adsabs/AstroCLIMB huggingface dataset:
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Images of two RR Lyrae stars, marked with green lines in the images. Upper panels: RV Hor, a star located in a relatively sparse stellar field. Bottom panels: OGLE–LMC–RRLYR–23457, at the outskirts of the LMC. Left panels: a single TESS cadence from Sector 1. Middle panels: a single differential frame. The images of RV Hor are affected by reflections from the stripes of CCD electronics but otherwise almost entirely clean. The LMC image shows many residuals after image subtraction but the variable is clearly visible in the center. Right panels: corresponding DSS images. All images are oriented to celestial directions (north is up; east is to the left). The TESS cutouts are 64 × 64 px or 22.′4 × 22.′4 large.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Left: period–luminosity relation of the sample. Brightness is in M  G  (top) and M  K  (bottom) absolute magnitudes. RRab and RRc stars are represented with blue diamonds and red dots, respectively. For RRd stars (black empty rectangles) we marked both periods. The two anomalous Cepheid (ACEP) candidates are marked with empty circles. Stars with erroneous extinction correction are marked with black crosses. Right: distribution of the sample in the absolute Gaia and J–K (bottom) color–magnitude planes: here we marked the blue and red edges of the instability strip, as calculated by Marconi et al. (2015), with the blue and red solid lines. Differences between the two extinction corrections are indicated with dashed lines for the three LMC foreground stars.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Main: the Gaia EDR3 M  G  absolute magnitudes and distances of the sample, color-coded with the A  G  absorption coefficients calculated with MWDUST. The diagonal line and light-gray area below it mark the approximate brightness cut of the sample. Large crosses mark eclipsing stars that we were able to classify based on light-curve shapes. The large pluses at the bottom are two stars where the light-curve shape was not decisive but their positions clearly rule them out. Different extinction corrections for the three LMC foreground stars are connected with the dashed lines. Insert: map of the targets with and the A  G  absorption coefficients in the EDR3 G band. The position of the Magellanic Clouds is marked with the arrow.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Relative Fourier parameters R  i1 and ϕ  i1 of the TESS first light sample (large symbols), overlaid on the OGLE I-band values (dots). Orange and purple points mark RRc and RRab stars. The two empty circles are the ACEP candidates; the three black crosses in the RRab group are the three LMC foreground stars. The two red crosses in the RRc group are two false-positive, non-pulsating stars.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Comparison of the FITSH differential-imaging aperture photometry (left row) with the ELEANOR photometries. Center: PSF fitting. Right: raw (gray) and corrected (black) pixel aperture photometry. From top to bottom, three relatively bright stars from each subclass (RRab, RRc, RRd) and a faint RR Lyrae star, SX Dor, from a crowded region near the Large Magellanic Cloud (LMC). Plots are on the same scale in each row.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Toomre diagram of 42 stars from our sample. Black dots are halo RR Lyrae stars; blue squares are variables that may be members of Gaia–Enceladus structure according to Prudil et al. (2020). Dashed lines mark constant total space velocities while green lines show the approximate thin–thick disk and disk–halo boundaries. The red crosses are two non-pulsating stars we identify in Section 3.2.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Comparison of the pulsation periods we derived from the TESS light curves and those calculated from the Gaia DR2 epoch photometry (gray) or present in VSX (red). Stars where two periods were identified only by either TESS or Gaia are connected with lines. The lower panel shows the difference values. Uncertainties are smaller than the symbols.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Five examples of modulated RRab stars. Upper row: light curves. Bottom row: loop diagrams of the A 1 and ϕ 1 Fourier terms. Arrows mark the direction of progression, where applicable, and color follows progression in time.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Same as Figure 9 but for modulated RRc stars.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Relative Fourier parameters of the two ACEP candidates, compared to the OGLE ACEP samples (Soszyński et al. 2015, 2020).
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Top: period distribution of individual RRab stars in which additional modes were detected: OGLE (gray), CoRoT/Kepler/K2 (orange), and TESS (red). Bottom: Petersen diagram for the RRab stars. Gray crosses are the OGLE bulge results, orange diamonds are from CoRoT, Kepler, and the K2-E2 engineering test run, and red points are the TESS observations. Small gray dots mark the distribution of the RRd stars and thus the position of the first overtone. The dashed line indicates the position of the half-integer frequency indicating period doubling. Large red crosses mark the ACEP candidate SX PsA. Note that stars may have multiple additional signals detected in them.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Same as Figure 12 but for the f X modes in RRc and RRd stars. Top: period distribution for OGLE (gray), TESS (red), and from two globular clusters, M3 (blue) and NGC 6362 (green). The light red extensions mark the TESS RRc stars where the modes are absent. Bottom: Petersen diagram of the f X or 0.61 type modes. Gray points are the OGLE detections by Netzel & Smolec (2019), orange diamonds are various stars collected by Moskalik et al. (2015) that include other space-based data, blue squares are the M3 stars by Jurcsik et al. (2015), green circles are the NGC 6362 stars (Smolec et al. 2017), and filled and empty red circles are the TESS RRc and RRd detections.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Amplitudes of the independent frequency components we found (bottom) and their ratios compared to the amplitude of the strongest frequency peak (top). The gray band is between 10–25 mmag and A/A 0 = 0.10–0.25, respectively. Black small circles are additional components in RRab stars; blue diamonds are additional components in RRc stars; red full and empty circles are the ratios between the main peaks of the two radial modes and the additional peaks and the strongest peak in RRd stars, respectively.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Distribution of the stars with additional modes within the RR Lyrae instability strip. Left: the f  X  and f 0.68 modes in RRc and RRd stars. Center: the f 1-type modes in RRab stars. Right: the f 2 and PD or other type of modes in RRab stars. Two stars marked (XX Dor and T Men) had their interstellar extinction values overestimated and hence appear too blue and too bright. The third star, BV Aqr, is the extreme RRd candidate.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Fourier spectra (left) and échelle diagrams (right) of selected RRab stars. In the frequency spectra, pulsation and modulation peaks that have been removed are marked with red lines. In the échelle diagrams, the locations of these peaks are marked with black dots. Black crosses mark the locations of those pulsation harmonics that are reflected back from the Nyquist frequency.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Petersen diagram of the five RRd stars we analyzed (red). Black dots are various field RRd stars, gray ones are OGLE stars from the bulge and the Magellanic Clouds. Sources are the same as the RRd stars collected in Molnár et al. (2015b). Crosses are anomalous RRd stars found in the Clouds (Soszyński et al. 2016).
