adsabs/AstroCLIMB huggingface dataset:
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Overview of line shape types and their different emitting regions based on the observed line kinematics and excitation, as discussed in Section 5 (see also Figure 15). The three plots at the top of the figure are the same as in Figure 10 but converting the CO FWHM into a representative emitting radius R CO and normalizing that to the dust sublimation radius R subl in each disk (see Section 4.8).
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Different excitation of emission components. Top: examples of NC in triangular lines. Middle: examples of BC in triangular lines. Bottom: examples of SC in double-peak lines. Line fluxes are not flux calibrated; therefore the rotation diagrams are vertically scaled to match the v = 1 − 0 lines in individual objects to better highlight the similarity or difference in curvature, which reflect the excitation conditions. LTE slab model fits to the v = 1 − 0 lines are overplotted in black for NC and BC, showing their prediction for the v = 2 − 1 and 13CO lines in the middle and right panels (see Section 4.7). Upper limits are not plotted for the v = 2 − 1 and 13CO lines for a better visualization of detections.
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Two Keplerian rings of CO emission observed in HD 259431. A model fit to the high-J stacked line profile (which do not suffer from telluric absorption) is shown in red, using the inversion method described in Bosman et al. (2021). Estimates of the emitting radius of CO from the measured HWHM, i.e., the R 50% values plotted in Figure 12, are shown for comparison in the middle plot. This disk also shows a Keplerian ring of CO overtone emission (Ilee et al. 2014) that corresponds to the inner ring observed in fundamental emission in this work. To illustrate that, in the left plot we include the line profile of v = 2 − 0 emission as recently observed with the Immersion Grating Infrared Spectrometer (IGRINS; Grant et al. 2022).
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Classification of CO lines based on the observed properties and interpretation discussed in this work (see also Figure 14). For the decomposition of triangular lines into BC and NC, see examples in Figure 4. Additional distinctive tracers discussed in the text are reported in gray boxes below each line type.
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Water line profiles observed in AS 205 N, as compared to the CO line profile (this work) and to the [O I] line profile (Banzatti et al. 2019). The three emission lines are scaled to highlight where line kinematics are similar between water and CO, whether over the wings only or at the line center too. The first plot shows water emission as observed with CRIRES near 3 μm (Banzatti et al. 2017). The second plot shows a stack of six clean water lines observed in the iSHELL spectrum (Figure 1). The third shows water emission near 12 μm as observed with Texas Echelon Cross Echelle Spectrograph (TEXES; Najita et al. 2018).
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Rotation diagrams of absorption components observed in highly inclined disks (inclination = 50°–65°), including an LTE model fitted to the highest rotationally excited absorption spectrum observed in RY Tau, which almost approaches the excitation of the emission NC components (Figure 11). Elias 20 is included as an example of the lower rotational excitation in spectra where absorption is detected only up to J < 8, showing a much steeper curve.
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Multiple wind components proposed to explain emission from different gas tracers as observed in HD 163296.
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Potential interpretation of BC and NC in triangular lines within the context of a multishell wind launched near the dust sublimation radius. The cartoon of the wind physical structure is adopted from Bans & Königl (2012), and the velocity structure from what typically expected in magnetocentrifugal winds, where the poloidal velocity increases along each streamline and decreases at larger launching radii (Blandford & Payne 1982). The figure is just for illustration of a different velocity and CO excitation in different regions of the wind, and it is not to scale.
Paper: On the Same Wavelength as the Space Telescope Imaging Spectrograph
Authors: Thomas R. Ayres
Figure caption: Examples of co-added STIS wavecal spectra. The lower intensity boundary is a heavily smoothed tracing of the 1σ photometric noise. A roughly horizontal, wavy dotted line represents a measurement threshold based on a multiple of the smoothed noise level. Identifications are provided for selected features. Vertical dotted lines indicate transitions that were rejected owing to close blends or other defects in the wavelengths. Solid vertical lines mark the emissions that were measured using a pseudo-Gaussian formalism. Red is for transitions with vetted laboratory wavelengths; blue (FUV only) are for empirically determined wavelengths (see text). The fitted profiles are depicted on top of the observed intensity points as smooth curves: green (S/N > 3 × the threshold) or orange (S/N ≤ 3 × the threshold). (a) A 50 Å section of E140M-1425, based on 25 wavecals totaling 17.9 ks of exposure. S/N threshold is 10σ. (b) A 50 Å section of E230H-2713, based on 13 wavecals totaling 7.0 ks. S/N threshold is 7σ.
