adsabs/AstroCLIMB huggingface dataset:
Paper: FAST Ultra-Deep Survey (FUDS): The Star Formation Histories of FUDS0 Galaxies
Authors: Hongwei Xi, Lister Staveley-Smith, Bo Peng, Bi-Qing For, Bin Liu, Dejian Ding
Figure caption: An example SED for a FUDS0 galaxy (ID: G039) in the observer frame. The observation data points are represented by black dots. The red dashed line is the best fit, while the gray lines are the 50 posterior samples randomly selected from 104.
Paper: FAST Ultra-Deep Survey (FUDS): The Star Formation Histories of FUDS0 Galaxies
Authors: Hongwei Xi, Lister Staveley-Smith, Bo Peng, Bi-Qing For, Bin Liu, Dejian Ding
Figure caption: The distribution of H I line width predicted by forbidden or Balmer line width from SDSS for the non-detections in FUDS0 field.
Paper: FAST Ultra-Deep Survey (FUDS): The Star Formation Histories of FUDS0 Galaxies
Authors: Hongwei Xi, Lister Staveley-Smith, Bo Peng, Bi-Qing For, Bin Liu, Dejian Ding
Figure caption: The comparison of stellar mass between GSWLC-2 and PROSPECT. The blue dots are the FUDS0 H I galaxies, while red dots are the non-detections in the FUDS0 field. The dotted line indicates equality, while the solid line is the best fit.
Paper: FAST Ultra-Deep Survey (FUDS): The Star Formation Histories of FUDS0 Galaxies
Authors: Hongwei Xi, Lister Staveley-Smith, Bo Peng, Bi-Qing For, Bin Liu, Dejian Ding
Figure caption: The galaxy numbers with counterparts from GALEX, SDSS, DESI, and WISE. The numbers for FUDS0 galaxies are given in blue, while the non-detections in red. The gray numbers indicate the galaxies in the overlap regions.
Paper: FAST Ultra-Deep Survey (FUDS): The Star Formation Histories of FUDS0 Galaxies
Authors: Hongwei Xi, Lister Staveley-Smith, Bo Peng, Bi-Qing For, Bin Liu, Dejian Ding
Figure caption: The distribution of detections (blue dots) and non-detections (red dots) in the SFR–M* plane. The solid dots indicate the galaxies with spectroscopic redshifts, while the empty dots indicate those without. The solid black line represents the SF sequence with the gray area indicating the 1σ uncertainty derived in this paper, while the black dotted line indicates the criterion for selecting SF galaxies (﹩\mathrm{log}({\rm{SFR}}/{{\rm{yr}}}^{-1})\gt -11﹩). The black dashed line indicates the upper limit for peak sSFR derived from the SFHs of FUDS0 galaxies. The red and blue solid lines are the SF lines for SF or SF/AGN galaxies from S. Salim et al. (2007).
Paper: FAST Ultra-Deep Survey (FUDS): The Star Formation Histories of FUDS0 Galaxies
Authors: Hongwei Xi, Lister Staveley-Smith, Bo Peng, Bi-Qing For, Bin Liu, Dejian Ding
Figure caption: The best-fit evolutionary tracks of H I galaxies in ﹩\mathrm{log}({\rm{SFR}})﹩–﹩\mathrm{log}({M}_{* })﹩ (upper panel) and ﹩\mathrm{log}({\rm{sSFR}})﹩–﹩\mathrm{log}({M}_{* })﹩ (lower panel). The colors represent the ages of the galaxies. The black lines have the same meanings as those in Figure 15.
Paper: FAST Ultra-Deep Survey (FUDS): The Star Formation Histories of FUDS0 Galaxies
Authors: Hongwei Xi, Lister Staveley-Smith, Bo Peng, Bi-Qing For, Bin Liu, Dejian Ding
Figure caption: Comparison between FUDS0 and GSWLC-2. The distribution of GSWLC-2 galaxies is shown with colored contours. The dashed red line shows the median SFR vs. stellar mass for SF galaxies in GSWLC-2. The black dots indicate the FUDS0 H I galaxies in the same redshift range as GSWLC-2 (z < 0.3), while the light gray dots are the rest of the FUDS0 detections. The distributions of stellar mass (upper panel) and SFR (right panel) are normalized.
