adsabs/AstroCLIMB huggingface dataset:
Paper: MINDS. The Detection of 13CO2 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk
Authors: Sierra L. Grant, Ewine F. van Dishoeck, Benoît Tabone, Danny Gasman, Thomas Henning, Inga Kamp, Manuel Güdel, Pierre-Olivier Lagage, Giulio Bettoni, Giulia Perotti, Valentin Christiaens, Matthias Samland, Aditya M. Arabhavi, Ioannis Argyriou, Alain Abergel, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alessio Caratti o Garatti, Vincent Geers, Adrian M. Glauser, Rodrigo Guadarrama, Hyerin Jang, Jayatee Kanwar, Fred Lahuis, Maria Morales-Calderón, Michael Mueller, Cyrine Nehmé, Göran Olofsson, Eric Pantin, Nicole Pawellek, Tom P. Ray, Donna Rodgers-Lee, Silvia Scheithauer, Jürgen Schreiber, Kamber Schwarz, Milou Temmink, Bart Vandenbussche, Marissa Vlasblom, L. B. F. M. Waters, Gillian Wright, Luis Colina, Thomas R. Greve, Kay Justannont, Göran Östlin
Figure caption: Zoom-ins of the 15 μm wavelength range of GW Lup, with the JWST-MIRI data (black) compared to a model (red) composed of emission from 12CO2 (green) and 13CO2 (purple). The continuum and the best-fit models of C2H2, HCN, H2O, and OH shown in Figure 2, have been subtracted from the GW Lup spectrum. The top row shows the best optically thick fit from Figure 2, while the bottom row shows the optically thin 12CO2 fit from Salyk et al. (2011). The optically thick model reproduces the 12CO2 hot-band Q branches at 13.9 and 16.2 μm better than the optically thin model. In the optically thin case, a 12CO2/13CO2 ratio of 68 is not able to reproduce the 13CO2 Q branch at 15.4 μm.
Paper: MINDS. The Detection of 13CO2 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk
Authors: Sierra L. Grant, Ewine F. van Dishoeck, Benoît Tabone, Danny Gasman, Thomas Henning, Inga Kamp, Manuel Güdel, Pierre-Olivier Lagage, Giulio Bettoni, Giulia Perotti, Valentin Christiaens, Matthias Samland, Aditya M. Arabhavi, Ioannis Argyriou, Alain Abergel, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alessio Caratti o Garatti, Vincent Geers, Adrian M. Glauser, Rodrigo Guadarrama, Hyerin Jang, Jayatee Kanwar, Fred Lahuis, Maria Morales-Calderón, Michael Mueller, Cyrine Nehmé, Göran Olofsson, Eric Pantin, Nicole Pawellek, Tom P. Ray, Donna Rodgers-Lee, Silvia Scheithauer, Jürgen Schreiber, Kamber Schwarz, Milou Temmink, Bart Vandenbussche, Marissa Vlasblom, L. B. F. M. Waters, Gillian Wright, Luis Colina, Thomas R. Greve, Kay Justannont, Göran Östlin
Figure caption: The 13–16.3 μm wavelength range of the GW Lup spectrum, with the JWST-MIRI data (black) compared to a model (red) composed of emission from C2H2 (yellow), HCN (orange), H2O (blue), 12CO2 (green), 13CO2 (purple), and OH (pink). The inset shows a zoom-in of the 13CO2 feature.
