adsabs/AstroCLIMB huggingface dataset:
Paper: GRB 221009A: Discovery of an Exceptionally Rare Nearby and Energetic Gamma-Ray Burst
Authors: Maia A. Williams, Jamie A. Kennea, S. Dichiara, Kohei Kobayashi, Wataru B. Iwakiri, Andrew P. Beardmore, P. A. Evans, Sebastian Heinz, Amy Lien, S. R. Oates, Hitoshi Negoro, S. Bradley Cenko, Douglas J. K. Buisson, Dieter H. Hartmann, Gaurava K. Jaisawal, N. P. M. Kuin, Stephen Lesage, Kim L. Page, Tyler Parsotan, Dheeraj R. Pasham, B. Sbarufatti, Michael H. Siegel, Satoshi Sugita, George Younes, Elena Ambrosi, Zaven Arzoumanian, M. G. Bernardini, S. Campana, Milvia Capalbi, Regina Caputo, Antonino D'Aì, P. D'Avanzo, V. D'Elia, Massimiliano De Pasquale, R. A. J. Eyles-Ferris, Elizabeth Ferrara, Keith C. Gendreau, Jeffrey D. Gropp, Nobuyuki Kawai, Noel Klingler, Sibasish Laha, A. Melandri, Tatehiro Mihara, Michael Moss, Paul O'Brien, Julian P. Osborne, David M. Palmer, Matteo Perri, Motoko Serino, E. Sonbas, Michael Stamatikos, Rhaana Starling, G. Tagliaferri, Aaron Tohuvavohu, Silvia Zane, Houri Ziaeepour
Figure caption: A comparison of GRB 221009A with all of those observed by XRT. The gray scales indicate the number of GRBs in each (time, brightness) bin; the blue light curve is GRB 221009A, with two notable bright GRBs, GRB 130427A (purple) and GRB 080319B (orange) shown for comparison. Top: observer frame, 0.3–10 keV observed flux light curves. Bottom: comoving-frame, 0.3–10 keV intrinsic (unabsorbed) luminosity light curves; the gray-scale sample data includes only those GRBs with published redshifts.
Paper: GRB 221009A: Discovery of an Exceptionally Rare Nearby and Energetic Gamma-Ray Burst
Authors: Maia A. Williams, Jamie A. Kennea, S. Dichiara, Kohei Kobayashi, Wataru B. Iwakiri, Andrew P. Beardmore, P. A. Evans, Sebastian Heinz, Amy Lien, S. R. Oates, Hitoshi Negoro, S. Bradley Cenko, Douglas J. K. Buisson, Dieter H. Hartmann, Gaurava K. Jaisawal, N. P. M. Kuin, Stephen Lesage, Kim L. Page, Tyler Parsotan, Dheeraj R. Pasham, B. Sbarufatti, Michael H. Siegel, Satoshi Sugita, George Younes, Elena Ambrosi, Zaven Arzoumanian, M. G. Bernardini, S. Campana, Milvia Capalbi, Regina Caputo, Antonino D'Aì, P. D'Avanzo, V. D'Elia, Massimiliano De Pasquale, R. A. J. Eyles-Ferris, Elizabeth Ferrara, Keith C. Gendreau, Jeffrey D. Gropp, Nobuyuki Kawai, Noel Klingler, Sibasish Laha, A. Melandri, Tatehiro Mihara, Michael Moss, Paul O'Brien, Julian P. Osborne, David M. Palmer, Matteo Perri, Motoko Serino, E. Sonbas, Michael Stamatikos, Rhaana Starling, G. Tagliaferri, Aaron Tohuvavohu, Silvia Zane, Houri Ziaeepour
Figure caption: Dust column density (expressed as equivalent hydrogen column density, assuming solar abundances) determined from fitting dust scattering models to the radial intensity profiles as a function of distance, for a standard MRN model. The dependence on the uncertain soft X-ray fluence of GRB 221009A is shown in the y-axis label. Vertical gray lines indicate 1σ error bars.
