adsabs/AstroCLIMB huggingface dataset:
Paper: TrES-1 b: A Case Study in Detecting Secular Evolution of Exoplanet Orbits
Authors: Simone R. Hagey, Billy Edwards, Angelos Tsiaras, Aaron C. Boley, Anastasia Kokori, Norio Narita, Pedro V. Sada, Filip Walter, Robert T. Zellem, Napaporn A-thano, Kevin B. Alton, Miguel Ángel Álava Amat, Paul Benni, Emmanuel Besson, Patrick Brandebourg, Marc Bretton, Mauro Caló, Martin Valentine Crow, Jean-Christophe Dalouzy, Marc Deldem, Tõnis Eenmäe, Stephane Ferratfiat, Pere Guerra, Gary Vander Haagen, Ken Hose, Adrian Jones, Yves Jongen, Didier Laloum, Stefano Lora, Alessandro Marchini, Jacques Michelet, Matej Mihelčič, Johannes Mieglitz, Eric Miny, David Molina, Mario Morales Aimar, Raphael Nicollerat, Ivo Peretto, Manfred Raetz, François Regembal, Robert Roth, Lionel Rousselot, Mark Salisbury, Darryl Sergison, Anaël Wünsche, Jaroslav Trnka
Figure caption: Lomb–Scargle periodogram of the residuals from the TrES-1 b RV model fit (see Figure 3). The x-axis displays frequencies in units of days−1 and the corresponding periods are shown on the top axis. The frequency range was selected by restricting the periods to between 1000 and 4300 days, the latter corresponding to the duration of the RV observation baseline. Labeled peaks indicate potentially significant periodic signals with periods of 3567, 1788, 1383, and 1194 days, suggesting possible planetary companions. These peaks informed subsequent RV fits to investigate evidence for a second planet in the TrES-1 system.
Paper: TrES-1 b: A Case Study in Detecting Secular Evolution of Exoplanet Orbits
Authors: Simone R. Hagey, Billy Edwards, Angelos Tsiaras, Aaron C. Boley, Anastasia Kokori, Norio Narita, Pedro V. Sada, Filip Walter, Robert T. Zellem, Napaporn A-thano, Kevin B. Alton, Miguel Ángel Álava Amat, Paul Benni, Emmanuel Besson, Patrick Brandebourg, Marc Bretton, Mauro Caló, Martin Valentine Crow, Jean-Christophe Dalouzy, Marc Deldem, Tõnis Eenmäe, Stephane Ferratfiat, Pere Guerra, Gary Vander Haagen, Ken Hose, Adrian Jones, Yves Jongen, Didier Laloum, Stefano Lora, Alessandro Marchini, Jacques Michelet, Matej Mihelčič, Johannes Mieglitz, Eric Miny, David Molina, Mario Morales Aimar, Raphael Nicollerat, Ivo Peretto, Manfred Raetz, François Regembal, Robert Roth, Lionel Rousselot, Mark Salisbury, Darryl Sergison, Anaël Wünsche, Jaroslav Trnka
Figure caption: Transit (top) and eclipse (bottom) timing variations for TrES-1 b. Each data point represents the difference between an observed time and the expected midpoint from the best-fit constant-period, circular orbit model. The plot shows 300 random samples from the weighted posterior distributions of the joint model fits—which included RV data—for the constant-period, orbital decay, and apsidal precession models.
