adsabs/AstroCLIMB huggingface dataset:
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: A VLA X-band image of the HH 24 MMS region from 2019. The position of the earlier epoch observation from 2000 of Reipurth et al. (2002b) is shown as a cross and labeled VLA-1A, while the current position is labeled VLA-1B. Right ascension is in seconds at 5h 46m, decl. is in arcseconds at −00° 10′.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Identification of the optical Hα 1–5 sources and additional infrared sources in the HH 24 region, marked on an Hα+[S II] image from the Subaru telescope. North is up, and east is left.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: HST near-infrared image of the HH 24 MMS region obtained with WFC3 in the [Fe II] 1.644 μm line. The knot MHO 323-1 c is an optically visible HH object here labeled HH 24L. The protostar HOPS 317 is seen to illuminate an outflow cavity that contains several objects in the HH 24L flow (see Figure 3). It is evident that the VLA source(s), associated with HH 24 MMS, and HOPS 317 are separate sources. The labels VLA-1A and VLA-1B refer to the positions marked in Figure 31.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Optical spectra of the M5.5 borderline brown dwarf Hα 5 and the M7 brown dwarf Hα 2 obtained with GMOS on Gemini-N.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: The energy distribution of Hα 5 obtained with the Vizier Photometry Viewer. The majority of data points are from SDSS, PanSTARRS, 2MASS, WISE, and Spitzer. The distribution is a clean Planck curve out to 5 μm, but the WISE 12 and 22 μm data points show a steeply rising infrared excess from circumstellar material. The abscissa is wavelength in microns.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: An H2 image of the HH 24 MMS region obtained with NIRI on the Gemini-N telescope. The HH 24L flow is very extended at near-IR wavelengths, and further H2 knots beyond knot 5 can be seen in Figure 17.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: The faint curved HH 1200 jet emanating from source Hα 1 as seen on a deep Hα image obtained at the Subaru telescope. The distance between knots D and G is 172″, corresponding to a projected separation of 0.33 pc. North is up, and east is left.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: (a) Integrated intensity maps for source NE of the blue- and redshifted high-velocity C18O emission (blue and red contours) overlaid on the 1.3 mm continuum map of source NE. The integrated velocity ranges of the blue- and redshifted high-velocity C18O emission are listed in Table 12, where the velocity ranges adopted in the model fitting are listed. The contour levels start from 4σ in steps of 4σ–20σ and then in steps of 10σ, where 1σ is 1.2 mJy beam−1 km s−1. (b) Total integrated intensity map of the C18O emission in the disk. A Keplerian mask generated based on our best-fit disk model was applied to the C18O velocity channel maps to minimize the contamination from the cloud emission. A white ellipse shows the beam size. (c) Azimuthally averaged intensity profiles of the C18O emission in the disk (data points) extracted from (b). Blue and red dashed lines present the intensity profiles extracted from the maps of the model disks with the power-law and Gaussian intensity profiles, respectively. (d) and (e) position–velocity (P–V) diagrams of the C18O emission along the major axis of the disk (grayscale) in comparison with those extracted from the best-fit disk models (red contours) with the power-law and Gaussian intensity profiles, respectively. The contour levels start from 2σ in steps of 1σ, where 1σ is 1.7 mJy beam−1.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption:  12CO mosaic of outflows in the HH 24 core region as observed with ALMA in the range −6.7 < V lsr < 30 km s−1, with the most extreme blue- and redshifted velocities in the upper-left panel, and the velocities closest to the core emission in the lower-right panel. The observations were done with the 12 m array and have a spatial resolution of about 0.″5.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Same as Figure 40 but for Source Wb. In (a), 1σ is 1.3 mJy beam−1 km s−1. In (d) and (e), the contour levels start from 2σ in steps of 3σ.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Same as Figure 40 but for Source Ea. In (a), 1σ is 1.3 mJy beam−1 km s−1. In (d) and (e), the contour levels start from 2σ in steps of 3σ.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Same as Figure 40 but for Source Eb. In (a), 1σ is 1 mJy beam−1 km s−1. In (d) and (e), the contour levels start from 2σ in steps of 3σ.