adsabs/AstroCLIMB huggingface dataset:
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Decimal logarithm of black hole mass in units of solar masses computed from the C IV  λ1549−based scaling law of M19 vs. the ones computed from the relation of Vestergaard & Peterson (2006) based on FWHM H β (blue) and from the Al III FWHM following Equation (5) (black). The dotted–dashed line is the equality line. The bottom panel shows the residuals as a function of M BH. Median and SIQR of the ﹩\mathrm{log}﹩                       M BH differences ﹩\delta \mathrm{log}{M}_{\mathrm{BH}}=\mathrm{log}{M}_{\mathrm{BH}}﹩ C IV                       ﹩-\mathrm{log}{M}_{\mathrm{BH}}﹩ Al III and ﹩\delta \mathrm{log}{M}_{\mathrm{BH}}=\mathrm{log}{M}_{\mathrm{BH}}﹩ C IV                       ﹩-\mathrm{log}{M}_{\mathrm{BH}}﹩                       H β are reported in the inside caption.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption:  H β and C III] profile parameter comparison as a function of luminosity. Shown is the behavior of FWHM C III] and H β (top) and of the ratio FWHM(C III])/FWHM(H β) (bottom) as a function of ﹩\mathrm{log}L﹩ at 1700 Å. The data points are color coded on the basis of ST. As in Figure 7, the filled line traces the expected increase of the FWHM in a virialized system with ﹩{L}^{\tfrac{1}{4}}﹩. The yellow band marks the region where FWHM(C IV  λ1549)/FWHM(H β) ≈0.8 within the errors. The width of the band has been set by the median value of the uncertainty of the ratios, ±0.17. The vertical dotted lines join H β and Al III parameters for the same object.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Top panel: FWHM(C III]) vs. FWHM(H β) for the joint sample. Data points are color coded according to STs, as for Figure 3. Middle panel: FWHM ratio of C III] and H β. The median ratio ﹩{\mu }_{\tfrac{1}{2}}(r)﹩, with r = FWHM C III]/FWHM H β, and the SIQR are reported. Bottom panel: same ratio, but with the data color coded according to C III] intensity: normalized intensity >10 (red) and ≤10 (blue). Values of ﹩{\mu }_{\tfrac{1}{2}}(r)﹩ and SIQR are reported for stronger and weaker C III] emitters.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Top panel: FWHM(Al III) vs. FWHM(H β) for the joint sample. Data points are color coded according to luminosity at 1700 Å, from red (lowest; ﹩\mathrm{log}{L}_{1700}\sim 44﹩) to blue (highest, ﹩\mathrm{log}{L}_{1700}\sim 47﹩). Bottom panel: FWHM ratio of Al III and H β. The median ratios ﹩{\mu }_{\tfrac{1}{2}}r﹩ and the SIQR r are reported for more luminous (﹩\mathrm{log}L\geqslant 46﹩ [erg s−1]) and less luminous (﹩\mathrm{log}L\lt 46﹩) quasars.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Decimal logarithm of black hole mass in units of solar masses computed from the scaling law based on FWHM C III] (Equation (7)) vs. the one computed from the Al III FWHM following Equation (5). The filled line traces an unweighted least-squares fit; the dotted–dashed line is the equality line.
Paper: High-precision Multichannel Solar Image Registration Using Image Intensity
Authors: Bo Liang, Xi Chen, Lan Yu, Song Feng, Yangfan Guo, Wenda Cao, Wei Dai, Yunfei Yang, Ding Yuan
Figure caption: (a) The Hα image taken from GST at Big Bear Solar Observatory on 2012 May 22 at 17:17:01 UT. (b) The TiO image taken from GST on 2012 May 22 at 17:17:10 UT. (c) The coarse registration result using NCC and RSGD. The bright bridge in red box “B” has been aligned, but the pores in box “A” are slightly misaligned. (d) The fine registration result using MMI and Powell.
Paper: High-precision Multichannel Solar Image Registration Using Image Intensity
Authors: Bo Liang, Xi Chen, Lan Yu, Song Feng, Yangfan Guo, Wenda Cao, Wei Dai, Yunfei Yang, Ding Yuan
Figure caption: (a), (b) TiO and Hα images observed by GST on 2015 May 21 at 20:40:02 UT. The TiO is the fixed image and the Hα image is the moving image. (c) The registration result of our method. (d) The result of SIFT. (e) The result of phase correlation. (f) The result of the PB and MMI. Every registration result is superposed on the TiO image.
