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: The distributions of both detections (blue) and non-detections (red) in the SFR–M* plane at z = 3, 2, 1, 0 as predicted by PROSPECT. The filled circles indicate that the redshift is larger than the observed redshift of the galaxies, while the empty circles indicate where the redshift is smaller than the observed redshift 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: The distributions of both detections (blue) and non-detections (red) in the sSFR–M* plane at z = 3, 2, 1, 0 as predicted by PROSPECT. The filled and empty circles have the same meanings as those in Figure 25. The black lines have the same meanings as those in Figure 15.
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 stellar mass distribution of the local low-mass galaxies in the training sample. The reason why there is a spike at M* = 107 M⊙ is that 107 M⊙ is the lower stellar mass limit in Y.-Y. Chang et al. (2015). But it does not affect our final results.
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 stellar mass vs. redshift of the contaminants in the training sample (top) and the r-band magnitude distribution for the signal and all contaminants (bottom).
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: Footprint of the sky covered by the Legacy Survey DR9 (A. Dey et al. 2019). It incorporates the DES in the south. The Galactic plane is traced by the red curve.
Paper: Experimental Branching Fractions, Transition Probabilities, and Oscillator Strengths of La II
Authors: Xue Shang, Chunxiao Zhou, Bolin Liu, Naosheng Qiao, Binfang Cao
Figure caption: Partial response functions of the instrument determined from the deuterium (D2) standard lamp and the tungsten (W) standard lamp. The response function in the 300–400 nm region corresponds to the spectrometer switching to a grating with groove densities of 3600 lines mm−1, and the response function in the 400–500 nm region corresponds to a grating with groove densities of 2400 lines mm−1.
Paper: Experimental Branching Fractions, Transition Probabilities, and Oscillator Strengths of La II
Authors: Xue Shang, Chunxiao Zhou, Bolin Liu, Naosheng Qiao, Binfang Cao
Figure caption: Relative differences between experimental log(gf)s from the literature and this work as a function of wavelength. The red circle symbols present a comparison with J. E. Lawler et al. (2001) measurements and the blue triangle symbols present a comparison with C. H. Corliss & W. R. Bozman (1962) measurements. The solid line presents a good agreement and the dashed lines present relative differences of ±20%.
Paper: Experimental Branching Fractions, Transition Probabilities, and Oscillator Strengths of La II
Authors: Xue Shang, Chunxiao Zhou, Bolin Liu, Naosheng Qiao, Binfang Cao
Figure caption: Comparison of experimental log(gf) values from the literature to results from this work as a function of wavelength. The red circle symbols present a comparison with J. E. Lawler et al. (2001) measurements. The blue triangle symbols present a comparison with C. H. Corliss & W. R. Bozman (1962) measurements. The solid line presents a good agreement and the dashed lines present differences of ±0.2 dex.
Paper: Experimental Branching Fractions, Transition Probabilities, and Oscillator Strengths of La II
Authors: Xue Shang, Chunxiao Zhou, Bolin Liu, Naosheng Qiao, Binfang Cao
Figure caption: Similar to Figure 4 except the comparisons are as a function of log(gf).
Paper: Experimental Branching Fractions, Transition Probabilities, and Oscillator Strengths of La II
Authors: Xue Shang, Chunxiao Zhou, Bolin Liu, Naosheng Qiao, Binfang Cao
Figure caption: Similar to Figure 2 except the comparisons are as a function of log(gf).
Paper: Experimental Branching Fractions, Transition Probabilities, and Oscillator Strengths of La II
Authors: Xue Shang, Chunxiao Zhou, Bolin Liu, Naosheng Qiao, Binfang Cao
Figure caption: Log(gf)s with error bars. The red circle symbols present data from J. E. Lawler et al. (2001) and the black circle symbols present data from this work.