Paper: TrES-1 b: A Case Study in Detecting Secular Evolution of Exoplanet Orbits
Authors: Simone R. Hagey, Billy Edwards, Angelos Tsiaras, Aaron C. Boley, Anastasia Kokori, Norio Narita, Pedro V. Sada, Filip Walter, Robert T. Zellem, Napaporn A-thano, Kevin B. Alton, Miguel Ángel Álava Amat, Paul Benni, Emmanuel Besson, Patrick Brandebourg, Marc Bretton, Mauro Caló, Martin Valentine Crow, Jean-Christophe Dalouzy, Marc Deldem, Tõnis Eenmäe, Stephane Ferratfiat, Pere Guerra, Gary Vander Haagen, Ken Hose, Adrian Jones, Yves Jongen, Didier Laloum, Stefano Lora, Alessandro Marchini, Jacques Michelet, Matej Mihelčič, Johannes Mieglitz, Eric Miny, David Molina, Mario Morales Aimar, Raphael Nicollerat, Ivo Peretto, Manfred Raetz, François Regembal, Robert Roth, Lionel Rousselot, Mark Salisbury, Darryl Sergison, Anaël Wünsche, Jaroslav Trnka
Figure caption: Stellar rotation period as a function of the modified stellar quality factor, ﹩{Q}_{\star }^{{\prime} }﹩, for a scenario in which stellar tides drive orbital decay at a rate of −7.1 ms yr−1. The calculations use the exact expression for decay due to tides in the star (Equation (A1)) for different combinations of stellar obliquity (ε⋆) and orbital eccentricity (e). There is no parameter space in which ﹩{Q}_{\star }^{{\prime} }﹩ falls within the empirically expected range of ﹩1{0}^{5}\lt {Q}_{\star }^{{\prime} }\lt 1{0}^{8}﹩ (K. Penev et al. 2018). Left: the required ﹩{Q}_{\star }^{{\prime} }﹩ for different eccentricities when the stellar obliquity is zero. Right: the required ﹩{Q}_{\star }^{{\prime} }﹩ for different obliquities when the orbital eccentricity is zero.
Paper: TrES-1 b: A Case Study in Detecting Secular Evolution of Exoplanet Orbits
Authors: Simone R. Hagey, Billy Edwards, Angelos Tsiaras, Aaron C. Boley, Anastasia Kokori, Norio Narita, Pedro V. Sada, Filip Walter, Robert T. Zellem, Napaporn A-thano, Kevin B. Alton, Miguel Ángel Álava Amat, Paul Benni, Emmanuel Besson, Patrick Brandebourg, Marc Bretton, Mauro Caló, Martin Valentine Crow, Jean-Christophe Dalouzy, Marc Deldem, Tõnis Eenmäe, Stephane Ferratfiat, Pere Guerra, Gary Vander Haagen, Ken Hose, Adrian Jones, Yves Jongen, Didier Laloum, Stefano Lora, Alessandro Marchini, Jacques Michelet, Matej Mihelčič, Johannes Mieglitz, Eric Miny, David Molina, Mario Morales Aimar, Raphael Nicollerat, Ivo Peretto, Manfred Raetz, François Regembal, Robert Roth, Lionel Rousselot, Mark Salisbury, Darryl Sergison, Anaël Wünsche, Jaroslav Trnka
Figure caption: RV residuals (see Figure 3) and best-fit orbital model for the proposed planetary companion TrES-1 c. Top left: RV measurements over time, with data points shifted by the systemic RV and observation times shifted to the reference time, t0. Bottom left: residuals obtained by subtracting the best-fit RV model from the data. Right: phase-folded RV measurements plotted against mean anomaly, with 300 random samples from the model posterior shown in gray to represent model uncertainty. Data sources are color coded as indicated in the legend.
Paper: TrES-1 b: A Case Study in Detecting Secular Evolution of Exoplanet Orbits
Authors: Simone R. Hagey, Billy Edwards, Angelos Tsiaras, Aaron C. Boley, Anastasia Kokori, Norio Narita, Pedro V. Sada, Filip Walter, Robert T. Zellem, Napaporn A-thano, Kevin B. Alton, Miguel Ángel Álava Amat, Paul Benni, Emmanuel Besson, Patrick Brandebourg, Marc Bretton, Mauro Caló, Martin Valentine Crow, Jean-Christophe Dalouzy, Marc Deldem, Tõnis Eenmäe, Stephane Ferratfiat, Pere Guerra, Gary Vander Haagen, Ken Hose, Adrian Jones, Yves Jongen, Didier Laloum, Stefano Lora, Alessandro Marchini, Jacques Michelet, Matej Mihelčič, Johannes Mieglitz, Eric Miny, David Molina, Mario Morales Aimar, Raphael Nicollerat, Ivo Peretto, Manfred Raetz, François Regembal, Robert Roth, Lionel Rousselot, Mark Salisbury, Darryl Sergison, Anaël Wünsche, Jaroslav Trnka
Figure caption: The expected orbital period derivative for TrES-1 b under the assumption that stellar tides dominate its orbital evolution, as a function of the modified stellar quality factor ﹩{Q}_{\star }^{{\prime} }﹩. The solid blue horizontal line represents the best-fit orbital decay rate for TrES-1 b, with the shaded region indicating the corresponding 68% credible interval. Three specific values of ﹩{Q}_{\star }^{{\prime} }﹩ are highlighted: (1) the value derived from the best-fit orbital decay rate using Equation (17), (2) the predicted value from the tidal forcing period of the system using Equation (18), and (3) the value inferred for WASP-12, an HJ decaying at ∼30 ms yr−1, from I. Wong et al. (2022).