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption:  13CO mosaic of outflows in the HH 24 core region as observed with ALMA in the range 4.07 < V lsr < 14.04 km s−1, with the highest blue- and redshifted velocities in the left panel, and the velocities closest to the core emission in the right panel. The observations were done with the 12 m array and have a spatial resolution of about 0.″5.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: An ALMA self-calibrated continuum 1.3 mm image showing the principal submillimeter sources of the SSV 63 multiple system. All except source S are detected.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: The ALMA primary-beam field of view overlaid on the HST [Fe II] image. The center of the ALMA observations is at 5:46:08.35–00:10:01.7 (2000), and the radius of the field is 20″, corresponding to where the sensitivity decreases to 20% of that of the phase center. The six sources detected by ALMA at 1.3 mm continuum are marked with red circles.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Integrated intensity map of the C18O emission in the HH 24 region obtained with the ALMA observations. The integrated velocity range is 8.5–11.5 km s−1. The map is centered at source Eb.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: The 12CO molecular outflow MO2 from Wb. Blue contours show the integrated intensity emission over −12.6 ≤ V LSR ≤ − 0.3 km s−1 (with first contour and contour steps of 0.045 and 0.02 Jy beam−1 km s−1, respectively), and red contours show the integrated intensity emission over 11.3 ≤ V LSR ≤ 27.1 km s−1 (with first contour and contour steps of 0.2 and 0.3 Jy beam−1 km s−1, respectively). The dashed black line shows the direction along which the P–V diagram in Figure 53 is extracted.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: The compact 12CO molecular outflow MO1 from source Eb. Blue contours show the integrated intensity emission over −3.0 ≤ V LSR ≤ 4.9 km s−1 (with first contour and contour steps of 0.06 Jy beam−1 km s−1), and red contours show the integrated intensity emission over 16.3 ≤ V LSR ≤ 27.1 km s−1 (with first contour and contour steps of 0.1 and 0.09 Jy beam−1 km s−1, respectively). The dashed black line shows the direction along which the P–V diagram shown in Figure 51 is taken. The flow is perpendicular to the axis of the disk around source Eb. The large red ellipse marks the primary peak of SiO emission, and the smaller circle marks the secondary SiO peak.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: The 12CO molecular outflow from source N. Blue contours show the integrated intensity emission over 4.9 ≤ V LSR ≤ 7.9 km s−1 (with first contour and contour steps of 0.05 Jy beam−1 km s−1), and red contours show the integrated intensity emission over 12.9 ≤ V LSR ≤ 17.3 km s−1 (with first contour and contour steps of 0.17 and 0.07 Jy beam−1 km s−1, respectively). The dashed black line shows the direction along which the P–V diagram shown in Figure 55 is taken.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: ALMA H2CO channel maps of the HH 24 core region from V lsr = 7.98 to V lsr = 12.35 km s−1. The velocity spacing between the panels is ∼0.5 km s−1. Each panel shows three velocities, in blue, green, and red as listed in each frame. The observations were done with the 12 m array and have a spatial resolution of about 0.″5.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: P–V diagram of 12CO emission along the molecular outflow axis of the molecular outflow MO2 from Wb.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: ALMA 13CO channel maps of the HH 24 core region from V lsr = 4.98 to V lsr = 12.38 km s−1, with a velocity spacing between the panels of ∼1.25 km s−1. Each panel shows three velocities, in blue, green, and red as listed in each frame. The observations were done with the 12 m array and have a spatial resolution of about 0.″5.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: ALMA C18O channel maps of the HH 24 core region from V lsr = 8.22 to V lsr = 12.14 km s−1. The velocity spacing between the panels is ∼0.25 km s−1. Each panel shows three velocities, in blue, green, and red as listed in each frame. The observations were done with the 12 m array and have a spatial resolution of about 0.″5.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: P–V diagram of 12CO emission along the axis of the molecular outflow MO1 from source Eb.