adsabs/AstroCLIMB huggingface dataset:
Paper: Do Both Black Holes Spin in Merging Binaries? Evidence from GWTC-4 and Astrophysical Implications
Authors: Christian Adamcewicz, Nir Guttman, Paul D. Lasky, Eric Thrane
Figure caption: Posterior distributions for the mixing fraction λ, mean and width of the cosine tilt distribution μt and σt, and power-law index of the mass-ratio distribution βq for each subpopulation. The posteriors in blue, solid green, dashed green, and orange give the posteriors for the non-spun-up, primary-spun-up, secondary-spun-up, and both-spun-up subpopulations, respectively. In these analyses non-spun-up black holes have nonzero spins, as they do in Section 4. The posteriors on mixing fractions λ are not meaningfully different to those seen in Figure 4, where all subpopulations have identical mass-ratio and tilt distributions.
Paper: Do Both Black Holes Spin in Merging Binaries? Evidence from GWTC-4 and Astrophysical Implications
Authors: Christian Adamcewicz, Nir Guttman, Paul D. Lasky, Eric Thrane
Figure caption: Posterior for the hyperparameters governing the shapes of the subpopulations’ spin magnitude distribution. From left to right, we have the mean μ0 and width σ0 of the default non-spun-up spin distribution, and the mean μ+ and width σ+ of the distribution of spins gained via spin-up. From darkest to lightest, contours in two-dimensional panels give the 50%, 90%, and 99% credible regions of the posterior. This plot gives the posteriors from an analysis allowing for all four subpopulations, however the posteriors are nearly identical to the favored model, which disallows binaries in which only one black hole is spun up.
Paper: Memoirs of Mass Accretion: Probing the Edges of Intracluster Light in Simulated Galaxy Clusters
Authors: Tara Dacunha, Phil Mansfield, Risa H. Wechsler
Figure caption: Projected stellar density maps for 10 example clusters out of our sample of 79 galaxy clusters illustrating the diversity of stellar distributions captured by the NIMBUS star-tagging framework.
Paper: Do Both Black Holes Spin in Merging Binaries? Evidence from GWTC-4 and Astrophysical Implications
Authors: Christian Adamcewicz, Nir Guttman, Paul D. Lasky, Eric Thrane
Figure caption: Posteriors on component spin magnitudes for the six events with the largest spin-Bayes factors ﹩\mathrm{ln}{{ \mathcal Z }}_{{\rm{spin}}}-\mathrm{ln}{{ \mathcal Z }}_{0}﹩. From left to right, top to bottom, events are ordered from largest (36) to smallest (8) values of ﹩\mathrm{ln}{{ \mathcal Z }}_{{\rm{spin}}}-\mathrm{ln}{{ \mathcal Z }}_{0}﹩. From darkest to lightest, the shaded regions in the two-dimensional contour plots give the 50%, 90%, and 99% credible regions.
Paper: Memoirs of Mass Accretion: Probing the Edges of Intracluster Light in Simulated Galaxy Clusters
Authors: Tara Dacunha, Phil Mansfield, Risa H. Wechsler
Figure caption: The optimized MCC classifying present-day Rsp⋆,1 and Rsp⋆,2 values in clusters that did or did not merge in time windows around T of width 0.5, 0.75, and 1.0 dynamical times. Curves corresponding to merger time window widths of 0.5, 0.75, and 1.0 are given by dotted, dashed, and solid lines, respectively. They also decrease in transparency. Horizontal line segments at the top indicate the time windows of mergers determined to be the best classified by the peaks of the MCC curves. For Rsp⋆,1, window widths of 0.75 and 1.0 result in particularly similar curves. For Rsp⋆,2, window widths of 0.5 and 0.75 result in similarly close curves that reach a similar peak.