Paper: GRB 221009A: Discovery of an Exceptionally Rare Nearby and Energetic Gamma-Ray Burst
Authors: Maia A. Williams, Jamie A. Kennea, S. Dichiara, Kohei Kobayashi, Wataru B. Iwakiri, Andrew P. Beardmore, P. A. Evans, Sebastian Heinz, Amy Lien, S. R. Oates, Hitoshi Negoro, S. Bradley Cenko, Douglas J. K. Buisson, Dieter H. Hartmann, Gaurava K. Jaisawal, N. P. M. Kuin, Stephen Lesage, Kim L. Page, Tyler Parsotan, Dheeraj R. Pasham, B. Sbarufatti, Michael H. Siegel, Satoshi Sugita, George Younes, Elena Ambrosi, Zaven Arzoumanian, M. G. Bernardini, S. Campana, Milvia Capalbi, Regina Caputo, Antonino D'Aì, P. D'Avanzo, V. D'Elia, Massimiliano De Pasquale, R. A. J. Eyles-Ferris, Elizabeth Ferrara, Keith C. Gendreau, Jeffrey D. Gropp, Nobuyuki Kawai, Noel Klingler, Sibasish Laha, A. Melandri, Tatehiro Mihara, Michael Moss, Paul O'Brien, Julian P. Osborne, David M. Palmer, Matteo Perri, Motoko Serino, E. Sonbas, Michael Stamatikos, Rhaana Starling, G. Tagliaferri, Aaron Tohuvavohu, Silvia Zane, Houri Ziaeepour
Figure caption: Spectral energy distributions at T 0 + 4.2 ks and T 0 + 43 ks, containing BAT, XRT, and UVOT data. The top panel displays the best-fit unabsorbed broken power-law model (red) together with the data (black) and the data folded with the model (orange). The bottom panel shows the ratio between the data and the model folded through the instrument response.
Paper: GRB 221009A: Discovery of an Exceptionally Rare Nearby and Energetic Gamma-Ray Burst
Authors: Maia A. Williams, Jamie A. Kennea, S. Dichiara, Kohei Kobayashi, Wataru B. Iwakiri, Andrew P. Beardmore, P. A. Evans, Sebastian Heinz, Amy Lien, S. R. Oates, Hitoshi Negoro, S. Bradley Cenko, Douglas J. K. Buisson, Dieter H. Hartmann, Gaurava K. Jaisawal, N. P. M. Kuin, Stephen Lesage, Kim L. Page, Tyler Parsotan, Dheeraj R. Pasham, B. Sbarufatti, Michael H. Siegel, Satoshi Sugita, George Younes, Elena Ambrosi, Zaven Arzoumanian, M. G. Bernardini, S. Campana, Milvia Capalbi, Regina Caputo, Antonino D'Aì, P. D'Avanzo, V. D'Elia, Massimiliano De Pasquale, R. A. J. Eyles-Ferris, Elizabeth Ferrara, Keith C. Gendreau, Jeffrey D. Gropp, Nobuyuki Kawai, Noel Klingler, Sibasish Laha, A. Melandri, Tatehiro Mihara, Michael Moss, Paul O'Brien, Julian P. Osborne, David M. Palmer, Matteo Perri, Motoko Serino, E. Sonbas, Michael Stamatikos, Rhaana Starling, G. Tagliaferri, Aaron Tohuvavohu, Silvia Zane, Houri Ziaeepour
Figure caption: XRT PC-mode 0.8–5.0 keV images from ObsIDs 01126853004 (top left), 01126853006 (top right), 01126853008/09 (bottom left), and 01126853010/11 (bottom right), illustrating the echo expansion with time. The echo event radial positions were scaled by t −0.5 to each observation midtime (given in the upper left corner of each image in days since GBM trigger) to counter the halo expansion within each observation.