Paper: FAST Ultra-Deep Survey (FUDS): The Star Formation Histories of FUDS0 Galaxies
Authors: Hongwei Xi, Lister Staveley-Smith, Bo Peng, Bi-Qing For, Bin Liu, Dejian Ding
Figure caption: The comparison between FUDS0 and xGASS catalog. The black dots indicate the FUDS0 galaxies at z < 0.1, while the light gray dots represent the rest of FUDS0 H I galaxies. The black lines have the same meanings as those in Figure 15. The contours represent the distribution of xGASS galaxies. The distributions of stellar mass (upper panel) and SFR (right panel) are normalized by the maximum.
Paper: FAST Ultra-Deep Survey (FUDS): The Star Formation Histories of FUDS0 Galaxies
Authors: Hongwei Xi, Lister Staveley-Smith, Bo Peng, Bi-Qing For, Bin Liu, Dejian Ding
Figure caption: The distribution of FUDS0 galaxies in the SFR–M* plane. The black and gray dots represent strong or weak detections separated by ﹩{T}_{\sigma }=\tfrac{{S}_{\mathrm{int}}}{\mathrm{Jy}\,\mathrm{Hz}}{\left(\tfrac{1{0}^{6}\,\mathrm{Hz}}{{W}_{20}}\right)}^{\alpha }=250﹩. The black lines have the same meanings as those in Figure 15.
Paper: FAST Ultra-Deep Survey (FUDS): The Star Formation Histories of FUDS0 Galaxies
Authors: Hongwei Xi, Lister Staveley-Smith, Bo Peng, Bi-Qing For, Bin Liu, Dejian Ding
Figure caption: The comparison between FUDS0 and HIGHz catalog. The black dots indicate the FUDS0 galaxies in the same redshift range as HIGHz (0.17 ≤ z ≤ 0.25), while the light gray dots the rest of FUDS0 H I galaxies. The black lines have the same meanings as those in Figure 15. The red dots represent the HIGHz galaxies.
Paper: FAST Ultra-Deep Survey (FUDS): The Star Formation Histories of FUDS0 Galaxies
Authors: Hongwei Xi, Lister Staveley-Smith, Bo Peng, Bi-Qing For, Bin Liu, Dejian Ding
Figure caption: The distributions of GSWLC-2 (contours) and FUDS0 (dots) galaxies. The colors indicate galaxies in different redshift bins (blue: 0–0.06, red: 0.06–0.3). The black lines have the same meanings as those in Figure 15.
Paper: FAST Ultra-Deep Survey (FUDS): The Star Formation Histories of FUDS0 Galaxies
Authors: Hongwei Xi, Lister Staveley-Smith, Bo Peng, Bi-Qing For, Bin Liu, Dejian Ding
Figure caption: The comparison between the FUDS0 and ALFALFA catalogs. The black dots represent the FUDS0 galaxies located at z < 0.1, while the gray dots are others. The contours display the distribution of ALFALFA galaxies. The red dashed line indicates the median ALFALFA SFR vs. stellar mass. The black lines have the same meanings as those in Figure 15.
Paper: FAST Ultra-Deep Survey (FUDS): The Star Formation Histories of FUDS0 Galaxies
Authors: Hongwei Xi, Lister Staveley-Smith, Bo Peng, Bi-Qing For, Bin Liu, Dejian Ding
Figure caption: Same as Figure 16, but for non-detections.
