adsabs/AstroCLIMB huggingface dataset:
Paper: A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images
Authors: Tianjun Gan, Charles Cadieux, Farbod Jahandar, Allona Vazan, Sharon X. Wang, Shude Mao, Jaime A. Alvarado-Montes, D. N. C. Lin, Étienne Artigau, Neil J. Cook, René Doyon, Andrew W. Mann, Keivan G. Stassun, Adam J. Burgasser, Benjamin V. Rackham, Steve B. Howell, Karen A. Collins, Khalid Barkaoui, Avi Shporer, Jerome de Leon, Luc Arnold, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Artem Burdanov, David Charbonneau, Georgina Dransfield, Akihiko Fukui, Elise Furlan, Michaël Gillon, Matthew J. Hooton, Hannah M. Lewis, Colin Littlefield, Ismael Mireles, Norio Narita, Chris W. Ormel, Samuel N. Quinn, Ramotholo Sefako, Mathilde Timmermans, Michael Vezie, Julien de Wit
Figure caption: SPIRou observation of OH and Fe I lines of TOI-4201 (black dashed line). The solid lines represent the ACES models for different overall metallicities [M/H] and the fixed T eff of 3800 K. These plots illustrate the good sensitivity of near-IR high-resolution spectroscopy for constraining the chemical abundances of OH and Fe lines.
Paper: A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images
Authors: Tianjun Gan, Charles Cadieux, Farbod Jahandar, Allona Vazan, Sharon X. Wang, Shude Mao, Jaime A. Alvarado-Montes, D. N. C. Lin, Étienne Artigau, Neil J. Cook, René Doyon, Andrew W. Mann, Keivan G. Stassun, Adam J. Burgasser, Benjamin V. Rackham, Steve B. Howell, Karen A. Collins, Khalid Barkaoui, Avi Shporer, Jerome de Leon, Luc Arnold, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Artem Burdanov, David Charbonneau, Georgina Dransfield, Akihiko Fukui, Elise Furlan, Michaël Gillon, Matthew J. Hooton, Hannah M. Lewis, Colin Littlefield, Ismael Mireles, Norio Narita, Chris W. Ormel, Samuel N. Quinn, Ramotholo Sefako, Mathilde Timmermans, Michael Vezie, Julien de Wit
Figure caption: The GLS periodograms of the TESS and ZTF photometry. The black solid and dashed lines are the results of TESS, while the colored lines are from ZTF, with filter and CCD ID shown in the legend. The vertical gray line represents the ∼17-day rotational signal of TOI-4201. A zoomed-in plot is shown in the upper right corner.
Paper: A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images
Authors: Tianjun Gan, Charles Cadieux, Farbod Jahandar, Allona Vazan, Sharon X. Wang, Shude Mao, Jaime A. Alvarado-Montes, D. N. C. Lin, Étienne Artigau, Neil J. Cook, René Doyon, Andrew W. Mann, Keivan G. Stassun, Adam J. Burgasser, Benjamin V. Rackham, Steve B. Howell, Karen A. Collins, Khalid Barkaoui, Avi Shporer, Jerome de Leon, Luc Arnold, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Artem Burdanov, David Charbonneau, Georgina Dransfield, Akihiko Fukui, Elise Furlan, Michaël Gillon, Matthew J. Hooton, Hannah M. Lewis, Colin Littlefield, Ismael Mireles, Norio Narita, Chris W. Ormel, Samuel N. Quinn, Ramotholo Sefako, Mathilde Timmermans, Michael Vezie, Julien de Wit
Figure caption: MagE optical spectrum of TOI-4201 in normalized F  λ  units (black line; uncertainties in gray), compared to the best-match M1 dwarf spectral template (magenta line; data from Bochanski et al. 2007). We also label typical spectral absorption features for M dwarfs and regions of uncorrected telluric absorption (⊕). The inset box shows a close-up of the 6530–6780 Å region, indicating Hα in absorption and no Li I detection.
