adsabs/AstroCLIMB huggingface dataset:
Paper: CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era 
Authors: Matilde Mingozzi, Bethan L. James, Karla Z. Arellano-Córdova, Danielle A. Berg, Peter Senchyna, John Chisholm, Jarle Brinchmann, Alessandra Aloisi, Ricardo O. Amorín, Stéphane Charlot, Anna Feltre, Matthew Hayes, Timothy Heckman, Alaina Henry, Svea Hernandez, Nimisha Kumari, Claus Leitherer, Mario Llerena, Crystal L. Martin, Themiya Nanayakkara, Swara Ravindranath, Evan D. Skillman, Yuma Sugahara, Aida Wofford, Xinfeng Xu
Figure caption: The n  e ([S II]) in logarithm as a function of n  e (Si III]) (up-pointing triangles) and n  e (N IV]) (hexagons), as well as n  e (C III]) (down-pointing triangles), color coded as a function of EW(C III]). The uncertainties on the displayed quantities are shown in both axes. The black dotted–dashed line shows the 1:1 relation, while the dotted–dashed black line represents the same relation shifted by 2 dex, which we added to highlight the level of the offset.
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption: The 2019 SOFIA mid-infrared spectra of V1047 Cen obtained on day 87. The blue symbols represent the SOFIA spectra (combination of two grating settings G111 and G227), which include all spectral points where the atmospheric transmission at the flight altitudes are greater than 70% (hence, the gap near ∼9.5  μm). The wavelength coverage of the two gratings is not continuous. Superposed is the best-fit composite blackbody (red solid line), i.e., the sum of a T bb = 7070 ± 950 K from the 2019 photometry data plus a T bb = 425 ± 12 K, the latter is interpreted as thermal emission from heated circumstellar material (dust) from the blast of the 2019 eruption. The inverted orange triangles are contemporaneous (2019) dereddened BVRI and NEOWISE photometry, while the filled-black circles are 2010 WISE photometry showing that the infrared SED peak was represented by a cooler blackbody (solid gray line) of T bb = 315 ± 30 K.
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption: Optical spectral evolution of V1047 Cen throughout different stages of its outburst. The numbers in brackets are days since t 0. We also quote the resolving power of the spectra on the plot. Note that the calibration pipeline introduced artifacts in the continuum of the spectrum of day 74, particularly below 5000 Å.
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption:  Top-left: the OGLE light curve between 2013 and 2019. Days are relative to the 2019 outburst start. Top-right: a red plate of the field of V1047 Cen from DSS obtained in February 1999 (position of V1047 Cen indicated by a green circle). Bottom-left: combined OGLE I-band images of V1047 Cen (circled in green) taken in February 2014. Bottom-right: SOAR unfiltered acquisition image of V1047 Cen (circled in green) taken in June 2019, during the 2019 outburst. In all the charts the field is 2′ × 2′. V1047 Cen lies on the edge of the OGLE images, which is the reason why the chart is cropped on the west edge.
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption: P Cygni line profiles of Hβ, He I 7065 Å, and O I 7773 Å taken on day 281 and O I 1.128 μm taken on day 323 (Numbers between brackets are days since t 0). The red and blue dashed lines represent v  r  = 0 and −1300 km −1, respectively.
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption: Line profile evolution of Hα throughout the outburst of V1047 Cen. The numbers between brackets are days after outburst. The red dashed lines represent the rest velocity (V vrad = 0 km s−1). A heliocentric correction is applied to the radial velocities.
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption: Evolution of the profiles of the O III lines at 4959 and 5007 Å in comparison to Hβ, throughout the outburst of V1047 Cen. The numbers between brackets are days after outburst. The red dashed lines represent the rest velocity (V vrad = 0 km s−1) of O III 4959 Å. A heliocentric correction is applied to the radial velocities. Note that on day 231 Hβ falls near the end of the spectral range.
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption: High-velocity satellite features in the late Hα line profiles, taken on days 615 and 643. The origin of these features is considered in the discussion in Section 4.
