adsabs/AstroCLIMB huggingface dataset:
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: The magnitude of a star image displacement during a flare compared to the quiescent star position as a function of flare temperature in LSST g band for four different air-mass values. The astrometric accuracy requirements of the Rubin system are shown as bands straddling the minimum requirement and the “stretch goal” (Ivezić & The LSST Science Collaboration 2018, see also Section 3), shown in light gray for absolute astrometric accuracy and darker gray for relative astrometric accuracy for star pairs separated by 5′. The ΔDCR should be measurable above the relative astrometric accuracy limit of the Rubin system as built (as discussed in Section 5). We do not expect measurements in the darkest gray region to be detectable.
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: Expected magnitude of the ΔDCR effect for a flare SED approximated by a 10,000 K blackbody as a function of air mass and filter in the Rubin Observatory ugrizy observing system (Olivier et al. 2008). Blue coloring corresponds to a ΔDCR shift detectable by Rubin, and red coloring corresponds to an undetectable shift, given the absolute astrometric accuracy goal of 0.″1.
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: In pink, the spectrum of an M5 dwarf (composite spectrum built partially from SDSS observations, Davenport et al. 2012). In blue, the spectrum of a 10,000 K blackbody used to simulate a flare. In purple, the sum of the two aforementioned spectra, representing the spectrum of the dM during the flare event, is shown. The blackbody and dM spectra contain the same total energy over the SDSS optical range (3850–9200 Å), indicated by the vertical dashed lines. The transmission functions for the LSST ugrizy photometric system are shown in gray.
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: Location of DECam DDF flare candidate g-band objects in the COSMOS field. The field centers and DECam’s field of view are indicated by the black x symbols and circles, respectively
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: Air-mass distribution of the current LSST survey strategy proposal (baseline_v3.0_10yrs; The Rubin Observatory Survey Cadence Optimization Committee 2023). Cumulative distribution showing the number of visits at or below a given air mass. Plot produced within the Rubin Metric Analysis Framework (Jones et al. 2014).
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: Light incident from a star is deflected by the atmosphere. The offset depends on the color (i.e., temperature) of the source and the amount of atmosphere the light passes through. The chromatic change during a flare event should produce an excess in the normal DCR at quiescence, labeled as ΔDCR in the figure.
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: Simulation of the impact of three possible DCR correction strategies applied in g-band DIA. The pixel scale of the LSST system (0.″2 pixel−1) is indicated by the grid and the zenith direction by an arrow. (a) A quiescent dM source observed at air mass X = 1.22. (b) The source is observed during a T = 10,000 K flare at the same air mass. In both panels (b) and (d), the flare flux is normalized such that the total flux during the flare is 50% greater than the total flux in quiescence. The difference of the flare and quiescent images is shown in the (c); contours help the reader quantify the PSF width and centroid in the difference image. The quiescent component is subtracted cleanly in DIA and the residuals associated with the flare directly quantify ΔDCR. Matching the DCR templates with correct assumptions on the quiescent SED would replicate this result. In (d), the same flare is observed at air mass X = 1.74. DCR shifts the centroid of the quiescent source in the zenith direction by ∼42″. This shift is corrected in the visualization. The flaring PSF center is offset from the center of the image by 0.″21 due to ΔDCR, and the PSF is significantly elongated in the zenith direction (with PSF variance increase ΔV = 0.14 arcsec2). (e) The quiescent and flare images are differenced after modeling the DCR effects on the quiescent source using the true dM SED. The quiescent components is removed cleanly and the residuals can be used to measure ΔDCR directly as in (c). (f) For the flare observed at air mass X = 1.74 (d), the same DCR corrections as for (e) are applied, but based on a G2V (solar-type) quiescent SED: the flare and quiescent images are differenced, resulting in nonzero residuals for the quiescent component and distorted residuals for the flare component.