Paper: A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images
Authors: Tianjun Gan, Charles Cadieux, Farbod Jahandar, Allona Vazan, Sharon X. Wang, Shude Mao, Jaime A. Alvarado-Montes, D. N. C. Lin, Étienne Artigau, Neil J. Cook, René Doyon, Andrew W. Mann, Keivan G. Stassun, Adam J. Burgasser, Benjamin V. Rackham, Steve B. Howell, Karen A. Collins, Khalid Barkaoui, Avi Shporer, Jerome de Leon, Luc Arnold, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Artem Burdanov, David Charbonneau, Georgina Dransfield, Akihiko Fukui, Elise Furlan, Michaël Gillon, Matthew J. Hooton, Hannah M. Lewis, Colin Littlefield, Ismael Mireles, Norio Narita, Chris W. Ormel, Samuel N. Quinn, Ramotholo Sefako, Mathilde Timmermans, Michael Vezie, Julien de Wit
Figure caption: SED of TOI-4201. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best-fit PHOENIX atmosphere model (black). The Gaia spectrum is shown as a gray swathe; the inset focuses on the Gaia spectrum.
Paper: A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images
Authors: Tianjun Gan, Charles Cadieux, Farbod Jahandar, Allona Vazan, Sharon X. Wang, Shude Mao, Jaime A. Alvarado-Montes, D. N. C. Lin, Étienne Artigau, Neil J. Cook, René Doyon, Andrew W. Mann, Keivan G. Stassun, Adam J. Burgasser, Benjamin V. Rackham, Steve B. Howell, Karen A. Collins, Khalid Barkaoui, Avi Shporer, Jerome de Leon, Luc Arnold, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Artem Burdanov, David Charbonneau, Georgina Dransfield, Akihiko Fukui, Elise Furlan, Michaël Gillon, Matthew J. Hooton, Hannah M. Lewis, Colin Littlefield, Ismael Mireles, Norio Narita, Chris W. Ormel, Samuel N. Quinn, Ramotholo Sefako, Mathilde Timmermans, Michael Vezie, Julien de Wit
Figure caption: Top panel: the GLS periodogram of SPIRou RVs of TOI-4201. Bottom panel: the GLS periodogram of SPIRou RVs but after subtracting the best-fitting Keplerian model of TOI-4201b. In both panels, the theoretical FAP levels of 10%, 1%, and 0.1% are shown with horizontal dashed, dotted–dashed and dotted lines. The orbital period of TOI-4201b is shown with a vertical solid line. Another two significant peaks around 0.78 and 1.38 days (vertical dashed lines) are the signals due to frequency beating.
Paper: A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images
Authors: Tianjun Gan, Charles Cadieux, Farbod Jahandar, Allona Vazan, Sharon X. Wang, Shude Mao, Jaime A. Alvarado-Montes, D. N. C. Lin, Étienne Artigau, Neil J. Cook, René Doyon, Andrew W. Mann, Keivan G. Stassun, Adam J. Burgasser, Benjamin V. Rackham, Steve B. Howell, Karen A. Collins, Khalid Barkaoui, Avi Shporer, Jerome de Leon, Luc Arnold, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Artem Burdanov, David Charbonneau, Georgina Dransfield, Akihiko Fukui, Elise Furlan, Michaël Gillon, Matthew J. Hooton, Hannah M. Lewis, Colin Littlefield, Ismael Mireles, Norio Narita, Chris W. Ormel, Samuel N. Quinn, Ramotholo Sefako, Mathilde Timmermans, Michael Vezie, Julien de Wit
Figure caption: The TESS and ground-based light curves folded in phase with the orbital period of TOI-4201b. The red solid lines are the best-fit transit models. Instrument name and filter information are given in the lower left corner of each panel.
