adsabs/AstroCLIMB huggingface dataset:
Paper: MHD Simulation of Homologous Eruptions from Solar Active Region 10930 Caused by Sunspot Rotation
Authors: Xinyi Wang, Chaowei Jiang, Xueshang Feng, Aiying Duan, Xinkai Bian
Figure caption: The magnetic evolution of P1. (A) Time series pictures of the exchanged field lines formed by reconnection in P1-CS. The color of the field lines denotes the value of the nonlinear force-free factor defined as α =  J  ·  B /B 2. The background shows the sunspot distribution at the photosphere. (B) Evolution of the isosurface of J/B = 8.7 × 10−2 Mm−1, which represents the current layer in different stages. (C) Slices of QSLs. (D) Slices of the current layer. The initial field has no obvious current so the first column is used to label the position of the slices in (C), (D), and (E). (E) Outflows at the position of the current layer in (D). (F), (G), and (H) have the same meaning as (C), (D), and (E), respectively, but at a different slice as labeled by the first column of (G). Rows (D) and (E) are shown at the top-left and the bottom-left panels in the animation of Figure 5.
Paper: MHD Simulation of Homologous Eruptions from Solar Active Region 10930 Caused by Sunspot Rotation
Authors: Xinyi Wang, Chaowei Jiang, Xueshang Feng, Aiying Duan, Xinkai Bian
Figure caption: The trigger process of P2. Positions of all slices in (C), (D), and (E) are the same as in the first column of Figure 6(G). (A) Top view of five bunches of magnetic field lines with fixed negative footpoints. (B) Side view of 3D magnetic field lines. (C) Slices of the current layer. (D) Outflows by slow reconnection at the position of the current layer in (C). (E) Side QSLs’ evolution of P2. (F) Isosurface of J/B = 8.7 × 10−2Mm−1. Row (A) is shown at the top-right panel, and rows (C) and (D) are shown at the top-left and the bottom-left panels in the animation of Figure 5, respectively.
Paper: MHD Simulation of Homologous Eruptions from Solar Active Region 10930 Caused by Sunspot Rotation
Authors: Xinyi Wang, Chaowei Jiang, Xueshang Feng, Aiying Duan, Xinkai Bian
Figure caption: Magnetic evolution of E2. All settings are the same as in Figure 7. Row (A) is shown at the top-right panel, and rows (C) and (D) are shown at the top-left and the bottom-left panels in the animation of Figure 5.
Paper: MHD Simulation of Homologous Eruptions from Solar Active Region 10930 Caused by Sunspot Rotation
Authors: Xinyi Wang, Chaowei Jiang, Xueshang Feng, Aiying Duan, Xinkai Bian
Figure caption: (A) The first column shows the MFR is located on the isosurface of J/B = 8.7 × 10−2Mm−1. The second to fourth columns denote the different slices of the outflow distribution. The color of the isosurface and field lines has the same meaning as in previous figures. (B) QSL of the xy plane at the altitude where it intersects with the isosurface in the first column of (A). Four images in order are at t = 0, before P2, E1 and E2 respectively.
Paper: MHD Simulation of Homologous Eruptions from Solar Active Region 10930 Caused by Sunspot Rotation
Authors: Xinyi Wang, Chaowei Jiang, Xueshang Feng, Aiying Duan, Xinkai Bian
Figure caption: Magnetic evolution of E1. All settings are the same as in Figure 7. Row (A) is shown at the top-right panel, and rows (C) and (D) are shown at the top-left and the bottom-left panels in the animation of Figure 5.
Paper: MHD Simulation of Homologous Eruptions from Solar Active Region 10930 Caused by Sunspot Rotation
Authors: Xinyi Wang, Chaowei Jiang, Xueshang Feng, Aiying Duan, Xinkai Bian
Figure caption: Comparison of the simulation results with the observation. (E1) In order are the field lines, XRT sigmoid, and the synthetic image of the coronal emission from the current density respectively before the first eruption. (E2) Same as E1 but before the second eruption.
