adsabs/AstroCLIMB huggingface dataset:
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. I. Observations, Orbital and Physical Properties, and Exozodi Upper Limits
Authors: Charles Beichman, Aniket Sanghi, Dimitri Mawet, Pierre Kervella, Kevin Wagner, Billy Quarles, Jack J. Lissauer, Max Sommer, Mark Wyatt, Nicolas Godoy, William O. Balmer, Laurent Pueyo, Jorge Llop-Sayson, Jonathan Aguilar, Rachel Akeson, Ruslan Belikov, Anthony Boccaletti, Elodie Choquet, Edward Fomalont, Thomas Henning, Dean Hines, Renyu Hu, Pierre-Olivier Lagage, Jarron Leisenring, James Mang, Michael Ressler, Eugene Serabyn, Pascal Tremblin, Marie Ygouf, Mantas Zilinskas
Figure caption: The change in the position of α Cen A relative to 2024 January 1 (Δα = 0, Δδ = 0) computed using proper motion and parallax as seen from JWST’s L2 vantage point. Markers denote 10 day intervals and days of the year. As a reference, the red star denotes the date of the 2024 August JWST observations (first epoch). The inset plot zooms in near the 2024 August observation date with markers spaced in 5 day intervals. Details of the astrometry for α Cen are given in Appendix B and in R. Akeson et al. (2021).
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. I. Observations, Orbital and Physical Properties, and Exozodi Upper Limits
Authors: Charles Beichman, Aniket Sanghi, Dimitri Mawet, Pierre Kervella, Kevin Wagner, Billy Quarles, Jack J. Lissauer, Max Sommer, Mark Wyatt, Nicolas Godoy, William O. Balmer, Laurent Pueyo, Jorge Llop-Sayson, Jonathan Aguilar, Rachel Akeson, Ruslan Belikov, Anthony Boccaletti, Elodie Choquet, Edward Fomalont, Thomas Henning, Dean Hines, Renyu Hu, Pierre-Olivier Lagage, Jarron Leisenring, James Mang, Michael Ressler, Eugene Serabyn, Pascal Tremblin, Marie Ygouf, Mantas Zilinskas
Figure caption: Range of minimum mutual inclination imut experienced by the prograde (a) and retrograde (b) planet in the inner orbit (a < 2 au family). Orbits colored yellow represent the imut range within the vZKL regime that would produce large amplitude oscillations, while blue denotes imut values that would have much lower oscillations.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. I. Observations, Orbital and Physical Properties, and Exozodi Upper Limits
Authors: Charles Beichman, Aniket Sanghi, Dimitri Mawet, Pierre Kervella, Kevin Wagner, Billy Quarles, Jack J. Lissauer, Max Sommer, Mark Wyatt, Nicolas Godoy, William O. Balmer, Laurent Pueyo, Jorge Llop-Sayson, Jonathan Aguilar, Rachel Akeson, Ruslan Belikov, Anthony Boccaletti, Elodie Choquet, Edward Fomalont, Thomas Henning, Dean Hines, Renyu Hu, Pierre-Olivier Lagage, Jarron Leisenring, James Mang, Michael Ressler, Eugene Serabyn, Pascal Tremblin, Marie Ygouf, Mantas Zilinskas
Figure caption: Observed masses and radii derived from transit observations for planets cooler than 750 K (from the Planets Catalog; S. Müller et al. 2024) are shown along with the properties of the S1 + C1 planet candidate inferred from the different models. The shaded area shows the approximate range of RV upper limits, depending on the exact inclination of the candidate’s orbit. The positions of Saturn and Jupiter are included.