Paper: High-precision Multichannel Solar Image Registration Using Image Intensity
Authors: Bo Liang, Xi Chen, Lan Yu, Song Feng, Yangfan Guo, Wenda Cao, Wei Dai, Yunfei Yang, Ding Yuan
Figure caption: (a) The Hα blue-wing (100 Å) image observed by GST on 2015 July 14 at 18:15:09 UT. (b) The Hα red-wing (80 Å) image observed by GST on 2015 July 14 at 18:15:14 UT. (c) The registered red-wing image to the blue-wing image. (d) The image stitched together with the blue-wing image and the registered red-wing image. The red arrows point to the aligned features in comparison with each other.
Paper: High-precision Multichannel Solar Image Registration Using Image Intensity
Authors: Bo Liang, Xi Chen, Lan Yu, Song Feng, Yangfan Guo, Wenda Cao, Wei Dai, Yunfei Yang, Ding Yuan
Figure caption: (a), (b) The Hα blue 40 Å and 80 Å wing images observed on 2014 August 5 at 16:51:31 UT. (c)–(f) The results of our method, SIFT, phase correlation, and PB and MMI.
Paper: High-precision Multichannel Solar Image Registration Using Image Intensity
Authors: Bo Liang, Xi Chen, Lan Yu, Song Feng, Yangfan Guo, Wenda Cao, Wei Dai, Yunfei Yang, Ding Yuan
Figure caption: (a) The HMI continuum image observed by SDO/HMI on 2015 January 5 at 19:11:39 UT. (b) The TiO image observed by GST on 2015 January 5 at 19:12:43 UT. (c) The subregion marked with a gray box in panel (a). (d) An overlapped image together with the registered TiO image and panel (c). The red arrows point the image features to comparison each other.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Top panel: FWHM(Al III) vs. FWHM(H β) (full profiles) for the joint sample. Data points are color coded according to ST: A1—aquamarine; A2—blue; A3—magenta; A4—purple. Bottom: FWHM ratio between Al III and H β. The median ratio ﹩{\mu }_{\tfrac{1}{2}}(r)﹩ = FWHM Al III/FWHM H β and SIQR are reported for STs A1 and A2, and the union of A3 and A4.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Top panel: FWHM(Al III) vs. FWHM(H β) (full profiles) for the joint sample. Data points are color coded according to subsample: FOS⋆—aquamarine; HE—blue; ISAAC—magenta; WISSH—purple. Dotted–dashed line: 1:1 relation; filled line: best fit obtained using the bisector technique; dotted line: best fit using the least orthogonal distance method (Press et al. 1992). Middle panel: ratio r of FWHM Al III over FWHM H β. The average ratio ﹩\bar{r}﹩, the standard deviation σ  r , and the normalized ﹩{\chi }_{\nu }^{2}﹩ are reported. Bottom: same as the middle panel, but with an expanded scale along the y-axis.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Top-left panel: behavior of shift s * of Al III with respect to rest frame as a function of the ST. Reported values are sample medians, and error bars are SIQR. Bottom-left panel: same as the top-left panel, but for the ratio FWHM Al III over FWHM H β. Right: parameter δ(Al III) as a function of ST.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Top panel: FWHM(Al III) vs. FWHM(H β BC) for the joint sample. Data points are color coded according to ST as in Figure 3. Bottom panel: FWHM ratio between Al III and H β BC, 1/ξ Al III. The median ratio ﹩{\mu }_{\tfrac{1}{2}}(1/{\xi }_{\mathrm{Al}\,\mathrm{III}})﹩ and the SIQR are reported for STs A1 and A2, and for the union of A3 and A4, as in Figure 3.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Distribution of redshift (left) and of luminosity at 1700 Å (right) for the four subsamples considered in this paper.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Analysis of the H β spectral range (left) and of the 1900 Å blend (right), for the sources of the FOS* subsample. Abscissa scales are rest-frame wavelength in Å and radial velocity from rest frame. Ordinate scale is normalized specific flux by the value at 5100 Å and at 1700 Å. The dashed magenta lines trace the sum of all emission components of the model. The black lines identify the H β broad component H β BC (left) and Al III, Si III], and C III] (right). The blue line is the blueshifted excess in the H β profile. Green lines trace the adopted Fe II (pale) and Fe III (dark) templates. Golden lines trace narrow emission lines or line components.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Analysis of the 1900 Å blend for the extreme Population A sources with excess emission on the blue side of Al III. Abscissa scales are rest-frame wavelength in Å and radial velocity from rest-frame wavelength of C III]. Ordinate scale is normalized specific flux by the value at 1700 Å. The black lines identify Al III and Si III]. The blueshifted excess BLUE is traced by a thick blue line. Green lines trace the adopted Fe II (pale) and Fe III (dark) templates. Note that C III] emission is almost absent, as all of the emission on the red side of Si III] can be ascribed to Fe III.