adsabs/AstroCLIMB huggingface dataset:
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Same as Figure 26 but for TIC 63708251. A potential quadruple candidate in QLP data (see blue curve in upper panel and blue arrows), which is a false positive due to a nearby EB located about 5 pixels below the target. The vertical gray bands indicate momentum dumps. We note that there is another EB in the upper right corner of the pixel field of view.
Paper: New Pulsating Stars Detected in EA-type Eclipsing-binary Systems Based on TESS Data
Authors: Xiang-dong Shi, 相东 施, Sheng-bang Qian, 声帮 钱, Lin-Jia Li, 临甲 李
Figure caption: The position of new pulsating stars in EA-type eclipsing binaries on the pulsation and orbital-period relation diagram for oEA stars. The red solid circles refer to these new detected objects, and the sizes of the circles indicate their pulsation amplitude. Meanwhile, those objects (green open circles) published by Liakos et al. (2012) and the theoretical relation (black solid line) derived by Zhang et al. (2013) are also displayed.
Paper: New Pulsating Stars Detected in EA-type Eclipsing-binary Systems Based on TESS Data
Authors: Xiang-dong Shi, 相东 施, Sheng-bang Qian, 声帮 钱, Lin-Jia Li, 临甲 李
Figure caption: Top panel: Fourier spectra for the light curve outside eclipse of TIC139701741. Bottom panel: Same as top panel, but after prewhitening all the orbital-harmonic peaks. The red dotted lines represent the harmonics of the orbital frequency. The most prominent frequency of 16.91 cycles day−1 is the pulsation frequency from the component.
Paper: New Pulsating Stars Detected in EA-type Eclipsing-binary Systems Based on TESS Data
Authors: Xiang-dong Shi, 相东 施, Sheng-bang Qian, 声帮 钱, Lin-Jia Li, 临甲 李
Figure caption: The light curves of new eclipsing-binary systems with pulsating components (TJD = BJD − 2,457,000.0). The TESS ID of each target is marked in each panel. Some targets have obvious pulsating variations, but others only can be seen in an enlarged view.
Paper: New Pulsating Stars Detected in EA-type Eclipsing-binary Systems Based on TESS Data
Authors: Xiang-dong Shi, 相东 施, Sheng-bang Qian, 声帮 钱, Lin-Jia Li, 临甲 李
Figure caption: Example light curves of TIC139701741. The black open circles refer to the light curve during eclipse. The red solid circles represent the light curve outside eclipse and are used to analyze the pulsation frequency.
Paper: New Pulsating Stars Detected in EA-type Eclipsing-binary Systems Based on TESS Data
Authors: Xiang-dong Shi, 相东 施, Sheng-bang Qian, 声帮 钱, Lin-Jia Li, 临甲 李
Figure caption: Same as Figure 1 but for different targets.
Paper: New Pulsating Stars Detected in EA-type Eclipsing-binary Systems Based on TESS Data
Authors: Xiang-dong Shi, 相东 施, Sheng-bang Qian, 声帮 钱, Lin-Jia Li, 临甲 李
Figure caption: The light curves of TIC299160301 and TIC322208686 after removing the data during eclipse.
Paper: Erratum “Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. II. Dark Cloud Cores” (2018, ApJS, 239, 6)
Authors: Juris Kalvāns
Figure caption: Corrected CR-induced WGH temperature spectra for 0.05 μm grains. The different column densities N H of interstellar gas are indicated with interstellar extinction A  V  values, where N H = A  V  × 2 × 1021 H atoms cm−2.
Paper: Erratum “Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. II. Dark Cloud Cores” (2018, ApJS, 239, 6)
Authors: Juris Kalvāns
Figure caption: Recalculated spectra of energy received by 0.05 μm grains from CR impacts, shielded by different column densities of interstellar gas with N H = A  V  × 2 × 1021 H atoms cm−2.
Paper: Erratum “Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. II. Dark Cloud Cores” (2018, ApJS, 239, 6)
Authors: Juris Kalvāns
Figure caption: Corrected example CR energy spectra used in this study: the spectra of potassium CR ions calculated at different values of A  V . Here, N H = A  V  × 2 × 1021.