Paper: A Local Dwarf Galaxy Search Using Machine Learning
Authors: Huanian Zhang, 华年 张, Guangping Ye, 广平 叶, Rongyu Wu, 嵘玉 吴, Dennis Zaritsky
Figure caption: The distribution of the local low-mass galaxy candidates (psignal > 0.90) across the sky in R.A. and decl (top) and the zoomed-in view for the local galaxy clusters (bottom). We label the well-known local overdensities (Fornax, Coma, and Virgo) for reference. The sizes of the symbols reflect twice the virial radius of these overdensities. The virial radii of these overdensities are as follows: Fornax, 0.49 Mpc or 1﹩\mathop{.}\limits^{\unicode{x000B0}}﹩71 from N. Maddox et al. (2019); Coma, 1.99 Mpc or 1﹩\mathop{.}\limits^{\unicode{x000B0}}﹩66 from J. M. Kubo et al. (2007); and Virgo, 1.08 Mpc or 5﹩\mathop{.}\limits^{\unicode{x000B0}}﹩50 from O. Urban et al. (2011).
Paper: A Local Dwarf Galaxy Search Using Machine Learning
Authors: Huanian Zhang, 华年 张, Guangping Ye, 广平 叶, Rongyu Wu, 嵘玉 吴, Dennis Zaritsky
Figure caption: The images and spectra of six signal galaxy candidates from DESI-EDR. The top three galaxies are relatively red, and their spectra do not show clear emission lines and are dominated by absorption lines. The bottom three galaxies are starbursting galaxies, and their spectra are dominated by emission lines although the continuum is very low. The gray, black, and red spectra represent the raw, smoothed, and model spectra, with the raw and model spectra sourced from DESI-EDR. The smoothed spectra are obtained by convolving the raw spectra with a one-dimensional Gaussian, whose standard deviation is set to 5. The vertical dashed lines indicate the position of featured emission lines and absorption lines.
Paper: A Local Dwarf Galaxy Search Using Machine Learning
Authors: Huanian Zhang, 华年 张, Guangping Ye, 广平 叶, Rongyu Wu, 嵘玉 吴, Dennis Zaritsky
Figure caption: The color–color distribution of the signal and contaminants in the training data set. Red dots represent the signal (local dwarf galaxies), sky-blue inverted triangles represent nearby sub-L* galaxies, tan squares stand for local massive galaxies, black stars denote nearby massive galaxies, green diamonds mark high-z massive galaxies, gray triangles represent nearby spiral galaxies, and yellow pentagons stand for artifact features.
Paper: A Local Dwarf Galaxy Search Using Machine Learning
Authors: Huanian Zhang, 华年 张, Guangping Ye, 广平 叶, Rongyu Wu, 嵘玉 吴, Dennis Zaritsky
Figure caption: M*–SFR relation (left panel) and mass–size relation (right panel) for the dwarf galaxies as well as for the massive galaxies in the DESI-EDR database. The blue symbols represent the blue galaxies with g − r < 0.7 and the red symbols stand for the red galaxies with g − r > 0.7. The dots denote the dwarf galaxy sample and the triangles indicate the massive galaxies with stellar mass greater than 109.2 M⊙.
Paper: A Local Dwarf Galaxy Search Using Machine Learning
Authors: Huanian Zhang, 华年 张, Guangping Ye, 广平 叶, Rongyu Wu, 嵘玉 吴, Dennis Zaritsky
Figure caption: Confusion matrix of the seven-class NN classification model for the test set. Each column in each row represents the predicted class count for the corresponding true class. The percentages on the diagonal represent the precision of each class, and the shades of color represent the recall of each class. The precision of the signal is 95.33%, and the recall of the signal can be calculated simply to be 76.07%, which means that more than 20% of the signal is incorrectly predicted as other types.
Paper: A Local Dwarf Galaxy Search Using Machine Learning
Authors: Huanian Zhang, 华年 张, Guangping Ye, 广平 叶, Rongyu Wu, 嵘玉 吴, Dennis Zaritsky
Figure caption: The distribution of the contamination and the signal for the test set in the parameter space. Green triangles represent all contaminants, red points indicate correctly classified signals, and blue points stand for misclassified signals.
