adsabs/AstroCLIMB huggingface dataset:
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 main steps in the CLASSY coaddition process. The CLASSY spectra are coadded from a combination of G130M, G160M, and one or more of the G185M, G225M, and G140L HST/COS gratings. The first step highlights how the segments of the FUV data sets and the stripes of the NUV data sets are resampled to a common wavelength grid. Then, in step two, any sets of multiple grating data sets for a given galaxy are coadded using the weighting method described in Section 2.3. Finally, to provide the optimal combination of wavelength coverage and spectral resolution for different science cases, the gratings for a given galaxy are coadded into four spectra with different resolutions.
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 multiextension fits (MEFs) file structure for the CLASSY coadd HLSPs. The top shows the informative keywords included in the primary header (extension 0), while the bottom shows the five extensions of spectra formats for each of the four resolution coadds. The extensions can be accessed by extension number or name, as given in each block. Following the HLSP file naming convention, the CLASSY coadded spectra naming template is hlsp_classy_hst_cos_ < target > _scaled_multi_v1_coadded.fits.
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) Spatial distribution of the measured width of the stellar locus w ⊥ using WAVG_MAG_PSF magnitudes for each nside = 128 HEALPix pixel in the DELVE DR2 footprint. The DES region can be seen to have much lower values of w ⊥ indicating a smaller statistical error in these measurements. (Right) Histogram of w ⊥ values (﹩{w}_{\perp }=\sqrt{{\sigma }^{2}+{w}_{\perp ,0}^{2}}﹩), where w ⊥,0 ∼ 8 mmag. The black line shows the same data as the spatial map (WAVG_MAG_PSF magnitudes for the full footprint, a clear bimodality can be seen due to the difference in relative statistical error in measurements between the DES region calibrated with FGCM (σ (FGCM,WAVG) ∼ 3 mmag), and the rest of the DELVE footprint calibrated with ATLAS Refcat2 (σ (ATLAS  R2,WAVG) ∼ 7 mmag). The gray histograms illustrate the difference in the measured width between the weighted-average (solid) and single best measurements (dotted).
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: Median difference between the DELVE DR2 photometry transformed into the Gaia G-band, G DELVE, and the measured magnitude from Gaia EDR3, G Gaia. The spatial distribution of the median difference in each pixel is shown in the left panel (color range clipped to ±10 mmag), while the right panel shows a histogram of the pixel values. A shift in the zero-point can be seen at decl. ∼ −30°, which corresponds to the boundary between the ATLAS Refcat2 use of PS1 and SkyMapper (Section 4.3). This comparison is restricted to the area with overlapping DELVE DR2 coverage in all four bands (g, r, i, z).
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) PSF FWHM distributions for DECam exposures included in DELVE DR2. (Right) Distributions of effective exposure time (t eff × ﹩{T}_{\exp }﹩) for exposures included in DELVE DR2.
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 covers >20,000 deg2 in each of the g, r, i, z bands (colored regions) and ∼17,000 deg2 in all four bands simultaneously (blue region). The ∼5000 deg2 footprint of DES is outlined in black. These and other sky maps are shown in the equal-area McBryde–Thomas flat polar quartic projection.
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) Median observational epoch for DECam observations in all bands (griz) that are used for calculating the coordinates of DELVE DR2 objects. (Right) Median astrometric offsets between DELVE DR2 objects with 16 < g < 19 and Gaia EDR3 objects matched within 2″. Note that no correction has been made for the proper motions of objects, which results in higher astrometric residuals in regions dominated by recent observations (e.g., see Figure 3 of DES Collaboration 2021).
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:  13CO structures identified by DBSCAN. The color maps represent the distributions of the velocity-integrated intensities of 13CO line emission. The black contours indicate the boundaries and the level of 50% at the 12CO line velocity-integrated intensities.
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: Examples of the spectra in the MaStar library, color coded according to their T eff as predicted by COSHA. The typical 1σ band in each spectrum is also shown. In light gray, we show the closest (in parameter space) GSL spectra to each MaStar spectrum. The mismatch from 27–1429 may be attributed to a mismatch between the actual properties of both sets of spectra. The first data release of the library spans a wide range of the physical parameter space that is suitable for training an ML model to predict the properties of the rest of the stellar spectra.
