adsabs/AstroCLIMB huggingface dataset:
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: Metallicity (O/H) and C/O recovered from our free-chemistry retrievals. In colors, we highlight the error on the retrieved abundance of water ﹩{\sigma }_{\mathrm{log}({{\rm{H}}}_{2}{\rm{O}})}﹩ because only the cases where water is recovered are reliable (purple to black). C/O remains very difficult to constrain because our observations lack sensitivity to carbon-bearing species. In the inset, we show the metallicity derived from free chemistry for the runs with ﹩{\sigma }_{\mathrm{log}({{\rm{H}}}_{2}{\rm{O}})}\lt 1﹩ vs. the metallicity recovered in the equilibrium chemistry cases.
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: Correlations at the dayside between the CO2 (top) and CH4 (bottom) abundances and the mean retrieved temperature weighted by the contribution function. The colors indicate the retrieved thermal gradient, defined as the temperature differences between the upper and lower quantiles of the contribution function. The shaded green region is the predicted abundances from equilibrium chemistry at solar metallicity and the C/O between 1 bar and 0.01 bar. In orange, the metallicity is increased to 100 times solar. In red, the metallicity is decreased to 0.1 times solar. In blue, the metallicity is solar and the C/O is increased to 1.
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: Top: recovered spectra from each visit and the final, averaged spectrum (black). Bottom: comparison of the spectrum recovered here to that of Line et al. (2016). We note that, while the spectra have similar shapes, they are offset by around 0.016% (160 ppm).
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: Weighted retrieved atmospheric temperature for the dayside (top) and terminator (bottom) as a function of the planet’s equilibrium temperature. The equilibrium temperature is calculated for a planetary Albedo of 0. The colors correspond to the abundance of e−, which traces H2 dissociation. As a reference, we also show in dashed lines the GCM predictions from Tan & Komacek (2019) with H2 dissociation/recombination included for their slow (orange) and fast (black) drag timescales.
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: Correlations at the dayside between the FeH (top) and CO (bottom) abundances and the mean retrieved temperature weighted by the contribution function. The colors indicate the retrieved thermal gradient, defined as the temperature differences between the upper and lower quantiles of the contribution function. The shaded green region is the predicted abundances from equilibrium chemistry at solar metallicity and the C/O between 1 bar and 0.01 bar. In orange, the metallicity is increased to 100 times solar. In red, the metallicity is decreased to 0.1 times solar. In blue, the metallicity is solar and the C/O is increased to 1. Note that in the FeH plot (top), the Solar and C/O = 1 cases overlap.
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: Correlations at the dayside between the VO (top) and TiO (bottom) abundances and the mean retrieved temperature weighted by the contribution function. The colors indicate the retrieved thermal gradient, defined as the temperature differences between the upper and lower quantiles of the contribution function. The shaded green region is the predicted abundances from equilibrium chemistry at solar metallicity and the C/O between 1 bar and 0.01 bar. In orange, the metallicity is increased to 100 times solar. In red, the metallicity is decreased to 0.1 times solar. In blue, the metallicity is solar and the C/O is increased to 1.
Paper: “Winged” Radio Sources from the LOFAR Two-meter Sky Survey First Data Release (LoTSS DR1)
Authors: Soumen Bera, Tapan K. Sasmal, Dusmanta Patra, Soumen Mondal
Figure caption: A comparative presentation of the contour plots for the 14 sources that are previously identified either in Cheung (2007) or Yang et al. (2019) or Bera et al. (2020) from VLA FIRST data. The LoTSS DR1 image and VLA FIRST image are presented side by side for each of the 14 sources. The radio contour images are overlaid on the respective optical DSS2 images.
Paper: “Winged” Radio Sources from the LOFAR Two-meter Sky Survey First Data Release (LoTSS DR1)
Authors: Soumen Bera, Tapan K. Sasmal, Dusmanta Patra, Soumen Mondal
Figure caption: Histogram showing the percentage of FR-I and FR-II sources among the XRGs and ZRGs reported in the present paper.
