adsabs/AstroCLIMB huggingface dataset:
Paper: TREASUREHUNT: Transients and Variability Discovered with HST in the JWST North Ecliptic Pole Time-domain Field
Authors: Rosalia O'Brien, Rolf A. Jansen, Norman A. Grogin, Seth H. Cohen, Brent M. Smith, Ross M. Silver, W. P. Maksym, Rogier A. Windhorst, Timothy Carleton, Anton M. Koekemoer, Nimish P. Hathi, Christopher N. A. Willmer, Brenda L. Frye, M. Alpaslan, M. L. N. Ashby, T. A. Ashcraft, S. Bonoli, W. Brisken, N. Cappelluti, F. Civano, C. J. Conselice, V. S. Dhillon, S. P. Driver, K. J. Duncan, R. Dupke, M. Elvis, G. G. Fazio, S. L. Finkelstein, H. B. Gim, A. Griffiths, H. B. Hammel, M. Hyun, M. Im, V. R. Jones, D. Kim, B. Ladjelate, R. L. Larson, S. Malhotra, M. A. Marshall, S. N. Milam, J. D. R. Pierel, J. E. Rhoads, S. A. Rodney, H. J. A. Röttgering, M. J. Rutkowski, R. E. Ryan, M. J. Ward, C. W. White, R. J. van Weeren, X. Zhao, J. Summers, J. C. J. D'Silva, R. Ortiz, A. S. G. Robotham, D. Coe, M. Nonino, N. Pirzkal, H. Yan, T. Acharya
Figure caption: Full extent of HST ACS/WFC coverage of the JWST NEP TDF. Regions of overlap between visits in the mosaic are highlighted in progressively darker shades of gray for areas of two-, three-, and four-epoch overlap. This paper focuses on these regions of overlap, with a total area of 87.94 arcmin2, to investigate transients and variable sources. Red circles mark the positions of the 12 identified transients, while blue squares and diamonds mark the 190 unique variable candidates discovered in this study. We expect ∼80 of these sources to be false positives (see Section 3.2). Symbol shapes and colors identify the samples from which individual variables were selected, as indicated by the legend at the top of the figure. For comparison, the JWST/NIRCam coverage of this field is outlined in orange. We estimate photometric redshifts (Section 4.3) for objects with both HST and JWST photometry. One visit (jeex02; at lower right) with a bad astrometric solution was ignored in this work.
Paper: Infrared Properties of Carbon Stars in Our Galaxy
Authors: Kyung-Won Suh
Figure caption: IRAS–2MASS 2CDs for various subclasses of CS_IC objects (see Table 1) and special subgroups of CAGB stars (see Section 3) compared with theoretical models (see Section 4). For CAGB models (AMC, T  c  = 1000 K): τ 10 = 0.0001, 0.01, 0.1, 0.5, 1, 2, and 4 from left to right. For each subclass, the number of objects is shown. The number in parenthesis denotes the number of objects plotted on the 2CD with good-quality observed colors. See Section 3.1.
Paper: Infrared Properties of Carbon Stars in Our Galaxy
Authors: Kyung-Won Suh
Figure caption: IRAS–2MASS CMDs for carbon stars with IRAS counterparts spanning various subclasses (see Table 1). For CAGB models (AMC, T  c  = 1000 K): τ 10 = 0.0001, 0.01, 0.1, 0.5, 1, 2, and 4 from left to right (see Section 4). For each subclass, the number of objects is shown. The number in parenthesis denotes the number of objects plotted with good-quality observed data. See Section 3.4.