Paper: The ZZ Ceti Instability Strip for the Most Massive White Dwarf Pulsators
Authors: Gracyn Jewett, Mukremin Kilic, Adam Moss, Alejandro H. Córsico, Matthew J. Green, Murat Uzundag, Pierre Bergeron, Warren R. Brown, Francisco C. De Gerónimo, Alberto Rebassa-Mansergas, Alex J. Brown, Vikram S. Dhillon, Stuart Littlefair
Figure caption: Color–magnitude diagram of the massive (M > 0.9 M⊙) white dwarfs with Teff ≥ 11,000 K in the MWDD 100 pc sample and the Pan-STARRS footprint from G. Jewett et al. (2024). The dotted lines show the evolutionary sequences for 0.9, 1.1, and 1.3 M⊙ white dwarfs with C/O cores (top to bottom, P. Bergeron et al. 2019). The green stars mark both the previously known and the newly discovered pulsating white dwarfs in the sample. Similarly, the red points mark the previously known and newly discovered NOVs.
Paper: Memoirs of Mass Accretion: Probing the Edges of Intracluster Light in Simulated Galaxy Clusters
Authors: Tara Dacunha, Phil Mansfield, Risa H. Wechsler
Figure caption: Cumulative distribution function (CDF) of clusters’ p-values, where the p-value is defined as the fraction of predicted sample MAHs that have a higher RMSE when compared to the median predicted sample MAH than the true MAH (see the text for further details). The solid black line indicates the CDF of a uniform distribution for comparison. As the CDF lays below the uniform distribution, MULTICAM’s scatter in predicted sample MAHs is a conservative description of the accuracy of its median predicted MAH.
Paper: The ZZ Ceti Instability Strip for the Most Massive White Dwarf Pulsators
Authors: Gracyn Jewett, Mukremin Kilic, Adam Moss, Alejandro H. Córsico, Matthew J. Green, Murat Uzundag, Pierre Bergeron, Warren R. Brown, Francisco C. De Gerónimo, Alberto Rebassa-Mansergas, Alex J. Brown, Vikram S. Dhillon, Stuart Littlefair
Figure caption: Light curves (left) and their Fourier transforms (right panels) for J0039−0357 observed on four different nights. The horizontal black dashed lines indicate 4 times the average amplitude in the Fourier transforms, while the vertical dashed blue lines mark the significant frequencies. Table 2 provides a list of the frequencies detected for each observation.
Paper: The ZZ Ceti Instability Strip for the Most Massive White Dwarf Pulsators
Authors: Gracyn Jewett, Mukremin Kilic, Adam Moss, Alejandro H. Córsico, Matthew J. Green, Murat Uzundag, Pierre Bergeron, Warren R. Brown, Francisco C. De Gerónimo, Alberto Rebassa-Mansergas, Alex J. Brown, Vikram S. Dhillon, Stuart Littlefair
Figure caption: Light curves (left) and their Fourier transforms (right panels) for J0039−0357 observed on 2024 November 11 at the GTC using HiPERCAM. The corresponding filter is labeled above the Fourier transform. Table 3 provides a list of the frequencies detected for each observation.
Paper: The ZZ Ceti Instability Strip for the Most Massive White Dwarf Pulsators
Authors: Gracyn Jewett, Mukremin Kilic, Adam Moss, Alejandro H. Córsico, Matthew J. Green, Murat Uzundag, Pierre Bergeron, Warren R. Brown, Francisco C. De Gerónimo, Alberto Rebassa-Mansergas, Alex J. Brown, Vikram S. Dhillon, Stuart Littlefair
Figure caption: Light curves and Fourier transforms for J0959−1828. The top and bottom rows show data taken at APO and NTT/ULTRACAM (g-band), respectively.
Paper: The ZZ Ceti Instability Strip for the Most Massive White Dwarf Pulsators
Authors: Gracyn Jewett, Mukremin Kilic, Adam Moss, Alejandro H. Córsico, Matthew J. Green, Murat Uzundag, Pierre Bergeron, Warren R. Brown, Francisco C. De Gerónimo, Alberto Rebassa-Mansergas, Alex J. Brown, Vikram S. Dhillon, Stuart Littlefair
Figure caption: Light curves and Fourier transforms for J0912−2642.