Paper: “Winged” Radio Sources from the LOFAR Two-meter Sky Survey First Data Release (LoTSS DR1)
Authors: Soumen Bera, Tapan K. Sasmal, Dusmanta Patra, Soumen Mondal
Figure caption: Histogram showing the distribution of spectral index (﹩{\alpha }_{144}^{1400}﹩) for the identified winged radio galaxies.
Paper: “Winged” Radio Sources from the LOFAR Two-meter Sky Survey First Data Release (LoTSS DR1)
Authors: Soumen Bera, Tapan K. Sasmal, Dusmanta Patra, Soumen Mondal
Figure caption: Distribution of radio luminosity (﹩\mathrm{log}({L}_{\mathrm{rad}}﹩)) with redshift (z) for both the XRGs and ZRGs.
Paper: “Winged” Radio Sources from the LOFAR Two-meter Sky Survey First Data Release (LoTSS DR1)
Authors: Soumen Bera, Tapan K. Sasmal, Dusmanta Patra, Soumen Mondal
Figure caption: Histogram showing the global spectral index (﹩{\alpha }_{144}^{1400}﹩) distribution of winged radio galaxies along with our identified winged radio galaxies.
Paper: MUSUBI (MegaCam Ultra-deep Survey: u*-band Imaging) Data for the COSMOS and SXDS Fields
Authors: Wei-Hao Wang, Sebastien Foucaud, Bau-Ching Hsieh, Hung-Yu Jian, Lihwai Lin, Yen-Ting Lin, Jean Coupon, Yasuhiro Hashimoto, Masami Ouchi, Kazuhiro Shimasaku, Youichi Ohyama, Keiichi Umetsu, Shiang-Yu Wang, Tzu-Ching Chang
Figure caption: Transmission profile of the CFHT MegaCam u* filter used in MUSUBI. The solid blue curve is the profile of the filter, while the dashed blue curve is the profile combined with the telescope/camera transmission and CCD quantum efficiency. For readers’ reference, we also show the profiles for the new CFHT u filter (solid cyan curve), the new CFHT u filter combined with the telescope/camera transmission and CCD quantum efficiency (dashed cyan curve), the SDSS U filter (dotted magenta curve), and the SDSS G filter (dotted green curve). All profiles shown here do not contain the effect of atmospheric absorption.
Paper: MUSUBI (MegaCam Ultra-deep Survey: u*-band Imaging) Data for the COSMOS and SXDS Fields
Authors: Wei-Hao Wang, Sebastien Foucaud, Bau-Ching Hsieh, Hung-Yu Jian, Lihwai Lin, Yen-Ting Lin, Jean Coupon, Yasuhiro Hashimoto, Masami Ouchi, Kazuhiro Shimasaku, Youichi Ohyama, Keiichi Umetsu, Shiang-Yu Wang, Tzu-Ching Chang
Figure caption: Image of the COSMOS field (left) and its weighted exposure distribution (right). The brightness scales are inverted. The entire area shown here has a size of ﹩108^{\prime} \times 108^{\prime} ﹩. The image shows that this field is relatively free from bright stars and the background subtraction in our reduction is excellent. The exposure map shows the very different mosaicking strategies adopted by various teams, producing an extremely deep core of approximately ﹩11^{\prime} \times 14^{\prime} ﹩ at the center and a deep area of approximately 60′ × 60′.