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: Schematic of the position change of candidate DC21engi during a DECam transient event captured in two detections, at times t 1 (2021 April 09 02:23:03.576) and t 2 (2021 April 09 02:41:18.079). The Gaia DR3 coordinates of the source are shown in black, and the coordinate axes are shifted such that the Gaia position is at the origin. The source is assumed to be quiescent at t quiescent (2021 April 09 02:00:00), and the direction to zenith at t quiescent and the position of the source in the DECam DIA subtraction are shown in blue. The maximum permitted median astrometric residual (0.″15) across the entire field is indicated by the error bars on the DECam event positions. Arrows point to the zenith-bound direction at the time of the observation, showing the axis along which the next observation should be found if its motion were dominated by DCR.
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: Probability of detecting ΔDCR induced by a flare at or above the peak effective temperature T for four different astrometric accuracy limits. The probability of DCR detection is measured as the conditional probability P(X > X crit∣T eff > T), where X crit(T, q) is the minimum air mass necessary for a flare of temperature T to produce a ΔDCR greater than the astrometric accuracy q. The temperature distribution follows the measured flare temperatures in Howard et al. (2020). The small number of flares at large T causes the discontinuities in the probability at T eff > 20,000 K.
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: Top: distribution of observation air masses over five LSST recent observing strategy proposals (as labeled). While it remains small, the planned fraction of high-air-mass observations in LSST has grown over time. Bottom: the corresponding probability of measuring a ΔDCR: as Figure 14, but fixing q = 0.05 and for the same five simulations of the LSST as in the top panel.
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: Center: ΔDCR induced as a function of flare temperature and air mass in LSST g band. Right: box-and-whiskers plot of peak effective flare temperatures measured by Howard et al. (2020). Top: histogram of the per-visit air mass in the current LSST baseline observing strategy (baseline_v3.0_10yrs; The Rubin Observatory Survey Cadence Optimization Committee 2023). The median air mass and temperature are indicated by orange lines.
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: Air-mass sky distribution of the current LSST survey strategy proposal (baseline_v3.0_10yrs; The Rubin Observatory Survey Cadence Optimization Committee 2023): sky maps are shown for the median air mass (left) and maximum air mass (right) in the g band. Plots are produced within the Rubin Metric Analysis Framework (Jones et al. 2014). To produce these maps, a sky segmentation into HEALPixels with a resolution of 64 was performed (Górski et al. 2005).
Paper: A Catalog of Early-type Runaway Stars from LAMOST DR8
Authors: Yanjun Guo, Luqian Wang, 璐茜 王, Chao Liu, 超 刘, You Wu, 优 吴, ZhanWen Han, 占文 韩, XueFei Chen, 雪飞 陈
Figure caption: (a) The top panel shows the RV curve for the binary candidate systems Gaia source ID 454293469890174976. RV measurements were collected from the prior study by Zhang et al. (2021). The bottom panel displays the observed RVs minus the calculated values obtained from the circular orbital fitting using the global minimization technique from Iglesias-Marzoa et al. (2015). RV curve for Gaia source ID 3453566198941548160 (b) is shown in the same format as (a).
Paper: A Catalog of Early-type Runaway Stars from LAMOST DR8
Authors: Yanjun Guo, Luqian Wang, 璐茜 王, Chao Liu, 超 刘, You Wu, 优 吴, ZhanWen Han, 占文 韩, XueFei Chen, 雪飞 陈
Figure caption: Distributions of ﹩V\sin i﹩ and peculiar space velocity (V Sp) of the newly identified runaway candidates.
Paper: A Catalog of Early-type Runaway Stars from LAMOST DR8
Authors: Yanjun Guo, Luqian Wang, 璐茜 王, Chao Liu, 超 刘, You Wu, 优 吴, ZhanWen Han, 占文 韩, XueFei Chen, 雪飞 陈
Figure caption:  U−V velocity diagram of the 229 runaway candidate stars identified from LAMOST MRS DR8.
Paper: A Catalog of Early-type Runaway Stars from LAMOST DR8
Authors: Yanjun Guo, Luqian Wang, 璐茜 王, Chao Liu, 超 刘, You Wu, 优 吴, ZhanWen Han, 占文 韩, XueFei Chen, 雪飞 陈
Figure caption: The number distribution of the projected rotational velocities (﹩V\sin i﹩) of the identified 229 runaway candidates.