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption:  Top: the optical light curve in the I band. Middle: the evolution of the flux ratio between Hβ and O III 5007 Å. Bottom: the evolution of the EW of the Hβ, O III 5007 Å, and O III 4995 Å emission lines.
Paper: The 2019 Outburst of the 2005 Classical Nova V1047 Cen: A Record Breaking Dwarf Nova Outburst or a New Phenomenon?
Authors: E. Aydi, K. V. Sokolovsky, J. S. Bright, E. Tremou, M. M. Nyamai, A. Evans, J. Strader, L. Chomiuk, G. Myers, F-J. Hambsch, K. L. Page, D. A. H. Buckley, C. E. Woodward, F. M. Walter, P. Mróz, P. J. Vallely, T. R. Geballe, D. P. K. Banerjee, R. D. Gehrz, R. P. Fender, M. Gromadzki, A. Kawash, C. Knigge, K. Mukai, U. Munari, M. Orio, V. A. R. M. Ribeiro, J. L. Sokoloski, S. Starrfield, A. Udalski, P. A. Woudt
Figure caption: Gemini-S 0.9–2.5 μm spectra obtained on days 323 and 330. We identify hydrogen recombination and other He and O lines. For the recombination lines, we show the transition of the longest wavelength member.
Paper: Magnetic Field Structure, Doppler Shift, and Intensity of Active Regions and Their Connections with the Solar Wind
Authors: Chi Ma, Hui Fu, Zhenghua Huang, Lidong Xia, Jinmei Zheng, Xinzheng Shi, Bo Li
Figure caption: Remote sensing of AR 12687 and its associated solar wind. The full-disk image taken by AIA 193 Å and the subregion map inside the rectangle (outline of the region scanned by the EIS) are presented in (a) and (b), the photospheric magnetic field measured by HMI is given in (c), the EIS Fe XII 195.12 Å intensity and Doppler maps of AR 12687 are shown in panels (d) and (e), the parameters of the solar wind are shown in (f). The red and blue crosses represent the footpoints of open magnetic field lines derived from the PFSS model. The sky-blue lines contour the magnetically concentrated area and the red lines outline the footpoint areas of blueshift.
Paper: Magnetic Field Structure, Doppler Shift, and Intensity of Active Regions and Their Connections with the Solar Wind
Authors: Chi Ma, Hui Fu, Zhenghua Huang, Lidong Xia, Jinmei Zheng, Xinzheng Shi, Bo Li
Figure caption: Remote sensing of AR 12665 and its associated solar wind. The full-disk image taken by AIA 193 Å and the subregion map inside the rectangle (outline of the region scanned by the EIS) are presented in (a) and (b), the photospheric magnetic field measured by HMI is given in (c), the EIS Fe XII 195.12 Å intensity and Doppler maps of AR 12665 are shown in panels (d) and (e), the parameters of the solar wind are shown in (f). The red and blue crosses represent the footpoints of the open magnetic field lines derived from the PFSS model. The sky-blue lines contour the magnetically concentrated area and the red lines outline the footpoint areas of blueshift.
Paper: Magnetic Field Structure, Doppler Shift, and Intensity of Active Regions and Their Connections with the Solar Wind
Authors: Chi Ma, Hui Fu, Zhenghua Huang, Lidong Xia, Jinmei Zheng, Xinzheng Shi, Bo Li
Figure caption: Remote sensing of AR 12661 and its associated solar wind. The full-disk image taken by AIA 193 Å and the subregion map inside the rectangle (outline of the region scanned by the EIS) are presented in (a) and (b), the photospheric magnetic field measured by HMI is given in (c), the EIS Fe XII 195.12 Å intensity and Doppler maps of AR 12661 are shown in panels (d) and (e), the parameters of the solar wind are shown in (f). The red and blue crosses represent the footpoints of open magnetic field lines derived from the PFSS model. The sky-blue lines contour the magnetically concentrated area and the red lines outline the footpoint areas of blueshift.
