adsabs/AstroCLIMB huggingface dataset:
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: Infrared images and [C II] and CO spectra highlighting the blueshifted clump described in Section 4.4, the only shell fragment detected in CO, on the edge of the opening of the western cavity. This clump links low-velocity emission from within the western cavity with a bright-rimmed cloud in high spatial resolution images, indicating that the clump is embedded within the foreground shell like those found in Orion by J. R. Goicoechea et al. (2020). The two images on top show a zoom-in on the blueshifted clump at 8 and 160 μm. The three circles mark three positions from which we extract spectra. One position lies toward the clump, and two lie to each side for comparison. The contours are [C II] (left) and 12CO(J = 3–2) (right) intensities integrated between VLSR = 7–10 km s−1. The spectra on the bottom are extracted at the positions numbered 1–3. [C II] spectra and 12CO (J = 1–0) and (J = 3–2) spectra are shown. We show the Nobeyama CO (J = 1–0) observations since the 20″ beam is similar to that of the APEX CO (J = 3–2) data. The [C II] contours and spectra are both shown at the CO (J = 3–2) beam. A clear line associated with the blueshifted clump appears around 8–9 km s−1, well separated from the diffuse 20–25 km s−1 emission. In Section 6.4, we measure the clump’s atomic gas mass to be ∼20 M⊙.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: Left panel: color composite showing [C II]-integrated intensities in three velocity intervals. Blue, green, and red show VLSR = 6–11, 21–27, and 35–40 km s−1, respectively. The blue and red velocity intervals highlight the detected foreground and background fragments of the expanding shell. Right panel: the same field at 160 μm for reference. The lobes, which extend outside the field shown here, are marked in both panels with white- or black-dashed lines near the corners of the field. The white circle in both panels shows the area from which the spectrum in Figure 16 is extracted.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: Averaged [C II], 12CO(J = 3–2), and 13CO(J = 3–2) spectra from within regions outlined on the VLSR = 10–27 km s−1 integrated [C II] intensity image in the center. White crosses show early-type members of NGC 6611, and the 15﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 [C II] beam is shown in the lower right corner. Spectra from the largest circle are shown above the image, and spectra from the numbered regions are shown in the panels below the image. 13CO spectra are shown multiplied by 3 for better visibility. Vertical lines mark every 2 km s−1 between 17–27 km s−1. This conveniently marks the Northern Cloud near 19 km s−1, the diffuse CO component at 21–23 km s−1, and the natal cloud emission near 25 km s−1.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: [C II] and 12CO(J = 3–2) line channel maps. All maps are on the same linear scale shown on the color bars to the right; two different color maps are used to distinguish [C II] from CO. Black crosses in the bottom left panel show early-type members of NGC 6611, and the beam is shown in the lower right corner of each map. All data are binned to 2 km s−1 channels to increase the signal-to-noise ratio. The [C II] data are convolved here to a 30″ beam. 12CO(J = 3–2) are presented at the original ∼20″ resolution.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: Infrared and millimeter view of the N19 ring. The color composite shown in both panels is 350 μm in red, 160 μm in green, and 8 μm in blue. Contours show [C II] (left) and 12CO(J = 3–2) (right) integrated between VLSR = 17–21 km s−1. [C II] contours mark 18, 24, 30, 36, 42, and 48 K km s−1. CO contours mark 20, 30, 40, 50, 60, 70, and 80 K km s−1. The white and green circles in the left panel mark the areas from which the spectra in Figure 13 are taken. The blue arrow in both frames shows the path for the PV diagram in Figure 14.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: PV diagram showing [C II] in color image and 13CO(J = 3–2) in contours. The N19 ring appears in [C II] VLSR < 21 km s−1, and the expanding 4 km s−1 foreground shell signature is marked with a white half-ellipse. The path along which this PV cut is taken is shown as a black arrow in Figure 12. Emission VLSR > 23 km s−1 is mostly associated with the Bright Northern Ridge, and the VLSR > 30 km s−1 emission is unrelated to N19, as discussed in the text.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: Color composites showing [C II] and 12CO(J = 3–2) integrated within four different velocity intervals. Velocity intervals are labeled in the top left corners. CO is shown in red, and [C II] in cyan.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: [C II] spectra toward and off the edge of the N19 PDR shell showing possible signs of self-absorption. The black spectrum toward the shell edge dips near 19 km s−1, and the nearby Northern Cloud spectrum in green peaks close to that velocity. The black and green spectra are taken from the white and green circles, respectively, marked in Figure 12.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: Velocity RGB composites made from [C II] (left) and 12CO(J = 3–2) (right) observations. Blue, green, and red show VLSR = 10–21, 21–23, and 23–27 km s−1, respectively.