Paper: Erratum “Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. II. Dark Cloud Cores” (2018, ApJS, 239, 6)
Authors: Juris Kalvāns
Figure caption: Recalculated comparison of WGH frequencies for 0.1 μm grains f >70 for heating to temperatures T CR of 70 K and above. The second curve from this work is for a reduced CR flux with plane-parallel geometry, irradiated from both sides.
Paper: Erratum “Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. II. Dark Cloud Cores” (2018, ApJS, 239, 6)
Authors: Juris Kalvāns
Figure caption: Corrected CR-induced WGH temperature spectra for 0.2 μm grains. The column densities are indicated with A  V , as in Figure 6.
Paper: Erratum “Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. II. Dark Cloud Cores” (2018, ApJS, 239, 6)
Authors: Juris Kalvāns
Figure caption: Recalculated spectra of energy received by 0.1 μm grains from CR impacts, shielded by different column densities, as in Figure 3.
Paper: Erratum “Temperature Spectra of Interstellar Dust Grains Heated by Cosmic Rays. II. Dark Cloud Cores” (2018, ApJS, 239, 6)
Authors: Juris Kalvāns
Figure caption: Corrected CR-induced WGH temperature spectra for 0.1 μm grains. The column densities are indicated with A  V , as in Figure 6.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: First panel from top: same as Figure 17 but for quadruple candidate TIC 141733685, showing the sectors 35 and 36 eleanor data. The target exhibits three EBs with P  A   = 5.29 days, P  B   = 7.37 days, and P  C   = 43.63 days, as highlighted in the figure. Second panel: same as first panel but showing the FITSH lightcurve. Lower left panel: BLS transform of the ASAS-SN archival data for TIC 141733685 after removing binary A from the data train. The transform is plotted as a function of frequency in order to better identify harmonics. The orbital period of binary C is found to be 43.63 days (ν = 0.02292 cycles/day). This peak is marked as “1” for the first harmonic. Other harmonics and subharmonics are also marked in red. Nearly all of the highest peaks (i.e., above the dotted line) are due to this period or its associated harmonics. Lower right panel: folded, binned, and averaged lightcurve from the ASAS-SN archival data. There are 150 phase bins in the plot, each corresponding to ∼0.3 days. The phasing is referenced to one of the TESS-detected primary eclipses. There is also a likely secondary eclipse near phase 0.5, but its statistical significance is much less than that of the primary eclipse.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Photocenter analysis for P  A   = 5.29 days (first row from top), P  B   = 7.37 days (second row), and P  C   = 43.63 days (third row) for TIC 141733685 (left panels) and the nearby field star TIC 141733701 (right panels) using sector 35 data. The panels show the corresponding difference images along with the location of the respective target on the detector (black star, label “TIC”), the measured per-eclipse photocenters (small red symbols, label “Indiv Cent”), and the average photocenters (large red symbols, label “Avg Cent”). The dashed white contours indicate the aperture used by eleanor for the respective target. For PC , there is a single eclipse detected in this sector (see Figure 18), corresponding to a single photocenter measurement. Our analysis clearly rules out TIC 141733701 as a potential source of PA , PB , and P  C  (right panels) and confirms that all three EBs are associated with TIC 141733685 (left panels). We note that the sky orientation of Figure 19 is flipped along the x-axis (i.e., x → −x) with respect to the images shown here.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Upper panel: eleanorlightcurve for sextuple candidate TIC 1337279468, showing the sector 39 data. The target exhibits three EBs with P  A   = 4.45 days, P  B   = 5.94 days, and P  C   = 10.57 days, as highlighted in the panel. Second, third, and fourth rows: photocenter analysis of TIC 1337279468 for P  A  (second row), P  B  (third row), and P  C  (fourth row) for sector 39. The right panels show zoom-ins on the central pixel along with the corresponding confidence intervals (gray colors, 1σ, 2σ, and 3σ, respectively) of the scatter in the measured photocenters. We note that there are only two eclipses of binary P  C  in this sector, corresponding to two measured photocenters, and thus the measured offset of 0.1 pixels (fourth row, right panel) is not significant. Thus all three EBs originate from TIC 1337279468.