Paper: A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images
Authors: Tianjun Gan, Charles Cadieux, Farbod Jahandar, Allona Vazan, Sharon X. Wang, Shude Mao, Jaime A. Alvarado-Montes, D. N. C. Lin, Étienne Artigau, Neil J. Cook, René Doyon, Andrew W. Mann, Keivan G. Stassun, Adam J. Burgasser, Benjamin V. Rackham, Steve B. Howell, Karen A. Collins, Khalid Barkaoui, Avi Shporer, Jerome de Leon, Luc Arnold, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Artem Burdanov, David Charbonneau, Georgina Dransfield, Akihiko Fukui, Elise Furlan, Michaël Gillon, Matthew J. Hooton, Hannah M. Lewis, Colin Littlefield, Ismael Mireles, Norio Narita, Chris W. Ormel, Samuel N. Quinn, Ramotholo Sefako, Mathilde Timmermans, Michael Vezie, Julien de Wit
Figure caption: Gemini high-resolution speckle imaging 5σ contrast limits as a function of angular separation. We show a separate curve for each filter and the 832 nm reconstructed image. TOI-4201 has no close companions within the angular and contrast levels achieved.
Paper: A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images
Authors: Tianjun Gan, Charles Cadieux, Farbod Jahandar, Allona Vazan, Sharon X. Wang, Shude Mao, Jaime A. Alvarado-Montes, D. N. C. Lin, Étienne Artigau, Neil J. Cook, René Doyon, Andrew W. Mann, Keivan G. Stassun, Adam J. Burgasser, Benjamin V. Rackham, Steve B. Howell, Karen A. Collins, Khalid Barkaoui, Avi Shporer, Jerome de Leon, Luc Arnold, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Artem Burdanov, David Charbonneau, Georgina Dransfield, Akihiko Fukui, Elise Furlan, Michaël Gillon, Matthew J. Hooton, Hannah M. Lewis, Colin Littlefield, Ismael Mireles, Norio Narita, Chris W. Ormel, Samuel N. Quinn, Ramotholo Sefako, Mathilde Timmermans, Michael Vezie, Julien de Wit
Figure caption: Left panel: the time-series SPIRou RVs of TOI-4201. Right panel: the RVs phased-folded to the orbit period of TOI-4201b. In both panels, the black solid lines are the best Keplerian model from the joint fit. The orange shaded region denotes the 1σ credible intervals of the RV model. Residuals are plotted below.
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: Violin plot for the posteriors of several key physical and chemical parameters derived from all the nine retrieval runs (Section 7). The left three columns (blue) correspond to the retrievals on the ﹩K1/K2/L^{\prime} ﹩ photometry and the Mesa et al. (2023) spectrum (Section 7.1). The middle three columns (green) correspond to the retrievals on the ﹩K1/K2/L^{\prime} ﹩ photometry and the De Rosa et al. (2023) spectrum (Section 7.2). The right three columns (red) correspond to the retrievals on the ﹩K1/K2/L^{\prime} ﹩ photometry and both the Mesa et al. (2023) and De Rosa et al. (2023) spectra. Plots with darker blue/green/red colors suggest the addition of narrower and constrained priors on M (slightly darker) or both M and R (much darker). The measured [Fe/H] of the host star AF Lep A (−0.27 ± 0.31 dex, Section 3) is shown as a purple shade in the top panel.
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: Results of the retrieval analysis on ﹩K1/K2/L^{\prime} ﹩ photometry and the Mesa et al. (2023) spectrum of AF Lep b (Section 7.1). In the top two panels, we compare the observed spectrophotometry (colored circles with the same format as Figure 1; the wavelength error bars of the ﹩K1/K2/L^{\prime} ﹩ photometric data represent the half effective widths of the corresponding filters) with the emission spectrum corresponding to the best-fit model (thick orange line). Emission spectra generated at 100 random draws from the parameter posteriors (thin orange lines) are overlaid. In the middle section, on the left panel, we present the 1σ/2σ/3σ confidence intervals (orange shades) of our retrieved T–P profiles. A profile with median T–P parameters is shown in black and the corresponding weighted contribution function (computed over the same wavelength range as the input data) is shown as a gray shade. The remaining panels present the posterior distributions of key physical parameters: [Fe/H], C/O, ﹩\mathrm{log}(g)﹩, R, and T eff. The median and confidence intervals of all parameters are summarized in Table 6.