Paper: CECILIA: Ultradeep Rest-optical Spectra of Faint Galaxies at Cosmic Noon
Authors: Menelaos Raptis, Ryan F. Trainor, Allison L. Strom, Gwen C. Rudie, Noah S. J. Rogers, Charles C. Steidel, Michael V. Maseda, Caroline von Raesfeld, Nathalie A. Korhonen Cuestas
Figure caption: N2 (left) and S2-BPT (right) diagrams. Our data points are compared to 11 galaxies at z ∼ 2–6 from R. L. Sanders et al. (2024; diamonds) and the stacked points from F. Bian et al. (2018; stars), both color-coded by their direct metallicities, as indicated by the color bar on the right. The F. Bian et al. (2018) sample was selected on the basis of N2-BPT line ratios, with the gray shading denoting the selection region. In the N2-BPT diagram, the stacked point from T16 and D40 from R24 (black and purple outlines, respectively) are shown as circles with the same O/H-based central color coding.
Paper: CECILIA: Ultradeep Rest-optical Spectra of Faint Galaxies at Cosmic Noon
Authors: Menelaos Raptis, Ryan F. Trainor, Allison L. Strom, Gwen C. Rudie, Noah S. J. Rogers, Charles C. Steidel, Michael V. Maseda, Caroline von Raesfeld, Nathalie A. Korhonen Cuestas
Figure caption: The rest-frame NIRSpec spectrum of the serendipitous source Q2343-C31b. Top: 2D spectrogram of the source, with the emission lines marked by red vertical lines and the two white dashed lines indicating the centers of the main and serendipitous sources. Adjacent to the spectrogram, the panel shows the 1D spatial distribution of the continuum for the main source in blue (with the blue dashed line marking the center of the main source). Additionally, the 1D spatial distribution of the brightest emission lines from the serendipitous source is shown in red (with the red dashed line marking the center of the serendipitous source). Middle: full spectral range of the G235M spectrum for the source. Black dashed vertical lines and shaded bands indicate the positions of key spectral features—most of which are shown in the bottom panels—and emission lines with >2σ detections. The 1D extracted spectrum is shown in purple. Bottom: zoom-in panels of key spectral features. The Gaussian+linear continuum fit to the emission lines is shown in light blue, and the error region is shown in gray.
Paper: CECILIA: Ultradeep Rest-optical Spectra of Faint Galaxies at Cosmic Noon
Authors: Menelaos Raptis, Ryan F. Trainor, Allison L. Strom, Gwen C. Rudie, Noah S. J. Rogers, Charles C. Steidel, Michael V. Maseda, Caroline von Raesfeld, Nathalie A. Korhonen Cuestas
Figure caption: The N2-BPT predictions from the Cloudy photoionization models are shown, using input spectra from BPASS stellar populations. The pink lines represent tracks of fixed ﹩{\mathrm{log}}\,U﹩, where higher ﹩{\mathrm{log}}\,U﹩ values result in higher O3 ratios. The model points are color-coded by O/H as indicated by the color bar. We overplot the CECILIA NB sample (pink points), fLBG sources (pink squares), and SDSS z ∼ 0 galaxies (gray contours).
Paper: CECILIA: Ultradeep Rest-optical Spectra of Faint Galaxies at Cosmic Noon
Authors: Menelaos Raptis, Ryan F. Trainor, Allison L. Strom, Gwen C. Rudie, Noah S. J. Rogers, Charles C. Steidel, Michael V. Maseda, Caroline von Raesfeld, Nathalie A. Korhonen Cuestas
Figure caption: O1-BPT (S. Veilleux & D. E. Osterbrock 1987) showing SDSS z ∼ 0 galaxies (gray contour lines), CECILIA faint LAEs (pink circles with 2σ limits), CECILIA faint LBGs (pink squares), CECILIA D40 (purple circle), Lyman-break galaxies from A. J. Cameron et al. (2023; green diamonds), and SF galaxies at z ∼ 2.5 (orange squares; stacked point with black outline) from L. Clarke et al. (2023). The solid black line represents the theoretical starburst classification curve from L. J. Kewley et al. (2001), separating SF galaxies from objects with other ionization mechanisms.
