adsabs/AstroCLIMB huggingface dataset:
Paper: A Hot Mars-sized Exoplanet Transiting an M Dwarf
Authors: Caleb I. Cañas, Suvrath Mahadevan, William D. Cochran, Chad F. Bender, Eric D. Feigelson, C. E. Harman, Ravi Kumar Kopparapu, Gabriel A. Caceres, Scott A. Diddams, Michael Endl, Eric B. Ford, Samuel Halverson, Fred Hearty, Sinclaire Jones, Shubham Kanodia, Andrea S. J. Lin, Andrew J. Metcalf, Andrew Monson, Joe P. Ninan, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: KOI-4777.01 compared in orbital period and planetary radius with other candidate USPs from Kepler (Sanchis-Ojeda et al. 2014; Caceres et al. 2019b) and K2 (Adams et al. 2021). USPs from the literature were queried from the NASA Exoplanet Archive (Akeson et al. 2013) on 2021 September 3. LHS 3844 b (Vanderspek et al. 2019) is marked as the blue star and another USP orbiting a similar M dwarf. KOI-4777.01, with a radius of 0.51 ± 0.03 R ⊕, is the smallest validated USP.
Paper: A Hot Mars-sized Exoplanet Transiting an M Dwarf
Authors: Caleb I. Cañas, Suvrath Mahadevan, William D. Cochran, Chad F. Bender, Eric D. Feigelson, C. E. Harman, Ravi Kumar Kopparapu, Gabriel A. Caceres, Scott A. Diddams, Michael Endl, Eric B. Ford, Samuel Halverson, Fred Hearty, Sinclaire Jones, Shubham Kanodia, Andrea S. J. Lin, Andrew J. Metcalf, Andrew Monson, Joe P. Ninan, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guđmundur Stefánsson
Figure caption: KOI-4777.01 on the mass–radius diagram. Without a mass measurement, we only constrain the most probable location of KOI-4777.01. The shaded regions indicate our 1σ and 3σ radius measurement, and incorporate limits on the mass from density constraints. For comparison, we include the inner solar system planets and the Moon (red diamonds), well-characterized and small Kepler planets (Almenara et al. 2018; Mills & Fabrycky 2017), the TRAPPIST-1 system (Agol et al. 2021), and known USPs (gray points) from the NASA Exoplanet Archive (queried 2021 September 3). We include several model composition curves from Zeng et al. (2019). KOI-4777.01 is hot (T eq > 1000K), and is incompatible with models that include an atmosphere with temperature effects. It is compatible with models of rocky planets with no significant volatile envelope.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: Comparisons of temperatures, orbital periods, and surface gravities between WD 0137B, EPIC 2122B, and transiting exoplanets. Left: The two irradiated brown dwarfs have shorter orbital periods and higher equilibrium temperatures than exoplanets. Right: Compared to exoplanets, the two brown dwarfs have higher surface gravity and higher dayside temperatures. We assume dayside-only heat redistribution in the derivation of T day. The exoplanet data are a subset of the NASA Exoplanet Archive. The selection criteria are “detection method = transit” and M  p  < 13M Jup.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: Summary of the time-resolved WFC3/G141 spectroscopic observational results for WD 0137 (upper) and EPIC 2122 (lower). In both figures, the top subplots show three representative spectra: the brightest (blue), the faintest (orange), and the average (black). The left subplots show the normalized 1.12–1.65 μm integrated phase curves. Our observations captured 4.1 and 5.6 periods of WD 0137 and EPIC 2122, respectively. The colors of the points also represent the normalized broadband brightness. The lower right subplots show the time-resolved spectra. The color map demonstrates the flux density relative to the mean value of the same wavelength—deep red/blue colors correspond to high modulation amplitudes in that wavelength.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: Fitting Fourier series models of various maximum orders (upper: N = 1, middle: N = 2, lower N = 4) to the light curves of WD0137 (left) and EPIC 2122 (right). The light curves are phase-folded to their best-fitting periods (1.917 hr for WD 0137 and 1.13368 hr for EPIC 2122) and shifted so that the peak of the k = 1 wave peak is at zero phase. Squared dots in different colors show broadband photometry in different HST orbits. The black solid lines show the best-fit Fourier series models, and the colored dashed lines show the model components. The N = 1 model is insufficient for either target and results in similar residual patterns that peak at ±π and 0 phases. The N = 2 and N = 4 models have much better fits in both cases. Based on BIC, the N = 2 model is the most favored for WD 0137 and N = 4 is the best one for EPIC 2122.