Paper: A Local Dwarf Galaxy Search Using Machine Learning
Authors: Huanian Zhang, 华年 张, Guangping Ye, 广平 叶, Rongyu Wu, 嵘玉 吴, Dennis Zaritsky
Figure caption: Cutout images of some of the signal selected from the training sample. Surprisingly, the panel in the bottom left shows very obvious spiral arms and the panel in the top left has a very bright bulge.
Paper: A Local Dwarf Galaxy Search Using Machine Learning
Authors: Huanian Zhang, 华年 张, Guangping Ye, 广平 叶, Rongyu Wu, 嵘玉 吴, Dennis Zaritsky
Figure caption: The probability distribution of the local low-mass dwarf galaxy candidates provided by the NN model.
Paper: A Local Dwarf Galaxy Search Using Machine Learning
Authors: Huanian Zhang, 华年 张, Guangping Ye, 广平 叶, Rongyu Wu, 嵘玉 吴, Dennis Zaritsky
Figure caption: Cutout images of some local dwarf galaxy candidates. The majority of these candidates show very blue colors and the structures are diverse.
Paper: Pulsation Properties of Blazhko and Non-Blazhko RRab Stars
Authors: Peng Zong, Jian-Ning Fu, Jie Su, Bing-Kai Zhang, Gao-Chao Liu, Weichao Sun, Jiaxin Wang, Bo Zhang, Xueying Hu, Zhongrui Bai, Weikai Zong
Figure caption: Fourier parameters of amplitude ratio diagram for those BL and nBL stars. Panel (a) shows the R21 against R31, and panels (b) and (c) show the cumulative distribution function of the two parameters between the Blazhko and non-Blazhko RRab stars with different colors.
Paper: Pulsation Properties of Blazhko and Non-Blazhko RRab Stars
Authors: Peng Zong, Jian-Ning Fu, Jie Su, Bing-Kai Zhang, Gao-Chao Liu, Weichao Sun, Jiaxin Wang, Bo Zhang, Xueying Hu, Zhongrui Bai, Weikai Zong
Figure caption: Fourier parameters of ϕ21 vs. ϕ31 diagram for those BL and nBL stars. Panel (a) presents the relation between the two parameters. The cumulative distribution function of the two parameters is shown in panel (b) and (c), respectively.
Paper: Pulsation Properties of Blazhko and Non-Blazhko RRab Stars
Authors: Peng Zong, Jian-Ning Fu, Jie Su, Bing-Kai Zhang, Gao-Chao Liu, Weichao Sun, Jiaxin Wang, Bo Zhang, Xueying Hu, Zhongrui Bai, Weikai Zong
Figure caption: Low-degree Fourier coefficients of the sample stars. Amplitude coefficients R21, R31 (top panels) and phase coefficients ϕ21 and ϕ31 (bottom panels), as a function of the Blazhko period, are shown. The gray points are the Blazhko RRab stars from the study of M. Skarka et al. (2020), and the green points are the Blazhko RRab stars determined in this work.
Paper: Pulsation Properties of Blazhko and Non-Blazhko RRab Stars
Authors: Peng Zong, Jian-Ning Fu, Jie Su, Bing-Kai Zhang, Gao-Chao Liu, Weichao Sun, Jiaxin Wang, Bo Zhang, Xueying Hu, Zhongrui Bai, Weikai Zong
Figure caption: Comparing the RT with other pulsation parameters of main periods with R31 for non-Blazhko and Blazhko RRab stars. Panels (a) and (b) show the Period vs. RT and R31 vs. RT, respectively.
Paper: Pulsation Properties of Blazhko and Non-Blazhko RRab Stars
Authors: Peng Zong, Jian-Ning Fu, Jie Su, Bing-Kai Zhang, Gao-Chao Liu, Weichao Sun, Jiaxin Wang, Bo Zhang, Xueying Hu, Zhongrui Bai, Weikai Zong
Figure caption: Light curves of the non-Blazhko and Blazhko ab-type RRLs. Panels (a) and (b) show the light curves of the non-Blazhko ab-type star EPIC 212719863, while (c) and (d) depict the light curves of the Blazhko ab-type star EPIC 220244829. The phased light curves of both stars are folded by their fundamental periods.