Paper: On the Same Wavelength as the Space Telescope Imaging Spectrograph
Authors: Thomas R. Ayres
Figure caption: Example STIS wavecal echellegram from FUV medium-resolution setting E140M-1425. Slightly slanted bands highlight the individual echelle orders: red for even m (numbered at right), blue for odd.
Paper: A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of π Men c
Authors: Daniel Huber, Timothy R. White, Travis S. Metcalfe, Ashley Chontos, Michael M. Fausnaugh, Cynthia S. K. Ho, Vincent Van Eylen, Warrick H. Ball, Sarbani Basu, Timothy R. Bedding, Othman Benomar, Diego Bossini, Sylvain Breton, Derek L. Buzasi, Tiago L. Campante, William J. Chaplin, Jørgen Christensen-Dalsgaard, Margarida S. Cunha, Morgan Deal, Rafael A. García, Antonio García Muñoz, Charlotte Gehan, Lucía González-Cuesta, Chen Jiang, Cenk Kayhan, Hans Kjeldsen, Mia S. Lundkvist, Stéphane Mathis, Savita Mathur, Mário J. P. F. G. Monteiro, Benard Nsamba, Jia Mian Joel Ong, Erika Pakštienė, Aldo M. Serenelli, Victor Silva Aguirre, Keivan G. Stassun, Dennis Stello, Sissel Norgaard Stilling, Mark Lykke Winther, Tao Wu, Thomas Barclay, Tansu Daylan, Maximilian N. Günther, J. J. Hermes, Jon M. Jenkins, David W. Latham, Alan M. Levine, George R. Ricker, Sara Seager, Avi Shporer, Joseph D. Twicken, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Stellar radius versus distance for the current population of asteroseismic host stars (excluding evolved stars with R > 3.5 R ⊙) with confirmed Δν measurements from ground-based radial velocity observations (orange), CoRoT (red), Kepler/K2 (light blue), and TESS (dark blue). Markers are sized by their visual magnitude and filled symbols show systems with known transiting planets. π Men is now the closest and brightest star with a transiting planet for which detailed asteroseismic modeling is possible. Label references (in order of proximity)—τ Cet (Teixeira et al. 2009), μ Ara (Bouchy et al. 2005), ι Hor (Vauclair et al. 2008), π Men (this work), 16 Cyg B (Metcalfe et al. 2012), λ 2 For (Nielsen et al. 2020), HD 52265 (Lebreton 2012; Escobar et al. 2012; Lebreton & Goupil 2014), Kepler-444 (Campante et al. 2015), HD 38529 (Ball et al. 2020), Kepler-93 (Ballard et al. 2014), TOI-257 (Addison et al. 2021), TOI-197 (Huber et al. 2019) and HIP 41378 (Vanderburg et al. 2016; Becker et al. 2019; Lund et al. 2019).
Paper: A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of π Men c
Authors: Daniel Huber, Timothy R. White, Travis S. Metcalfe, Ashley Chontos, Michael M. Fausnaugh, Cynthia S. K. Ho, Vincent Van Eylen, Warrick H. Ball, Sarbani Basu, Timothy R. Bedding, Othman Benomar, Diego Bossini, Sylvain Breton, Derek L. Buzasi, Tiago L. Campante, William J. Chaplin, Jørgen Christensen-Dalsgaard, Margarida S. Cunha, Morgan Deal, Rafael A. García, Antonio García Muñoz, Charlotte Gehan, Lucía González-Cuesta, Chen Jiang, Cenk Kayhan, Hans Kjeldsen, Mia S. Lundkvist, Stéphane Mathis, Savita Mathur, Mário J. P. F. G. Monteiro, Benard Nsamba, Jia Mian Joel Ong, Erika Pakštienė, Aldo M. Serenelli, Victor Silva Aguirre, Keivan G. Stassun, Dennis Stello, Sissel Norgaard Stilling, Mark Lykke Winther, Tao Wu, Thomas Barclay, Tansu Daylan, Maximilian N. Günther, J. J. Hermes, Jon M. Jenkins, David W. Latham, Alan M. Levine, George R. Ricker, Sara Seager, Avi Shporer, Joseph D. Twicken, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Power density spectra of the solar analogs γ Pav (left), ζ Tuc (middle), and π Men (right) calculated using original 2 minute cadence data (top) and 20 second cadence data (bottom). Gray lines show original power spectra, colored lines show power spectra smoothed by 2 μHz. The S/N of the detection dramatically increases for the 20 second cadence data.
