adsabs/AstroCLIMB huggingface dataset:
Paper: Zwicky Transient Facility and Globular Clusters: The Period–Luminosity and Period–Wesenheit Relations for SX Phoenicis Variables in the gri Band
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Matthew J. Graham, Brian F. Healy, Russ R. Laher, Reed Riddle, Avery Wold
Figure caption: ZTF light curves for NGC  6838 P 13 folded with P LSM (left panel) and twice of P LSM (right panel).
Paper: Zwicky Transient Facility and Globular Clusters: The Period–Luminosity and Period–Wesenheit Relations for SX Phoenicis Variables in the gri Band
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Matthew J. Graham, Brian F. Healy, Russ R. Laher, Reed Riddle, Avery Wold
Figure caption: Same as Figure 2, but for SXP stars selected in the final sample.
Paper: Zwicky Transient Facility and Globular Clusters: The Period–Luminosity and Period–Wesenheit Relations for SX Phoenicis Variables in the gri Band
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Matthew J. Graham, Brian F. Healy, Russ R. Laher, Reed Riddle, Avery Wold
Figure caption: Left panel: the transformed V-band mean magnitudes for the 48 SXP stars, shown as open circles, listed in Table 1 as a function of pulsation period P. The solid, dashed, and dotted lines are the F, 1O, and 2O PL relation published in Arellano Ferro et al. (2011; see text for more details). SXP stars labeled as open red circles are assumed to pulsate in the second-overtone mode. After fundamentalizing their periods, their new locations on the PL plane are marked as filled red circles. Right panel: same as the left panel, but for the 15 SXP stars identified as pulsating in the first-overtone mode, as described in the text. Open and filled blue squares are their locations on the PL plane before and after fundamentalizing their periods, respectively.
Paper: Zwicky Transient Facility and Globular Clusters: The Period–Luminosity and Period–Wesenheit Relations for SX Phoenicis Variables in the gri Band
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Matthew J. Graham, Brian F. Healy, Russ R. Laher, Reed Riddle, Avery Wold
Figure caption: Fitted V-band PL relation, shown as the solid line, to the F (circles), 1O (squares), and 2O (triangles) SXP stars in the sample. The dotted-dashed lines represent the ±2.5σ boundaries, where σ is the dispersion of the fitted PL relation. The data points are color coded with the metallicities of the host globular clusters ([Fe/H]), adopted from the GlObular clusTer Homogeneous Abundances Measurements survey (Dias et al. 2015, 2016a, 2016b; Vásquez et al. 2018), where the metallicity ranged from −1.00 dex (NGC  6171) to −2.33 dex (NGC  7099).
Paper: Zwicky Transient Facility and Globular Clusters: The Period–Luminosity and Period–Wesenheit Relations for SX Phoenicis Variables in the gri Band
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Matthew J. Graham, Brian F. Healy, Russ R. Laher, Reed Riddle, Avery Wold
Figure caption: Comparison of the observed V-band PL relations for the 48 SXP stars listed in Table 1 to the published PL relations for fundamental-mode pulsators (solid lines) in the literature. The dashed and dotted lines are the corresponding PL relations for the first-overtone and the second-overtone pulsators, respectively (see text for more details).
Paper: Zwicky Transient Facility and Globular Clusters: The Period–Luminosity and Period–Wesenheit Relations for SX Phoenicis Variables in the gri Band
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Matthew J. Graham, Brian F. Healy, Russ R. Laher, Reed Riddle, Avery Wold
Figure caption: Extinction-corrected PC relations and the extinction-free PQ relations in the gri band. Note that the periods for 1O and 2O SXP have been fundamentalized. The open circle marks the outlier NGC 6341 V33 in the (g − i) PC relation.
Paper: Zwicky Transient Facility and Globular Clusters: The Period–Luminosity and Period–Wesenheit Relations for SX Phoenicis Variables in the gri Band
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Matthew J. Graham, Brian F. Healy, Russ R. Laher, Reed Riddle, Avery Wold
Figure caption: Extinction-corrected PL relations (left panel) and the extinction-free PW relations (right panel) in the gri band for our sample of SXP stars in the globular clusters. The solid lines are the fitted relations as given in Equations (6) to (11).
