adsabs/AstroCLIMB huggingface dataset:
Paper: Comprehensive Analysis of a Symbiotic Candidate V503 Her
Authors: Jaroslav Merc, Rudolf Gális, Marek Wolf, Pavol A. Dubovský, Jan Kára, Forrest Sims, James R. Foster, Tomáš Medulka, Christophe Boussin, John P. Coffin, Christian Buil, David Boyd, Jacques Montier
Figure caption: Results of WWZ analysis of ASAS-SN data of V503 Her performed in software Peranso. Colors denote the wavelet power, with dark blue having the lowest power and dark red having the highest. Colors of photometric data points in the corresponding light curve shown in the top panel are the same as in Figure 1.
Paper: Comprehensive Analysis of a Symbiotic Candidate V503 Her
Authors: Jaroslav Merc, Rudolf Gális, Marek Wolf, Pavol A. Dubovský, Jan Kára, Forrest Sims, James R. Foster, Tomáš Medulka, Christophe Boussin, John P. Coffin, Christian Buil, David Boyd, Jacques Montier
Figure caption: Optical spectra of V503 Her obtained by the ARAS Group.
Paper: Comprehensive Analysis of a Symbiotic Candidate V503 Her
Authors: Jaroslav Merc, Rudolf Gális, Marek Wolf, Pavol A. Dubovský, Jan Kára, Forrest Sims, James R. Foster, Tomáš Medulka, Christophe Boussin, John P. Coffin, Christian Buil, David Boyd, Jacques Montier
Figure caption: Model light curve of V503 Her (black) based on the analysis of ASAS-SN V+g data (Table 4). Colors of observed photometric data points in the light curve are the same as in Figure 1.
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: (Left-hand panel): active stars (red dots) and inactive stars (blue dots) on the enhanced HRD, identified using Hα equivalent widths (EW) in CHIRON spectra. Eight equal size zones are outlined inside the ROI. The gap edge (GE) is shown with a short heavy black line, and the best-fit main sequence line is shown with a long thin black line. (Center) panel: The absolute values of EWs for active stars are plotted as a function of the size of red circles. The single active star represented by the very small red circle below the GE is GAI0406-5011 with a very low EW = −0.18 Å. (Right-hand panel): The EWs of inactive stars are indicated by the size of blue circles; all have similar EWs.
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: The sample of 2249 M dwarf targets (black dots) meeting our selection criteria are shown in a small region of the HRD (Jao & Feiden 2020), where the thin black line traces the best-fit main sequence. The white shading is the gap first reported in Jao et al. (2018), which is enhanced here to show where the stellar density is lower than expected. The thick-black line marks the high-luminosity gap edge hereafter referred to as “GE.” Details of defining the main sequence and GE lines are given in Appendix A. The tilted white region of the gap across the main sequence drives our selection of the white-dashed parallelogram that is the region interest (ROI); this permits evaluation of subsamples in incremental offsets above and below the GE. The same parallelogram ROI is used throughout this work.
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: The Galactic UVW velocities of our targets are shown in two panels. The two black ellipses are centered on the UVW values of (1, 14, 0) km s−1 for M dwarfs from Zhang et al. (2021). The ellipses trace 1σ (solid line) and 2σ (dotted line) regions of the dispersions with (47, 32, 28) km s−1 (Zhang et al. 2021). Red dots are active stars, and blue dots are inactive stars. The location of mean UV values for cool subdwarfs (5, −248) in the left-hand panel is off the left-hand side of the plot. The velocities presented here are relative to the local standard of rest given in Schönrich et al. (2010).
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: (Left-hand panel): the CaH band strength distribution for our targets in the enhanced HRD. This figure is similar to Figure 3, but the two dark lines are omitted to show the contrast and distribution of the points. Smaller CaH1 EW values correspond to shallower CaH band strengths and higher metallicities. (Right-hand panel): the EWs of Hα and CaH1 features for active (red dots) and inactive stars (blue dots). The two arrows mark the directions of relatively older and younger stars.
Paper: Comprehensive Analysis of a Symbiotic Candidate V503 Her
Authors: Jaroslav Merc, Rudolf Gális, Marek Wolf, Pavol A. Dubovský, Jan Kára, Forrest Sims, James R. Foster, Tomáš Medulka, Christophe Boussin, John P. Coffin, Christian Buil, David Boyd, Jacques Montier
Figure caption: Short-term light curves of V503 Her (green), TYC 2076-1319-1 (blue), and two other fainter stars (shown in gray) in the vicinity obtained in the B filter. The text in the figure gives the B − V color of the particular star and the standard deviation of the data. Note that the light curves of fainter stars have been shifted by a constant shown in the figure for clarity.