Paper: TREASUREHUNT: Transients and Variability Discovered with HST in the JWST North Ecliptic Pole Time-domain Field
Authors: Rosalia O'Brien, Rolf A. Jansen, Norman A. Grogin, Seth H. Cohen, Brent M. Smith, Ross M. Silver, W. P. Maksym, Rogier A. Windhorst, Timothy Carleton, Anton M. Koekemoer, Nimish P. Hathi, Christopher N. A. Willmer, Brenda L. Frye, M. Alpaslan, M. L. N. Ashby, T. A. Ashcraft, S. Bonoli, W. Brisken, N. Cappelluti, F. Civano, C. J. Conselice, V. S. Dhillon, S. P. Driver, K. J. Duncan, R. Dupke, M. Elvis, G. G. Fazio, S. L. Finkelstein, H. B. Gim, A. Griffiths, H. B. Hammel, M. Hyun, M. Im, V. R. Jones, D. Kim, B. Ladjelate, R. L. Larson, S. Malhotra, M. A. Marshall, S. N. Milam, J. D. R. Pierel, J. E. Rhoads, S. A. Rodney, H. J. A. Röttgering, M. J. Rutkowski, R. E. Ryan, M. J. Ward, C. W. White, R. J. van Weeren, X. Zhao, J. Summers, J. C. J. D'Silva, R. Ortiz, A. S. G. Robotham, D. Coe, M. Nonino, N. Pirzkal, H. Yan, T. Acharya
Figure caption: Histogram of the distribution of magnitudes differences measured between two epochs (Δm 0.24) for 4059 galaxies between 28.0 mag < m AB < 28.5 mag. We compare the sample of CR-affected galaxies (red) to the full sample (black). The points show the fraction of CR-affected galaxies (N) for each Δm 0.24 bin, where the error bar is ﹩\sqrt{N}﹩. The solid lines are Gaussian fits to the data. The black solid line represents the Gaussian fit to the full sample. Our empirical uncertainties estimated in Figure 3 already account for CR effects, as shown by the black line closely following the red line.
Paper: Infrared Properties of Carbon Stars in Our Galaxy
Authors: Kyung-Won Suh
Figure caption: WISE–2MASS CMDs for carbon stars spanning various subclasses (see Tables 1 and 2). For CAGB models (AMC, T  c  = 1000 K): τ 10=0.0001, 0.01, 0.1, 0.5, 1, 2, and 4 from left to right (see Section 4). For each subclass, the number of objects is shown. The number in parenthesis denotes the number of objects plotted with good-quality observed data. See Section 3.4.
Paper: Infrared Properties of Carbon Stars in Our Galaxy
Authors: Kyung-Won Suh
Figure caption: WISE–2MASS 2CDs for CS_IC and CS_NI objects (see Tables 1 and 2) compared with theoretical models (see Section 4). For CAGB models (AMC, T  c  = 1000 K): τ 10 = 0.0001, 0.01, 0.1, 0.5, 1, 2, and 4 from left to right. For each subclass, the number of objects is shown. The number in parenthesis denotes the number of objects plotted on the 2CD with good-quality observed colors. See Section 3.3.
Paper: Infrared Properties of Carbon Stars in Our Galaxy
Authors: Kyung-Won Suh
Figure caption: Error-bar plots of averaged colors and magnitudes for various subclasses of carbon stars. For each subclass, the number of objects is shown. The number in parenthesis denotes the number of objects plotted with good-quality observed data. See Section 3.5.
Paper: Infrared Properties of Carbon Stars in Our Galaxy
Authors: Kyung-Won Suh
Figure caption: Histograms of the K[2.2]−W3[12] colors for CAGB stars (CAGB_IC objects) with thick dust shells. CAGB stars that can be classified as C-rich stars based on the Gaia DR3 spectra are compared with all CAGB stars. See Section 3.3.
Paper: Infrared Properties of Carbon Stars in Our Galaxy
Authors: Kyung-Won Suh
Figure caption: Error-bar plot of the WISE–2MASS 2CD for all carbon stars (CS_IC and CS_NI objects; see Figure 4). See Section 3.3.