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: Distributions of periodic variable stars and flaring stars across the CMD. The general periodic variable stars, short-period variable stars, and flaring stars were selected by the three different methods introduced in Section 3. The additional flaring stars were discovered by visually checking the variable star candidates with high 1/η values rather than by Osten’s method. Several interesting objects are highlighted by purple squares. The gray dots in the background are the sources detected from the 15 hr WFST observations. We denote the instability strip edges of δ Sct (S. J. Murphy et al. 2019) and ZZ Cet (I. Caiazzo et al. 2021) with dashed lines and dotted–dashed lines, 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: Distributions for number (upper), robust standard deviation (middle), and inverse von Neumann ratio (lower) against the median AB magnitude, derived from the light curves extracted from g-band observation GP-20240209 (left) and r-band observation GP-20240509 (right). Upper panels: the gray lines represent the number of light curves (with ≥20 epochs) per bin, while the blue lines represent the number of candidate variable stars (with 1/η above the 10σ threshold) per bin. The bin size is 0.2 mag. Middle panels and lower panels: the black and red lines represent the medians and 10σ excesses for the distributions of variability indices, respectively. The gray and green/blue points represent the light curves with variability indices below and above the 10σ thresholds, 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: A gallery of phase-folded light curves for nine general periodic variable stars revealed by the splicing observations. All light curves are obtained from the g-band observations of WFST, and the exposure is 20 s. For the objects identified by VSX, their light curves (panels (a)–(f)) are folded by the period provided by VSX; for the variables first identified by WFST, the light curves (panels (g)–(i)) are folded using twice the photometric periods (i.e., ﹩1/{f}_{{\rm{\max }}}﹩) obtained from the WFST LSPs. We label the classification type for the objects identified by VSX: EW = EW-type eclipsing binary, HADS = high-amplitude δ Sct star, RRAB = RRab Lyrae, and BY = BY Dra–type variable. The light curves having relatively complete phase coverage (i.e., panels (c), (d), and (i)) are modeled using a fourth-order Fourier series (the gray solid lines).
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: Distributions of maximum power ﹩{{\rm{Pwr}}}_{{\rm{\max }}}﹩ vs. the corresponding frequency ﹩{f}_{{\rm{\max }}}﹩. Data points in panels (a)–(e) are LSPs derived from five WFST minute-cadence observations. The red solid line represents 10σ excesses, and the total numbers (N) of sources above/below the 10σ threshold are indicated in the legends. Several interesting short-period objects are highlighted with hollow symbols.
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: CDFs of FDRs for flare detection from WFST minute-cadence observations. The FDR histograms (blue solid lines) in panels (a)–(e) are ϕV V sequences derived from five WFST minute-cadence observations. And the red solid lines are the best-fit linear models for the histogram bins at ﹩{\mathrm{log}}\,({\rm{CDF}})\geqslant -1﹩. The bin size is 0.2. The hatched areas indicate that the observed FDR distributions exceed the models.
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: Accumulated fractions for the position deviations from the minute-cadence observations on 2024 February 9. Left: position deviations anchored at average coordinates of the position measurements. Right: position deviations anchored at the coordinates from the first detections of sources. The bin width is 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩02, and the red lines represent the best-fit linear models for the bins with an accumulated fraction >10%.
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: CDFs of FAPs for periodicity detection from the splicing observations. The data sets were obtained from GP-20230918+GP-20231116 (upper) and GP-20240206+GP-20240209 (lower). The blue lines represent the CDFs derived from WFST observation data, and the red lines are the best-fit linear models for the bins with ﹩{\mathrm{log}}\,({\rm{CDF}})\geqslant -1﹩. The bin size is 1.0.
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: Density distribution of the Gaia DR3–WFST sources across the CMD. Only the Gaia DR3 sources having a reliable parallax measurement are included in the distribution. Both magnitudes and colors are calibrated for interstellar dust extinction and reddening. The bin size is 0.1 × 0.1 mag2.
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: Top row: crosshand phase spectra for two different beamformers pointing on the same days are shown by red and blue lines. The left panel shows observations of MWA Phase I, and the right panel shows the MWA Phase II extended configuration. Crosshand phase spectra for two different beamformer pointings at different elevations and azimuths match with each other. Bottom row: temporal variations of MWA crosshand phase spectra from some example observations chosen randomly from the archive are shown. The same reference antenna, Tile168, has been used for all observations. The left panel shows the temporal variations on a timescale of days, and the right panel shows the temporal variations on timescales spanning months to years.