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: CZ Ind, an RRab star with a strong extra mode. Top row, from left to right: original light curve, frequency spectrum in red, with the prewhitened FM frequency components in blue, and échelle diagram. Bottom row: disentangled light curves of the fundamental mode (blue) and the extra mode (red), and only the disentangled extra mode, as seen in each of the two orbits during the sector.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: The 0.68-type modes: small black circles are the OGLE stars from Netzel & Smolec (2019); large red circles are the TESS detections.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Non-Blazhko RRab stars. Left: residual spectra with the positions of the pulsation peak and its harmonics (red dashed lines) and the 4.0 S/N level (blue line) marked. Right: folded light curves.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: The comparison of the TESS Sector 2 30 minute and 2 minute cadence data to various observations taken from the ground. Light curves (upper left panel), spectral windows (upper right panel), frequency spectra (lower left panel), and the modulation side peaks around the pulsation frequency (lower right panel) in the different data sets of RU Scl are plotted, respectively.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: A bright δ Scuti contaminating an RR Lyrae star. Top row: the light-curve and Fourier spectrum of SU Hyi. Dashed lines mark the harmonic series of the pulsation peak that has been removed for clarity. The contamination appears as an extra set of peaks between 6–9 days−1. Bottom row: light-curve and Fourier spectrum of the nearby bright star HD 10925. The frequency content matches the distribution of excess peaks in the spectrum of SU Hyi.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Comparison of lower-order Fourier parameters of TESS light curves (filled triangles) with RR Lyrae pulsation models (open squares) from Marconi et al. (2015) in I band. The color bar represents different stellar masses for RR Lyrae models.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Two faint targets from Sector 2. Left: light curves, Right: phase-folded curves. Red dashed lines indicate flux excesses from asteroids crossing the photometric aperture.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Ground-based observations of BO Gru, the strongly modulated RRc star. Top row: the entire light curve. Bottom row: phase curves, folded both with the pulsation and with the modulation periods. Colors follow time of the observations.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Positions of the RR Lyrae targets in the sky. The blue line is the Galactic plane. Blue dots are single-sector targets, red dots were observed in both S1 and S2. Sizes correspond to brightness.
Paper: First Results on RR Lyrae Stars with the TESS Space Telescope: Untangling the Connections between Mode Content, Colors, and Distances
Authors: L. Molnár, A. Bódi, A. Pál, A. Bhardwaj, F–J. Hambsch, J. M. Benkő, A. Derekas, M. Ebadi, M. Joyce, A. Hasanzadeh, K. Kolenberg, M. B. Lund, J. M. Nemec, H. Netzel, C. –C. Ngeow, J. Pepper, E. Plachy, Z. Prudil, R. J. Siverd, M. Skarka, R. Smolec, Á. Sódor, S. Sylla, P. Szabó, R. Szabó, H. Kjeldsen, J. Christensen-Dalsgaard, G. R. Ricker
Figure caption: Comparison of the TESS (top panels) and OGLE (bottom panels) light curves for the shared targets. Color scale shows progression of time, going from orange to purple.
Paper: A Fresh Look at AGB Stars in Galactic Open Clusters with Gaia: Impact on Stellar Models and the Initial–Final Mass Relation
Authors: Paola Marigo, Diego Bossini, Michele Trabucchi, Francesco Addari, Léo Girardi, Jeffrey D. Cummings, Giada Pastorelli, Piero Dal Tio, Guglielmo Costa, Alessandro Bressan
Figure caption: Luminosities and core masses of TP-AGB stars in open clusters as a function of the initial stellar mass. The M, S, and C stars (reported in the legend) are marked with colored symbols and error bars. For comparison we overplot the luminosity and core mass at the first thermal pulse, L 1TP and M  c  ,1TP, predicted by the PARSEC stellar models at solar metallicity (dashed lines). The cluster ages and visual extinctions are taken from the work of Cantat-Gaudin et al. (2020). Moving downward, the panels show the results for three prescriptions of the Gaia EDR3 parallax zero-point (ZP): no ZP correction (top), Lindegren et al. (2021a; middle), and Groenewegen (2021; bottom). Note that the X-axis is stretched over the range ﹩0.8\leqslant {M}_{i}^{\mathrm{AGB}}/{M}_{\odot }\leqslant 4.0﹩. Left panels: bolometric luminosities derived from the fitting of the SEDs. Right panels: the IFMR of white dwarfs in the Milky Way is compared to the current core masses of TP-AGB stars in open clusters. The semiempirical IFMR (gray diamonds with error bars) is taken from Marigo et al. (2020) and Cummings et al. (2018). The solid line is a fit to the IFMR data.