Paper: Exploring the Maximum Magnitude versus Rate of Decline Relation for Novae in M31
Authors: J. Grace Clark, Kamil Hornoch, Allen W. Shafter, Hana Kučáková, Jan Vraštil, Peter Kušnirák, Marek Wolf
Figure caption: The MMRD relation for M31. The data show a weak correlation between the absolute magnitude of a nova at the peak of its eruption and the time for the nova to fade 2 mag from maximum light. Following Shafter et al. (2023), the MMRD plane is divided into four quadrants as indicated by the light gray lines. Linear, Break, and Jitter class novae as well as the known recurrent novae are distinguished as indicated in the legend. Broadly speaking, the Break and Jitter class novae are found primarily among the fastest and slowest novae, respectively, with the known recurrent systems being mostly confined to the lower-left quadrant (Q2) of the MMRD plane. The dashed line represents the best-fitting linear MMRD relation (excluding known recurrent novae) with the dotted lines showing ±1σ departures from this relation. Novae that significantly depart from the MMRD relation (e.g., known and suspected recurrent novae) are identified.
Paper: Stellar Atmospheric Parameters of ∼11,000 RR Lyrae Stars from LAMOST Spectra
Authors: Jiangtao Wang, Jianrong Shi, Jianning Fu, Weikai Zong, Chunqian Li
Figure caption: The variations of stellar atmospheric parameters during the pulsation cycle. The left panels represent the LRS, while the right panels are for MRS. From the top to the bottom panels, the variations in T eff, ﹩\mathrm{log}\,g﹩, and [M/H] with phase are shown. The method for determining the mean value curves (black lines) and error bars is the same as that employed in Figure 6.
Paper: Stellar Atmospheric Parameters of ∼11,000 RR Lyrae Stars from LAMOST Spectra
Authors: Jiangtao Wang, Jianrong Shi, Jianning Fu, Weikai Zong, Chunqian Li
Figure caption: The variations of RVs during the pulsation cycle. The left panels represent the RVHα  while the right panels are for the RVmetal, and the top two panels show the RV of RRab (RV ab), while the bottom panels are for RRc (RV c). The blue and orange data correspond to LRS and MRS, respectively. The black line is the mean within the phase of 0.1 bins, and the error bars indicate the standard deviation. The center of mass radial velocity (RV 0) is obtained from the RRL catalog of Gaia DR3 (Clementini et al. 2023).
Paper: Stellar Atmospheric Parameters of ∼11,000 RR Lyrae Stars from LAMOST Spectra
Authors: Jiangtao Wang, Jianrong Shi, Jianning Fu, Weikai Zong, Chunqian Li
Figure caption: The comparison of T eff with the other data sets. The blue, orange, and green data correspond to Gaia, APOGEE, and SEGUE, respectively. The numbers indicate the count of common targets. The residuals of T eff between other data sets and our values are shown at the bottom, along with their mean (μ) and standard deviation (σ) in the text. The black solid and dashed lines indicate the bisector and zero position, respectively. The left panel displays the T eff of LRS, and the right panel is for MRS.
Paper: Stellar Atmospheric Parameters of ∼11,000 RR Lyrae Stars from LAMOST Spectra
Authors: Jiangtao Wang, Jianrong Shi, Jianning Fu, Weikai Zong, Chunqian Li
Figure caption: The comparison of [M/H] with the other data sets. The red points represent the data from Liu et al. (2019), and the other colors and legends are the same as in Figure 8 but for [M/H].
Paper: Stellar Atmospheric Parameters of ∼11,000 RR Lyrae Stars from LAMOST Spectra
Authors: Jiangtao Wang, Jianrong Shi, Jianning Fu, Weikai Zong, Chunqian Li
Figure caption: The comparison of ﹩\mathrm{log}\,g﹩ with the other data sets. The colors of data points and legends are the same as in Figure 8 but for ﹩\mathrm{log}\,g﹩.
Paper: Advancing Solar Energetic Particle Event Prediction through Survival Analysis and Cloud Computing. I. Kaplan–Meier Estimation and Cox Proportional Hazards Modeling
Authors: India Jackson, Petrus Martens
Figure caption: Survival curves for the ≥10 MeV threshold.