Paper: Contemporaneous Observations of Hα Luminosities and Photometric Amplitudes for M Dwarfs
Authors: Aylin García Soto, Elisabeth R. Newton, Stephanie T. Douglas, Abigail Burrows, Aurora Y. Kesseli
Figure caption: A lightkurve time series comparing SAP flux and PDCSAP flux for TIC 343268431 (TESS magnitude 13.1). Long-term systematic trends are seen from ∼1710 to ∼1722 Barycentric TESS Julian Date (BTJD–2,457,000), the SAP flux decreases almost linearly and then increases after ∼1722. We also see that the pattern repeats in the second observation cycle. Meanwhile, the PDCSAP flux remains constant aside from the rotation modulations.
Paper: Contemporaneous Observations of Hα Luminosities and Photometric Amplitudes for M Dwarfs
Authors: Aylin García Soto, Elisabeth R. Newton, Stephanie T. Douglas, Abigail Burrows, Aurora Y. Kesseli
Figure caption: Semiamplitude, R var, plotted against the Hα strength, L Hα /L bol. The x-axis error bars for the OSMOS data in this case represent the range in L Hα /L bol. There is a possible correlation between R var and L Hα /L bol, with more active stars showing higher photometric variability.
Paper: Contemporaneous Observations of Hα Luminosities and Photometric Amplitudes for M Dwarfs
Authors: Aylin García Soto, Elisabeth R. Newton, Stephanie T. Douglas, Abigail Burrows, Aurora Y. Kesseli
Figure caption: The original PDCSAP light curve on the top, Hα EWs in the middle, and number of σ std from the mean Hα EWs in the bottom against time. Left: two nights for TIC 220044948, Middle: two nights for TIC 415508270, Right: two nights for TIC 178947176. The light green circles are the raw light curve and the black circles is the light curve after stella removed the flares. For the middle and bottom panel, the light green circles are each target-specific Hα EW observation.
Paper: Contemporaneous Observations of Hα Luminosities and Photometric Amplitudes for M Dwarfs
Authors: Aylin García Soto, Elisabeth R. Newton, Stephanie T. Douglas, Abigail Burrows, Aurora Y. Kesseli
Figure caption: Same setup as Figure 5, except the color bar is inclination. Top: stars with mass <0.25 M ⊙. Bottom: stars with mass >0.25 M ⊙, separated as detailed in Newton et al. (2016b). The “error bars” in this case represent the full range in Hα luminosity measurements. Inclination does not visibly correlate with with L Hα /L bol but there might some indication in the low-mass bin that smaller R var have smaller inclinations.
Paper: Contemporaneous Observations of Hα Luminosities and Photometric Amplitudes for M Dwarfs
Authors: Aylin García Soto, Elisabeth R. Newton, Stephanie T. Douglas, Abigail Burrows, Aurora Y. Kesseli
Figure caption: A comparison between the periods we find from starspot and rotation periods in the literature. The black star symbol denotes TIC 17970570, where our period is not quite double the period from Newton et al. (2016b). Reanalysis of data from MEarth shows that P rot = 0.5593 ± 0.0004 day is the true period, consistent with the result from TESS. We are therefore confident in our P rot values for all 30 of our targets.
Paper: Contemporaneous Observations of Hα Luminosities and Photometric Amplitudes for M Dwarfs
Authors: Aylin García Soto, Elisabeth R. Newton, Stephanie T. Douglas, Abigail Burrows, Aurora Y. Kesseli
Figure caption: Two graphs of semiamplitude–R var plotted over time. Top: TIC 229614158 and Bottom: TIC 233068870. The vertical lines represent the length of a TESS sector, approximately every 27.4 days.
Paper: Contemporaneous Observations of Hα Luminosities and Photometric Amplitudes for M Dwarfs
Authors: Aylin García Soto, Elisabeth R. Newton, Stephanie T. Douglas, Abigail Burrows, Aurora Y. Kesseli
Figure caption: This plot is the MEarth fitted-amplitude plotted against the ﹩\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} }﹩ (RUWE < 1.6) using data from Boudreaux et al. (2022). In order to compare to our sample, we differentiate stars in the unsaturated regime (triangles) and stars in the saturated regime (circles). The stars in the saturated regime are defined as stars with Rossby <0.17 ± 0.04.
