adsabs/AstroCLIMB huggingface dataset:
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The occurrence rate of hot planets (P = 1–10 days) as a function of chemical abundances for ten different chemical elements. The colors represent planets of different size classes (Jupiters: orange, sub-Saturns: pink, sub-Neptunes: teal, super-Earths: black). The points show the number of planets per 100 stars per bins equally spaced across the inner 90% of the abundance distribution for each element. The triangles show upper limits (90th percentile) on the planet occurrence rate, and the lines and shaded regions show our best fit and 1σ uncertainty to a power-law distribution of the form, fX,P ∝ Pα 10βX, where we have integrated over the period dependence to display the fit in one dimension. Models are not shown for sub-Saturns and Jupiters when the fit is poorly constrained. We emphasize once again that the occurrence rates and upper limits displayed in this figure are for larger bin sizes than those used to fit the power-law distribution, and are included to guide the eye.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The same as in Figure 15, but for warm planets (P = 10–100 days). We see overall weaker trends for each element and planet size class, with the possible exception of sub-Saturns given the low number of detections at short periods.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The derived β and uncertainties for each chemical species, and each planet size class with periods ranging between 1 and 10 days. The colors show the planet size class for which β was derived (black: super-Earths, teal: sub-Neptunes, orange: Jupiters). The dashed line shows the mean across all elements, and the shaded region shows the inner 68% of the posteriors to the fits performed across all elements in Section 4.3.3. In order of increasing planet size class, the averages are βavg = +0.7, +2.0, and +6.4, though the Jupiters in our sample have a range of β ∼ 3–12.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The derived β and uncertainties for each chemical species, and each planet size class with 10 < P < 100 days. The legend is the same as in Figure 17, with the planet size classes represented by differing colors (black: super-Earths, teal: sub-Neptunes, pink: sub-Saturns, orange: Jupiters). In order of increasing planet size class, the averages are βavg = −0.5, +0.4, +1.8, and +0.6.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The metallicity distribution functions of the planet hosts in the “Young” and “Old” samples from Berger et al. (2020a) that were observed by APOGEE. The metallicities for each planet host are displayed as vertical ticks near the top of the figure.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The DR24 Kepler pipeline detection efficiency. The shading shows the probability of the Kepler TPS module to recover a transit signal (prec) with an expected Multiple Event Statistic (MESexp) and Period (P). Darker shades of red represent a lower recovery fraction, and lighter shades represent a higher recovery fraction. Top: the recovery probability (prec) of the Kepler pipeline from the injection and recovery experiments in Christiansen et al. (2016). White spaces denote bins with no data. Bottom: the interpolated, and smoothed grid of prec that we apply for our completeness corrections.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The average DR24 Kepler TPS pipeline detection efficiency for the stars in ﹩{ \mathcal S }﹩. Darker shades of blue represent a lower detection fraction, and lighter shades represent a higher detection fraction.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The probability that a particular planet candidate is observed in the three fields with early target selection in the APOGEE-KOI survey. There is a bias incurred from selecting planet candidates from a pre-DR24, nonstatic catalog, as well as avoiding APOGEE fiber collisions. The points show the fraction of DR24 planet candidates observed in APOGEE at a given transit S/N for field K16 (top) and fields K10 and K21 (bottom). The error bars are derived assuming a binomial distribution. The blue lines show our adopted models to correct for this bias.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The ASPCAP failure rate as a function of H magnitude. The data points are the fraction of stars observed in the APOGEE-KOI program where ASPCAP did not derive a solution in a given magnitude bin, with error bars assumed from a binomial distribution. The blue line shows our fitted model for the failure rate.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: Our measurements for ﹩{{ \mathcal F }}_{\star }({X}_{i})﹩, applying a Gaussian KDE. The tan line shows our derived KDE, with the shaded region showing the 1σ region of credible models obtained from Monte Carlo sampling and bootstrapping. The abundance ratio distributions in ﹩{ \mathcal P }﹩ are shown in purple for comparison. The bandwidth used to model the abundance ratio distributions for ﹩{ \mathcal C }﹩ are represented by the tan error bar in the upper corner, and the vertical dashed lines mark off the inner 90th percentiles used in the occurrence rate analyses. The black error bar shows the median abundance uncertainty. The element is noted in the top left of each panel.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The likelihood of a correlation between the survey efficiency, η(P, Rp), and chemical abundance for stars in ﹩{ \mathcal C }﹩. In each panel, each box in the P–Rp plane is colored by the Spearman correlation coefficient, and the numbers in each box are the p-values from the Spearman correlation test. With the possible exception of a correlation between Al and the detectability of super-Earths with P ∼ 3–10 days, there are no statistically significant correlations between abundance ratio and survey efficiency for stars in ﹩{ \mathcal C }﹩.