Paper: CECILIA: Ultradeep Rest-optical Spectra of Faint Galaxies at Cosmic Noon
Authors: Menelaos Raptis, Ryan F. Trainor, Allison L. Strom, Gwen C. Rudie, Noah S. J. Rogers, Charles C. Steidel, Michael V. Maseda, Caroline von Raesfeld, Nathalie A. Korhonen Cuestas
Figure caption: N2-BPT diagram with the same features as Figure 6 but excluding all stacked points and galaxies without reported Lyα EWs. CECILIA faint sources are shown as circles for NB detections and squares for fLGBs. The T16 stack point is plotted as a circle with a black outline. All points are color-coded by their Lyα EWs.
Paper: CECILIA: Ultradeep Rest-optical Spectra of Faint Galaxies at Cosmic Noon
Authors: Menelaos Raptis, Ryan F. Trainor, Allison L. Strom, Gwen C. Rudie, Noah S. J. Rogers, Charles C. Steidel, Michael V. Maseda, Caroline von Raesfeld, Nathalie A. Korhonen Cuestas
Figure caption: The rest-frame NIRSpec spectrum of the serendipitous source Q2343-BX587b.
Paper: Galactic Superaccreting X-Ray Binaries as Super-PeVatron Accelerators
Authors: Jieshuang Wang, 界双 王, Brian Reville, Felix A. Aharonian
Figure caption: Illustration indicating the key features in the XRB nebula and halo (not to scale). The nebula is inflated by the jet/wind. The CR halo is produced by escaping CRs interacting with the ISM. The jet may be collimated by the ambient medium. Close to the binary, the jet profile can be parabolic or conical. Further away from the binary, it can be quasi-cylindrical.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. I. Observations, Orbital and Physical Properties, and Exozodi Upper Limits
Authors: Charles Beichman, Aniket Sanghi, Dimitri Mawet, Pierre Kervella, Kevin Wagner, Billy Quarles, Jack J. Lissauer, Max Sommer, Mark Wyatt, Nicolas Godoy, William O. Balmer, Laurent Pueyo, Jorge Llop-Sayson, Jonathan Aguilar, Rachel Akeson, Ruslan Belikov, Anthony Boccaletti, Elodie Choquet, Edward Fomalont, Thomas Henning, Dean Hines, Renyu Hu, Pierre-Olivier Lagage, Jarron Leisenring, James Mang, Michael Ressler, Eugene Serabyn, Pascal Tremblin, Marie Ygouf, Mantas Zilinskas
Figure caption: JWST’s view of the α Cen AB system. Shown above is a background-subtracted Stage 2b F1550C image of the α Cen AB system from 2024 August. The image is oriented north up and east left. The white stars denote the approximate positions of α Cen B, saturated near the top of the image, and α Cen A in the lower part of the image hidden behind the F1550C mask. The right color bar (logarithmically scaled) is associated with this image. At the edge of the detector, to the west of α Cen A, is the known background source KS5 (P. Kervella et al. 2016). To the east of α Cen A is the known background source KS2 (P. Kervella et al. 2016), shown as an inset, as it is only detected after performing PSF subtraction (no color bar shown for the inset, scaled linearly between −5 and 50 MJy sr−1). An ≈2﹩\mathop{.}\limits^{^{\prime\prime} }﹩75 radius region around α Cen A is shaded and mapped to three PSF-subtracted images, one for each observation epoch. Candidate S1 is seen only in 2024 August. The bottom color bar (linearly scaled) is associated with the three PSF-subtracted images. For reference, 1 MJy sr−1 ≈ 4.6 × 10−6 Jy AiryCore–1, where AiryCore is defined as the area of a circular aperture of diameter = 1 FWHM (﹩\approx 0\mathop{.}\limits^{^{\prime\prime} }5﹩).