Paper: MUSUBI (MegaCam Ultra-deep Survey: u*-band Imaging) Data for the COSMOS and SXDS Fields
Authors: Wei-Hao Wang, Sebastien Foucaud, Bau-Ching Hsieh, Hung-Yu Jian, Lihwai Lin, Yen-Ting Lin, Jean Coupon, Yasuhiro Hashimoto, Masami Ouchi, Kazuhiro Shimasaku, Youichi Ohyama, Keiichi Umetsu, Shiang-Yu Wang, Tzu-Ching Chang
Figure caption: Image of the SXDS field (left) and its weighted exposure distribution (right). The brightness scales are inverted. The entire area shown here has a size of ﹩77^{\prime} \times 80^{\prime} ﹩. The bright star near the northwestern corner has V = 6.49 and induces a slightly less than ideal background subtraction in its neighborhood. The exposure distribution is more uniform and the map size is smaller than the COSMOS field. The deep area is approximately 52′ × 44′.
Paper: MUSUBI (MegaCam Ultra-deep Survey: u*-band Imaging) Data for the COSMOS and SXDS Fields
Authors: Wei-Hao Wang, Sebastien Foucaud, Bau-Ching Hsieh, Hung-Yu Jian, Lihwai Lin, Yen-Ting Lin, Jean Coupon, Yasuhiro Hashimoto, Masami Ouchi, Kazuhiro Shimasaku, Youichi Ohyama, Keiichi Umetsu, Shiang-Yu Wang, Tzu-Ching Chang
Figure caption: Comparison between our SXDS photometry and the synthetic SDSS u* photometry on objects with SDSS U < 21. We used D = 5″ apertures from our catalog. The median at u* > 16.5 is 0.012. At u* < 16.5, nonlinear effects start to show up in the MegaCam data. Such bright objects were not used for calibration. They are shown here only to show the nonlinear effects.
Paper: MUSUBI (MegaCam Ultra-deep Survey: u*-band Imaging) Data for the COSMOS and SXDS Fields
Authors: Wei-Hao Wang, Sebastien Foucaud, Bau-Ching Hsieh, Hung-Yu Jian, Lihwai Lin, Yen-Ting Lin, Jean Coupon, Yasuhiro Hashimoto, Masami Ouchi, Kazuhiro Shimasaku, Youichi Ohyama, Keiichi Umetsu, Shiang-Yu Wang, Tzu-Ching Chang
Figure caption: Comparison between our COSMOS photometry and the SNLS photometry on objects with u* errors less than 0.05 mag in both catalogs. We used D = 5″ apertures from our catalog, which are comparable to the aperture size used in the SNLS. The median for the full sample is −0.0018. The cyan dashed line is a linear fit to data within y  =   ±0.1, suggesting that there is a tilt. The nature of this tilt is unclear, and it is nevertheless very small.
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: Example fits to regions in the order defined in Table 1. (a) Region 1 (IERS 1645+365), (b) region 2 (IERS 1509+054), (c) region 3 (IERS 1330+022), (d) region 4 (IERS 2305+187), (e) region 5 (IERS 1415+385), (f) region 6 (IERS 0037+011), (g) region 7 (IERS 0043+246), and (h) region 8 (IERS 0955+476).
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: Examples of the full-spectrum continuum fitting performed to constrain large-scale parameters such as the host/stellar and AGN fractions and power-law index (α  λ ). Prominent emission features that appear in the residuals are labeled. (a) Example continuum fit typical of Sy 1 and quasar-type objects (IERS 0043+246), exhibiting strong power-law and Balmer continuum, and weaker host/stellar contributions. (b) Example continuum fit of a typical Sy 2 (IERS 0026-015) exhibiting a strong host/stellar and weaker AGN power-law contributions.
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: The fit quality distributions for BH mass line calibrators. The width of each distribution represents the relative fraction of objects with a given fit quality for each line calibrator, with the total number of objects in each region posted below each distribution. The interquartile range is shown inside of each distribution by dashed lines. The red dashed line represents the fit quality of 0.85, considered here to be excellent.
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: The reduced χ 2 distributions for each fitting region. The width of each distribution represents the relative fraction of objects of a given ﹩{\chi }_{\nu }^{2}﹩ value in each region, with the total number of objects in each region given below. The interquartile range is shown inside each distribution by dashed lines. The red dashed line represents ﹩{\chi }_{\nu }^{2}=1﹩.