Paper: Advancing Solar Energetic Particle Event Prediction through Survival Analysis and Cloud Computing. I. Kaplan–Meier Estimation and Cox Proportional Hazards Modeling
Authors: India Jackson, Petrus Martens
Figure caption: Distribution of SEP time to detection.
Paper: Advancing Solar Energetic Particle Event Prediction through Survival Analysis and Cloud Computing. I. Kaplan–Meier Estimation and Cox Proportional Hazards Modeling
Authors: India Jackson, Petrus Martens
Figure caption: Schoenfeld residuals plot for the ≥10 MeV threshold.
Paper: Advancing Solar Energetic Particle Event Prediction through Survival Analysis and Cloud Computing. I. Kaplan–Meier Estimation and Cox Proportional Hazards Modeling
Authors: India Jackson, Petrus Martens
Figure caption: Parametric survival curve for (X, ≥10).
Paper: Advancing Solar Energetic Particle Event Prediction through Survival Analysis and Cloud Computing. I. Kaplan–Meier Estimation and Cox Proportional Hazards Modeling
Authors: India Jackson, Petrus Martens
Figure caption: Parametric survival curve for (M, ≥10).
Paper: Advancing Solar Energetic Particle Event Prediction through Survival Analysis and Cloud Computing. I. Kaplan–Meier Estimation and Cox Proportional Hazards Modeling
Authors: India Jackson, Petrus Martens
Figure caption: Parametric survival curve for (C, ≥10).
Paper: UPCluster-SZ: The Updated Catalog of Galaxy Clusters from the List of Planck Sunyaev–Zel’dovich Sources
Authors: Hyeonguk Bahk, Ho Seong Hwang
Figure caption: The scaling relations between (a) X-ray luminosity in the 0.5–2.0 keV band (L 500), M SZ, and redshift; and (b) the MCMF richness parameter (λ) and M SZ. Both the L 500 and λ values are sourced from the RASS-MCMF catalog. Colored markers represent confirmed clusters whose redshifts were determined through analysis of the galaxy redshift catalog, with colors corresponding to those used in Figures 4 and 8. Open circles show the total set of PSZ2 counterparts in the RASS-MCMF clusters, where we show their 1σ error bars except for L 500. The power-law form and its parameters for the L 500–M SZ–z scaling relation are derived from Bulbul et al. (2019). Solid and dashed lines represent the best-fit relation and the 3σ intrinsic scatter range, respectively.
Paper: UPCluster-SZ: The Updated Catalog of Galaxy Clusters from the List of Planck Sunyaev–Zel’dovich Sources
Authors: Hyeonguk Bahk, Ho Seong Hwang
Figure caption: The X-ray flux at 0.5–2.0 keV and the fraction of clusters η X with X-ray counterparts from the RASS-MCMF catalog, plotted against the integrated Compton y-parameter (﹩{Y}_{5{R}_{500}}﹩) and the S/N of the SZ signal. The colored markers represent the confirmed clusters blindly detected using our galaxy catalog method following the same color scheme as in Figure 4, corresponding to thresholds of 7 (blue), 9 (orange), and 10 (red). The SZ parameters (﹩{Y}_{5{R}_{500}}﹩ and S/N) are binned to ensure an equal number of elements within each bin.
Paper: UPCluster-SZ: The Updated Catalog of Galaxy Clusters from the List of Planck Sunyaev–Zel’dovich Sources
Authors: Hyeonguk Bahk, Ho Seong Hwang
Figure caption: The distribution of cluster detections obtained from our method (Section 3.3) for the confirmed PSZ2 clusters with respect to the normalized galaxy counts and (a) separation and (b) ﹩\bar{R}﹩. The normalized galaxy count is the galaxy count normalized by the number of member galaxies of the detections of their closest redshift. The separation d is the offset of the optical galaxy center from the PSZ2 center, and ﹩\bar{R}﹩ is the mean distance of the galaxies from the PSZ2 center. In panel (b), blue represents detections that satisfy the separation criterion (d < 1.5 Mpc), while black dots represent all detections prior to the separation cut. The red shaded area indicates the region where detections may result in false-positive selections.