Paper: MINDS. The Detection of 13CO2 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk
Authors: Sierra L. Grant, Ewine F. van Dishoeck, Benoît Tabone, Danny Gasman, Thomas Henning, Inga Kamp, Manuel Güdel, Pierre-Olivier Lagage, Giulio Bettoni, Giulia Perotti, Valentin Christiaens, Matthias Samland, Aditya M. Arabhavi, Ioannis Argyriou, Alain Abergel, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alessio Caratti o Garatti, Vincent Geers, Adrian M. Glauser, Rodrigo Guadarrama, Hyerin Jang, Jayatee Kanwar, Fred Lahuis, Maria Morales-Calderón, Michael Mueller, Cyrine Nehmé, Göran Olofsson, Eric Pantin, Nicole Pawellek, Tom P. Ray, Donna Rodgers-Lee, Silvia Scheithauer, Jürgen Schreiber, Kamber Schwarz, Milou Temmink, Bart Vandenbussche, Marissa Vlasblom, L. B. F. M. Waters, Gillian Wright, Luis Colina, Thomas R. Greve, Kay Justannont, Göran Östlin
Figure caption: The JWST-MIRI MRS spectrum for GW Lup through Channel 4A. Several of the strongest emission features are labeled and insets show additional molecular features. The beginning and end of each subband has been trimmed to reduce spurious features due to the increased noise at the ends of the bands.
Paper: MINDS. The Detection of 13CO2 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk
Authors: Sierra L. Grant, Ewine F. van Dishoeck, Benoît Tabone, Danny Gasman, Thomas Henning, Inga Kamp, Manuel Güdel, Pierre-Olivier Lagage, Giulio Bettoni, Giulia Perotti, Valentin Christiaens, Matthias Samland, Aditya M. Arabhavi, Ioannis Argyriou, Alain Abergel, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alessio Caratti o Garatti, Vincent Geers, Adrian M. Glauser, Rodrigo Guadarrama, Hyerin Jang, Jayatee Kanwar, Fred Lahuis, Maria Morales-Calderón, Michael Mueller, Cyrine Nehmé, Göran Olofsson, Eric Pantin, Nicole Pawellek, Tom P. Ray, Donna Rodgers-Lee, Silvia Scheithauer, Jürgen Schreiber, Kamber Schwarz, Milou Temmink, Bart Vandenbussche, Marissa Vlasblom, L. B. F. M. Waters, Gillian Wright, Luis Colina, Thomas R. Greve, Kay Justannont, Göran Östlin
Figure caption: The χ 2 maps for H2O, HCN, C2H2, 12CO2, 13CO2, and OH (from top to bottom). The color scale shows ﹩{\chi }_{\min }^{2}/{\chi }^{2}﹩. The red, orange, and yellow contours correspond to the 1σ, 2σ, and 3σ levels. The white contours show the emitting radii in astronomical units, as given by the labels. The best-fit model is marked as the black plus. The best-fit model corresponds to ﹩{\chi }_{\min }^{2}﹩/χ 2 = 1. These maps correspond to the χ 2 and uncertainties after the third round in the iterative fitting procedure. The blue curve in the 12CO2 plot is the best-fitting emitting radius for H2O for comparison.
Paper: MINDS. The Detection of 13CO2 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk
Authors: Sierra L. Grant, Ewine F. van Dishoeck, Benoît Tabone, Danny Gasman, Thomas Henning, Inga Kamp, Manuel Güdel, Pierre-Olivier Lagage, Giulio Bettoni, Giulia Perotti, Valentin Christiaens, Matthias Samland, Aditya M. Arabhavi, Ioannis Argyriou, Alain Abergel, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alessio Caratti o Garatti, Vincent Geers, Adrian M. Glauser, Rodrigo Guadarrama, Hyerin Jang, Jayatee Kanwar, Fred Lahuis, Maria Morales-Calderón, Michael Mueller, Cyrine Nehmé, Göran Olofsson, Eric Pantin, Nicole Pawellek, Tom P. Ray, Donna Rodgers-Lee, Silvia Scheithauer, Jürgen Schreiber, Kamber Schwarz, Milou Temmink, Bart Vandenbussche, Marissa Vlasblom, L. B. F. M. Waters, Gillian Wright, Luis Colina, Thomas R. Greve, Kay Justannont, Göran Östlin
Figure caption: The best-fit model procedure is shown here. The top panel shows the best-fit H2O model (blue) overlaid on the continuum-subtracted JWST-MIRI spectrum. In the second panel, the black spectrum is the observed spectrum after subtracting the H2O model from the first panel. The best-fit HCN model is found using this as the input spectrum. This process continues down the panels. The spectral windows used for each species fit are shown as the horizontal bars, with the given starting and ending points. A region with minimal line emission from 15.90 to 15.94 μm is chosen to determine the noise level (top panel). This region, before subtracting the models has a standard deviation of 0.76 mJy; however, some low-level molecular emission is still present.