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. II. Correlation between Velocity Map Morphology, Star Formation, and Metallicity in Regular Disk Galaxies
Authors: Shuai Feng, 帅 冯, Shiyin Shen, 世 银 沈, Yanmei Chen, 燕 梅 陈, Y. Sophia Dai, 昱 戴, Jun Yin, 君 尹, Wenyuan Cui, 文 元 崔, Mengting Ju, 梦 婷 居, Linlin Li, 林 林 李
Figure caption: Dependence of the SFMS (top) and the MZR (bottom) on velocity map morphology. In the left panels, colors represent ﹩{\rm{\Delta }}{\mathrm{log}}{\overline{v}}_{\,\rm{asym}\,}﹩, while in the right panels, colors represent ﹩{\rm{\Delta }}{\mathrm{log}}{\overline{v}}_{{a}_{1}/{b}_{1}}﹩. The dashed lines mark the best-fitting trend of SFMS or MZR, and the dotted lines indicate the 25th and 75th percentiles.
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. II. Correlation between Velocity Map Morphology, Star Formation, and Metallicity in Regular Disk Galaxies
Authors: Shuai Feng, 帅 冯, Shiyin Shen, 世 银 沈, Yanmei Chen, 燕 梅 陈, Y. Sophia Dai, 昱 戴, Jun Yin, 君 尹, Wenyuan Cui, 文 元 崔, Mengting Ju, 梦 婷 居, Linlin Li, 林 林 李
Figure caption: Distribution of velocity map asymmetry and H I gas content in the ﹩{\rm{\Delta }}{\mathrm{log}}{\rm{SFR}}﹩–﹩{\rm{\Delta }}{\mathrm{log}}{({\rm{O}}/{\rm{H}})}_{{\rm{Re}}}﹩ plane for galaxies with H I detections. Left: colors represent ﹩{\rm{\Delta }}{\mathrm{log}}{\overline{v}}_{\,\rm{asym}\,}﹩. Right: colors represent the residual H I gas fraction, ΔfH I, i.e., the difference in H I content relative to galaxies of similar stellar mass.
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. II. Correlation between Velocity Map Morphology, Star Formation, and Metallicity in Regular Disk Galaxies
Authors: Shuai Feng, 帅 冯, Shiyin Shen, 世 银 沈, Yanmei Chen, 燕 梅 陈, Y. Sophia Dai, 昱 戴, Jun Yin, 君 尹, Wenyuan Cui, 文 元 崔, Mengting Ju, 梦 婷 居, Linlin Li, 林 林 李
Figure caption: Left: galaxies in the stellar mass–sSFR plane, color-coded by their metallicity offset from the best-fit MZR. Right: galaxies in the stellar mass–metallicity plane, color-coded by their SFR offset from the SFMS.
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. II. Correlation between Velocity Map Morphology, Star Formation, and Metallicity in Regular Disk Galaxies
Authors: Shuai Feng, 帅 冯, Shiyin Shen, 世 银 沈, Yanmei Chen, 燕 梅 陈, Y. Sophia Dai, 昱 戴, Jun Yin, 君 尹, Wenyuan Cui, 文 元 崔, Mengting Ju, 梦 婷 居, Linlin Li, 林 林 李
Figure caption: Cumulative distributions of ﹩{\rm{\Delta }}{\mathrm{log}}{\overline{v}}_{\,\rm{asym}\,}﹩ (left) and ﹩{\rm{\Delta }}{\mathrm{log}}{\overline{v}}_{{a}_{1}/{b}_{1}}﹩ (right) for galaxies located at different positions relative to the SFMS (top panels) and the MZR (bottom panels). The cumulative distributions are constructed from the individual distribution functions of ﹩{\rm{\Delta }}{\mathrm{log}}{\overline{v}}_{\,\rm{asym}\,}﹩ and ﹩{\rm{\Delta }}{\mathrm{log}}{\overline{v}}_{{a}_{1}/{b}_{1}}﹩ derived for each galaxy.