Paper: A Catalog of Early-type Runaway Stars from LAMOST DR8
Authors: Yanjun Guo, Luqian Wang, 璐茜 王, Chao Liu, 超 刘, You Wu, 优 吴, ZhanWen Han, 占文 韩, XueFei Chen, 雪飞 陈
Figure caption: The density distribution of our final sample in a Hertzsprung–Russell diagram. The purple and blue lines represent isochrones generated using the Padova and Trieste Stellar Evolutionary Code for ages of 1, 10, and 100 Myr, with each set corresponding to different metallicity values: [M/H] = −1.0 dex and [M/H] = 0.0 dex, respectively.
Paper: A Catalog of Early-type Runaway Stars from LAMOST DR8
Authors: Yanjun Guo, Luqian Wang, 璐茜 王, Chao Liu, 超 刘, You Wu, 优 吴, ZhanWen Han, 占文 韩, XueFei Chen, 雪飞 陈
Figure caption: Example spectra of Hα emission profiles identified in the preliminary sample from the CNN ResNet. These spectra were eliminated from the sample due to the erroneous RV measurements reported in Zhang et al. (2021). Left panel: Gaia source ID 3437654474685782912. Right panel: Gaia source ID 3326400154406915712.
Paper: A Catalog of Early-type Runaway Stars from LAMOST DR8
Authors: Yanjun Guo, Luqian Wang, 璐茜 王, Chao Liu, 超 刘, You Wu, 优 吴, ZhanWen Han, 占文 韩, XueFei Chen, 雪飞 陈
Figure caption: Example spectra displaying Hα absorption profile in our sample Left panel: Gaia source ID 3104143533939403264. Right panel: Gaia source ID 2189024507268284416.
Paper: A Catalog of Early-type Runaway Stars from LAMOST DR8
Authors: Yanjun Guo, Luqian Wang, 璐茜 王, Chao Liu, 超 刘, You Wu, 优 吴, ZhanWen Han, 占文 韩, XueFei Chen, 雪飞 陈
Figure caption: The spatial distribution of the initial sample of 9382 early-type stars released from Guo et al. (2022, gray circles) and the final filtered sample of 4432 OB stars (red cross). The 229 newly identified runaway candidate stars discussed in Section 3 are shown in blue squares. The histogram on top of the spatial plot shows the number distribution of stars within each R.A. interval with a bin size of 30°. In this representation, the black steps represent early-type stars released from Guo et al. (2022), and the red steps represent the final filtered sample. A similar number distribution of stars for decl. is shown on the right side of the spatial plot with a bin size of 15°. A zoomed-in square subplot in the lower-right corner shows the spatial distribution of sample stars distributed with a window size of 30° × 15° (R.A. spans from 60° to 90° and 30° to 45° for decl.). Within the selected area, there are 1237 OB stars, 630 filtered stars, and 17 identified runaway candidates. Number counts are labeled adjacent to the subplot.
Paper: A Catalog of Early-type Runaway Stars from LAMOST DR8
Authors: Yanjun Guo, Luqian Wang, 璐茜 王, Chao Liu, 超 刘, You Wu, 优 吴, ZhanWen Han, 占文 韩, XueFei Chen, 雪飞 陈
Figure caption: From the bottom to the top panel: the number distributions of peculiar tangential velocity, absolute values of peculiar radial velocity, and peculiar space velocities are shown for 4432 early-type stars identified from LAMOST MRS DR8. A Maxwellian velocity distribution fit was applied to the peculiar space velocity and overplotted in the top panel.