Paper: The ZZ Ceti Instability Strip for the Most Massive White Dwarf Pulsators
Authors: Gracyn Jewett, Mukremin Kilic, Adam Moss, Alejandro H. Córsico, Matthew J. Green, Murat Uzundag, Pierre Bergeron, Warren R. Brown, Francisco C. De Gerónimo, Alberto Rebassa-Mansergas, Alex J. Brown, Vikram S. Dhillon, Stuart Littlefair
Figure caption: Light curves and Fourier transforms for J0158−2503.
Paper: The Southern Photometrical Local Universe Survey (S-PLUS): Searching for Metal-poor Dwarf Galaxies
Authors: M. Grossi, D. R. Gonçalves, A. C. Krabbe, L. A. Gutiérrez Soto, E. Telles, L. S. Ribeiro, T. S. Gonçalves, A. E. de Araujo-Carvalho, A. R. Lopes, A. V. Smith Castelli, M. E. De Rossi, C. Lima-Dias, G. Limberg, C. E. Ferreira Lopes, J. A. Hernandez-Jimenez, P. K. Humire, A. L. Chies Santos, L. Lomelí-Núñez, S. Torres-Flores, F. R. Herpich, G. B. Oliveira Schwarz, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: Legacy grz cutouts of the six metal-poor dwarf galaxy candidates selected in this work. Legacy images are deeper than S-PLUS, allowing us to infer more details about the galaxy's morphology and structure. The cutout size is 55″ × 55″. See Table 1 for the definition of the ID numbers given at the top-left and bottom-left corners of each postage stamp.
Paper: The Southern Photometrical Local Universe Survey (S-PLUS): Searching for Metal-poor Dwarf Galaxies
Authors: M. Grossi, D. R. Gonçalves, A. C. Krabbe, L. A. Gutiérrez Soto, E. Telles, L. S. Ribeiro, T. S. Gonçalves, A. E. de Araujo-Carvalho, A. R. Lopes, A. V. Smith Castelli, M. E. De Rossi, C. Lima-Dias, G. Limberg, C. E. Ferreira Lopes, J. A. Hernandez-Jimenez, P. K. Humire, A. L. Chies Santos, L. Lomelí-Núñez, S. Torres-Flores, F. R. Herpich, G. B. Oliveira Schwarz, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: Gemini-S/GMOS spectra of DR4_3_SPLUS-s27s07_0011404 (ID 1, first panel from top to bottom), DR4_3_SPLUS-n14s01_0028263 (ID 2, second panel), DR4_3_SPLUS-n13s01_0024584 (ID 3, third panel), and DR4_3_SPLUS-n02n27_0037849 (ID 4, fourth panel) obtained with the B600 grating. The [O III]λ4363 and the [N II], [O II] doublets are highlighted in the insets. The red lines show the best-fit model of the spectrum.
Paper: The Southern Photometrical Local Universe Survey (S-PLUS): Searching for Metal-poor Dwarf Galaxies
Authors: M. Grossi, D. R. Gonçalves, A. C. Krabbe, L. A. Gutiérrez Soto, E. Telles, L. S. Ribeiro, T. S. Gonçalves, A. E. de Araujo-Carvalho, A. R. Lopes, A. V. Smith Castelli, M. E. De Rossi, C. Lima-Dias, G. Limberg, C. E. Ferreira Lopes, J. A. Hernandez-Jimenez, P. K. Humire, A. L. Chies Santos, L. Lomelí-Núñez, S. Torres-Flores, F. R. Herpich, G. B. Oliveira Schwarz, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: Transmission curves of the 12 S-PLUS filters overlaid on the SDSS spectrum of one of the targets of this work (DR4_3_SPLUS-n03s22_0021537). The Hα emission line falls within the wavelength range of the J0660 filter, illustrating the importance of the narrowband filters in identifying star-forming dwarf galaxy candidates.