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: Comparison of error-normalized distributions of select parameters from our catalog and the Shen et al. (2011) QSO catalog. The dashed line represents the normal distribution ﹩{ \mathcal N }(0,1)﹩.
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: The Mollweide projection of all 4536 S/X ICRF3 sources from Charlot et al. (2020). Outlined regions correspond to various SDSS programs from which SDSS spectra of ICRF3 sources are obtained. The 1014 ICRF3 sources with available spectra are shown as red points.
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: Histogram of the redshift distribution of ICRF3 SDSS spectra for which redshifts could be accurately determined (N = 892). The dashed red line marks the median redshift of z = 1.245.
Paper: The R-process Alliance: A Nearly Complete R-process Abundance Template Derived from Ultraviolet Spectroscopy of the R-process-enhanced Metal-poor Star HD 222925 
Authors: Ian U. Roederer, James E. Lawler, Elizabeth A. Den Hartog, Vinicius M. Placco, Rebecca Surman, Timothy C. Beers, Rana Ezzeddine, Anna Frebel, Terese T. Hansen, Kohei Hattori, Erika M. Holmbeck, Charli M. Sakari
Figure caption: STIS E230H spectra of HD 222925 compared with model spectra around lines of interest, which are marked and labeled. The thick red line indicates the best-fit abundance for the line(s) of interest. The light red bands indicate variations in this abundance by ±0.3 dex (≈1.5–2.0 times the typical uncertainties), to facilitate visibility. The thick black line indicates a model that excludes the element of interest.
Paper: The R-process Alliance: A Nearly Complete R-process Abundance Template Derived from Ultraviolet Spectroscopy of the R-process-enhanced Metal-poor Star HD 222925 
Authors: Ian U. Roederer, James E. Lawler, Elizabeth A. Den Hartog, Vinicius M. Placco, Rebecca Surman, Timothy C. Beers, Rana Ezzeddine, Anna Frebel, Terese T. Hansen, Kohei Hattori, Erika M. Holmbeck, Charli M. Sakari
Figure caption: STIS E230H spectra of HD 222925 compared with model spectra around lines of interest. The symbols are the same as in Figure 2.
Paper: Variability of the Sun’s Luminosity Places Constraints on the Thermal Equilibrium of the Convection Zone
Authors: L. E. A. Vieira, G. Kopp, T. Dudok de Wit, L. A. da Silva, F. Carlesso, A. R. Barbosa, A. Muralikrishna, R. Santos
Figure caption: Energetics in the solar convection zone for cycles 23 and 24. (a) Evolution of the luminosity. The vertical red lines “T22” and “T23” indicate the terminator for cycles 22 and 23, respectively, as estimated by McIntosh et al. (2020). These terminators supposedly indicate the completion of the corresponding numbered solar cycle. (b) Variation of the thermal energy for two steady-state energy-input scenarios from the radiative zone: (1) constant at solar minimum level (L ref; red); and (2) average that would maintain convection-zone thermal equilibrium over solar cycles for 23 and 24 (L eq; blue). The time tick labels are in the format dd/mm/yy.
Paper: The R-process Alliance: A Nearly Complete R-process Abundance Template Derived from Ultraviolet Spectroscopy of the R-process-enhanced Metal-poor Star HD 222925 
Authors: Ian U. Roederer, James E. Lawler, Elizabeth A. Den Hartog, Vinicius M. Placco, Rebecca Surman, Timothy C. Beers, Rana Ezzeddine, Anna Frebel, Terese T. Hansen, Kohei Hattori, Erika M. Holmbeck, Charli M. Sakari
Figure caption: STIS E230H spectra of HD 222925 compared with model spectra around lines of interest. The symbols are the same as in Figure 2. The gray band in the second panel on the left marks a change in the blending Nb II line by its uncertainty, ±0.20 dex.
