adsabs/AstroCLIMB huggingface dataset:
Paper: APOGEE Net: An Expanded Spectral Model of Both Low-mass and High-mass Stars
Authors: Dani Sprague, Connor Culhane, Marina Kounkel, Richard Olney, K. R. Covey, Brian Hutchinson, Ryan Lingg, Keivan G. Stassun, Carlos G. Román-Zúñiga, Alexandre Roman-Lopes, David Nidever, Rachael L. Beaton, Jura Borissova, Amelia Stutz, Guy S. Stringfellow, Karla Peña Ramírez, Valeria Ramírez-Preciado, Jesús Hernández, Jinyoung Serena Kim, and Richard R. Lane
Figure caption: Left: comparison between spectral types in literature and the Teff measured for the stars in the sample, color coded by the luminosity class. Yellow circles show the sources with spectral types measured directly from the APOGEE spectra, from Roman-Lopes et al. (2019, 2020) and Ramírez-Preciado et al. (2020). Spectral types are formatted to range as O = 0–10, B = 10–20, A = 20–30, etc. Right: distribution of Teff and ﹩\mathrm{log}g﹩ color coded by the literature luminosity class. Note that the concentration of the supergiants at Teff ∼ 6000 K and ﹩\mathrm{log}g﹩ = 3.5 is primarily from the Magellanic clouds (Section 4.3).
Paper: APOGEE Net: An Expanded Spectral Model of Both Low-mass and High-mass Stars
Authors: Dani Sprague, Connor Culhane, Marina Kounkel, Richard Olney, K. R. Covey, Brian Hutchinson, Ryan Lingg, Keivan G. Stassun, Carlos G. Román-Zúñiga, Alexandre Roman-Lopes, David Nidever, Rachael L. Beaton, Jura Borissova, Amelia Stutz, Guy S. Stringfellow, Karla Peña Ramírez, Valeria Ramírez-Preciado, Jesús Hernández, Jinyoung Serena Kim, and Richard R. Lane
Figure caption: Top: example APOGEE spectra for sources with ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ ranging from 4.5 (blue) to 3.6 (red), with a step of 0.1 dex. The spectra are arbitrarily scaled in flux. Some of the temperature-sensitive lines that can be used to infer parameters of hot stars are shown in gray, such as Brackett H lines and He II lines. The gaps in the spectra correspond to the chip gap. Bottom: spectra with similar ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ ∼ 4.1, but with three different ﹩\mathrm{log}g﹩.
Paper: APOGEE Net: An Expanded Spectral Model of Both Low-mass and High-mass Stars
Authors: Dani Sprague, Connor Culhane, Marina Kounkel, Richard Olney, K. R. Covey, Brian Hutchinson, Ryan Lingg, Keivan G. Stassun, Carlos G. Román-Zúñiga, Alexandre Roman-Lopes, David Nidever, Rachael L. Beaton, Jura Borissova, Amelia Stutz, Guy S. Stringfellow, Karla Peña Ramírez, Valeria Ramírez-Preciado, Jesús Hernández, Jinyoung Serena Kim, and Richard R. Lane
Figure caption: HR diagram of the APOGEE sample of higher-mass stars, color coded by the predicted Teff (left) and ﹩\mathrm{log}g﹩ (right). Black arrows show the reddening vector corresponding to 1 AV.
Paper: APOGEE Net: An Expanded Spectral Model of Both Low-mass and High-mass Stars
Authors: Dani Sprague, Connor Culhane, Marina Kounkel, Richard Olney, K. R. Covey, Brian Hutchinson, Ryan Lingg, Keivan G. Stassun, Carlos G. Román-Zúñiga, Alexandre Roman-Lopes, David Nidever, Rachael L. Beaton, Jura Borissova, Amelia Stutz, Guy S. Stringfellow, Karla Peña Ramírez, Valeria Ramírez-Preciado, Jesús Hernández, Jinyoung Serena Kim, and Richard R. Lane
Figure caption: Top: distribution of sources in the APOGEE DR17 data in galactic coordinates, color coded by the maximum Teff of a source along a line of sight. Note that sources with Teff > 10,000 K tend to be concentrated in the plane, and sources with Teff > 20,000 K tend to primarily trace young star-forming regions. Bottom: distribution of the sources, but limited to only sources with Teff > 8000 K, with the symbol size representative of ﹩\mathrm{log}g﹩ < 3.5, to highlight the position of blue and yellow giants and supergiants.