Paper: UPCluster-SZ: The Updated Catalog of Galaxy Clusters from the List of Planck Sunyaev–Zel’dovich Sources
Authors: Hyeonguk Bahk, Ho Seong Hwang
Figure caption: Mass–redshift distribution of galaxy clusters in our UPCluster-SZ. The black dots represent the confirmed cluster of the original PSZ2 whose redshift information is available. The red dots represent the confirmed clusters updated from the cluster catalogs, and the green dots show the strong candidates classified based on our method using the galaxy catalog. The blue squares indicate the candidates of cluster detection with only ﹩\bar{R}\gt 2﹩ Mpc, which is excluded for the strong candidates. Histograms for the redshift and mass are displayed along each axis, with the same colors for the main panel. Candidate clusters and confirmed clusters without any redshift measurements are not shown in this figure.
Paper: A Sample of Am and Ap Candidates from LAMOST DR10 (v1.0) Based on the Ensemble Regression Model
Authors: Hai-Feng Yang, 海峰 杨, Rui Wang, 瑞 王, Jiang-Hui Cai, 江辉 蔡, A-Li Luo, 阿理 罗, Bing Du, 冰 杜, Yan-Ting He, 艳婷 贺, Mei-Hong Su, 美红 苏, Chen-Hui Shi, 晨辉 史, Xu-Jun Zhao, 旭俊 赵, Ya-Ling Xun, 亚玲 荀, Yi-Nan Yuan, 艺楠 员
Figure caption: The distributions in the H-R diagram of Am and Ap candidates are shown in the left and right panels, respectively. The color is coded by the metallicity [Fe/H]. The dashed lines in both panels represent the isochrones from the PARSEC model with the same age 1 Gyr but different metallicities, i.e., −1.4, −0.8, −0.2, and 0.4 dex, respectively.
Paper: A Sample of Am and Ap Candidates from LAMOST DR10 (v1.0) Based on the Ensemble Regression Model
Authors: Hai-Feng Yang, 海峰 杨, Rui Wang, 瑞 王, Jiang-Hui Cai, 江辉 蔡, A-Li Luo, 阿理 罗, Bing Du, 冰 杜, Yan-Ting He, 艳婷 贺, Mei-Hong Su, 美红 苏, Chen-Hui Shi, 晨辉 史, Xu-Jun Zhao, 旭俊 赵, Ya-Ling Xun, 亚玲 荀, Yi-Nan Yuan, 艺楠 员
Figure caption: The comparison of effective temperature, surface gravity, and metallicity between KURUCZ and Gaia of the Am and Ap candidates, respectively.
Paper: A Sample of Am and Ap Candidates from LAMOST DR10 (v1.0) Based on the Ensemble Regression Model
Authors: Hai-Feng Yang, 海峰 杨, Rui Wang, 瑞 王, Jiang-Hui Cai, 江辉 蔡, A-Li Luo, 阿理 罗, Bing Du, 冰 杜, Yan-Ting He, 艳婷 贺, Mei-Hong Su, 美红 苏, Chen-Hui Shi, 晨辉 史, Xu-Jun Zhao, 旭俊 赵, Ya-Ling Xun, 亚玲 荀, Yi-Nan Yuan, 艺楠 员
Figure caption: The impact of S/Ng and T eff on the [Fe/H] value.
Paper: A Sample of Am and Ap Candidates from LAMOST DR10 (v1.0) Based on the Ensemble Regression Model
Authors: Hai-Feng Yang, 海峰 杨, Rui Wang, 瑞 王, Jiang-Hui Cai, 江辉 蔡, A-Li Luo, 阿理 罗, Bing Du, 冰 杜, Yan-Ting He, 艳婷 贺, Mei-Hong Su, 美红 苏, Chen-Hui Shi, 晨辉 史, Xu-Jun Zhao, 旭俊 赵, Ya-Ling Xun, 亚玲 荀, Yi-Nan Yuan, 艺楠 员
Figure caption: Averaged spectral maps of Am and Ap stars.