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Shift s of Al III vs. shift of C IV  λ1549 with respect to rest frame. Data points are identified according to the ST, with the same color-coding of Figure 3. The filled and dotted–dashed lines trace an unweighted least-squares fit and the equality line, respectively. The gray bands identify uncertainty ranges in radial velocity ±400 km s−1 where the lines are not significantly shifted. Squares refer to the c﹩\left(\tfrac{1}{2}\right)﹩ Al III in the case in which the excess emission on the blue side of Al III has been ascribed to Al III. See Section 5.3.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: The distribution of xA sources in the plane defined by the intensity ratios C III]/Si III] vs. Al III/Si III]. The area associated with xA sources is the lower left shaded box. Sources are color coded according to ST as in the previous figures.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Left: distribution of the log of parameter ﹩{ \mathcal Q }﹩ parameter for Al III (blue) and H β (red) for the joint sample considered in this paper. Right: distribution of ﹩\mathrm{log}{ \mathcal Q }﹩ differences between H β and Al III.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: The distribution of the parameter ﹩{ \mathcal A }﹩, as defined in Section 5.3, for three groups of quasars: STs A1+A2, STs A3+A4, and the six quasars with a blueshifted excess fit to the 1900 Å blend (Figure 16).
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Relation between the fractional uncertainty δFWHM/FWHM and the logarithm of parameter ﹩{ \mathcal Q }﹩. Red circles are for H β, black for Al III, and blue for C III]. The thick lines trace the relations reported in Table 3 for the FWHM of Al III (black) and C III] (blue).
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Parameter δ(Al III) as a function of luminosity. Median values are plotted for 1 dex luminosity intervals. Error bars are sample SIQR.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Analysis of H β and of the 1900 Å blend for Population A sources of the ISAAC sample. Meaning of color-coding is the same as in the previous figures in this appendix.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption: Analysis of H β and of the 1900 Å blend for Population A sources of the WISSH sample. Meaning of color-coding is the same as in the previous figures in this appendix.
Paper: The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars 
Authors: Paola Marziani, Ascensión del Olmo, C. Alenka Negrete, Deborah Dultzin, Enrico Piconcelli, Giustina Vietri, Mary Loli Martínez-Aldama, Mauro D'Onofrio, Edi Bon, Natasa Bon, Alice Deconto Machado, Giovanna M. Stirpe, Tania Mayte Buendia Rios
Figure caption:                         Analysis of the 1900 Å blend, for 10 Population A sources of the HE subsample. Meaning of color-coding is the same as in Figure 21.
Paper: A Model RRNet for Spectral Information Exploitation and LAMOST Medium-resolution Spectrum Parameter Estimation
Authors: Shengchun Xiong, Xiangru Li, Caixiu Liao
Figure caption: A diagram of the RRNet model. The input layer is a preprocessed spectrum (Section 2.2). Immediately following the input layer are N  r  residual blocks. The residual blocks share a common structure and are used to reinforce the spectral features and restrain the negative effects from noises and irrelevant components based on their correlations with the parameter to be estimated. Subsequently, the spectrum is reshaped into sequence data S of length N  s , and further processed by a recurrent layer to obtain ﹩S^{\prime} ﹩. The recurrent module extracts spectral information by analyzing the correlations between the spectral features on various wavelength sub-bands and fusing their information. The final step is to establish a mapping from the spectral feature to the probability density function (PDF) of stellar parameters and elemental abundances.
Paper: A Model RRNet for Spectral Information Exploitation and LAMOST Medium-resolution Spectrum Parameter Estimation
Authors: Shengchun Xiong, Xiangru Li, Caixiu Liao
Figure caption: The average partial derivatives of the stellar parameters by StarNet, StarNet-R, and RRNet models over the cool and hot stars. The upper and lower panels present the average partial derivatives respectively for cool stars (T eff ∈ [4000, 4300] K) and hot stars (T eff ∈ [6000, 6300] K). Each average partial derivative is computed from 1000 randomly selected spectra in the test set. The sub-bands shaded in red indicate that the model can extract more weak spectral features with the recurrent module, and the sub-bands with borders shaded in green show that the model can perform more detailed features with the residual module.