Paper: GRB 221009A: Discovery of an Exceptionally Rare Nearby and Energetic Gamma-Ray Burst
Authors: Maia A. Williams, Jamie A. Kennea, S. Dichiara, Kohei Kobayashi, Wataru B. Iwakiri, Andrew P. Beardmore, P. A. Evans, Sebastian Heinz, Amy Lien, S. R. Oates, Hitoshi Negoro, S. Bradley Cenko, Douglas J. K. Buisson, Dieter H. Hartmann, Gaurava K. Jaisawal, N. P. M. Kuin, Stephen Lesage, Kim L. Page, Tyler Parsotan, Dheeraj R. Pasham, B. Sbarufatti, Michael H. Siegel, Satoshi Sugita, George Younes, Elena Ambrosi, Zaven Arzoumanian, M. G. Bernardini, S. Campana, Milvia Capalbi, Regina Caputo, Antonino D'Aì, P. D'Avanzo, V. D'Elia, Massimiliano De Pasquale, R. A. J. Eyles-Ferris, Elizabeth Ferrara, Keith C. Gendreau, Jeffrey D. Gropp, Nobuyuki Kawai, Noel Klingler, Sibasish Laha, A. Melandri, Tatehiro Mihara, Michael Moss, Paul O'Brien, Julian P. Osborne, David M. Palmer, Matteo Perri, Motoko Serino, E. Sonbas, Michael Stamatikos, Rhaana Starling, G. Tagliaferri, Aaron Tohuvavohu, Silvia Zane, Houri Ziaeepour
Figure caption: Upper panel: XRT WT-mode 1D PSF profile from the first snapshot of data at T 0 + 3.4 ks (solid line) and the modeled point-source profile (dashed line). Lower panel: the data minus model residual.
Paper: GRB 221009A: Discovery of an Exceptionally Rare Nearby and Energetic Gamma-Ray Burst
Authors: Maia A. Williams, Jamie A. Kennea, S. Dichiara, Kohei Kobayashi, Wataru B. Iwakiri, Andrew P. Beardmore, P. A. Evans, Sebastian Heinz, Amy Lien, S. R. Oates, Hitoshi Negoro, S. Bradley Cenko, Douglas J. K. Buisson, Dieter H. Hartmann, Gaurava K. Jaisawal, N. P. M. Kuin, Stephen Lesage, Kim L. Page, Tyler Parsotan, Dheeraj R. Pasham, B. Sbarufatti, Michael H. Siegel, Satoshi Sugita, George Younes, Elena Ambrosi, Zaven Arzoumanian, M. G. Bernardini, S. Campana, Milvia Capalbi, Regina Caputo, Antonino D'Aì, P. D'Avanzo, V. D'Elia, Massimiliano De Pasquale, R. A. J. Eyles-Ferris, Elizabeth Ferrara, Keith C. Gendreau, Jeffrey D. Gropp, Nobuyuki Kawai, Noel Klingler, Sibasish Laha, A. Melandri, Tatehiro Mihara, Michael Moss, Paul O'Brien, Julian P. Osborne, David M. Palmer, Matteo Perri, Motoko Serino, E. Sonbas, Michael Stamatikos, Rhaana Starling, G. Tagliaferri, Aaron Tohuvavohu, Silvia Zane, Houri Ziaeepour
Figure caption: XRT WT-mode 1D PSF profiles as a function of time in the 0.8–5.0 keV band, illustrating the evolution of the echo in the early WT data.