Paper: Galactic Superaccreting X-Ray Binaries as Super-PeVatron Accelerators
Authors: Jieshuang Wang, 界双 王, Brian Reville, Felix A. Aharonian
Figure caption: The maximum rigidity of Equation (1) for YSCs, SNe, and SNRs, pulsar wind nebulae (exemplified by Crab Nebula), the GC, and superaccreting XRBs. The corresponding kinetic power, magnetization, and velocity for this plot are summarized in Table 1. We assume ﹩\tilde{\omega }=4﹩ for the background shading area with different values of σ. For microquasar jets, the maximum energy can be higher than the shaded area because of ﹩\tilde{\omega }=1﹩.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. I. Observations, Orbital and Physical Properties, and Exozodi Upper Limits
Authors: Charles Beichman, Aniket Sanghi, Dimitri Mawet, Pierre Kervella, Kevin Wagner, Billy Quarles, Jack J. Lissauer, Max Sommer, Mark Wyatt, Nicolas Godoy, William O. Balmer, Laurent Pueyo, Jorge Llop-Sayson, Jonathan Aguilar, Rachel Akeson, Ruslan Belikov, Anthony Boccaletti, Elodie Choquet, Edward Fomalont, Thomas Henning, Dean Hines, Renyu Hu, Pierre-Olivier Lagage, Jarron Leisenring, James Mang, Michael Ressler, Eugene Serabyn, Pascal Tremblin, Marie Ygouf, Mantas Zilinskas
Figure caption: Left: F1000W image of α Cen AB showing Gaia stars (green boxes) and MIRI detections (red boxes). The stars labeled G0 and G5 were used for TA of α Cen A. Right: similar F1000W image for ϵ Mus. The star labeled G9 was used for TA of ϵ Mus.
Paper: Worlds Next Door: A Candidate Giant Planet Imaged in the Habitable Zone of α Centauri A. I. Observations, Orbital and Physical Properties, and Exozodi Upper Limits
Authors: Charles Beichman, Aniket Sanghi, Dimitri Mawet, Pierre Kervella, Kevin Wagner, Billy Quarles, Jack J. Lissauer, Max Sommer, Mark Wyatt, Nicolas Godoy, William O. Balmer, Laurent Pueyo, Jorge Llop-Sayson, Jonathan Aguilar, Rachel Akeson, Ruslan Belikov, Anthony Boccaletti, Elodie Choquet, Edward Fomalont, Thomas Henning, Dean Hines, Renyu Hu, Pierre-Olivier Lagage, Jarron Leisenring, James Mang, Michael Ressler, Eugene Serabyn, Pascal Tremblin, Marie Ygouf, Mantas Zilinskas
Figure caption: PSF-subtracted image centered on α Cen A for the 2025 April observations, which provides the longest temporal baseline to test the stationary background source hypothesis. A square marks the location where S1 was detected in the 2024 August epoch. A cross marks the expected location of S1 if it were a fixed background object and showed apparent motion with respect to α Cen A due to the star’s parallactic and proper motion. No source is detected at this location.
Paper: An Eccentric Sub-Neptune Moving Into the Evaporation Desert 
Authors: Sydney A. Jenkins, Andrew Vanderburg, Ritika Sethi, Sarah Millholland, Joseph E. Rodriguez, Luca Fossati, Andreas Krenn, Emily Pass, Alexander Venner, R. Paul Butler, Hugh Osborn, Aaron Householder, Carl Ziegler, Juliette Becker, Perry Berlind, Allyson Bieryla, Christopher Broeg, Michael L. Calkins, Jeffrey D. Crane, Tansu Daylan, Julien de Wit, Jason D. Eastman, David Ehrenreich, Gilbert A. Esquerdo, Michael Fausnaugh, Yadira Gaibor, David W. Latham, Monika Lendl, Andrew W. Mayo, Gaetano Scandariato, Steve Shectman, Stephanie Striegel, Johanna Teske, Thomas G Wilson
Figure caption: Left: eccentricity and semimajor axis in units of stellar radii for all confirmed planets between 1.9 and 4.0 R⊕ listed on the NASA Exoplanet Archive. TOI-5800 b’s e and a/R⋆ values are indicated by purple and orange lines, respectively. 1σ uncertainties are indicated by the shaded regions. Right: transmission spectroscopy metric (TSM) values and effective temperatures for all confirmed planets between 1.9 and 4.0 R⊕ with available measurements. Because of its eccentric orbit, the planet may experience a range of temperatures. Using revised values for the radius and mass of the planet, we show the range of equilibrium temperatures and TSM values between apocenter and pericenter in purple. Additionally, the planet is likely experiencing tidal heating. We show the resulting range in orange, assuming ﹩{Q}_{p}^{{\prime} }\,=\,1{0}^{4}﹩ (S. Millholland et al. 2020).