Paper: Contemporaneous Observations of Hα Luminosities and Photometric Amplitudes for M Dwarfs
Authors: Aylin García Soto, Elisabeth R. Newton, Stephanie T. Douglas, Abigail Burrows, Aurora Y. Kesseli
Figure caption: The comparison of the average relative Hα EWs for each M dwarf against their range of relative Hα EWs. The dotted lines represent 10% variation from the mean value. TIC 415508270 has the largest range: 30.2% to 60.8% variation from the mean value.
Paper: Coronal X-Ray Emission from Nearby, Low-mass, Exoplanet Host Stars Observed by the MUSCLES and Mega-MUSCLES HST Treasury Survey Projects
Authors: Alexander Brown, P. Christian Schneider, Kevin France, Cynthia S. Froning, Allison A. Youngblood, David J. Wilson, R. O. Parke Loyd, J. Sebastian Pineda, Girish M. Duvvuri, Adam F. Kowalski, Zachory K. Berta-Thompson
Figure caption: X-ray (0.3–10.0 keV) luminosity and X-ray-to-bolometric luminosity ratio as functions of stellar mass (left) and effective temperature (right). Observations of the same star in quiescent and flaring states are connected by vertical lines. Color coding: blue M ≥ 0.6 M ⊙; green 0.35 ≤ M ≤ 0.6 M ⊙; red M ≤ 0.35 M ⊙. Error bars are plotted in black with some being smaller than the plotting symbols.
Paper: Coronal X-Ray Emission from Nearby, Low-mass, Exoplanet Host Stars Observed by the MUSCLES and Mega-MUSCLES HST Treasury Survey Projects
Authors: Alexander Brown, P. Christian Schneider, Kevin France, Cynthia S. Froning, Allison A. Youngblood, David J. Wilson, R. O. Parke Loyd, J. Sebastian Pineda, Girish M. Duvvuri, Adam F. Kowalski, Zachory K. Berta-Thompson
Figure caption: X-ray luminosity and X-ray-to-bolometric luminosity ratio as functions of stellar rotation period (left) and age (right). For comparison, the equivalent numbers for the quiet Sun (QS) and active Sun (AS) are shown as orange symbols. Most stars in the sample are older than the Sun (4.5 Gyr). Three stars are younger than 1 Gyr. For older stars the age uncertainties are large. Color coding as in Figure 1.
Paper: Coronal X-Ray Emission from Nearby, Low-mass, Exoplanet Host Stars Observed by the MUSCLES and Mega-MUSCLES HST Treasury Survey Projects
Authors: Alexander Brown, P. Christian Schneider, Kevin France, Cynthia S. Froning, Allison A. Youngblood, David J. Wilson, R. O. Parke Loyd, J. Sebastian Pineda, Girish M. Duvvuri, Adam F. Kowalski, Zachory K. Berta-Thompson
Figure caption: Chandra ACIS-S3 light curve of GJ 15 A and B using 2 ks sampling bins. 1σ error bars are plotted.
Paper: Coronal X-Ray Emission from Nearby, Low-mass, Exoplanet Host Stars Observed by the MUSCLES and Mega-MUSCLES HST Treasury Survey Projects
Authors: Alexander Brown, P. Christian Schneider, Kevin France, Cynthia S. Froning, Allison A. Youngblood, David J. Wilson, R. O. Parke Loyd, J. Sebastian Pineda, Girish M. Duvvuri, Adam F. Kowalski, Zachory K. Berta-Thompson
Figure caption: Chandra ACIS-S3 light curves of GJ 876A (M4 V; P rot = 81 days) and GJ 581 (M3 V; P rot = 132 days). Both stars have masses between 0.30 and 0.35 M ⊙ and are thus in the fully convective mass range. Despite having long rotation periods, both stars show dramatic coronal flaring. 1σ error bars are plotted. The vertical dotted line in the GJ 581 figure marks the time split between the quiescent and flaring time intervals—the quiescent exposure totals 40.6 ks, while the flare is observed for 7.0 ks.