Paper: TrES-1 b: A Case Study in Detecting Secular Evolution of Exoplanet Orbits
Authors: Simone R. Hagey, Billy Edwards, Angelos Tsiaras, Aaron C. Boley, Anastasia Kokori, Norio Narita, Pedro V. Sada, Filip Walter, Robert T. Zellem, Napaporn A-thano, Kevin B. Alton, Miguel Ángel Álava Amat, Paul Benni, Emmanuel Besson, Patrick Brandebourg, Marc Bretton, Mauro Caló, Martin Valentine Crow, Jean-Christophe Dalouzy, Marc Deldem, Tõnis Eenmäe, Stephane Ferratfiat, Pere Guerra, Gary Vander Haagen, Ken Hose, Adrian Jones, Yves Jongen, Didier Laloum, Stefano Lora, Alessandro Marchini, Jacques Michelet, Matej Mihelčič, Johannes Mieglitz, Eric Miny, David Molina, Mario Morales Aimar, Raphael Nicollerat, Ivo Peretto, Manfred Raetz, François Regembal, Robert Roth, Lionel Rousselot, Mark Salisbury, Darryl Sergison, Anaël Wünsche, Jaroslav Trnka
Figure caption: Required planetary obliquity (εp) as a function of the modified tidal quality factor (﹩{Q}_{p}^{{\prime} }﹩) for TrES-1 b, assuming obliquity tides are the dominant mechanism driving orbital decay. The black curve and surrounding gray region show the obliquity values needed to match the best-fit decay rate of ﹩-7.{1}_{-1.6}^{+\,1.5}﹩ ms yr−1. The shaded blue region represents the theoretically expected range of ﹩{Q}_{p}^{{\prime} }﹩ for HJs (M. M. Mahmud et al. 2023), while the red dashed line marks the estimated value for Jupiter (V. Lainey et al. 2009). Obliquity values εp ≳ 30° yield ﹩{Q}_{p}^{{\prime} }﹩ estimates that are consistent with theoretical expectations.
Paper: TrES-1 b: A Case Study in Detecting Secular Evolution of Exoplanet Orbits
Authors: Simone R. Hagey, Billy Edwards, Angelos Tsiaras, Aaron C. Boley, Anastasia Kokori, Norio Narita, Pedro V. Sada, Filip Walter, Robert T. Zellem, Napaporn A-thano, Kevin B. Alton, Miguel Ángel Álava Amat, Paul Benni, Emmanuel Besson, Patrick Brandebourg, Marc Bretton, Mauro Caló, Martin Valentine Crow, Jean-Christophe Dalouzy, Marc Deldem, Tõnis Eenmäe, Stephane Ferratfiat, Pere Guerra, Gary Vander Haagen, Ken Hose, Adrian Jones, Yves Jongen, Didier Laloum, Stefano Lora, Alessandro Marchini, Jacques Michelet, Matej Mihelčič, Johannes Mieglitz, Eric Miny, David Molina, Mario Morales Aimar, Raphael Nicollerat, Ivo Peretto, Manfred Raetz, François Regembal, Robert Roth, Lionel Rousselot, Mark Salisbury, Darryl Sergison, Anaël Wünsche, Jaroslav Trnka
Figure caption: Required orbit eccentricity (e) as a function of the modified tidal quality factor (﹩{Q}_{p}^{{\prime} }﹩) for TrES-1 b, assuming eccentricity tides are the dominant mechanism driving orbital decay. The black curve and surrounding gray region show the eccentricity values needed to match the best-fit decay rate of ﹩-7.{1}_{-1.6}^{+\,1.5}﹩ ms yr−1. The shaded blue region represents the theoretically expected range of ﹩{Q}_{p}^{{\prime} }﹩ for HJs (M. M. Mahmud et al. 2023), while the red dashed line marks the estimated value for Jupiter (V. Lainey et al. 2009). The fact that the required eccentricity (e ≳ 0.2) falls well outside observational constraints suggests that eccentricity tides cannot drive orbital decay.