Paper: Pulsation Properties of Blazhko and Non-Blazhko RRab Stars
Authors: Peng Zong, Jian-Ning Fu, Jie Su, Bing-Kai Zhang, Gao-Chao Liu, Weichao Sun, Jiaxin Wang, Bo Zhang, Xueying Hu, Zhongrui Bai, Weikai Zong
Figure caption: Cumulative distribution function of the two parameters of the metallicities of Blazhko and non-Blazhko stars.
Paper: Pulsation Properties of Blazhko and Non-Blazhko RRab Stars
Authors: Peng Zong, Jian-Ning Fu, Jie Su, Bing-Kai Zhang, Gao-Chao Liu, Weichao Sun, Jiaxin Wang, Bo Zhang, Xueying Hu, Zhongrui Bai, Weikai Zong
Figure caption: Comparison of Fourier parameters with OGLE-IV LMC field RR Lyrae stars (I. Soszyński et al. 2016). The red points represent RRab, and yellow points are RRc stars. The black and blue pentagons are non-Blazhko and Blazhko stars in the field of Kepler/K2.
Paper: Pulsation Properties of Blazhko and Non-Blazhko RRab Stars
Authors: Peng Zong, Jian-Ning Fu, Jie Su, Bing-Kai Zhang, Gao-Chao Liu, Weichao Sun, Jiaxin Wang, Bo Zhang, Xueying Hu, Zhongrui Bai, Weikai Zong
Figure caption: Absolute magnitudes and color indices of Blazhko and non-Blazhko RRab stars. Panel (a) presents the distributions of colors vs. absolute magnitudes. The cumulative distribution function of the two parameters is shown in panel (b) and (c), respectively.
Paper: Minute-cadence Observations of the Galactic Plane with the Wide Field Survey Telescope (WFST): Overview, Methodology, and Early Results
Authors: Jie Lin, Tinggui Wang, Minxuan Cai, Zhen Wan, Xuzhi Li, Lulu Fan, Qingfeng Zhu, Ji-an Jiang, Ning Jiang, Xu Kong, Zheyu Lin, Jiazheng Zhu, Zhengyan Liu, Jie Gao, Bin Li, Feng Li, Ming Liang, Hao Liu, Wei Liu, Wentao Luo, Jinlong Tang, Hairen Wang, Jian Wang, Yongquan Xue, Dazhi Yao, Hongfei Zhang, Xiaoling Zhang, Wen Zhao, Xianzhong Zheng
Figure caption: Uninterrupted light curves (panels (a)–(d)) and phase-folded light curves (panels (e)–(h)) for four short-period variable stars selected from WFST minute-cadence observations. These objects are 1.3 hr δ Sct star J1743+0134 (panels (a) and (e)), 20.5 minute UCB J0526+5934 (panels (b) and (f)), 6.7 minute ZZ Cet variable J0530+5945 (panels (c) and (g)), and 25.3 minute unspecific variable hot WD J0530+5945 (panels (d) and (h)). To double-check the periodicity, we present the phase-folded light curves for J0530+5945 obtained from two nights (panel (h)). The gray solid lines represent the best-fit fourth-order Fourier series.
Paper: A Formalism for Calibrating the Instrumental Polarization of Radio Interferometric Arrays at Meter Wavelengths Using Unpolarized Sky: A Demonstration Using MWA Observations
Authors: Devojyoti Kansabanik, Angelos Vourlidas, Soham Dey, Surajit Mondal, Divya Oberoi
Figure caption: An example of estimated pol-rotation terms for an observation is shown. In the left panel, solid black and green lines represent the geometric angle and ellipticity errors, respectively, which remain near zero and display similar trends across the frequency range in both epochs. Blue cross markers indicate the estimated crosshand phase assuming other pol-rotation terms are zero, closely matching the red line, which accounts for all terms. The right panel illustrates the posterior distribution of all pol-rotation terms for a single spectral channel, confirming no degeneracy among the three terms. Vertical dotted lines in the one-dimensional histograms show the 16%, 50%, and 84% quantities of the distribution.