Paper: The Family of V1311 Ori: a Young Sextuple System or a Minicluster?
Authors: Andrei Tokovinin
Figure caption: Location of the four stars on the sky. The underlying image is from 2MASS band K (Skrutskie et al. 2006). The object is 2° north of the Orion nebula.
Paper: The Family of V1311 Ori: a Young Sextuple System or a Minicluster?
Authors: Andrei Tokovinin
Figure caption: Possible hierarchy of the V1311 Ori system. The numbers in italics are estimated masses of the components.
Paper: The Family of V1311 Ori: a Young Sextuple System or a Minicluster?
Authors: Andrei Tokovinin
Figure caption: Color–magnitude diagrams. The full and dashed lines are PARSEC isochrones (Bressan et al. 2012) for 24 Myr and 1 Gyr, respectively.
Paper: The Family of V1311 Ori: a Young Sextuple System or a Minicluster?
Authors: Andrei Tokovinin
Figure caption: Speckle power spectra of the four stars (in negative logarithmic rendering) recorded on 2021 November 19 at SOAR. Fringes in the spectra of A and B indicate that they are resolved close pairs, while C and D do not have companions with separations above 0.″04.
Paper: The Family of V1311 Ori: a Young Sextuple System or a Minicluster?
Authors: Andrei Tokovinin
Figure caption: Tentative visual and spectroscopic orbit of Aa,Ab (orbit 1). The upper panel shows position measurements with scale in arcseconds (the SOAR measurements in 2021 are plotted in red, those of Janson et al. in green). The dashed line shows the alternative long-periodorbit 2. The lower panel is the RV curve (the dotted line shows the systemic velocity, the cross marks the rejected measurement).
Paper: The Family of V1311 Ori: a Young Sextuple System or a Minicluster?
Authors: Andrei Tokovinin
Figure caption: Fragments of the light curves of stars A and BC recorded by TESS in sector 32 (2020 November). The first point is at JD 2459174.2234.
Paper: The Family of V1311 Ori: a Young Sextuple System or a Minicluster?
Authors: Andrei Tokovinin
Figure caption: CCFs of the FEROS and CHIRON spectra of V1311 Ori (full lines) and their Gaussian approximations (crosses). The CHIRON CCF is displaced vertically by −0.2. The vertical dotted line marks the systemic velocity of Aa,Ab, the short dashed–dotted line corresponds to the expected RV of the secondary component in 2017.28.
Paper: The Family of V1311 Ori: a Young Sextuple System or a Minicluster?
Authors: Andrei Tokovinin
Figure caption: Hydrogen emission lines in the CHIRON spectrum (full lines) and fitted Gaussians (dashed lines).
Paper: The Family of V1311 Ori: a Young Sextuple System or a Minicluster?
Authors: Andrei Tokovinin
Figure caption: Parallaxes of four stars in Gaia EDR3 and DR2. The dotted line marks the mean parallax of C and D, 25.94 mas.
Paper: The Family of V1311 Ori: a Young Sextuple System or a Minicluster?