Paper: The Southern Photometrical Local Universe Survey (S-PLUS): Searching for Metal-poor Dwarf Galaxies
Authors: M. Grossi, D. R. Gonçalves, A. C. Krabbe, L. A. Gutiérrez Soto, E. Telles, L. S. Ribeiro, T. S. Gonçalves, A. E. de Araujo-Carvalho, A. R. Lopes, A. V. Smith Castelli, M. E. De Rossi, C. Lima-Dias, G. Limberg, C. E. Ferreira Lopes, J. A. Hernandez-Jimenez, P. K. Humire, A. L. Chies Santos, L. Lomelí-Núñez, S. Torres-Flores, F. R. Herpich, G. B. Oliveira Schwarz, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: BPT diagram of the six targets in this work, colored according to their respective ID number. The dashed line (L. J. Kewley et al. 2001) and solid line (G. Kauffmann et al. 2003) indicate the regions where ionization is driven by star formation, AGN activity, or a combination of the two mechanisms.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Power-law and multi-Gaussian [O III]λ5007 fits for galaxies classified with ambiguous wing morphologies. The Gaussian parameters shown in the legend are in the following units: amplitudes A in 10−15 erg s−1 cm−2 Å−1, centroids V0 and widths σ in km s−1. The blue- and red-wing power-law fits are shown with their corresponding colors, and the respective best-fit slopes are shown in the legend. The red wing is offset to arbitrarily lower fluxes for display purposes. The best-fit local continuum is shown as a gray dashed line, and the maximum wing velocity ﹩{V}_{{\rm{Max}}}﹩ is shown as dashed–dotted brown lines.
Paper: The Southern Photometrical Local Universe Survey (S-PLUS): Searching for Metal-poor Dwarf Galaxies
Authors: M. Grossi, D. R. Gonçalves, A. C. Krabbe, L. A. Gutiérrez Soto, E. Telles, L. S. Ribeiro, T. S. Gonçalves, A. E. de Araujo-Carvalho, A. R. Lopes, A. V. Smith Castelli, M. E. De Rossi, C. Lima-Dias, G. Limberg, C. E. Ferreira Lopes, J. A. Hernandez-Jimenez, P. K. Humire, A. L. Chies Santos, L. Lomelí-Núñez, S. Torres-Flores, F. R. Herpich, G. B. Oliveira Schwarz, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: Example of SED fitting with CIGALE. Best-fit result for ID 1 (﹩{\chi }_{r}^{2}=0.7﹩, top) and ID 4 (﹩{\chi }_{r}^{2}=0.8﹩, bottom). The best-fit stellar metallicity is 1/30th and 1/20th the solar value, respectively. Diamonds represent the observed fluxes, while crosses and hexagons indicate the model fluxes for the wideband and narrowband filters, respectively.
Paper: Unveiling Stellar Feedback and Cloud Structure in the ρ Ophiuchi-A Region Using ALMA and JWST: Discovery of Substellar Cores, C18O Striations, and Protostellar Outflows
Authors: Fumitaka Nakamura, Ryohei Kawabe, Shuo Huang, Kazuya Saigo, Naomi Hirano, Shigehisa Takakuwa, Takeshi Kamazaki, Motohide Tamura, James Di Francesco, Rachel Friesen, Kazunari Iwasaki, Chihomi Hara
Figure caption: Positions and close-up views of newly identified cores without pointlike infrared emission, i.e., PSS core candidates. (a) JWST near-infrared image overlaid with 1.3 mm dust continuum contours; (b) ALMA 1.3 mm dust continuum contours overlaid on the 12CO (J = 2–1) integrated intensity map around VLA 1623. The smaller panels surrounding (a) and (b) display zoomed-in views of 5″ × 5″. PSS core candidates are marked with white dashed circles in panel (a). The positions of VLA 1623Aa/b and VLA 1623B are indicated in cyan, based on VLA 41 GHz continuum data (R. Kawabe et al. 2018). Dust continuum contours are shown in gray at levels of 4, 6, 8, ⋯ σ. In panel (b), the 12CO emission is integrated over velocities from 1.0 to 1.5 km s−1. Finger-like CO structures, highlighted by cyan arrows, extend outward from VLA 1623, seemingly pointing toward the PSS cores. In each small panel, dust continuum contours are drawn at 3, 5, 7, ⋯ σ. The synthesized beam is shown in the bottom-left corner of each panel.