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: Windows used to determine Hα EW values. The black lines trace spectra for 79 stars with Hα absorption features and the red line represents the mean spectrum for these stars. The red box is the nominal spectral window used to measure the Hα line, with the dashed line marking the feature at 6562.8 Å in air. The two blue boxes mark the windows for the pseudo-continuum on either side. Wavelength values for all three window edges are given in Table 2.
Paper: Comprehensive Analysis of a Symbiotic Candidate V503 Her
Authors: Jaroslav Merc, Rudolf Gális, Marek Wolf, Pavol A. Dubovský, Jan Kára, Forrest Sims, James R. Foster, Tomáš Medulka, Christophe Boussin, John P. Coffin, Christian Buil, David Boyd, Jacques Montier
Figure caption: Two parts of the V503 Her light curve phased according to Equation (1). The blue and brown circles depict the minimum observed in 2004 by ASAS (V filter) and SuperWASP (unfiltered, shifted by +0.14 mag to the level of the ASAS V observations), respectively. The green and orange circles depict the minimum observed in 2017 by ASAS-SN in V and g (shifted by −0.59 mag) filters, respectively.
Paper: Comprehensive Analysis of a Symbiotic Candidate V503 Her
Authors: Jaroslav Merc, Rudolf Gális, Marek Wolf, Pavol A. Dubovský, Jan Kára, Forrest Sims, James R. Foster, Tomáš Medulka, Christophe Boussin, John P. Coffin, Christian Buil, David Boyd, Jacques Montier
Figure caption: Position of V503 Her in the H-R diagram for the obtained effective temperature 4500 ± 50 K and luminosity 1907 ± 377 L ⊙. The stellar evolutionary tracks shown in red and blue are from MIST (Choi et al. 2016; Dotter 2016).
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: Distributions of inactive (top panel) and active (bottom panel) stars in the HRD from the LAMOST using our new criteria. The two left-hand plots are scattering plots for inactive and active stars. The center four plots are two-dimensional histograms with a bin size of ∼0.05 mag at M  G  and G BP − G RP. The two-dimensional histograms for active stars are on a linear scale but on a log scale for inactive stars. The four black lines are the same lines defined in Figure 6 and are shown in two of the center plots, and they are served as a guide for the distribution of the main sequence and the gap. The red and blue dashed lines represent the best-fitted distribution for active and inactive stars, respectively. The right two plots are the histograms of M  G  with a bin size of 0.05 mag. The two dashed–dotted lines represent the fitted distribution for inactive and active stars.
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: The HRD of nearby M dwarfs from Newton et al. (2017). The left-hand plot is for M dwarfs flagged as “active” in Newton et al. (2017), and the center left-hand plot is for “inactive” M dwarfs. The center right-hand plot merges the samples in the two left-hand panels. The main sequence is divided into four regions, shown in the right-hand plot. The black lines in these four plots represent the GE (short heavy line), the fitted main sequence, and the upper and lower envelopes of the main sequence. The polynomial coefficients of these fitted lines are given in Appendix C. The insets highlight a region around our ROI, which is shown as a dashed parallelogram tracing the full ROI defined in Figure 1.
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: (Left-hand panel): the activity dip is marked as a square bracket on the enhanced HRD. This bracket is shown in all four plots. A stellar low-density region first identified in Jao & Feiden (2020, 2021) is marked in yellow. The dashed box is our ROI. (Center left-hand panel): a portion of the two-dimensional histogram of active stars in the bottom panel of Figure 11. (Center right-hand panel): a histogram of active stars. Both the center left-hand and center right-hand plots are the same as the right-hand two plots in the bottom row of Figure 11. (Right-hand panel): A distribution of percentages of active stars. The inset plot covers a larger range of this distribution. The red-dashed lines are the second-order polynomial fits of the percentages vs. M  G  from 9 to 12 mag.
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: Selected M dwarfs from Jeffers et al. (2018) in the HRD. Symbols and lines are defined in Figures 1 and 6.