Paper: A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of π Men c
Authors: Daniel Huber, Timothy R. White, Travis S. Metcalfe, Ashley Chontos, Michael M. Fausnaugh, Cynthia S. K. Ho, Vincent Van Eylen, Warrick H. Ball, Sarbani Basu, Timothy R. Bedding, Othman Benomar, Diego Bossini, Sylvain Breton, Derek L. Buzasi, Tiago L. Campante, William J. Chaplin, Jørgen Christensen-Dalsgaard, Margarida S. Cunha, Morgan Deal, Rafael A. García, Antonio García Muñoz, Charlotte Gehan, Lucía González-Cuesta, Chen Jiang, Cenk Kayhan, Hans Kjeldsen, Mia S. Lundkvist, Stéphane Mathis, Savita Mathur, Mário J. P. F. G. Monteiro, Benard Nsamba, Jia Mian Joel Ong, Erika Pakštienė, Aldo M. Serenelli, Victor Silva Aguirre, Keivan G. Stassun, Dennis Stello, Sissel Norgaard Stilling, Mark Lykke Winther, Tao Wu, Thomas Barclay, Tansu Daylan, Maximilian N. Günther, J. J. Hermes, Jon M. Jenkins, David W. Latham, Alan M. Levine, George R. Ricker, Sara Seager, Avi Shporer, Joseph D. Twicken, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Chromospheric activity versus stellar age for a sample of spectroscopic solar twins from Lorenzo-Oliveira et al. (2018) with ages determined from isochrone fitting (gray circles). The fitted relation is shown as a solid line, with uncertainties indicated by dotted lines. Overplotted are bright stars with asteroseismic ages from TESS and Kepler (blue symbols).
Paper: A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of π Men c
Authors: Daniel Huber, Timothy R. White, Travis S. Metcalfe, Ashley Chontos, Michael M. Fausnaugh, Cynthia S. K. Ho, Vincent Van Eylen, Warrick H. Ball, Sarbani Basu, Timothy R. Bedding, Othman Benomar, Diego Bossini, Sylvain Breton, Derek L. Buzasi, Tiago L. Campante, William J. Chaplin, Jørgen Christensen-Dalsgaard, Margarida S. Cunha, Morgan Deal, Rafael A. García, Antonio García Muñoz, Charlotte Gehan, Lucía González-Cuesta, Chen Jiang, Cenk Kayhan, Hans Kjeldsen, Mia S. Lundkvist, Stéphane Mathis, Savita Mathur, Mário J. P. F. G. Monteiro, Benard Nsamba, Jia Mian Joel Ong, Erika Pakštienė, Aldo M. Serenelli, Victor Silva Aguirre, Keivan G. Stassun, Dennis Stello, Sissel Norgaard Stilling, Mark Lykke Winther, Tao Wu, Thomas Barclay, Tansu Daylan, Maximilian N. Günther, J. J. Hermes, Jon M. Jenkins, David W. Latham, Alan M. Levine, George R. Ricker, Sara Seager, Avi Shporer, Joseph D. Twicken, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Ratio of the time-domain scatter for 20 second (blue triangles) and 2 minute (orange circles) data using three quality-flag masks as defined in the Lightkurve package: “Hardest” (rejecting all data with nonzero quality), “Hard” (rejecting severe and cosmic-ray flags), and “Default” (rejecting severe flags only). Points show individual sectors, filled symbols are median bins, and the dashed line marks unity.
Paper: A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of π Men c
Authors: Daniel Huber, Timothy R. White, Travis S. Metcalfe, Ashley Chontos, Michael M. Fausnaugh, Cynthia S. K. Ho, Vincent Van Eylen, Warrick H. Ball, Sarbani Basu, Timothy R. Bedding, Othman Benomar, Diego Bossini, Sylvain Breton, Derek L. Buzasi, Tiago L. Campante, William J. Chaplin, Jørgen Christensen-Dalsgaard, Margarida S. Cunha, Morgan Deal, Rafael A. García, Antonio García Muñoz, Charlotte Gehan, Lucía González-Cuesta, Chen Jiang, Cenk Kayhan, Hans Kjeldsen, Mia S. Lundkvist, Stéphane Mathis, Savita Mathur, Mário J. P. F. G. Monteiro, Benard Nsamba, Jia Mian Joel Ong, Erika Pakštienė, Aldo M. Serenelli, Victor Silva Aguirre, Keivan G. Stassun, Dennis Stello, Sissel Norgaard Stilling, Mark Lykke Winther, Tao Wu, Thomas Barclay, Tansu Daylan, Maximilian N. Günther, J. J. Hermes, Jon M. Jenkins, David W. Latham, Alan M. Levine, George R. Ricker, Sara Seager, Avi Shporer, Joseph D. Twicken, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Marginalized posterior distribution on the orbital eccentricity of π Men c based on the 20 second cadence transit fitting with asteroseismic stellar parameters alone (red) and including information from radial velocities (blue).