Paper: TrES-1 b: A Case Study in Detecting Secular Evolution of Exoplanet Orbits
Authors: Simone R. Hagey, Billy Edwards, Angelos Tsiaras, Aaron C. Boley, Anastasia Kokori, Norio Narita, Pedro V. Sada, Filip Walter, Robert T. Zellem, Napaporn A-thano, Kevin B. Alton, Miguel Ángel Álava Amat, Paul Benni, Emmanuel Besson, Patrick Brandebourg, Marc Bretton, Mauro Caló, Martin Valentine Crow, Jean-Christophe Dalouzy, Marc Deldem, Tõnis Eenmäe, Stephane Ferratfiat, Pere Guerra, Gary Vander Haagen, Ken Hose, Adrian Jones, Yves Jongen, Didier Laloum, Stefano Lora, Alessandro Marchini, Jacques Michelet, Matej Mihelčič, Johannes Mieglitz, Eric Miny, David Molina, Mario Morales Aimar, Raphael Nicollerat, Ivo Peretto, Manfred Raetz, François Regembal, Robert Roth, Lionel Rousselot, Mark Salisbury, Darryl Sergison, Anaël Wünsche, Jaroslav Trnka
Figure caption: Similar to Figure 6, but extended to include orbital periods up to 1 yr. The three mass categories—planet, brown dwarf, and star—are illustrated along the y-axis. The green shaded region again denotes the RV detection limit, same as in Figure 6.
Paper: TrES-1 b: A Case Study in Detecting Secular Evolution of Exoplanet Orbits
Authors: Simone R. Hagey, Billy Edwards, Angelos Tsiaras, Aaron C. Boley, Anastasia Kokori, Norio Narita, Pedro V. Sada, Filip Walter, Robert T. Zellem, Napaporn A-thano, Kevin B. Alton, Miguel Ángel Álava Amat, Paul Benni, Emmanuel Besson, Patrick Brandebourg, Marc Bretton, Mauro Caló, Martin Valentine Crow, Jean-Christophe Dalouzy, Marc Deldem, Tõnis Eenmäe, Stephane Ferratfiat, Pere Guerra, Gary Vander Haagen, Ken Hose, Adrian Jones, Yves Jongen, Didier Laloum, Stefano Lora, Alessandro Marchini, Jacques Michelet, Matej Mihelčič, Johannes Mieglitz, Eric Miny, David Molina, Mario Morales Aimar, Raphael Nicollerat, Ivo Peretto, Manfred Raetz, François Regembal, Robert Roth, Lionel Rousselot, Mark Salisbury, Darryl Sergison, Anaël Wünsche, Jaroslav Trnka
Figure caption: Transit (top) and eclipse (bottom) timing variations for TrES-1 b, allowing for nonzero eccentricity in the constant-period and orbital decay models. The plot displays 300 random samples from the weighted posterior distributions of the joint model fits. Each data point represents the difference between an observed timing and the midpoint expected from the best-fitting constant-period, eccentric orbit model.