Paper: MHD Simulation of Homologous Eruptions from Solar Active Region 10930 Caused by Sunspot Rotation
Authors: Xinyi Wang, Chaowei Jiang, Xueshang Feng, Aiying Duan, Xinkai Bian
Figure caption: Hα ribbon images taken from SOT/BFI. (A) The Hα brightening at the similar location to P1-CS. (B) The Hα brightening at the similar location to P2-QSL. (C) Same as (B) but at a different time.
Paper: The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). IV. Star Cluster Catalog
Authors: L. Clifton Johnson, Tobin M. Wainer, Estephani E. TorresVillanueva, Anil C. Seth, Benjamin F. Williams, Meredith J. Durbin, Julianne J. Dalcanton, Daniel R. Weisz, Eric F. Bell, Puragra Guhathakurta, Evan Skillman, Adam Smercina
Figure caption: Left: f consensus and ﹩{\overline{f}}_{\mathrm{cluster}}﹩ user metric scores used for weighting. Circular points represent metrics for individuals with >20 classifications; point shading denotes the volunteer classification count, where darker colors highlight individuals with more classifications. Star markers represent the average metrics for a group of users, binned in groups according to classification count. The blue dashed line represents the maximum ﹩{\overline{f}}_{\mathrm{cluster}}﹩ a volunteer can achieve based on the fraction of high-quality consensus clusters identified. Right: star markers correspond to the same binned user groups presented in the left panel, but now showing the average number of classifications for each group on the x-axis. The red number next to each star is the number of users represented in each respective bin. For volunteers with <20 classifications (gray shaded region) users were weighted according to aggregate user metric values calculated for the binned group rather than using individual values.
Paper: The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). IV. Star Cluster Catalog
Authors: L. Clifton Johnson, Tobin M. Wainer, Estephani E. TorresVillanueva, Anil C. Seth, Benjamin F. Williams, Meredith J. Durbin, Julianne J. Dalcanton, Daniel R. Weisz, Eric F. Bell, Puragra Guhathakurta, Evan Skillman, Adam Smercina
Figure caption: Top: catalog completeness vs. contamination for the original, unweighted sample (dashed black line), and the optimal user weighting system (solid black line). The orange dashed line represents the d optimal threshold, where d optimal is the distance from this point to the bottom right corner of the plot. The green line shows the adopted threshold chosen to reduce catalog contamination. Bottom: catalog completeness vs. f cluster,W, which provides reference to where each threshold is drawn.
Paper: The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). IV. Star Cluster Catalog
Authors: L. Clifton Johnson, Tobin M. Wainer, Estephani E. TorresVillanueva, Anil C. Seth, Benjamin F. Williams, Meredith J. Durbin, Julianne J. Dalcanton, Daniel R. Weisz, Eric F. Bell, Puragra Guhathakurta, Evan Skillman, Adam Smercina
Figure caption: Classification statistics of individual LGCS users, sorted in decreasing order of the total submitted classifications. Top: the cumulative fraction of the LGCS’s ∼269,000 classifications. Bottom: the number of classifications submitted by the Nth ranked volunteer. The red dashed–dotted lines illustrate that 50% of all the classifications were performed by the 50 most active volunteers, who each contributed at least 1267 classifications. The blue dashed–dotted lines illustrate that 90% of all classifications were performed by 463 volunteers who each contributed at least 62 classifications.
Paper: The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). IV. Star Cluster Catalog
Authors: L. Clifton Johnson, Tobin M. Wainer, Estephani E. TorresVillanueva, Anil C. Seth, Benjamin F. Williams, Meredith J. Durbin, Julianne J. Dalcanton, Daniel R. Weisz, Eric F. Bell, Puragra Guhathakurta, Evan Skillman, Adam Smercina
Figure caption: Weighted and unweighted f cluster values are plotted for the subset of expert-ranked clusters. The blue dots are expert-identified good clusters, and the red dots are expert-identified contaminants. The dashed green line represents the f cluster,W catalog threshold of 0.674, while the orange dashed line represents the f cluster,W catalog threshold of 0.568. We prefer the higher adopted f cluster,W threshold as it rejects a larger number of expert-identified bad cluster candidates, as seen by the larger number of red points that that fall below the green horizontal line.