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. II. Correlation between Velocity Map Morphology, Star Formation, and Metallicity in Regular Disk Galaxies
Authors: Shuai Feng, 帅 冯, Shiyin Shen, 世 银 沈, Yanmei Chen, 燕 梅 陈, Y. Sophia Dai, 昱 戴, Jun Yin, 君 尹, Wenyuan Cui, 文 元 崔, Mengting Ju, 梦 婷 居, Linlin Li, 林 林 李
Figure caption: The relationship between stellar mass and velocity map morphology (left, kinematic asymmetry ﹩{\mathrm{log}}{\overline{v}}_{\,\rm{asym}\,}﹩; right, first-order term ratio ﹩{\mathrm{log}}{\overline{v}}_{{a}_{1}/{b}_{1}}﹩). The red triangles represent the median value of the velocity map morphology parameters within the given stellar mass bin. The dashed line is a linear fit to these median values as a function of stellar mass.
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. II. Correlation between Velocity Map Morphology, Star Formation, and Metallicity in Regular Disk Galaxies
Authors: Shuai Feng, 帅 冯, Shiyin Shen, 世 银 沈, Yanmei Chen, 燕 梅 陈, Y. Sophia Dai, 昱 戴, Jun Yin, 君 尹, Wenyuan Cui, 文 元 崔, Mengting Ju, 梦 婷 居, Linlin Li, 林 林 李
Figure caption: The distribution of the offsets from the SFMS and MZR, where the colors represent ﹩{\rm{\Delta }}{\mathrm{log}}{\overline{v}}_{\,\rm{asym}\,}﹩. The left and right panels display the results of low-mass galaxies (﹩{\mathrm{log}}{M}_{\star }\lt 10.2﹩) and high-mass galaxies (﹩{\mathrm{log}}{M}_{\star }\gt 10.2﹩), respectively.
Paper: How Many Bursts Does It Take to Form a Core at the Center of a Galaxy?
Authors: Olivia Mostow, Paul Torrey, Jonah C. Rose, Alex M. Garcia, Niusha Ahvazi, Mariangela Lisanti, Nitya Kallivayalil
Figure caption: Comparison of DM density for the smooth (top panels) and bursty (bottom panels) models implemented using the modified DMO approach for a halo with mass 9.2 × 109M⊙. Left: DM mass projection made from a 30 × 30 × 30 kpc box surrounding the central halo. The halos look similar, save for their central regions. The smooth model produces a clear peak in density at the very center, while the bursty model reaches a constant density (forms a core) 2.05 kpc from the center. Right: tracer mass vs. time as well as density profiles for the smooth and bursty models. In both cases, the final stellar mass is 3.9 × 106M⊙. The tracer mass in the upper panel represents a galaxy with a smooth history, which follows the SHMR shown in black. The tracer mass evolution in the lower panel represents a galaxy that undergoes five bursts of star formation, expelling 3.6 × 107M⊙ of gas in each burst. The z = 0 DM density profiles produced from each of these models are also shown. The gray dashed line marks 2.8 times the DM particle softening, the point below which numerical effects begin to be important. The smooth model has an inner log-slope α = –1.40 when averaged over 1%–2% of the virial radius, consistent with an NFW profile. By contrast, when there are episodic bursts, we find a log-slope α = −0.63.
Paper: How Many Bursts Does It Take to Form a Core at the Center of a Galaxy?
Authors: Olivia Mostow, Paul Torrey, Jonah C. Rose, Alex M. Garcia, Niusha Ahvazi, Mariangela Lisanti, Nitya Kallivayalil
Figure caption: Comparison of the relationship between the number of bursts and both the core size (right) and inner log-slope (left) for variable (blue) vs. fixed (red) total energy transferred to the DM particles via bursty feedback for the classical dwarf galaxy. When the amount of mass expelled in each burst is constant, we find that the profile simply becomes more cored as we increase the number of bursts (increasing the total energy transferred). If, instead, the mass expelled in each burst is varied, such that the total mass expelled is constant, we find a more complex relationship. As the number of bursts is decreased, initially this leads to an increase in the core size. However, if there are fewer than five bursts, this trend reverses. The point marked with an “x” indicates that for this model, the core-Einasto fit is poor.
Paper: How Many Bursts Does It Take to Form a Core at the Center of a Galaxy?
Authors: Olivia Mostow, Paul Torrey, Jonah C. Rose, Alex M. Garcia, Niusha Ahvazi, Mariangela Lisanti, Nitya Kallivayalil
Figure caption: Left: best-fit values for the core radius rc as a function of redshift at the time at which the single outflow occurs for the UFD. The color depicts the size of the outflow in terms of the mass expelled. Notably, cores of appreciable size do not form prior to z = 5, indicating that DM cores do not easily form when bursty activity is relegated to the earliest times, even when extreme mass outflow events are considered. Right: inner DM density profile slope, α, as a function of redshift at which the single outflow occurs. The shaded band represents the expected range of slopes for an NFW profile (accounting for concentration scatter). Just as with the left panel, the upper left region is unoccupied, showing consistency between these two metrics.