Paper: JWST COMPASS: A NIRSpec G395H Transmission Spectrum of the Super-Earth GJ 357 b
Authors: Jea Adams Redai, Nicholas Wogan, Nicole L. Wallack, Munazza K. Alam, Artyom Aguichine, Angie Wolfgang, Hannah R. Wakeford, Johanna Teske, Nicholas Scarsdale, Sarah E. Moran, Mercedes López-Morales, Annabella Meech, Peter Gao, Anna Gagnebin, Natasha E. Batalha, Natalie M. Batalha, Lili Alderson
Figure caption: The atmospheric compositions ruled out by the Tiberius data set binned at 60 pixels. In all subfigures, the y-axis indicates the pressure at the top of an infinitely opaque layer (i.e., the surface or a cloud deck). Panels on the left consider atmospheres at chemical equilibrium at a given metallicity, while the panels on the right are simple H2O–H2 mixtures. Top panels show the statistical significance with which one can reject the null hypothesis that the difference between the observations and the model are produced purely by chance using a simple χ2 test, and the bottom panels provide the 1σ, 2σ, and 3σ contours of the posterior probability based on Bayesian retrievals. The black region is ruled out to >99.7% confidence (i.e., >3σ). To this high confidence, the JWST observations rule out metallicities < 102.5 × solar (i.e., MMW ≲ 10) for opaque pressure levels ≳ 10−4 bar regardless of the model–data comparison method (left). For H2O–H2 atmospheres (right) with opaque pressure levels ≳ 10−1 bar, the data rule out MMW ≲ 8.
Paper: JWST COMPASS: A NIRSpec G395H Transmission Spectrum of the Super-Earth GJ 357 b
Authors: Jea Adams Redai, Nicholas Wogan, Nicole L. Wallack, Munazza K. Alam, Artyom Aguichine, Angie Wolfgang, Hannah R. Wakeford, Johanna Teske, Nicholas Scarsdale, Sarah E. Moran, Mercedes López-Morales, Annabella Meech, Peter Gao, Anna Gagnebin, Natasha E. Batalha, Natalie M. Batalha, Lili Alderson
Figure caption: Top: Tiberius white light curves for each detector and reduction. Our best-fit models, including systematics, are overplotted on the data in white (NRS1) and black (NRS2). Right column: the residuals from the models. Binned light curves and residuals are also shown. Bottom: same as the top, but for Eureka! reduction.
Paper: JWST COMPASS: A NIRSpec G395H Transmission Spectrum of the Super-Earth GJ 357 b
Authors: Jea Adams Redai, Nicholas Wogan, Nicole L. Wallack, Munazza K. Alam, Artyom Aguichine, Angie Wolfgang, Hannah R. Wakeford, Johanna Teske, Nicholas Scarsdale, Sarah E. Moran, Mercedes López-Morales, Annabella Meech, Peter Gao, Anna Gagnebin, Natasha E. Batalha, Natalie M. Batalha, Lili Alderson
Figure caption: The Tiberius reduction compared to several atmospheric compositions for GJ 357 b. Modeled atmospheres are fit to the the NRS1 and NRS2 data sets independently, as indicated by the vertical gray bar. The 100 × solar metallicity atmosphere is confidently ruled out by the data. All other compositions (1000 × solar metallicity, CH4, CO2, and H2O), are all permitted by the observations to within 1.2σ. The data are also compatible with a bare rock with no atmosphere.
Paper: JWST COMPASS: A NIRSpec G395H Transmission Spectrum of the Super-Earth GJ 357 b
Authors: Jea Adams Redai, Nicholas Wogan, Nicole L. Wallack, Munazza K. Alam, Artyom Aguichine, Angie Wolfgang, Hannah R. Wakeford, Johanna Teske, Nicholas Scarsdale, Sarah E. Moran, Mercedes López-Morales, Annabella Meech, Peter Gao, Anna Gagnebin, Natasha E. Batalha, Natalie M. Batalha, Lili Alderson
Figure caption: Top: comparison of the Tiberius (pale blue) and Eureka! (dark blue) transmission spectra of GJ 357 b in 60 pixel bins. Bottom: difference between the two reductions.