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 comparison between the traditional and newly proposed methods for crosshand phase correction is shown using J0636-2042. The three panels show Stokes V images at peak RM for the three cases—before crosshand phase correction, crosshand phase corrected using the newly proposed method, and crosshand phase corrected using the traditional method, respectively. In all images, green contours are Stokes I emission at 2%, 6%, 20%, 40%, 60%, and 80% of the peak flux and white contours correspond to σV, 3σV, and 5σV of Stokes V at peak RM, where σV is the rms noise level of the Stokes V map at peak RM.
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: Validation of the new proposed method using linearly polarized sources. 1D FDFs at the peak of Stokes I, linear and circular polarization at the peak RM are shown respectively in three panels for GLEAM J063633-204225 (J0636-2042) in the top row and for GLEAM J035140-27435 (J0351-2743) in the middle row. In all images, green contours are Stokes I emission at 2%, 6%, 20%, 40%, 60%, and 80% of the peak flux density.
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 1−12 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 color slopes and color evolution of ices 13−24 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 ices 13−18 measured during the irradiation. 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 radiation dose increases. Dashed lines represent the spectra of ices before and after irradiation.
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 ices 1−6 measured during the irradiation. Ices 1−6 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 radiation dose increases. Dashed lines represent the spectra of ices before and after irradiation.
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 ices 7−12 measured during the irradiation. Ices 7−12 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 radiation dose increases. Dashed lines represent the spectra of ices before and after irradiation.
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 ices 25−30 measured during the irradiation. Ices 25−30 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 radiation dose increases. Dashed lines represent the spectra of ices before and after irradiation.
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 ices 19−24 measured during the irradiation. 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 radiation dose increases. Dashed lines represent the spectra of ices before and after irradiation.
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 evolution of irradiated ices taken during heating to 320 K, sequenced in panels (a)–(f). Error bars shown are from the linear fitting of reflectance spectra.
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 2D offset distribution of optical counterparts from the centroids of H I galaxies (﹩{\rm{\Delta }}\rm{R.A.}=({\rm{R.A.}}_{{\rm{opt}}}-{\rm{R.A.}}_{{\rm{H}}\,{\rm{I}}})\times \cos ({\rm{decl.}}_{{\rm{H}}\,{\rm{I}}})﹩ and Δdecl. = decl.opt − decl.H I). The red dots represent the galaxies with spectroscopic redshift, while blue dots are the galaxies with only photometric redshifts. The median values and 1σ uncertainties (dashed circles in the same colors) are calculated after removing the four outliers. The beam size at 1.0 and 1.42 GHz is shown by the black solid and dotted circles, respectively.
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 redshift separation for galaxies only with photometric redshift (Δz = zopt,photo − zH I). Considering the accuracy, we use photometric redshift from DESI Imaging Legacy Survey.
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 spatial distribution of FUDS0 galaxies, color coded by redshift. The gray line indicates the boundary of the FUDS0 field, estimated from ideal scan lines and the geometry of the 19-beam receiver.
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 Δcz = c × (zopt,spect − zH I) for galaxies with spectroscopic redshift.
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 H I line width (W20,H I) as a function of the forbidden (blue) and Balmer (red) line widths from SDSS in the rest frame. The best-fit lines are given in the same color.
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 best-fit parameters for both detections (blue) and non-detections (red) 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 upper limits of H I masses as a function of redshift for non-detections (gray arrows) along with H I galaxies (black dots).
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 ratio of SFR from GSWLC-2 and PROSPECT as a function of sSFR from PROSPECT. The blue symbols represent the FUDS0 H I galaxies, while the red symbols the non-detections. The best fit is indicated by the solid black line.
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 sSFR, SFR, stellar mass, and metallicity as functions of time for a FUDS0 galaxy (ID: G039). The red dashed lines are the best-fit SFH. The gray lines are the same 50 posterior sampling shown in Figure 10, while the blue dashed lines are the median values. The black dotted lines indicate the redshift of the galaxy.
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 SFR between GSWLC-2 and PROSPECT after adjustment. The blue dots are the FUDS0 H I galaxies, while red dots are the non-detections in the FUDS0 field. The 1:1 line is given by the black dotted line.