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: Active and inactive stars in different Hα parameter spaces, i.e., EWHa, SNHa, Height, and SNr. (a) New criteria based on re-classified 639 M dwarfs within 100 pc. New limits are marked in black-dashed lines. The blue and red dots represent inactive and active stars determined by Z21, respectively. The colored regions are defined as active stars using the new criteria defined in this work. (b) The top panel is for inactive stars (blue dots), and the bottom panel is for active stars (red dots) originally flagged in Z21. The dashed lines mark the new criteria given in (a). This shows that some of the active stars flagged by Z21 will not be identified as active by our new criteria.
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: M dwarfs from Reiners et al. (2022) in the HRD. The left-hand plot shows stars with 〈B〉 < 1800 G in open circles, and the center plot is for stars with 〈B〉 > 1800 G in filled circles. Because of the relation between magnetic fields and Hα fluxes, the distributions shown here are proxies of Hα lines. The right-hand plot shows the entire samples in Reiners et al. (2022) and the strengths of magnetic fields in colors. The black lines and ROI are defined in Figures 1 and 6.
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: Stars from Lu et al. (2022) on the HRD. The left-hand and right-hand plots are for stars with P rot > and P rot < 10 days, respectively. Lu et al. (2022) showed that 5% of the periods longer than 10 days and 50% of the periods shorter than 10 days are possibly incorrect.
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: LAMOST spectra of two stars with multi-epoch observations. All spectra are normalized and shifted by an integer. These two stars are classified as M-type in Z21, and, obviously, the red lines are not M dwarfs. Both targets are inactive.
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: Active and inactive stars in LAMOST are selected using our new criteria. This figure is similar to Figure 1.
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: The entire sample in Reinhold & Hekker (2020) is shown in the left-hand plot. Because their targets include various young and old dwarfs selected in different K2 Campaigns, we only focus on stars falling between the upper and lower envelopes of the main sequence. Stars excluded from our statistics are plotted in black dots. The two left-hand plots are for stars with periods greater (blue dots) or less (red dots) than the critical period (P crit). The right-hand plot shows the percentage of fast-rotation stars in each bin of ΔM  G  = 0.25 in a black line. The error bars are calculated using the same method discussed in Table 5. The blue bands mark the Hα activity dip in LAMOST. The green line is the number of fast rotators in each bin. Inserted plots highlight stars within the ROI in this work.
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: The left-hand figure shows active (red dots) and inactive (blue dots) stars reported in Kiman et al. (2019) in our ROI. The top right-hand and the bottom right-hand figures are histograms of estimated V magnitudes and distances respectively for stars shown in the left-hand figure. The red and blue histograms are for active and inactive stars, respectively.
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: This figure is the same as Figure 11, but all active stars flagged by Z21 are shown. The histogram dip at M  G  ∼ 10.5 is still seen. In contrast, the histogram of inactive stars continues to be smooth as the distribution seen in Figure 11. This shows that identifying this dip is not related to how the active/inactive stars are selected.
Paper: Mind the Gap. I. Hα Activity of M Dwarfs Near the Partially/Fully Convective Boundary and a New Hα Emission Deficiency Zone on the Main Sequence
Authors: Wei-Chun Jao, 惟君 饒, Todd J. Henry, Russel J. White, Azmain H. Nisak, Hodari-Sadiki Hubbard-James, Leonardo A. Paredes, Vanders B. Lewis
Figure caption: Field stars (black dots in the left-hand plot) and young stars (red dots in the right-hand plot) in clusters with rotational periods from Popinchalk et al. (2021). The blue boxes indicate the activity dip in Figure 13.
Paper: Newly Discovered Wolf–Rayet Stars in M31
Authors: Kathryn F. Neugent, Philip Massey
Figure caption: Locations of known WRs in M31 as well as new fields observed in this survey. The blue ×’s represent WN-type stars while the red +’s represent WC-type stars from Neugent et al. (2012). The green circle is the reddened WR discovered by Shara et al. (2016). The three fields observed in this survey with LMI are denoted by black boxes.
Paper: Newly Discovered Wolf–Rayet Stars in M31
Authors: Kathryn F. Neugent, Philip Massey
Figure caption: Distribution of WN-filter magnitudes of WRs in M31 and M33. The first (a) histogram shows the magnitude distribution of the previously known WRs in M31, mostly found in the Neugent et al. (2012) Mosaic camera survey. The second (b) histogram shows the distribution of the WN magnitudes of the newly found WRs in this survey; we have also included the magnitude we measured for the star found by Shara et al. (2016). The third (c) histogram shows the distribution of the known WRs in M33, mostly found by Neugent & Massey (2011) but also including the handful of WRs found subsequently (e.g., Neugent & Massey 2014; Massey et al. 2016). In all three histograms, the vertical line shows our estimated limiting magnitude based on a S/N of 35. The data suggest that the Mosaic M31 survey was incomplete due to sensitivity, but that our new LMI frames go deep enough. In contrast, there are unlikely to be many new WRs to be found in M33.