Paper: APOGEE Net: An Expanded Spectral Model of Both Low-mass and High-mass Stars
Authors: Dani Sprague, Connor Culhane, Marina Kounkel, Richard Olney, K. R. Covey, Brian Hutchinson, Ryan Lingg, Keivan G. Stassun, Carlos G. Román-Zúñiga, Alexandre Roman-Lopes, David Nidever, Rachael L. Beaton, Jura Borissova, Amelia Stutz, Guy S. Stringfellow, Karla Peña Ramírez, Valeria Ramírez-Preciado, Jesús Hernández, Jinyoung Serena Kim, and Richard R. Lane
Figure caption: Stars observed by APOGEE toward the Magellanic clouds. Top left: distribution of Teff and ﹩\mathrm{log}g﹩ of the likely members (red), superimposed on the Milky Way stars in grayscale background. Top middle: same as before, only with stars color coded by their estimated [Fe/H]. Top right: same as before, but separating the stars into five categories based on the parameter space: red giant branch/red supergiant (RGB/RSG), carbon-rich AGB stars (C-AGB), oxygen-rich AGB stars (O-AGB), blue and yellow supergiants (BSG/YSG), and the Cepheid variables. Second row left: 2MASS color–magnitude diagram of the stars that fall into this parameter space. Second row right: ASPCAP parameters for the stars in this parameter space. Although three sequences of RGB/AGB stars overlap, they are nonetheless distinct from one another in this data set as well. Other panels show the spatial distribution of the stars in these categories.
Paper: Gems of the Galaxy Zoos—A Wide-ranging Hubble Space Telescope Gap-filler Program  
Authors: William C. Keel, Jean Tate, O. Ivy Wong, Julie K. Banfield, Chris J. Lintott, Karen L. Masters, Brooke D. Simmons, Claudia Scarlata, Carolin Cardamone, Rebecca Smethurst, Lucy Fortson, Jesse Shanahan, Sandor Kruk, Izzy L. Garland, Colin Hancock, and David O'Ryan
Figure caption: Screen capture of the voting interface for Galaxy Zoo targets. Clicking on “Need some help with this task?” displayed a longer description and a montage of all galaxies in the same voting category. The red banner at upper left indicates that a user has already seen this object.
Paper: Gems of the Galaxy Zoos—A Wide-ranging Hubble Space Telescope Gap-filler Program  
Authors: William C. Keel, Jean Tate, O. Ivy Wong, Julie K. Banfield, Chris J. Lintott, Karen L. Masters, Brooke D. Simmons, Claudia Scarlata, Carolin Cardamone, Rebecca Smethurst, Lucy Fortson, Jesse Shanahan, Sandor Kruk, Izzy L. Garland, Colin Hancock, and David O'Ryan
Figure caption: Emission-line contribution in the F555W, F775W, and F850LP passbands for a typical Green Pea spectrum, SDSS J131036.73+214817.0 at z = 0.2832, evaluated at various redshifts, showing the range near z = 0.24 where both the very broad F555W and F850LP filters have <10% contribution from emission lines, and the very deep minimum in the F775W filter from z = 0.32–0.36 where the contamination from line emission is well below 1%.
Paper: Gems of the Galaxy Zoos—A Wide-ranging Hubble Space Telescope Gap-filler Program  
Authors: William C. Keel, Jean Tate, O. Ivy Wong, Julie K. Banfield, Chris J. Lintott, Karen L. Masters, Brooke D. Simmons, Claudia Scarlata, Carolin Cardamone, Rebecca Smethurst, Lucy Fortson, Jesse Shanahan, Sandor Kruk, Izzy L. Garland, Colin Hancock, and David O'Ryan
Figure caption: Montage of SDSS gri images of galaxies highest-ranked in the voting among four large categories. Object names are shown for those that have been observed at the time of submission.