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Skyview image of TIC 141733685 (black plus symbol) for sector 35, showing all Gaia sources brighter than G = 21 mag. There is a nearby field star, TIC 141733688 (dashed arrow), separated from the target by 4.″53, and with magnitude difference ΔT ≈ 3.15 mag. Another field star, TIC 141733701 (solid arrow), has a separation of 12.″6 and magnitude difference ΔT ≈ 2.03 mag. TIC 141733685 and TIC 141733688 have comparable parallax and, to a lesser degree, proper motion. See text for details.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: 5 × 5 pixels Skyview image of TIC 1337279468 for sector 39, showing all Gaia sources brighter than G = 21 mag. There are three nearby field stars (TIC 1337279457, TIC 1337279471, and TIC 1337279458), all with separations of ∼4″–5″ and magnitude differences ΔT = 5.5–6 mag each (marked with dashed red arrows). None of them is bright enough to produce any of the eclipses seen in the target’s lightcurve. The coordinates, parallax, and proper motion for TIC 1337279468 and TIC 1337279471 are within ∼1σ, suggesting a potential comoving septuple system.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Upper panel: eleanor (red) and QLP (blue) lightcurves for TIC 13120007, showing clear eclipses in the latter but no eclipses in the former. The vertical gray bands indicate momentum dumps. Lower left panel: TESS’s 13 × 13 pixel field of view centered on the target. The red contour indicates the aperture used by eleanor to extract the lightcurve. Lower right panel: pixel-by-pixel eleanor data for TIC 13120007 showing that the source of the EB is 2 pixels above the target.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Lightcurve of TIC 438226195, highlighting the extra events in sectors 6 and 33 (first and last green vertical bands) that mimic a circumbinary planet. Close inspection shows that the two events are due to a second EB with a period of ∼ 11.7 days, with a third event blended with the first secondary eclipse in sector 33 (second vertical green band), slightly deeper compared with the other secondaries in sector 33.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Measured ETVs for P  A  (left) and P  B  (right) for TIC 141733685, showing nonlinear effects and indicating that the two are likely to be gravitationally bound.
Paper: Ninety-seven Eclipsing Quadruple Star Candidates Discovered in TESS Full-frame Images
Authors: Veselin B. Kostov, Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Robert Gagliano, Thomas L. Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Jerome Orosz, Allan R. Schmitt, Hans M. Schwengeler, Ivan A. Terentev, Guillermo Torres, Thomas Barclay, Adam H. Friedman, Ethan Kruse, Greg Olmschenk, Andrew Vanderburg, William Welsh
Figure caption: Phase-folded DASCH data of TIC 172900988—an EB hosting a transiting circumbinary planet. The upper panel shows the data folded on the primary eclipse (dashed red line), and the lower panel shows the data folded on the secondary eclipse (dashed blue line). The two eclipses follow slightly different periods due to the apsidal motion of the binary caused by dynamical perturbation from the planet.
Paper: Free Inclinations for Trans-Neptunian Objects in the Main Kuiper Belt
Authors: Yukun Huang, 宇坤 黄, Brett Gladman, Kathryn Volk
Figure caption: Upper panel: our computed values of current I free for each TNO as a function of its barycentric semimajor axis a (note the log scale on the y-axis). Resonant objects are shown in orange and classical TNOs in blue, with light blue and dark blue denoting classical TNOs with I free < 4° and I free > 4°, respectively. The dashed curves in the lower-left portion of the plot give the center of the ν 8 (black) and ν 18 (gray) secular resonances, with curves on the left being e = 0 and those on the right being e = 0.1 (see text). Bottom panel: the range in calculated I free values (log scale) over our 10 Myr integrations as a function of a. For objects with a ≃ 39.7–42.5 au, the proximity of the ν 18 secular resonance results in the TNO’s expected precession rate being dramatically incorrect, resulting in widely varying values of I free when calculated using the linear theory (red crosses). When the nodal precession rate for nonresonant TNOs is corrected (using the double-average method), well-preserved free inclinations are obtained for the classical TNOs (blue dots); resonant TNOs (orange dots) can have highly variable values for their calculated I free even with the double-average method because the resonant dynamics are not accounted for.