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 color vs. central surface brightness in the g band. The upper left panel shows the completeness-corrected binned distribution while the upper right panel shows the smoothed distribution of the same data. In the lower panel, we compare the distribution of colors for brighter surface brightness (﹩24\lt {\mu }_{0,g}/\mathrm{mag}\ {\mathrm{arcsec}}^{-2}\lt 24.5﹩) in gray and the somewhat lower surface brightness (﹩25\lt {\mu }_{0,g}/\mathrm{mag}\ {\mathrm{arcsec}}^{-2}\lt 25.5﹩) candidates in green. Blue UDG candidates are mostly confined to the higher central surface brightnesses. The blue cloud nearly disappears by μ 0,g  ∼ 25 mag arcsec−2. The red sequence of objects has a slight tilt that we will return to when discussing the color–magnitude relation in Section 6.2.2. A small number of candidates have μ 0,g  < 24 mag arcsec−2 once the measurement is bias corrected.
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: Comparison of spectroscopic and estimated redshifts. Darker symbols represent those objects for which the estimated redshift is within 10% or 3σ of the spectroscopic redshift, while the lighter symbols indicate those where it is not. In the left panel, we show the results for galaxies drawn randomly from the SIMBAD database; in the middle panel, we show those for UDGs with spectroscopic redshifts; and in the right panel, we show those for a sample of HUDs with spectroscopic redshifts. Shaded regions show exclusion zones based on estimated redshifts that eliminate instances where cz is too low to yield a reliable distance.
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 color vs. Sérsic n index. The upper left panel shows the completeness-corrected binned distribution while the upper right panel shows the smoothed distribution of the same data. The lower panel shows the distribution of blue candidates (g − r < 0.45) in the blue histogram and red candidates (g − r > 0.55) in the red histogram. Bluer candidates tend slightly toward smaller values of n, while those with the largest n values are red. This large n-red wing of the distribution is sparsely populated and highly incomplete, and therefore it is less certain than the blue-small n wing. The sample is dominated by sources with n ∼ 0.8 and g − r ∼ 0.6 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: Surface brightness distribution of sources in the current SMUDGes catalog. The thin green bars represent the raw distribution, while the broader, darker bars represent the completeness corrected distribution. Error bars represent Poisson noise, multiplied by completeness fraction. The line is a least-squares fit to all bins with >1000 counts. A small number of candidates have μ 0,g  < 24 mag arcsec−2 once the measurement is bias corrected.
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 fraction of galaxies with recovered estimated redshifts as a function of the environment they are associated with by our technique. As expected, we tend to accept the redshift association more often in richer systems. Also as anticipated, the HUD sample avoids rich systems. The recovered redshifts for the full SMUDGes sample (solid line in middle panel) follows the trend established with the spectroscopic sample, showing no clear bias in the environments that are sampled relative to the training sets. Shaded regions represent 1σ confidence bounds estimated using Poisson errors.
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 fraction of galaxies with recovered estimated redshifts as a function of the spectroscopic redshift. We find little dependence of the recovery fraction on redshift across the relevant redshift range for the random and HUD samples. The SMUDGes sample shows strong fluctuations, but these map the influence of the Virgo and Coma clusters on this particular data set. Shaded regions represent 1σ confidence bounds estimated using Poisson errors.
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 estimated redshift errors as a function of inferred r  e  in physical units. Points coded as in Figure 7. Shaded region shows exclusion region for UDGs. Catastrophic errors are scattered along r  e , and scatter among successful redshift estimates is independent of r  e .
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: Redshift errors vs. the number of galaxies in the associated overdensity. Symbols coded as in Figure 7.
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 basic observational parameters for the cataloged UDG candidate sample. A small number of candidates have μ 0,g  < 24 mag arcsec−2 once the measurement is bias corrected.
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: The correlations of angular sizes, velocity spans, peak intensities, and integrated fluxes of 12CO(1–0) emission with those of 13CO(1–0) line emission. Each dot represents a 12CO cloud with 13CO structures. The 12CO emission parameters of a 12CO cloud represent the global physical parameters of that cloud. The 13CO emission parameters are derived from all the 13CO structures inside a single 12CO cloud. The black lines represent the upper limits (﹩{{ \mathcal A }}_{{}^{13}\mathrm{CO}}﹩ vs. ﹩{{ \mathcal A }}_{{}^{12}\mathrm{CO}}﹩, ﹩{F}_{{}^{13}\mathrm{CO}}﹩ vs. ﹩{F}_{{}^{12}\mathrm{CO}}﹩) and linear least-squares fits (﹩{T}_{\mathrm{peak},{\ }^{13}\mathrm{CO}}﹩ vs. ﹩{T}_{\mathrm{peak},{\ }^{12}\mathrm{CO}}﹩) to the data. The colors on the points represent the distribution of the probability density functions of the 13CO-detects’ counts (2D-PDFs), which are calculated by utilizing kernel density estimation through Gaussian kernels in the Python package scipy.stats.Gaussian_kde.