Paper: Gems of the Galaxy Zoos—A Wide-ranging Hubble Space Telescope Gap-filler Program  
Authors: William C. Keel, Jean Tate, O. Ivy Wong, Julie K. Banfield, Chris J. Lintott, Karen L. Masters, Brooke D. Simmons, Claudia Scarlata, Carolin Cardamone, Rebecca Smethurst, Lucy Fortson, Jesse Shanahan, Sandor Kruk, Izzy L. Garland, Colin Hancock, and David O'Ryan
Figure caption: The first 15 Green Pea systems observed in single filters, as listed in Table 2. Abbreviated names showing the first four digits of the R.A. are used for convenience. Each panel is a 6 × 6″ region, typically 24 × 24 kpc, and all are shown to the same intensity scale, logarithmic above a slight negative offset. North is up, and east to the left in each case. The 2″ scale bar matches the limiting Petrosian radius from SDSS data used in the sample selection. All were observed in the F775M band except 0815, 0905, and 0924, observed in F850LP.
Paper: Gems of the Galaxy Zoos—A Wide-ranging Hubble Space Telescope Gap-filler Program  
Authors: William C. Keel, Jean Tate, O. Ivy Wong, Julie K. Banfield, Chris J. Lintott, Karen L. Masters, Brooke D. Simmons, Claudia Scarlata, Carolin Cardamone, Rebecca Smethurst, Lucy Fortson, Jesse Shanahan, Sandor Kruk, Izzy L. Garland, Colin Hancock, and David O'Ryan
Figure caption: Blue early-type galaxies, in the F475W filter to emphasize young stellar populations. The bottom two are classified as having spectroscopic AGN by the SDSS automated system. Each galaxy shows a tightly wound spiral pattern near the nucleus; the superimposed circles have radius 2.″5, showing how strongly these patterns are blended together in typical survey images. Insets show SDSS composite images, 60″ square, as used by Galaxy Zoo participants in the initial classifications. Some show various levels of structure in these images, but only CGCG 432-030 might have been classified as a clear spiral from SDSS data. North is up, and east to the left, in each case.
Paper: Gems of the Galaxy Zoos—A Wide-ranging Hubble Space Telescope Gap-filler Program  
Authors: William C. Keel, Jean Tate, O. Ivy Wong, Julie K. Banfield, Chris J. Lintott, Karen L. Masters, Brooke D. Simmons, Claudia Scarlata, Carolin Cardamone, Rebecca Smethurst, Lucy Fortson, Jesse Shanahan, Sandor Kruk, Izzy L. Garland, Colin Hancock, and David O'Ryan
Figure caption: Red spiral galaxy UGC 3935, comparing the usual gri composite from SDSS data with the HST ACS F606W image. The region shown is 77″ × 78″ with north at the top.
Paper: Gems of the Galaxy Zoos—A Wide-ranging Hubble Space Telescope Gap-filler Program  
Authors: William C. Keel, Jean Tate, O. Ivy Wong, Julie K. Banfield, Chris J. Lintott, Karen L. Masters, Brooke D. Simmons, Claudia Scarlata, Carolin Cardamone, Rebecca Smethurst, Lucy Fortson, Jesse Shanahan, Sandor Kruk, Izzy L. Garland, Colin Hancock, and David O'Ryan
Figure caption: Some of the kinds of disk structures included in Zoo Gems data. Top row: nuclear bars and bar lenses. Middle row: three-armed spirals. Bottom row: backlit spiral arms and disk with dust attenuation. All images have north at the top and east to the left; vertical white scale bars indicate 10″ in each case. The gray scale is logarithmic, with zero levels and contrast tailored to show the structures in each object. In the object names, SDSS destinations are truncated for legibility.