Paper: Minute-cadence Observations of the Galactic Plane with the Wide Field Survey Telescope (WFST): Overview, Methodology, and Early Results
Authors: Jie Lin, Tinggui Wang, Minxuan Cai, Zhen Wan, Xuzhi Li, Lulu Fan, Qingfeng Zhu, Ji-an Jiang, Ning Jiang, Xu Kong, Zheyu Lin, Jiazheng Zhu, Zhengyan Liu, Jie Gao, Bin Li, Feng Li, Ming Liang, Hao Liu, Wei Liu, Wentao Luo, Jinlong Tang, Hairen Wang, Jian Wang, Yongquan Xue, Dazhi Yao, Hongfei Zhang, Xiaoling Zhang, Wen Zhao, Xianzhong Zheng
Figure caption: Uninterrupted light curves for eight flaring stars selected from WFST minute-cadence observations. All flaring stars are sorted by their quiescent magnitudes. We annotate the light-curve morphology for the flares (black arrows) as well as the observation issues (red arrows). Notice that, since each (4608 × 4616 pixel) region on the CCDs is processed separately in current pipelines, the bright sources switching among multiple detector regions could produce tiny systematic shifts in their light curves (see panel (a)).
Paper: A Formalism for Calibrating the Instrumental Polarization of Radio Interferometric Arrays at Meter Wavelengths Using Unpolarized Sky: A Demonstration Using MWA Observations
Authors: Devojyoti Kansabanik, Angelos Vourlidas, Soham Dey, Surajit Mondal, Divya Oberoi
Figure caption: A schematic diagram representing origins of three pol-rotation terms in the linear polarization basis. Black arrows show the axes of the sky coordinate system as per IAU convention (IAU 1973). Bold blue and red lines represent X and Y dipoles. The first panel shows the geometrical rotation with respect to the IAU-defined antenna polarization frame by an angle θ, the second panel shows the ellipticity error due to non-orthogonality by an angle ϵ, and the third panel shows the phase difference by an angle ϕ between signals coming from X and Y dipoles.
Paper: Minute-cadence Observations of the Galactic Plane with the Wide Field Survey Telescope (WFST): Overview, Methodology, and Early Results
Authors: Jie Lin, Tinggui Wang, Minxuan Cai, Zhen Wan, Xuzhi Li, Lulu Fan, Qingfeng Zhu, Ji-an Jiang, Ning Jiang, Xu Kong, Zheyu Lin, Jiazheng Zhu, Zhengyan Liu, Jie Gao, Bin Li, Feng Li, Ming Liang, Hao Liu, Wei Liu, Wentao Luo, Jinlong Tang, Hairen Wang, Jian Wang, Yongquan Xue, Dazhi Yao, Hongfei Zhang, Xiaoling Zhang, Wen Zhao, Xianzhong Zheng
Figure caption: Uninterrupted light curve and finding charts for flaring star J0427+7034. The purple dotted–dashed lines overlaid on the light curve (panel (a)) indicate the epochs corresponding to the finding charts (panels (b)–(d)) in sequence. The red bars indicate the position of J0427+7034 in the images. The size of each image is 300 pixels × 300 pixels.
Paper: Minute-cadence Observations of the Galactic Plane with the Wide Field Survey Telescope (WFST): Overview, Methodology, and Early Results
Authors: Jie Lin, Tinggui Wang, Minxuan Cai, Zhen Wan, Xuzhi Li, Lulu Fan, Qingfeng Zhu, Ji-an Jiang, Ning Jiang, Xu Kong, Zheyu Lin, Jiazheng Zhu, Zhengyan Liu, Jie Gao, Bin Li, Feng Li, Ming Liang, Hao Liu, Wei Liu, Wentao Luo, Jinlong Tang, Hairen Wang, Jian Wang, Yongquan Xue, Dazhi Yao, Hongfei Zhang, Xiaoling Zhang, Wen Zhao, Xianzhong Zheng
Figure caption: Phase-folded light curves of J0446+7219 provided by ZTF DR22 (upper panel) and WFST minute-cadence observations (lower panel). Both light curves are folded by the photometric period (P = 2.95126 hr) derived from the 6 yr ZTF g-band observations. For an ellipsoidal binary, its orbital period is twice the photometric period. The gray solid lines represent the best-fit sinusoidal models.