Paper: JWST COMPASS: A NIRSpec G395H Transmission Spectrum of the Super-Earth GJ 357 b
Authors: Jea Adams Redai, Nicholas Wogan, Nicole L. Wallack, Munazza K. Alam, Artyom Aguichine, Angie Wolfgang, Hannah R. Wakeford, Johanna Teske, Nicholas Scarsdale, Sarah E. Moran, Mercedes López-Morales, Annabella Meech, Peter Gao, Anna Gagnebin, Natasha E. Batalha, Natalie M. Batalha, Lili Alderson
Figure caption: Mass–radius diagram for small planets (0.2 ≤ Mp ≤ 30 M⊕) derived from the NASA Exoplanet Archive, with planets shown as points and color coded by composition. The left panel depicts the bulk water mass fraction (A. Aguichine et al. 2021), while the right panel shows the bulk H2–He mass fraction (E. D. Lopez & J. J. Fortney 2014). Solid lines represent theoretical models of planetary composition at an equilibrium temperature of 500 K, including rocky Earth-like compositions from L. Zeng & S. B. Jacobsen (2016). Bold, labeled stars mark other published COMPASS targets. GJ 357 b is highlighted with a larger symbol and label.
Paper: JWST COMPASS: A NIRSpec G395H Transmission Spectrum of the Super-Earth GJ 357 b
Authors: Jea Adams Redai, Nicholas Wogan, Nicole L. Wallack, Munazza K. Alam, Artyom Aguichine, Angie Wolfgang, Hannah R. Wakeford, Johanna Teske, Nicholas Scarsdale, Sarah E. Moran, Mercedes López-Morales, Annabella Meech, Peter Gao, Anna Gagnebin, Natasha E. Batalha, Natalie M. Batalha, Lili Alderson
Figure caption: Predicted dayside thermal emission from GJ 357 b for a bare rock with zero albedo (black line), bare basalt (gray line), a pure CO2 atmosphere with surface pressures of 0.1 and 100 bar (red and blue lines, respectively), and an atmosphere with 0.1 bar CO2 and 10 bar O2 (orange line). The black data point is a synthetic JWST MIRI F1500W measurement for a single secondary eclipse. One F1500W eclipse should be able to distinguish bare basalt from a >0.1 bar CO2 atmosphere to ≳2σ confidence, constituting tentative evidence for or against an atmosphere.
Paper: JWST COMPASS: A NIRSpec G395H Transmission Spectrum of the Super-Earth GJ 357 b
Authors: Jea Adams Redai, Nicholas Wogan, Nicole L. Wallack, Munazza K. Alam, Artyom Aguichine, Angie Wolfgang, Hannah R. Wakeford, Johanna Teske, Nicholas Scarsdale, Sarah E. Moran, Mercedes López-Morales, Annabella Meech, Peter Gao, Anna Gagnebin, Natasha E. Batalha, Natalie M. Batalha, Lili Alderson
Figure caption: Comparison of transit depth precision achieved by each independent reduction (Tiberius in pale blue, Eureka! in dark blue) compared to the predicted values from PandExo simulations.
Paper: NutMaat: A Python Package for Stellar Spectral Classification on the MK System
Authors: R. I. El-Kholy, Z. M. Hayman
Figure caption: The confusion matrix of the main temperature type classification using NutMaat for the merged CFLIB and MILES test sets.
Paper: The Unexplored Dusty Nova LMCN 2009-05a in the Large Magellanic Cloud
Authors: Mohit Singh Bisht, A. Raj, F. M. Walter, Anatoly S. Miroshnichenko, D. Bisht, K. Belwal, Shraddha Biswas
Figure caption: Optical light curves of LMCN 2009-05a from day 3.5 to 3591 generated using optical data from AAVSO and SMARTS. An inset highlights the first 200 days, showing the light curve behavior during the optical minimum, indicating obscuration of optical flux by dust (see Section 3.1 for more details).
Paper: NutMaat: A Python Package for Stellar Spectral Classification on the MK System
Authors: R. I. El-Kholy, Z. M. Hayman
Figure caption: Distribution over main spectral and luminosity classes for the stars from the CFLIB and MILES data bases. The distribution is shown only for those stars that are selected for this study and not for all the spectra in these libraries.
Paper: NutMaat: A Python Package for Stellar Spectral Classification on the MK System
Authors: R. I. El-Kholy, Z. M. Hayman
Figure caption: Cumulative luminosity-class distributions for the human, MKCLASS, and NutMaat types. The number of stars with luminosity classes more luminous than the abscissa is plotted to form the cumulative distribution.