Authors: Andrei Tokovinin
Figure caption: Location of stars A to E projected onto the Galactic plane, assuming their EDR3 parallaxes. The dotted line is a linear fit.
Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: Same as Figure 1, here we show the observations of HATS-75 together with our best-fit model. The TESS light curve for this system is shown in Figure 6.
Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: Same as Figure 1, here we show the observations of HATS-76 together with our best-fit model. The TESS light curve for this system is shown in Figure 7.
Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: Same as Figure 1, here we show the observations of HATS-77 together with our best-fit model. The TESS light curve for this system is shown in Figure 8.
Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: TESS short-cadence light curve for HATS-74A. We show the full unphased light curve as a function of time (top), the full phase-folded light curve (middle left), the phase-folded light curve zoomed in on the planetary transit (middle right), the phase-folded light curve zoomed in on the secondary eclipse (bottom left), and the residuals from the best-fit model, phase-folded and zoomed in on the planetary transit (bottom right). The solid line in each panel shows the model fit to the light curve. The dark filled circles show the light curve binned in phase with a bin size of 0.002. Other observations included in our analysis of this system are shown in Figure 1.
Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: Similar to Figure 5, here we show the TESS short-cadence light curve for HATS-75. Other observations included in our analysis of this system are shown in Figure 2.
Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: Similar to Figure 5, here we show the TESS short-cadence light curve for HATS-76. Other observations included in our analysis of this system are shown in Figure 3.
Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: Similar to Figure 8, here we show the TESS short-cadence light curve for HATS-77. Other observations included in our analysis of this system are shown in Figure 4.
Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: Detection of a P = 4.745422 ± 0.000040 day photometric rotation period signal in the TESS light curve of HATS-74A (left) and P = 35.0435 ± 0.0017 day signal in the HATSouth light curve of HATS-75 (right). In each case we show the following panels. Top: the Generalized Lomb-Scargle (GLS) periodogram of the light curve after subtracting the best-fit transit model. The horizontal blue line shows the bootstrap-calibrated 10−3 false alarm probability level for HATS-74A and the 10−5 false alarm probability level for HATS-75. Second from top: the Box-fitting Least Squares (BLS) periodogram of the same light curve. For HATS-74A there is a peak in the BLS periodogram at twice the period of the strongest peak in the GLS periodogram. For HATS-75 no significant peak is present in the BLS periodogram. Second from bottom: the TESS (left) and HATSouth (right) light curve phase-folded at the peak GLS period. The gray points show the individual photometric measurements, while the dark-red filled squares show the observations binned in phase with a bin size of 0.02. Bottom: same as the second from bottom, here we restrict the vertical range of the plot to better show the variation seen in the phase-binned measurements.
Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: Similar to Figure 9, here we show the detection of a P = 15.16063 ± 0.00048 day photometric rotation period in the HATSouth light curve of HATS-76.
Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: ARCoIRIS spectra for our targets, along with IRTF/SpeX and ArcoIRIS spectra for M dwarfs with known stellar atmospheric parameters. The ARCoIRIS spectra have been degraded to the resolution of IRTF/SpeX for this figure. The effective temperatures derived using the procedure of Newton et al. (2014, 2015) are indicated over the K-band spectra.
Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: Top: high-resolution images in Brγ (left) and J-continuum (middle) and associated contrast curve for HATS-74A (TOI 737) from Keck II/NIRC2. The 0.″844 neighbor HATS-74B is apparent in these images. Bottom: contrast curves at 562 and 832 nm from the `Alopeke/Gemini 8 m observations of HATS-74A. The 832 nm image is also shown in the inset.
Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: Left: contrast curves for HATS-75 (TOI 552) derived from high-resolution images at 562 and 832 nm obtained with `Alopeke/Gemini8 m. The 832 nm image is also shown in the inset. Right: contrast curve for HATS-75 derived from high-resolution Ks-band imaging with NaCo/VLT.