Paper: A Sample of Am and Ap Candidates from LAMOST DR10 (v1.0) Based on the Ensemble Regression Model
Authors: Hai-Feng Yang, 海峰 杨, Rui Wang, 瑞 王, Jiang-Hui Cai, 江辉 蔡, A-Li Luo, 阿理 罗, Bing Du, 冰 杜, Yan-Ting He, 艳婷 贺, Mei-Hong Su, 美红 苏, Chen-Hui Shi, 晨辉 史, Xu-Jun Zhao, 旭俊 赵, Ya-Ling Xun, 亚玲 荀, Yi-Nan Yuan, 艺楠 员
Figure caption: Comparison of the distribution of old and new candidates for Am and Ap over different atmospheric parameters.
Paper: A Sample of Am and Ap Candidates from LAMOST DR10 (v1.0) Based on the Ensemble Regression Model
Authors: Hai-Feng Yang, 海峰 杨, Rui Wang, 瑞 王, Jiang-Hui Cai, 江辉 蔡, A-Li Luo, 阿理 罗, Bing Du, 冰 杜, Yan-Ting He, 艳婷 贺, Mei-Hong Su, 美红 苏, Chen-Hui Shi, 晨辉 史, Xu-Jun Zhao, 旭俊 赵, Ya-Ling Xun, 亚玲 荀, Yi-Nan Yuan, 艺楠 员
Figure caption: Spatial distribution of Am and Ap candidates.
Paper: A Sample of Am and Ap Candidates from LAMOST DR10 (v1.0) Based on the Ensemble Regression Model
Authors: Hai-Feng Yang, 海峰 杨, Rui Wang, 瑞 王, Jiang-Hui Cai, 江辉 蔡, A-Li Luo, 阿理 罗, Bing Du, 冰 杜, Yan-Ting He, 艳婷 贺, Mei-Hong Su, 美红 苏, Chen-Hui Shi, 晨辉 史, Xu-Jun Zhao, 旭俊 赵, Ya-Ling Xun, 亚玲 荀, Yi-Nan Yuan, 艺楠 员
Figure caption: Statistical distributions of different combinations of parameters for Am and Ap candidates.
Paper: A Sample of Am and Ap Candidates from LAMOST DR10 (v1.0) Based on the Ensemble Regression Model
Authors: Hai-Feng Yang, 海峰 杨, Rui Wang, 瑞 王, Jiang-Hui Cai, 江辉 蔡, A-Li Luo, 阿理 罗, Bing Du, 冰 杜, Yan-Ting He, 艳婷 贺, Mei-Hong Su, 美红 苏, Chen-Hui Shi, 晨辉 史, Xu-Jun Zhao, 旭俊 赵, Ya-Ling Xun, 亚玲 荀, Yi-Nan Yuan, 艺楠 员
Figure caption: Statistical distribution of subclasses of Am and Ap candidates provided by LAMOST.
Paper: Every Data Point Counts: Stellar Flares as a Case Study of Atmosphere-aided Studies of Transients in the LSST Era
Authors: Riley W. Clarke, James R. A. Davenport, John Gizis, Melissa L. Graham, Xiaolong Li, Willow Fortino, Easton J. Honaker, Ian Sullivan, Yusra Alsayyad, James Bosch, Robert A. Knop, Federica B. Bianco
Figure caption: Angular offset from true position for a source with a 10,000 K blackbody spectrum for air masses 1.1 ≤ X ≤ 2.1 in all six LSST bands. A zoomed-in section is shown to reveal the separations between the curves corresponding to separate bandpasses.