Paper: Magnetic Field Structure, Doppler Shift, and Intensity of Active Regions and Their Connections with the Solar Wind
Authors: Chi Ma, Hui Fu, Zhenghua Huang, Lidong Xia, Jinmei Zheng, Xinzheng Shi, Bo Li
Figure caption: Remote sensing of AR 12824 and its associated solar wind. The full-disk image taken by AIA 193 Å and the subregion map inside the rectangle (outline of the region scanned by the EIS) are presented in (a) and (b), the photospheric magnetic field measured by HMI is given in (c), the EIS Fe XII 195.12 Å intensity and Doppler maps of AR 12824 are shown in panels (d) and (e), the parameters of the solar wind are shown in (f). The red and blue crosses represent the footpoints of open magnetic field lines derived from the PFSS model. The sky-blue lines contour the magnetically concentrated area and the red lines outline the footpoint areas of blueshift.
Paper: Magnetic Field Structure, Doppler Shift, and Intensity of Active Regions and Their Connections with the Solar Wind
Authors: Chi Ma, Hui Fu, Zhenghua Huang, Lidong Xia, Jinmei Zheng, Xinzheng Shi, Bo Li
Figure caption: Remote sensing of AR 12599 and its associated solar wind. The full-disk image taken by AIA 193 Å and the subregion map inside the rectangle (outline of the region scanned by the EIS) are presented in (a) and (b), the photospheric magnetic field measured by HMI is given in (c), the EIS Fe XII 195.12 Å intensity and Doppler maps of AR 12599 are shown in panels (d) and (e), the parameters of the solar wind are shown in (f). The red and blue crosses represent the footpoints of open magnetic field lines derived from the PFSS model. The sky-blue lines contour the magnetically concentrated area and the red lines outline the footpoint areas of blueshift.
Paper: Magnetic Field Structure, Doppler Shift, and Intensity of Active Regions and Their Connections with the Solar Wind
Authors: Chi Ma, Hui Fu, Zhenghua Huang, Lidong Xia, Jinmei Zheng, Xinzheng Shi, Bo Li
Figure caption: Associations between the blueshift (blue), PFSS open magnetic field (red), and whether an active region contributes to the solar wind (yellow) are presented in pairs. The associations between the blueshift and PFSS open magnetic field, PFSS open magnetic field and whether an active region contributes to the solar wind, blueshift and whether an active region contributes to the solar wind are presented in the left, middle, and right panels, respectively.
Paper: Magnetic Field Structure, Doppler Shift, and Intensity of Active Regions and Their Connections with the Solar Wind
Authors: Chi Ma, Hui Fu, Zhenghua Huang, Lidong Xia, Jinmei Zheng, Xinzheng Shi, Bo Li
Figure caption: Associations between the PFSS open magnetic field, blueshift, and the solar wind. Whether the PFSS open magnetic field lines and blueshift appear in active regions are presented in the top and middle panels, respectively. The associations between the active regions and the solar wind are shown in the bottom panel. The results are presented by the magnetic polarities and the left (right) bar represents the positive (negative) polarity. The blue and red bars represent yes and no, respectively.
Paper: Magnetic Field Structure, Doppler Shift, and Intensity of Active Regions and Their Connections with the Solar Wind
Authors: Chi Ma, Hui Fu, Zhenghua Huang, Lidong Xia, Jinmei Zheng, Xinzheng Shi, Bo Li
Figure caption: Scatter plots between the relative intensity and Doppler speed of the blueshift areas. The x-axis is the intensity ratios between the blueshift areas and the MCAs as a whole (excluding the blueshift areas). The y-axis represents the average blueshift speed of the blueshift areas. The red line is the linear fitting result. It is clear that the relative intensity is negatively correlated with the average Doppler speed.