Paper: Gems of the Galaxy Zoos—A Wide-ranging Hubble Space Telescope Gap-filler Program  
Authors: William C. Keel, Jean Tate, O. Ivy Wong, Julie K. Banfield, Chris J. Lintott, Karen L. Masters, Brooke D. Simmons, Claudia Scarlata, Carolin Cardamone, Rebecca Smethurst, Lucy Fortson, Jesse Shanahan, Sandor Kruk, Izzy L. Garland, Colin Hancock, and David O'Ryan
Figure caption: Deep-red F814W image of the lensed arc around the central galaxy SDSS 133145.32+513431.2 (z = 0.2894). The upward inflection to the north may indicate perturbation by the separate potential of the bright galaxy just outside the arc. The partial ring has characteristic radius 4.″0, projecting to 17.5 kpc at the distance of the lensing system.
Paper: Gems of the Galaxy Zoos—A Wide-ranging Hubble Space Telescope Gap-filler Program  
Authors: William C. Keel, Jean Tate, O. Ivy Wong, Julie K. Banfield, Chris J. Lintott, Karen L. Masters, Brooke D. Simmons, Claudia Scarlata, Carolin Cardamone, Rebecca Smethurst, Lucy Fortson, Jesse Shanahan, Sandor Kruk, Izzy L. Garland, Colin Hancock, and David O'Ryan
Figure caption: Montage of merging galaxies, including two typical mergers (upper row) and two potential regrowing disks (lower row). The layout is as in Figure 7, with 10″ scale bars. The regrowing disks illustrated here span large enough areas on the sky to include the stripe of cosmic-ray events across the middle, where only a single exposure was obtained as the telescope made a dither motion to give double coverage elsewhere. For NGC 2292, the edges of the ACS combined field appear in the corners.
Paper: A Spatially Dependent Correction of Gaia EDR3 Parallax Zero-point Offset based on 0.3 million LAMOST DR8 Giant Stars
Authors: Chun Wang, Haibo Yuan, and Yang Huang
Figure caption: Maps of ωEDR3 − ωG (top panels) and ﹩{\omega }_{\mathrm{EDR}3}^{\mathrm{corr}}-{\omega }_{{\rm{G}}}﹩ (bottom panels) in equatorial coordinate (left panels) and Galactic coordinate (right panels) for the five-parameter solutions. Each pixel covers equal sky area of about 3.36 square degrees. Number of stars in each pixel is larger than 50.
Paper: A Spatially Dependent Correction of Gaia EDR3 Parallax Zero-point Offset based on 0.3 million LAMOST DR8 Giant Stars
Authors: Chun Wang, Haibo Yuan, and Yang Huang
Figure caption: The distributions of MKs difference between MKs coming from Wang et al. (2022MKsW) and that estimated using the distance of Bailer-Jones et al. (2021; MKsGaia) of the test sample in Wang et al. (2022). The left and right panels are the results of dwarfs and giants, respectively. The black dashed line represent Gaussian fits for the difference distributions. The mean values and standard deviations of the two distributions are labeled in the top-left corner of each panel. The ΔMKs is the ﹩{M}_{\mathrm{Ks}}^{\mathrm{Gaia}}-{M}_{\mathrm{Ks}}^{W}﹩.
Paper: A Spatially Dependent Correction of Gaia EDR3 Parallax Zero-point Offset based on 0.3 million LAMOST DR8 Giant Stars
Authors: Chun Wang, Haibo Yuan, and Yang Huang
Figure caption: The absolute magnitude (left panel) and spectral color (right panel) distributions of the LGMWAS training sample (black lines) and our final giant sample (blue lines).
Paper: A Spatially Dependent Correction of Gaia EDR3 Parallax Zero-point Offset based on 0.3 million LAMOST DR8 Giant Stars
Authors: Chun Wang, Haibo Yuan, and Yang Huang
Figure caption: Top panel: the comparison between our parallax and PRC parallax. Bottom panel: the variations of relative parallax difference between our parallax and PRC parallax with the PRC parallax. The black dashed lines in the bottom panel are zero minus/plus 1% or 3%.