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: The amplitudes and phase offsets of the k = 1 (blue circles) and k = 2 (yellow squares) waves as functions of wavelength for WD 0137 (left) and EPIC 2122 (right). In the amplitude plots, the left and right axes show the scales for the k = 1 and k = 2 waves, respectively. For easy visual comparisons, the k = 2 amplitudes are scaled up by 10× and 8× for WD 0137 and EPIC 2122, respectively. In the phase offset plots, the blue and yellow horizontal shades show the ±1σ ranges of the average phase offsets of the k = 1 and k = 2 waves, respectively.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: Retrieving top-of-the-atmospheric flux maps from the phase curves of WD 0137B and EPIC 2122B. Upper panels show comparisons of the 1.12–1.65 μm phase curves to three models: the best-fit starry phase curve, the scaled GCM phase curve, and the phase curve derived based on radiative-convective equilibrium. All three models fit well to the observations and are almost indistinguishable from each other. In the figure legends, the model names are followed by the reduced-χ 2 values. Lower panels show the retrieved starry and GCM top-of-the-atmospheric flux maps. While different in details, both maps share the same dominant features: a confined hot spot centered on the brown dwarfs’ substellar points.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: The amplitude ratios between the k = 1 and k = 2 waves in the phase curve of a hot spot map. Regardless of viewing geometry (i = 35° and 56° for WD 0137B and EPIC 2122B, respectively), the smaller the spot, the more significant the k = 2 wave is. Therefore, higher-order Fourier components constrain the hot spot size.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: Temperature distributions at 0.05, 5, and 50 bar in the GCM simulation of WD 0137B. Deep into the atmosphere, the temperature is approximately uniformly distributed. Near the top of the atmosphere, the temperature bifurcates into the two extrema of the day- and nightsides. At an intermediate pressure level, the hot spot is the most pronounced.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: The day/night spectra of WD 0137B (left) and EPIC 2122B (right). The yellow and purple dots represent the observed day- and nightsides spectra, respectively; the error bars show their 1σ uncertainties. The solid lines and swashes are observations and 1σ uncertainties convolved with a Gaussian kernel with a width equal to the spectral resolution of the G141 grism (R ∼ 130 at 1.4 μm), illustrating the actual resolving power of our observations. The y-axes are discontinuous in order to properly visualize the flux density and temperature ranges and demonstrate their wavelength dependence.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: Spectra of the brown dwarfs in WD 0137 (left) and EPIC 2122 (right) in four representative rotational phases between the day- and nightsides (ϕ = ± π/3π and ±2π/3). The spectra are color-coded by their phases, with light colors indicating the dayside and dark colors indicating the nightside. The same as in Figure 8, dots and error bars show the immediate observational results; lines and swashes show spectra smoothed with the instrument’s spectral resolution unit. All spectra are plotted in absolute flux densities without normalization or vertical offsets applied. The differences between spectra are real flux differences.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: WD+BD spectral model fitting results for WD 0137 at four representative phases between the day- and nightsides at ϕ = ±1/3π and ϕ ± 2/3π. The best-fitting white dwarf components are subtracted from all spectra. The lines are the best-fitting brown dwarf models, which are the sum of the scaled dayside component (yellow dashed lines) and the scaled nightside component (dashed lines). In every case, this semi-empirical model fits the observations well.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: Similar to Figure 10, but for EPIC 2122.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: Comparing the dayside spectral contribution factors as functions of rotational phase between WD 0137B (blue squares) and EPIC 2122B (yellow triangle). Both have nearly sinusoidal shapes, but the EPIC 2122B curve has a flatter valley and a more narrow peak.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: The day- and nightsides brightness temperatures of WD 0137B (left) and EPIC 2122B (right). The plotting styles and conventions follow Figure 8: The yellow and purple dots are T  B  of day- and nightsides, respectively; error bars are 1σ uncertainties; lines and swashes are observations convolved with a Gaussian kernel, to demonstrate the instrument’s spectral resolving power. The y-axes are discontinuous, to properly zoom into the flux density and temperature ranges and demonstrate their wavelength dependence.