Paper: Coronal X-Ray Emission from Nearby, Low-mass, Exoplanet Host Stars Observed by the MUSCLES and Mega-MUSCLES HST Treasury Survey Projects
Authors: Alexander Brown, P. Christian Schneider, Kevin France, Cynthia S. Froning, Allison A. Youngblood, David J. Wilson, R. O. Parke Loyd, J. Sebastian Pineda, Girish M. Duvvuri, Adam F. Kowalski, Zachory K. Berta-Thompson
Figure caption: Comparison of X-ray-to-bolometric luminosity ratio as a function of rotational period (upper panel) and Rossby number (lower panel). The empirical relationships between the X-ray-to-bolometric luminosity ratio and Rossby number (rotation period/convective turnover timescale) derived by Wright et al. (2011, 2018) from large samples of M dwarfs are plotted as solid and dashed lines, respectively. The saturated activity level for M dwarfs from Pizzolato et al. (2003) is shown as a dotted–dashed line. The sample of nearby M dwarfs from Wright et al. (2011, 2018) are shown as black asterisks. Color coding as in Figure 1.
Paper: Coronal X-Ray Emission from Nearby, Low-mass, Exoplanet Host Stars Observed by the MUSCLES and Mega-MUSCLES HST Treasury Survey Projects
Authors: Alexander Brown, P. Christian Schneider, Kevin France, Cynthia S. Froning, Allison A. Youngblood, David J. Wilson, R. O. Parke Loyd, J. Sebastian Pineda, Girish M. Duvvuri, Adam F. Kowalski, Zachory K. Berta-Thompson
Figure caption: Chandra ACIS-S3 light curves of LHS 2686 (M4.5 V; P rot = 29 days) and GJ 699 (M4 V; P rot = 145 days). These stars are likely to be fully convective having masses near 0.16 M ⊙. While GJ 699 is a slow rotator and LHS 2686 is a much faster rotator, both stars show significant flaring. Both plots are for 1 ks sampling bins. 1σ error bars are plotted.
Paper: Coronal X-Ray Emission from Nearby, Low-mass, Exoplanet Host Stars Observed by the MUSCLES and Mega-MUSCLES HST Treasury Survey Projects
Authors: Alexander Brown, P. Christian Schneider, Kevin France, Cynthia S. Froning, Allison A. Youngblood, David J. Wilson, R. O. Parke Loyd, J. Sebastian Pineda, Girish M. Duvvuri, Adam F. Kowalski, Zachory K. Berta-Thompson
Figure caption: Volume emission measure as a function of coronal temperature. The highest volume emission measure marks the dominant coronal thermal component for each star. The coronal temperatures for GJ 1132 and TRAPPIST-1 are assumed values and not measured values from the spectral fits. Dashed lines connect the characteristic temperatures from 2T fits. For clarity, the characteristic temperatures from 3T fits are connected by solid lines. Square boxes mark data dominated by flare plasma. Color coding as in Figure 1.
Paper: Coronal X-Ray Emission from Nearby, Low-mass, Exoplanet Host Stars Observed by the MUSCLES and Mega-MUSCLES HST Treasury Survey Projects
Authors: Alexander Brown, P. Christian Schneider, Kevin France, Cynthia S. Froning, Allison A. Youngblood, David J. Wilson, R. O. Parke Loyd, J. Sebastian Pineda, Girish M. Duvvuri, Adam F. Kowalski, Zachory K. Berta-Thompson
Figure caption: XMM-Newton EPIC pn light curves of the young star GJ 674 (M3 V; P rot = 33 days). This star has a mass of 0.35 M ⊙ and thus lies right at the fully convective boundary. GJ 674 showed significant X-ray flaring in 2008 but little variability in 2018. However, immediately after the 2018 XMM-Newton observation ended an extremely large, high-temperature FUV flare was seen by HST Cosmic Origins Spectrograph (COS, Froning et al. 2019). Dashed vertical lines delineate the large 2008 flare. 1σ error bars are plotted.
Paper: Coronal X-Ray Emission from Nearby, Low-mass, Exoplanet Host Stars Observed by the MUSCLES and Mega-MUSCLES HST Treasury Survey Projects
Authors: Alexander Brown, P. Christian Schneider, Kevin France, Cynthia S. Froning, Allison A. Youngblood, David J. Wilson, R. O. Parke Loyd, J. Sebastian Pineda, Girish M. Duvvuri, Adam F. Kowalski, Zachory K. Berta-Thompson
Figure caption: Examples of XSPEC spectral fitting to Chandra CCD-resolution spectra of GJ 876. These figures demonstrate the fitting framework within XSPEC. The spectral data with associated error bars are overlaid on the final model shown as a histogram. Right panel: a two-temperature (2T) fit to the high-activity (ObsID 17315) spectrum grouped with 35 events per channel. Left panel: a 2T fit to the low-activity (ObsID 17316) spectrum, recorded 12 hr earlier, grouped with 15 events per channel.
