Kutyrev, W. H. Lee, J. X. Prochaska, E. Ramirez-Ruiz, M. G. Richer, S. Zola
Figure caption: Left panel: the differential distribution of ﹩{T}_{X,a}^{* }﹩ (white solid line) and ﹩{T}_{\mathrm{opt},a}^{* }﹩ (blue dashed line). Middle panel: the same as the left panel, but corrected for evolution. Right panel: the observed luminosity vs. redshift with limiting luminosity curves given by the observability with Tomo-e Gozen.
Paper: The Optical Two- and Three-dimensional Fundamental Plane Correlations for Nearly 180 Gamma-Ray Burst Afterglows with Swift/UVOT, RATIR, and the Subaru Telescope
Authors: M. G. Dainotti, S. Young, L. Li, D. Levine, K. K. Kalinowski, D. A. Kann, B. Tran, L. Zambrano-Tapia, A. Zambrano-Tapia, S. B. Cenko, M. Fuentes, E. G. Sánchez-Vázquez, S. R. Oates, N. Fraija, R. L. Becerra, A. M. Watson, N. R. Butler, J. J. González, A. S. Kutyrev, W. H. Lee, J. X. Prochaska, E. Ramirez-Ruiz, M. G. Richer, S. Zola
Figure caption: Top left panel: plot of ﹩{T}_{{a}_{X}}^{* }﹩ vs. ﹩{T}_{{a}_{\mathrm{opt}}}^{* }﹩ for uncorrected data.Top right panel: the same as the top left panel, but for corrected data. Middle panels: example of GRBs in which the plateau is chromatic in more than 1σ between the X-ray and optical LCs. Bottom panels: examples of GRBs in which the plateau is achromatic between the X-ray and optical LCs within 1σ. ﹩{T}_{a}^{* }﹩ from the W07 fitting appears as a vertical line, denoted in bright red for X-ray and bright blue for the optical in both the middle and bottom panels.
Paper: The Optical Two- and Three-dimensional Fundamental Plane Correlations for Nearly 180 Gamma-Ray Burst Afterglows with Swift/UVOT, RATIR, and the Subaru Telescope
Authors: M. G. Dainotti, S. Young, L. Li, D. Levine, K. K. Kalinowski, D. A. Kann, B. Tran, L. Zambrano-Tapia, A. Zambrano-Tapia, S. B. Cenko, M. Fuentes, E. G. Sánchez-Vázquez, S. R. Oates, N. Fraija, R. L. Becerra, A. M. Watson, N. R. Butler, J. J. González, A. S. Kutyrev, W. H. Lee, J. X. Prochaska, E. Ramirez-Ruiz, M. G. Richer, S. Zola
Figure caption: Left panel: plot of L  X,a  and L opt,a  vs. ﹩{T}_{X,a}^{* }﹩ and ﹩{T}_{\mathrm{opt},a}^{* }﹩ in X-ray (blue) and optical (red). Right panel: same as the left panel, but corrected for evolution.
Paper: Comparison of Spatial Distributions of Intracluster Light and Dark Matter
Authors: Jaewon Yoo, Jongwan Ko, Cristiano G. Sabiu, Jihye Shin, Kyungwon Chun, Ho Seong Hwang, Juhan Kim, M. James Jee, Hyowon Kim, Rory Smith
Figure caption: WOC results for different components of galaxy clusters (upper panel), different dynamical stages of galaxy clusters (middle panel), and the MHD results for different dynamical stages of galaxy clusters (lower panel) are plotted. A smoothing factor of 17 is used for all images. The three data points with the same symbols come from the three projection angles of each galaxy cluster, which are connected with lines. The MHD method results using only the largest contour at each level are plotted as the solid lines, while the results using all the contours are plotted as the dashed faint lines. We shift the MHD results with all the contours by +0.03 on the x-axis for readability. For further details, see Section 5.
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: Example of failure cases for three candidate UDGs. Each panel shows the line-of-sight galaxy distribution, as selected for using the description in the text. The dashed blue vertical line shows the calculated mean redshift of the main concentration of galaxies identified along the line of sight, and the solid vertical line shows the spectroscopic redshift of the UDG candidate. The blue histograms highlight the galaxies in the main peak, as defined in the text. The blue dashed curve shows the Gaussian fit to these galaxies, while the red dashed curve shows the fit to all of the galaxies along each line of sight. The left panel shows an example where the estimated and spectroscopic redshifts agree well, but the Gaussian fit to all of the galaxies is much broader, suggesting the possibility for confusion due to other galaxies along the line of sight. Unfortunately, we would reject this estimated redshift even though it is indeed correct. The middle panel shows another case that is likely to be rejected because of the different widths of the fitted Gaussians, but here we see that the estimated redshift is an inaccurate estimate of the spectroscopic redshift. Finally, in the right panel we show a case where the fit is accepted because the full distribution and main peak are identical, but the UDG lies at a redshift with no cataloged galaxies. This is an example of a catastrophic redshift estimation failure that is impervious to our choice of criteria.
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: Footprint of the Legacy Survey DR9 observations used in this study in R.A. and decl. In the top three panels, shading denotes the observation density for each band as shown in the top color bar. The bottom panel shows regions with coverage available in all three filters. Footprints for our previous work in Coma (Paper I) and SDSS Stripe 82 (Paper II) are shown in green and red, respectively. The Galactic plane is traced by the orange curve.