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: Fitting the irradiated atmospheric models to the dayside spectra of WD 0137B (left) and EPIC 2122B (right). In both panels, observational data are plotted in the same conventions as in Figure 8. The best-fitting models are represented by orange solid lines. In both cases, the irradiated atmospheric models fit the observations well, resulting in reduced-χ 2 values close to unity. Irradiation makes the model spectra become steeper than the blackbody (blue dashed line) and thus fit the observations better.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: The opacity sources and atmospheric profiles of the best-fitting dayside models of WD 0137B (left) and EPIC 2122B (right). The upper panels demonstrate the opacity contributions from various sources. Atomic, molecular, continuum (mostly H2-H2/H2-He CIA for WD 0137B and H− for EPIC 2122B), and total opacities are shown in blue, yellow, green, and pink lines. The thick red lines show the total opacities downsampled to G141's spectral resolution (R ∼ 130 at 1.4 μm). WD 0137B’s opacities are measured at P = 6  bar, and EPIC 2122B’s opacities are measured at P = 1 bar. These pressure levels correspond to the approximate positions where the contribution functions at the 1.4 μm H2O band peak. The flux contribution functions and thermal profiles are presented in the lower panels. The blue, green, orange, and red solid lines show the normalized flux contribution functions at wavelengths of 1.1, 1.3, 1.5, and 1.6 μm. The black dashed lines are the thermal profiles. In the daysides of both objects, temperature inversions occur in the pressure range of 1 bar to 10 bar.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: The nightside spectra of WD 0137B (left) and EPIC 2122B (right) and their best-fitting models. The same as in Figure 14, the observations are shown in black solid lines, the 1σ uncertainties are in black shades, and the models are in colored lines. The left panel compares the BT Settl and Sonora models with the nightside spectrum of WD 0137B. In the right panel, a ∼1300 K blackbody fits reasonably well to the low-S/N nightside spectrum of EPIC 2122B.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: Comparing the day/night flux (left) and brightness temperature contrasts (right) of WD 0137B and EPIC 2122B with hot Jupiters. The left panel includes relative flux contrasts of hot Jupiters measured in Spitzer/IRAC 3.6 μm (open triangle) and 4.5 μm (closed triangle) and HST/WFC3/G141 (blue circle). The flux contrasts of WD 0137B and EPIC 2122B are represented as rectangular patches, with the vertical lengths representing the standard deviation of A  F  within the span from 1.12 to 1.65 μm. Several representative band-averaged flux and brightness contrasts are overplotted to demonstrate the wavelength-dependent variations. The right panel demonstrates the brightness temperature contrasts using markers identical to those in the left panel. Theoretical ΔT  B –T eq relations based on Komacek & Tan (2018) are overplotted in solid and dashed lines, representing whether or not hydrogen dissociation and recombination are considered in the models.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: The evolution of WD 0137B and EPIC 2122B on the substellar color–magnitude diagram. We use the synthetic F127M and F153M photometry of WD 0137B and EPIC 2122B to estimate the J and H magnitude and overplot their tracks (green and magenta squares) onto the substellar CMD established using data from Best et al. (2020). Several measurements of EPIC 2122B near its nightside are discarded because of low S/Ns. For the WD 0137B and EPIC 2122B tracks, we also overlay the best-fitting second-degree polynomials with solid lines to highlight the overall trends. The substellar CMD is color-coded by spectral types: M in brown, L in red, and T in blue. For comparison, we overplot the Sonora cloudless CMD tracks in three surface gravities (dashed–dotted line: ﹩\mathrm{log}g=4.5;﹩ dashed line: ﹩\mathrm{log}g=5.0;﹩ solid line ﹩\mathrm{log}g=5.5﹩). The WD 0137B track connects the early-L and mid-T regions in approximately a straight line that is parallel to the Sonora tracks in the same color range. The EPIC 2122B track is parallel to the M to mid-L evolution, but has a bluer color. The gray solid line shows a semi-empirical model for EPIC 2122B. It is constructed by conducting synthetic photometry on a series of spectral mixtures composed of its best-fitting day- and nightside models.