Paper: A Spatially Dependent Correction of Gaia EDR3 Parallax Zero-point Offset based on 0.3 million LAMOST DR8 Giant Stars
Authors: Chun Wang, Haibo Yuan, and Yang Huang
Figure caption: Differences distributions of parallaxes between the LAMOST giant stellar sample and Gaia EDR3 five-parameter solution (left panel) or six-parameter solution (right panel). The blue and red histograms represent the ωEDR3 − ωG and ﹩{\omega }_{\mathrm{EDR}3}^{\mathrm{corr}}-{\omega }_{{\rm{G}}}﹩ distributions, respectively. The blue and red dashed lines represent Gaussian fits for the two parallax difference distributions, respectively. The mean values and standard deviations of the two distributions are labeled in the top corner using their corresponding colors.
Paper: A Spatially Dependent Correction of Gaia EDR3 Parallax Zero-point Offset based on 0.3 million LAMOST DR8 Giant Stars
Authors: Chun Wang, Haibo Yuan, and Yang Huang
Figure caption: Parallax differences between our LAMOST giant sample and Gaia EDR3 five-parameter solution (left panel) or Gaia EDR3 six-parameter solution (right panel), as a function of G-band magnitudes (top panels), color information (middle panels: νeff for five-parameter solution, psceudocolour for six-parameter solution), and ecliptic latitude sinβ (bottom panels). The blue and red points represent the (ωEDR3 − ωG) and (﹩{\omega }_{\mathrm{EDR}3}^{\mathrm{corr}}-{\omega }_{{\rm{G}}}﹩), respectively. In each bin, the number of stars is no less than 100. The black dashed lines in each panel mark the differences of −30 μas and 0 μas.
Paper: Flares, Rotation, and Planets of the AU Mic System from TESS Observations
Authors: Emily A. Gilbert, Thomas Barclay, Elisa V. Quintana, Lucianne M. Walkowicz, Laura D. Vega, Joshua E. Schlieder, Teresa Monsue, Bryson Cale, Kevin I. Collins, Eric Gaidos, Mohammed El Mufti, Michael Reefe, Peter Plavchan, Angelle Tanner, Robert A. Wittenmyer, Justin M. Wittrock, Jon M. Jenkins, David W. Latham, George R. Ricker, Mark E. Rose, S. Seager, Roland K. Vanderspek, and Joshua N. Winn
Figure caption: TESS Sector 1, 2 minute cadence observations of AU Mic. The top panel shows our GP spot model, the middle shows our flare model, and the bottom shows the residuals.
Paper: Flares, Rotation, and Planets of the AU Mic System from TESS Observations
Authors: Emily A. Gilbert, Thomas Barclay, Elisa V. Quintana, Lucianne M. Walkowicz, Laura D. Vega, Joshua E. Schlieder, Teresa Monsue, Bryson Cale, Kevin I. Collins, Eric Gaidos, Mohammed El Mufti, Michael Reefe, Peter Plavchan, Angelle Tanner, Robert A. Wittenmyer, Justin M. Wittrock, Jon M. Jenkins, David W. Latham, George R. Ricker, Mark E. Rose, S. Seager, Roland K. Vanderspek, and Joshua N. Winn
Figure caption: TESS Sector 27, 2 minute cadence observations of AU Mic. The top panel shows our GP spot model, the middle shows our flare model, and the bottom shows the residuals.
Paper: Flares, Rotation, and Planets of the AU Mic System from TESS Observations
Authors: Emily A. Gilbert, Thomas Barclay, Elisa V. Quintana, Lucianne M. Walkowicz, Laura D. Vega, Joshua E. Schlieder, Teresa Monsue, Bryson Cale, Kevin I. Collins, Eric Gaidos, Mohammed El Mufti, Michael Reefe, Peter Plavchan, Angelle Tanner, Robert A. Wittenmyer, Justin M. Wittrock, Jon M. Jenkins, David W. Latham, George R. Ricker, Mark E. Rose, S. Seager, Roland K. Vanderspek, and Joshua N. Winn
Figure caption: TESS Sector 27, 20 s cadence observations of AU Mic. The top panel shows our GP spot model, the middle shows our flare model, and the bottom shows the residuals.