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: P–V diagram of 12CO emission along the axis of the molecular outflow MO3 from source N.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: (Left) Low-velocity 12CO possibly associated with the walls of a cavity surrounding the C and E jets from source Ea plotted on top of the HST WFC3 (F164N filter) image of the region. Blue contours show the integrated intensity emission over 6.5 ≤ V LSR ≤ 7.1 km s−1 (with first contour and contour steps of 0.04 and 0.05 Jy beam−1 km s−1, respectively), and red contours show the integrated intensity emission over 10.6 ≤ V LSR ≤ 14.4 km s−1 (with first contour and contour steps of 0.3 Jy beam−1 km s−1). Only emission south of decl. −00:09:57 (J2000) is shown. Emission that does not extend beyond 3″ of the map edge is not shown, as it is most likely noise from the low-sensitivity edge of the map. Crosses show the position of the continuum sources. (Right) The 13CO outflow cavity walls plotted on top of the HST WFC3 (F164N filter) image of the region. Contours show the integrated intensity emission over 10.0 ≤ V LSR ≤ 11.8 km s−1 (with first contour and contour steps of 0.052 and 0.07 Jy beam−1 km s−1, respectively). The dashed circle shows the field of view of the ALMA map, given by the distance from the center where the sensitivity decreases to 20% of that of the phase center. Emission within 6″ of the map edge is not shown, as it is most likely noise from the low-sensitivity edge of the map. Crosses show the position of the continuum sources. (Center insert) The HH 24 E jet has a dramatic change in the ratio of [Fe II] and [S II] emission. As discussed in the text, this primarily reflects changes in extinction. The insert shows the ratio [Fe II]/[S II] of the HST images, such that black is [Fe II] strong and white is [S II] strong. It is clear that the blueshifted 12CO emission is associated with high extinction.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: C18O emission integrated over blueshifted velocities shows a streamer feature toward the southwest of the field. The dashed white line shows the direction along which the P–V diagram in Figure 59 is taken.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: P–V diagram of C18O emission along the major axis of the C18O streamer (see Figure 58). The center and the edge of the ALMA field are to the left and right, respectively.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: An example of a numerical simulation of an unstable eight-body equal-mass system illustrating the chaotic nature of the interactions. The decay products are single stars as well as a close and a wide binary. The tick marks are in astronomical unit, and the angular scale assumes a distance of 400 pc.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: A 1.3 mm map made with ALMA of the Eb source. The disk is clearly irregular, with an arm protruding to the east. The color scale starts from 1.5σ [Eb disk] and goes up to 50% of the maximum intensity.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: A low-velocity formaldehyde flow stretches toward the northeast, seemingly following the base of the optical G-jet emanating from source NE. The contours are integrated over V lsr from 8.6–9.7 km s−1.
Paper: High-resolution Emission Spectroscopy of the Ultrahot Jupiter KELT-9b: Little Variation in Day- and Nightside Emission Line Contrasts
Authors: Andrew Ridden-Harper, Ernst de Mooij, Ray Jayawardhana, Neale Gibson, Raine Karjalainen, Marie Karjalainen
Figure caption: The phase coverage of our observed data sets. The central black circle and the outer black circle are to scale representations of the radius of KELT-9 and the orbital semimajor axis of KELT-9b, respectively.
Paper: High-resolution Emission Spectroscopy of the Ultrahot Jupiter KELT-9b: Little Variation in Day- and Nightside Emission Line Contrasts
Authors: Andrew Ridden-Harper, Ernst de Mooij, Ray Jayawardhana, Neale Gibson, Raine Karjalainen, Marie Karjalainen
Figure caption: Cross-correlations from top to bottom of Fe I, Ca II, Mg I, and Si I respectively. Left: the cross-correlation signal as a function of KELT-9b’s orbital phase (vertical axis) and systemic velocity (horizontal axis) for Nights 2 and 3. The planet signal is in the middle of the white dotted guiding lines. Middle: the phase-folded cross-correlation signal as a function of planet orbital velocity (K  p ) and systemic velocity. The vertical and horizontal white dotted lines indicate the best systemic velocity and orbital velocity, respectively. Right: the phase-folded cross-correlation signal at the best value of K  p .