Paper: The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). IV. Star Cluster Catalog
Authors: L. Clifton Johnson, Tobin M. Wainer, Estephani E. TorresVillanueva, Anil C. Seth, Benjamin F. Williams, Meredith J. Durbin, Julianne J. Dalcanton, Daniel R. Weisz, Eric F. Bell, Puragra Guhathakurta, Evan Skillman, Adam Smercina
Figure caption: Screenshot of the LGCS annotation interface.
Paper: The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). IV. Star Cluster Catalog
Authors: L. Clifton Johnson, Tobin M. Wainer, Estephani E. TorresVillanueva, Anil C. Seth, Benjamin F. Williams, Meredith J. Durbin, Julianne J. Dalcanton, Daniel R. Weisz, Eric F. Bell, Puragra Guhathakurta, Evan Skillman, Adam Smercina
Figure caption: Spatial distribution of PHATTER star clusters (blue) overlaid on a F475W survey-wide mosaic image.
Paper: The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). IV. Star Cluster Catalog
Authors: L. Clifton Johnson, Tobin M. Wainer, Estephani E. TorresVillanueva, Anil C. Seth, Benjamin F. Williams, Meredith J. Durbin, Julianne J. Dalcanton, Daniel R. Weisz, Eric F. Bell, Puragra Guhathakurta, Evan Skillman, Adam Smercina
Figure caption: Distribution of f cluster values for our full sample of cluster candidates.
Paper: 2D and Slab Turbulent Cascade Rates in the Inner Heliosphere
Authors: L. Adhikari, G. P. Zank, L.-L. Zhao, D. Telloni
Figure caption: Comparison between the theoretical (2D, slab, and 2D+slab), and observed (2D, slab, and total transverse) turbulent cascade rates of the total turbulence energy (a), cross helicity (b), outward Elsässer energy (c), inward Elsässer energy (d), fluctuating magnetic energy density (e), and fluctuating kinetic energy (f) as a function of heliocentric distance. The solid black curve is the theoretical 2D turbulent cascade rate, the dashed black curve is the theoretical slab turbulent cascade rate, and the dashed–dotted–dashed is the theoretical 2D+slab turbulent cascade rate. Green stars denote total observed transverse turbulent cascade rates, red dots the observed 2D turbulent cascade rate, and blue dots the observed slab turbulent cascade rate.
Paper: 2D and Slab Turbulent Cascade Rates in the Inner Heliosphere
Authors: L. Adhikari, G. P. Zank, L.-L. Zhao, D. Telloni
Figure caption: Comparison between the theoretical and observed 2D and slab total turbulent energy (a), normalized cross helicity (b), normalized residual energy (c), outward and inward Elsässer energies (d) and (e), and the correlation lengths corresponding to outward and inward Elsässer energies (f) and (g) as a function of heliocentric distance. The solid red curve, and red and cyan scatter plots denote the theoretical and observed 2D component. The solid blue curve, and blue and black scatter plots denote the theoretical and observed slab component (reproduced from Adhikari et al. 2022).
Paper: 2D and Slab Turbulent Cascade Rates in the Inner Heliosphere
Authors: L. Adhikari, G. P. Zank, L.-L. Zhao, D. Telloni
Figure caption: (a) Histogram of the angle between the mean solar wind speed and mean magnetic field (θ UB) during the period 2018 November 13 (or DOY 317) measured by PSP at ∼66.3 R ⊙. The transverse turbulent cascade rate of the transverse total turbulent energy (b), transverse cross helicity (c), transverse energy in forward propagating modes (d), transverse energy in backward propagating modes (e), transverse fluctuating magnetic energy density (f), and transverse fluctuating kinetic energy (g) is shown as a function of θ UB. Dots denote all the transverse turbulent cascade rates, and filled circles denote the binned transverse turbulent cascade rates over a 10° width.