Paper: Unveiling Stellar Feedback and Cloud Structure in the ρ Ophiuchi-A Region Using ALMA and JWST: Discovery of Substellar Cores, C18O Striations, and Protostellar Outflows
Authors: Fumitaka Nakamura, Ryohei Kawabe, Shuo Huang, Kazuya Saigo, Naomi Hirano, Shigehisa Takakuwa, Takeshi Kamazaki, Motohide Tamura, James Di Francesco, Rachel Friesen, Kazunari Iwasaki, Chihomi Hara
Figure caption: Wide-field JWST NIRCam F470N image, overlaid with the contours of the smoothed 1.3 mm continuum emission. The contours are drawn at 6, 12, 24, 60, 180, and 240σ with 1σ =  0.45 mJy beam−1. The outflows of VLA 1623, [GY92]30, GSS 30, ISO-Oph 26, and [GY92]20 are indicated. The close-up view of the [GY92]20 outflow is presented in Section 4.2.3. The ripple structures possibly created by the Kelvin–Helmholtz instability are enclosed in open dotted squares.
Paper: Unveiling Stellar Feedback and Cloud Structure in the ρ Ophiuchi-A Region Using ALMA and JWST: Discovery of Substellar Cores, C18O Striations, and Protostellar Outflows
Authors: Fumitaka Nakamura, Ryohei Kawabe, Shuo Huang, Kazuya Saigo, Naomi Hirano, Shigehisa Takakuwa, Takeshi Kamazaki, Motohide Tamura, James Di Francesco, Rachel Friesen, Kazunari Iwasaki, Chihomi Hara
Figure caption: Positions and close-up views of the newly detected infrared sources. The images present JWST F444W infrared emission (color scale) overlaid with 1.3 mm dust continuum contours. The central large panel shows a wide-field view with contours of the smoothed continuum image. The smaller panels display 5″ × 5″ zoomed-in views, each overlaid with contours from the original image. The synthesized beam is indicated in the bottom-left corner of each panel. Contour levels are drawn at 3, 5, 7, 9, 11, 15, 20, 30, ⋯ , 100, 200, and 300σ, where 1σ corresponds to 0.25 mJy beam−1 for the original image and 0.445 mJy beam−1 for the smoothed image (see Table 2).
Paper: Unveiling Stellar Feedback and Cloud Structure in the ρ Ophiuchi-A Region Using ALMA and JWST: Discovery of Substellar Cores, C18O Striations, and Protostellar Outflows
Authors: Fumitaka Nakamura, Ryohei Kawabe, Shuo Huang, Kazuya Saigo, Naomi Hirano, Shigehisa Takakuwa, Takeshi Kamazaki, Motohide Tamura, James Di Francesco, Rachel Friesen, Kazunari Iwasaki, Chihomi Hara
Figure caption: (a) 12CO (J = 2–1) and (b) C18O (J = 2–1) velocity-integrated intensity images. In both panels, the gray and yellow contours are identical to those shown in Figure 4, for panels (a) and (b), respectively. In panel (b), we also show contours of the blueshifted (0.5–1.5 km s−1; cyan) and redshifted (5.5–6.5 km s−1; magenta) 12CO components. Both contours are drawn at 30, 60, 90, ⋯, 210σ with 1σ 43 mJy beam−1. Several notable features are indicated with arrows (see the text). The expanding shell structure is highlighted by a dotted ellipse.