Paper: A Model RRNet for Spectral Information Exploitation and LAMOST Medium-resolution Spectrum Parameter Estimation
Authors: Shengchun Xiong, Xiangru Li, Caixiu Liao
Figure caption: The consistencies between RRNet prediction and APOGEE-Payne catalog and the robustness against data quality. The black line is the distribution curve of the inconsistencies (difference) between RRNet predictions and the APOGEE-Payne catalog, and three colored curves (blue, green, and red) present the uncertainties (standard deviation) of the inconsistencies. μ  r  and σ  r  are respectively the mean and standard deviation of the difference, and ﹩{\hat{\sigma }}_{m}﹩ is the mean of the 1σ uncertainty predicted by RRNet.
Paper: A Model RRNet for Spectral Information Exploitation and LAMOST Medium-resolution Spectrum Parameter Estimation
Authors: Shengchun Xiong, Xiangru Li, Caixiu Liao
Figure caption: Performance comparisions: RRNet, ResNet , StarNet, and StarNet-R. The performance is evaluated based on the MAE (Equation (4)). The StarNet-R is a variant of StarNet with recurrent modules same as the RRNet.
Paper: A Model RRNet for Spectral Information Exploitation and LAMOST Medium-resolution Spectrum Parameter Estimation
Authors: Shengchun Xiong, Xiangru Li, Caixiu Liao
Figure caption: Distribution of stellar parameters from the LAMOST-RRNet catalog. The color characterizes [Fe/H], and the three isochrones represent the MIST stellar evolution tracks with stellar ages of 7 Gyr ([Fe/H] of −0.5, 0.0, and 0.5 respectively). The S/N intervals are 10 ≤ S/N < 20, 20 ≤ S/N < 40, 40 ≤ S/N < 60, and 60 ≤ S/N < 100, respectively.
Paper: A Model RRNet for Spectral Information Exploitation and LAMOST Medium-resolution Spectrum Parameter Estimation
Authors: Shengchun Xiong, Xiangru Li, Caixiu Liao
Figure caption: Dependencies of parameter estimation uncertainties on S/N. The dots indicate the uncertainty predicted by RRNet, and the length of the line segments centered on the dots indicates the uncertainty estimated from repeated observations (>5 times).
Paper: A Model RRNet for Spectral Information Exploitation and LAMOST Medium-resolution Spectrum Parameter Estimation
Authors: Shengchun Xiong, Xiangru Li, Caixiu Liao
Figure caption: Distribution of elemental abundances [X/Fe] relative to [Fe/H] from the LAMOST-RRNet catalog. The left panel is for giants (﹩\mathrm{log}\,g\lt 4﹩) and the right panel is for dwarfs (﹩\mathrm{log}\,g\gt 4﹩).
Paper: A Model RRNet for Spectral Information Exploitation and LAMOST Medium-resolution Spectrum Parameter Estimation
Authors: Shengchun Xiong, Xiangru Li, Caixiu Liao
Figure caption: The elemental abundances (from LAMOST-RRNet) variations with T eff in the three open clusters of Melotte 22, NGC 2682, and NGC 2632. The three colors in the figure correspond to the three open clusters, and the mean μ and standard deviation σ of the chemical abundances are added to each panel. The reference line is obtained by linear regression fit.
Paper: A Model RRNet for Spectral Information Exploitation and LAMOST Medium-resolution Spectrum Parameter Estimation
Authors: Shengchun Xiong, Xiangru Li, Caixiu Liao
Figure caption: Performance evaluation of RRNet in estimating three stellar atmospheric parameters (T eff, ﹩\mathrm{log}\,g﹩, [Fe/H]). In the above figure, the vertical axis presents the distribution of the z-score residuals (difference) between RRNet predictions and the APOGEE-Payne catalog test set.
Paper: A Model RRNet for Spectral Information Exploitation and LAMOST Medium-resolution Spectrum Parameter Estimation
Authors: Shengchun Xiong, Xiangru Li, Caixiu Liao
Figure caption: The loss curves of RRNet on the training set and validation set. The solid line indicates the mean of the M model losses (M = 6 in this paper), and the shaded area indicates the 1σ range of the M models.
Paper: A Model RRNet for Spectral Information Exploitation and LAMOST Medium-resolution Spectrum Parameter Estimation
Authors: Shengchun Xiong, Xiangru Li, Caixiu Liao
Figure caption: Some comparisons of the chemical abundances from LAMOST-RRNet and SPCANet catalogs in the three open clusters (Melotte 22, NGC 2682, and NGC 2632).