Paper: Detecting Magnetospheric Radio Emission from Giant Exoplanets
Authors: Reza Ashtari, Anthony Sciola, Jake D. Turner, Kevin Stevenson
Figure caption: (a) Schematic depicting stellar wind, flowing from the right with velocity v sw and magnetic field B sw, incident on a planetary magnetosphere, with R mp determined by the force balance described by Equation (6), and the mapping of the associated field line to the ionosphere with invariant latitude θ  R1, assuming a dipolar field. The green arrow denotes the dipole moment axis, and the white circle denotes the emission oval. (b) Magnetosphere view of a 3D MHD simulation with a wind–magnetosphere force balance that results in an R mp of 2.7 R  p . The colored plane shows the plasma density in the equatorial plane. Thin white lines trace the magnetic field. The topology of the field lines at the wind–magnetosphere boundary is denoted as completely connected to the stellar wind (green), fully closed to the planet (blue), and having one footpoint on the planet but connected to the stellar wind (red). Inlaid is a view of the simulated planet’s ionosphere with color contours of the upward (blue) and downward (red) FACs. The black circle in each view denotes the 52.5° latitude line as estimated by Equation (8). (c) Same as (b) but with a wind–magnetosphere force balance that results in an R mp of 11.5 R  p  and an emission latitude of 72.8° as estimated by Equation (8), more representative of conditions at Earth.
Paper: Detecting Magnetospheric Radio Emission from Giant Exoplanets
Authors: Reza Ashtari, Anthony Sciola, Jake D. Turner, Kevin Stevenson
Figure caption: Sky position of exoplanets versus sky coverage of observatories. Left—Maximum elevation angle of exoplanets relative to the latitude of each observatory. Right—Duration (in hours) above 20° minimum elevation limit for beamformed ground-based observations. Minimum station elevations are shown as dashed white lines.
Paper: Detecting Magnetospheric Radio Emission from Giant Exoplanets
Authors: Reza Ashtari, Anthony Sciola, Jake D. Turner, Kevin Stevenson
Figure caption: Detectability of predicted exoplanet burst emissions (high stellar activity).
Paper: Detecting Magnetospheric Radio Emission from Giant Exoplanets
Authors: Reza Ashtari, Anthony Sciola, Jake D. Turner, Kevin Stevenson
Figure caption: Detectability of predicted exoplanet burst emissions (low stellar activity) using current radio observatories of interest.
Paper: Detecting Magnetospheric Radio Emission from Giant Exoplanets
Authors: Reza Ashtari, Anthony Sciola, Jake D. Turner, Kevin Stevenson
Figure caption: Detectability of predicted exoplanet burst emissions (low stellar activity).
Paper: Detecting Magnetospheric Radio Emission from Giant Exoplanets
Authors: Reza Ashtari, Anthony Sciola, Jake D. Turner, Kevin Stevenson
Figure caption: Characteristics of the 671 surveyed exoplanets.
Paper: Detecting Magnetospheric Radio Emission from Giant Exoplanets
Authors: Reza Ashtari, Anthony Sciola, Jake D. Turner, Kevin Stevenson
Figure caption: Detectability of predicted exoplanet burst emissions (high stellar activity) using current radio observatories of interest.
Paper: A Comparative Study of Ionospheric Response to Solar Flares at Earth, Venus, and Mars
Authors: Maodong Yan, Tong Dang, Yu-Tian Cao, Jun Cui, Binzheng Zhang, Zerui Liu, Jiuhou Lei
Figure caption: Term analysis of differential force per mass between simulations with and without the X9.3 flare, for the dominant ﹩{{\rm{O}}}^{+}﹩ ion. The orange, blue, red, and green lines denote the contributions from the plasma density gradient, plasma temperature gradient, ion-neutral drag, and Lorentz force, respectively. For Venus and Mars, the changes of the inertial term ﹩\tfrac{\partial {W}_{i}}{\partial t}﹩ are represented by the black line. The basis altitudes (600 km for Earth, 300 km for Venus and Mars) are selected for comparison between three planets associated with their respective exobase altitudes.
Paper: CHAOS. VII. A Large-scale Direct Abundance Study in M33
Authors: Noah S. J. Rogers, Evan D. Skillman, Richard W. Pogge, Danielle A. Berg, Kevin V. Croxall, Jordan Bartlett, Karla Z. Arellano-Córdova, John Moustakas
Figure caption: The CHAOS-measured T  e –T  e  trends in the H II  regions of M33. Each point represents an H II  region containing a direct T  e  from the corresponding ion. The dashed red and blue lines are the T  e –T  e  relations of Garnett (1992) and Rogers et al. (2021), respectively. The number of regions with both direct temperatures, the intrinsic and total scatter in the dependent T  e  are provided in the lower right. (a) and (b): The high- vs. low-ionization zone temperatures, the former as measured by T  e [O III] and the latter measured by T  e [O II] (a) and T  e [N II] (b). (c) and (d): Intermediate-ionization zone temperatures from T  e [S III] as compared to T  e [N II] (c) and T  e [O III] (d). (e) and (f): A comparison of the low-ionization zone temperatures measured by T  e [N II] to the temperatures in the same zone as measured from T  e [O II] (e) and T  e [S II] (f).