Paper: Unveiling Stellar Feedback and Cloud Structure in the ρ Ophiuchi-A Region Using ALMA and JWST: Discovery of Substellar Cores, C18O Striations, and Protostellar Outflows
Authors: Fumitaka Nakamura, Ryohei Kawabe, Shuo Huang, Kazuya Saigo, Naomi Hirano, Shigehisa Takakuwa, Takeshi Kamazaki, Motohide Tamura, James Di Francesco, Rachel Friesen, Kazunari Iwasaki, Chihomi Hara
Figure caption: 1.3 mm dust continuum image of Oph A, created by combining the 7 and 12 m array data. The gray-scale bar represents intensity in Jy beam−1. The image has been smoothed to an angular resolution of 2″ × 2″. The synthesized beam is shown as an open circle in the bottom-left corner. The positions of prestellar cores identified by F. Motte et al. (1998) are marked with open yellow circles. Known YSOs and newly discovered sources identified in our ALMA data are indicated by open black and red squares, respectively. Sources associated with 1.3 mm continuum emission are shown with bold symbols. Newly discovered substellar objects without infrared emission are not marked here, as they are difficult to discern in the image. See Section 4.1.1 for detailed continuum images of these sources. For reference, the Herbig Be star S1 is also marked with an open square.
Paper: Unveiling Stellar Feedback and Cloud Structure in the ρ Ophiuchi-A Region Using ALMA and JWST: Discovery of Substellar Cores, C18O Striations, and Protostellar Outflows
Authors: Fumitaka Nakamura, Ryohei Kawabe, Shuo Huang, Kazuya Saigo, Naomi Hirano, Shigehisa Takakuwa, Takeshi Kamazaki, Motohide Tamura, James Di Francesco, Rachel Friesen, Kazunari Iwasaki, Chihomi Hara
Figure caption: SEDs of several low-mass objects. The open red squares represent the SED of ALMA Oph A 3, which is compared with those of the following sources: the extremely young Class 0 object ALMA Oph A 2 (open black squares; adapted from Figure 7 of R. Kawabe et al. 2018), the young brown dwarf GY 204 (filled black squares from V. Joergens et al. 2013), with its best-fit model shown as a black dashed line), and the free-floating planetary-mass object OTS 44 (blue diamonds from A. Natta et al. 2002), with its best-fit model shown as a blue dashed line). The fluxes for ALMA Oph A 3 are derived from multiple instruments: Spitzer IRAC (3.6, 4.5, 5.8, and 8 μm; obtained from the NASA/IPAC Infrared Science Archive), Herschel PACS (70 μm; from the Herschel Science Archive), and ALMA (1.3 mm; this work).
Paper: Photometric Redshift Forecast for the 7-Dimensional Sky Survey
Authors: Eunhee Ko, 은희 고, Myungshin Im, Yujin Yang, Ji Hoon Kim, Seong-Kook Lee, Gregory S.-H. Paek
Figure caption: Same as Figure  9 but for mi − m775 color.
Paper: Photometric Redshift Forecast for the 7-Dimensional Sky Survey
Authors: Eunhee Ko, 은희 고, Myungshin Im, Yujin Yang, Ji Hoon Kim, Seong-Kook Lee, Gregory S.-H. Paek
Figure caption: Same as Figure 9 but for mg − m475 color.