Paper: GRB 221009A: Discovery of an Exceptionally Rare Nearby and Energetic Gamma-Ray Burst
Authors: Maia A. Williams, Jamie A. Kennea, S. Dichiara, Kohei Kobayashi, Wataru B. Iwakiri, Andrew P. Beardmore, P. A. Evans, Sebastian Heinz, Amy Lien, S. R. Oates, Hitoshi Negoro, S. Bradley Cenko, Douglas J. K. Buisson, Dieter H. Hartmann, Gaurava K. Jaisawal, N. P. M. Kuin, Stephen Lesage, Kim L. Page, Tyler Parsotan, Dheeraj R. Pasham, B. Sbarufatti, Michael H. Siegel, Satoshi Sugita, George Younes, Elena Ambrosi, Zaven Arzoumanian, M. G. Bernardini, S. Campana, Milvia Capalbi, Regina Caputo, Antonino D'Aì, P. D'Avanzo, V. D'Elia, Massimiliano De Pasquale, R. A. J. Eyles-Ferris, Elizabeth Ferrara, Keith C. Gendreau, Jeffrey D. Gropp, Nobuyuki Kawai, Noel Klingler, Sibasish Laha, A. Melandri, Tatehiro Mihara, Michael Moss, Paul O'Brien, Julian P. Osborne, David M. Palmer, Matteo Perri, Motoko Serino, E. Sonbas, Michael Stamatikos, Rhaana Starling, G. Tagliaferri, Aaron Tohuvavohu, Silvia Zane, Houri Ziaeepour
Figure caption: XRT PC-mode radial intensity profiles in the 0.8–5.0 keV band (blue solid lines); later profiles show stacked observations in indicated time windows, with radii scaled to the beginning of the observing window using Equation (1) so that radial intensity features at the same distance appear at the same radius. Overplotted lines show the PSF and background model (green dashed) and the dust model (orange dashed) and the best-fit model (solid red).
Paper: GRB 221009A: Discovery of an Exceptionally Rare Nearby and Energetic Gamma-Ray Burst
Authors: Maia A. Williams, Jamie A. Kennea, S. Dichiara, Kohei Kobayashi, Wataru B. Iwakiri, Andrew P. Beardmore, P. A. Evans, Sebastian Heinz, Amy Lien, S. R. Oates, Hitoshi Negoro, S. Bradley Cenko, Douglas J. K. Buisson, Dieter H. Hartmann, Gaurava K. Jaisawal, N. P. M. Kuin, Stephen Lesage, Kim L. Page, Tyler Parsotan, Dheeraj R. Pasham, B. Sbarufatti, Michael H. Siegel, Satoshi Sugita, George Younes, Elena Ambrosi, Zaven Arzoumanian, M. G. Bernardini, S. Campana, Milvia Capalbi, Regina Caputo, Antonino D'Aì, P. D'Avanzo, V. D'Elia, Massimiliano De Pasquale, R. A. J. Eyles-Ferris, Elizabeth Ferrara, Keith C. Gendreau, Jeffrey D. Gropp, Nobuyuki Kawai, Noel Klingler, Sibasish Laha, A. Melandri, Tatehiro Mihara, Michael Moss, Paul O'Brien, Julian P. Osborne, David M. Palmer, Matteo Perri, Motoko Serino, E. Sonbas, Michael Stamatikos, Rhaana Starling, G. Tagliaferri, Aaron Tohuvavohu, Silvia Zane, Houri Ziaeepour
Figure caption: GSC spectra at T 0 + 2.5 ks (left panel) and at T 0 + 8.0 ks (right). The blue solid lines show the direct power-law component with Γ free for the spectrum at T 0 + 2.5 ks and fixed at 1.85 at T 0 + 8.0 ks. The light blue dashed lines are the power-law model with Γ = 3.94. The red points and lines are background data and models, respectively. The background model is the sum of two power laws. The best-fit data to the model ratio is also shown in each panel.