Paper: 2D and Slab Turbulent Cascade Rates in the Inner Heliosphere
Authors: L. Adhikari, G. P. Zank, L.-L. Zhao, D. Telloni
Figure caption: (a) Histogram of the angle between the mean solar wind speed and mean magnetic field (θ UB) during the period 2020 August 13 measured by SolO at ∼176.3 R ⊙. The format of the figure is similar to Figure 1.
Paper: A Hydro-based MCMC Analysis of SNR 0509−67.5: Revealing the Explosion Properties from Fluid Discontinuities Alone
Authors: Prasiddha Arunachalam, John P. Hughes, Luke Hovey, Kristoffer Eriksen
Figure caption: Three-color composite image of the central regions of SNR 0509−67.5. The red cross and ellipse mark the dynamical center and its total measurement uncertainty. The magenta and yellow circles respectively show the search radius for MS and WD companion candidates. The white cross and the dotted circle mark the explosion center and the error circle of SP12. The blue circles marked within the yellow circle show four potential companion candidates (star G from SP12 and three previously unidentified ones labeled AHHE1, AHHE2, and AHHE3). On the right, within the orange box, we show the epoch-1 Hα image from 2006, where we mark the five stars (green circles) with significant PM in the epoch-1 and epoch-2 Hα images. The PMs are marked with green vectors whose lengths are scaled by a factor of 20 (only a factor of 5 in the zoomed color image). The star with the largest PM is the red star (star M from SP12) moving at 0.″01 yr−1. The keen reader will note that the red star in the composite image (from 2010) is slightly offset from the location of the green circle (which marks the star’s location in 2006). This is consistent with the magnitude and direction of the red star’s PM.
Paper: A Hydro-based MCMC Analysis of SNR 0509−67.5: Revealing the Explosion Properties from Fluid Discontinuities Alone
Authors: Prasiddha Arunachalam, John P. Hughes, Luke Hovey, Kristoffer Eriksen
Figure caption: Corner plot showing the posterior distributions of the MCMC runs that fit for the explosion energy (E 51), for the two cases of γ eff = 5/3, 4/3 ((a) and (b), respectively). The parameters are highly sensitive to γ eff, as reflected in their estimated values.
Paper: TIC 114936199: A Quadruple Star System with a 12 Day Outer-orbit Eclipse
Authors: Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Veselin B. Kostov, Guillermo Torres, Rahul Jayaraman, David W. Latham, Hana Kučáková, Zoltán Garai, Theodor Pribulla, Andrew Vanderburg, Ethan Kruse, Thomas Barclay, Greg Olmschenk, Martti H. K. Kristiansen, Robert Gagliano, Thomas L. Jacobs, Daryll M. LaCourse, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Allan R. Schmitt
Figure caption: Additional extra eclipses in the 21st century. Vertical lines indicate time breaks.
Paper: TIC 114936199: A Quadruple Star System with a 12 Day Outer-orbit Eclipse
Authors: Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Veselin B. Kostov, Guillermo Torres, Rahul Jayaraman, David W. Latham, Hana Kučáková, Zoltán Garai, Theodor Pribulla, Andrew Vanderburg, Ethan Kruse, Thomas Barclay, Greg Olmschenk, Martti H. K. Kristiansen, Robert Gagliano, Thomas L. Jacobs, Daryll M. LaCourse, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Allan R. Schmitt
Figure caption: SED fit to 19 spectral fluxes that have been archived for TIC 114936199 (Ochsenbein et al. 2000). The model curves, color-coded for the contributions from the individual stars and the total flux, are from BT-Settl stellar atmospheres models (Allard 2014) of solar composition.
Paper: Fan-beamed X-Ray Emission from 1 to above 130 keV from the Ultraluminous X-Ray Pulsar RX J0209.6-7427 in the Small Magellanic Cloud
Authors: X. Hou, M. Y. Ge, L. Ji, S. N. Zhang, Y. You, L. Tao, S. Zhang, R. Soria, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: The hardness–intensity diagram of RX J0209.6−7427, where the hardness is defined as the count rate ratio of 2–10 to 0.5–2 keV observed with NICER. We fitted the HID with broken red lines, which results in two turning points. The two dashed black lines represent luminosities of the turning points, i.e., (0.57 ± 0.01) × 1038 and (3.02 ± 0.02) × 1038 erg s−1. All the error bars are given at the 68% confidence level.