Paper: MINDS. The Detection of 13CO2 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk
Authors: Sierra L. Grant, Ewine F. van Dishoeck, Benoît Tabone, Danny Gasman, Thomas Henning, Inga Kamp, Manuel Güdel, Pierre-Olivier Lagage, Giulio Bettoni, Giulia Perotti, Valentin Christiaens, Matthias Samland, Aditya M. Arabhavi, Ioannis Argyriou, Alain Abergel, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alessio Caratti o Garatti, Vincent Geers, Adrian M. Glauser, Rodrigo Guadarrama, Hyerin Jang, Jayatee Kanwar, Fred Lahuis, Maria Morales-Calderón, Michael Mueller, Cyrine Nehmé, Göran Olofsson, Eric Pantin, Nicole Pawellek, Tom P. Ray, Donna Rodgers-Lee, Silvia Scheithauer, Jürgen Schreiber, Kamber Schwarz, Milou Temmink, Bart Vandenbussche, Marissa Vlasblom, L. B. F. M. Waters, Gillian Wright, Luis Colina, Thomas R. Greve, Kay Justannont, Göran Östlin
Figure caption: The same as Figure 8, but now showing the final best fits after the iterative process. The spectra shown in black are the observed data after subtracting the best-fit models from the previous iterations for all molecules except that being fitted; these spectra are what is used in determining the best-fit for the species in each panel. The noise level is decreased from Figure 8 because the excess emission, mostly from 12CO2 in this region has been removed.
Paper: Pointlike Sources among z > 11 Galaxy Candidates: Contaminants due to Supernovae at High Redshifts?
Authors: Haojing Yan, Lifan Wang, Zhiyuan Ma, Lei Hu
Figure caption: Six-band image stamps and profile fitting results of the six point-source F150W dropouts in the Y23 sample (among 60 in total). The image stamps (2.″4 × 2.″4 in size) are based on the 30 mas stacks, and the white circles (0.″5 in radius) are centered on the dropouts. The dropout “short IDs” (as in Y23) are labeled to left, while the passbands are labeled on top. The images used for the 2D Gaussian profile fitting are outlined by the green (for F200W) and orange (for F277W) boxes. The corresponding fitting results are shown in the boxes to right, outlined by the same colors. The legends show the image FWHM values in units of pixels along both axes, and the averages in units of arcseconds are also labeled.
Paper: MINDS. The Detection of 13CO2 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk
Authors: Sierra L. Grant, Ewine F. van Dishoeck, Benoît Tabone, Danny Gasman, Thomas Henning, Inga Kamp, Manuel Güdel, Pierre-Olivier Lagage, Giulio Bettoni, Giulia Perotti, Valentin Christiaens, Matthias Samland, Aditya M. Arabhavi, Ioannis Argyriou, Alain Abergel, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alessio Caratti o Garatti, Vincent Geers, Adrian M. Glauser, Rodrigo Guadarrama, Hyerin Jang, Jayatee Kanwar, Fred Lahuis, Maria Morales-Calderón, Michael Mueller, Cyrine Nehmé, Göran Olofsson, Eric Pantin, Nicole Pawellek, Tom P. Ray, Donna Rodgers-Lee, Silvia Scheithauer, Jürgen Schreiber, Kamber Schwarz, Milou Temmink, Bart Vandenbussche, Marissa Vlasblom, L. B. F. M. Waters, Gillian Wright, Luis Colina, Thomas R. Greve, Kay Justannont, Göran Östlin
Figure caption: The 12CO2-only data, as in Figure 9, with models showing the impact of temperature (± 100 K; top) and column density (± 0.5 dex; bottom). The emitting area for the models has been chosen to best match the data. The best-fit model found for 12CO2, with a temperature of 400 K and a column density of 2.2 × 1018 cm−2, is shown in green. The temperature controls the width of the Q branches and the column density controls the position of the main Q-branch peak and the height of the hot-band peaks.