Paper: NutMaat: A Python Package for Stellar Spectral Classification on the MK System
Authors: R. I. El-Kholy, Z. M. Hayman
Figure caption: Histogram showing the difference in luminosity class between NutMaat and the human types, where a difference between luminosity classes of II and III, for example, corresponds to a difference of one.
Paper: NutMaat: A Python Package for Stellar Spectral Classification on the MK System
Authors: R. I. El-Kholy, Z. M. Hayman
Figure caption: NutMaat temperature types for the CFLIB and MILES sets plotted against the published temperature types of F. Valdes et al. (2004) and P. Sanchez-Blazquez et al. (2006a). The size of a circle is proportional to the number of spectra represented by it. A total of 1642 spectra were used to construct this figure.
Paper: The Unexplored Dusty Nova LMCN 2009-05a in the Large Magellanic Cloud
Authors: Mohit Singh Bisht, A. Raj, F. M. Walter, Anatoly S. Miroshnichenko, D. Bisht, K. Belwal, Shraddha Biswas
Figure caption: NIR light curves of LMCN 2009-05a from day 11 to 3591 generated using SMARTS.
Paper: The Unexplored Dusty Nova LMCN 2009-05a in the Large Magellanic Cloud
Authors: Mohit Singh Bisht, A. Raj, F. M. Walter, Anatoly S. Miroshnichenko, D. Bisht, K. Belwal, Shraddha Biswas
Figure caption: Optical color of LMCN 2009-05a from day 11 to 650 generated using SMARTS. The large error bars near day 126 correspond to data obtained under nonphotometric conditions.
Paper: The Unexplored Dusty Nova LMCN 2009-05a in the Large Magellanic Cloud
Authors: Mohit Singh Bisht, A. Raj, F. M. Walter, Anatoly S. Miroshnichenko, D. Bisht, K. Belwal, Shraddha Biswas
Figure caption: Evolution of the Hα line profiles in the nova spectrum from 68 to 93 days after outburst. All profiles are plotted in velocity space, corrected for the LMC velocity (278 km s−1; O. G. Richter et al. 1987). The vertical dashed black line marks the zero velocity. A discrete absorption feature is highlighted by a shaded region, centered at approximately +300 km s−1 and marked by a vertical dashed blue line, corresponding to the disappearance of the redward part of the profile near the onset of the photometric minimum.
Paper: The Unexplored Dusty Nova LMCN 2009-05a in the Large Magellanic Cloud
Authors: Mohit Singh Bisht, A. Raj, F. M. Walter, Anatoly S. Miroshnichenko, D. Bisht, K. Belwal, Shraddha Biswas
Figure caption: Hα and [O I] 6300 Å line profiles with radial velocities corrected for the LMC velocity (278 km s−1 O. G. Richter et al. 1987). The shaded regions mark the location of the reversal feature observed during the nebular phase (more details in Section 3.4).
Paper: The Unexplored Dusty Nova LMCN 2009-05a in the Large Magellanic Cloud
Authors: Mohit Singh Bisht, A. Raj, F. M. Walter, Anatoly S. Miroshnichenko, D. Bisht, K. Belwal, Shraddha Biswas
Figure caption: A mosaic of a 3′ × 3′ square field around LMCN 2009-05a. The source is detected in all 4 WISE bands: W1 (3.4 μm), W2 (4.6 μm), W3 (12 μm), and W4 (22 μm); the emission at W2 and W3 bands is pronounced. The WISE images were obtained from the WISE portal and represent coadded data from observations taken between 2010 January and 2011 January (more details in Section 3.7).
Paper: The Unexplored Dusty Nova LMCN 2009-05a in the Large Magellanic Cloud
Authors: Mohit Singh Bisht, A. Raj, F. M. Walter, Anatoly S. Miroshnichenko, D. Bisht, K. Belwal, Shraddha Biswas
Figure caption: Early spectroscopic evolution of Nova LMCN 2009-05a, obtained from day 8 (2009 May 12) to day 79 (2009 July 23). The spectra prominently feature Fe II multiplets and hydrogen Balmer lines. Identified lines are marked, and the time since discovery (in days) is labeled beside each spectrum.