Paper: Coronal X-Ray Emission from Nearby, Low-mass, Exoplanet Host Stars Observed by the MUSCLES and Mega-MUSCLES HST Treasury Survey Projects
Authors: Alexander Brown, P. Christian Schneider, Kevin France, Cynthia S. Froning, Allison A. Youngblood, David J. Wilson, R. O. Parke Loyd, J. Sebastian Pineda, Girish M. Duvvuri, Adam F. Kowalski, Zachory K. Berta-Thompson
Figure caption: Chandra ACIS-S3 light curves of the K3+K5 binary GJ 667AB (upper panel) using 500 s binning and GJ 667C (lower panel) using 2 ks sampling bins. 1σ error bars are plotted. Note that the GJ 667C y-axis covers only one quarter the range of count rate of the GJ 667AB plot. GJ 667C is only a weak source and no statistically significant variability is detected. A red upward arrow marks the time when an FUV flare was detected (Loyd et al. 2018).
Paper: Coronal X-Ray Emission from Nearby, Low-mass, Exoplanet Host Stars Observed by the MUSCLES and Mega-MUSCLES HST Treasury Survey Projects
Authors: Alexander Brown, P. Christian Schneider, Kevin France, Cynthia S. Froning, Allison A. Youngblood, David J. Wilson, R. O. Parke Loyd, J. Sebastian Pineda, Girish M. Duvvuri, Adam F. Kowalski, Zachory K. Berta-Thompson
Figure caption: XMM-Newton EPIC pn light curves of the young star GJ 729 (M4 V; P rot = 2.85 days) from observations in 2018 and 2010. GJ 729 shows persistent X-ray flaring. Dashed vertical lines delineate the 2010 flare discussed in the text. 1σ error bars are plotted.
Paper: Coronal X-Ray Emission from Nearby, Low-mass, Exoplanet Host Stars Observed by the MUSCLES and Mega-MUSCLES HST Treasury Survey Projects
Authors: Alexander Brown, P. Christian Schneider, Kevin France, Cynthia S. Froning, Allison A. Youngblood, David J. Wilson, R. O. Parke Loyd, J. Sebastian Pineda, Girish M. Duvvuri, Adam F. Kowalski, Zachory K. Berta-Thompson
Figure caption: Chandra ACIS-S3 light curves using 1.0 and 1.5 ks sampling bins from both observations of GJ 176 (M2 V). The mean count rate levels are shown as dotted lines and labeled in red. Dashed lines mark the zero count rate level. Red downward arrows marks the times when the largest FUV flares seen by Loyd et al. (2018) were detected. 1σ error bars are plotted.
Paper: Coronal X-Ray Emission from Nearby, Low-mass, Exoplanet Host Stars Observed by the MUSCLES and Mega-MUSCLES HST Treasury Survey Projects
Authors: Alexander Brown, P. Christian Schneider, Kevin France, Cynthia S. Froning, Allison A. Youngblood, David J. Wilson, R. O. Parke Loyd, J. Sebastian Pineda, Girish M. Duvvuri, Adam F. Kowalski, Zachory K. Berta-Thompson
Figure caption: Chandra ACIS-S3 light curves using 3 ks sampling bins from six observations of GJ 436 (M3 V). No statistically significant variability is detected over the complete data set, which includes a total of 105 ks of X-ray monitoring. The mean count rates for the individual observations are listed in the relevant panel and marked by a dotted line. The average of the six measured count rates is 0.0026 ± 0.0004 counts s−1. 1σ error bars are plotted.
Paper: Coronal X-Ray Emission from Nearby, Low-mass, Exoplanet Host Stars Observed by the MUSCLES and Mega-MUSCLES HST Treasury Survey Projects
Authors: Alexander Brown, P. Christian Schneider, Kevin France, Cynthia S. Froning, Allison A. Youngblood, David J. Wilson, R. O. Parke Loyd, J. Sebastian Pineda, Girish M. Duvvuri, Adam F. Kowalski, Zachory K. Berta-Thompson
Figure caption: Chandra ACIS-S3 light curve of GJ 163 (M3.5 V, 0.405 M ⊙) using 3 ks sampling bins. 1σ error bars are plotted. No statistically significant variability is detected with a glvary VARINDEX = 2.