Paper: A Catalog of Early-type Runaway Stars from LAMOST DR8
Authors: Yanjun Guo, Luqian Wang, 璐茜 王, Chao Liu, 超 刘, You Wu, 优 吴, ZhanWen Han, 占文 韩, XueFei Chen, 雪飞 陈
Figure caption: The density contour plot shows the distributions of peculiar radial and tangential velocities for the 4432 OB stars. The velocity entries for the newly identified 229 runaway candidates are overplotted in the figure in black dots and their associated errors are shown as red crosses. Error bars (in red) displaying the uncertainties of peculiar velocities are included for the 229 identified runaway candidates. The dashed arcs represent the constant values of ﹩{({V}_{{Rp}})}^{2}+({V}_{{Tp}}^{2})/2﹩ ranging from 60 to 260 km s−1, with an increment of 40 km s−1.
Paper: A Catalog of Early-type Runaway Stars from LAMOST DR8
Authors: Yanjun Guo, Luqian Wang, 璐茜 王, Chao Liu, 超 刘, You Wu, 优 吴, ZhanWen Han, 占文 韩, XueFei Chen, 雪飞 陈
Figure caption: Uncertainty distributions of the peculiar radial (blue) and tangential (orange) velocity measurements are shown as a function of distance. The median values are plotted as solid lines, and the 16th to 84th percentiles of the error distributions are shown as the shaded regions. Since 98% of our sample stars have distances within 4 kpc, the distributions are plotted for that range only.
Paper: A Catalog of Early-type Runaway Stars from LAMOST DR8
Authors: Yanjun Guo, Luqian Wang, 璐茜 王, Chao Liu, 超 刘, You Wu, 优 吴, ZhanWen Han, 占文 韩, XueFei Chen, 雪飞 陈
Figure caption: The RV distribution of the two catalogs. The 162 stars with Flag = S in both Tables 2 and 3 are indicated by the red step. The 67 stars only present in Table 2 with Flag = N are marked by the gray shading, while the 318 stars exclusively shown in Table 3 with Flag = N are represented by the blue step.
Paper: A Catalog of Early-type Runaway Stars from LAMOST DR8
Authors: Yanjun Guo, Luqian Wang, 璐茜 王, Chao Liu, 超 刘, You Wu, 优 吴, ZhanWen Han, 占文 韩, XueFei Chen, 雪飞 陈
Figure caption: The distribution of observed number for the final filtered sample of 4432 OB stars (see Section 2).
Paper: A Catalog of Early-type Runaway Stars from LAMOST DR8
Authors: Yanjun Guo, Luqian Wang, 璐茜 王, Chao Liu, 超 刘, You Wu, 优 吴, ZhanWen Han, 占文 韩, XueFei Chen, 雪飞 陈
Figure caption: The distribution of Galactic heights (associated errors shown as red crosses) of the 229 newly identified runaway candidate stars as a function of Galactic longitude. Most of the errors are too small to be shown in the figure.
Paper: A Catalog of Early-type Runaway Stars from LAMOST DR8
Authors: Yanjun Guo, Luqian Wang, 璐茜 王, Chao Liu, 超 刘, You Wu, 优 吴, ZhanWen Han, 占文 韩, XueFei Chen, 雪飞 陈
Figure caption: The CDFs of ﹩V\sin i﹩ values for both runaway candidates (cross signs) and nonrunaway population (solid curve) for the OB sample stars from LAMOST MRS. The p-value is obtained from a K-S test.
Paper: A Catalog of Early-type Runaway Stars from LAMOST DR8
Authors: Yanjun Guo, Luqian Wang, 璐茜 王, Chao Liu, 超 刘, You Wu, 优 吴, ZhanWen Han, 占文 韩, XueFei Chen, 雪飞 陈
Figure caption: The number distribution of the measured effective temperatures (T eff) of the identified 229 runaway candidate stars.