Paper: GRB 221009A: Discovery of an Exceptionally Rare Nearby and Energetic Gamma-Ray Burst
Authors: Maia A. Williams, Jamie A. Kennea, S. Dichiara, Kohei Kobayashi, Wataru B. Iwakiri, Andrew P. Beardmore, P. A. Evans, Sebastian Heinz, Amy Lien, S. R. Oates, Hitoshi Negoro, S. Bradley Cenko, Douglas J. K. Buisson, Dieter H. Hartmann, Gaurava K. Jaisawal, N. P. M. Kuin, Stephen Lesage, Kim L. Page, Tyler Parsotan, Dheeraj R. Pasham, B. Sbarufatti, Michael H. Siegel, Satoshi Sugita, George Younes, Elena Ambrosi, Zaven Arzoumanian, M. G. Bernardini, S. Campana, Milvia Capalbi, Regina Caputo, Antonino D'Aì, P. D'Avanzo, V. D'Elia, Massimiliano De Pasquale, R. A. J. Eyles-Ferris, Elizabeth Ferrara, Keith C. Gendreau, Jeffrey D. Gropp, Nobuyuki Kawai, Noel Klingler, Sibasish Laha, A. Melandri, Tatehiro Mihara, Michael Moss, Paul O'Brien, Julian P. Osborne, David M. Palmer, Matteo Perri, Motoko Serino, E. Sonbas, Michael Stamatikos, Rhaana Starling, G. Tagliaferri, Aaron Tohuvavohu, Silvia Zane, Houri Ziaeepour
Figure caption: The extracted PC-mode data designed to mimic the WT-mode extraction to investigate the impact of dust. Left: the source region. Right: the background region. The regions are tilted at the roll angle of the spacecraft.
Paper: GRB 221009A: Discovery of an Exceptionally Rare Nearby and Energetic Gamma-Ray Burst
Authors: Maia A. Williams, Jamie A. Kennea, S. Dichiara, Kohei Kobayashi, Wataru B. Iwakiri, Andrew P. Beardmore, P. A. Evans, Sebastian Heinz, Amy Lien, S. R. Oates, Hitoshi Negoro, S. Bradley Cenko, Douglas J. K. Buisson, Dieter H. Hartmann, Gaurava K. Jaisawal, N. P. M. Kuin, Stephen Lesage, Kim L. Page, Tyler Parsotan, Dheeraj R. Pasham, B. Sbarufatti, Michael H. Siegel, Satoshi Sugita, George Younes, Elena Ambrosi, Zaven Arzoumanian, M. G. Bernardini, S. Campana, Milvia Capalbi, Regina Caputo, Antonino D'Aì, P. D'Avanzo, V. D'Elia, Massimiliano De Pasquale, R. A. J. Eyles-Ferris, Elizabeth Ferrara, Keith C. Gendreau, Jeffrey D. Gropp, Nobuyuki Kawai, Noel Klingler, Sibasish Laha, A. Melandri, Tatehiro Mihara, Michael Moss, Paul O'Brien, Julian P. Osborne, David M. Palmer, Matteo Perri, Motoko Serino, E. Sonbas, Michael Stamatikos, Rhaana Starling, G. Tagliaferri, Aaron Tohuvavohu, Silvia Zane, Houri Ziaeepour
Figure caption: A comparison of a PC-mode spectrum (black), in which dust has been correctly accounted for, and a mimicked WT-mode spectrum (red) of the same data, enabling us to quantify the impact of the dust on the WT-mode data.