Paper: MINDS. The Detection of 13CO2 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk
Authors: Sierra L. Grant, Ewine F. van Dishoeck, Benoît Tabone, Danny Gasman, Thomas Henning, Inga Kamp, Manuel Güdel, Pierre-Olivier Lagage, Giulio Bettoni, Giulia Perotti, Valentin Christiaens, Matthias Samland, Aditya M. Arabhavi, Ioannis Argyriou, Alain Abergel, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alessio Caratti o Garatti, Vincent Geers, Adrian M. Glauser, Rodrigo Guadarrama, Hyerin Jang, Jayatee Kanwar, Fred Lahuis, Maria Morales-Calderón, Michael Mueller, Cyrine Nehmé, Göran Olofsson, Eric Pantin, Nicole Pawellek, Tom P. Ray, Donna Rodgers-Lee, Silvia Scheithauer, Jürgen Schreiber, Kamber Schwarz, Milou Temmink, Bart Vandenbussche, Marissa Vlasblom, L. B. F. M. Waters, Gillian Wright, Luis Colina, Thomas R. Greve, Kay Justannont, Göran Östlin
Figure caption: The Spitzer CO2 Q branch vs. 17 μm H2O fluxes in the sample studied in Banzatti et al. (2020). Downward-facing triangles are those with CO2 not detected above 3σ, leftward-facing triangles are those with H2O not detected above 3σ, and open points are those with neither detected above 3σ. Blue points are stars with stellar masses between 0.1 and 0.5 M ⊙, to be comparable to GW Lup (red), which has a stellar mass of 0.46 M ⊙. We show the luminosities determined from Spitzer and JWST for GW Lup.
Paper: MINDS. The Detection of 13CO2 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk
Authors: Sierra L. Grant, Ewine F. van Dishoeck, Benoît Tabone, Danny Gasman, Thomas Henning, Inga Kamp, Manuel Güdel, Pierre-Olivier Lagage, Giulio Bettoni, Giulia Perotti, Valentin Christiaens, Matthias Samland, Aditya M. Arabhavi, Ioannis Argyriou, Alain Abergel, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alessio Caratti o Garatti, Vincent Geers, Adrian M. Glauser, Rodrigo Guadarrama, Hyerin Jang, Jayatee Kanwar, Fred Lahuis, Maria Morales-Calderón, Michael Mueller, Cyrine Nehmé, Göran Olofsson, Eric Pantin, Nicole Pawellek, Tom P. Ray, Donna Rodgers-Lee, Silvia Scheithauer, Jürgen Schreiber, Kamber Schwarz, Milou Temmink, Bart Vandenbussche, Marissa Vlasblom, L. B. F. M. Waters, Gillian Wright, Luis Colina, Thomas R. Greve, Kay Justannont, Göran Östlin
Figure caption: Top: The 13–16.3 μm wavelength range of our JWST-MIRI MRS data of GW Lup (black). The continuum points that we select are shown as the red points and the interpolated continuum is shown as the red line. Middle: The continuum-subtracted spectrum. Bottom: The best-fit models, as in Figure 2, showing the continuum points relative to the molecular features.