Paper: A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of π Men c
Authors: Daniel Huber, Timothy R. White, Travis S. Metcalfe, Ashley Chontos, Michael M. Fausnaugh, Cynthia S. K. Ho, Vincent Van Eylen, Warrick H. Ball, Sarbani Basu, Timothy R. Bedding, Othman Benomar, Diego Bossini, Sylvain Breton, Derek L. Buzasi, Tiago L. Campante, William J. Chaplin, Jørgen Christensen-Dalsgaard, Margarida S. Cunha, Morgan Deal, Rafael A. García, Antonio García Muñoz, Charlotte Gehan, Lucía González-Cuesta, Chen Jiang, Cenk Kayhan, Hans Kjeldsen, Mia S. Lundkvist, Stéphane Mathis, Savita Mathur, Mário J. P. F. G. Monteiro, Benard Nsamba, Jia Mian Joel Ong, Erika Pakštienė, Aldo M. Serenelli, Victor Silva Aguirre, Keivan G. Stassun, Dennis Stello, Sissel Norgaard Stilling, Mark Lykke Winther, Tao Wu, Thomas Barclay, Tansu Daylan, Maximilian N. Günther, J. J. Hermes, Jon M. Jenkins, David W. Latham, Alan M. Levine, George R. Ricker, Sara Seager, Avi Shporer, Joseph D. Twicken, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Échelle diagrams for γ Pav (left), ζ Tuc (middle), and π Men (right) using granulation-background corrected power spectra. Different symbols show measured radial modes (circles), dipole modes (squares), and quadrupole modes (diamonds). Error bars are smaller than symbol sizes in all cases.
Paper: A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of π Men c
Authors: Daniel Huber, Timothy R. White, Travis S. Metcalfe, Ashley Chontos, Michael M. Fausnaugh, Cynthia S. K. Ho, Vincent Van Eylen, Warrick H. Ball, Sarbani Basu, Timothy R. Bedding, Othman Benomar, Diego Bossini, Sylvain Breton, Derek L. Buzasi, Tiago L. Campante, William J. Chaplin, Jørgen Christensen-Dalsgaard, Margarida S. Cunha, Morgan Deal, Rafael A. García, Antonio García Muñoz, Charlotte Gehan, Lucía González-Cuesta, Chen Jiang, Cenk Kayhan, Hans Kjeldsen, Mia S. Lundkvist, Stéphane Mathis, Savita Mathur, Mário J. P. F. G. Monteiro, Benard Nsamba, Jia Mian Joel Ong, Erika Pakštienė, Aldo M. Serenelli, Victor Silva Aguirre, Keivan G. Stassun, Dennis Stello, Sissel Norgaard Stilling, Mark Lykke Winther, Tao Wu, Thomas Barclay, Tansu Daylan, Maximilian N. Günther, J. J. Hermes, Jon M. Jenkins, David W. Latham, Alan M. Levine, George R. Ricker, Sara Seager, Avi Shporer, Joseph D. Twicken, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Phase-folded transit light of π Men c using 20 second data from Sectors 27 and 28 after removal of a Gaussian process model to account for trends due to stellar and instrumental effects. Diamonds and squares show the original 20 second cadence data (gray circles) binned into 2 minute and 30 minute cadence. The best-fitting transit model is shown as the solid line.