Paper: GRB 221009A: Discovery of an Exceptionally Rare Nearby and Energetic Gamma-Ray Burst
Authors: Maia A. Williams, Jamie A. Kennea, S. Dichiara, Kohei Kobayashi, Wataru B. Iwakiri, Andrew P. Beardmore, P. A. Evans, Sebastian Heinz, Amy Lien, S. R. Oates, Hitoshi Negoro, S. Bradley Cenko, Douglas J. K. Buisson, Dieter H. Hartmann, Gaurava K. Jaisawal, N. P. M. Kuin, Stephen Lesage, Kim L. Page, Tyler Parsotan, Dheeraj R. Pasham, B. Sbarufatti, Michael H. Siegel, Satoshi Sugita, George Younes, Elena Ambrosi, Zaven Arzoumanian, M. G. Bernardini, S. Campana, Milvia Capalbi, Regina Caputo, Antonino D'Aì, P. D'Avanzo, V. D'Elia, Massimiliano De Pasquale, R. A. J. Eyles-Ferris, Elizabeth Ferrara, Keith C. Gendreau, Jeffrey D. Gropp, Nobuyuki Kawai, Noel Klingler, Sibasish Laha, A. Melandri, Tatehiro Mihara, Michael Moss, Paul O'Brien, Julian P. Osborne, David M. Palmer, Matteo Perri, Motoko Serino, E. Sonbas, Michael Stamatikos, Rhaana Starling, G. Tagliaferri, Aaron Tohuvavohu, Silvia Zane, Houri Ziaeepour
Figure caption: GSC 2–20 keV images obtained with GSC_5 at T 0 + 2.5 ks (left) and GSC_4 at T 0 + 13.6 ks (right). Source and background regions are shown by the solid lines and the dashed lines, respectively.
Paper: Estimating the Oblateness of Dark Matter Halos Using Neutral Hydrogen Velocity Dispersion
Authors: Mousumi Das, Roger Ianjamasimanana, Stacy S. McGaugh, James Schombert, K. S. Dwarakanath
Figure caption: Left: the halo oblateness parameter q measured at the R (25) radius of a galaxy plotted against gas mass to total disk mass or baryon ratio, where the baryon mass is given as M(baryon) = M(∗)+1.36M(H I)+1.36M(H2), where the 1.36 factor is the correction for the presence of helium. The gas mass is thus M(gas) = 1.36M(H I)+1.36M(H2).
Paper: Estimating the Oblateness of Dark Matter Halos Using Neutral Hydrogen Velocity Dispersion
Authors: Mousumi Das, Roger Ianjamasimanana, Stacy S. McGaugh, James Schombert, K. S. Dwarakanath
Figure caption: The H I velocity dispersion plotted against the radius of the galaxy. The dashed line is the R 25 radius.
Paper: Estimating the Oblateness of Dark Matter Halos Using Neutral Hydrogen Velocity Dispersion
Authors: Mousumi Das, Roger Ianjamasimanana, Stacy S. McGaugh, James Schombert, K. S. Dwarakanath
Figure caption: The halo oblateness parameter q measured at the R 25 (black) and 1.5R 25 radii (red) of the sample galaxies, plotted against stellar mass.
Paper: Estimating the Oblateness of Dark Matter Halos Using Neutral Hydrogen Velocity Dispersion
Authors: Mousumi Das, Roger Ianjamasimanana, Stacy S. McGaugh, James Schombert, K. S. Dwarakanath
Figure caption: The halo oblateness parameter q as measured from the H I velocity dispersion plotted against the radius of the galaxy, for the large galaxies that have stellar masses M(∗) > 109 M ⊙ (first two rows) and for the dwarf galaxies that have stellar masses M(∗) < 109 M ⊙. The dashed line is the R 25 radius.
Paper: A 2:1 Mean-motion Resonance Super-Jovian Pair Revealed by TESS, FEROS, and HARPS 
Authors: Vladimir Bozhilov, Desislava Antonova, Melissa J. Hobson, Rafael Brahm, Andrés Jordán, Thomas Henning, Jan Eberhardt, Felipe I. Rojas, Konstantin Batygin, Pascal Torres-Miranda, Keivan G. Stassun, Sarah C. Millholland, Denitza Stoeva, Milen Minev, Nestor Espinoza, George R. Ricker, David W. Latham, Diana Dragomir, Michelle Kunimoto, Jon M. Jenkins, Eric B. Ting, Sara Seager, Joshua N. Winn, Jesus Noel Villasenor, Luke G. Bouma, Jennifer Medina, Trifon Trifonov
Figure caption: The left panel shows the TPF image of TIC 279401253 for TESS Sector 31. The red pixels indicate the combined aperture used to compute the photometry. The Gaia targets are shown with red circles, whose size is coded by their G magnitude. The right panel shows the TESSERACT 10 minute FFI light curve of TIC 279401253 around the single-transit event recorded in Sector 31. The model curve shows a transit model to the data, and the small bottom panel shows the residuals of the fit.