Paper: Variability of the Sun’s Luminosity Places Constraints on the Thermal Equilibrium of the Convection Zone
Authors: L. E. A. Vieira, G. Kopp, T. Dudok de Wit, L. A. da Silva, F. Carlesso, A. R. Barbosa, A. Muralikrishna, R. Santos
Figure caption: The latitudinal dependence of the irradiance over the last two solar cycles. (a) Latitudinal distribution of the irradiance for an observer at Earth’s heliographic longitude. (b) The TSI composite (gray line) and the solar irradiance viewed from the heliographic south (blue line; model) and north poles (red line; model). (c) Average latitudinal irradiance profile for the whole period (blue line), at solar maximum (2001–2002 and 2013–2014), during the descending phase (2005–2006), and at solar minimum (2007–2008). The latitude of the maximum for each hemisphere for the whole period average is indicated in the figure (red circles). (d) Latitudinal standard deviation profile for the same periods in the upper panel. The red circle indicates the maximum for the average profile for the whole period. The tick labels for the time for panels (a) and (b) are in the format dd/mm/yy.
Paper: Variability of the Sun’s Luminosity Places Constraints on the Thermal Equilibrium of the Convection Zone
Authors: L. E. A. Vieira, G. Kopp, T. Dudok de Wit, L. A. da Silva, F. Carlesso, A. R. Barbosa, A. Muralikrishna, R. Santos
Figure caption: Convection-zone thermal energetics place constraints on the variability of solar luminosity on solar-cycle to multicentury timescales. (a) Yearly average irradiance reconstructions for the TSI SATIRE and NRLTSI2 models are shown in blue and red, respectively. The recent solar-cycle minimum level (L ref/(4πr 2)), the average that would maintain convection-zone thermal equilibrium over Solar Cycle 23 (L eq/(4πr 2)), and the level at the Maunder Minimum for the TSI/SATIRE model are indicated by the three horizontal lines in the figure. (b) The corresponding thermal-energy evolution for each TSI model for depths in the convection zone between the surface and 24.2 Mm for an input-energy scenario in which the energy at the base of the convection zone is constant and equal to the level of that at the Maunder Minimum. Note that in this figure the solar radius is assumed to be constant (r = R ⊙).
Paper: The R-process Alliance: A Nearly Complete R-process Abundance Template Derived from Ultraviolet Spectroscopy of the R-process-enhanced Metal-poor Star HD 222925 
Authors: Ian U. Roederer, James E. Lawler, Elizabeth A. Den Hartog, Vinicius M. Placco, Rebecca Surman, Timothy C. Beers, Rana Ezzeddine, Anna Frebel, Terese T. Hansen, Kohei Hattori, Erika M. Holmbeck, Charli M. Sakari
Figure caption: Derived abundances for the elements with 20 ≤ Z ≤ 30 in HD 222925. The legend identifies the meanings of the symbols, and the dotted line represents the solar ratio. The vertical error bars mark 1σ statistical uncertainties. The points are slightly offset along the horizontal axis to improve clarity.
Paper: The R-process Alliance: A Nearly Complete R-process Abundance Template Derived from Ultraviolet Spectroscopy of the R-process-enhanced Metal-poor Star HD 222925 
Authors: Ian U. Roederer, James E. Lawler, Elizabeth A. Den Hartog, Vinicius M. Placco, Rebecca Surman, Timothy C. Beers, Rana Ezzeddine, Anna Frebel, Terese T. Hansen, Kohei Hattori, Erika M. Holmbeck, Charli M. Sakari
Figure caption: Illustration of the wavelengths of the lines that are detected and used to derive the abundances in HD 222925. Each dot represents a line. The atmospheric cutoff is marked and labeled. The gap between ≈3145 Å and ≈3330 Å reflects the gap between our STIS and MIKE spectra of HD 222925.