Paper: Free Inclinations for Trans-Neptunian Objects in the Main Kuiper Belt
Authors: Yukun Huang, 宇坤 黄, Brett Gladman, Kathryn Volk
Figure caption: Left panel: polar and rectangular coordinate depiction of the ecliptic (orange), the forced (red), and the resultant free (blue) inclination vectors of a TNO in the main classical belt. For this object, the forcing center (red cross) rotates around the solar system’s invariable pole (black cross) with a ≃2  Myr period, the path of which is the black dashed circle. The free-inclination (blue) vector rotates around the time-varying forcing center at a constant nodal precession rate B, keeping its magnitude I free unchanged. The composition of these two movements gives rise to a more complicated inclination evolution in the ecliptic reference frame (orange vector with arrow denoting its approximate sense of motion). Right panel: the difference between a 4° cut in ecliptic inclination (orange circle centered at the origin) and a 4° cut in free inclination (blue circle centered at the forcing pole). Three TNOs with almost identical forcing centers are marked in blue crosses, with light blue being the cold object (I free < 4°) and dark blue being the hot object (I free > 4°). If one uses ecliptic inclinations to split the populations, 472231 (2014 FU71) would be misclassified as cold while 2015 GH59 (see Figure 4) would be misclassified as hot. TNOs in the overlapping area will maintain I free < 4° and are correctly classified currently but some with I free > 2°, such as 2014 UY228, will cycle to ecliptic I > 4° on megayear timescales.
Paper: Free Inclinations for Trans-Neptunian Objects in the Main Kuiper Belt
Authors: Yukun Huang, 宇坤 黄, Brett Gladman, Kathryn Volk
Figure caption: Evolution in a (upper panels; blue curves), ecliptic I (lower panels; blue curves), and I free (lower panels; red curves) over 10 Myr for the classical TNO 2015 GH59 (left) and the resonant TNO 119956 (2002 PA149;  right). The classical TNO has an initial J2000 I > 5°, but its I free is always less than 4° (see also Figure 1, right panel). The resonant object is in the 7/4 resonance, and its I free (as calculated by the double-average method) is not conserved; this is expected because neither linear secular theory nor the double-average method is appropriate for resonant TNOs.
Paper: Free Inclinations for Trans-Neptunian Objects in the Main Kuiper Belt
Authors: Yukun Huang, 宇坤 黄, Brett Gladman, Kathryn Volk
Figure caption: Blue curves: barycentric a (top panel) and ecliptic I (bottom panel) evolution of 2014 QU510 over 10 Myr. The orange dashed line in the upper panel marks the semimajor axis of the ν 18 secular resonance for circular and planar orbits. Red curves: I free calculated by the linear theory (dotted curve) and the semianalytical double-average method (solid curve). The ranges of the blue curve, the dotted curve, and the solid line are 3.°2, 14.°4, and 0.°06, respectively; the double-average method yields a much better-conserved value of I free.
Paper: Free Inclinations for Trans-Neptunian Objects in the Main Kuiper Belt
Authors: Yukun Huang, 宇坤 黄, Brett Gladman, Kathryn Volk
Figure caption: ΔI free measured across a 4 Gyr integration as a function of barycentric a for main-belt classical TNOs. The blue and red dots represent I free < 4° and I free > 4°, respectively. The majority of TNOs in both categories have values of I free that are conserved to within 1° even over 4 Gyr.
Paper: Free Inclinations for Trans-Neptunian Objects in the Main Kuiper Belt
Authors: Yukun Huang, 宇坤 黄, Brett Gladman, Kathryn Volk
Figure caption: A fractional histogram of free inclinations (blue bars) and ecliptic inclinations (red outlines) for 1450 main-belt classical TNOs beyond the 5/3 resonance (a > 42.3 au). Only a few such objects (not shown) have >40° inclinations. Note that because most TNO surveys have been conducted at relatively low latitudes, there is an observational bias against the large-inclination TNOs; thus, the high-I tail in this histogram should not be taken to represent the true hot TNO inclination distribution. However, the dramatic spike at low inclinations (which is due to the cold population) is still clear in the observed population and even more obvious in the I free histogram (which is shifted toward zero due to the true secular dynamics of the belt). A 4° cut is shown by the vertical line; few TNOs in the 0°–4° range would be hot-population interlopers.