Paper: MINDS. The Detection of 13CO2 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk
Authors: Sierra L. Grant, Ewine F. van Dishoeck, Benoît Tabone, Danny Gasman, Thomas Henning, Inga Kamp, Manuel Güdel, Pierre-Olivier Lagage, Giulio Bettoni, Giulia Perotti, Valentin Christiaens, Matthias Samland, Aditya M. Arabhavi, Ioannis Argyriou, Alain Abergel, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alessio Caratti o Garatti, Vincent Geers, Adrian M. Glauser, Rodrigo Guadarrama, Hyerin Jang, Jayatee Kanwar, Fred Lahuis, Maria Morales-Calderón, Michael Mueller, Cyrine Nehmé, Göran Olofsson, Eric Pantin, Nicole Pawellek, Tom P. Ray, Donna Rodgers-Lee, Silvia Scheithauer, Jürgen Schreiber, Kamber Schwarz, Milou Temmink, Bart Vandenbussche, Marissa Vlasblom, L. B. F. M. Waters, Gillian Wright, Luis Colina, Thomas R. Greve, Kay Justannont, Göran Östlin
Figure caption: The JWST-MIRI MRS spectrum for GW Lup is shown with the subbands in different colors. The Spitzer-IRS high-resolution (HR) and low-resolution (LR) data are shown for comparison.
Paper: Pointlike Sources among z > 11 Galaxy Candidates: Contaminants due to Supernovae at High Redshifts?
Authors: Haojing Yan, Lifan Wang, Zhiyuan Ma, Lei Hu
Figure caption: SED fitting results of the point-source dropouts using Type Ia supernova templates. The object IDs are given at the top of each panel. The red symbols show the photometry as in Table 1. The solid lines are the best-fit Type Ia SN templates, and the black diamonds are the synthesized magnitudes in the six NIRCam bands (indicated by the dotted lines in each panel). The legends show the time since the optical maximum (a negative value means the time before the B maximum) in the rest-frame days, the best-fit redshift, the magnitude offset from the best-fit model, and the SALT3NIR (x 1, c) parameters. Note that a positive magnitude offset means that observed SED is fainter than the template used, as defined by the equation in Section 3. The insets show how the redshift and time of SN are constrained, with the black, red, and blue contours indicating the 1σ, 2σ, and 3σ levels, respectively.
Paper: Pointlike Sources among z > 11 Galaxy Candidates: Contaminants due to Supernovae at High Redshifts?
Authors: Haojing Yan, Lifan Wang, Zhiyuan Ma, Lei Hu
Figure caption: Similar to Figure 1, but for the two point-source F200W dropouts in the Y23 sample (among 15 in total). The images used for the profile fitting are outlined by the orange (for F277W) and red (for F356W) boxes. F200DA-033 also satisfies the point-source criteria in F444W, which is not shown due to the limited space.
Paper: Pointlike Sources among z > 11 Galaxy Candidates: Contaminants due to Supernovae at High Redshifts?
Authors: Haojing Yan, Lifan Wang, Zhiyuan Ma, Lei Hu
Figure caption: Similar to Figure 1, but for the only object in the new F356W dropout sample truncated at m 444 ≤ 29.0 mag. The F444W image (outlined by the purple box) of this object satisfies our point-source criteria.
Paper: Pointlike Sources among z > 11 Galaxy Candidates: Contaminants due to Supernovae at High Redshifts?
Authors: Haojing Yan, Lifan Wang, Zhiyuan Ma, Lei Hu
Figure caption: Similar to Figure 1, but for the one point-source F277W dropout in the Y23 sample (among 12 in total). The images used for the profile fitting are outlined by the red (for F356W) and purple (for F444W) boxes.
Paper: Pointlike Sources among z > 11 Galaxy Candidates: Contaminants due to Supernovae at High Redshifts?
Authors: Haojing Yan, Lifan Wang, Zhiyuan Ma, Lei Hu
Figure caption: Selection of bright point sources to measure the FWHM distribution, using F200W as an example. The left panel is for module A and the right panel is for module B, respectively. The y-axis is the SExtractor MAG_AUTO magnitude, while the x-axis is the radius (in pixels; 30 mas pixel scale) of a circle aperture that contains half of the total flux. The point sources are within a narrow “belt” as outlined. The red dots are the sources retained for the statistics.
Paper: Pointlike Sources among z > 11 Galaxy Candidates: Contaminants due to Supernovae at High Redshifts?