Paper: How Many Bursts Does It Take to Form a Core at the Center of a Galaxy?
Authors: Olivia Mostow, Paul Torrey, Jonah C. Rose, Alex M. Garcia, Niusha Ahvazi, Mariangela Lisanti, Nitya Kallivayalil
Figure caption: Present-day density profiles for a fixed amount of total mass expelled (1.8 × 108M⊙) over time and a varied number of bursts. The black line depicts the smooth model. As the number of bursts decreases (and, therefore, the amount of mass expelled per burst increases), larger cores form. However, cores stop forming altogether when the number of bursts becomes very small (i.e., ∼one to two), despite the large amount of mass being expelled. The gray dashed line indicates the radius at which numerical softening effects begin to impact the results. Note that the results are shown for one, two, three, and five bursts (and not four).
Paper: How Many Bursts Does It Take to Form a Core at the Center of a Galaxy?
Authors: Olivia Mostow, Paul Torrey, Jonah C. Rose, Alex M. Garcia, Niusha Ahvazi, Mariangela Lisanti, Nitya Kallivayalil
Figure caption: Summary of the inner log-slopes (﹩\alpha =\tfrac{d\mathrm{log}\rho }{d\mathrm{log}r}﹩) and best-fit core radii rc for a classical dwarf galaxy as a function of number of bursts and burst mass.
Paper: On the Gravitational Collapse of Small Dust Grains in Self-gravitating Disk Structures
Authors: Hans Baehr, Ken Rice, Chao-Chin Yang, 朝欽 楊, Cassandra Hall
Figure caption: Left: kinetic power spectrum of the gas around the midplane in the simulation small_Z001 and its lower-resolution counterpart, averaged over three snapshots at t = 50 Ω−1, t = 54 Ω−1, and t = 58 Ω−1. Right: similarly, the kinetic energy spectrum of the dust particles around the midplane. The thin black line indicates a slope of k−5/3.
Paper: How Many Bursts Does It Take to Form a Core at the Center of a Galaxy?
Authors: Olivia Mostow, Paul Torrey, Jonah C. Rose, Alex M. Garcia, Niusha Ahvazi, Mariangela Lisanti, Nitya Kallivayalil
Figure caption: Comparison of the present-day DM density profile for a UFD galaxy if it has a smooth growth history (black) or forms in a single burst at z = 7 (red), resulting in the ejection of 1.4 × 104M⊙. The density profiles are both cusped, with rc = 0.07, 0.05 and α = –1.25, –1.35 for the smooth-growth and single-burst models, respectively.
Paper: Investigation on the Predictive Potentiality of Photospheric Magnetic Parameters for Distinguishing Confined from Eruptive Solar Flares
Authors: Jinhui Pan, Rui Liu
Figure caption: Example of the calculation results of all the parameters in AR 12192 (first column) and AR 12673 (second column). The top row shows the magnetograms of ARs. Red dots and dashed lines indicate the flux-weighted centers and centroid distance. Orange color indicates the PIL regions, and blue color outlines the HiFERs. The middle row shows the maps of JZ. Magenta color indicates the negative Jz, while green color represents positive Jz. The last row shows the maps of the magnetic shear. The regions where the absolute value of the magnetic field is weaker than 150 G are shown in white.
Paper: Investigation on the Predictive Potentiality of Photospheric Magnetic Parameters for Distinguishing Confined from Eruptive Solar Flares
Authors: Jinhui Pan, Rui Liu
Figure caption: Overview of the solar flare events. Red (blue) dots mark the eruptive (confined) events, which are bracketed by the 45∘ range from the central meridian. A list of the events and corresponding magnetic parameters is available as the data behind the figure. This list can also be used to derive Figures 3, 4, and 5.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Stellar Loci. IX. Estimation of Stellar Parameters from CSST-like Photometry
Authors: Xue Lu, Haibo Yuan, Kai Xiao, Bowen Huang, Ruoyi Zhang, Lin Yang, Timothy C. Beers, Shuai Xu
Figure caption: Monte Carlo simulation results for [M/H] and ﹩{\rm{log}}\,{g}﹩ estimates for stars with assumed 0.01 mag photometric errors and different parameters, as labeled in each panel. Panels from left to right: g − i from bluer to redder. The top two rows show giants with ﹩{\rm{log}}\,{g}=2﹩; the bottom two rows show dwarfs with ﹩{\rm{log}}\,{g}=4﹩. The first and third rows have [M/H] = −0.5, the second and fourth rows have [M/H] = −2.0.