Paper: Long-term Optical Monitoring of the TeV BL Lacertae Object 1ES 2344 + 514
Authors: J. T. Cai, S. O. Kurtanidze, Y. Liu, O. M. Kurtanidze, M. G. Nikolashvili, H. B. Xiao, J. H. Fan
Figure caption: The SED fitting of 1ES 2344 + 514. The solid black line represents the EBL-corrected SED, the dashed red line represents the synchrotron radiation spectrum, and the dashed blue curve represents the IC emission curve from a synchrotron self-Compton (SSC) mechanism. The data set is twofold: SSDC-documented data (with flare data removed) are marked as black dots, and our R-band data are shown in red.
Paper: Long-term Optical Monitoring of the TeV BL Lacertae Object 1ES 2344 + 514
Authors: J. T. Cai, S. O. Kurtanidze, Y. Liu, O. M. Kurtanidze, M. G. Nikolashvili, H. B. Xiao, J. H. Fan
Figure caption: Periodic diagrams of 1ES 2344 + 514 in the optical R-band light curve as found by DCDFT+CLEANest. The black solid curve represents the Fourier power spectrum. The red and blue dashed curves represent the FAP levels of 95% and 99%, respectively.
Paper: An Excited-state OH Maser Survey toward WISE Point Sources
Authors: Xu-Jia Ouyang, Xi Chen, Zhi-Qiang Shen, Bin Li, Ya-Jun Wu, Hong-Ying Chen, Xiao-Qiong Li, Kai Yang, Shi-Min Song, Hai-Hua Qiao
Figure caption: Spectra of the 4765.56 MHz (2∏1/2, J−1/2, F = 1−0) OH masers detected in the TMRT survey. Blue and red lines denote the spectra on the LHCP and RHCP, respectively.
Paper: Long-term Optical Monitoring of the TeV BL Lacertae Object 1ES 2344 + 514
Authors: J. T. Cai, S. O. Kurtanidze, Y. Liu, O. M. Kurtanidze, M. G. Nikolashvili, H. B. Xiao, J. H. Fan
Figure caption: The SED fitting of a flare with quasi-simultaneous observation of 1ES 2344 + 514.
Paper: Long-term Optical Monitoring of the TeV BL Lacertae Object 1ES 2344 + 514
Authors: J. T. Cai, S. O. Kurtanidze, Y. Liu, O. M. Kurtanidze, M. G. Nikolashvili, H. B. Xiao, J. H. Fan
Figure caption: Jurkevich method result of 1ES 2344 + 514 in the optical R-band light curve. Red dots indicate components that were detected in DCDFT+CLEANest.
Paper: Long-term Optical Monitoring of the TeV BL Lacertae Object 1ES 2344 + 514
Authors: J. T. Cai, S. O. Kurtanidze, Y. Liu, O. M. Kurtanidze, M. G. Nikolashvili, H. B. Xiao, J. H. Fan
Figure caption: Periodic analysis of 1ES 2344 + 514 in the optical R-band light curve (black solid curve) was performed using the DCF. The DCFs of the theoretical light curves (blue solid curve) of the seven CLEANest components are given as a comparison.
Paper: Long-term Optical Monitoring of the TeV BL Lacertae Object 1ES 2344 + 514
Authors: J. T. Cai, S. O. Kurtanidze, Y. Liu, O. M. Kurtanidze, M. G. Nikolashvili, H. B. Xiao, J. H. Fan
Figure caption: The theoretical light curve (blue solid curve) and the observed light curve (black filled dots) are presented.
Paper: An Excited-state OH Maser Survey toward WISE Point Sources
Authors: Xu-Jia Ouyang, Xi Chen, Zhi-Qiang Shen, Bin Li, Ya-Jun Wu, Hong-Ying Chen, Xiao-Qiong Li, Kai Yang, Shi-Min Song, Hai-Hua Qiao
Figure caption: Spectra of the 6030.75 MHz (2∏3/2, J−5/2, F = 2−2) OH masers detected in the TMRT survey. Blue and red lines denote the spectra on the LHCP and RHCP, respectively.