Authors: Haojing Yan, Lifan Wang, Zhiyuan Ma, Lei Hu
Figure caption: Similar to Figure 5, but using Type IIP supernova templates and with the best-fit E(B − V) value shown in the legend.
Paper: Pointlike Sources among z > 11 Galaxy Candidates: Contaminants due to Supernovae at High Redshifts?
Authors: Haojing Yan, Lifan Wang, Zhiyuan Ma, Lei Hu
Figure caption: FWHM distribution of bright point sources as a function of image coordinates (X on the left and Y on the right, respectively). The case in F200W is shown here as an example. The top panels are for module A, and the bottom panels are for module B, respectively. The FWHM values are in pixels; the pixel scale is 30 mas.
Paper: Global Dynamic Scaling Relations of H I-rich Ultra-diffuse Galaxies
Authors: Hui-Jie Hu, 慧杰 胡, Qi Guo, 琦 郭, Zheng Zheng, 征 郑, Hang Yang, 航 杨, Chao-Wei Tsai, 肇伟 蔡, Hong-Xin Zhang, 红欣 张, Zhi-Yu Zhang, 智昱 张
Figure caption: Left: Tully–Fisher Relation: r-band absolute magnitude vs. circular velocity. Red-filled circles are 88 H I-rich ultra-diffuse galaxies (HUDGs) in this work. Dark triangles with error bars present massive galaxies from Blanton et al. (2008) with the least-square fitting shown as the black straight line. Gray dots are dwarf galaxies from α.40 (G20). The light gray line shows the incompleteness limit (see text for more details). Right: Baryonic Tully–Fisher Relation: baryonic mass vs. circular velocity. Normal galaxies are shown with gray symbols, and HUDGs are shown with color-filled circles. The gray dots are G20 dwarf galaxies with number density contours shown in gray lines. Gray diamonds, gray right triangles, and gray down-triangles are taken from Little Things (Oh et al. 2015) and SHIELD (McNichols et al. 2016) and FIGGS (Begum et al. 2008). The gray star is Leo P (McQuinn et al. 2015). Blue (NGC1052-DF2, van Dokkum et al. 2018), and yellow (NGC1052-DF4, van Dokkum et al. 2019) crosses are the dark matter–deficient UDGs with the upper limits shown with the arrows. Green-filled circles are HUDGs taken from ALFALFA α.40 (He et al. 2019), blue-filled circles are HUDGs using VLA (Mancera Piña et al. 2019), yellow-filled circles are HUDGs observed with GBT (Karunakaran et al. 2020) and the blue-filled circle is the UGC 2162 (Sengupta et al. 2019). Gray hollow squares are for SPARC massive galaxies (Lelli et al. 2016) for which the least-square fitting is presented with the black dashed line. The blue dashed line is the best linear fit for edge-on gas-dominated ALFA galaxies (Papastergis et al. 2016). Gray dashed line indicated universal (f bary = 0.157) baryonic mass within M 200 (McGaugh 2012).
Paper: Global Dynamic Scaling Relations of H I-rich Ultra-diffuse Galaxies
Authors: Hui-Jie Hu, 慧杰 胡, Qi Guo, 琦 郭, Zheng Zheng, 征 郑, Hang Yang, 航 杨, Chao-Wei Tsai, 肇伟 蔡, Hong-Xin Zhang, 红欣 张, Zhi-Yu Zhang, 智昱 张
Figure caption: Panels (a) and (b): Tully–Fisher and baryonic Tully–Fisher relations in TNG50 simulation. Gray dots and blue squares are isolated H I-rich dwarf galaxies and H I-rich ultra-diffuse galaxies (HUDGs) in the TNG50 simulation. Red circles are HUDGs in α.100. The black line in panel (a) is the best fit of massive galaxies (same as the left panel of Figure 1). Black and blue dashed lines in panel (b) are the fittings of massive galaxies from observations (same color coding as the right panel of Figure 1). Panel (c): gas fraction dependence of BTFR. Dots are dwarf galaxies from TNG50. Different colors present galaxies with different gas fractions, as denoted by the color bar in the right bottom corner. Panel (d): gas fraction vs. circular velocity. HUDGs in TNG50 have higher gas fractions by selection.