Paper: A Formalism for Calibrating the Instrumental Polarization of Radio Interferometric Arrays at Meter Wavelengths Using Unpolarized Sky: A Demonstration Using MWA Observations
Authors: Devojyoti Kansabanik, Angelos Vourlidas, Soham Dey, Surajit Mondal, Divya Oberoi
Figure caption: A schematic diagram illustrating the propagation of electromagnetic radiation as it undergoes various atmospheric and instrumental effects, along with the associated Jones terms described in Equation (3).
Paper: A Formalism for Calibrating the Instrumental Polarization of Radio Interferometric Arrays at Meter Wavelengths Using Unpolarized Sky: A Demonstration Using MWA Observations
Authors: Devojyoti Kansabanik, Angelos Vourlidas, Soham Dey, Surajit Mondal, Divya Oberoi
Figure caption: Average source sizes of MWA calibrator sources are shown by horizontal dotted lines. Angular size corresponding to thrice the angular resolution of the MWA Phase I and Phase II extended configurations are shown by blue and orange solid lines, respectively.
Paper: Spectroscopic Evolution in Ice Analogs of Trans-Neptunian Objects Exposed to Ionizing Radiation. I. Visible Reflectance Spectra and Colors
Authors: Chaojiang Zhang, Jia Wang, Andrew M. Turner, Leslie A. Young, Ralf I. Kaiser
Figure caption: The color slope and color evolution of ices 25−36 as the radiation dose increases, sequenced in panels (a)–(l). Error bars shown are from linear fitting of spectra. The gray area is the colors of TNOs from observations (O. R. Hainaut et al. 2012).
Paper: Spectroscopic Evolution in Ice Analogs of Trans-Neptunian Objects Exposed to Ionizing Radiation. I. Visible Reflectance Spectra and Colors
Authors: Chaojiang Zhang, Jia Wang, Andrew M. Turner, Leslie A. Young, Ralf I. Kaiser
Figure caption: The visible reflectance spectra of irradiated ices 31−36 taken during heating to 320 K. Ices 31−36 in Table 1 are displayed in the order of (a)–(f). All spectra are normalized at 550 nm and plotted as a gradient color from blue to red as temperature increases. Dashed lines represent the spectra of irradiated ices before and after heating to 320 K.
Paper: Spectroscopic Evolution in Ice Analogs of Trans-Neptunian Objects Exposed to Ionizing Radiation. I. Visible Reflectance Spectra and Colors
Authors: Chaojiang Zhang, Jia Wang, Andrew M. Turner, Leslie A. Young, Ralf I. Kaiser
Figure caption: The visible reflectance spectra of irradiated ices 19−24 taken during heating to 320 K. Ices 19−24 in Table 1 are displayed in the order of (a)–(f). All spectra are normalized at 550 nm and plotted as a gradient color from blue to red as temperature increases. Dashed lines represent the spectra of irradiated ices before and after heating to 320 K.
Paper: Spectroscopic Evolution in Ice Analogs of Trans-Neptunian Objects Exposed to Ionizing Radiation. I. Visible Reflectance Spectra and Colors
Authors: Chaojiang Zhang, Jia Wang, Andrew M. Turner, Leslie A. Young, Ralf I. Kaiser
Figure caption: The visible reflectance spectra of irradiated ices 13−18 taken during heating to 320 K. Ices 13−18 in Table 1 are displayed in the order of (a)–(f). All spectra are normalized at 550 nm and plotted as a gradient color from blue to red as temperature increases. Dashed lines represent the spectra of irradiated ices before and after heating to 320 K.