Paper: HST/WFC3 Complete Phase-resolved Spectroscopy of White-dwarf-brown-dwarf Binaries WD 0137 and EPIC 2122
Authors: Yifan Zhou, Dániel Apai, Xianyu Tan, Joshua D. Lothringer, Ben W. P. Lew, Sarah L. Casewell, Vivien Parmentier, Mark S. Marley, Siyi Xu, 偲艺 许, L. C. Mayorga
Figure caption: A comparison of the nightside temperatures of the irradiated brown dwarfs and the substellar evolutionary track. The blue curve is the M = 55 M Jup substellar cooling track in the Saumon & Marley (2008) model. The yellow and green dashed lines mark the nightside temperatures of WD 0137B and EPIC 2122B, respectively, and the shades show the uncertainties (note the asymmetrical error in T eff night−side of EPIC 2122B). The nightside temperature parallels intercept the cooling curve at 4.0 Gyr and 2.1 Gyr.
Paper: DELVE-ing into the Jet: A Thin Stellar Stream on a Retrograde Orbit at 30 kpc
Authors: P. S. Ferguson, N. Shipp, A. Drlica-Wagner, T. S. Li, W. Cerny, K. Tavangar, A. B. Pace, J. L. Marshall, A. H. Riley, M. Adamów, J. L. Carlin, Y. Choi, D. Erkal, D. J. James, Sergey E. Koposov, N. Kuropatkin, C. E. Martínez-Vázquez, S. Mau, B. Mutlu-Pakdil, K. A. G. Olsen, J. D. Sakowska, G. S. Stringfellow, B. Yanny
Figure caption: The DELVE DR1 region where our search was performed is shown in light blue. The additional region (the Jet Bridge) that was searched is shown as a light orange patch. The solid black line indicates the plane of the Milky Way (b = 0°) and the two dashed lines indicate b = ± 10°.
Paper: DELVE-ing into the Jet: A Thin Stellar Stream on a Retrograde Orbit at 30 kpc
Authors: P. S. Ferguson, N. Shipp, A. Drlica-Wagner, T. S. Li, W. Cerny, K. Tavangar, A. B. Pace, J. L. Marshall, A. H. Riley, M. Adamów, J. L. Carlin, Y. Choi, D. Erkal, D. J. James, Sergey E. Koposov, N. Kuropatkin, C. E. Martínez-Vázquez, S. Mau, B. Mutlu-Pakdil, K. A. G. Olsen, J. D. Sakowska, G. S. Stringfellow, B. Yanny
Figure caption: Stellar density map from the DELVE photometry showing the Jet stream at a distance modulus of m − M = 17.28 (D ⊙ = 28.6 kpc). The orange points show the extent of the stream identified by Jethwa et al. (2018), and the blue points denote the new extent of the stream as detected in main-sequence turn-off (MSTO) and blue horizontal branch (BHB) stars as determined in this study. The solid black line in the bottom right indicates the plane of the Milky Way (b = 0°), and the dashed line shows b = 10°.