Paper: Global Dynamic Scaling Relations of H I-rich Ultra-diffuse Galaxies
Authors: Hui-Jie Hu, 慧杰 胡, Qi Guo, 琦 郭, Zheng Zheng, 征 郑, Hang Yang, 航 杨, Chao-Wei Tsai, 肇伟 蔡, Hong-Xin Zhang, 红欣 张, Zhi-Yu Zhang, 智昱 张
Figure caption: Upper: H I mass vs. circular velocity. The blue and black dashed lines are the best linear fit for massive galaxies with the same color coding as those in Figure 1. Gray dots are dwarf galaxies from G20. Red-filled circles are our 88 H I-rich ultra-diffuse galaxies (HUDGs). Lower: gas fraction vs. circular velocity. The horizontal line denotes the 1:1 ratio between H I mass and stellar mass. In general HUDGs have higher gas fraction than normal dwarf galaxies.
Paper: Global Dynamic Scaling Relations of H I-rich Ultra-diffuse Galaxies
Authors: Hui-Jie Hu, 慧杰 胡, Qi Guo, 琦 郭, Zheng Zheng, 征 郑, Hang Yang, 航 杨, Chao-Wei Tsai, 肇伟 蔡, Hong-Xin Zhang, 红欣 张, Zhi-Yu Zhang, 智昱 张
Figure caption: Distance vs. heliocentric velocity for 88 H I-rich UDGs. The blue (green) crosses are distances inferred from TFR (BTFR). Black dots are distances taken from the ALFALFA catalog, and the red line indicates the Hubble flow distance.
Paper: Global Dynamic Scaling Relations of H I-rich Ultra-diffuse Galaxies
Authors: Hui-Jie Hu, 慧杰 胡, Qi Guo, 琦 郭, Zheng Zheng, 征 郑, Hang Yang, 航 杨, Chao-Wei Tsai, 肇伟 蔡, Hong-Xin Zhang, 红欣 张, Zhi-Yu Zhang, 智昱 张
Figure caption:  w 20 vs. w 50. Left: both values are taken from α.100 Right: w 50 are taken from α.100, red dots are the reprocessed values for our method.
Paper: Global Dynamic Scaling Relations of H I-rich Ultra-diffuse Galaxies
Authors: Hui-Jie Hu, 慧杰 胡, Qi Guo, 琦 郭, Zheng Zheng, 征 郑, Hang Yang, 航 杨, Chao-Wei Tsai, 肇伟 蔡, Hong-Xin Zhang, 红欣 张, Zhi-Yu Zhang, 智昱 张
Figure caption: Significance of the deviation of H I-rich ultra-diffuse galaxies: deviation significance in BTFR vs. in TFR. The significance histograms of TFR (black) and BTFR (red) are shown on the upper and right sides of the figure, with the median values as shown with black/red lines. The significance is calculated according to the scatter of the G20 dwarf with ﹩1.6\lt \mathrm{log}{V}_{{\rm{H}}\,{\rm\small{I}}}\lt 2.1﹩ in the TFR and BTFR, respectively.
Paper: Global Dynamic Scaling Relations of H I-rich Ultra-diffuse Galaxies
Authors: Hui-Jie Hu, 慧杰 胡, Qi Guo, 琦 郭, Zheng Zheng, 征 郑, Hang Yang, 航 杨, Chao-Wei Tsai, 肇伟 蔡, Hong-Xin Zhang, 红欣 张, Zhi-Yu Zhang, 智昱 张
Figure caption: Stellar mass Tully–Fisher Relation: symbol types and colors are the same coding as those in Figure 1. The dashed line denotes the best fit of the SPARC galaxies.