Paper: The Southern Photometrical Local Universe Survey (S-PLUS): Searching for Metal-poor Dwarf Galaxies
Authors: M. Grossi, D. R. Gonçalves, A. C. Krabbe, L. A. Gutiérrez Soto, E. Telles, L. S. Ribeiro, T. S. Gonçalves, A. E. de Araujo-Carvalho, A. R. Lopes, A. V. Smith Castelli, M. E. De Rossi, C. Lima-Dias, G. Limberg, C. E. Ferreira Lopes, J. A. Hernandez-Jimenez, P. K. Humire, A. L. Chies Santos, L. Lomelí-Núñez, S. Torres-Flores, F. R. Herpich, G. B. Oliveira Schwarz, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: Left: mass–metallicity relation for our sample of metal-poor dwarfs (hexagon symbols) compared to galaxies selected in different photometric surveys—SDSS (circles) and DES (squares) using the same color cuts. The galaxies are compared to the relation found in the Local Volume Legacy (LVL) survey (D. A. Berg et al. 2012, black line), rescaled to a Kroupa IMF. The galaxies selected from the S-PLUS survey (hexagons) show an offset larger than 1σ (shaded region) from the main relation of the LVL galaxies. IDs 1 and 5 are the most extreme outliers displaying the largest offset from the MZR. Stellar masses and oxygen abundances have been derived using the same methodology for all three samples. Right: luminosity–metallicity relation for the three samples compared to the LVL relation (black line).
Paper: The Southern Photometrical Local Universe Survey (S-PLUS): Searching for Metal-poor Dwarf Galaxies
Authors: M. Grossi, D. R. Gonçalves, A. C. Krabbe, L. A. Gutiérrez Soto, E. Telles, L. S. Ribeiro, T. S. Gonçalves, A. E. de Araujo-Carvalho, A. R. Lopes, A. V. Smith Castelli, M. E. De Rossi, C. Lima-Dias, G. Limberg, C. E. Ferreira Lopes, J. A. Hernandez-Jimenez, P. K. Humire, A. L. Chies Santos, L. Lomelí-Núñez, S. Torres-Flores, F. R. Herpich, G. B. Oliveira Schwarz, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption:                         Top panels: legacy images of the four dwarf galaxies observed with GMOS, with the position of the slit overlaid. Central panels: S-PLUS J0660 continuum-subtracted images of the four targets, illustrating the location of the slit over the main star-forming regions. Bottom panels: 2D long-slit spectra of the four galaxies with the observed wavelength on the horizontal axis and the spatial position on the vertical axis. The image shows the Hα and the [N II] doublet emission from the different star-forming knots included in the slits. The gray lines delimit the aperture chosen for the extraction of the 1D spectra of Figure 5.
Paper: The Southern Photometrical Local Universe Survey (S-PLUS): Searching for Metal-poor Dwarf Galaxies
Authors: M. Grossi, D. R. Gonçalves, A. C. Krabbe, L. A. Gutiérrez Soto, E. Telles, L. S. Ribeiro, T. S. Gonçalves, A. E. de Araujo-Carvalho, A. R. Lopes, A. V. Smith Castelli, M. E. De Rossi, C. Lima-Dias, G. Limberg, C. E. Ferreira Lopes, J. A. Hernandez-Jimenez, P. K. Humire, A. L. Chies Santos, L. Lomelí-Núñez, S. Torres-Flores, F. R. Herpich, G. B. Oliveira Schwarz, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: N/O vs. oxygen abundance. The S-PLUS galaxies observed with GMOS (hexagons, colored according to their respective ID number) are compared to other samples with available measurements of the oxygen abundances derived with the direct method: plus (Y. I. Izotov & T. X. Thuan 1999), circles (Y. I. Izotov et al. 2006), diamonds (L. van Zee & M. P. Haynes 2006), crosses (B. H. Andrews & P. Martini 2013), downward triangles (F. Annibali et al. 2019), squares (I. A. Zinchenko et al. 2024). We also display the model of M. B. Vila-Costas & M. G. Edmunds (1993) showing the primary (dotted–dashed line) and secondary (dashed line) nitrogen formation components and their combination (solid line).