Paper: Fan-beamed X-Ray Emission from 1 to above 130 keV from the Ultraluminous X-Ray Pulsar RX J0209.6-7427 in the Small Magellanic Cloud
Authors: X. Hou, M. Y. Ge, L. Ji, S. N. Zhang, Y. You, L. Tao, S. Zhang, R. Soria, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: The long-term luminosity evolution of RX J0209.6−7427 during its outburst in 2019. The orange (dashed) and green (dashed–dotted) lines represent the times of NuSTAR and Insight-HXMT observations, respectively.
Paper: Fan-beamed X-Ray Emission from 1 to above 130 keV from the Ultraluminous X-Ray Pulsar RX J0209.6-7427 in the Small Magellanic Cloud
Authors: X. Hou, M. Y. Ge, L. Ji, S. N. Zhang, Y. You, L. Tao, S. Zhang, R. Soria, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: The spin evolution of RX 0209.6−7427 with time using NICER data. The blue and green points represent the observed spin frequency and that with orbital correction, respectively.
Paper: The Chocolate Chip Cookie Model: Dust Geometry of Milky Way–like Disk Galaxies
Authors: Jiafeng Lu, 家风 卢, Shiyin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Zhengyi Shao, 正义 邵, Jinliang Hou, 金良 侯, Xianzhong Zheng, 宪忠 郑
Figure caption: Inclination-dependent Hα flux and r-band fiber magnitude explained by the CCC model and aperture effect. Top panel: observed median fiber magnitude in θ bins (dots), attenuated central surface brightness predicted by the CCC model (dashed line), aperture-corrected fiber magnitude after applying aperture corrections for the model galaxy with R a/h g = 10 (solid line). Middle panel: observed median Hα flux in θ bins (dots), attenuated central nebular line fluxes predicted by the CCC model (dashed line), aperture-corrected nebular line fluxes after applying aperture corrections for three model galaxies with different physical sizes (solid lines, different colors represent different h g values). Bottom panel: projection of a double-exponential disk into a fiber with radius R a (2.2 kpc) at different inclinations. The three solid lines show the projected area S as a function of the disk inclinations for three model galaxies, which are all set to unit value at θ = 0°. The three schematic icons show the projection of a model galaxy with a scale length of 3.2 kpc and a scale height of 0.2 kpc into the fiber aperture (2.2 kpc) for face-on (case I), edge-on (case II), and critical (case III) inclinations, respectively.
Paper: The Chocolate Chip Cookie Model: Dust Geometry of Milky Way–like Disk Galaxies
Authors: Jiafeng Lu, 家风 卢, Shiyin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Zhengyi Shao, 正义 邵, Jinliang Hou, 金良 侯, Xianzhong Zheng, 宪忠 郑
Figure caption: Distributions of nebular color excess E g and stellar color excess E s as functions of the disk inclination θ. Panel (a): Joint distribution map of E g and E s of our sample galaxies, where θ is indicated by the color. The black line shows the regression line with forced zero intercept, E g = 0.4E s. Panel (b): E s as a function of θ, where the median of E s distribution at each θ bin is shown as square dots connected with a solid line and the 16th and 84th percentiles are indicated by two solid curves. Panel (c): E g as a function of θ; the same structure as panel (b).