Paper: DELVE-ing into the Jet: A Thin Stellar Stream on a Retrograde Orbit at 30 kpc
Authors: P. S. Ferguson, N. Shipp, A. Drlica-Wagner, T. S. Li, W. Cerny, K. Tavangar, A. B. Pace, J. L. Marshall, A. H. Riley, M. Adamów, J. L. Carlin, Y. Choi, D. Erkal, D. J. James, Sergey E. Koposov, N. Kuropatkin, C. E. Martínez-Vázquez, S. Mau, B. Mutlu-Pakdil, K. A. G. Olsen, J. D. Sakowska, G. S. Stringfellow, B. Yanny
Figure caption: Top: Jet stream density after applying the same matched filter as Figure 2. Additionally, deviations from great circle path ϕ 2 = 0° are clearly seen. The orange points show the extent of the stream identified by Jethwa et al. (2018), and the blue points denote the new extent of the stream as detected in MSTO and BHB stars. For the range ϕ 1 < − 12.°7 or > 10° the stream is only detected using BHB stars. Middle: Schlegel et al. (1998) dust map of the same region. Bottom: survey coverage map where the color shows the fraction of each pixel that is observed in the DELVE survey. White corresponds to observed fractions lower that 0.5 which are excluded from our analysis, and the grayscale ranges from light to dark with observed fractions of 0.7–1. The red dashed lines show the track of the Jet stream.
Paper: DELVE-ing into the Jet: A Thin Stellar Stream on a Retrograde Orbit at 30 kpc
Authors: P. S. Ferguson, N. Shipp, A. Drlica-Wagner, T. S. Li, W. Cerny, K. Tavangar, A. B. Pace, J. L. Marshall, A. H. Riley, M. Adamów, J. L. Carlin, Y. Choi, D. Erkal, D. J. James, Sergey E. Koposov, N. Kuropatkin, C. E. Martínez-Vázquez, S. Mau, B. Mutlu-Pakdil, K. A. G. Olsen, J. D. Sakowska, G. S. Stringfellow, B. Yanny
Figure caption: Left: proper motions of candidate BHB stars along the Jet stream. The green box shows our proper motion selection for likely members. Contributions from the Milky Way foreground and stellar halo are seen at ﹩({\mu }_{{\phi }_{1}}^{\star },{\mu }_{{\phi }_{2}})\sim (0.5,2)﹩ and (0.5, 0) mas yr−1 respectively Right: on-sky distribution (top) and distances modulus (bottom) of candidate BHB stars that are likely associated with the Jet stream. The matched-filter stream track (Equation (2)) is shown as a green dashed line on the top plot, and the linear fit on distance modulus, (m − M), of the candidate BHB stars (Equation (3)) is shown as a green dashed line on the bottom plot.
Paper: DELVE-ing into the Jet: A Thin Stellar Stream on a Retrograde Orbit at 30 kpc
Authors: P. S. Ferguson, N. Shipp, A. Drlica-Wagner, T. S. Li, W. Cerny, K. Tavangar, A. B. Pace, J. L. Marshall, A. H. Riley, M. Adamów, J. L. Carlin, Y. Choi, D. Erkal, D. J. James, Sergey E. Koposov, N. Kuropatkin, C. E. Martínez-Vázquez, S. Mau, B. Mutlu-Pakdil, K. A. G. Olsen, J. D. Sakowska, G. S. Stringfellow, B. Yanny
Figure caption: Hess difference diagram created by subtracting a background region from the on-stream region. The main sequence of the Jet stream is clearly seen. The Dotter et al. (2008) isochrone we use for our analysis with a metallicity of [Fe/H]= −1.57 and age of τ = 12.1 Gyr is shown as a solid black line. The red line shows the matched filter used to create the optimized map shown in the top row of Figure 6. The left y-axis shows the absolute magnitude of sources and the right y-axis shows the corresponding apparent magnitude at ϕ 1 = 0°.