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 current SMUDGes sample of 5598 UDG candidates on the sky in equatorial coordinates. Top panel shows the individual candidates more clearly, while the lower highlights overdensities. Several well-known structures are circled and labeled, with the strongest concentration being the Virgo cluster, even though the catalog is significantly incomplete in large UDGs for low redshifts (cz < 1800 km s−1) because they are so large on the sky. The sizes of the projected circles have no physical meaning.
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: Cirrus contamination within the DECaLS footprint. The top panel shows the distribution of WISE 12 μm, while the middle panels show it for τ 353. Regions in dark blue in the bottom panel exceed our dust proxy thresholds of either 0.1 MJy sr−1 for WISE 12 μm or 0.05 for τ 353, and comprise ∼30% of the entire footprint. Overlays in green and red in the bottom panel correspond to the footprints from our previous work in Coma (Paper I) and SDSS Stripe 82 (Paper II), respectively. The Galactic plane is shown in orange.
Paper: CoSHA: Code for Stellar Properties Heuristic Assignment—for the MaStar Stellar Library
Authors: Alfredo Mejía-Narváez, Gustavo Bruzual, Sebastian. F. Sánchez, Leticia Carigi, Jorge Barrera-Ballesteros, Mabel Valerdi, Renbin Yan, Niv Drory
Figure caption: Comparison between the MILES (pink), IndoUS (green), and MaStar (purple) parameter coverage. The MaStar contours enclose 25%, 50%, and 75% of the density distributions. MILES and IndoUS enclose 75%. MaStar is only superseded by MILES and IndoUS on the high effective temperature side of the parameter space, while all libraries in ﹩\mathrm{log}g﹩ have similar coverage, and in [Fe/H] MaStar extends the lower metallicity extreme by one order of magnitude. We show the [α/Fe] distributions as computed by COSHA (the dashed lines) for completeness. Again, all libraries share similar coverage for this parameter.
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: Distribution of matched UDG candidates on the sky for three different catalogs compared to the current SMUDGes catalog distribution. The blue diamonds correspond to galaxies from Greco et al. (2018), the red triangles are those from Prole et al. (2019), and the green squares are those from Tanoglidis et al. (2021). The small dots represent the SMUDGes candidates.
Paper: CoSHA: Code for Stellar Properties Heuristic Assignment—for the MaStar Stellar Library
Authors: Alfredo Mejía-Narváez, Gustavo Bruzual, Sebastian. F. Sánchez, Leticia Carigi, Jorge Barrera-Ballesteros, Mabel Valerdi, Renbin Yan, Niv Drory
Figure caption: Similar to Figure 5, but for GSL.
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: Distribution of sources matched with those of Tanoglidis et al. (2021) vs. central surface brightness. The darker histogram represents the distribution of surface brightnesses in the SMUDGes catalog. The lighter histogram, with thinner bars, represents the distribution of surface brightnesses among matched sources. This figure shows that the matched source distribution is skewed toward higher central surface brightness, demonstrating that the fainter objects in SMUDGes are underrepresented in the Tanoglidis et al. (2021) catalog.
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 HST/COS NUV acquisition images of the 45 galaxies in the CLASSY sample are shown in blue, overlaid on top of optical SDSS r-band imaging (unless otherwise noted; red–yellow color bar). The 2.″5 COS aperture used for the UV CLASSY spectra is shown as a blue circle and is very similar to the SDSS 3″ aperture in orange. Galaxies missing SDSS optical spectra do not have a 3″ orange circle. Relative to the HST/COS aperture, most of the NUV light is captured, but a significant fraction of the extended optical light, and subsequently nebular emission from strong emitters (e.g., with EW(Hα ≳ 103 Å), may still be missed. (Continued on next page.)
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 covers broad ranges in typical galaxy parameters, as measured from the optical spectra and UV+optical photometry (see Section 4). Property trends are plotted for the total star formation rate vs. total stellar mass (SFMR; left) and gas-phase oxygen abundance vs. total stellar mass, or the mass–metallicity relationship (MZR; right). For comparison, we plot the z ∼ 0 trends of Chang et al. (2015; SDSS, blue dashed line) and Berg et al. (2012; LMLVL, green dotted–dashed line), as well as the z ∼ 1–2.5 SFMR trends from Whitaker et al. (2014; yellow lines), for the SFMR, and the Berg et al. (2012; LMLVL, green dotted–dashed line) direct-metallicity trend for the MZR. Clearly the CLASSY MZR is typical of local low-mass star-forming galaxies, but the sample is offset to higher SFRs that are more typical of galaxies at cosmic noon.
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 J0036-3333 (black line) is rich with stellar wind features, such as the Si IV and C IV features, and interstellar medium absorption lines, including the strong Si II and C II features. J0036-3333, however, contains no significant UV emission features besides Lyα. Additionally, the flux ± error spectrum, shown in gray, demonstrates the high S/N of CLASSY and the ability to resolve absorption in J0036-3333 from contamination by geocoronal and Milky Way features (regions where the spectrum/black line is not shown).