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: The forward-modeled emission spectra (R = 1000) over a mini-grid of parameter space in the vicinity of AF Lep b’s properties (Section 6.4). The black spectrum corresponds to a cloudy model with T eff = 800 K, ﹩\mathrm{log}(g)=4.0﹩ dex, [Fe/H] = 0.5 dex, C/O = 0.55 dex, ﹩\mathrm{log}({P}_{\mathrm{quench}}/1\ \mathrm{bar})=3﹩, and f sed = 2 and ﹩\mathrm{log}({K}_{zz})=8﹩ for both MgSiO3 and Fe clouds, whose mass fractions at the base pressures are ﹩\mathrm{log}({X}_{0})=-2﹩ dex and −4 dex, respectively. In each panel, we use orange/blue colors to show the spectral effect when a certain parameter is increased/decreased by the labeled amount (top and middle panels) or is removed (bottom panels).
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: Top left: Our adopted Gaussian priors for the temperature gradient ﹩(d\mathrm{ln}T/d\mathrm{ln}P)﹩ at six pressure layers, with layer numbers one and six corresponding to the bottom and top of the atmosphere with P = 103 bar and 10−3 bar, respectively. Top right: The ﹩{(d\mathrm{ln}T/d\mathrm{ln}P)}_{\mathrm{RCE}}﹩ profile of the ATMO2020 model grid. The black line is the median profile among all grid points and the blue shaded regions represent (from dark to light) the 1σ, 2σ, and 3σ confidence intervals. Black circles mark the ﹩{(d\mathrm{ln}T/d\mathrm{ln}P)}_{\mathrm{RCE}}﹩ value of the six pressure layers. Overlaid orange lines (solid: median; dashed–dotted: 1σ boundary; dashed: 2σ boundary; dotted: 3σ boundary) represent our adopted priors. For these prior profiles, the median and confidence intervals at the six pressure layers are described in the top left panel, and the values between these layers are calculated via a quadratic interpolation (in logarithmic scale of pressure). Middle and bottom: These panels share the format of the top right panel but with different forward model grids as summarized in Table 4.
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: Corner plot for the retrieval runs performed with default parameter priors (gray) and with constrained priors on the planet’s mass, ﹩{ \mathcal N }(\mu =2.8\ {M}_{\mathrm{Jup}},\sigma =0.6\ {M}_{\mathrm{Jup}})﹩, and radius, ﹩{ \mathcal U }(1.20\ {R}_{\mathrm{Jup}},1.55\ {R}_{\mathrm{Jup}})﹩ (orange). We show 1σ/2σ/3σ confidence intervals for parameters inferred by the former retrieval (with default priors), but only present 1σ/2σ confidence intervals for the latter in order to prevent visual overlap. Both retrieval runs are performed on ﹩K1/K2/L^{\prime} ﹩ photometry and both the Mesa et al. (2023) and De Rosa et al. (2023) spectra (Section 7.3).
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: Results of the retrieval analysis on ﹩K1/K2/L^{\prime} ﹩ photometry and both the Mesa et al. (2023) and De Rosa et al. (2023) spectra of AF Lep b (Section 7.2), with the same format as Figure 7.
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: Violin plot for the physical properties of AF Lep b inferred by various evolution models (sorted by radii), based on the planet’s dynamical mass and age. The vertical dashed line inside each component highlights the median value of the parameter, while the two dotted lines mark the first and third quartiles of the distribution. The labels and the parameter confidence intervals are shown in Table 3.
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: Sketch of the temperature model described in Section 6.1.
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: Results of the retrieval analysis on ﹩K1/K2/L^{\prime} ﹩ photometry and the De Rosa et al. (2023) spectrum of AF Lep b (Section 7.2), with the same format as Figure 7.