Paper: An Eccentric Sub-Neptune Moving Into the Evaporation Desert 
Authors: Sydney A. Jenkins, Andrew Vanderburg, Ritika Sethi, Sarah Millholland, Joseph E. Rodriguez, Luca Fossati, Andreas Krenn, Emily Pass, Alexander Venner, R. Paul Butler, Hugh Osborn, Aaron Householder, Carl Ziegler, Juliette Becker, Perry Berlind, Allyson Bieryla, Christopher Broeg, Michael L. Calkins, Jeffrey D. Crane, Tansu Daylan, Julien de Wit, Jason D. Eastman, David Ehrenreich, Gilbert A. Esquerdo, Michael Fausnaugh, Yadira Gaibor, David W. Latham, Monika Lendl, Andrew W. Mayo, Gaetano Scandariato, Steve Shectman, Stephanie Striegel, Johanna Teske, Thomas G Wilson
Figure caption: Mass–radius diagram with known sub-Neptunes and super-Earths. We include planets from the NASA Exoplanet Archive (accessed 2025 April 3) that have masses constrained within 20%. Theoretical models for a variety of interior compositions (L. Zeng et al. 2016) and for a cold H2 world (S. Seager et al. 2007) are shown as colored lines. Models for Earth-like cores with H2 atmospheres are shown in light purple (L. Zeng et al. 2019). Solar system planets are shown in orange.
Paper: An Eccentric Sub-Neptune Moving Into the Evaporation Desert 
Authors: Sydney A. Jenkins, Andrew Vanderburg, Ritika Sethi, Sarah Millholland, Joseph E. Rodriguez, Luca Fossati, Andreas Krenn, Emily Pass, Alexander Venner, R. Paul Butler, Hugh Osborn, Aaron Householder, Carl Ziegler, Juliette Becker, Perry Berlind, Allyson Bieryla, Christopher Broeg, Michael L. Calkins, Jeffrey D. Crane, Tansu Daylan, Julien de Wit, Jason D. Eastman, David Ehrenreich, Gilbert A. Esquerdo, Michael Fausnaugh, Yadira Gaibor, David W. Latham, Monika Lendl, Andrew W. Mayo, Gaetano Scandariato, Steve Shectman, Stephanie Striegel, Johanna Teske, Thomas G Wilson
Figure caption: Archival imaging of TOI-5800. From left to right, images are from Palomar Observatory Sky Survey (G. O. Abell 1955), the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS; K. C. Chambers et al. 2016) survey in the y band, the Pan-STARRS survey in the i band, and coadded TESS images from Sector 54. In all images, we show the current position of TOI-5800 with a red cross. The photometric apertures for Sectors 54 and 81 are shown in red and purple, respectively. In the rightmost image, nearby stars within 6 mag (Gaia Collaboration et al. 2016, 2023) of TOI-5800 are shown as red points.