Paper: CHAOS. VII. A Large-scale Direct Abundance Study in M33
Authors: Noah S. J. Rogers, Evan D. Skillman, Richard W. Pogge, Danielle A. Berg, Kevin V. Croxall, Jordan Bartlett, Karla Z. Arellano-Córdova, John Moustakas
Figure caption: A comparison of the recalculated T  e [O III], T  e [N II], and 12+log(O/H) in the common H II  regions observed by the literature studies and CHAOS. Each point is color-coded based on the literature study (see legend). (a): Recalculated T  e [O III] from the literature study vs. the CHAOS T  e [O III] measured in the same region. The black solid line represents a one-to-one relation. (b): Recalculated 12+log(O/H) from the literature study vs. the CHAOS 12+log(O/H). (c): δ(O/H), defined as the difference between the CHAOS and literature oxygen abundances in the same region, vs. δT  e [O III], the difference between the CHAOS and literature T  e [O III]. (d): Recalculated T  e [N II] from the literature study vs. the CHAOS T  e [N II]. (e): δ(O/H) vs. δT  e [N II].
Paper: CHAOS. VII. A Large-scale Direct Abundance Study in M33
Authors: Noah S. J. Rogers, Evan D. Skillman, Richard W. Pogge, Danielle A. Berg, Kevin V. Croxall, Jordan Bartlett, Karla Z. Arellano-Córdova, John Moustakas
Figure caption: The direct oxygen abundance trends in the M33 H II  regions observed by CHAOS (black points with same representation as Figure 4) and the recalculated literature abundance trends (various colored points with same representation). The gradients and intrinsic dispersions in O/H about the gradient are provided in the legends and are plotted as the solid lines and shaded regions, respectively. The number of literature H II  regions used in the fits are provided in the lower right corner. The panels provide the recalculated abundances of (a) C06 (pink); (b) R08 (blue); (c) B11 (green); (d) T16 (orange); (e) L16 (red); and (f): A22 (brown).
Paper: CHAOS. VII. A Large-scale Direct Abundance Study in M33
Authors: Noah S. J. Rogers, Evan D. Skillman, Richard W. Pogge, Danielle A. Berg, Kevin V. Croxall, Jordan Bartlett, Karla Z. Arellano-Córdova, John Moustakas
Figure caption: The direct N abundance gradients in M33. In each panel, the gradient and intrinsic scatter are provided as the solid line and shaded regions, respectively, and are reported in the plot legends. The symbols follow the same representation as Figure 4. Top Panel: 12+log(N/H) as a function of R kpc. Bottom Panel: log(N/O) relative abundances as a function of R  g /R  e , or the galactocentric radius normalized to the effective radius of M33. The gradient and dispersion in this fit are for regions with R  g /R  e  < 2, to isolate the secondary N/O gradient.
Paper: CHAOS. VII. A Large-scale Direct Abundance Study in M33
Authors: Noah S. J. Rogers, Evan D. Skillman, Richard W. Pogge, Danielle A. Berg, Kevin V. Croxall, Jordan Bartlett, Karla Z. Arellano-Córdova, John Moustakas
Figure caption: The direct oxygen abundance gradient in M33 measured by CHAOS. The oxygen abundance, 12+log(O/H) (dex), of each region is plotted against the galactocentric radius (in kpc) of the region. The shape of the point represents the number of direct temperatures used to calculate the abundances within the region, as indicated in the legend. The best-fit gradient and intrinsic scatter in O/H about the gradient (provided in the legend) are represented as a solid line and a shaded area about the line, respectively.