Paper: A 2:1 Mean-motion Resonance Super-Jovian Pair Revealed by TESS, FEROS, and HARPS 
Authors: Vladimir Bozhilov, Desislava Antonova, Melissa J. Hobson, Rafael Brahm, Andrés Jordán, Thomas Henning, Jan Eberhardt, Felipe I. Rojas, Konstantin Batygin, Pascal Torres-Miranda, Keivan G. Stassun, Sarah C. Millholland, Denitza Stoeva, Milen Minev, Nestor Espinoza, George R. Ricker, David W. Latham, Diana Dragomir, Michelle Kunimoto, Jon M. Jenkins, Eric B. Ting, Sara Seager, Joshua N. Winn, Jesus Noel Villasenor, Luke G. Bouma, Jennifer Medina, Trifon Trifonov
Figure caption: The top main panel shows the Doppler measurements from FEROS (blue) and HARPS (red) and the best two-planet model for these combined data. The left bottom panel shows the PDCSAP 2 minute TESS light curve of TIC 279401253 around the single-transit event recorded in Sector 31. The model curve shows the transit counterpart of the best-fit model applied jointly to the Doppler data obtained with FEROS and HARPS. The middle and right bottom panels show a phase-folded representation of the two planetary signals after the RV signal of the other companion was subtracted. The respective residuals are shown under each panel, accordingly.
Paper: A 2:1 Mean-motion Resonance Super-Jovian Pair Revealed by TESS, FEROS, and HARPS 
Authors: Vladimir Bozhilov, Desislava Antonova, Melissa J. Hobson, Rafael Brahm, Andrés Jordán, Thomas Henning, Jan Eberhardt, Felipe I. Rojas, Konstantin Batygin, Pascal Torres-Miranda, Keivan G. Stassun, Sarah C. Millholland, Denitza Stoeva, Milen Minev, Nestor Espinoza, George R. Ricker, David W. Latham, Diana Dragomir, Michelle Kunimoto, Jon M. Jenkins, Eric B. Ting, Sara Seager, Joshua N. Winn, Jesus Noel Villasenor, Luke G. Bouma, Jennifer Medina, Trifon Trifonov
Figure caption: The MLP power spectrum of the combined FEROS and HARPS Doppler measurements of TIC 279401253. Horizontal lines reflect the ﹩{\rm{\Delta }}\mathrm{ln}L﹩ values, which correspond to 0.1%, 1%, and 10% false alarm probabilities (from top to bottom). Two significant periods are detected: one near 79.4 days and the other near 160.6 days. The bottom panel shows the residuals of our two-planet best-fit model (see Table 2), no significant peaks are observed.
Paper: A 2:1 Mean-motion Resonance Super-Jovian Pair Revealed by TESS, FEROS, and HARPS 
Authors: Vladimir Bozhilov, Desislava Antonova, Melissa J. Hobson, Rafael Brahm, Andrés Jordán, Thomas Henning, Jan Eberhardt, Felipe I. Rojas, Konstantin Batygin, Pascal Torres-Miranda, Keivan G. Stassun, Sarah C. Millholland, Denitza Stoeva, Milen Minev, Nestor Espinoza, George R. Ricker, David W. Latham, Diana Dragomir, Michelle Kunimoto, Jon M. Jenkins, Eric B. Ting, Sara Seager, Joshua N. Winn, Jesus Noel Villasenor, Luke G. Bouma, Jennifer Medina, Trifon Trifonov
Figure caption: Orbital evolution of the TIC 279401253 system for a 500 yr extent for the best-fit solution. The top panels show the evolution of the semimajor axes a b,c, the eccentricities e b,c (blue color indicates the inner, red color the outer planet), and planetary period ratio P rat.. The bottom panels show the evolution of the apsidal alignment argument Δω = ω  c  − ω  b  and the resonance angles θ 1 and θ 2, which librate around 0°, i.e., in a 2:1 MMR. See the text for details.