Paper: Deep Learning of Dark Energy Spectroscopic Instrument Mock Spectra to Find Damped Lyα Systems
Authors: Ben Wang, Jiaqi Zou, Zheng Cai, J. Xavier Prochaska, Zechang Sun, Jiani Ding, Andreu Font-Ribera, Alma Gonzalez, Hiram K. Herrera-Alcantar, Vid Irsic, Xiaojing Lin, David Brooks, Soléne Chabanier, Roger de Belsunce, Nathalie Palanque-Delabrouille, Gregory Tarle, Zhimin Zhou
Figure caption: The three mock spectra of a QSO at z em ≈ 3.395, which exhibits two DLAs at z abs ≈ 2.733, 3.330 with N H I  ≈ 1020.69 cm−2, 1020.23 cm−2 that can be seen on the graph at wavelengths λ abs ≈ 4538 Å, 5142 Å, respectively. The S/N is shown at the upper left of each panel. The black line is the flux, and the red dashed line is the error.
Paper: Deep Learning of Dark Energy Spectroscopic Instrument Mock Spectra to Find Damped Lyα Systems
Authors: Ben Wang, Jiaqi Zou, Zheng Cai, J. Xavier Prochaska, Zechang Sun, Jiani Ding, Andreu Font-Ribera, Alma Gonzalez, Hiram K. Herrera-Alcantar, Vid Irsic, Xiaojing Lin, David Brooks, Soléne Chabanier, Roger de Belsunce, Nathalie Palanque-Delabrouille, Gregory Tarle, Zhimin Zhou
Figure caption: S/N distribution of four mocks. The three different mocks, desi-0.2-100, desi-0.2-4, and desi-0.2-1, are used to train the CNN model at different S/N. It can be seen that the mock desiY1-0.2-DLA has more spectra with S/N < 1.
Paper: Deep Learning of Dark Energy Spectroscopic Instrument Mock Spectra to Find Damped Lyα Systems
Authors: Ben Wang, Jiaqi Zou, Zheng Cai, J. Xavier Prochaska, Zechang Sun, Jiani Ding, Andreu Font-Ribera, Alma Gonzalez, Hiram K. Herrera-Alcantar, Vid Irsic, Xiaojing Lin, David Brooks, Soléne Chabanier, Roger de Belsunce, Nathalie Palanque-Delabrouille, Gregory Tarle, Zhimin Zhou
Figure caption: In the data structure of the DESIMOCK class, the wavelength array and the information of every spectrum are stored separately, including TARGETID, RA, DEC, etc.
Paper: Deep Learning of Dark Energy Spectroscopic Instrument Mock Spectra to Find Damped Lyα Systems
Authors: Ben Wang, Jiaqi Zou, Zheng Cai, J. Xavier Prochaska, Zechang Sun, Jiani Ding, Andreu Font-Ribera, Alma Gonzalez, Hiram K. Herrera-Alcantar, Vid Irsic, Xiaojing Lin, David Brooks, Soléne Chabanier, Roger de Belsunce, Nathalie Palanque-Delabrouille, Gregory Tarle, Zhimin Zhou
Figure caption: Purity results for different S/N levels and column densities using the desi-Y1 mock spectra. This is the result choosing the critical value of C min as 0.5. Some bins on the top have a value of 1; this is because there are few DLAs with logN H I  above 22 from the Y1 mock. For example, there are just two DLAs in the bin with S/N 4 to 5 and logN H I  above 22. The DLA finder detects them both and no FP samples, so the purity goes to 1. There are just five DLAs in the bin with S/N 3 to 4 and logN H I  above 22. The DLA finder detects three of them and produces two FP samples, so the purity goes down to 0.6. That is why the purity for HCD DLAs changes a lot in different bins.