Paper: An Eccentric Sub-Neptune Moving Into the Evaporation Desert 
Authors: Sydney A. Jenkins, Andrew Vanderburg, Ritika Sethi, Sarah Millholland, Joseph E. Rodriguez, Luca Fossati, Andreas Krenn, Emily Pass, Alexander Venner, R. Paul Butler, Hugh Osborn, Aaron Householder, Carl Ziegler, Juliette Becker, Perry Berlind, Allyson Bieryla, Christopher Broeg, Michael L. Calkins, Jeffrey D. Crane, Tansu Daylan, Julien de Wit, Jason D. Eastman, David Ehrenreich, Gilbert A. Esquerdo, Michael Fausnaugh, Yadira Gaibor, David W. Latham, Monika Lendl, Andrew W. Mayo, Gaetano Scandariato, Steve Shectman, Stephanie Striegel, Johanna Teske, Thomas G Wilson
Figure caption: Left: radius and semimajor axis of planets listed in the NASA Exoplanet Archive. The Neptune desert is demarked by the black dashed lines (T. Mazeh et al. 2016). We also include updated boundaries from A. Castro-González et al. (2024), denoted by the black dotted lines. TOI-5800 b is shown in orange. We expect the planet to circularize to a closer-in orbit, indicated by the black arrow. Right: semimajor axis of TOI-5800 b as a function of time. Models for different values of Q⋆ and Qp are shown in orange and purple, respectively. Assuming Q⋆ = 8.0 and Qp = 5.5, we estimate a final semimajor axis of ∼0.03 au.
Paper: An Eccentric Sub-Neptune Moving Into the Evaporation Desert 
Authors: Sydney A. Jenkins, Andrew Vanderburg, Ritika Sethi, Sarah Millholland, Joseph E. Rodriguez, Luca Fossati, Andreas Krenn, Emily Pass, Alexander Venner, R. Paul Butler, Hugh Osborn, Aaron Householder, Carl Ziegler, Juliette Becker, Perry Berlind, Allyson Bieryla, Christopher Broeg, Michael L. Calkins, Jeffrey D. Crane, Tansu Daylan, Julien de Wit, Jason D. Eastman, David Ehrenreich, Gilbert A. Esquerdo, Michael Fausnaugh, Yadira Gaibor, David W. Latham, Monika Lendl, Andrew W. Mayo, Gaetano Scandariato, Steve Shectman, Stephanie Striegel, Johanna Teske, Thomas G Wilson
Figure caption: RV data from PFS (see Section 2.1), shown in black. The best-fit model (see Section 4) is shown in dark purple, and 100 draws from the posterior distribution are shown in light purple. Left: phase-folded data and model with quadratic component subtracted. Right: quadratic fit. We find tentative evidence for a quadratic trend in the RV data, potential evidence of an outer planetary companion.
Paper: An Eccentric Sub-Neptune Moving Into the Evaporation Desert 
Authors: Sydney A. Jenkins, Andrew Vanderburg, Ritika Sethi, Sarah Millholland, Joseph E. Rodriguez, Luca Fossati, Andreas Krenn, Emily Pass, Alexander Venner, R. Paul Butler, Hugh Osborn, Aaron Householder, Carl Ziegler, Juliette Becker, Perry Berlind, Allyson Bieryla, Christopher Broeg, Michael L. Calkins, Jeffrey D. Crane, Tansu Daylan, Julien de Wit, Jason D. Eastman, David Ehrenreich, Gilbert A. Esquerdo, Michael Fausnaugh, Yadira Gaibor, David W. Latham, Monika Lendl, Andrew W. Mayo, Gaetano Scandariato, Steve Shectman, Stephanie Striegel, Johanna Teske, Thomas G Wilson
Figure caption: Photometric data from TESS and CHEOPS (see Sections 2.1 and 2.3), shown in gray. Binned data are shown in orange, best-fit models (see Section 4) are shown in dark purple, and 100 draws from the posterior distribution are shown in light purple.