Paper: A 2:1 Mean-motion Resonance Super-Jovian Pair Revealed by TESS, FEROS, and HARPS 
Authors: Vladimir Bozhilov, Desislava Antonova, Melissa J. Hobson, Rafael Brahm, Andrés Jordán, Thomas Henning, Jan Eberhardt, Felipe I. Rojas, Konstantin Batygin, Pascal Torres-Miranda, Keivan G. Stassun, Sarah C. Millholland, Denitza Stoeva, Milen Minev, Nestor Espinoza, George R. Ricker, David W. Latham, Diana Dragomir, Michelle Kunimoto, Jon M. Jenkins, Eric B. Ting, Sara Seager, Joshua N. Winn, Jesus Noel Villasenor, Luke G. Bouma, Jennifer Medina, Trifon Trifonov
Figure caption: Nested Sampling posteriors the two-planet system TIC 279401253.
Paper: A 2:1 Mean-motion Resonance Super-Jovian Pair Revealed by TESS, FEROS, and HARPS 
Authors: Vladimir Bozhilov, Desislava Antonova, Melissa J. Hobson, Rafael Brahm, Andrés Jordán, Thomas Henning, Jan Eberhardt, Felipe I. Rojas, Konstantin Batygin, Pascal Torres-Miranda, Keivan G. Stassun, Sarah C. Millholland, Denitza Stoeva, Milen Minev, Nestor Espinoza, George R. Ricker, David W. Latham, Diana Dragomir, Michelle Kunimoto, Jon M. Jenkins, Eric B. Ting, Sara Seager, Joshua N. Winn, Jesus Noel Villasenor, Luke G. Bouma, Jennifer Medina, Trifon Trifonov
Figure caption: Mass–radius distribution of exoplanets, color-coded by their estimated mean density. TIC 279401253 b is marked with a triangle, among the densest warm Jovian planets found up-to-date. Assuming that TIC 279401253 c also has a Jupiter-like radius, its position is marked with a diamond-shaped sign.
Paper: The Undiscovered Ultradiffuse Galaxies of the Local Group
Authors: Oliver Newton, Arianna Di Cintio, Salvador Cardona–Barrero, Noam I. Libeskind, Yehuda Hoffman, Alexander Knebe, Jenny G. Sorce, Matthias Steinmetz, Elmo Tempel
Figure caption: The total luminosity functions of field UDGs within 2.5 Mpc of each high-resolution Local Group simulation in the HESTIA suite. Left panel: we estimate the absolute V-band magnitude luminosity functions as a fraction of the total number of UDGs, N UDG,tot, likely to be observed in whole-sky SDSS-, DES-, and LSST-like surveys by applying a limiting surface-brightness cut in the r band when assuming that the stars in each galaxy are individually resolved (SDSS: 29 mag arcsec−2, DES: 30 mag arcsec−2, LSST: 31 mag arcsec−2). With the exception of the SDSS and DES curves in the 09_18 simulation, the luminosity functions of all surveys overlap with the “Total” luminosity function. Right panel: the cumulative number of field UDGs in the simulations as a function of apparent V-band magnitude, m V. The solid and dashed lines show the luminosity functions measured by observers in the Milky Way and M31 analogs, respectively. The vertical arrows indicate the faintest dwarf galaxies that could be detected in several past and future surveys: SDSS (m V = 16), DES (m V = 17.5), HSC (m V = 20), and LSST (m V = 21.5).