Paper: Coronal X-Ray Emission from Nearby, Low-mass, Exoplanet Host Stars Observed by the MUSCLES and Mega-MUSCLES HST Treasury Survey Projects
Authors: Alexander Brown, P. Christian Schneider, Kevin France, Cynthia S. Froning, Allison A. Youngblood, David J. Wilson, R. O. Parke Loyd, J. Sebastian Pineda, Girish M. Duvvuri, Adam F. Kowalski, Zachory K. Berta-Thompson
Figure caption: Chandra ACIS-S3 light curve of GJ 849 (M3.5 V, 0.465 M ⊙) using 2 ks sampling bins. 1σ error bars are plotted. No statistically significant variability is detected with a glvary VARINDEX = 0.
Paper: Disks around Young Planetary-mass Objects: Ultradeep Spitzer Imaging of NGC 1333
Authors: Aleks Scholz, Koraljka Muzic, Ray Jayawardhana, Victor Almendros-Abad, Isaac Wilson
Figure caption: Comparison of a single epoch Spitzer/IRAC image of NGC 1333 in channel 2 (4.5 μm, AOR 29324032) and the stacked version of the same area (70 frames). The marked object in the center is the L3 brown dwarf SONYC-NGC1333-36, one of the lowest-mass spectroscopically confirmed objects in this cluster. The image size is ﹩2^{\prime} \times 2^{\prime} ﹩, north is up and east is left.
Paper: Disks around Young Planetary-mass Objects: Ultradeep Spitzer Imaging of NGC 1333
Authors: Aleks Scholz, Koraljka Muzic, Ray Jayawardhana, Victor Almendros-Abad, Isaac Wilson
Figure caption: Infrared colors of brown dwarfs in NGC 1333 vs. spectral types, after dereddening the colors to A  J  = 0. The spectral type range is M6–L3. In the right panel, three objects of spectral type M9 have very similar colors and have been plotted slightly offset in spectral type for clarity. The estimated photospheric colors are shown with a solid black line, with the typical scatter shown as the colored area (see the text for details). The dashed–dotted line is the chosen demarcation for our sample; all objects plotted on the right side of it can be described as PMOs.
Paper: Disks around Young Planetary-mass Objects: Ultradeep Spitzer Imaging of NGC 1333
Authors: Aleks Scholz, Koraljka Muzic, Ray Jayawardhana, Victor Almendros-Abad, Isaac Wilson
Figure caption: Disk fraction for samples of stars and brown dwarfs with known spectral type, from Luhman et al. (2016) (blue symbols), Scholz et al. (2012), and this paper (orange symbols). The spectral types are numerically coded, M0 is 0.0, L0 is 10.0.
Paper: Disks around Young Planetary-mass Objects: Ultradeep Spitzer Imaging of NGC 1333
Authors: Aleks Scholz, Koraljka Muzic, Ray Jayawardhana, Victor Almendros-Abad, Isaac Wilson
Figure caption: Left: spectral type vs. K-band magnitude for brown dwarfs in NGC 1333. The dots mark all objects in this spectral type range from the list by Luhman et al. (2016). The crosses mark the ones covered by our deep coadded Spitzer images. The spectral types are numerically coded, where M6 is 6.0, L0 is 10.0. Right: spatial distribution of brown dwarfs (small dots), PMOs (crosses), and PMOs with disks (empty circles) in NGC 1333. We also show the position and extent of the cluster as determined by Gutermuth et al. (2008), as well as approximate coverage of the deep IRAC images produced here.
Paper: The Orbital and Physical Properties of Five Southern Be+sdO Binary Systems
Authors: Luqian Wang, 茜 王璐, Douglas R. Gies, Geraldine J. Peters, Zhanwen Han
Figure caption: Example of the Hα profile observed on the night of HJD 2,458,482 for HD 113120. The horizontal line indicates 25% of the peak height of the profile, and two oppositely signed Gaussian functions were located at the intersection points to sample the wings of the profile and determine the bisector position of the Doppler shift (shown as the tick mark).