Paper: A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of π Men c
Authors: Daniel Huber, Timothy R. White, Travis S. Metcalfe, Ashley Chontos, Michael M. Fausnaugh, Cynthia S. K. Ho, Vincent Van Eylen, Warrick H. Ball, Sarbani Basu, Timothy R. Bedding, Othman Benomar, Diego Bossini, Sylvain Breton, Derek L. Buzasi, Tiago L. Campante, William J. Chaplin, Jørgen Christensen-Dalsgaard, Margarida S. Cunha, Morgan Deal, Rafael A. García, Antonio García Muñoz, Charlotte Gehan, Lucía González-Cuesta, Chen Jiang, Cenk Kayhan, Hans Kjeldsen, Mia S. Lundkvist, Stéphane Mathis, Savita Mathur, Mário J. P. F. G. Monteiro, Benard Nsamba, Jia Mian Joel Ong, Erika Pakštienė, Aldo M. Serenelli, Victor Silva Aguirre, Keivan G. Stassun, Dennis Stello, Sissel Norgaard Stilling, Mark Lykke Winther, Tao Wu, Thomas Barclay, Tansu Daylan, Maximilian N. Günther, J. J. Hermes, Jon M. Jenkins, David W. Latham, Alan M. Levine, George R. Ricker, Sara Seager, Avi Shporer, Joseph D. Twicken, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Power density spectra on a log–log scale using the 20 second cadence light curves for γ Pav (top), ζ Tuc (middle), and π Men (bottom). Each power spectrum was smoothed with a Gaussian with an FWHM of 1 μHz. Lines show the fractional power attenuation as given by Equation (2) on the right-hand y-axis for sampling at 2 minute cadence (solid lines) and 20 second cadence (dashed lines) in each panel.
Paper: A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of π Men c
Authors: Daniel Huber, Timothy R. White, Travis S. Metcalfe, Ashley Chontos, Michael M. Fausnaugh, Cynthia S. K. Ho, Vincent Van Eylen, Warrick H. Ball, Sarbani Basu, Timothy R. Bedding, Othman Benomar, Diego Bossini, Sylvain Breton, Derek L. Buzasi, Tiago L. Campante, William J. Chaplin, Jørgen Christensen-Dalsgaard, Margarida S. Cunha, Morgan Deal, Rafael A. García, Antonio García Muñoz, Charlotte Gehan, Lucía González-Cuesta, Chen Jiang, Cenk Kayhan, Hans Kjeldsen, Mia S. Lundkvist, Stéphane Mathis, Savita Mathur, Mário J. P. F. G. Monteiro, Benard Nsamba, Jia Mian Joel Ong, Erika Pakštienė, Aldo M. Serenelli, Victor Silva Aguirre, Keivan G. Stassun, Dennis Stello, Sissel Norgaard Stilling, Mark Lykke Winther, Tao Wu, Thomas Barclay, Tansu Daylan, Maximilian N. Günther, J. J. Hermes, Jon M. Jenkins, David W. Latham, Alan M. Levine, George R. Ricker, Sara Seager, Avi Shporer, Joseph D. Twicken, Roland K. Vanderspek, Joshua N. Winn
Figure caption: Radial velocity data phase-folded to the orbital periods of π Men b (top panel) and π Men c (bottom panel). The bottom panel shows all instruments except for ESPRESSO in gray. Each panel shows the RV data with the contribution from the other planet removed.
Paper: Scanning Disk Rings and Winds in CO at 0.01–10 au: A High-resolution M-band Spectroscopy Survey with IRTF-iSHELL
Authors: Andrea Banzatti, Kirsten M. Abernathy, Sean Brittain, Arthur D. Bosman, Klaus M. Pontoppidan, Adwin Boogert, Stanley Jensen, John Carr, Joan Najita, Sierra Grant, Rocio M. Sigler, Michael A. Sanchez, Joshua Kern, John T. Rayner
Figure caption: Overview of M-band spectral emission observed in this survey. The top panel shows one full spectrum to illustrate the completeness in coverage obtained with iSHELL in one shot; shaded regions mark H I emission lines, and the atmospheric transmission is reported for reference in green. In the other panels, the full spectrum is broken up into portions from different targets (as indicated above each panel) to illustrate both the richness and diversity of the spectra: from some of the narrowest emission lines with high vibrational excitation (up to v = 6-5, in V892 Tau) to some of the broadest lines (in HD 35929). In each panel, some CO lines are labeled for guidance, in orange for 13CO and all other colors for 12CO. AS 205 N in the last two panels illustrates the first detection of rovibrational water lines near 5 μm (marked in light blue).
Paper: Searching for Diamagnetic Blob Accretion in the 74 day K2 Observation of V2400 Ophiuchi
Authors: Andrew Langford, Colin Littlefield, Peter Garnavich, Mark R. Kennedy, Simone Scaringi, Paula Szkody
Figure caption: The modulation of notable signals with reference to the relative brightness throughout the K2 V2400 Oph observation. The dominant signal is denoted for each ∼5 hr observation window. Strong variability in the beat signal amplitude allows for both spin and beat harmonic signals to appear dominant for periods of observation. There is no distinct correlation between any of the signals or relative brightness throughout the observation. (T 0 ≈ 2823.33559 BKJD).