Paper: Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b
Authors: Napaporn A-thano, Supachai Awiphan, Ing-Guey Jiang, Eamonn Kerins, Akshay Priyadarshi, Iain McDonald, Yogesh C. Joshi, Thansuda Chulikorn, Joshua J. C. Hayes, Stephen Charles, Chung-Kai Huang, Ronnakrit Rattanamala, Li-Chin Yeh, Vik S Dhillon
Figure caption: Individual SPEARNET transit light curves of HAT-P-26 b from observations in 2015–2018. The light curves are normalized (gray dots) and modeled by TransitFit (solid lines). The light curves are observed in the ﹩g^{\prime} ﹩ (blue), ﹩r^{\prime} ﹩ (yellow), R (orange), ﹩i^{\prime} ﹩ (red), I (dark red), and ﹩z^{\prime} ﹩ (brown) filters. 5 minute binned light curves are shown by the red dots.
Paper: Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b
Authors: Napaporn A-thano, Supachai Awiphan, Ing-Guey Jiang, Eamonn Kerins, Akshay Priyadarshi, Iain McDonald, Yogesh C. Joshi, Thansuda Chulikorn, Joshua J. C. Hayes, Stephen Charles, Chung-Kai Huang, Ronnakrit Rattanamala, Li-Chin Yeh, Vik S Dhillon
Figure caption: Posterior probability distribution of the linear ephemeris MCMC fitting parameters for the 33 midtransit times obtained from TransitFit.
Paper: Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b
Authors: Napaporn A-thano, Supachai Awiphan, Ing-Guey Jiang, Eamonn Kerins, Akshay Priyadarshi, Iain McDonald, Yogesh C. Joshi, Thansuda Chulikorn, Joshua J. C. Hayes, Stephen Charles, Chung-Kai Huang, Ronnakrit Rattanamala, Li-Chin Yeh, Vik S Dhillon
Figure caption: Posterior probability distribution of the linear ephemeris MCMC fitting parameters for considering all 39 midtransit times.
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: Photometric data on V503 Her. (a) Historical light curve of V503 Her, covering the period 1922–2023, constructed on the basis of data from DASCH, Sonnenberg plates (Meinunger 1980), NSVS, AAVSO, ASAS, SuperWASP, ASAS-SN, and ZTF. (b) Part of the V503 Her light curve (2002–2023). The solid vertical gray lines mark the position of deep minima discussed in the text, while the dashed vertical line denotes the minimum considered an eclipse by Gromadzki et al. (2013). The horizontal dotted lines show the level of the brightness of the object in the middle of the minima in 2004 and 2009, respectively. Arrows denote the times when our spectra were obtained. (c, d) Changes in the pulsation amplitude and timescale in the light curve of V503 Her.
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: Multifrequency SED of V503 Her (green circles) constructed on the basis of data from the GALEX satellite, Gaia EDR3, Pan-STARRS, APASS, 2MASS, and WISE. The best-fitting theoretical spectrum (Allard 2014) is shown in red. The spectrum shown in gray corresponds to the collective radiation of two background sources calibrated to its combined flux in the Gaia G filter (blue circle). See the text for more details.
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: Periodogram (top panel) and spectral window (bottom panel) of the initial step of the period analysis of the V503 Her light curve based on the ASAS-SN survey data in the V and g filters. The most prominent periods (see Table 4) and their 1 yr aliases (assigned based on colors) are indicated by vertical lines with labels. Note that periods 142.4 and 161.5 days were only detected after removing the period responses found in the previous steps of the sequential analysis, and thus their peaks are overlaid by the nearby periods 149.1 and 171.7 days.
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: Low-resolution spectra of V503 Her (green) obtained in various photometric phases (pulsation maxima in 2021 and 2023, pulsation minima in 2013 and 2021, acquired at JD 2,459,270, 2,460,037, 2,456,448, and 2,459,373, respectively). The best-fitting empirical spectra from the MILES library (Falcón-Barroso et al. 2011) are shown in red.