Paper: High-resolution Emission Spectroscopy of the Ultrahot Jupiter KELT-9b: Little Variation in Day- and Nightside Emission Line Contrasts
Authors: Andrew Ridden-Harper, Ernst de Mooij, Ray Jayawardhana, Neale Gibson, Raine Karjalainen, Marie Karjalainen
Figure caption: Summary of the data processing steps used in this analysis, shown for Night 3. The top panel shows the initial one-dimensional spectra from the CARACAL pipeline. The second panel shows the blaze-corrected spectra. The third panel shows the data after one SYSREM iteration. The fourth panel shows the data after weighing down wavelengths with high noise.
Paper: High-resolution Emission Spectroscopy of the Ultrahot Jupiter KELT-9b: Little Variation in Day- and Nightside Emission Line Contrasts
Authors: Andrew Ridden-Harper, Ernst de Mooij, Ray Jayawardhana, Neale Gibson, Raine Karjalainen, Marie Karjalainen
Figure caption: Detection significance of Fe I as a function of the number of SYSREM iterations applied to the data. The blue, red, and black lines use the Goyal et al. (2020), Lothringer et al. (2018), and Fossati et al. (2021) pressure–temperature profiles, respectively. The top left, top right, lower left, and lower right show the result of combining all nights, combining Nights 2 and 3, Night 2 alone, and Night 3 alone, respectively.
Paper: High-resolution Emission Spectroscopy of the Ultrahot Jupiter KELT-9b: Little Variation in Day- and Nightside Emission Line Contrasts
Authors: Andrew Ridden-Harper, Ernst de Mooij, Ray Jayawardhana, Neale Gibson, Raine Karjalainen, Marie Karjalainen
Figure caption: Same as Figure 7 except with the addition of the θ and C parameters.
Paper: High-resolution Emission Spectroscopy of the Ultrahot Jupiter KELT-9b: Little Variation in Day- and Nightside Emission Line Contrasts
Authors: Andrew Ridden-Harper, Ernst de Mooij, Ray Jayawardhana, Neale Gibson, Raine Karjalainen, Marie Karjalainen
Figure caption: Continuum-subtracted model emission spectra of individual species in the atmosphere of KELT-9b, assuming the Lothringer et al. (2018) pressure–temperature profile. We find evidence for the presence of species shown in blue but no evidence for those shown in orange. The vertical axes for all species are in units of parts per million (ppm), except for TiO and VO, which are in units of parts per billion (ppb).
Paper: High-resolution Emission Spectroscopy of the Ultrahot Jupiter KELT-9b: Little Variation in Day- and Nightside Emission Line Contrasts
Authors: Andrew Ridden-Harper, Ernst de Mooij, Ray Jayawardhana, Neale Gibson, Raine Karjalainen, Marie Karjalainen
Figure caption: The conditional (2D) and marginalized (1D) likelihood distributions for Fe I using the Lothringer et al. (2018) pressure–temperature profile after combining the log-likelihoods from all nights.
Paper: High-resolution Emission Spectroscopy of the Ultrahot Jupiter KELT-9b: Little Variation in Day- and Nightside Emission Line Contrasts
Authors: Andrew Ridden-Harper, Ernst de Mooij, Ray Jayawardhana, Neale Gibson, Raine Karjalainen, Marie Karjalainen
Figure caption: Pressure–temperature profiles used to create model emission spectra of KELT-9b. The profiles from Goyal et al. (2020) are only defined for pressures greater than 10−6 bar.
Paper: High-resolution Emission Spectroscopy of the Ultrahot Jupiter KELT-9b: Little Variation in Day- and Nightside Emission Line Contrasts
Authors: Andrew Ridden-Harper, Ernst de Mooij, Ray Jayawardhana, Neale Gibson, Raine Karjalainen, Marie Karjalainen
Figure caption: The conditional (2D) and marginalized (1D) likelihood distributions for Fe I using the Lothringer et al. (2018) pressure–temperature profile for Night 3.
Paper: High-resolution Emission Spectroscopy of the Ultrahot Jupiter KELT-9b: Little Variation in Day- and Nightside Emission Line Contrasts
Authors: Andrew Ridden-Harper, Ernst de Mooij, Ray Jayawardhana, Neale Gibson, Raine Karjalainen, Marie Karjalainen
Figure caption: The conditional (2D) and marginalized (1D) likelihood distributions for Fe I using the Lothringer et al. (2018) pressure–temperature profile for Night 2.