Paper: The Chocolate Chip Cookie Model: Dust Geometry of Milky Way–like Disk Galaxies
Authors: Jiafeng Lu, 家风 卢, Shiyin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Zhengyi Shao, 正义 邵, Jinliang Hou, 金良 侯, Xianzhong Zheng, 宪忠 郑
Figure caption: Modeling of the E g–θ and E s–θ relations with the Chocolate Chip Cookie (CCC) model. Panel (a) : schematic map of the CCC model, where R g, h g, R s, h s are the scale length and scale height of the clumpy nebular disk and diffuse ISM disk, respectively, and τ cl is the optical depth of each individual clump. The dashed arrow line shows the off-axis effect of a line of sight, where the stellar emission has not been extincted by the nebular disk (see Section 4.4 for detail). Panel (b): the corner plot of the MCMC fitting for the six free model parameters (Table 1) of the CCC model, where the best fittings of E g–θ and E s–θ relations are inserted at the top right corner of this panel.
Paper: The Chocolate Chip Cookie Model: Dust Geometry of Milky Way–like Disk Galaxies
Authors: Jiafeng Lu, 家风 卢, Shiyin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Zhengyi Shao, 正义 邵, Jinliang Hou, 金良 侯, Xianzhong Zheng, 宪忠 郑
Figure caption: Modeling of the inclination dependence of E s and E g with simple models. Panel (a): uniform mixture model for E s. The small dots show the observed median E s–θ relation, while the solid line shows the best model fitting presented in Section 3.1. Panel (b): screen model for E g. The small dots show the observed median E g–θ relation, while the solid line shows the best model fitting presented in Section 3.2. The schematic diagram of each model and the values of the best model parameters are inserted in each panel.
Paper: Fan-beamed X-Ray Emission from 1 to above 130 keV from the Ultraluminous X-Ray Pulsar RX J0209.6-7427 in the Small Magellanic Cloud
Authors: X. Hou, M. Y. Ge, L. Ji, S. N. Zhang, Y. You, L. Tao, S. Zhang, R. Soria, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: Illustration of the AC and the emission region of photons with different energies. Low- and intermediate-energy photons (e.g., 1–40 keV) may be emitted in both pencil beam and the upper fan beam, but high-energy photons (e.g., from about 50 to above 130 keV) can only be emitted in the lower fan beam and also reflected from the surface of the neutron star; the reflected flux should have nonspin or very low spin modulation, thus reducing the PF in the highest energy bands. H is the height of the radiation-dominated shock, and dr is the thickness of the radiation shell of the fan beam. See Basko & Sunyaev (1976) for detailed description of the AC.
Paper: Fan-beamed X-Ray Emission from 1 to above 130 keV from the Ultraluminous X-Ray Pulsar RX J0209.6-7427 in the Small Magellanic Cloud
Authors: X. Hou, M. Y. Ge, L. Ji, S. N. Zhang, Y. You, L. Tao, S. Zhang, R. Soria, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: The cross correlation from 1,000,000 simulations of two noncorrelated profiles and the corresponding chance probability. The dashed vertical and horizontal lines denote the cross correlation and chance probability for the HE 130–180 keV profile, respectively. Note that the chance probability for a 3σ significance is 0.0027. The significance of the HE 130–180 keV profile is 4.3σ.
Paper: The Chocolate Chip Cookie Model: Dust Geometry of Milky Way–like Disk Galaxies
Authors: Jiafeng Lu, 家风 卢, Shiyin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Zhengyi Shao, 正义 邵, Jinliang Hou, 金良 侯, Xianzhong Zheng, 宪忠 郑
Figure caption: (a) Histograms of disk inclinations. The dotted line shows all the SFGs in MGS, while the sold line represents SFGs at z < 0.1. Both histograms are normalized to the unit area. (b) Density map of the stellar mass and disk inclination of the SFGs at z < 0.1, where the black dots represent the median stellar mass at different inclinations.
Paper: The Chocolate Chip Cookie Model: Dust Geometry of Milky Way–like Disk Galaxies
Authors: Jiafeng Lu, 家风 卢, Shiyin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Zhengyi Shao, 正义 邵, Jinliang Hou, 金良 侯, Xianzhong Zheng, 宪忠 郑
Figure caption: Absolute r-band fiber magnitude (top panel) and H α  flux (bottom panel) as a function of the disk inclination θ for our MW-like SFGs, where the number density of the sample galaxies in the parameter space are color coded. The median values at different inclinations are shown as solid dots in each panel.