Paper: Flares, Rotation, and Planets of the AU Mic System from TESS Observations
Authors: Emily A. Gilbert, Thomas Barclay, Elisa V. Quintana, Lucianne M. Walkowicz, Laura D. Vega, Joshua E. Schlieder, Teresa Monsue, Bryson Cale, Kevin I. Collins, Eric Gaidos, Mohammed El Mufti, Michael Reefe, Peter Plavchan, Angelle Tanner, Robert A. Wittenmyer, Justin M. Wittrock, Jon M. Jenkins, David W. Latham, George R. Ricker, Mark E. Rose, S. Seager, Roland K. Vanderspek, and Joshua N. Winn
Figure caption: We determine the reference energy for AU Mic by multiplying its spectrum by the TESS transmission function. The resulting convolved spectrum is shown in black. Integrating under the convolved spectrum gives us the quiescent energy emitted by AU Mic within the TESS bandpass.
Paper: Flares, Rotation, and Planets of the AU Mic System from TESS Observations
Authors: Emily A. Gilbert, Thomas Barclay, Elisa V. Quintana, Lucianne M. Walkowicz, Laura D. Vega, Joshua E. Schlieder, Teresa Monsue, Bryson Cale, Kevin I. Collins, Eric Gaidos, Mohammed El Mufti, Michael Reefe, Peter Plavchan, Angelle Tanner, Robert A. Wittenmyer, Justin M. Wittrock, Jon M. Jenkins, David W. Latham, George R. Ricker, Mark E. Rose, S. Seager, Roland K. Vanderspek, and Joshua N. Winn
Figure caption: The flare frequency distributions for AU Mic show the flares modeled in both Sectors 1 and 27, as well as 2 minute and 20 s data for Sector 27 with the shaded regions showing the 1σ and 2σ uncertainties. 20 s data significantly improves our ability to detect smaller (on order ∼1032 erg) flares and resolve the full morphology of larger flares, resulting in larger flare energies. 2 minute data represents a lower limit on flare frequency and total energy.
Paper: Flares, Rotation, and Planets of the AU Mic System from TESS Observations
Authors: Emily A. Gilbert, Thomas Barclay, Elisa V. Quintana, Lucianne M. Walkowicz, Laura D. Vega, Joshua E. Schlieder, Teresa Monsue, Bryson Cale, Kevin I. Collins, Eric Gaidos, Mohammed El Mufti, Michael Reefe, Peter Plavchan, Angelle Tanner, Robert A. Wittenmyer, Justin M. Wittrock, Jon M. Jenkins, David W. Latham, George R. Ricker, Mark E. Rose, S. Seager, Roland K. Vanderspek, and Joshua N. Winn
Figure caption: 20 s cadence data (black) allow us to better resolve flare peak amplitudes as compared to the 2 minute cadence data (pink).
Paper: Flares, Rotation, and Planets of the AU Mic System from TESS Observations
Authors: Emily A. Gilbert, Thomas Barclay, Elisa V. Quintana, Lucianne M. Walkowicz, Laura D. Vega, Joshua E. Schlieder, Teresa Monsue, Bryson Cale, Kevin I. Collins, Eric Gaidos, Mohammed El Mufti, Michael Reefe, Peter Plavchan, Angelle Tanner, Robert A. Wittenmyer, Justin M. Wittrock, Jon M. Jenkins, David W. Latham, George R. Ricker, Mark E. Rose, S. Seager, Roland K. Vanderspek, and Joshua N. Winn
Figure caption: Posterior model of the rotation of AU Mic, measured from the TESS photometric data. The Sector 1 data give stronger constraints on the rotation period, primarily because there seems to be a little more light-curve morphology change or phase drift in the Sector 27 data.