Paper: An Eccentric Sub-Neptune Moving Into the Evaporation Desert 
Authors: Sydney A. Jenkins, Andrew Vanderburg, Ritika Sethi, Sarah Millholland, Joseph E. Rodriguez, Luca Fossati, Andreas Krenn, Emily Pass, Alexander Venner, R. Paul Butler, Hugh Osborn, Aaron Householder, Carl Ziegler, Juliette Becker, Perry Berlind, Allyson Bieryla, Christopher Broeg, Michael L. Calkins, Jeffrey D. Crane, Tansu Daylan, Julien de Wit, Jason D. Eastman, David Ehrenreich, Gilbert A. Esquerdo, Michael Fausnaugh, Yadira Gaibor, David W. Latham, Monika Lendl, Andrew W. Mayo, Gaetano Scandariato, Steve Shectman, Stephanie Striegel, Johanna Teske, Thomas G Wilson
Figure caption: Eccentricity evolution of TOI-5800 b, assuming a hypothetical outer companion (Mp,2 = 30 M⊕, P2 = 60 days). We show evolution curves for different outer planet eccentricities using the secular perturbation with tidal evolution model. We find that, regardless of the outer companion’s eccentricity, TOI-5800 b always stabilizes to a relatively low (<0.1) eccentricity.
Paper: An Eccentric Sub-Neptune Moving Into the Evaporation Desert 
Authors: Sydney A. Jenkins, Andrew Vanderburg, Ritika Sethi, Sarah Millholland, Joseph E. Rodriguez, Luca Fossati, Andreas Krenn, Emily Pass, Alexander Venner, R. Paul Butler, Hugh Osborn, Aaron Householder, Carl Ziegler, Juliette Becker, Perry Berlind, Allyson Bieryla, Christopher Broeg, Michael L. Calkins, Jeffrey D. Crane, Tansu Daylan, Julien de Wit, Jason D. Eastman, David Ehrenreich, Gilbert A. Esquerdo, Michael Fausnaugh, Yadira Gaibor, David W. Latham, Monika Lendl, Andrew W. Mayo, Gaetano Scandariato, Steve Shectman, Stephanie Striegel, Johanna Teske, Thomas G Wilson
Figure caption: Diagram of the TOI-5800 system. The star is shown to scale with the planet’s orbit.
Paper: The Discovery of 25 μm Interstellar Methanol
Authors: Sarah L. Nickerson, Naseem Rangwala, Keeyoon Sung, Xinchuan Huang, Edward J. Montiel, Curtis DeWitt, Valentin J. M. Le Gouellec, Sean W. J. Colgan, Jason Dittmann, José Pablo Fonfría, Graham M. Harper, Kathleen E. Kraemer, Jialu Li, Conor A. Nixon, Maisie Frances Rashman, Clara Sousa-Silva, Alexander G. G. M. Tielens, William D. Vacca
Figure caption: 25.3 μm map of the NGC 7538 region from SOFIA/Faint Object infraRed Camera (FORCAST; T. L. Herter et al. 2013) archival data (Cycle 1 Program 0034, PI: A. G. G. M. Tielens). Our target and brightest source, IRS 1, is at the center with offset 0″, 0″ corresponding to α(J2000) = 23:13:45.37, δ(J2000) = +61:28:10.5. The positions of IRS 1 and the dimmer sources (IRS 2, IRS 3, IRS 1E, and IRS 1SE) are given by G. Sandell et al. (2020). In solid green is the 8﹩\mathop{.}\limits^{\unicode{x02033}}﹩7 × 3﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 EXES slit from this work’s 23.9 μm setting (Table A1), and in dashed blue the 14″ and 18″ JCMT beams (F. F. S. van der Tak et al. 2000; S. E. Bisschop et al. 2007) whose CH3OH results we will use for a comparison (Section 5.1). The au scale uses a distance of 2.65 kpc (L. Moscadelli et al. 2009). Note the logarithmic scale for the flux, which exaggerates the brightness of the non-IRS 1 sources.