Paper: Stellar Loci. IX. Estimation of Stellar Parameters from CSST-like Photometry
Authors: Xue Lu, Haibo Yuan, Kai Xiao, Bowen Huang, Ruoyi Zhang, Lin Yang, Timothy C. Beers, Shuai Xu
Figure caption: Top panels: the dependence of the (NUV − g)m (left) and (u − g)m (right) colors on [M/H], color coded by [M/H] in the color bars to the right. Bottom panels: The dependence of the (NUV − g)m (left) and (u − g)m (right) colors on log g, color coded by log g in the color bars to the right.
Paper: Stellar Loci. IX. Estimation of Stellar Parameters from CSST-like Photometry
Authors: Xue Lu, Haibo Yuan, Kai Xiao, Bowen Huang, Ruoyi Zhang, Lin Yang, Timothy C. Beers, Shuai Xu
Figure caption: NUV − g (left panels) and u − g (right panels) colors as a function of [M/H] and log g for different g − i colors as labeled on each panel. The g − i colors closely match Figure 6.
Paper: Stellar Loci. IX. Estimation of Stellar Parameters from CSST-like Photometry
Authors: Xue Lu, Haibo Yuan, Kai Xiao, Bowen Huang, Ruoyi Zhang, Lin Yang, Timothy C. Beers, Shuai Xu
Figure caption: Fitting residuals for the [Fe/H]- and log g-dependent stellar-loci based on observational data. The left six panels are for the NUV − g color, which contain the histogram distribution of fitting residuals, with the Gaussian fitting profile overplotted in black, and the NUV − g versus g − i stellar loci at different [Fe/H] values for dwarfs(﹩{\rm{log}}\,{g}=4.5﹩) and giants(﹩{\rm{log}}\,{g}=2.5﹩), and fitting residuals as a function of [Fe/H], log g, g − i, and E(B − V) with the median values and standard deviations overplotted in red. The right six panels are similar to the left ones, but for the u − g color. The points are color coded by their number density.
Paper: Stellar Loci. IX. Estimation of Stellar Parameters from CSST-like Photometry
Authors: Xue Lu, Haibo Yuan, Kai Xiao, Bowen Huang, Ruoyi Zhang, Lin Yang, Timothy C. Beers, Shuai Xu
Figure caption: Left panels: the result for photometric-metallicity estimates [M/H]. From top to bottom, the panels show histogram distributions of the residuals Δ[M/H], with the Gaussian fitting profile overplotted in black, comparison of the photometric-metallicity estimates with input values, Δ[M/H] as a function of g − i color, [M/H], and log g. Right panels: similar to the left ones but for log g. The points are color coded by their number density.
Paper: Stellar Loci. IX. Estimation of Stellar Parameters from CSST-like Photometry
Authors: Xue Lu, Haibo Yuan, Kai Xiao, Bowen Huang, Ruoyi Zhang, Lin Yang, Timothy C. Beers, Shuai Xu
Figure caption: Fitting residuals of the [Fe/H]- and log g-dependent stellar loci. The left four panels are for the NUV − g color, which contain the histogram distribution of fitting residuals, with the Gaussian fitting profile overplotted in black, and fitting residuals as a function of g − i, [M/H], and log g, with the median values and standard deviations overplotted in red. The right four panels are similar to the left ones, but for the u − g color. The points are color coded by their number density.
Paper: Stellar Loci. IX. Estimation of Stellar Parameters from CSST-like Photometry
Authors: Xue Lu, Haibo Yuan, Kai Xiao, Bowen Huang, Ruoyi Zhang, Lin Yang, Timothy C. Beers, Shuai Xu
Figure caption: The distribution of Δ[Fe/H] and ﹩{\rm{\Delta }}{\rm{log}}\,{g}﹩ in the H-R diagram. The color bars represent Δ[Fe/H] and ﹩{\rm{\Delta }}{\rm{log}}\,{g}﹩, respectively.
Paper: Stellar Loci. IX. Estimation of Stellar Parameters from CSST-like Photometry
Authors: Xue Lu, Haibo Yuan, Kai Xiao, Bowen Huang, Ruoyi Zhang, Lin Yang, Timothy C. Beers, Shuai Xu
Figure caption: Similar to Figure 5 but for results based on observational data.