Paper: Every Data Point Counts: Stellar Flares as a Case Study of Atmosphere-aided Studies of Transients in the LSST Era
Authors: Riley W. Clarke, James R. A. Davenport, John Gizis, Melissa L. Graham, Xiaolong Li, Willow Fortino, Easton J. Honaker, Ian Sullivan, Yusra Alsayyad, James Bosch, Robert A. Knop, Federica B. Bianco
Figure caption: Scatter plots of 1015 flare candidates in the DECam DDF survey of the COSMOS field (the selection criteria are discussed in Section 4.2). The x-axis is the change in g magnitude between the objects and the y-axis is the change in the component of the source’s movement in the direction of the zenith. Each point represents one unique candidate ID with at least two DIA “objects” (two distinct observations). The change in magnitude and in position are calculated as the difference between the two objects with the largest absolute change in magnitude. Left panel: for observations with air mass X < 1.2, points are shown as gray circles. Points are colored by the air mass of the initial detection for air masses X > 1.2. Right panel: each point is colored by the change in air mass between the two objects and histograms show the marginalized distributions of g-magnitude change (top) and zenith-bound displacement (right). Three candidates of interest, as described Section 4.2, are circled. The single candidate whose quiescent counterpart can be identified in the Gaia DR3 data set, DC21engi, is marked by an arrow.
Paper: Every Data Point Counts: Stellar Flares as a Case Study of Atmosphere-aided Studies of Transients in the LSST Era
Authors: Riley W. Clarke, James R. A. Davenport, John Gizis, Melissa L. Graham, Xiaolong Li, Willow Fortino, Easton J. Honaker, Ian Sullivan, Yusra Alsayyad, James Bosch, Robert A. Knop, Federica B. Bianco
Figure caption: Visual description of the conversion from Equation (6) to (7). Because the expected positional offsets are small (≤0.″3, see Figure 5), the celestial sphere can be locally approximated as a Cartesian plane. The distances to the zenith and NCP are assumed to be large compared to the offset between the two source positions. P 1 and P 2 are the parallactic angles at the time of quiescence and event, respectively. η 1 and η 2 are the angles between  d  and ﹩\hat{{z}_{1}}﹩ and ﹩\hat{{z}_{2}}﹩, respectively. η 2 can thus be calculated as ﹩{\eta }_{2}=\left(\displaystyle \frac{\pi }{2}-{P}_{2}-\arctan \tfrac{{\rm{\Delta }}\delta }{{\rm{\Delta }}\alpha }\right)﹩. The difference between η 1 and η 2 is expected to be very small, but it is amplified in this illustration to be obvious to the reader’s eye.
Paper: Every Data Point Counts: Stellar Flares as a Case Study of Atmosphere-aided Studies of Transients in the LSST Era
Authors: Riley W. Clarke, James R. A. Davenport, John Gizis, Melissa L. Graham, Xiaolong Li, Willow Fortino, Easton J. Honaker, Ian Sullivan, Yusra Alsayyad, James Bosch, Robert A. Knop, Federica B. Bianco
Figure caption: WISE W1 band images; the coordinates of candidate flares DC21flly, DC21fjnb, DC21fygb, and DC21engi are marked as labeled. In all panels, north is up and east is left. Each panel is 3.8′ on the side. A 12″ radius circle centered on each detection reported in Table 1 is plotted (where only one circle is visible, as for DC21engi, the detections are overlapping). No source can unambiguously be identified at the location of the transients, except for DC21engi.
Paper: Every Data Point Counts: Stellar Flares as a Case Study of Atmosphere-aided Studies of Transients in the LSST Era
Authors: Riley W. Clarke, James R. A. Davenport, John Gizis, Melissa L. Graham, Xiaolong Li, Willow Fortino, Easton J. Honaker, Ian Sullivan, Yusra Alsayyad, James Bosch, Robert A. Knop, Federica B. Bianco
Figure caption: Image triplets for DECam DDF candidates, as shown by the DECAT LBL Pipeline Candidate Viewer. From top to bottom, the candidates are DC21fjnb, DC21fygb, DC21flly, and DC21engi. “New” denotes the search image, “Ref” the reference image, and “Sub” the difference image. A quiescent source consistent with a dM is seen in the reference image for DC21engi.