Paper: Flares, Rotation, and Planets of the AU Mic System from TESS Observations
Authors: Emily A. Gilbert, Thomas Barclay, Elisa V. Quintana, Lucianne M. Walkowicz, Laura D. Vega, Joshua E. Schlieder, Teresa Monsue, Bryson Cale, Kevin I. Collins, Eric Gaidos, Mohammed El Mufti, Michael Reefe, Peter Plavchan, Angelle Tanner, Robert A. Wittenmyer, Justin M. Wittrock, Jon M. Jenkins, David W. Latham, George R. Ricker, Mark E. Rose, S. Seager, Roland K. Vanderspek, and Joshua N. Winn
Figure caption: Sector 1 and Sector 27 phase folded at the rotation period of the star, P = 4.85 days. Each phase is offset vertically for clarity, with time progressing downward. The overall shape of the light curve shows remarkable consistency over the 2 year observation baseline. The Sector 27 data has been shifted in phase to align with Sector 1 data.
Paper: Flares, Rotation, and Planets of the AU Mic System from TESS Observations
Authors: Emily A. Gilbert, Thomas Barclay, Elisa V. Quintana, Lucianne M. Walkowicz, Laura D. Vega, Joshua E. Schlieder, Teresa Monsue, Bryson Cale, Kevin I. Collins, Eric Gaidos, Mohammed El Mufti, Michael Reefe, Peter Plavchan, Angelle Tanner, Robert A. Wittenmyer, Justin M. Wittrock, Jon M. Jenkins, David W. Latham, George R. Ricker, Mark E. Rose, S. Seager, Roland K. Vanderspek, and Joshua N. Winn
Figure caption: Our model of the five TESS transits of AU Mic b and stellar flares that occur in and around the transit. The first two transits are Sector 1, 2 minute cadence, and the others are Sector 27, 20 s cadence.
Paper: Flares, Rotation, and Planets of the AU Mic System from TESS Observations
Authors: Emily A. Gilbert, Thomas Barclay, Elisa V. Quintana, Lucianne M. Walkowicz, Laura D. Vega, Joshua E. Schlieder, Teresa Monsue, Bryson Cale, Kevin I. Collins, Eric Gaidos, Mohammed El Mufti, Michael Reefe, Peter Plavchan, Angelle Tanner, Robert A. Wittenmyer, Justin M. Wittrock, Jon M. Jenkins, David W. Latham, George R. Ricker, Mark E. Rose, S. Seager, Roland K. Vanderspek, and Joshua N. Winn
Figure caption: The five TESS transits of AU Mic b with the the best-fitting GP mean model subtracted from the data. The first two transits are Sector 1, 2 minute cadence, and the others are Sector 27, 20 s cadence.
Paper: Flares, Rotation, and Planets of the AU Mic System from TESS Observations
Authors: Emily A. Gilbert, Thomas Barclay, Elisa V. Quintana, Lucianne M. Walkowicz, Laura D. Vega, Joshua E. Schlieder, Teresa Monsue, Bryson Cale, Kevin I. Collins, Eric Gaidos, Mohammed El Mufti, Michael Reefe, Peter Plavchan, Angelle Tanner, Robert A. Wittenmyer, Justin M. Wittrock, Jon M. Jenkins, David W. Latham, George R. Ricker, Mark E. Rose, S. Seager, Roland K. Vanderspek, and Joshua N. Winn
Figure caption: Transit times as compared to the derived orbital period for all five transits of AU Mic b observed by TESS.
Paper: Flares, Rotation, and Planets of the AU Mic System from TESS Observations
Authors: Emily A. Gilbert, Thomas Barclay, Elisa V. Quintana, Lucianne M. Walkowicz, Laura D. Vega, Joshua E. Schlieder, Teresa Monsue, Bryson Cale, Kevin I. Collins, Eric Gaidos, Mohammed El Mufti, Michael Reefe, Peter Plavchan, Angelle Tanner, Robert A. Wittenmyer, Justin M. Wittrock, Jon M. Jenkins, David W. Latham, George R. Ricker, Mark E. Rose, S. Seager, Roland K. Vanderspek, and Joshua N. Winn
Figure caption: Three transits of AU Mic c. One from Sector 1 observed at 2 minute cadence, and two transits from Sector 27 observed at 20 s cadence.