Paper: Virial Black Hole Masses for Active Galactic Nuclei behind the Magellanic Clouds
Authors: Swayamtrupta Panda, Szymon Kozłowski, Mariusz Gromadzki, Marcin Wrona, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Krzysztof Ulaczyk, Jan Skowron, Radosław Poleski, Przemek Mróz, Dorota M. Skowron, Krzysztof Rybicki, Mateusz Mróz
Figure caption: Left panel: schematic diagram of the optical plane of Eigenvector 1. Abridged version from Panda et al. (2020). The horizontal line denotes the threshold in FWHM(Hβ) at 4000 km s−1 that separates the Population A and Population B sources. The ”classical” NLS1s are located below FWHM(Hβ) ≤ 2000 km s−1 (dotted–dashed line). The vertical blue line marks the limit for R Fe II = 1 separating the weak and strong Fe II emitters (or xA sources). Right panel: the optical plane for the MQS sources. Similar to the left panel, the horizontal dashed and dotted lines represent the 4000 and 2000 km s−1 thresholds, respectively, while the dashed vertical line marks the R Fe II = 1 limit. The sources are colored based on their Eddington ratios (in the log scale). Here we demonstrate the sources where both the FWHM(Hβ) and R Fe II are of high quality, i.e., corresponding errors are within 20% of the estimated values. The sources from the SDSS DR14 QSO sample are shown using contours where a similar quality filtering is adopted. Spectra for the three sources marked with the bull's-eyes are shown in Figure 8.
Paper: Virial Black Hole Masses for Active Galactic Nuclei behind the Magellanic Clouds
Authors: Swayamtrupta Panda, Szymon Kozłowski, Mariusz Gromadzki, Marcin Wrona, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Krzysztof Ulaczyk, Jan Skowron, Radosław Poleski, Przemek Mróz, Dorota M. Skowron, Krzysztof Rybicki, Mateusz Mróz
Figure caption: Exemplary fit using PYQSOFIT (Guo et al. 2018) for a quasar spectrum (MQS J045538.57–690455.1) without significant host galaxy contribution. In each panel, we show the MQS data (black), power-law continuum (yellow), Fe II pseudocontinuum (in addition to the power-law continuum; light green), broad emission lines (red), narrow emission lines (dark green), and the total best-fit qso model (blue), which is the sum of continuum and emission lines. The host galaxy contribution is shown in magenta, while the host-subtracted data are shown with a continuous gray line, and the sum of the host and qso model is shown in pink. Top panel: the rest-frame central wavelengths for prominent emission lines are shown using the dashed vertical lines. The sky coordinates (in degrees) and the redshift for the sources are quoted in the title of the figure. Bottom panels: a zoomed-in version of individual line complexes. The residuals are shown in dotted gray in each panel.
Paper: Virial Black Hole Masses for Active Galactic Nuclei behind the Magellanic Clouds
Authors: Swayamtrupta Panda, Szymon Kozłowski, Mariusz Gromadzki, Marcin Wrona, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Krzysztof Ulaczyk, Jan Skowron, Radosław Poleski, Przemek Mróz, Dorota M. Skowron, Krzysztof Rybicki, Mateusz Mróz
Figure caption: BH masses vs. Eddington ratios for the sources in our sample. The sources are colored based on the monochromatic luminosity–emission-line pairs. The sources from the SDSS DR14 QSO sample are shown using contours where the Hβ- (in pink), Mg II- (in light green), and C IV-based (in light blue) BH masses are considered. The SDSS sources are filtered based on the adopted fiducial L bol and M BH with the QUAL flags = 0. We do not show the uncertainties associated with the M BH and λ Edd for the MQS AGNs for clarity.
Paper: Virial Black Hole Masses for Active Galactic Nuclei behind the Magellanic Clouds
Authors: Swayamtrupta Panda, Szymon Kozłowski, Mariusz Gromadzki, Marcin Wrona, Patryk Iwanek, Andrzej Udalski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Krzysztof Ulaczyk, Jan Skowron, Radosław Poleski, Przemek Mróz, Dorota M. Skowron, Krzysztof Rybicki, Mateusz Mróz
Figure caption: Bolometric luminosity as a function of redshift for the sources in our sample. The sources are colored by the AGN monochromatic luminosity used to estimate the bolometric luminosity. The sources from the SDSS DR14 QSO sample are shown using contours where the fiducial L bol are reported with the QUAL flag = 0. We show nine levels for the contour map, which correspond to the isodensity of the SDSS sources, with the outermost contour encompassing 90% of the sources and decreasing inward by 10%.