Paper: Newly Discovered Wolf–Rayet Stars in M31
Authors: Kathryn F. Neugent, Philip Massey
Figure caption: Spectra of representative WNs. We show four example spectra of newly found WN-type stars in M31. The spectra have been normalized, and only a portion of our wavelength coverage is shown for clarity. Each spectrum is offset from the previous by a relative intensity of 3.0. Lines identified include N IV λ4058, the He II/Hδ blend (contaminated by nebular emission in X004431.39+412114.0 and J004433.91+412501.2), He II λ4200, the He II/Hγ blend (with similar nebular contamination), He II λ4542, and the N V λ λ4603, 19 and N III λ4634, 42 doublets, as well as He II λ4686. Note that the unnormalized version of these, and all of our spectra, are being made available in FITS format as part of this publication as “data behind figures.”(The data used to create this figure are available.)
Paper: Newly Discovered Wolf–Rayet Stars in M31
Authors: Kathryn F. Neugent, Philip Massey
Figure caption: Using image subtraction to identify WR candidates. We used HOTPANTS (Becker 2015) to subtract the continuum image from the WN image to produce the final result. This particular region of the sky shows a previously known WR (yellow dashed circle), a saturated star that leads to a poor image-subtraction result (green box), a M-type star that shows up due to TiO absorption in the continuum filter (red ×), and a new WR candidate that was missed in our previous survey due to its faint magnitude (blue solid circle).
Paper: Newly Discovered Wolf–Rayet Stars in M31
Authors: Kathryn F. Neugent, Philip Massey
Figure caption: Spectra of representative WC/WOs. We show three example spectra of newly found WC/WO-type stars in M31. The spectra have been normalized, and only a portion of our wavelength coverage is shown for clarity. Each spectrum is offset from the previous by a relative intensity of 2.0. Lines identified include the O VI doublet λ λ3811, 34 (X004418.10+411850.8), the upper Balmer lines (visible in X004032.57+403901.3 and X004425.09+412046.4), the C III/IV λ4650 feature, and the classification lines O V λ5592, C III λ5696, and C IV λ5806. Note that the unnormalized version of these, and all of our spectra, are being made available in FITS format as part of this publication as “data behind figures.”
Paper: Newly Discovered Wolf–Rayet Stars in M31
Authors: Kathryn F. Neugent, Philip Massey
Figure caption: The relative proportion of WN subtypes compared to both the previously known and newly discovered sample of M31 WNs. While the total number of stars in each group differs, their distributions are fairly similar. This suggests that the newly discovered WRs in M31 are not predominantly part of an intrinsically fainter group of WRs.
Paper: What’s the Difference? The Potential for Convolutional Neural Networks for Transient Detection without Template Subtraction
Authors: Tatiana Acero-Cuellar, Federica Bianco, Gregory Dobler, Masao Sako, Helen Qu
Figure caption: Transients (diff–srch–tmpl) and their respective saliency maps for DIA-based model FPs (bogus predicted as real). We remind the reader again that the labels are inherited from Goldstein et al. (2015) and cannot be verified. Some level of label inaccuracy is expected. Bogus transients were labeled by human scanners among astrophysical images with detection. However, in this collection, we cannot verify the nature of the transient, and we argue that in the cases presented here, there is no obvious evidence of its bogus nature. Important pixels are most commonly found in the diff, but in tmpl and srch, we again see that the CNN analyzes the central source and its surroundings but avoids the tail of the central source in a way similar to traditional aperture photometry techniques.
Paper: What’s the Difference? The Potential for Convolutional Neural Networks for Transient Detection without Template Subtraction
Authors: Tatiana Acero-Cuellar, Federica Bianco, Gregory Dobler, Masao Sako, Helen Qu
Figure caption: Transients (srch–tmpl) and their respective saliency maps for the noDIA model FPs (bogus classified as real). Important pixels are found everywhere in the image as the CNN learns how to compare the diff and tmpl by taking a synoptic look at the properties of each image component.